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NATIONAL RADIO ASTRONOMY OBSERVATORY

FINAL PROGRAM OPERATINGFY 20 14

Associated- Universities. Inc

PLAN

Title: Program Operating Plan FY 2014 Author: Wingate, ADs Date: 03/26/2014

NRAO Doc. #: PMD00025 Version: Final

The Final NRAO Program Operating Plan

FY 2014

PREPARED BY ORGANIZATION DATE

Wingate, AD’s NRAO 03/26/2014

APPROVALS (Name and Signature) ORGANIZATION DATE

T. Beasley Director’s Office 03/26/2014

Title: Program Operating Plan FY 2014 Author: ADs Date: 03/26/2014

NRAO Doc. #: PMD00025 Version: Final

Change Record

VERSION DATE REASON Final 03/26/2014 Updated the Financial tables:

• Added CDL as a separate column • Added WBS Number Code • Added FTE’s for all cells; where FTEs < 3, that is

noted with an * • New Table: Observatory Financial/FTE Projections

by Site – shows activity occurring at each site. Note, all VLBA activity is recorded in Socorro.

• New Table: NRAO Observatory Central Services, By Location - shows Common Cost activity by location. Observatory Central Services expenses are allocated across all fund sources via a 30% surcharge on expenditures. Both the costs allocated and the allocation mechanism are compliant with A-21 and A-133.

03/26/2014 Updated the Diversity section 1.0 09/30/2013 Preliminary POP

The Final NRAO

Program Operating Plan

FY 2014

March 28, 2014

The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.

Table of Contents

1 Overview ...................................................................................................................... 2 1.1 Structure of the Plan ...................................................................................................... 2 1.2 Financial and Budget Considerations ........................................................................... 3

2 Science Programs ....................................................................................................... 4

3 Observatory Science Operations .............................................................................. 7 3.1 Science Support and Research ...................................................................................... 7

3.1.1 Telescope Time Allocation ....................................................................................................................... 7 3.1.2 Science User Support ................................................................................................................................ 8 3.1.3 Science and Academic Affairs ................................................................................................................ 11 3.1.4 Science Support and Research Services .............................................................................................. 13 3.1.5 Science Support Research Major Milestones ..................................................................................... 14

3.2 Observatory Science Operations Financial/FTE Projection ..................................... 15

4 Observatory Telescope Operations ........................................................................ 16 4.1 Atacama Large Millimeter/submillimeter Array....................................................... 16

4.1.1 Construction .............................................................................................................................................. 16 4.1.2 Operations ................................................................................................................................................. 18 4.1.3 Maintenance and Renewal ...................................................................................................................... 21 4.1.4 ALMA Major Milestones ......................................................................................................................... 23

4.2 Very Large Array .......................................................................................................... 24 4.2.1 Operations ................................................................................................................................................. 24 4.2.2 Upgrade and Enhancement Projects .................................................................................................... 27 4.2.3 Maintenance and Renewal ...................................................................................................................... 30 4.2.4 VLA Major Milestones ............................................................................................................................. 32

4.3 Very Long Baseline Array ............................................................................................ 34 4.3.1 Operations ................................................................................................................................................. 34 4.3.2 Upgrade and Enhancement Projects .................................................................................................... 36 4.3.3 Maintenance and Renewal ...................................................................................................................... 37 4.3.4 VLBA Major Milestones ........................................................................................................................... 39

4.4 Green Bank Telescope ................................................................................................. 40 4.4.1 Operations ................................................................................................................................................. 41 4.4.2 Upgrade and Enhancement Projects .................................................................................................... 43 4.4.3 Maintenance and Renewal ...................................................................................................................... 43 4.4.4 GBT Major Milestones ............................................................................................................................. 45

4.5 Observatory Telescope Operations Financial/FTE Projections ............................... 46

5 Observatory Development Programs .................................................................... 48 5.1 CDL Development ....................................................................................................... 48

5.1.1 Phased Array Feeds .................................................................................................................................. 48 5.1.2 Integrated Receivers ................................................................................................................................ 49 5.1.3 CDL Development Major Milestones .................................................................................................. 50

5.2 ALMA Development .................................................................................................... 51 5.2.1 Development Studies ............................................................................................................................... 51 5.2.2 Development Projects ............................................................................................................................. 52 5.2.3 Ongoing Projects Summary .................................................................................................................... 52

5.3 GBT Developments ...................................................................................................... 53 5.3.1 ARGUS ........................................................................................................................................................ 54

5.3.2 MUSTANG ................................................................................................................................................. 54 5.3.3 GBT Development Major Milestones .................................................................................................. 54

5.4 Observatory Development Programs Financial/FTE Projection ............................. 55

6 Observatory-wide Services ...................................................................................... 56 6.1 Central Development Laboratory Productions, Maintenance & Repair ................ 56

6.1.1 CDL Major Milestones ............................................................................................................................ 58 6.2 Data Management & Software Department (DMSD) .............................................. 59

6.2.1 Software Development ............................................................................................................................ 59 6.2.2 ALMA System Software .......................................................................................................................... 60 6.2.3 VLA/VLBA System Software .................................................................................................................. 62 6.2.4 GBT System Software .............................................................................................................................. 62 6.2.5 Scientific Information Services ............................................................................................................... 63 6.2.6 DMSD Major Milestones ......................................................................................................................... 64

6.3 Program Management Department ........................................................................... 67 6.3.1 PMD Major Milestones ............................................................................................................................ 68

6.4 Education and Public Outreach .................................................................................. 69 6.4.1 STEM Education ........................................................................................................................................ 69 6.4.2 News and Public Information ................................................................................................................. 71 6.4.3 EPO Major Milestones ............................................................................................................................. 73

6.5 Administration .............................................................................................................. 74 6.5.1 Business Services ....................................................................................................................................... 74 6.5.2 Contracts and Procurement .................................................................................................................. 74 6.5.3 Environmental, Safety & Security .......................................................................................................... 74 6.5.4 Management Information Systems ........................................................................................................ 74 6.5.5 Technology Transfer Office ................................................................................................................... 75 6.5.6 Administration Major Milestones .......................................................................................................... 75

6.6 Human Resources ......................................................................................................... 76 6.6.1 Human Resources Major Milestones ................................................................................................... 76

6.7 Diversity ........................................................................................................................ 77 6.7.1 Diversity Major Milestones ..................................................................................................................... 77

6.8 Computing & Information Services ............................................................................ 78 6.8.1 Common Computing Environments .................................................................................................... 79 6.8.2 Communications and Network ............................................................................................................. 79 6.8.3 Computing Security .................................................................................................................................. 79 6.8.4 Site Specific Facilities Infrastructure ..................................................................................................... 79 6.8.5 CIS Major Milestones ............................................................................................................................... 80

6.9 Director’s Office ........................................................................................................... 81 6.9.1 Communications ....................................................................................................................................... 81 6.9.2 New Initiatives ........................................................................................................................................... 82 6.9.3 Spectrum Management ............................................................................................................................ 82 6.9.4 Director’s Office Major Milestones ...................................................................................................... 83

6.10 Observatory-wide Services Financial/FTE Projections ............................................. 84 Appendix A: Preliminary Financial Plan & Work Breakdown Structure .................. 86 Appendix B: Major Milestones Summary .................................................................... 93 Appendix C: FY 2014 NRAO Infrastructure Maintenance & Renewal Summary .. 103 Appendix D: FY 2013 Annual Progress Summary ..................................................... 110 Appendix E: Work For Others ..................................................................................... 117 Appendix F: Acronyms .................................................................................................. 119

NRAO | FY 2014 Program Operating Plan 1

Executive Summary

FY 2014 will mark the completion of the ALMA-North America construction project and the transition to full ALMA science operations, a highly anticipated event across the international community. The North American ALMA Science Center (NAASC) will support the user community in their exploration of Early Science data, offering expert assistance with proposal and observing preparation, data acquisition, reduction, and analysis. The Very Large Array will be the world’s most capable and versatile centimeter-wave imaging array, offering a suite of robust and scientifically powerful observational capabilities that have been designed to address the highest priority scientific interests of the community. The highly successful Resident Shared Risk Observing program will continue to support on-site visits by community experts. VLBA operations in FY 2014 will emphasize stabilizing and documenting existing capabilities, and improving the array’s ease-of-use and reliability. Science operations will emphasize Large/Key Science Projects, especially those that make effective use of the array’s unique astrometric capabilities. In addition to a regular infrastructure maintenance and renewal program, upgrade projects will focus on retiring legacy hardware and software systems. The GBT will continue to offer the community robust single-dish operation in FY 2014 from meter to millimeter wavelengths. GBT development programs will continue in FY 2014 in collaboration with research groups at universities and colleges that will take advantage of the latest technologies to provide new capabilities. A portfolio of development programs will drive forward-looking research and development in FY 2014 that is aligned with the 2010 Decadal Survey science and recommendations. The Central Development Laboratory will continue to support the evolution of NRAO’s existing facilities and will develop the technologies required to help the community realize the next generation of radio astronomy facilities. ALMA, VLA, GBT, and VLBA Development programs will support FY 2014 projects and studies that will deliver new research capabilities to the community. Data Management and Software (DMS) will continue to develop vital post-processing capabilities for the Common Astronomy Software Applications (CASA) package, emphasizing VLA and ALMA support. The CASA pipeline will significantly evolve with the commissioning of new observing modes. The NRAO Science Archive structure and interface will be modernized. New requirements will drive updates to NRAO proposal submission and observation preparation software tools. DMS will continue to develop and improve the ALMA, GBT, VLA, and VLBA system software. NRAO will engage the public in the scientific and technical adventure of radio astronomy through its Education and Public Outreach (EPO) program. FY 2014 will yield numerous opportunities for increasing public awareness, particularly the accelerating scientific output from ALMA and VLA. To effectively and efficiently carry out the numerous tasks required to fulfill its mission, NRAO will continue to improve its cost-effective operations model that is based on Observatory-wide planning, prioritization, administration, and management and that uses the collective expertise and resources available across the Observatory.


1 OVERVIEW

This National Radio Astronomy Observatory (NRAO) Program Operating Plan (POP) describes the planned allocation of the Observatory’s Fiscal Year (FY) 2014 funding from the National Science Foundation Division of Astronomical Sciences (NSF-AST) in support of its mission to enable forefront research into the Universe at radio wavelengths. The period of performance is 1 October 2013 through 30 September 2014. 1.1 Structure of the Plan The NRAO POP structure reflects the Observatory’s primary functions – Science Programs, Science Operations, Telescope Operations, Development Programs, and Observatory-wide Services – and describes the FY 2014 goals, milestones, and deliverables for each major NRAO organization, program, and project. Section 2 describes the key community-driven science programs and goals that NRAO envisions supporting in FY 2014. Operating synergistically with optical, infrared, and X-ray telescopes on the ground and in space, NRAO telescopes will enable astrophysical discovery in FY 2014 over a broad range of key problems in modern astrophysics and with a focus on the highest priority science themes of the 2010 Decadal Survey report, New Worlds, New Horizons in Astronomy & Astrophysics (NWNH). Section 3 details the NRAO FY 2014 Science Support and Research (SSR) activities that will strive to maximize the scientific impact of NRAO telescopes, provide ready access to all NRAO telescopes and services, expand access to new users, improve user services, and directly support the Observatory’s user community. Section 4 details the numerous and vital FY 2014 activities that will be associated with telescope construction and operations at each of the four NRAO telescopes: the Atacama Large Millimeter/submillimeter Array (ALMA); the Jansky Very Large Array (VLA); the Very Long Baseline Array (VLBA); and the Robert C. Byrd Green Bank Telescope (GBT). Section 5 describes FY 2014 NRAO Development Programs that: (a) will develop critical capabilities for upgrading NRAO facility performance and next generation facilities; (b) will assist the community in realizing high priority mid-scale projects recommended by NWNH; (c) support community and industry collaborations, new scientific initiatives, advancements in state-of-the art technologies, and/or new funding opportunities. Section 6 describes FY 2014 plans for Observatory-wide services, including: (a) Central Development Lab (CDL) Laboratory production, maintenance, and repair; (b) data management and software; (c) program management; (d) education and public outreach; (e) administration, (f) human resources and diversity; (g) computing and information systems, and (h) the Director’s Office. Seven appendices provide additional information in support of Sections 2 through 6. Appendix A is the Preliminary Financial Plan and Work Breakdown Structure (WBS) for FY 2014. Appendix B summarizes the major FY 2014 milestones given in each of Sections 2 – 6. Appendix C provides the NRAO FY 2014 Infrastructure Maintenance and Renewal plan and schedule for each of ALMA, VLA, VLBA, GBT, CDL, and NRAO Headquarters (HQ). Appendix D is the Q1-Q3 version of the NRAO FY 2013 Annual Progress Summary that will be delivered with the final NRAO FY 2014 POP. Appendix G lists and defines all acronyms appearing in this POP.


1.2 Financial and Budget Considerations This POP is written to a balanced budget based on NSF-AST FY 2014 projections for NRAO and the following NSF Scientific Program Orders (SPOs), Cooperative Support Agreements (CSAs) and other funding elements:

• NSF SPO-2 ALMA Construction • NSF SPO-4 Green Bank Solar Burst Radio Spectrometer • NSF SPO-7 ALMA Japan • NSF CSA-1 Management and Operations of the NRAO • NSF CSA-2 Operations and Maintenance of the ALMA • NSF CSA-3 Interagency Agreements Associated with Base Operations • NSF CSA-4 Research Experience-Teachers and Undergraduates • Non-programmatic activities associated with NSF, (i.e., collaborations with other NSF Divisions,

other educational institutions funded by NSF, etc.)

ALMA North American Operations funding is expected to continue its planned, long-term ramp up in FY 2014, though NRAO North American (non-ALMA) operations funding is expected to decline. A small amount of financial carryover is typically maintained as reserve to address expected deficits in future years, unexpected U.S. dollar to Chilean Peso exchange rate fluctuations, variations in assumed inflation or benefit rates, or sudden cash needs for unpredictable events such as infrastructure or other emergencies.

The FY 2014 WBS enables visibility and clarity across all business units and sites. All financial tables in this POP reflect this WBS structure. Details of the preliminary funding profile – new funds, carryover, total available, construction – and the WBS are provided in Appendix A.


2 SCIENCE PROGRAMS

In 2014, NRAO’s monumental projects ALMA and the Karl G. Jansky Very Large Array (VLA) will have moved from construction and early science phase, to full operations. This is a major milestone in modern astronomy, representing an order of magnitude or more improvement in observational capabilities from 1 GHz up to 1 THz. In parallel, the Robert C. Byrd Green Bank Telescope (GBT) and Very Long Baseline Array (VLBA) will continue their dramatic improvement, including expanded frequency coverage, increased sensitivity and wide field imaging capabilities. Operating synergistically with the next generation optical, infrared, and X-ray telescopes, the NRAO facilities will enable astrophysical discovery over a remarkably broad range of key problems in modern astrophysics, as identified in NWNH. Using the Observatory facilities, the community will carry out precision cosmological measurements, test fundamental physics, and study astrophysics and chemistry from our Galaxy to the first galaxies in the Universe. These programs will probe deep into the earliest, most intense, and optically obscured phases of planet, star, galaxy, and black hole formation; reveal the cool dense gas from which stars form; and provide essential tools for studying magnetic fields and high energy cosmic phenomena. In FY 2013, results from the ALMA Cycle 0 program demonstrated clearly the revolutionary advance in submillimeter astronomy which ALMA represents, with unprecedented images being made of planet, star, and galaxy formation. Likewise, the first 8 GHz bandwidth VLA observations ushered in a new era in centimeter astronomy, with numerous, dramatic science results published in areas ranging from Galactic protostellar clouds to imaging the molecular gas in the earliest galaxies. The VLBA represents the world’s ultimate facility for microarcsecond astrometric studies, and sub-milliarcsecond imaging, at frequencies up to 90 GHz. Similarly, the GBT continues to be the most versatile single-dish radio telescope in the world, pioneering studies of extremely low surface-brightness phenomena from cm- to mm-wavelengths, and remains the premier instrument for pulsar studies. These facilities are tools for the entire astrophysical community, as clearly demonstrated by the impressive demand for ALMA, with an oversubscription rate of 8:1, rivaling that of the Hubble Space Telescope (HST). The VLA continues its dominance of centimeter astronomy, with a continued high demand from a broad community, and this demand will only increase as the new capabilities of widefield, wideband, high resolution interferometric imaging are fully realized in 2014. The GBT in 2014 will realize increased use of its wide-field focal plane for rapid and sensitive imaging as the seven element focal plane array at 22 GHz moves into standard operation, and testing commences on new multi-pixel systems at 90 GHz. This is just the first step in the long-range plan to develop truly wide-field imaging with the GBT from 1 GHz to 90 GHz. The VLBA will make full use of sensitivity improvements made over the last two years in performing ground-breaking science return using the ultimate precision astrometry and imaging. The NRAO facilities in 2014 will pursue a community-driven, broad-ranging scientific program with the VLA and ALMA in full operation, and relying on the continually improving capabilities of the GBT and VLBA. Following are some of the examples of programs being pursued over the coming year: Extrasolar planets: The field of extrasolar planets is entering a new age with the discovery of hundreds of planets and proto-planetary disks at optical, near-infrared (IR), and radio wavelengths. The first observations with the VLA and ALMA are already playing a crucial role in the study of the early phases of planet formation, by imaging the dust and gas in protoplanetary disks, potentially down to AU-scales. The VLA and ALMA provide the high resolution required to image dust gaps cleared by forming planets in protoplanetary disks. ALMA may detect directly the warm dust associated with forming Jupiter-like planets. VLA is crucial for probing the most optically thick inner regions of protoplanetary


disks and will be sensitive to large dust grains. The GBT in 2014 will perform large-scale surveys for dark, protoplanetary disks, and study the composition of debris disks. A higher sensitivity VLBA will be used to search for planets by their astrometric signatures on nearby radio-emitting stars. The radio observations complement the studies of proplyds, or the dusty shadows of protoplanetary disks, as imaged in the optical, and the IR studies of dust spectra. Testing Gravity: A major goal in modern physics is to open up a totally new window on the Cosmos through the detection of gravity waves. The GBT has begun a search for nano-Hertz gravitational waves from super-massive black holes (SMBH) throughout the Universe, using a network of pulsars as ultra-high precision clocks spread across the Galaxy. These pulsars act as the far ends of the arms of a Galactic-scale gravitational wave detector. The North American program, known as NANOGrav, is a collaborative effort between Universities and the NRAO. In 2013, NANOGrav, using data from the GBT, published the first limits on the nHz gravitational wave background, which approach the expected signal from astronomical sources (merging binary supermassive black holes). In the coming year, they will be expanding this program using the dramatic improvements from new pulsar timing back-ends and timing techniques, with the potential for the first detection of the gravity wave stochastic background within two or three years. NANOGrav’s objectives and technology will complement the higher frequency laser interferometer searches such as Advanced LIGO (Laser Interferometer Gravitational Wave Observatory), and LISA (Laser Interferometer Space Antenna). In parallel, searches for new pulsars continue with the GBT, with the hope of finding a black hole-pulsar binary, while a search is underway for pulsars orbiting the SMBH at the Galactic center. Either or both of these will result in the ultimate laboratory to study strong field General Relativity. Precision Astrometry: The field of ultra-high precision astrometry has reached maturity, relying fundamentally on the capabilities of the VLBA. Revolutionary results have been produced in the last year on areas ranging from Galactic structure and the dynamics of star forming regions, to proper motions in local galaxies, to obtaining a key cosmological benchmark measurement of the local expansion rate of the Universe. The coming year will see continued progress in this area, with large programs on the VLBA to map out the Galactic spiral arms and determine Galactic structure in unprecedented detail. A truly remarkable prospect is the potential to determine the three-dimensional motions of nearby galaxies, and hence constrain the dynamical mass model for the local group. Galaxy Formation: Centimeter through submillimeter wavelength observations play crucial roles in the studies of the molecular lines that probe the fuel for star formation in forming galaxies; the atomic fine structure lines that are the principal coolants for the interstellar medium gas in distant galaxies; the thermal dust continuum emission that is a key star formation rate estimator; and the radio synchrotron emission that measures star formation and signals the presence of relativistic jets. In the last year, the sensitivity and imaging capabilities of the VLA and ALMA have been demonstrated with dramatic effect, imaging at sub-arcsecond resolution the molecular gas in the first galaxies. In parallel, the GBT has performed valuable surveys for molecular line galaxies in the distant Universe, and obtained ‘blind’ redshifts for dust-obscured galaxies using molecular lines. An area that has seen an explosion of interest through the new capabilities of ALMA is the study of atomic fine structure line emission from early galaxies, both as a ‘redshift machine’ for the first galaxies, and as the most effective method to determine gas dynamics in forming galaxies at sub-kiloparsec resolution. Fine structure line observations now dominate distant galaxy studies with ALMA. These centimeter through (sub)mm observations of the cool gas in early galaxies are an essential complement to the near-IR observations that probe the stars and ionized gas, and the X-ray observations that reveal the Active Galactic Nuclei (AGN). Together, observatories operating from centimeter to X-ray wavelengths in the coming decade are providing the requisite panchromatic view of the processes involved in the formation of the first generation of galaxies and SMBHs, and cosmic reionization. Indeed, it is clear that, in the coming years,


studies of galaxy formation will be dominated by observations of the cool atomic and molecular gas, dust, and star formation, at cm through submillimeter (submm) wavelengths using the NRAO facilities. VLA deep, wide surveys: the new broad band system at the VLA will revolutionize radio surveys in the coming year, through subarcsecond resolution surveys of wide areas with sensitivities approaching a 1uJy. Surveys are currently underway of the Cosmos field and other cosmological deep fields with areas of a few square degrees. All of the areas above have been called-out by the astronomy community in NWNH as high-priority goals in the coming decade. Over the next year the NRAO is fostering development of telescopes and techniques to realize other high-priority scientific areas highlighted in NWNH, including: Cosmic Reionization: Exploring cosmic reionization, when light from the first galaxies acts to reionize the pervasive neutral intergalactic medium left over from recombination, represents the last frontier in studies of large scale structure formation. NRAO is involved with the development of low frequency radio arrays to image the HI 21 cm signal from the neutral gas, considered the best probe of this last unexplored phase of cosmic evolution. Frequency Agile Solar Radiotelescope (FASR): The FASR project represents the next major step in studies of the Sun and space weather. The project is technically ready, and rated as one of the highest science priorities in NWNH. NRAO is a founding institutional member of the FASR consortium. Time-domain: Exploring the time-domain is a key area of discovery in astronomy. The dramatically improved and unique power of the NRAO facilities will play a dominant role in studies of the variable radio sky, and is adopting operational models and developing technical capabilities that will enable rapid response studies of the variable radio sky with microJy sensitivity. NRAO is a member of the Large Synoptic Survey Telescope (LSST) consortium, and working with the NVO on time-domain astronomy. In FY 2014, the VLBA will begin exploring early stage time evolution of Gamma Ray Bursts by steering onto sources within minutes of a high-energy trigger.


3 OBSERVATORY SCIENCE OPERATIONS

3.1 Science Support and Research The NRAO Science Support and Research (SSR) department coordinates, aligns, and manages the collective efforts of the three NRAO sites—Charlottesville, Virginia; Socorro, New Mexico; and Green Bank, West Virginia—to support science users of NRAO facilities, to broaden the Observatory’s impact through education and visitor programs, and to oversee the research and performance of the scientific staff. It does so through three divisions:

• Telescope Time Allocation (TTA) manages the process and tools by which users prepare and submit proposals for use of NRAO telescopes, as well as the proposal evaluation and time allocation process.

• Science User Support (SUS) is responsible for providing the scientific community with the support necessary to execute successful scientific programs with NRAO facilities including the GBT, VLA, VLBA and ALMA.

• Science and Academic Affairs (SAA) oversees the research activities of the scientific staff, and staff development, as well as education and visitor programs.

In addition, SSR provides two observatory-wide services: 1) NRAO reference comprises the NRAO Library and the Historical Archives; 2) Statistics and metrics aggregates data used to report various metrics to the NSF, to AUI, to external review committees, and for internal use. 3.1.1 Telescope Time Allocation The Telescope Time Allocation (TTA) division is responsible for overseeing the process by which proposals for the use of NRAO North American telescopes—the VLA, the VLBA, and the GBT—are prepared, submitted, and peer reviewed; and by which time allocation recommendations are made to the NRAO Director and then communicated to proposers and suitably publicized to the community. As an international project, ALMA proposals are managed separately by the JAO. This proposal process is common to all three telescopes. It is semester-based with proposal deadlines of 1 February and 1 August annually. For each semester, proposals are evaluated on the basis of scientific merit by eight Science Review Panels (SRPs) whose members are recruited from the community. Proposals are also reviewed for technical feasibility by members of the NRAO scientific staff. All reviews are forwarded to the Time Allocation Committee (TAC). The TAC consists of the chairs of the SRPs and is charged with recommending time allocations to the NRAO Director. After Director review and approval, disposition letters are sent to proposers and the approved science program is posted. TTA is also responsible for gathering the requirements for the software tool suite used in support of this process, conveying those requirements to Data Management and Software department (DMS) for implementation, as well as testing and validating new releases of these tools from DMS. The tools include the Proposal Submission Tool (PST), used for proposal preparation and submission, and for management of the science and technical review process; and the Proposal Handling Tool (PHT) and the Green Bank Session Editor (GBSE), used in support of the TAC meeting. Finally, TTA is responsible for ensuring that the necessary documentation in support of all TTA activities and tools is available and up to date. Documentation supporting ALMA Call for Proposals (CfPs) and observing proposals is currently handled through SUS.


Calls for Proposals: The CfP for semester 14A occurred in Quarter Four (Q4) of Fiscal Year (FY) 2013 and will continue in Q1 of FY 2014 with the TAC meeting and the Director’s Review. It will conclude with the posting of the approved science program. The NRAO will issue a CfP for semester 2014B in early Q2 FY 2014, with a proposal submission deadline of Feb 1. The CfP for semester 2015A will be early in Q4 FY 2014, with a proposal submission deadline of Aug 1. Documentation will be updated to alert users to new observing modes supported by telescope operations, new PST features, and news regarding changes to policies or procedures. The ALMA Cycle 2 CfP will occur on 24 October 2013 and will be coordinated through the Joint ALMA Observatory (JAO) and the regional centers. Proposal Review: Proposals for semester 2014B will be reviewed in parallel for scientific merit (by the SRPs) and for technical feasibility (by members of the NRAO scientific staff) in Q2 FY 2014. Similarly, proposals for semester 2015A will be reviewed in Q4 FY 2014. Members of the NRAO SRPs typically serve for two years, or four semesters. New SRP members are recruited during Q1 of each fiscal year. Time Allocation: The TAC will meet to recommend time allocations for semester 2014A in Q1FY 2014 and will meet to recommend time allocations for semester 2014B in Q3 FY 2014. Software Requirements and Testing: Software requirements for TTA tools begins shortly after each TAC meeting. PST requirements are gathered from TTA staff with input from users, the SRPs, and the TAC. The TAC also provides NRAO with useful feedback on the PHT and the GBSE, used to support TAC function. Priority is given to the PST initially as it must be ready for use when the CfPs are made. Hence, the implementation and testing of PST features will occur in Q1 and Q3 of FY 2014, whereas the implementation and testing of PHT/GBSE features will occur in Q2 and Q4 of FY 2014. TTA Review: The NRAO will have completed six semesters of proposal evaluation and time allocation under the panel-based system at the end of Q1 FY 2014. SSR will therefore conduct a review of TTA to assess the effectiveness of the process and the tools used to support it. The review will take place at the end of Q1 FY 2014 and will include relevant members of TTA staff, former members of SRPs and the TAC, and users from the community. Joint ALMA and NRAO NA Proposals: In Q4 FY 2013 a plan for coordinating proposals submitted for ALMA Cycle 2 observing jointly with NRAO’s North American facilities was developed. This will be implemented in Q2 FY 2014 in the NRAO 2014B CfP. 3.1.2 Science User Support Science User Support (SUS) is responsible for providing the scientific community with the support necessary to execute successful scientific programs with NRAO facilities: the GBT, VLA, VLBA and ALMA. The group structures will encompass:

• Community Education and Outreach Services: face-to-face visitor support (including observing runs, data reduction visits, etc.), helpdesk tickets, triage, knowledgebase articles, science forums, scheduling block validation and review, astronomy community days; science meetings and conferences, Science Web content and NRAO user portal interface, user documentation, workshops and tutorials, online training and educational material.


• User Data and Scientific Software Services: pipeline (re)processing, pipeline heuristics and definitions, manual data reduction and quality assurance (QA2 process), Software benchmarking, access and protocols, CASA Scientific Steering Committee (CSSC), large/key/special project support, Archive Access Tool/ALMA Science Archive (AAT/ASA) user interface, integrated help desk services, preprocessing pipeline interface, data staging.

User Documentation, Web Material, and Online Training Material: The NRAO has adopted the PLONE content management system for its web-based content. Many of the documents are now converted and maintained in PLONE, including the VLA and VLBA observational status summaries. In addition, in Q4 FY 2013, the GBTIDL user guide was evaluated and deployed as a PLONE document. As a result of initial investigations by the SUS Web “Tiger Team” in FY 2013, a proposal was prepared and presented to DMS for additional web support to finish the conversion of existing online user documents for the NRAO NA facilities into PLONE in Q4 FY 2013. As such, it is anticipated that the bulk of the remaining work needed for the conversion of these documents in to PLONE will be completed by Q4 FY 2014.

For ALMA, by international agreement, the end user documentation including the ALMA Proposers Guide and Technical Handbook are prepared by the JAO as a stand-alone pdf and as PLONE documents, available off the ALMA Science Portal. Given the anticipated Cycle 2 CfP in October, a review and final edit of all user documentation will be completed before being deployed off the ALMA Science Portal in Q1 FY 2014. As with Cycles 0 and 1, a Cycle 2 User Survey will occur soon after the proposal deadline in Q1 FY 2014 to assess the ease of use of the tools, the proposal preparation process, and interactions with ALMA Regional Center (ARC) staff. A “Lessons Learned” document will be prepared from this survey and for review by the ARCs and the JAO. Finally, in anticipation of ALMA Cycle 3, initial document review and edits will start in Q4 FY 2014.In anticipation of the next CASA releases in FY 2014, all CASAGUIDES will be reviewed, edited and deployed after being fully tested on the new versions of CASA. The deployment of the new CASAGUIDES will take place in Q1 and Q3 FY 2014. Scientific workshops and conferences: NRAO will host or support several scientific workshops and conferences over the course of FY 2014. These include:

• Q1: o International Astronomical Union (IAU) Symposium 303, "The Galactic Center: Feeding

and Feedback in a Normal Galactic Nucleus," will be held in Santa Fe, organized by NRAO staff with sponsorship from NRAO.

• Q2: o NRAO Town Hall and Splinter Sessions organized at the winter American Astronomical

Society (AAS) meeting in Washington, D.C. o 2014 American Association for the Advancement of Science (AAAS) Annual Meeting

(13-17 February 2014) 180 Minute Symposium: Technological Innovations and Their Impact on

Astronomical Discovery (includes ALMA) 180 Minute Symposium: From Dust and Molecules to Planets and Stars 90 Minute Symposium: The Evolution of Galaxies in the Early Universe

• Q3: o Joint Green Bank/China Science Workshop

• Q4: o Special/Splinter Sessions organized at the summer AAS meeting in Boston, MA


o 8th North American ALMA Science Center (NAASC) Sponsored Science Workshop, Charlottesville, VA, Sept 14-18, 2014

User Data and Scientific Software Services In many cases, the role of SUS in user data and scientific software services will be in delivery of data products to the user community, setting science requirements and testing the software before release. For example, ALMA data delivery starting Q1 FY 2014 will be done through the ASA and users can access their data through that interface. However, on those occasions where the NRAO data products are too large, NRAO plans are to continue to provide the necessary data delivery services (i.e. shipping hard disks) to our users staged primarily by user support Data Analysts (DAs) at each site. Observing Preparation and Support Tools: Before each observing semester or cycle, the NRAO and ALMA suites of observing preparation tools need to be fully tested before deployment. Given the timeline of the ALMA Cycle 2 CfP, most of the testing of the ALMA OT and associated ALMA proposal preparation tools will take place in FY 2013. However, NAASC staff will provide input into the requirements for Phase 2 of the OT for Cycle 2 observing preparation anticipated to begin in Q3 FY 2014. ALMA scheduling block (SB) generation and PI approvals will start in Q3 FY 2014 with the first batch of PI approvals due May 1. This process will continue throughout FY 2014. For the NRAO North American facilities, testing of the Observing Preparation Tool (OPT) will take place in Q1 FY 2014 in preparation for the VLA A and D configuration changes and testing for the new release of SCHED for the VLBA will take place in Q4 FY 2014. Pipeline Processing and Heuristics: Throughout FY 2014, while the ALMA reduction pipeline is being tested and refined, manual data reduction will continue on all Cycle 1 data before being released to the user community. For the VLA, testing of the pipeline heuristics and integration of those heuristics into CASA will be completed in Q1 FY 2014. Full testing of the VLA CASA data reduction pipeline will be completed in Q1 FY 2014 with the deployment of that pipeline in the same quarter. For the GBT, testing of the data reduction pipeline will take place starting in FY 2014 on archival GBT data with the expectation that the GBT reduction pipeline will be able to process the archival data products for standard modes (excluding pulsar data) by the end of Q2 FY 2014. Pipeline Reprocessing Interface (RPI): The RPI is to be a web-based application that allows our users to access the NRAO computing clusters in Charlottesville and Socorro to re-run pipeline reductions on their data. Starting in FY 2013, SUS coordinated a RPI Working Group to set the science requirements for the RPI, a process that will continue into FY 2014. During the course of FY 2014, the final science requirements and preliminary user-interface requirements for the RPI will be conveyed to DMS. Integrated ASA/AAT and NRAO/ALMA Science Portal: A large part of the RPI is user access to all data products held either in the ALMA Science Archive or the NRAO Data Archive. Starting in FY 2014, the initial science requirements will be developed on what an integrated access portal to the ASA/AAT will encompass and presented to DMS for prioritization. Completion of the science requirements will be presented to DMS at the end of Q1 FY 2014. Similarly, the NRAO User Portal and ALMA Science Portal are currently built and deployed on very different platforms. In FY 2014, SUS will investigate the feasibility of refactoring the NRAO User Portal and determine the science requirements for a redesign of the portal. A full evaluation of the functionality and usability of the user portal will be conducted before science requirements are developed and delivered to the DMS department in Q3 FY 2014.


3.1.3 Science and Academic Affairs Fostering a strong scientific community of researchers and helping to train the next generation of scientists and engineers remain important parts of the NRAO mission. The NRAO maintains a scientific staff and supports a broad range of student opportunities including undergraduate, graduate, and post-graduate programs; instrument and visitor programs to enhance university-NRAO collaborations; and workshops, schools, and conferences. Despite budgetary pressures, these high priority programs will largely continue in FY 2014. NRAO Scientific Staff The scientific staff is key to telescope testing, operations, user support, and long-range development and planning. Staff members also lead efforts in education of the professional community, as well as public outreach. The SAA, under the SSR, has primary responsibility for the scientific productivity and research environment at the NRAO, overseeing the research aspects of all astronomers, computer scientists, and research engineers at all sites. Specifically, SAA responsibilities include: oversight of scientific staff research travel budget, annual scientific performance appraisals, scientific staff hiring and academic promotions. SAA also supports a modest visitor program, the colloquium series at each site, and the Jansky Lecture. Postdoctoral Fellows SAA oversees the postdoctoral fellowship programs at the NRAO, including the Jansky fellows and project postdoctoral appointments. The Jansky fellowship program is NRAO’s long-standing prize research fellowship program. It is a highly competitive process that attracts some of the best young scientists in the field. Jansky Fellows can be in residence at an NRAO site, or be located at external institutions in the USA. The Jansky selection process occurs in Q1 of each fiscal year. Owing to financial constraints only two new Jansky fellows entered the program this year; hence, there will be a total number of 8 Jansky fellows in FY 2014, with a comparable number of project and other postdoctoral appointments. NRAO also hosts postdoctoral fellows funded by other institutions, such as Hubble, Einstein, and NSF fellows. NRAO has numerous programs in place that foster the professional development of postdocs, highlighted by the annual postdoc symposium: an excellent forum for all postdocs at NRAO (including external Jansky fellows) to present their latest work, and to establish collaborations with their colleagues. The symposium rotates between NRAO sites. Each site has an informal postdoc lunch once per week. Lectures have been presented on career development, and professional development is a key aspect of the mentoring duties of the NRAO staff primarily responsible for the postdoc programs. Each site has various lectures and formal instruction on key skill areas, such as Python programming or training in the use of astronomical tools. NRAO provides substantial research support, including travel, page charge support, and computing resources. Some of the mechanisms that are being implemented for postdoc monitoring include the biannual submittal of progress reports and annual interviews for Jansky Fellows. For external Fellows, NRAO requires an annual progress report from the host institution. Project postdocs are required to participate in the annual NRAO Performance Evaluation Process as per standard scientific staff policy. This includes a functional review by the immediate supervisor, and a scientific review by SAA.


Broader Impacts Undergraduate Programs: The long-running (since 1959) NRAO summer student program continues to be very successful. This 10–12 week program allows approximately 25 students to work under the supervision of NRAO staff members at sites in New Mexico, West Virginia, and Virginia, to carry out original research in astronomy, computing, and engineering. Most of these students are funded through the NSF Research Experience for Undergraduates (REU) program. The REU program is a competed program with an application deadline on February 1 (Q2) of each year. Offers are made on March 1 at the beginning of Q3; students typically arrive at each site in May (Q3) and depart in August (Q4). The NRAO runs a co-op program that enables undergraduate engineering students to gain practical, career-based experience as part of their formal academic education. Students from participating institutions work at NRAO sites for two non-consecutive semesters. Under the supervision of NRAO technical staff, co-op students are engaged in problems on the technological frontier. Historically, three students per semester have been funded through the NRAO operating funds although the program has been curtailed for FY 2014 as a result of fiscal pressures. A modest amount of funds are available for undergraduate internships, where promising undergraduate students participate in scientific or engineering activities, supervised by NRAO staff, over a period of weeks to a semester. Graduate Programs: The NRAO is committed to training the next generation of scientists in radio astronomical science, techniques, and technology. Several NRAO programs exist for this purpose. Graduating seniors and first- and second-year graduate students are able to participate in the NRAO summer student program described above. This gives students experience in radio astronomy research early in their graduate careers, allowing them to incorporate these skills into their thesis research. The NRAO also awards Reber Pre-Doctoral Fellowships to students who have completed institutional requirements for doctoral candidacy so that only their thesis research remains for them to complete their PhDs. Such fellows take up residence at one of the NRAO sites, typically for two years, while they complete their research and thesis under the supervision of an NRAO staff member. The NRAO currently supports seven Reber Pre-doctoral Fellows, a level of support that will continue through FY 2014. The NRAO also supports many of the 100+ PhD students making use of NRAO telescopes each year. Travel reimbursement, low-cost accommodations, and computing facilities are provided on-site to assist these students. The Observatory also supports stays lasting several weeks to several months by students who wish to collaborate with NRAO staff scientists as part of their PhD research. Student Observing Support: Financial support will be available on a competitive basis for students performing observations with ALMA in FY 2014. Students at U.S. universities are eligible for the Student Observing Support (SOS) program, which is designed to cover stipend and miscellaneous expenses such as computers and travel to conferences to a maximum of $35,000. For ALMA Cycle 2 the NAASC will be responsible for the processing and review of SOS proposals associated with ALMA proposals.


3.1.4 Science Support and Research Services Reference The NRAO Library: The NRAO Library has been proactive in migrating to online, distributed access to research and reference materials for NRAO staff and the wider community. In the coming year Library will also continue to expand eBook titles. Contracts for eJournals packages and eJournals access will be negotiated in Q2 FY 2014. Historical Archives: The NRAO Archives actively seeks out, collects, organizes, and preserves institutional records, personal papers, multimedia materials, and oral histories of enduring value that document NRAO development, institutional history, and instrument construction. As the national facility for radio astronomy, the Archives also include materials on the history and development of radio astronomy in the United States, and our growing reputation has made our Archives the de facto repository for U.S. radio astronomy history. As time allows, the Archives will continue to transcribe interviews and mount transcripts on the Web from our collection of Prof. Woodruff T. Sullivan's 255 audio-taped interviews of 20th century radio astronomers. As requested by users, as well as by EPO as they develop public Web pages for NRAO, the Archives will continue to digitize and provide audiovisual and textual material from our collections. Ongoing work will include processing newly received materials to add to the records of NRAO and to our collections of individual scientists' papers, answering NRAO staff requests for information and resources, as well as requests from members of the press and from researchers and writers at other institutions.


3.1.5 Science Support Research Major Milestones

FY 2014

Program Project Q1 Q2 Q3 Q4

Telescope Time Allocation (TTA)

TTA Review 1 Call for proposals 2 3 Science and technical review 4 5 TAC meeting 6 7 Software requirements and testing 8 9 10 11 Documentation 12 13

Science User Services (SUS) Documentation 14,15,16 17 Scientific Workshops and Conferences 18 19 20 Scientific Support for Software 21, 22 23 24,25,26 27,28 Science & Academic Affairs (SAA) Broadening impact 29 30 31,32 33 SSR Services Library 34 Milestones: 1. SSR review of TTA 2. CfP for semester 2014B 3. CfP for semester 2015A 4. SRP and tech review process, semester 2014B 5. SRP and tech review process, semester 2015A 6. TAC meeting for semester 2014A 7. TAC meeting for semester 2014B 8. Update SW tools requirements for TAC support 2014A 9. Update SW tools requirements for PST 2014B 10. Update SW tools requirements for TAC support 2014B 11. Update SW requirements tools for PST 2015A 12. Update documentation for CfP and tools 2014B 13. Update documentation for CfP and tools 2015A 14. HD 4.5 documentation 15. Update ALMA Cycle 2 proposal preparation documentation 16. Update CASAGUIDES 17. Update CASAGUIDES 18. IAU Symposium 303 – The Galactic Center 19. NRAO/China Science Workshop 20. 8th NAASC sponsored science workshop 21. AAT/ASA science requirements 22. Manual reduction of ALMA science data and QA2 23. Manual reduction of ALMA science data and QA2 24. ALMA pipeline tests complete between manual & pipeline products 25. Requirements for integrated science portal 26. Manual reduction of ALMA science data and QA2 27. Reprocessing pipeline interface tested 28. Manual reduction of ALMA science data and QA2 29. Jansky Fellow selection 30. NRAO summer student selection 31. SOS program selection for ALMA Cycle 2 32. Summer Student program begins 33. Summer Student program concludes 34. Renegotiate electronic journals

Deliverables: [1] Review [2] eNews announcement [3] eNews announcement [4] Science and technical reviews [5] Science and technical reviews [6] TAC meeting [7] TAC meeting [8] Requirements for PHT and GBSE [9] Requirements for PST [10] Requirements for PHT and GBSE [11] Requirements for PST [12] User documentation [13] User documentation [14] User documentation [15] User documentation [16] User documentation [17] User documentation [18] Science Symposium [19] Science workshop [20] Science workshop [21] ATT/ASA science requirements [22] Manual reduction of ALMA science data and Q A2 [23] Manual reduction of ALMA science data and Q A2 [24] ALMA pipeline tests complete between manual an pipeline products [25] Requirements for integrated science portal [26] Manual reduction of ALMA science data and Q A2 [27] Reprocessing pipeline interface tested [28] Manual reduction of ALMA science data and Q A2 [29] Jansky Fellow selection [30] NRAO summer student selection [31] SOS program selection for ALMA Cycle 2 [32] Summer student program begins [33] Summer student program concludes [34] Electronic journals


3.2 Observatory Science Operations Financial/FTE Projection


4 OBSERVATORY TELESCOPE OPERATIONS

4.1 Atacama Large Millimeter/submillimeter Array Overview ALMA, an interferometer consisting of 66 total array elements and located at 5000 meters altitude in the high Atacama Desert of northern Chile, was inaugurated in March 2013. All construction of the science instrument will be completed in 2014. Early Science observing is already yielding spectacular results and is changing our understanding of planet and galaxy formation and stellar evolution, among other areas. This global project has been a remarkable example of scientific cooperation and promises to be a world-leading discovery instrument for years to come. FY 2014 marks the end of ALMA-NA construction and the transition to ALMA operations. The production and delivery of antennas, integrated front ends, front end and back end components, correlator quadrants, roads at the Array Operations Site (AOS), and construction software releases were largely completed in calendar year 2012. NA deliverables lingering into FY 2014 include the completion of the installation of the fuse disconnects and 400V cables at the AOS, the delivery of the Front End Thermal Interlock Module, and the delivery of the Front End Handling Vehicles. The NA Integrated Product Teams (IPTs) will focus on warranty support and corrective maintenance of deliverables and the conversion of their conditional acceptances to full with the assistance of the product assurance (PA), quality assurance (QA), and Systems Engineering (SE) staff. NA ALMA personnel will also continue to support assembly, integration, verification, and commissioning activities. 4.1.1 Construction The major FY 2014 activities for each IPT in the ALMA-NA construction project are described below. Management: Regularly scheduled, project-wide meetings for schedule, budget, and configuration control will continue through Q2 FY 2014, with an emphasis on budget control and project close-out. An ALMA Construction Completion and Operations Readiness Review (ACCOR) will be held in January 2014. The Office of Chile Affairs (OCA) in Santiago supports the legal and business affairs of AUI/NRAO in Chile for both construction and operations. The office will continue its administrative services at the ALMA site. The OCA will also continue its oversight of ALMA human resources activities, including contracts, payroll, travel support, and interactions with the labor union of local AUI staff. The office is also responsible for local property management and NRAO import/export activities for ALMA. OCA participation in the aforementioned activities continues into ALMA’s operational phase. The NA construction activities supported by the OCA in Chile include the installation of the AOS power and fiber optic distribution to the antenna stations. The OCA will also monitor NRAO safety in Chile with the supervision of NA Site Safety Officers. Site: The AOS Roads were accepted by the JAO in December 2012. The installation of the AOS Utilities, which is the network of fiber optic and electrical power cables at the high site, is over 99 percent complete. However, adverse weather during the altiplanic and Chilean winters has continued to hamper the completion of this work. The work was also delayed due to an error in the installation of the 400V cables that carry electrical power to the antenna stations. The remaining work is the


installation of the 400V cables and the fuse disconnects in the 23kV system at the AOS. This work is currently scheduled for completion in December 2013. The NA Site IPT will close out the AOS Utilities and Roads contracts in FY 2014. The IPT has already successfully resolved a potential claim of $5M made by the original AOS Utilities contractor who was dismissed from the work. The IPT is addressing another claim initiated by AUI to recover the performance bond that was not paid by the insurance company of the dismissed contractor. While difficult to predict, the decision on this arbitration is expected to be rendered in Q1 FY 2014. Antenna: The last Vertex antenna was accepted by the JAO in November 2012, and was delivered to the AOS in February 2013. All 25 Vertex antennas have now been accepted by the JAO. The NA Antenna IPT will work with PA/QA staff to address any remaining issues with the antennas to convert their conditional acceptances to full. In FY 2014, the IPT will also work with Vertex to address any corrective maintenance and warranty issues with the antennas. Particular attention is being devoted to investigations of temperature-dependent deformations in the antenna surface that cause the surface RMS to exceed specifications at the temperature extremes of the antenna’s operating range. The first of five nutators was conditionally accepted by the JAO in July 2013. The four remaining units have successfully completed their factory acceptance tests in Taiwan, and are being delivered to Chile. The acceptance reviews for these nutators will be held in August 2013. Thus, their delivery will be complete in Q4 2013. All six optical pointing telescopes (OPTs) were delivered to the Operations Support Facility (OSF) by February 2012. The units have been modified to minimize heat dissipation and its related effects within the OPT enclosure to address a temperature-dependent drift of the image produced by the OPT. The OPT acceptance reviews await the vendor’s delivery of as-built drawings and an updated operations manual. The revised documents should be delivered in Q4 FY 2013, and the OPT acceptance reviews should then occur in Q1 FY 2014. Front End: The NA Front End Integration Center (NA FEIC) delivered its last (22nd) front end (FE) in September 2012. NA FE IPT staff will work with the PA/QA staff to address any remaining issues so that FE acceptances can be converted from conditional to full. The deliveries of the Cold Cartridges Assemblies (CCAs) for Bands 3 and 6 were completed in February 2012 and August 2012, respectively. The NRAO also receives non-MREFC (SPO-7) funding from the National Astronomical Observatory of Japan (NAOJ) through the NSF to support the production and delivery of ALMA FE components as part of a Goods and Services Agreement with the NAOJ. The production of the Local Oscillator Warm Cartridge Assemblies (WCAs) for Bands 4 and 8 was completed in January 2013, and the production of the Band 10 WCAs was completed in June 2013. Two major items remain to be completed on the Good and Services Agreement. These are the delivery of 14 additional cold multipliers for each of Bands 4, 8, and 10, and the financial support for the JAO’s integration of Bands 4, 8, and 10 into the assembled FEs at the OSF. The multiplier delivery will be complete in Q2 FY 2014, and the integration work will be complete in FY 2015. A FE Thermal Interlock Module (FETIM) was added late in the project. The module is of low priority, but its design is complete and the first unit has been sent to the OSF for a fit test in an ALMA FE. The production and delivery of the remaining FETIMs will commence with the successful completion of the test. The delivery of the FETIMs is scheduled for completion in Q2 FY 2014.


The production of the FE Handling Vehicles (FEHVs) in 2012 was originally delayed to resolve clearance issues inside the receiver cabin of the European antennas. Once the clearance issue was resolved, the financial forecast for NA at the time indicated there were insufficient funds to support FEHV production. As steps were taken to improve the NA budget, the final critical design review for the FEHV was completed in March 2013, the FEHV design was finalized, and an FEHV production plan was developed. FEHV production will be launched in Q4 FY 2013 provided an upcoming cost to complete analysis shows it can be supported financially. That being the case, the first FEHV is scheduled for delivery in Q2 FY 2014 and the three remaining units should be delivered in Q4 FY 2014. Back End: All construction deliverables from the NA Back End (BE) IPT have been completed. In FY 2014, the NA BE IPT will support the construction warranty and Tier 3 maintenance of BE items. Correlator. The fourth quadrant of the correlator was placed in operation in September 2012. The acceptance review of the full correlator was successfully completed in December 2012. Some correlator documents had to be revised as a result of the review, and those revisions were completed in FY 2013. Correlator staff now assist with routine trouble-shooting of the correlator as part of operations. Computing: The Computing IPT delivered its last software release under the construction project in September 2012, thereby completing its construction activities. In December 2012, the IPT transitioned into the Integrated Computing Team (ICT), which focuses on operational support of the ALMA Department of Science Operations (DSO). Systems Engineering and Integration: PA/QA staff will assist the NA IPTs in resolving issues to facilitate the full acceptance of NA deliverables. The effort involves facilitating the evaluation of Requests for Waivers and the resolution of Corrective Action Requests to enable the full acceptance of deliverables. Science: The NA Science IPT will be engaged in a number of activities related to the commissioning and science verification of the ALMA array elements and in the execution of projects selected for ALMA Early Science observations. 4.1.2 Operations North American ALMA Operations (NA ALMA Ops) is the NRAO department that provides North America’s scientific and technical partnership support to the international ALMA Observatory and supports the North American community in their use of ALMA. Specifically, NA ALMA Ops ensures that the North American scientific community has the tools, information, support, and access to make optimal scientific use of ALMA. It also provides scientific, technical, and business support to observatory operations in Chile in concert with the JAO staff and our international partners. In addition, it supports a long-term development program for the technical enhancement of ALMA. NA ALMA Ops consists of four divisional elements that were brought into one NRAO department in FY 2013. These divisions are the NAASC which has been in operation for several years, the Offsite Technical Maintenance groups (software and hardware), the NA ALMA Development Program, and the Office of Chilean Affairs – also in operation for several years, which is managed cooperatively with Associated Universities, Inc.


The North American ALMA Science Center The NAASC is the scientific support arm of NA ALMA Ops. The NAASC is the North American scientific community’s interface to the ALMA Observatory for expert advice and assistance in the use of ALMA, including proposal preparation and submission, data reduction and reprocessing, ALMA-specific documentation, and on-line tools and resources. Embedded within the NAASC is the NA ARC, which provides the core services specified by the ALMA Observatory for scientific support in the regions and contributed support for Chile operations. The NAASC also coordinates with the science operations of the other ALMA partners in Europe and East Asia. The NAASC has three management groups – the Telescope Support Group (telescope-facing), the User Support Group (user-facing, ALMA-specific), and the SUS Group, which reports to the SSR department and is matrixed to the NAASC. SUS is the NRAO-wide science operations group that unifies common support programs across the NRAO. The NAASC specifies its requirements for science operational support, and contributes staff into this pool, which can then be effectively leveraged for best economy of scale and uniformity of approach. NA ALMA Telescope JAO Support The NAASC provides support for JAO operations, both from NA and through temporary deployments to Chile. The NAASC provides domain-expert assistance to the JAO Commissioning and Science Verificao9tion (CSV) effort in areas where the NAASC has key expertise that is missing or understaffed at the JAO. This includes one full time staff on re-deployment to the CSV through the end of FY 2014, and the temporary deployment (2-3 month tours) of four additional domain experts from September 2013 through March 2014, which is a critical time for the CSV team as the construction project wraps up. Thereafter the NAASC will coordinate with the JAO CSV Lead to identify additional areas of need where NRAO experience can be leveraged. This support will need to be balanced against the workload needed to support the NA community (see following sub-section), but we expect to support ~two more temporary deployments for the 2nd half of FY 2014. In addition to these CSV support missions, the NAASC provides 14 Astronomer on Duty (AoD) shifts or “turnos” each year. These are fulfilled via seven ~three week deployments of NAASC and NRC scientists to the ALMA Operations Support Facility, where they help plan weekly observing sessions, select projects for observing, perform initial quality assurance, and update observing logs and session summaries. During these trips they also interact closely with their counterparts at the JAO and visiting AoDs from the other ARCs. Additional support of JAO operations is by participation in bi-annual software acceptance test of all ALMA operations software subsystems, and by providing Subsystem Scientists and regional “Cognizant Leads” for each software subsystem and each international ALMA working group. Subsystem scientists provide expert scientific advice to the software developers on new requirements and desired capabilities, help plan and organize software tests and write test reports, and report to the rest of the project on software issues. Cognizant leads provide regional input to the subsystem scientist and arrange local participation in tests or input on operations procedures and policies. The NAASC provides two subsystem scientist (CASA and helpdesk) and eight Cognizant Leads. The NA ARC Manager arranges for NA participation in ALMA core documentation review, software testing, and panel review support. He is a member of the Science Operations IPT to define and track ALMA operations procedures and policies and software priorities. Frequent trips to JAO and the other ARCs are required.


In Q2 FY 2014 the ALMA Operations management team will participate in the ACCOR review. The NA ALMA Ops and NAASC management team will also be heavily engaged in writing a new proposal for renewed NSF funding since the present proposal is for the years FY 2012- FY 2015. NA ALMA User Support In FY 2014, the NAASC leads those aspects of NA ALMA user support that are ALMA specific, whereas those tasks that benefit from a pan-NRAO approach are led by the Observatory-wide SUS group. NAASC staff support both efforts. User support responsibilities centered at the NAASC include preparation for upcoming observing cycles, generation and review of scheduling blocks, data reduction and visitor support for data reduction, and contact scientist responsibilities. NAASC staff will be involved in many aspects of user outreach and training, observation preparation support, and data reduction for ALMA observing cycles. The NAASC provides a Contact Scientist (CS) for each PI project. The duties of CSs include assisting PI projects with the review of their SBs, assisting with data reduction and analysis for visiting PI teams, and supporting remote requests for pipeline re-processing. For Cycle 1 (C1) a primary NAASC support activity will be manual data reduction. Data processing using the ALMA pipeline will begin in parallel during Q1 FY 2014; however, manual data reduction is expected to continue throughout the year until the pipeline expands to full capability. SUS will organize and NAASC staff will support several short webinars on specific data reduction and analysis topics, and data reduction training events at AAS and other large community meetings. After the completion of C1 observations (Q3 FY 2014), NAASC staff will review the quality of all partially completed data sets and package and deliver all those of scientific value. Support of the ALMA Cycle 2 (C2) proposal process during FY 2014 will begin with the release of the call for Proposals by the JAO (beginning of Q1 FY 2014), and will be intensive between then and the proposal deadline six weeks later. C2 user support will continue after the proposal deadline with the hosting of the proposal review in North America, for which NAASC will provide technical secretaries and technical assessors, as well as logistical support. Meanwhile NAASC staff will also contribute effort to the definition of the requirements for the C2 SB preparation software and testing of that software. NAASC staff will then proceed with the preparation of the SBs for all successful NA-supported proposals, an activity requiring the effort of four NAASC staff full time for ~six months beginning with attendance at a training “bootcamp” in Santiago. CS staff will review the SBs with their assigned PI projects throughout this period. Data processing by NAASC staff, both manual and by pipeline, will begin shortly after the start of the C2 observations in Q3 FY 2014 and will require similar resources to the C1 data reduction effort; pipeline reduction will reduce the work effort per project compared to C1, but significantly more projects are anticipated in C2. Visits by C2 PI teams may begin over the summer and will be supported by the CS staff. Visits and remote support for scientists using non-proprietary archival C0 (and possibly C1) ALMA data will require CS support throughout the year. Preparation for ALMA Cycle 3 (C3) will begin in FY 2014 with planning the capabilities that will be offered by the observatory, an activity led by the JAO, with the involvement of several NAASC staff. Although the long-term timeline for ALMA cycles is still not decided, the preparation of the C3 proposal call materials is likely to begin in FY 2014 Q4, and will involve many NAASC staff in the review editing


and writing of the many documents and materials involved, from the Proposer’s Guide and the Primer to the Technical Handbook. NA ALMA Student and Visitor Programs NA ALMA Ops will support several programs for students and scientific professionals in FY 2014.

• SOS Program. The SSR department will administer the SOS program for eligible NA graduate and undergraduate students with successful ALMA Cycle 2 Early Science (high priority) observing proposals. The program is described on the science.nrao.edu website. Stipends of up to $35,000 per investigator per year are possible.

• Data Reduction Visitor Support. The NAASC encourages data reduction visits and can support up to two, two-person teams per week. The NAASC will reimburse the travel and lodging for one person from each team, and a second person if he/she is a student.

• Sabbatical visitors. The NAASC is providing partial support for one sabbatical visitor in FY 2014 and encourages additional requests. The NAASC is particularly interested in scientific or technical visitors willing to contribute to ALMA commissioning and development.

4.1.3 Maintenance and Renewal North American ALMA Offsite Maintenance North American ALMA Offsite Maintenance provides technical support and maintenance services for ALMA devices and instrumentation by agreement with the JAO. In most cases, the NRAO NA ALMA offsite group is responsible for the repair and maintenance of the same devices that it developed and manufactured during the construction project. The ALMA maintenance plan is divided into tiers, with the JAO staff responsible in most cases for Tier 1 and Tier 2 maintenance on site, and the regional (offsite) labs responsible for Tier 3 maintenance, which involve component-level diagnostics and repairs. NRAO Offsite Hardware Maintenance consists of several groups in Charlottesville including: FE components plus the Band 6 cold cartridge; Local Oscillator (LO)- warm cartridge assembly and cryogenic multipliers; Photonics-central LO modules and antenna articles; Correlator; and Antenna; as well as the BE group in Socorro (antenna articles, data receiver articles, and some of the central LO articles). Front End support for the Band 3 cold cartridges is provided by our Canadian partners at NRC-Herzberg. Through the hardware expertise and experience of NRAO technical staff, efficient use of resources, and the coordination with onsite Chilean staff and offsite support staff from our international ALMA partners, the Offsite Hardware Maintenance Division helps to ensure that the ALMA Observatory operates at its maximum scientific potential. Specific ongoing operational activities of the NRAO hardware maintenance groups in support of this mission include:

• Planning the level and type of hardware maintenance support based on available resources and a continuous analysis of operational failure rate data

• Assisting with onsite troubleshooting and repair through regular coordination with Chilean maintenance staff and hardware support staff from our international partners

• Troubleshooting and repair of items returned to NRAO that require NRAO expertise and facilities

• Coordination and oversight of maintenance contracts for vendor-built modules supplied by NRAO during construction


• Troubleshooting and maintenance, including software support, of test systems used by Chilean maintenance staff designed and/or delivered by NRAO as part of the Construction project

• Training of Chilean maintenance staff in troubleshooting and repair of both ALMA hardware deliverables and the systems to test them

• Procurement, assembly, and testing of spare components to maintain an appropriate stock consistent with observed failure rates

• Continued improvement of testing and repair procedures in collaboration with onsite Chilean staff

• Serving as a technical knowledge resource for the ALMA project (such as serving on design reviews for ALMA development projects)

• Supporting the ICT in implementing new Correlator modes • Shipping and receiving of equipment between NRAO, vendors, and Chile

Specific FY 2014 initiatives include (i) commissioning of a front end test cryostat by the FE maintenance group in Charlottesville; (ii) establishing long-term maintenance contracts for vendor-built modules, such as the BE Intermediate Frequency (IF) Downconverters; (iii) conducting onsite training visits by each major hardware group (BE, FE, LO, and photonic). NA ALMA Offsite Software support is described in the Data Management and Software section of the Program Operating Plan.


4.1.4 ALMA Major Milestones

FY 2014


Construction

Conduct End of Construction Review 1 Acceptance of Optical Pointing Telescopes 2 Complete installation of 400V cables and fuse disconnects at AOS 3

Complete delivery of FE Thermal Interlock Modules 4

Complete delivery of NAOJ Band 4, 8, and 10 multipliers 5

Delivery of first Front End Handling Vehicle (FEHV) 6

Delivery of three remaining FEHVs 7

Operations

NAASC / NA ARC ACCOR Review 8 ALMA C1 User Survey 9 C2 Phase 2 Software Tests 10 Start of C2 observing season 11 C1 Data Delivery Closeout 12 Offsite HW Establish long-term maintenance contracts for vendor-built modules 13

Milestones: 1. ALMA Construction Completion and Operations Readiness Review 2. Acceptance of Optical Pointing Telescopes 3. Complete installation of 400V cables and fuse disconnects at AOS 4. Complete delivery of FE Thermal Interlock Modules 5. Complete delivery of NAOJ Band 4, 8, and 10 multipliers 6. Delivery of first Front End Handling Vehicle (FEHV) 7. Delivery of three remaining FEHVs 8. ALMA Construction Completion and Operations Readiness Review 9. ALMA C1 User Survey 10. C2 Phase 2 Software Tests 11. Start of C2 observing season 12. C1 Data Delivery Closeout 13. Establish long-term maintenance contracts for vendor bulk modules

Deliverables: [1] Reports and analysis on Construction closeout prepared and presented. [2] Final Optical Pointing Telescopes accepted. [3] 400V cables installed on all remaining stations [4] FEThermal Interlock Modules completed and delivered [5] Band 4, 8, and 10 multipliers completed and delivered [6] FEHV 1 completed and delivered. [7] FEHV 2-4 completed and delivered. [8] Reports and analysis on maintenance planning and operations readiness; Science Operations procedures document(s) prepared and presented. [9.] C1 User Survey Report [10] Completed test matrices and test reports [11] PI validated schedule blocks for initial NA C2 observing projects [12] Data delivery packages and PI notifications for all unfinished C1 datasets [13] Approved maintenance contracts for vendor-built modules


4.2 Very Large Array Overview In FY 2014 NRAO will continue to offer a suite of robust and scientifically powerful observational capabilities on the VLA, designed and tailored to address the highest priority scientific needs of the general community. In telescope operations much of the effort will go into ensuring that the array is calibrated, maintained and performing optimally. There will be a small number of upgrade projects chosen to improve performance in several areas including antenna pointing, receiver stability, and digital sampler reliability and performance." 4.2.1 Operations

Observing Programs The NRAO VLA will continue to offer three types of observing programs to users in FY 2014: General Observing, Shared Risk Observing (SRO) and RSRO. Observing capabilities are first offered to the community through the RSRO program, which enables the community to express their scientific interest in potential capabilities through peer-reviewed proposals, provides resources to help with testing and scientific verification, and helps to ready new capabilities for end-to-end operation. Once a capability has been demonstrated and tested, and can be dynamically scheduled, it is offered through the SRO program pending full testing and documentation. When a mode is robust and well tested, it is offered as a General capability. The General Observing program comprises a suite of robust observational capabilities designed and tailored to address the highest priority scientific needs of the general community. An overview of the capabilities being offered for General Observing for semester 2014A is given in Table 4.2 below:

Table 4-1: VLA Capabilities Capability Description 8-bit samplers • Standard Default setups for:

o 2 GHz bandwidth continuum observations at S/C/X/Ku/K/Ka/Q bands (16 x 128 MHz sub-bands) o 1 GHz bandwidth continuum observations at L Band (16 x 64 MHz sub-bands)

• Flexible set-ups for spectroscopy, using two independently tunable 1 GHz basebands, each of which can be split into up to 16 flexibly tunable sub-bands

• Single, dual and full polarization products • Up to 16,384 channels (summed over all polarization products)

3-bit samplers • Standard Default setups for: o 8 GHz bandwidth continuum observations at K/Ka/Q bands o 6 GHz bandwidth at Ku Band o 4 GHz bandwidth at C/X bands

• Flexible set-ups for spectroscopy, using four independently tunable 2 GHz basebands, each of which can be split into up to 16 flexibly tunable sub-bands

• Single, dual and full polarization products • Up to 16,384 channels (summed over all polarization products)

Sub-arrays • Up to 3 independent sub-arrays using standard 8-bit continuum setups Phased array for VLBI • All antennas phased to simulate a single collecting area (“Y27”)

The SRO program allows users access to capabilities that can be set up via the OPT and run through the dynamic scheduler (without intervention), but are not as well tested as general capabilities. Shared Risk capabilities being offered for semester 2014A are correlator dump times as short as 50 ms, mixed 3-bit and 8-bit set-ups, and use of the new low frequency system in the frequency range 230 to 470 MHz for Stokes I continuum imaging.


The RSRO program will continue to provide access to more extended capabilities of the VLA in FY 2014. RSRO capabilities are those that require additional testing, and are provided to the community in exchange for a period of residence to help test and verify those capabilities. The requirements for the RSRO residency have relaxed since the completion of the Expanded Very Large Array (EVLA) Construction Project. A minimum residency is no longer required, and increased flexibility in the length and timing of visits may be implemented in the coming year. The kinds of capabilities available through the RSRO program include, e.g., correlator dump times shorter than 50 ms, data rates above 60 MB/s, use of recirculation in the correlator, use of the P-Band system for polarimetry or spectroscopy, more than 3 sub-arrays or sub-arrays with the 3-bit system, on-the-fly (OTF) interferometric mosaicking, and complex phased array observations (e.g., pulsar and complex VLBI observing modes). Further details of the capabilities planned for the two shared risk observing programs can be found below. Scientific Support for Maintenance of Receiver, Antenna, and Array Performance The VLA has now fully transitioned to an operational state in which most of the effort goes toward maintaining array performance and ensuring that our user community has access to quality instrumentation and updated information to effectively use the VLA. Operational tasks that will be carried out by the scientific staff during FY 2014 include (but are not limited to):

• Support Calls for Proposals: Prepare user documentation for offered capabilities before the call goes out, provide scientific testing of user tools needed to prepare proposals (e.g., PST, General Observing Spectral line Tool, Exposure Calculator), provide technical reviews for proposals and evaluate proposals for RSRO contributions.

• Hardware, Software, and Operational Documentation: Write technical documentation detailing hardware and software functionality for staff and users, develop and improve operational procedures and write documentation for the operations staff. This includes updating the VLA “Observational Status Summary” before each Call for Proposals and providing content for the “Guide to Observing with the VLA” on the NRAO web site.

• Track and Measure VLA Performance: Sensitivity, Gain Curves, Holography, Antenna Positions, Collimation, Pointing: o Characterize the sensitivity and gain response of each antenna at each band. This must be

done periodically as receivers and equipment are replaced (e.g., due to failures in the field) or as software is upgraded that may change the system performance.

o Check the surface accuracy with holography periodically to ensure optimal efficiency at the highest frequency bands.

o Determine antenna positions, collimation offsets and pointing accuracy when the array is moved into a new configuration.

• Scientific Testing of Antennas Completing Major Maintenance: o Determine antenna positions, collimation offsets and pointing accuracy each time an

antenna comes out of the Antenna Assembly Building after a maintenance overhaul. o Evaluation of new Antenna Control Units (ACU): Two antennas are scheduled to be

outfitted with new ACUs during FY 2014 during major maintenance overhauls (see “Upgrade Projects” below). As new ACUs are installed they will undergo testing and evaluation by scientific staff.

• System Health and Maintenance Feedback: Run routine health checks to determine if there are any hardware failures that must be followed up with maintenance tickets. Troubleshoot problems found and confirm fixes are implemented. Run RFI tests to characterize and help mitigate RFI contamination in the bands.


• Data Quality Assurance Checks: Evaluate data quality based on the Pipeline results and run test observations to identify and diagnose problems that are not caught by the standardized tests and engineering checks.

• Calibration Data: o Flux calibrator models, flux density run: Develop and maintain the infrastructure needed

by users to establish an accurate absolute flux density calibration scale for the VLA at each observing frequency. Extensive, multi-configuration observations of calibrators are made to develop models that can be applied during the data calibration process.

o Polarization stability and service calibration tests: Develop and maintain optimal polarization calibration infrastructure and tools for our users. In FY 2014 this includes documentation, full polarization source models and measurements of the polarization stability of the system. Service observations are also made for VLBA polarization observations to enable better calibration of VLBA data.

• Stabilize New Additions to the VLA: “Y27” phased array observations with the VLBA, sub-arrays, fast dumps. Although observing with the VLA phased array with all available antennas (Y27) is possible, there are still issues that arise occasionally as this new capability is exercised. Similarly, sub-arrays and fast dumps may continue to have issues that need to be worked out. These issues will be trouble-shot and solved as they arise.

• Evaluation of a New Atmospheric Phase Interferometer (API): The API is used to continuously measure the atmospheric stability, providing a means to estimate the needed observation cycle times when using fast switching phase calibration at the highest frequency bands and to guide the dynamic scheduler as to when the weather conditions are appropriate for high frequency observations. The existing API is beginning to fail and a new system will be ready for testing and evaluation during FY 2014.

Support for the Calls for Proposals and associated documentation updates and software testing have milestones on a cyclic time scale that is matched to the proposal cycle. Understanding and characterizing, e.g., antenna positions, gain curves, collimation and pointing have a high impact during and just after each array re-configuration and then decrease to a lower level of effort that is needed to support antennas coming back to the array after major maintenance. ACU evaluation will be linked to when those antennas return to the array after maintenance (one is expected to be installed during Q2 and one during Q4). Thus, these tasks have milestones after each configuration as well as a base of continuing effort. System health and data QA evaluation along with polarization service observations and support of phased-array observations require an on-going level of effort that is expected to remain relatively constant throughout the year. Array Operations Array Configurations: Over a 16-month period the VLA cycles between four primary configurations, and three “hybrid” configurations, in order to provide sensitivity to different spatial scales as needed to achieve various science goals. Re-configurations occur every four months, to ensure that a particular configuration cycles through all the seasons averaged over multiple configuration cycles. These antenna moves require most of the site staff (typically 10 persons for each of two transporters), and can require anywhere from one to three weeks each, depending on which configuration is being set. Array configuration changes along with transportation for antenna overhauls results in approximately 60 antennas being relocated annually. All moves require track crew, antenna mechanics, transporter operators, electricians, and receiver, cryogenic, fiber optic, and LO/IF technicians. Personnel involved in the array reconfigurations are used to perform maintenance activities (antenna overhauls, track maintenance, electrical infrastructure maintenance, receiver, fiber optic, and LO/IF maintenance) at


other times, and are highly integrated with the rest of operations. The reconfigurations planned for FY 2014 are shown in Table 4.3.

Table 4-2: VLA Reconfigurations Operating Model: Currently, the VLA is manned 24 hours per day, seven days per week from the VLA site by six array operators on rotating shifts. Along with the established supervisory duties, the VLA supervisor also acts as the scheduler for major maintenance and overhauls for the VLA and the VLBA. Additionally, custodians and security guards are present for all evening and night shifts as well as weekend day shifts. VLA Operations continues to explore the possibility of moving operator control to Socorro for the evening and night shifts in order to achieve savings in vehicle use and to reduce the number of operators needed to maintain full operational coverage. The staff that provides custodial and security services will continue to work at the site. Maintaining appropriate levels of safety for site personnel and equipment will be a major factor in whether this plan will move forward. 4.2.2 Upgrade and Enhancement Projects VLA ACU Replacement Project: The electronics parts to repair the existing ACUs are no longer available. Antennas with failed ACUs would no longer be able to participate in observations, posing a serious operational risk. All of the legacy VLA antenna control units must be replaced with newer technology units, which enables a more supportable ACU, as well as eliminating some inherent problems with the original design and greatly improving the pointing and tracking capabilities of the antennas. The first new VLA ACU was installed in antenna 21 during the last quarter of FY 2013. The 2nd and 3rd ACU replacements will occur in FY 2014, in Q2 and Q4. Additional ACUs will be replaced as funding permits. Once an antenna has been outfitted with a new ACU its performance will be evaluated by scientific staff. 4-Band Feed Development Project: To date, 4-Band observations on the VLA require special dipoles that cross under the subreflector and attach to the quadrupod legs. Although these dipoles are adequate for observing at 4-Band, their presence reduces the sensitivity at L and S-bands, and the dipoles must be mounted temporarily for observing “campaigns,” requiring manpower both to mount and remove the dipoles. A new design is being explored in collaboration with Virginia Tech that would “strut straddle” the quadrupod legs in a square shape with minimal blockage of the subreflector, and so could be left up permanently. The new 4-Band feed development project will be completed by the end of FY 2013. At the time of writing tests indicate that the feed has not yet met sensitivity requirements, but additional testing continues. In the event that the new feed design does not meet the required sensitivity with minimal blockage then the legacy Erickson dipoles will be refurbished for use in the next 4-Band observing campaign, and will undergo testing and scientific verification by scientific staff. C and L-Band Thermal Gap Retrofits: The new thermal gap designs were completed in late FY 2012. These thermal gaps have been shown to decrease the noise temperature of both the C and L-Band receivers and significantly improve performance. At the end of FY 2013 three C-Band and six L-Band receivers had been retrofitted. Three additional C-Band and six L-Band receivers will be modified in FY 2014.

To Config B BnA A D DnC

C Start 9/23/2013 1/13/2014 2/3/2014 5/27/2014 9/8/2014 9/29/2014 Complete 10/4/2013 1/17/2014 2/14/2014 6/13/2014 9/12/2014 10/10/2014


Card Cage Upgrades: Approximately three to four receiver card cage failures are reported each week for the VLA, which make the receiver involved unusable. A revised FE card cage design to address these reliability issues was completed in FY 2013. The rollout of upgrades will begin in Q1 FY 2014, with 12 upgrades completed each quarter.

VLA 3-bit Sampler Upgrade: There are 224 3-bit sampler boards installed in the VLA, which provide the widest bandwidths. Some of the boards do not perform as well as others, and installation of all the best performers in the array has reduced the number of good spare sampler boards below a comfortable level. The current 3-bit sampler chip is obsolete, so a board that uses a commercially available chip is being designed and tested. The new Data Transmission System (DTS) transmitter module 3-bit sampler boards will be installed in two modules in the array by end of Q2. An analysis and presentation on performance will be given to senior staff in Q3. VLA Atmospheric Phase Interferometer (API) Hardware Upgrade: A major upgrade to the API was started in FY 2013 to address technical issues that make the existing system prone to failure, and which also includes installing two additional dishes (for a total of four) to provide two-dimensional information about the structure function of the troposphere. A complete new set of electronics and software has been installed. The installation of the new API system at the VLA will be completed in Q1 FY 2014, with testing by scientific staff continuing into Q2. If the performance of the API meets specifications its output will be incorporated into the VLA dynamic scheduling system by the end of Q3. Capability Enhancements for Semesters 2014A, 2014B, and 2015A The VLA continues to provide new capabilities to the user community to optimize and enhance the science that can be done with the array. This strategy has proven to be effective in keeping users engaged, and it is a critical factor in keeping the scientific productivity of the VLA high. To this end, NRAO continues to provide incremental capability enhancements above and beyond our operational efforts. During the EVLA project, development and commissioning of new capabilities were a top priority. Now, however, Operations has taken center stage and the pace of development of new capabilities is now matched to the available FTEs who are not fully engaged with daily operations. Enhancements in a number of areas are identified in the Table 4-3 below. Note that the rate at which a capability moves from Resident Shared Risk to Shared Risk to a General Observing mode depends upon the complexity of the task, the available manpower of RSRO participants, funding for hardware (in some cases) and the available FTEs within NRAO. Some assumptions about effort from participants in the RSRO program have been made in the schedule below; since these resources lie outside NRAO’s control, the delivery schedule for these capabilities may vary from that outlined below.

Table 4-3: VLA Capability Enhancements Enhanced Observing Mode Capability 2014A 2014B 2015A Mixed 3/8-bit samplers for increased flexibility to observe mixed line and continuum projects

SR General General

P-Band Stokes I observations SR SR General Dump times below 1 s (but greater than 50 ms) SR SR General Recirculation x 4 in the correlator to increase the spectral resolution

RSR SR General

8 spectral windows (VLBA channels) recording mode for Y27 to match VLBA PFB/DDC-8

RSR SR General

Sub-arrays using the 3-bit samplers RSR RSR SR On-the-fly interferometric mosaicking RSR RSR SR


Enhanced Observing Mode Capability 2014A 2014B 2015A Single antenna sub-array for VLBI while observing a standard VLA program with remaining antennas (“Y1”)

RSR RSR SR

Dump times below 50 ms and/or data rates above 60 MB/s RSR RSR RSR Pulsar de-dispersion mode RSR RSR RSR Real-time transient detection mode RSR RSR RSR New 4-Band system (58-84 MHz) RSR RSR RSR P-Band spectral line and/or polarimetry RSR RSR RSR Pulsar phase binning RSR RSR RSR Increase # sub-bands per 8-bit baseband from 16 to 32 RSR RSR RSR

Installation of the new low frequency system for the VLA that has been developed in collaboration with the Naval Research Laboratory will be completed in FY 2013. Scientific testing and verification will continue into FY 2014, and development of polarimetry and spectroscopic capabilities with these receivers at P-Band are noted in the table above. At 4-Band the potential use of new strut-straddling feeds depends on the outcome of tests taking place towards the end of FY 2013. If the new design does not meet specifications some effort may be required to re-commission the Erickson dipoles, including scientific verification tests. Operational Enhancements Several enhancements to VLA calibration procedures and scheduling are planned for FY 2014:

• Implement Referenced Pointing Using Multiple Spectral Windows: Referenced pointing has been implemented using a relatively narrow bandwidth associated with a single spectral window, with that window being at a fixed relative position in the baseband. In addition, the reference antenna is currently fixed. Options for selecting the reference antenna, and the use of more complex combinations of spectral windows allowing for mitigation of RFI and pointing on weaker sources will be tested.

• Implement Tipping Scans for Opacity Correction: When it is not possible to observe an absolute flux density calibrator within the same elevation range as that spanned by the science target, it is necessary at high frequencies to estimate the difference in atmospheric opacity between the calibrator and the science target. A tipping scan can be used to derive the zenith opacity during an observation to characterize elevation-dependent gain terms, improving the accuracy of the absolute flux density scale. Although this was possible with the old VLA system, it has not yet been implemented with the EVLA, and is currently potentially limiting the absolute flux density calibration accuracy at high frequencies.

• Develop a Method to Use Switched Power Values for Improved Calibration: The switched power calibration values can be used to remove gain variations as a function of time if the measured system power is stable. Thus, it has the potential to decrease observing overhead and simplify the post-processing steps in several observing bands. Several problems remain to be solved with respect to the use of switched power calibration, and commissioning of the switched power system and development of the best practices for how to use the values will continue into FY 2014.

• Pipeline Heuristic Development: The VLA Calibration Pipeline currently delivers calibrated visibility data for continuum experiments. Heuristics will continue to be developed during FY 2014 to extend the use of the pipeline to those experiments using “weak” calibrators (relative to the fractional bandwidth, including spectroscopy), and to improve the flagging heuristics for L-Band.


4.2.3 Maintenance and Renewal New Mexico Operations also supports over 3,300 modules, power supplies, and receivers for the VLA, VLBA, and the ALMA BE, as well as all mechanical parts in the antennas, such as motors, gears, and structural elements. Support work includes addressing the over 3000 maintenance forms generated yearly and requires engineers and technicians to investigate, diagnose, trouble shoot and ultimately resolve these reports. To this end, there is a daily maintenance meeting attended by the group leads of all electronics and engineering service personnel to review all new problem reports to assure all problems are assigned to the proper group. Older forms are reviewed to avoid stagnation of those issues and to identify recurring issues that may require an improvement or redesign of a module or procedure. Technicians are also available for after-hours callouts to address problems that seriously impact the safety of the array, such power failures, electrical problems, antennas stuck in un-safe positions. Callouts also occur if there are more than three antennas unusable for astronomy due to problems that may not be safety related, such as warmed receivers following a power glitch. Specific maintenance activities are described further below. Antennas: VLA antennas are routinely cycled through the Antenna Assembly Building for checkout and overhaul throughout the year. Under normal maintenance circumstances, up to eight antennas per year could be cycled through the assembly building. In FY 2014, several antennas will be upgraded with new control circuitry (ACU), and as such each will require roughly double the period of time given that these will be the first antennas which undergo this retrofit. In FY 2014, NRAO plans to perform overhauls on six antennas. In addition to the mechanical work associated with the ACU upgrade, the overhaul process includes (1) structural inspections that may reveal existing and potential problems; (2) the installation of upgrades to mechanical parts, electrical systems and electronic equipment; (3) addressing maintenance issues that require the Antenna Assembly Building resources, such as azimuth gear and bearing replacement; (4) inspecting and changing oil in gear boxes; (5) carrying out touch-up painting on the structure; and (6) repairing and replacing parts as needed. After a one year hiatus, the process of replacing one antenna azimuth bearing per year will resume in FY 2014. Preventive maintenance is conducted in the field to inspect, clean, and lubricate each antenna’s Focus Rotation Mount (FRM) and azimuth and elevation bearings. Antenna mechanics routinely check grease for metal chips on all antennas in the field so as to be alerted for potential failure of moving parts. This is especially important for the sustainability of the azimuth gears. The goal is for each antenna to undergo this maintenance every six months. The antenna mechanics will continue to respond to mechanical/structural problems that occur regularly, such as inoperative motors, water leaks into the antenna, equipment rooms, broken anemometers located on the dish lip, realigning misaligned FRMs, and addressing other antenna issues brought to their attention. The two transporters used to move the antennas during reconfigurations undergo maintenance and repair between move periods. Maintenance on the almost forty year old transporters includes servicing the motors, checking the generators that keep critical power to the antenna during a move, lubricating the moving parts, checking on the twenty-four wheel axles and wheels and maintaining electrical and hydraulic systems. Antenna mechanics also inspect the 72 concrete antenna pads to ensure their structural integrity and to measure for signs of shifting. If the tripod legs of the pad were to shift too far apart, the antenna would not be able to be bolted to the pad. Track: During FY 2014, inspection of the VLA railroad tracks will continue, checking for problems that could compromise the safety of the transporters that carry the antennas during array reconfigurations


and other antenna moves. These inspections also guard against problems that could jeopardize the safety of the maintenance rail vehicles that are used by technicians to service the antennas. Maintaining track integrity requires specialized railroad repair vehicles and equipment, as well as ballast, rails and track sections. The supply of ballast purchased with ARRA stimulus funding in FY 2010 is quickly being exhausted, so a line item for this has been added back into the operations budget. The VLA track contains approximately 200,000 ties. With a nominal life expectancy of 25 years for pine railroad tie, ideally we would replace on the order of 8000 ties per year, or more given the dry conditions at the site. This task alone would require the constant attention of seven FTE over the course of a year. Given that the track crew comprises of six FTE, and that there exists other necessary maintenance tasks to keep the tracks in reasonable shape, the goal is to locate and replace only 2500 ties along the approximate 44 miles of track in FY 2014. Seventy-three intersections to antenna pads are included in the VLA Wye. As with the track cross-ties, the ties which make up these intersections must be replaced on a regular basis. Due to the complexity of rebuilding an intersection, the decision was made to replace failing intersections with fabricated concrete ties rather than wooden ones. This requires more time to accomplish than working with wooden ties, but the payoff is extended life and less maintenance. To date, approximately 10 of the 73 intersections have been replaced. Another 3 will be fabricated and replaced in FY 2014. Site Infrastructure: The VLA site buildings, utility systems, and grounds will continue to undergo routine annual inspection and preventive maintenance in FY 2014. This includes annual road grading; roof repairs; heating and cooling systems maintenance; pest and weed control; fire brigade and emergency medical response team training; and the routine servicing of gas pumps, sewer and water supply systems, backup generator power, electrical lines, switches, and transformers, and other related systems.

In FY 2014 a plan will be developed to recommend the best course of action to take for the site’s original VAX building, which used to host the VLA VAX computing resources. This building, also referred to as the Scientist and Library office building, also held the VLA library books and some scientific staff offices. After the DSOC was built in 1988, this building was repurposed for storage and the track crew, and later the fiber group. These two groups now have new homes in the cold storage bldg (track) and the VLA control bldg (fiber), leaving this building empty. Also, a campaign will be carried out to replace the failing transformer which supplies the VLA Activity Center, Visitor’s Center, and soon to be decommissioned ALMA Test Facility.

Vehicle Support: The VLA continues to operate more than 50 vehicles and heavy equipment items, such as forklifts, cranes, loaders, tampers, backhoes, trenchers, and buses. Many of these are used daily and will continue to be routinely serviced and repaired to remain in safe, efficient working condition through FY 2014 and on. Electronics Division Support: In addition to the upgrade projects described above, the New Mexico Electronics Division is responsible for maintaining all VLA electronic components and the WIDAR Correlator. Routine work for FY 2014 will consist of the following:

• Overhaul at least 30 receiver cold heads per quarter to keep FEs operating. • Replace Low Noise Amplifiers (LNAs) in 12 L-Band receivers (one per month) to correct wire

bond breakage problem. • Recondition and replace receiver desiccant in each of 240 units twice per year.


• Perform preventive maintenance on 25 VLA compressor lines twice per year. • Overhaul two EVLA compressors due to normal wear-and-tear. • Perform preventive maintenance on four helium circuits to maintain cryogenic performance. • Repair and replace 24 FE receivers per year. • Perform checks on the Correlator boards, replace as needed. • Perform checks of the fiber optics system to ensure proper operations, reset as needed. • Build 20 fiber optic cables for the Computing Division and replace 20 fiber optic cables on the

EVLA antenna infrastructure per quarter. • Investigate issues with locking, fringing, output power, and general communication dropouts. • Perform routine power supply and battery maintenance. • Retrofit upgrades or additions to enhance equipment safety. • Perform bench work on modules for repair or assembly. • Monitor modules responsible for array timing, adjusting as needed. • Perform maintenance on ACUs and FRM controllers. • Replace 10 SCR driver cards in the VLA antenna servo cabinet. • Maintain monitor for local radio frequency interference (RFI) at the VLA site. • Swap out the site weather station twice yearly for preventive maintenance.

RFI Mitigation: Plans for reducing and mitigating RFI for FY 2014 include:

• Reduce or eliminate high frequency and very high frequency RFI originating from Transporter Building florescent lighting. Current lighting interferes with the VLA low band observing and Long Wavelength Array (LWA) observing.

• Re-enable the W8, L-Band automated spectrum monitor. The legacy W8 monitor was found to produce ripples in the L-Band spectrum during early EVLA observations and was disconnected.

4.2.4 VLA Major Milestones

FY 2014


Scientific Support for Operations

Support the 2014B semester (2014 Feb 1) Call for Proposals 1 Support the 2015A semester (2014 Aug 1) Call for Proposals 2 Support reconfiguration to B-config 3 Support reconfiguration to BnA and A-configs 4 Support reconfiguration to D-config 5 Support reconfiguration to DnC-config 6 Stabilize VLA capabilities: Y27, sub-arrays, and fast dumps 7

Array Operations Array Configuration Changes 8 9 10 11 Complete evaluation of array ops move to Socorro 12

VLA Prototype ACU

Critical Design Review prior to 2nd installation 13 Install 2nd ACU 14 Scientific evaluation of ACU performance 15 Install 3rd ACU 16

VLA Thermal Gap Retrofit

Thermal gap modification of 3 C-Band receivers 17 Thermal gap modification of 6 L-Band receivers 18

VLA Card Cage Upgrade Install 48 card cage upgrades for VLA front ends 19

VLA 3-Bit Sampler Upgrade

Install 3-bit sampler PCB in 2 VLA DTS modules 22 Present 3-bit sampler performance analysis to NRAO staff 21


FY 2014 Q1 Q1 Q1 Q1

VLA API Upgrade Install final 2 API dishes 22 Incorporate API output into VLA dynamic scheduler 23

Capability Enhancements Define and demonstrate new capabilities for 2014B 24 Define and demonstrate new capabilities for 2015A 25

Operational Enhancements

Improved referenced pointing 26 Tipping scans implemented 27 Improved switched power calibration 28 Pipeline heuristic development 29

Infrastructure Maintenance and Renewal

Antenna overhauls 30 31 32 33 Replace azimuth bearing on one antenna 34 Replace 2500 cross-ties 35 Replace 3 intersections 36 Develop proposal for VLA VAX building 37 Replace VLA Activity Center transformer 38 Preventive maintenance on 90 VLA site transformers 39 Preventive maintenance on hatch gear 40 41

Milestones: 1-2. Scientific Support for the 1 Feb and 1 Aug calls for proposals, including software testing and updating documentation. 3-6. Support array reconfigurations (e.g., antenna position, collimation and pointing determinations). 7. Stabilize operation of Y27, sub-arrays, and fast dumps. 8. Re-configurations to B config. 9. Re-configurations to BnA and A configs. 10. Re-configuration to D config. 11. Re-configuration to DnC config. 12. Complete evaluation of whether evening and nighttime array operations can be moved to Socorro. 13. Critical Design Review of ACU prior to 2nd installation. 14. Install 2nd ACU. 15. Scientific evaluation of ACU performance. 16. Install 3rd ACU. 17. Install thermal gap on 3 VLA C-Band receivers. 18. Install thermal gap on 6 VLA L-Band receivers. 19. Install 48 card cage upgrades for VLA front ends. 20. Install 3-bit sampler PCB in 2 VLA DTS modules. 21. Present performance analysis to NRAO staff. 22. Install final 2 API dishes. 23. Incorporate API output into VLA dynamic scheduler. 24. Define and demonstrate new SR and general capabilities for 2014B. 25. Define and demonstrate new SR and general capabilities for 2015A. 26. Improved referenced pointing. 27. Tipping scans implemented. 28. Improved switched power calibration. 29. Pipeline heuristic development. 30-34. Overhaul total of 6 antennas. 35. Replace azimuth bearing on one antenna (probably EA21). 36. Replace 2500 ties. 37. Replace 3 intersections. 38. Develop proposal for VLA VAX building. 39. Replace VLA Activity Center transformer. 40-41. Preventive maintenance on 90 VLA site transformers

Deliverables: [1-2] Documentation and software testing. [3-6] Arrays ready for science observing. [7] Capabilities stabilized, with sub-arrays and fast dumps dynamically schedulable. [8-11] Arrays ready for scientific validation prior to observing. [12] Decision on implementation of move of evening and nighttime operations to Socorro. [13] CDR documentation. [14] Operational antenna hardware. [15] Report on pointing performance of antenna with new ACU. [16] Operational antenna hardware. [17-18] Operational antenna hardware. [19] Operational antenna hardware. [20] Operational antenna hardware. [21] Presentation. [22] Operational antenna hardware. [23] API incorporated into operations following scientific evaluation. [24-25] New capabilities for SR and General observing documented and demonstrated operational through the dynamic scheduler. [26] Robust referenced pointing. [27] Tipping scan capability ready for testing. [28] Robust switched power calibration. [29] Pipeline operational for weak calibrators. [30-33] Antennas overhauled and returned to array. [34] Azimuth bearing replaced and returned to array. [35] Railroad hardware. [36] Railroad hardware. [37] Proposal. [38] Electrical hardware. [39] Electrical hardware maintenance. [40-41] Electrical hardware maintenance.


4.3 Very Long Baseline Array Overview In FY 2014 scientific commissioning of the VLBA Sensitivity Upgrade hardware will be completed, and the full continuum bandwidth (already available for more than a year) along with the spectroscopic and tuning flexibility provided by the new hardware will be moved into full science operations. New capabilities will continue to be added for the NRAO user community but the emphasis in telescope operations for FY 2014 will be to stabilize and document existing capabilities, as well as increase the ease of use and reliability of the array. Incremental capability enhancements include implementing the use of a single VLA antenna in a sub-array for VLBI, the development of a rapid response for triggered VLBA observations, and demonstrating a narrow bandwidth, quasi-real-time correlation capability that would be suitable for real-time fringe checks and spacecraft tracking. Due to manpower limitations, implementing some of these new capabilities will require community participation in the VLBA version of the RSRO program. In addition to a regular program of infrastructure maintenance and renewal, there will be several upgrade projects primarily focused on retiring legacy hardware and software systems to ease operational loads. 4.3.1 Operations Observing Programs The NRAO VLBA will offer three types of observing programs for the users: General Observing, SRO and RSRO. The VLBA General Observing program comprises access to well-tested observing modes using the new Sensitivity Upgrade equipment that provides data rates up to 2 Gbps. For semester 2014A two observing systems are available within the “RDBE” digital backend units: the relatively limited Polyphase Filterbank (PFB) and the more flexible Digital Down-Converter (DDC). Two RDBEs using the DDC observing system offer 8-channel modes that are equivalent to what was available with the legacy system. The new C-Band receivers provide wider bandwidth coverage than previously possible and allows for observations of the excited OH line at 6.0 GHz and the methanol line at 6.7 GHz. In addition, it is possible to combine the VLBA with the phased VLA (phasing all VLA antennas together, “Y27”), GBT, Arecibo and Effelsberg. The observing system that can be used for General Observing depends upon what is available for each station (e.g., Arecibo and Effelsberg only support the PFB mode while Y27 only supports a limited, 4-channel DDC General observing mode). The Calls for Proposals identify explicitly what the available options will be for each semester. The SRO program allows users access to capabilities that can be set up via the standard VLBA software packages and run without intervention, but are not as well tested as General capabilities. The Shared Risk capabilities being offered for semester 2014A comprise any narrow bandwidth observing modes used in conjunction with the phased VLA (“Y27”). The RSRO program provides users with early access to new capabilities in exchange for a period of residence to help test and verify those capabilities. As an example, the phased VLA system was developed through the VLA RSRO program. For FY 2014 NRAO is encouraging additional RSRO participation to expand the phased VLA and High Sensitivity Array (HSA) capabilities, implement the use of a single VLA antenna in a sub-array for VLBI observing while the remaining VLA antennas perform VLA observations (“Y1”), develop a rapid response (5 to 10 minutes latency) for triggered VLBA observations, and develop a narrow bandwidth, quasi-real-time correlation capability that would be suitable for real-time fringe checks and spacecraft tracking.


Scientific Support for Maintenance of Receiver, Antenna, and Array Performance As the VLBA Sensitivity Upgrade is now completed the focus in FY 2014 will be on completing the scientific commissioning and transitioning the telescope to an operational state in which a significant fraction of the effort goes toward maintaining array performance and ensuring that the user community has access to quality instrumentation and updated information to effectively use the VLBA. Operational tasks that will be carried out by the scientific staff during FY 2014 include (but are not limited to):

• Support Calls for Proposals: Prepare user documentation for offered capabilities before the call goes out, provide scientific testing of user tools needed to prepare proposals (e.g., PST, EVN Sensitivity Calculator), provide technical reviews for proposals and evaluate proposals for Resident Shared Risk contributions.

• Hardware, Software, and Operational Documentation: Write technical documentation detailing hardware and software functionality for staff and users, develop and improve operational procedures and write documentation for the operations staff. This includes updating the VLBA “Observational Status Summary” before each Call for Proposals.

• Track and Measure VLBA Sensitivity, Pointing, Focus: Characterize the sensitivity, pointing and focus of each antenna at each band. This must be done periodically as receivers and equipment are replaced or as software is upgraded.

• Clock Maintenance: Accurate time keeping is central to VLBI, and is provided by hydrogen masers and reference signals inserted into the astronomical data. Quality assurance checks are performed periodically by scientific staff and data analysts.

• RFI Characterization and Mitigation: Run RFI tests to characterize and help mitigate RFI contamination in the observing bands.

• System Health and Maintenance Feedback: Run routine health checks and critically analyze the data to determine if there are any hardware failures that must be followed up with maintenance tickets.

• Data Quality Assurance Checks: Evaluate data quality and run test observations to identify and diagnose problems that are not caught by engineering checks. In particular, potential issues with the new DDC observing modes will require continued vigilance during FY 2014.

• Calibration of the RDBEs: New switches will be installed by the end of FY 2013 to enable the use of two RDBEs simultaneously, providing the 8-channel observing mode with the DDC. Scientific verification of the dual RDBE operation will continue into FY 2014, along with establishing calibration procedures for the new equipment.

• Stabilize VLBA+Y27/GBT Operations: Although observing with the VLA phased array with all available antennas (Y27) is possible, there remain occasional issues as these capabilities are exercised with the new Sensitivity Upgrade hardware. A significant effort will be made during FY 2014 towards stabilizing operation of these observing modes.

• Coordination with Other Observatories for Global mm VLBI and the HSA: The VLBA occasionally observes in parallel with other observatories, as requested by users whose scientific goals require the inclusion of baselines to large-aperture and/or distant facilities. Scheduling and correlation of these observations requires coordination with local schedulers at each participating observatory, a significantly more complex process than normal VLBA-only observations require.

As for the VLA, support for the Calls for Proposals and associated documentation updates and software testing have milestones on a timescale matched to the proposal cycle. Unlike the VLA, the VLBA does not reconfigure its antennas so the measurement and characterization of system health, gain curves, receiver collimations, etc., is a continuous effort tied to the regular maintenance activities.


Array Operations The VLBA is operated twenty-four hours a day, seven days a week, supported by five array operators stationed at the operations center in Socorro and by two site technicians per station living within driving distance of each site. The array operators also concurrently operate the DiFX Correlator. Two Data Analysts prepare the proper scripts for the correlation and perform quality checks on the correlated data. The supervisor for the VLBA operators also dynamically schedules the array from a list of approved projects, and manages the software to log maintenance and problem reports for both the VLA and the VLBA. A Media Specialist ensures that recording media are available at the sites and manages the software used to track the media. Data are recorded at the VLBA sites on the disk packs on the Mk5A/C recorders as appropriate, and shipped to the Correlator for processing. The media are then returned to the sites. The VLBA site techs perform all manner of maintenance and diagnostics tasks, as well as ensuring the recording media is loaded and then shipped to the appropriate Correlator. These techs are available for after-hours call-outs to address failures that impact antenna performance as well as issues related to the safety of the antenna (power outages, severe weather conditions, etc.). Possible changes to this operation model may take place during FY 2014 that may include combining the VLBA and VLA operator pools, if it becomes feasible to move the VLA operators to the Socorro center for some shifts. 4.3.2 Upgrade and Enhancement Projects Retirement of the VLBA VMEs: The legacy VME computers that control the operation of the VLBA antennas are reaching end-of-life. As part of the Sensitivity Upgrade project, new hardware has been installed at the VLBA stations; all of this new hardware is controlled with a modified version of the EVLA Executor. The computer which hosts the Executor will be used to replace the VMEs, but is not currently able to communicate with the legacy VLBA hardware. An interface box will be designed, built, and installed in the laboratory for software development in Q1 FY 2014. An operational unit will be installed at a VLBA site for testing in Q4. Retirement of VLBA Legacy Recording System: The legacy VLBA recording system has been kept running through FY 2013 in order to accommodate requests from the user community to maintain continuity in observing set-up and instrumental calibration for long-term monitoring and parallax projects. The legacy hardware has become increasingly difficult to maintain, however, and NRAO will complete the transition of any remaining VLBA observing projects still requiring the legacy recording system to using the DDC by FY 2014 Q3. This will also enable the Mark 5A recording units to be re-integrated into the correlator to increase the number of available playback units. C-Band Receiver System Completion: Ten 4-8 GHz C-Band receivers were installed in the VLBA in FY 2012 but some work still needs to be done. The Electronics Division needs to complete and test the spare VLBA C-Band receiver (Q2) and upgrade two of the early C-Band receivers (Q4). System performance will then be evaluated by scientific staff. Capability Enhancements for Semesters 2014A, 2014B, and 2015A The VLBA continues to provide capability enhancements to the user community in an effort to increase the ease of use and the science that can be done with the array. To this end, NRAO continues to provide incremental capability enhancements above and beyond the operational efforts outlined above.


The pace of development for capability enhancements is matched to the available FTEs who are not fully engaged with daily operations. The VLBA can be operated as a stand-alone interferometer, in combination with other NRAO telescopes (phased VLA and the GBT) and as the foundation to the HSA in combination with the collaborating observatories (Effelsberg and Arecibo). We therefore split the planning for future enhancements into two categories: 1) those internal to NRAO (where the priorities are uniform across the observatory); and 2) those that depend on effort from (and priorities of) other observatories. Enhancements that can be managed solely within the NRAO are identified in Table 4-4 below. The rate at which a capability moves from being an RSRO to SRO to a General Observing capability depends upon the complexity of the task, the available manpower of visiting, resident experts, funding for hardware (in some cases) and the available FTEs within NRAO. Some assumptions about effort from participants in the RSRO program have been made in the schedule below; since these resources lie outside NRAO’s control, the delivery schedule for these capabilities may vary from that outlined below.

Table 4-4: VLBA Capability Enhancements Enhanced Observing Mode Capability 2014A 2014B 2015A Develop Y27 mode to match VLBA PFB and 8-channel dual-RDBE DDC mode (“PFB/DDC-8”).

RSR SR General

Develop single antenna sub-array for VLBI while observing a standard VLA program with remaining antennas (“Y1”).

RSR RSR SR

Implement ultra-rapid response capability. RSR RSR RSR Develop a narrow BW, quasi-real-time correlation capability to support real-time fringe checks and spacecraft tracking.

RSR RSR RSR

In addition to the enhancements described above, it is a high priority to enable a spectroscopic mode for the non-NRAO HSA antennas, to make available the full collecting area of the HSA for spectroscopic projects. This requires a DDC-compatible observing mode on Effelsberg and Arecibo, and although new instrumentation has been developed with similar general specifications to those of the DDC, detailed compatibility of both operation and control between the VLBA and these other stations has yet to be established. NRAO staff will work with these external observatories during FY 2014 to define a development path to complete this process. 4.3.3 Maintenance and Renewal The VLBA is approaching the twentieth anniversary of the end of its construction phase. Some critical components are becoming more problematic as they reach the end of their normal lifespan. These items include the masers, the azimuth track and the grouting, elevation bearings, and rust problems at the Hancock and Saint Croix sites. Maser issues are likely to continue in 2014 – two masers failed in FY 2013. Symmetricom, the supplier of these masers, will only consider repair of the newer models, and not the older ones. We are currently renting one maser and will probably rent another in FY 2014. One of the two failed masers is repairable, but the other cannot be repaired. The Saint Croix and Hancock sites, due to their local weather conditions, will soon require extensive re-painting to control rust on the structure. The local technicians perform spot painting on areas showing signs of rust, but more extensive painting is likely to be needed at some point. The grout on the rails of the azimuth track deteriorates with time and typically one antenna per year has needed re-grouting, patching of the concrete, and/or replacement of the rail, making it probable that this may be needed in FY 2014. Other


electronic components are also on the verge of becoming unsupportable due to obsolete repair parts and/or incompatibility with recent electronic updates. Those potential failures that pose the most serious risk to operations are being addressed through upgrade projects. Antennas: In FY 2014, the North Liberty and Hancock VLBA stations are scheduled to receive major maintenance visits by the VLBA Tiger Team comprising personnel from the antenna mechanics and servo groups. The number of visits will remain at two per year for FY 2014 (compared with three per year in FY 2012 and earlier) in order to reduce operations costs. We will continue to monitor the impact of the reduced Tiger Team visits to VLBA stations. The Tiger Team will inspect, repair, and upgrade mechanical and electronic components, as needed. Gears will be greased and checked for early signs of potential failure, and elevation bearings checked. Most, if not all, of the VLBA antennas will likely need both elevation bearings replaced over the next five years. Detailed descriptions of past VLBA Tiger team tasks are documented in the Antenna memo series available on the VLBA web site. Electronics Division Support: Each VLBA antenna contains eight cooled receivers, two compressors and numerous other electronics components. Although some of these components are supported in the Socorro labs, for efficiency, many are sent to the 20 VLBA site technicians for repair and maintenance. In FY 2014 sites technicians will continue to carry out the bulk of the routine maintenance tasks of:

• Inspection and lubrication of FRM, Az/El drive motors, encoder and pintle bearings, elevation gears, elevation hoist, change gearbox oil, etc.

• Check/test encoder motor tachometers, servo limits, ACU, vacuum pumps, all HVAC systems, dry air system, weather station equipment, etc.

• Ensure safety equipment such as UPS’s and generators, emergency power, fire alarm systems, fire extinguishers, security systems, etc. are operating normally.

• Ensure all other preventive maintenance tasks such as checking motor brushes and commutators are checked and replaced, check of Azimuth wheel position, check for metal in grease samples, cable wrap maintenance, replace oil filters, etc., completed in a timely fashion.

• Repair some VLBA specific modules to relieve some of this task from the technical staff at the DSOC and the VLA sites.

• Maintain the grounds and building infrastructure. • Other diagnostic and repair tasks as needed.

Other tasks performed by the Electronic Division personnel include support for the FEs. Because some of the VLBA receivers still use old-style LNAs (e.g., S-Band) that are no longer serviced by CDL, occasionally an entire receiver may have to be rebuilt with new LNAs in order to maintain full operational functionality. The Division is also responsible for the repair of 24 VLBA recording and playback modules, and repairs 100 Mark 5 disk packs per year. The maser lab is also part of the Electronics Division. It is currently in need of modernization, and NRAO will develop a plan for addressing the long-term support of the VLBA and VLA masers during FY 2014. RFI Mitigation: RFI mitigation efforts in FY 2014 will address the Brewster, WA 6cm RFI problem by working with the “USEI-Teleport” engineers to reduce the effects of their 6676 MHz satellite uplink signal on VLBA-BR C-Band Methanol line observing.


4.3.4 VLBA Major Milestones

FY 2014


Scientific Support for Operations

Support the 2014B semester (2014 Feb 1) Call for Proposals 1

Support the 2015A semester (2014 Aug 1) Call for Proposals 2

Complete verification tests of VLBA dual RDBE system 3 Define and document calibration procedures for VLBA dual RDBEs 4

Stabilize VLBA + Y27/GBT operations 5

Retirement of VLBA VMEs Design, build, and install VLBA Control Computer Interface Box in laboratory 6

Test VLBA Interface Box in VLBA Antenna 7

Retirement of Legacy Recording System

Complete transition of projects using legacy system to DDC 8

Re-integrate Mark 5A recorders from sites into correlator 9

C-Band Receivers Complete construction of spare VLBA C-Band receiver 10 Upgrade 2 pre-production VLBA C-Band receivers 11

Capability Enhancements Define and demonstrate new capabilities for 2014B 12 Define and demonstrate new capabilities for 2015A 13

Infrastructure Maintenance and Renewal Tiger Team maintenance campaigns 14 15

Milestones: 1-2. Scientific Support for the 1 Feb and 1 Aug calls for proposals, including software testing and updating documentation. 3. Complete verification tests of VLBA dual RDBE system. 4. Define and document calibration procedures for VLBA dual RDBEs. 5. Stabilize VLBA + Y27/GBT operations. 6. Design, build, and install VLBA Control Computer Interface Box in laboratory. 7. Test VLBA interface box in VLBA antenna. 8. Complete transition of projects using legacy system to DDC. 9. Re-integrate Mark 5A recorders from sites into correlator. 10. Complete construction of spare VLBA C-Band receiver. 11. Upgrade 2 pre-production VLBA C-Band receivers. 12. Define and demonstrate new SR and general capabilities for 2014B. 13. Define and demonstrate new SR and general capabilities for 2015A. 14. Tiger Team maintenance visit to North Liberty. 15. Tiger Team maintenance visit to Hancock.

Deliverables: [1-2] Documentation and software testing. [3] Operational dual RDBE system. [4] Documentation. [5] Capabilities stabilized. [6] Operational hardware. [7] Operational hardware. [8] Complete transition of projects using legacy system. [9] Operational hardware and software replacement. [10-11] Operational hardware. [12-13] New capabilities for SR and General observing documented and demonstrated operational. [14-15] Antenna and receiver maintenance.


4.4 Green Bank Telescope Overview In FY 2014 the GBT will remain in general operation with approximately 6500 hours of time devoted to science. A number of new instruments will be available in FY 2014, including a new 32–element 82-100 GHz bolometer array and an FPGA+GPU-based back end for spectral line and pulsar observations. Throughout FY 2014 routine maintenance and calibration of the telescope will take place, but there will be no significant modifications or upgrades to the telescope. There will, though, be an increase in the RFI identification and mitigations efforts on site, to ensure the site remains radio quiet. The Robert C. Byrd Green Bank Telescope, or GBT, is the world’s premier single-dish radio telescope operating at meter to millimeter wavelengths. Its enormous 100-meter diameter collecting area, its unblocked aperture, and its excellent surface accuracy provide unprecedented sensitivity across the telescope's full 0.1 - 116 GHz (3.0m - 2.6mm) operating range. The GBT is used by hundreds of scientists each year for a large and varied series of programs. It has a collecting area and sensitivity comparable to ALMA and the VLA and thus excellent response to point sources such as pulsars. But as a filled aperture it also has the highest possible sensitivity to extended, low surface-brightness emission of the kind associated with comets, molecular clouds, and distortions of the cosmic microwave background. The GBT also joins the VLBA for interferometric observations to provide a critical threshold of sensitivity for the highest angular resolution studies. The single focal plane is ideal for rapid, wide-field imaging using multipixel cameras. It thus serves as the wide-field imaging complement to ALMA and the VLA. The single focal plane is ideal for rapid, wide-field imaging systems – cameras. Because the GBT has access to 85% of the celestial sphere, it serves as the wide-field imaging complement to ALMA and the EVLA. Its operation is highly efficient, and it is used for astronomy about 6500 hours every year, with 2000-3000 hours per year available to high frequency science. The GBT is flexible and easy to use, and can respond to new ideas from the scientific community rapidly. It is straightforward for a small group to build and install a new instrument, providing them access to a world-class research facility. State-of-the-art instruments now under development in collaboration with university groups will continue to keep the GBT equipped with the latest technology. Graduate students use the GBT to gain hands-on experience with a major telescope, an increasingly rare opportunity and critical for their training. The telescope is oversubscribed, on average by a factor of four, with a much higher oversubscription at high frequencies and for some parts of the sky. It is scheduled dynamically to match project needs to the available weather, and is used for astronomy about 6500 hours per year. Green Bank has several thousand hours of clear skies with a precipitable water vapor content <10mm throughout the year, allowing extensive operations at short wavelengths. Since 2010 about 2000 hours have been available for weather-dependent high-frequency observations, a number which should increase as telescope control is improved. The GBT has the best protection of any U.S. observatory from many forms of man-made radio frequency interference as it is located in the National Radio Quiet Zone and the West Virginia Radio Astronomy Zone. The Observatory's location in a lightly populated valley in the Monongahela National Forest, surrounded by extensive ranges of mountains in all directions, providing further protection from interfering signals.


The Observatory is also a major resource for education and public outreach, and as such is an outstanding advocate for basic research and the work of the National Science Foundation. The Observatory produces nationally acclaimed programs in education, and the training of science and engineering students and teachers. These activities center on the Green Bank Science Center, with its auditorium, classrooms, and large exhibit hall, which is visited by 50,000 people every year. Thousands of K-12 teachers and students partake of residential educational programs using older radio telescopes no longer involved in research. The Observatory’s laboratories, utilities and support facilities make it an attractive location for independent research experiments and it serves as the field station for several university-based research teams. 4.4.1 Operations The GBT is in operation 362 days of each year, with an average of 6400 hours of science time annually. The GBT has achieved excellent 3 mm capabilities, with a 35% and 18% aperture efficiency at 90 and 115 GHz, respectively. GBT also has a dynamic scheduling system that will optimize the current weather conditions against each observing project’s scientific goals. By the start of FY 2014, the GBT instrument suite consists of single/dual-pixel receivers from 300 MHz - 96 GHz (non-contiguous), a 7-pixel heterodyne focal plane array at 18 - 26 GHz, and an improved bolometer array at 81 - 100 GHz. Industry-leading signal processing systems for the GBT are now in place, with a new high dynamic range, state of the art hardware for high time and high frequency resolution observations installed as well as ability to make very wide bandwidth (≥10GHz) observations for spectral line and pulsar detection experiments. The total amount of science on the GBT in FY 2014 is expected to remain at roughly 6,400 hours. Of these hours, roughly 450 (7%) will be provided to West Virginia University for use by their faculty while the remaining hours will be available under NRAO’s “open skies” policy to all qualified astronomers. Of the open skies time, typically 10% will be spent as part of the VLBI array, 30% on pulsar science, 5% doing continuum studies, and the remaining time on spectral line projects. A complete list of supported GBT receivers and backends is given below. Observer supplied backends also exist on site and are open for use with agreement of the instrument PI.

• Prime Focus: The prime focus receiver is mounted in an FRM on a retractable boom. The boom is moved to the prime focus position when prime focus receiver is in use, and retracted when Gregorian receivers are required.

o Prime Focus 1 (PF1): The PF1 receiver is divided into 4 frequency bands within the same receiver box. The frequency ranges are 290 - 395 MHz, 385 - 520 MHz, 510 - 690 MHz and 680 - 920 MHz. The receivers are cooled Field Effect Transistor (FET) amplifiers. The feeds for the first three bands are short-back re dipoles. The feed for the fourth is a corrugated feed horn with an Orthomode transducer (OMT) polarization splitter.

o Prime Focus 2 (PF2) (0.910 - 1.23 GHz): PF2 uses a cooled FET and a corrugated feed horn with an OMT.

• Gregorian Receivers: The receiver room located at the Gregorian Focus contains a rotating

turret in which the Gregorian receivers are mounted. There are 8 portals for receiver boxes in the turret. All eight receivers can be kept cold and active at all times. The Gregorian subreflector can be used for slow chopping. Unless otherwise stated, each of the Gregorian receivers is a cooled HFET amplifier and every feed/beam has a corrugated horn wave-guide. All calibration for the Gregorian receivers are done via injection of a signal from a noise diode.


o L-Band (1.15 - 1.73 GHz): This receiver has one beam on the sky, with dual polarizations. The feed has a cooled OMT producing linear polarization, but a circular hybrid can be chosen.

o S-Band (1.73 - 2.60 GHz): This receiver has one beam with dual polarizations. The feed has a cooled OMT producing linear polarization, but a circular hybrid can be chosen.

o C-Band (3.95 - 8 GHz): This receiver has one beam, with dual polarizations. The feed has a cooled OMT producing linear polarization, but a circular hybrid can be chosen.

o X-Band (8.0 - 10.0 GHz): This receiver has one beam, with dual circular polarizations. The feed has a cooled polarizer producing circular polarizations.

o Ku-Band (12.0 - 15.4 GHz): This receiver has two beams on the sky, each with dual circular polarization.

o K-Band Focal Plane Array (18.0 - 27.5 GHz): The K-Band Focal Plane Array has seven beams total, each with dual circular polarization. Each beam covers the 18-27.5 GHz frequency range. The feeds have cooled polarizers producing circular polarization.

o Ka-Band (26.0 - 39.5 GHz): This receiver has two beams, each with a single linear polarization. The polarizations of the two beams are orthogonal and are aligned at 45° angles to the elevation (and cross-elevation) direction. The receiver is built according to a pseudo-correlation design.

o Q-Band (38.2 - 49.8 GHz): This receiver has two beams, each dual circular polarization. o W-Band 4mm (67 - 93.3 GHz): This receiver has two feeds both with is a native circular

polarization. o MUSTANG-1.5 (75-105 GHz): MUSTANG-1.5 is 32 dual polarization, feedhorn coupled

bolometers with an instantaneous ~2

.5 field of view.

• Backends: o GBT Spectrometer: The GBT Spectrometer is a modular system, with four quadrants.

Quadrants may be used independently or grouped together into banks of 1, 2 or4 quadrants. This provides the observer with one to three different levels of spectral resolutions for each observing mode. The spectrometer performs auto correlations of the input signals. The spectrometer modes are divided into two major types, wide bandwidth, low resolution and narrow bandwidth, high resolution. The spectrometer has a dynamic range of about ±2.5dB from its optimal balance.

o Spectral Processor: The Spectral Processor is an Fast Fourier Transform (FFT) spectrometer primarily designed for high time resolution observations. Because of its wide dynamic range it is also useful for spectral line observations at low frequencies where strong interference is a problem. It contains two FFT engines, each with 1024 channels over a maximum bandwidth of 40 MHz which may be divided into 1, 2, or 4 separate pass bands. The two FFT engines are synchronous and their outputs may be cross-multiplied to measure polarization. The most commonly used types of observing with the spectral processor either total power or frequency-switched spectral line observations.

o VEGAS: The VErsatile GBT Astronomical Spectrometer (VEGAS) is an FPGA+GPU based backend which will be available for shared-risk observations in the 14A semester. VEGAS is comprised of eight separate spectrometers that can be run independently of each other. Observers can use any combination of spectrometers - from a single spectrometer to all eight—at the same time. VEGAS has a larger dynamic range than the GBT spectrometer and can retain a linear response in the presence of stronger RFI than the GBT spectrometer. In comparison with the spectrometer, VEGAS also has a wider total bandwidth, higher time resolution, and provides all four stokes polarizations.


VEGAS also has significantly higher time and spectral resolution that the spectral processor as well as more bandwidth. It is anticipated that VEGAS will replace all functionality of the GBT spectrometer and spectral processor over time.

o DCR: The digital continuum receiver (DCR) is the GBT's general purpose continuum backend. It is used both for utility observations such as pointing, focus, and beam-map calibrations, as well such as for continuum astronomical observations including point-source on/off, and extended source mapping.

o CCB: The Caltech Continuum Backend (CCB) is a sensitive, wideband backend designed exclusively for use with the GBT Ka-Band receiver over the frequency range of 26{40 GHz. It provides carefully optimized RF (not IF) detector circuits and the capability to beam-switch the receiver rapidly to suppress instrumental gain fluctuations.

o Mark5: VLBI/VLBA observing with the GBT is supported with a VLBA backend using the Mark5 recording system. The Mark5 VLBA disk recorder may also be used for single dish observing as a high time resolution (> 2ns) back end with up to a 256 MHz bandwidth.

Observing Programs The NRAO GBT offers two types of observing programs for our users: General Observing and Shared Risk Observing. The GBT General Observing program comprises access to well-tested observing modes/instruments while the Shared Risk Observing is used for new instruments as they are moved from the development program to general use. All GBT projects are assigned a project “friend” – a person to shepherd the project forward from the time it is accepted for observations by the NRAO’s Time Allocation Committee through the publication of its results. Additionally a telescope operator is on duty 24 hours a day, 7-days a week to watch over all site telescopes and to provide basic help to observers. A staff scientist is also on call 24 hours a day to respond to any problems which may arise during observations and to train any new GBT observers. Scientific Support for Maintenance of Receivers and Antenna Performance The GBT is in an operational state in which all effort goes toward maintaining telescope/instrument performance and ensuring that the user community has access to quality instrumentation and updated information to effectively use the GBT. During FY 2014 no new work on the GBT will be undertaken, and routine maintenance of all existing receivers and backends will occur. A complete listing of all GBT supported hardware is given above. Periodic checks for the overall telescope performance are undertaken, chiefly by the GBT telescope operators. A new telescope pointing model will be developed in fall, 2013 to ensure the most accurate telescope performance. 4.4.2 Upgrade and Enhancement Projects No upgrades or enhancements to the Green Bank Telescope are currently planned for FY 2014. 4.4.3 Maintenance and Renewal Track replacement/repair: The GBT track is now ten years old and is showing signs of wear. Beginning in FY 2014 NRAO will, on an annual basis, be replacing those GBT track pieces which show significant wear.


Telescope painting: Painting of the GBT is necessary to preserve the overall integrity of the structure. In FY 2014 we will continue the annual painting efforts at roughly the same levels as in FY 2013 and FY 2012. Green Bank Radio Frequency Interference Mitigation: Working with colleagues from the federal Sugar Grove, WV facility, NRAO will continue to administer all FCC applications within the National Radio Quiet Zone. NRAO also monitors the West Virginia Radio Zone, a ten mile radius around the GBT. NRAO will continue looking for potentially harmful interference and working with the community to find solutions for their needs which do not impinge upon GBT observers. Finally, in FY 2014 NRAO will be increasing efforts to eliminate internally created RFI on the Green Bank site, bringing an additional engineer into the interference protection group. Digital Servo Replacement: The original analog servo system for the GBT is out-dated and difficult to maintain. It is being replaced by a digital servo system that will provide the platform for model-based servo control, allowing for significantly improved telescope pointing and motion. The servo replacement is being run as part of operations and will continue in FY 2014. GBT and other telescopes: Ongoing telescope front-end and back-end maintenance will continue routinely in FY 2012, including cold-head and compressor maintenance for the cryogenic receivers, repair of failed parts in the front ends, servo and LO-IF systems, and the maintenance and repair of fiber optic connections. Antenna mechanics also check grease for metal chips, on the GBT and all other antennas, in the field to be alerted for potential failure of moving parts, especially azimuth truck bearings and elevation gears and bearings. Site Infrastructure: The GB site buildings and grounds will continue to undergo routine annual inspection and maintenance in FY 2012. This includes annual road repair and winter plowing; roof repairs; heating and cooling systems maintenance; pest and weed control; servicing of sewer systems, water supply, backup generator power, HVAC systems, electrical lines and related systems. Road repair, maintenance, and plowing (as needed): The GB site owns and maintains all roads within its boundary, and is therefore responsible to repair all damage and keep the roads clear for proper use and, most importantly, for the passage of emergency vehicles when necessary. To that end, the maintenance group is responsible to repair all road damage caused by accident or weather extreme, and plow the roads of snow in the winter. Proper maintenance of the roads has kept them in outstanding shape over the course of the last 50 years with minimal outlay of funds for replacement. These activities are required to ensure the GB site and the GBT remain in a current state of repair. Vehicle Support: The GB site continues to operate more than 65 vehicles and heavy equipment items, such as loaders, dozers, backhoes, trenchers, tractors, mowers, fleet vehicles, and buses. All of these are used daily and will continue to be routinely serviced and repaired to remain in safe, efficient working condition through FY 2012 and onward.


4.4.4 GBT Major Milestones

FY 2014


GBT Maintenance Telescope Painting 1 2

GBT Track inspection and Repair 3 Antenna Performance Development new pointing model for GBT 4

GBT Operations Retirement plan for GBT spectrometer, spectral processor 5

Milestones: 1. Beginning of summer painting 2. End of summer painting 3. GBT track inspection will take place, any needed repairs completed 4. A new pointing model for the GBT will be developed 5. A retirement plan for the GBT spectrometer and spectral processor will be put in place

Deliverables: [1] Telescope painters hired, trained [2] Telescope painting complete [3] Track inspection and repair report [4] New pointing model [5] Retirement plan announcement


4.5 Observatory Telescope Operations Financial/FTE Projections

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5 OBSERVATORY DEVELOPMENT PROGRAMS

5.1 CDL Development Overview The mission of the CDL is to support the evolution of NRAO’s existing facilities and to provide the technology and expertise needed to build the next generation of radio astronomy instruments. This is accomplished through development of the enabling technologies: low-noise amplifiers, millimeter and sub-millimeter detectors, optics and electromagnetic components including feeds and phased arrays, digital signal processing, and new receiver architectures. The CDL has a long history as a world leader in each of these areas. The CDL maintains a core expertise in each of these critical areas for support of NRAO instruments and for support of the astronomical community at large on a work for others basis. This core production and support activity for FY 2014 is described in Section 6.1. 5.1.1 Phased Array Feeds To increase the speed at which large areas of the sky can be surveyed, it would be hugely beneficial to more fully populate and sample the focal plane of large radio telescopes using multi-beam PAF receivers. Previous attempts of this approach have suffered from sensitivity losses which have effectively cancelled out the gains in field of view. The CDL PAF R&D program addresses the sensitivity issue using cryogenic cooling, which offers well-known clear improvements in noise temperature at the expense of cost and complexity. The focus in FY 2014 will be on improving PAF components, models, software and technologies to the point such that by the end of FY 2014, NRAO is ready to utilize these new features in an advanced PAF receiver for either single-dish or interferometric use, which can be specified and scoped with a reasonable amount of certainty. To accomplish this primary goal, we will focus efforts in FY 2014 on the following areas: Design studies for improved PAF front end components: Component studies and demonstrations in FY 2014 will include antenna elements, balanced low-noise amplifiers, low-loss cryogenic windows and filters, higher-efficiency cryogenics, novel Dewar construction concepts, and more modular and scalable technologies. Integrated Downconverter and Digital Photonic Transmitter: The CDL Integrated Receivers R&D program (see Section 5.1.2) has prototyped a digital sideband-separating downconverter with integrated photonic transmitter that represents a compact and efficient approach to receiver and array instrumentation. Wideband Digital Beamformer: A FGPA-based digital processor will be built and tested to perform the processing necessary to provide multiple beams on the sky. PAF Electromagnetic Modeling: An ongoing effort has been the development of modeling tools to characterize the radiation pattern, mutual coupling, and noise properties of the PAF. Ultra-wideband PAF Design Study: In FY 2014, we intend to study and model new wideband antenna elements and, in concert with the front end thermal design, study methods by which these elements can be cooled.


Software Development: In FY 2014, we plan to improve the usability of existing software by introducing version control and improved documentation. 5.1.2 Integrated Receivers The CDL has embarked on the development of a highly integrated receiver beginning at the antenna feed terminals or waveguide and ending in a digital data stream that may be delivered to any number of numerical signal processors. The signal will be digitized very close to the antenna output and sent via optical fiber to the central processing facility. Conventional electromagnetic polarization splitters will be largely replaced by much more accurate digital signal processing, and multiple frequency conversions will be replaced by a single mixer with high isolation digital sideband separation. Digital OMT: An S-Band triangular Digital OMT (DOMT) has been successfully developed for centimeter waves and will be tested on the sky. Additional research is scheduled in the coming years for development of millimeter and sub-millimeter DOMTs using modifications to probe geometry and implementation in the current design as well as researching a new turnstile design. Local Oscillator Distribution: Testing of the W-Band local oscillator distributor is scheduled for the 4th quarter of 2013 to measure the impact on phase stability. Success will be followed by implementation of the design on a larger scale, suitable for deployment in large format focal plane arrays and PAFs. Flexible Thermal Transition: Research into the trade-offs between thermal conductivity, flexibility, isolation, and transmission line losses to find an optimum solution for a printed circuit flexible thermal transition will continue over the coming years. The optimal solution will be key to achieving the scalability required for a compact integrated receiver. Compact Low-Power Digital Photonic Links: Due to the large successes achieved in 2013 with the digital sideband separating mixer, the compact integrated analog-to-digital-to-photonic converter, serial analog to digital converter (SADC), the unformatted digital fiber-optic link, and the integration of all these technologies, this research group is now in position to work towards miniaturization of this technology, while at the same time providing a digital back-end for the advancement and testing of the other technologies used in the integrated receiver. The SADC was successfully developed using off-the-shelf components.


5.1.3 CDL Development Major Milestones

FY 2014


Phased Array Feeds

PAF Low Noise Amplifiers 1 2 PAF Cryogenics 3 PAF Integrated Downconverter and Digital Photonic Link 4 5

PAF Wideband Digital Beamformer 6 7 PAF Electromagnetic Modeling 8 PAF Wideband Antenna Elements 9 PAF Software Development 10 11

Advanced Receiver Technologies

Digital Orthomode Transducers (DOMTs) 12 13 Local Oscillator Distribution 14 Flexible Thermal Transitions 15 Compact Digital Photonic Links 16

Milestones: 1. Design improved low-noise amplifier with lower noise and improved reliability 2. Design balanced low-noise amplifier for PAF integration 3. Complete study on cryogenic efficiency, new window and IR filter materials, and modular cryogenic architectures for large PAFs 4. Demonstrate single L-Band prototype integrated downconverter digital photonic link 5. Integrate and test digital downconverter photonic links on existing PAF 6. Demonstrate single-FPGA narrowband beamformer prototype 7. Demonstrate three-FPGA intermediate-bandwidth beamformer prototype 8. Demonstrate and verify PAF optimization algorithm with impedance matching network and feed geometry as input parameters 9. Complete design study on optimum wideband antenna elements for a PAF 10. Implement version control and document existing PAF software 11. Demonstrate new release of PAF software with improved user interface and real-time analysis capability 12. Test triangular Digital OMT (DOMT) on the sky 13. Demonstrate polarization isolation of DOMT using FPGA 14. Measure W-Band phase stability of the LO distribution network 15. Demonstrate printed circuit flexible thermal transition with low loss up to 40 GHz 16. Build multi-channel digital back end for testing of digital photonic links

Deliverables: [1] 1.1-1.7 GHz LNA design for PAF integration [2] 1.1-1.7 GHz balanced LNA design for PAF integration [3] Study report on cryogenic issues for large PAFs [4] Data on L-Band integrated downconverter digital photonic link tested in lab [5,16] Data on L-Band integrated downconverter digital photonic link tested on PAF [6] Tested single-FPGA beamformer [7]Tested three-FPGA beamformer [8] Verified PAF optimization algorithm [9] Study report on optimum wideband antenna elements for PAF [10] Documentation for PAF software [11] New release of PAF software with improved user interface and real-time analysis capability [12] Triangular DOMT data for on-sky testing [13] Polarization isolation test data of DOMT using FGPA [14] Phase stability test data for LO distribution network [15] Test data (RF loss and thermal conductance) from printed circuit flexible thermal transition [16] Multi-channel digital back end to test digital photonic links


5.2 ALMA Development Overview Upgrades typically progress through three successive phases of development, and correspond to an increasing level of technology readiness. The principal phases are:

• conceptual study (including scientific justification, specification, and outline costing), • prototype/pre-production, and • rate production and implementation.

The North American ALMA partnership typically funds conceptual studies (hereafter referred to as “Studies”) every year. Prototype/pre-production and rate production initiatives (hereafter referred to as “Projects”) are typically funded every two (2) years. A total of $5.3M is available for funding Studies and Projects during the FY 2014 Development Program cycle (subject to the FY 2014 Federal Budget and allocation of funds). Program overhead is equivalent to approximately five percent (5%) of the operating budget. Calls, proposal evaluation, and award of Studies and Projects are governed by different (albeit similar) processes. The following text describes the processes governing Studies and Projects, anticipated FY 2014 Studies, ongoing Projects, and anticipated FY 2014 Projects. 5.2.1 Development Studies Studies Process: The ALMA Operations Plan provides funding for targeted exploratory research and feasibility studies aimed at facilitating or assessing the viability of possible development projects, including assessments of opportunities for collaboration. This Hardware Small Projects and Upgrades (OFF-002) budget line is equivalent to approximately nineteen percent (19%) of the funds available for the FY 2014 NA ALMA Development Program. The North American ALMA Development Program Manager, in coordination with the ADSC, issues a Call for Study Proposals annually. An independent review panel evaluates and ranks the proposals, and submits its recommendations to the ADSC. The ADSC reviews, endorses (with or without modification) the recommendations of the independent review panel, and makes final recommendations to the North American ALMA Executive Office. The NA ALMA Executive has funding authority, and responsibility, for executing the NA ALMA Development Studies plan. FY 2014 Call for Study Proposals A total of $1.0M is available for funding Studies during the FY 2014 Development Program cycle (subject to the FY 2014 Federal Budget and allocation of funds). The NRAO expects to fund several Studies; no individual Study will be funded in excess of $200K. The FY 2014 Call for Study Proposals was released on 01 May 2013; notification of awards will be made on 30 August 2013. The Proposal submittal deadline was 12 July 2013. A total of nine (9) Study Proposals were submitted; five (5) were submitted by the NRAO and four (4) were submitted by various external institutions.


5.2.2 Development Projects Projects Process: The ALMA Operations Plan provides funding for final development and implementation of advanced techniques, hardware, and software. The North American ALMA Development Projects budget is equivalent to approximately 81% of the funds available for the FY 2014 NA ALMA Development Program. The JAO periodically hosts an ALMA Development Coordination Workshop. The timing of the Workshop is synchronized with a series of Regional ALMA Development Workshops (hosted by the respective Executives) which address regional scientific and technical interests. The JAO thereafter initiates a synchronized “Call for Development Project Proposals” on a cycle that is expected to repeat every two to three years. The NRAO conducts an internal review of its proposal(s) in preparation for the JAO Call. The sponsoring Executive presents each of its Project Proposals to the ADSC. The ADSC (considering the needs of the JAO, advice from the ASAC, scientific benefit, cost, schedule, safety, product/quality assurance, software, integration, operations, maintenance, and any associated risks) develops an integrated and balanced program of proposed projects. The ALMA Director submits this Integrated Development Plan proposal, along with suggested prioritization, to the Directors Council for concurrence and then to the ALMA Board for approval. The Executives (in possible collaboration with other institutes they may choose) oversee or carry out the development projects within their respective regions. The ADSC coordinates mid-term reviews to assess and recommend updates and adjustments to the program as a whole. The ADSC appoints small, external panels to conduct these reviews and they are undertaken in an open and transparent manner. The ADSC Chair presents the conclusions from each mid-term review to the ASAC for comment, and then the ALMA Director presents the report, together with recommendations for actions, to the Board. The ADSC monitors the expenditure from the Executives and tracks each Executive’s integrated expenditure over time. Contributions from the ALMA Executives are expected to match (or exceed) the agreed development expenditure when smoothed over a five-year timescale. The ADSC informs the Directors Council and the ALMA Board if expenditures fall below this level by more than twenty percent (20%). The under-expending Executive provides the ADSC with a plan consistent with the expectation that it will undertake additional development projects and rectify the shortfall within 24 months. The ADSC makes a recommendation to the ALMA Director regarding the appropriateness of the plan, and the ALMA Director, in turn, makes a recommendation to the Board. The ALMA Director, acting on the recommendation of the Chair of an Acceptance Review Committee, is the acceptance authority for completed development projects. 5.2.3 Ongoing Projects Summary Band 5 Local Oscillator (Lead Institution; NRAO): The NRAO is collaborating with the European Southern Observatory (ESO) to develop and deliver the ALMA Band 5 receiver (163 – 211 Hz). ESO, specifically a partnership of GARD (Sweden) and NOVA (Netherlands), is producing seventy-five (75) cold cartridges. The NRAO CDL is producing an LO (also known as a Warm Cartridge Assembly) for each Band 5 cold cartridge. The project is proceeding in accord with a two-phase development plan. Phase 1 – the design, fabrication, assembly and testing of one (1) pre-production Band 5 WCA – is complete. Phase 2 – production scale up and delivery of seventy-five (75) Band 5 WCAs – is underway.


NRAO is also responsible for providing cold multipliers (two per cartridge); NRAO will subcontract the production of one hundred-fifty (150) multipliers. Two potential sources are competing for the work and each is proposing a different design. Consequently, the entire order of will be issued to one supplier. “Down-selection” of the preferred design has not occurred as of this writing. This multi-year project began in Q4 FY 2012 and is scheduled to conclude in Q4 FY 2014. Total funding for this project is $3,328,717.00. ALMA Phasing Project (Lead Institution; MIT Haystack Observatory): The North American ALMA Development Program is providing $461,686 in supplemental FY 2014 funding to a pre-established, NSF Major Research Instrumentation project. This initiative, known as the “ALMA Phasing Project”, was approved by the ALMA Board of Directors in Q1 FY 2013. Altogether, the project goal is to make the ALMA observatory fit for Very Long Baseline Interferometry. The supplemental NA ALMA Development funds are allocated for software development, hardware/software installation, and commissioning at the Operations Support Facility and the Array Operations Site. The NRAO is also a subrecipient of the MIT Haystack NSF/MRI grant; the scope of this work package (comprised of correlator hardware and firmware upgrades) is covered in the “Work for Others” Appendix of this Plan. Fiber Optic Connectivity (Lead Institutions; JAO/NRAO. Subcontractors; Silica Networks, Telefónica Empresas Chile S.A., and REUNA): The ALMA Board approved this project to create an optical-based communication link between the ALMA Observatory and the Santiago Central Office (SCO) at its April 2012 meeting. The NRAO is funding the construction of an optical path from the AOS to Calama, and the upgrade of an existing optical path from Calama to Antofagasta (which will enable the use of a dedicated channel on one fiber of this cable). The European Southern Observatory (ESO) is contributing the use of an existing optical path from Antofagasta to the ESO-ALMA campus in Santiago. The project’s scope of work has since expanded, without additional cost, to include a redundant optical path as Silica Networks expands its infrastructure from the AOS, through Argentina, to Santiago. The fiber optic system supports higher data rates than the present microwave link (2.5 Gigabits per second versus 0.1 Gbps), and does so at a lower operating cost. The project commenced in Q4 FY 2012 and is scheduled to complete in Q2 FY 2014. Total funding for this “turn-key” project is $1.9M. FY 2014 Call for Project Proposals A total of $4.3M is available for funding Projects during the FY 2014 Development Program cycle (subject to the FY 2014 Federal Budget and allocation of funds). The NRAO expects to fund at least two Projects; no individual Project will be funded in excess of $1.5M. 5.3 GBT Developments Overview The GBT was designed to allow ready upgrades and changes to all aspects of its hardware and software. A specialty (or PI-driven) instrument can be installed on the telescope with relative ease, making it feasible for an individual or group of researchers to outfit the telescope to meet their particular science goals. The GBT also has a vigorous development program in collaboration with university groups to take advantage of the latest technology and provide the user community with a constantly improving facility. Development projects will continue through the coming decade and have already led to important discoveries in a number of areas. These include:


• Constraining the Nuclear Equation of State through detection of the most massive neutron star

known. • Probing Dark Energy through HI intensity mapping. • Imaging the Large Scale Structure in Galaxy Clusters by creating the highest resolution, most

sensitive images of the Sunyaev-Zel’dovich effect. • Understanding the Solar System through radar maps of the Moon, probing the atmosphere of

Titan, and bi-static radar observations of Mercury, Venus and Europa. 5.3.1 ARGUS In FY 2014 a group led by the University of Stanford began the construction of a 16-pixel 90-116GHz traditional feed horn array, funded through the NSF-AST ATI program. The GBT is the best telescope in the world for molecular line studies in the 70-100 GHz band. The proposed camera would capitalize on that fact by using the GBT’s sensitivity to create an on-the-fly image of cometary molecules. When combined with the GBT’s sensitivity, the camera would be the only system in the world which could provide information about the structure of comets as they move through the solar system. Development of the instrument will continue in FY 2014, with commissioning of the instrument taking place in the winter of 2014/2015. NRAO staff will be deployed to the project to aid in the adaption of the instrument to a full user instrument. 5.3.2 MUSTANG In FY 2013 a group led by the University of Pennsylvania began building a new 81-98 GHz bolometer array for the GBT. This array is assembled from new frequency-domain microwave SQUID (mSQUID) multiplexers recently developed by NIST (using the same backend electronic as mKIDS) and contoured feed horns. Due to the small size of the array (32-64 pixels), it will not provide a significant increase in the overall sensitivity and mapping speed of the GBT. The array will, though, provide a more stable array than exists and the infrastructure needed to install the full 200+ pixel MUSTANG2 system which will provide a greater than 100x increase in the GBT’s mapping speed. The MUSTANG2 array is not yet funded. The project was schedule to be complete in FY 2013. However, delays in getting NIST to deliver the detectors for the instrument have resulted in delays from the original schedule provided by. New receiver commissioning will occur in Q1-Q2, FY 2014. 5.3.3 GBT Development Major Milestones

FY 2014


Camera Development ARGUS 1,4 2,3 5 MUSTANG 1.5 6 7

Milestones: 1. ARGUS Cryostat Complete 2. ARGUS Module delivery complete 3. ARGUS IF/LO complete 4. ARGUS Warm electronics complete 5. ARGUS Feeds complete 6. MUSTANG 1.5 Science commissioning begins 7. MUSTANG 1.5 project complete

Deliverables: [1] ARGUS Cryostat [2] ARGUS Module [3] ARGUS IF/LO [4] ARGUS Warm electronics [5] ARGUS Feeds [6] None [7] MUSTANG 1.5 commissioning report


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6 OBSERVATORY-WIDE SERVICES

6.1 Central Development Laboratory Productions, Maintenance & Repair Low Noise Amplifiers The CDL has for the past thirty years provided NRAO and the astronomical community with the world’s lowest noise amplifiers from 0.1-115 GHz. These low-noise amplifiers have not only been responsible for the high sensitivity and success of the VLA, GBT, VLBA, and ALMA, but they have been used by nearly every other astronomical instrument requiring cm-wave low-noise amplifiers built in the last thirty years, including WMAP, CARMA, DASI, CBI, Planck, and many others. In FY 2013, the CDL will have completed production of all the spare LNAs needed for the VLA. It was discovered in 2012 that higher levels of vibration in the new VLA refrigerators were causing a large failure rate in the L-Band LNAs due to wire bonds disconnecting from capacitors. A fix was implemented involving the replacement of thin-film capacitors with ceramic capacitors. During the next year, as receivers come in for maintenance, these amplifiers will be returned to the CDL and upgraded as a preemptive measure. These repairs began in early 2012 and are expected to be complete by the end of FY 2014. In addition to these and other LNA repairs for the VLA and GBT, the CDL LNA group will continue to support the general radio astronomical community on a work-for-others basis. For example, it is expected that a large contract for ALMA Band 1 LNAs will be placed by ASIAA, resulting in the production of approximately 150 35-52 GHz LNA being produced and delivered from FY 2014-FY 2016. This proposed effort is addressed in Appendix F as Work for Others. Millimeter & Submillimeter Detectors The current generation of mm/sub-mm SIS receivers, as used on all the higher frequency bands of ALMA, was the result of a long period of development at the CDL in collaboration with the University of Virginia Microfabrication Laboratory (UVML). This includes the introduction of niobium-based superconducting circuits for radio astronomy, development of wideband SIS mixer MMICs, and the use of sideband-separating SIS mixers which were pioneered at the CDL. In FY 2014, the CDL will continue to support the offsite maintenance of the ALMA Band 6 receivers, maintaining a sufficient quantity of spare mixers and preamps. The CDL will also support community projects, such as outfitting other sub-mm telescopes for the sub-mm VLBI, such as Mt Graham, South Pole Telescope, Greenland Telescope, etc. on a work for others basis. In addition, the CDL will continue efforts to develop the next generation of SIS mixers for ALMA enhancements. Specifically, in FY 2014, the CDL will continue development of (i) an improved ALMA Band 6 mixer with a balanced dual-sideband topology and wider 4-12 GHz, and (ii) SIS mixers with NbTiN electrodes for lower noise above 600 GHz, near the superconducting bandgap of Nb. The upgraded Band 6 mixer will utilize AlN barriers, improving noise performance at the band edges, and incorporate an expanded 4-12 GHz IF bandwidth. The wider IF requires the development of a 4-12 GHz balanced LNA (for improved match with mixer output) that has sufficiently low power dissipation to be used in the ALMA receiver. Development of an operational balanced multi-junction SIS mixer also requires development of techniques for improved magnetic suppression of the Josephson effect. On the NbTiN SIS development path, the CDL and UVML will in FY 2014 fabricate and test a single-ended Nb/Al-AlN/NbTiN SIS mixer designed to have near-quantum-limited noise performance up to 1 THz. In order to produce a balanced mixer at these frequencies (which will reduce the LO power requirements


and suppress the LO noise), the CDL will also build and test hybrids that operate at these frequencies. These hybrids can either be waveguide (where THz waveguide hybrids require extremely precise machining) or planar (using ultra-thin Si membranes with AU beam leads in a process developed by UVML). Optics and Electromagnetic Components Crucial to the sensitivity, beam quality, and polarization purity of NRAO’s instruments has been the design of the receiver optics and electromagnetic components, including the feeds, OMTs (orthomode transducers), and phase shifters. For example, almost every one of these components that went into the VLA upgraded receivers could not be commercially purchased, but were developed, measured and mostly manufactured at the CDL. In addition to continued support in FY 2014 of the electromagnetic needs of the GBT, VLA, VLBA, and other partners on a work for others basis (see Appendix F), the CDL will continue work on the optics plan for ALMA Band 2 (67-90 GHz). It is proposed to develop compact reflective optics that fit on top of the cryostat, matching the telescope beam waist to that of the feed. The components for this will be built and tested during FY 2014. Digital Signal Processing During the past several years, the CDL digital group dedicated itself to the successful production and testing of the main correlator for ALMA. During the past year, this effort has wound down considerably with the provisional acceptance of the correlator by ALMA. During FY 2014, work on this project will consist mainly of supporting the continuing high-level software development. In FY 2014, the CDL Digital Group will begin to support the PAF R&D program described in Section 5.1.1 by assisting with the design of the FPGA digital beamformer. In FY 2014, the CDL digital group will also be supporting the PAPER commissioning (see next paragraph) and the ALMA Phasing Project (see Appendix F). In support of PAPER, the digital group is collaborating with a group at U.C. Berkeley to upgrade the data acquisition system. The upgraded system will provide inputs for 12 analog channels with bandwidths up to 500 MHz, digitize them, and route them to a large FGPA which will time tag and format for 10 Gbps fiber outputs. Low Frequency Radiometry In collaboration with U.C. Berkeley and U. Pennsylvania, the CDL delivered the dipole elements for the expansion of PAPER-128, the 128-element dual polarization dipole array stationed in South Africa. In FY 2014, the CDL will continue to support the commissioning of the expanded PAPER as it attempts detection of the Epoch of Reionization (EoR) signature. Although PAPER is funded mostly through a subcontract, there is contributed effort from the CDL since this is a high-priority project on the roadmap to HERA (Hydrogen Epoch of Reionization Array).


6.1.1 CDL Major Milestones

FY 2014

Program Project Q1 Q2 Q3 Q4 Low Noise Amplifiers VLA L-Band Repair 1

MM & Sub-MM Detectors

Band 6 Spare Mixer Production 2 Band 6 Balanced SIS Mixer Upgrade 3 4 THz SIS Mixers 5 6

Electromagnetics & Optics Band 2 Receiver Optics 7 8

Digital Signal Processing PAPER 9

Low Frequency Radiometry

PAPER 10 Solar Radio Burst Monitor 11,12 DARE 13

Milestones: 1. Complete repairs of VLA L-Band LNAs 2. Complete production of eight spare Band 6 SIS mixers 3. Demonstrate 4-12 GHz balanced IF LNA with low power dissipation 4. Demonstrate balanced 2SB SIS mixer with 4-12 GHz IF that exceeds noise performance of current Band 6 mixer 5. Demonstrate Nb/Al-AlN/NbTiN SIS mixer with low noise up to 900 GHz 6. Demonstrate low-loss hybrid for 800-950 GHz 7. Complete design of reflective Band 2 optics 8. Build and measure Band 2 feed 9. Produce prototype data acquisition upgrade for PAPER 10. Characterize beam pattern of MWA tiles and PAPER antennas using ORBCOMM satellite 11. Deploy upgraded low-frequency antenna on Green Bank solar radio burst monitor 12. Deploy improved data acquisition system on Green Bank solar radio burst monitor 13. Deploy DARE engineering prototype in Green Bank

Deliverables: [1.] Repaired and tested VLA L-Band LNAs [2.] Eight fully qualified spare Band 6 SIS mixers [3.] Test data for 4-12 GHz balanced LNA [4.] Test data for balanced 2SB SIS mixer [5.] Test data for 900-GHz Nb/Al-AlN/NbTiN SIS mixer [6.] Test data for 800-950 GHz hybrid [7.] Design report for reflective Band 2 (67-90 GHz) optics [8.] Band 2 (67-90 GHz) feed with test data [9.] Test data for PAPER data acquisition upgrade [10.] Measured beam patterns of MWA tiles and PAPER antennas [11.] Upgraded low-frequency antenna on GB solar radio burst spectrometer [12.] Upgraded data acquisition system on GB solar radio burst spectrometer [13.] DARE engineering prototype installed in GB


6.2 Data Management & Software Department (DMSD) Overview The NRAO DMS in FY 2014 will make key contributions to the NRAO. A new NRAO Archive will be designed and prototyped while maintaining access to data through the existing NRAO and ALMA Archives. Pipeline capabilities will be further enhanced, most notably through improved imaging capabilities, but also including operational improvements such as automatic invocation for ALMA and QA parameters and displays for the VLA. The ALMA Systems group will support Cycle 1 and 2 observing, while preparing the needed capabilities for Cycle 1. The Green Bank and New Mexico Systems groups will provide support for observing and the planned new observing capabilities, including for the very high data rate VEGAS spectrometer. NRAO will make its computing facilities available to the external community both through direct cluster access, and for ALMA and the VLA through a reprocessing user interface. 6.2.1 Software Development This section contains user-facing software developed at the NRAO, with the exception of GBT post-processing software which is described in GB System, below. Archive Access Tool: The NRAO Archive (which is separate from the ALMA Archive; an ESO deliverable) has been in production for over 10 years, serving many 100s of terabytes of raw data. However an internal review in FY 2013 has shown that the infrastructure is showing its age, and that it is time to modernize the NRAO Archive infrastructure, and its user interface (the AAT). In FY 2014 NRAO will solicit requirements for this update from SSR/SUS and the external community (already partially addressed through User Committee input). DMS personnel will thereafter analyze the requirements, and develop an architecture, implementation plan, and a functional prototype for evaluation before the final implementation. In forming this architecture, commonality with ALMA (both interface and code reuse) will be taken into account to the extent practical, as will Virtual Observatory (VO) interoperability. The new NRAO Archive will be able to technically support all NRAO telescopes, including ALMA public data, both raw and pipeline processed. GBT VEGAS raw data at full resolution (time, spectral) will not be made available, at least in FY 2014, for financial reasons. This effort is a critical one. If its pace of development is inadequate with the currently allocated resources, DMS will divert resources from other areas (most likely OPT, PHT, and PST) to ensure that it advances satisfactorily. CASA: The NRAO post-processing software, CASA, development continues to emphasize support for the VLA and ALMA unlocking the scientific potential of these world-leading telescopes. During FY 2014, NRAO will continue to add capabilities and support our evolving understanding of the requirements of these forefront telescopes. The eighth public release of CASA will be identified as version 4.2 and made available to the public in Q1 FY 2014. This release brings performance optimizations in most aspects of the system; of particular note are improvements in the data visualization capabilities, the inclusion of the ALMA Cycle 1 pipeline heuristics and improved handling of weighted data. CASA 4.3 will expand the capabilities of the CASA based pipeline, deploy a refactored imaging suite, and introduce the Calibration Library (cutting disk space requirements by approximately one third).


The international team, led by NRAO, continues to increase support for single dish data reduction and high performance computing capabilities working on the integration of HPC capabilities with the standard reduction pipelines. The CASA team will continue to support and develop new imaging and calibration algorithms. Wide-band wide-field imaging algorithms and polarization calibration for linear feeds will begin being used by the wider community during FY 2014. CASA Pipeline: The CASA pipeline will be used throughout ALMA Cycle 1 data reduction, assisting in the data analysis and undergoing advanced commissioning. Both interferometric and single dish observations are currently supported. The heuristics of the VLA scripted pipeline will be integrated with the CASA pipeline by Q1 FY 2014. The pipeline will continue to evolve throughout the FY 2014 time period as experience more observing modes are commissioned and additional experience is gained by the community in using ALMA and the VLA. Most importantly, the focus will switch from calibration and flagging to evaluating and improving the pipeline imaging stages. Additionally, ALMA Cycle 1 experience in Single Dish and ALMA Compact Array observations are expected to drive additional heuristic development in preparation for ALMA Cycle 2. Observation Preparation Tool: The OPT for the VLA will be updated to support new instrumental capabilities during each observing semester. This includes support for commissioning (including RSRO) observations, and once commissioned for general observing. Updates for commissioning occur in the semester prior to when they are needed for general observing. New capabilities for the VLA, along with their status for the 2014A, 2014B, and 2015A observing semesters, are listed in section 4.2.3 above. Proposal Handling Tool: The PHT will be updated to support required functionality for the TAC meetings for the 2014A and 2014B observing semesters. Initial work to support the TAC meeting for the 2015A observing semester will occur in Q4, but will not be complete until Q1 of FY 2015. Proposal Submission Tool: The PST will be updated to support required functionality for the 2014B and 2015A calls for proposals. New functionality that is needed for those calls is described in sections 4.2.3 and 4.3.3. Reprocessing Interface: DMS has received requirements for a unified data processing interface for ALMA, GBT and the VLA. In FY 2014, DMS will implement a standalone web application allowing astronomers to describe and submit data processing requests to NRAO’s processing pipeline. This first stage of the application will offer a 'basic view' of the interface, allowing simplified control of commonly used parameters and providing sensible default values. In a later stage it will be integrated with the new NRAO Archive and an 'advanced view' will be provided. This processing interface is in addition to the system level cluster access described in the Scientific Information Services section below. 6.2.2 ALMA System Software NRAO is responsible for delivering software to the JAO as part of the ICT. The ICT is staffed by personnel in all three ALMA Executives and the JAO. In North America, some work is provided by the National Research Council of Canada in the ALMA Archive Subsystem. This contribution is technically managed by ESO and is not described here. The bulk of the work done at NRAO by the ALMA System Software group consists of Offsite Maintenance and Repair, which in the ALMA Operations Plan version D is described by the OFF-004


budget line. In addition, the ALMA System Software group is responsible for the NRAO software (not firmware) contribution to the ALMA Phasing Project. The NRAO ALMA System Software group contributes to the following ALMA ICT work areas:

• Control/Correlator Software. This is the software that controls and monitors all the ALMA equipment excluding the ACA correlator, interprets the scheduling blocks, and forms the bulk data and auxiliary data for the post-observing and Archive systems. It includes many online GUIs, including the quick-look display screens. It also includes the NRAO contributions to the ALMA Phasing Project. This software is almost entirely the responsibility of the NRAO (< 0.5 FTE at ESO).

• Scheduling. The NRAO is responsible for the dynamic scheduling ranking software (the dynamic scheduling parameters and weights are the responsibility of DSO), manual and queued observing modes, scheduling GUIs, and an offline planning mode. This functionality is entirely the responsibility of the NRAO.

• Other. NRAO makes other software contributions to the JAO, including a contribution to overall ICT management, software testing, and modest (0.5 FTE) contributions to various operations GUIs (primary responsibility ESO).

It has to be understood that the planning priorities for this group are the responsibility of the JAO; in particular the Science Operations IPT, lead by the DSO, defines the priorities. The below items represent only the highest priority items or summarize items which in details are split into several sub-items. The planning items for the ALMA System group are as follows: Dynamic Scheduling: Dynamic scheduling has largely been implemented. This item is to follow-up as DSO tests this software to make the changes necessary to enable the software to be used during science observing. Quick-look Improvements: General improvements in the user interfaces used to visualize calibration results, e.g., allowing the selection of antennas, and the ability to browse through past results. Scan sequences (incorporating online calibrations): For more efficient observing the application of calibration results should be included within programmed sets of scans i.e., a scan sequence. This will avoid an additional delay of around 15 seconds between scans which require a calibration before proceeding. This is a part of the overall scan sequence implementation which started in 2012 and has contributed to dramatic improvements in ALMA observing efficiency. Correlator Improvements: These consist of:

• Implementing multiple sub-arrays in the correlator software. • Verifying that the correlator software can deliver the full specification (60 MB/s) to the Archive

ingest process. • Finishing the remaining (low priority) modes in the correlator: 2x Nyquist, 3x3 and 4x4 bit

modes.


ALMA Phasing Project Correlator Software: NRAO will contribute the following areas to the ALMA Phasing Project (under the overall management of Haystack Observatory) as our contribution to that project.

• Ensuring that the software is developed according to ALMA standards. • Implementing/revisiting the correlator protocols. • Shared development responsibility of the VLBI Observing Mode software component. • Development of simulation capabilities. • Integration and testing support.

6.2.3 VLA/VLBA System Software VLA/VLBA Support for Commissioning and Observing in semesters 2013B, 2014A, and 2014B: The new capabilities described in sections 4.2.3 and 4.3.3 above will be supported in the system software for the two telescopes. This includes tipping scans, improved switched power handling, and improved observation scheduling for the VLA, and ultra-fast response and quasi-real-time correlation capability for the VLBA. VLA – Full OTF Mosaic Support: The VLA will implement an observing mode in which mosaics are taken with the antennas in continuous motion (compared to sidereal rate). This should be considerably more efficient in observing time since data can be taken nearly continuously (other than turnaround time at the end of rows, and calibration scans); as opposed to having to wait while the antenna settles to each new position in a multi-pointing mosaic. There is some work in the online required software to enable this mode. VLBA – Partial Implementation of VME Replacement: The VME real-time computers at the VLBA stations are now quite old and a maintenance risk. We will prototype replacing the VME computers with digital I/O connected to a modern control computer already at the VLBA stations. If successful, this will mitigate risk of catastrophic failure arising from this obsolete hardware. VLBA – Quasi-Real-Time Spacecraft Tracking: The VLBA can already accurately determine the position of spacecraft. When combined with the capability to do quasi-real-time correlation, this will provide the capability to have rapid turnaround on those position determinations. VLBA – Wideband Observing stabilization: The new wideband observing system for the VLBA is still operationally immature. During FY 2014, an emphasis will be placed on stabilization and documentation of existing capabilities, across all of the telescopes that participate in wideband VLBA observations. 6.2.4 GBT System Software WV Systems Archive: In FY 2013, GB SDD developed software to include GBT data in the NRAO Archive. A list of subsequent requirements was developed and we have been implemented with 0.3 FTE. DMS expects to complete the remaining requirements in Q2 FY 2014. WV Systems Monitor and Control: FITS files are currently used as the inter-process communication mechanism between the monitor and control system and the data post processing software for near real-time processing during observations. This arrangement is not ideal given the development of the VEGAS spectrometer, which can potentially produce massive data sets. DMS has


therefore begun the process of modifying the monitor and control system to stream data using TCP-based software technology. Most of the core infrastructure changes were completed in FY 2013; that work and complete modifications to the data post processing software is expected to be complete in FY 2014. Modifications to Astrid to utilize the streaming-related changes will be started. GBTPP – Pipeline: In FY 2014, DMS will modify the pipeline to support the highest non-pulsar VEGAS data rates necessary for mapping. This is expected to involve use of the GBT streaming infrastructure and parallel use of CASA for imaging. DMS will also expand upon the use cases supported by the spectral pipeline. 6.2.5 Scientific Information Services The Scientific Information Services (SIS) division was successfully matrixed into the new DMS during FY13, sharing resources with the existing information Technology-centric Computing and Information Services (CIS) division (under OAS see section 6.8). This has enabled transparent sharing of highly skilled Information Services resources to be available for both telescope supporting science responsibilities (DMS), as well as general staff IT support duties (CIS). There are 4 major functional groups in SIS: Computing Operations (NAASC, NM, GB): These site centric groups directly support the day-to-day telescope operations and delivery of data to the archive. They ensure that development projects are appropriately staffed with resources being assigned based on commitments and timelines tracked within the Program Management Department (PMD) and at the site. Project and milestones for these resources are tracked under the appropriate telescope support sections. Archive & Cluster Processing: This group is responsible for the support of the production archive, parallel processing clusters and user storage resources needed in support of pipeline processing and science data analysis. It defines their operational model for these shared resources (e.g. with batch and resource scheduling) and works closely with the Software Division. There is substantial staffing and skills overlap with Common Computing Environment (CCE). Although not explicitly tracked as a milestone, this group will ensure sufficient storage is provisioned throughout FY14 to keep up with observations, within the budget envelope. Science Computing Infrastructure: This group provides technology driven Computer Engineering support, and is tasked with delivering the next generation of data processing solutions, working in close cooperation with the Software Division, CDL and external CyberInfrastructure partners (e.g. XSEDE, National HPC centers, Internet2/NLR). This group is responsible for escalations from Archive and Cluster Processing and CIS in the event of systematic performance issues with the production infrastructure. Science Portal Service: Responsible for the installation and management of the Observer facing services obtained from external entities (e.g. Kayako Helpdesk, ALMA Science Portal, NRAO User Forum). It is also responsible for the Observer identity/permission Database and the close integration of the service access which they enable. Wide-Area Networking: Science data capacity driven group responsible for provisioning the long-haul, high bandwidth, connectivity to deliver reliable throughput in support of observation data transport. Operational support for commodity circuits will be handed off to CIS once a network service has been accepted into production.


The following sections outline the activities and milestones coordinated by SIS, to ensure an optimum computing, storage, and communications environment for staff and users of NRAO telescopes as well as providing agile service support for an active research and development program. Post-processing resource access: In FY 2014 NRAO will begin making post processing cluster and storage resources formally available to external users. By Q1 FY 2014 DMS will submit a final computer access policy for ratification by the NAASC and New Mexico Operations and implementation by SIS. In Q2 FY 2014 DMS will advertise the availability of resources along with documentation describing the usage policy and access details. Availability of resources is subject to demand with higher priority going to pipeline processing and reprocessing through the planned reprocessing interface. Incremental improvements will be made throughout FY 2014 based on user feedback. Network performance: To accommodate optimized transport of larger data sets, remote access and potential integration with external compute facilities SIS will implement rigorous testing of NRAO’s external network links. In Q1 FY 2014 SIS will install test points based on the NSF funded Internet2 Perfsonar test suite to allow for regular performance monitoring of NRAO links. In Q3 FY 2014 documentation for the use of these test points will be provided for external users to isolate network loss and bandwidth issues at their end. Cluster performance: Throughout FY 2014 SIS will work with CASA developers to improve resource utilization, monitor post processing cluster utilization and investigate alternate cluster configuration technologies like ScaleMP™ or alternative architectures involving GPUs or the Intel Phi™ coprocessor. In Q4-FY 2014 SIS will issue a report characterizing cluster utilization efficiency with recommendations for FY 2015. The Pipeline processing hardware for CASA, and incremental archive expansion, will follow science driven demand with the NAASC and VLA backup leveraging a 10Gigabit local area network (LAN) link (Q1) and hosted data center access to the University of Virginia to minimize the Charlottesville site facilities upgrade costs (Q2 FY 2014). The anticipated 10Gigabit link into the Green Bank site should be accepted into production in Q1 FY 2014 conditional upon Internet2 access fees being negotiated with WVU/3ROX by Q2. This link will lead to the option for remote data storage leveraging XSEDE national center CyberInfrastructure (conditional upon DIBBs award with PSC) in Q3. 6.2.6 DMSD Major Milestones This section is reserved for significant managerial or administrative functions of the DMS department itself. Technical items are reported in the previous sections. DMS Formation Complete: To finalize the DMS department formation a permanent head of the software division needs to be appointed, and an NRAO Data Management Plan needs to be written and accepted by the NRAO Director at the version 1 level. DMS Review: The NRAO Director will organize a review of the NRAO DMS department to advise AD on further changes or additions that should be implemented.


FY 2014

Program Project Q1 Q2 Q3 Q4 Software Development

AAT Initial design 1 Prototype 2

CASA Pipeline Early Science ALMA Cycle 1 3 Integration of VLA Scripted Pipeline 4 Early Science ALMA Cycle 2 5

CASA

4.2 Release 6 4.3 Release 7 4.4 Development (FY 2015 Release) 8 8 8 8 VO Support 9

OPT 2014A VLA Observing Updates 10 2014B VLA Observing Updates 11

PHT Updated for 2014A TAC Meeting 12 Updated for 2014B TAC Meeting 13

PST Updated for 2014B Call for Proposals 14 Updated for 2015A Call for Proposals 15

Reprocessing Reprocessing Interface 16 ALMA System Software

System Software Updates, Bundle 1

Dynamic Scheduling 17 Quick-look Improvements 18 Scan Sequences (Incorporate TelCal calibrations) 19

System Software, Updates, Bundle II Correlator improvements 20

VLBI Modifications ALMA Phasing Project Correlator Software 21 VLA/VLBA System

VLA/VLBA

Support 2013B Observing 22 Support 2014A Commissioning 23 Support 2014A Observing 24 Support 2014B Commissioning 25 VLA - Full OTF Mosaic Support 26 VLBA - Partial Implementation of VME Replacement 27 VLBA – Quasi-Real-Time Spacecraft Tracking 28 VLBA - Wideband Observing Stabilization 29

GBT System WVSys – Archive Complete GBT Data into NRAO Archive 30

WVSys – M&C

Data Streaming Phase 1, complete core infrastructure changes 31 Data Streaming Phase II, modify M&C system to use new infrastructure 32

Modify Astrid to use streaming 33

GBTPP – Pipeline Use CASA for GBT Imaging 34 VEGAS support at highest data rates 35 Parallelize Pipeline 36

Scientific Information Services

Archive & Cluster Computer access policy for external users 37 Early access to cluster resources 38

XSEDE/Cloud Grid/Cloud Middleware installation 39 Prototype access to non-NRAO cycles 40

Network Performance Improved monitoring of Internet 2 links 41 Remote link test procedures released to users 42

Cluster Performance Cluster characterization recommendations 43

Co-location at UVa Installation of 10Gigabit/s link to UVa Data Center 44 Installation of storage at UVa 45


FY 2014

Q1 Q1 Q1 Q1

Green Bank data link Delivery/install of 10Gigabit network hardware 46 Go-live of GB link 47 Conditional access to PSC Data Supercell 48

DMSD Administration

DMSD Administration DMSD Formation Complete 49 DMSD Review 50

Milestones: 1. Develop initial design of ALMA Archive Tool 2. Develop ALMA Archive Tool prototype 3. Develop CASA pipeline for ALMA Cycle 1 Early Science 4. Integrate VLA Scripted Pipeline 5. Develop CASA pipeline for ALMA Cycle 2 Early Science 6. Release CASA version 4.2 7. Release CASA version 4.3 8. Develop CASA version 4.4 9. Develop CASA VO support 10. Implement OPT updates for Semester 2014A VLA observing 11. Implement OPT updates for Semester 2014B VLA observing 12. Implement PHT updates for Semester 2014A TAC meeting 13. Implement PHT updates for Semester 2014B TAC meeting 14. Implement PST updates for Semester 2014B Call for Proposals 15. Implement PST updates for Semester 2015A Call for Proposals 16. Complete Reprocessing interface 17. Deploy Dynamic Scheduling software 18. Deploy Quick-look improvements software 19. Incorporate TelCal calibrations in scan sequences 20. Implement correlator improvements 21. Deploy ALMA phasing project correlator software 22. Deploy software to support Semester 2013B observing 23. Deploy software to support Semester 2014A commissioning 24. Deploy software to support Semester 2014A observing 25. Deploy software to support Semester 2014B commissioning 26. Deploy hardware & software to support Full On-The-Fly Mosaics for VLA Resident Shared Risk Observing use 27. Conduct observations with new, non-VME hardware 28. Demonstrate quasi-real time spacecraft tracking 29. Demonstrate wideband observing stabilization 30. GBT Data in NRAO Archive 31. Core infrastructure changes complete 32. M&C system modified to use new infrastructure 33. Deliver Astrid modifications & commission on-site 34. Deliver GBT imaging capability in CASA 35. VEGAS supports highest data rates 36. Complete GBT Pipeline parallelization 37. Draft computer access policy for external users 38. Enable early access to cluster resources 39. Install Grid/Cloud Middleware 40. Prototype access available to non-NRAO computing cycles 41. Enable improved monitoring of Internet 2 links 42. Release remote link test procedures to users 43. Complete cluster performance characterization 44. Install 10 Gigabit/s link to UVa Data Center 45. Install storage at UVa 46. Install 10 Gigabit network hardware 47. GB link go-live 48. Condition access to PSC Data Supercell 49. Complete Data Management & Services formation 50. Organize and hold a Data Management & Services Review

Deliverables: [1] ALMA Archive Tool initial design documentation [2] ALMA Archive Tool prototype software [3] CASA pipeline software for ALMA Cycle 1 Early Science [4] Software for integrated VLA Scripted Pipeline [5] CASA pipeline software for ALMA Cycle 2 Early Science [6] CASA package, version 4.2 [7] CASA package, version 4.3 [8] CASA development package, version 4.4 [9] CASA VO support package [10] OPT software updates for Semester 2014A VLA observing [11] OPT software updates for Semester 2014B VLA observing [12] PHT software updates for Semester 2014A TAC meeting [13] PHT software updates for Semester 2014B TAC meeting [14] PST software updates for Semester 2014B Call for Proposals [15] PST software updates for Semester 2015A Call for Proposals [16] Reprocessing interface software [17] Dynamic Scheduling software [18] Quick-look improvements software in System Software Updates, Bundle 1 [19] Scan sequences software in System Software Updates, Bundle 1 [20] Improved correlator software in System Software, Bundle II [21] ALMA phasing project correlator software, ready for Phase V testing [22] Semester 2013B observing software [23] Semester 2014A commissioning software [24] Semester 2014A observing software [25] Semester 2014B commissioning software [26] VLA Full On-The-Fly Mosaic software [27] VLBA partial VME replacement software and hardware at one or more VLBA station(s) [28] Quasi-real time spacecraft tracking software [29] Wideband observing stabilization software [30] Software & documentation for GBT Archive [31] Software & documentation for core infrastructure changes [32] Software & documentation for M&C system modifications [33] Software & documentation for Astrid modifications and commissioning [34] Software & documentation for GBT imaging in CASA [35] Software & documentation for VEGAS support at highest data rates [36] Software & documentation for GBT Pipeline parallelization [37] Computer access policy documentation for external users [38] Services for early access to cluster resources [39] Grid/Cloud Middleware services [40] Prototype access services to non-NRAO computing cycles [41] Services for monitoring Internet 2 link performance [42] Remote link test procedures [43] Cluster characterization recommendations [44] 10 Gigabit/s link services to UVa Center [45] Improved storage services [46] 10 Gigabit network hardware services [47] Improved GB data access via 10 Gigabit network [48] Improved GB data access via conditional access to PSC Data Supercell [49] NRAO Data Management Plan [50] Data Management & Services Review Report and Response documents


6.3 Program Management Department The four primary areas of PMD responsibility are facilitating proposal development, ensuring best practices in management of projects/managing projects, development of program and grant documentation, and providing analytics for NRAO executive decision support.

• Proposal Development – Proposal development standards for NRAO – Proposal definition – Configuration control – Workflow management – Risk identification, assessment and mitigation

• Program/Project Management – Project/Systems engineering standards for NRAO – Project definition, planning, controls – Project performance and change management – Risk identification, assessment and mitigation – Proposal development standards and strategic alignment – Metrics, decision support & analysis – Systems Engineering

• Lifecycle analysis, architecture development, frameworks • Configuration Control • Document Management • Verification and validation • Quality Assurance • Modeling, simulation, analytics and visualization

• Observatory Documentation – Document requirements tracking – Compilation, development and editing for NSF and non-NSF grants

• Executive Analytics and Decision Support – Metrics compilation – Monthly assessments of performance – Quarterly assessments of performance – FTE oversubscriptions – Impacts to existing work/commitments

In FY14, PMD shifts from an initial implementation phase to operating, auditing, and optimizing. PMD will continue to provide qualified, formally trained and experienced program and project managers, and systems engineers. These individuals provide direct support to projects as requested by principal investigators and project leaders, and consulting support for all other projects or activities on an as requested basis. PM/SE processes, tools, templates, and techniques are also available to all NRAO staff. A Standard Operating Procedures (SOP) document for PMD will be developed and distributed as well. Formal training will be provided to PMD direct and dotted line staff to enhance their skills during a face-to-face meeting in Q1, FY14. PMD will continue to enhance its decision support capabilities. Analytics derived from systems used by PMD, such as Sharepoint and Project Insight, are used to ensure that prior to new work being undertaken, impacts to NRAO existing work are well understood and that any new work is aligned with NRAO’s strategic goals and objectives. PMD uses these tools to complete the various executive level


reports that are required and will continue to drive these systems to better performance in order to obtain better quality results. In collaboration with CIS, PMD will actively pursue a solution to the Sharepoint Browser incompatibility issue, which should resolve the inability to use a workflow in the tool. And working closely with Fiscal, MIS, and HR, obtain higher quality project charging information. In addition, PMD will assist the Budget department in developing a cost model for use on proposals to ensure a consistent, transparent approach. PMD will also develop and start implementing a cross-Observatory training program for broader NRAO on project management and systems engineering. PMD will work with HR to implement a process to capture staff participation in PMD training. And to publish a list of PM/SE courses to NRAO staff that can be taken to achieve an internationally recognized level of competence in these disciplines. This training may include high-quality video and web learning opportunities, as well as opportunities for PMD staff to obtain official certifications. Eight PMD cross-functional processes have been implemented and support these four primary areas of responsibility. During FY14, PMD will audit these processes for completeness and integrity, will look for optimization opportunities, and will provide training where necessary and appropriate.

• Proposal Development: three PMD processes support proposal development. o Workflow for New Idea o Workflow for Sponsored Research Support o Workflow for Component Pre-award

• Project Management: three PMD processes support Project Management Activities. o Workflow for Projects o Workflow for Sponsored Research Support o Workflow for Component Post-award

• Documentation: two PMD processes support Documentation Activities. o Workflow for Document Development o Workflow for Internal Project Prioritization

• Executive Analytics and Decision Support: three systems support executive analytics and decision support. o Sharepoint document library o Project Insight o NRAO Internal website/PMD

6.3.1 PMD Major Milestones

FY 2014

Program Project Q1 Q2 Q3 Q4 PMD Standards SOP Developed 1 PM Process audit and training Proposal Development Processes 2 Project Management 3 Documentation 4 Executive Analytics and Decision Support 5 PMD F2F Meeting Training and Process Reviews 6 Milestones: 1. PMD SOP Development complete 2. Audit complete – Proposal Development 3. Audit complete – Project Management 4, Audit complete – Documentation 5. Audit complete – Analytics and Decision Support 6. PMD F2F complete

Deliverables: [1.] SOP [2.] Audit outbrief and action items [3.] Audit outbrief and action items [4.] Audit outbrief and action items [5.] Audit outbrief and action items [6.] Training and Process Review complete


6.4 Education and Public Outreach Overview The observatory’s Education and Public Outreach (EPO) department provides major components of the public’s return-on-investment by (1) marshaling observatory resources in support of STEM (Science, Technology, Education, and Math) Education, and (2) informing the interested public about the observatory, its facilities, and the latest technical and scientific achievements of its staff and users. This dual mission is reflected in the department’s organizational structure and in the two main section headings that follow. The outward-facing nature of EPO means that some of our work is scheduled by us and some is driven by opportunities that arise spontaneously from both NRAO’s science users and EPO’s “customers.” We thus define our work in two categories:

• Continuous Level-of-Effort Programs: We prepare for a semi-predictable level of pressure for various forms of customer service based on experience. This includes newsworthy science results, requests for media visits, and school and other group visits.

• Planned Projects: These are defined projects that we undertake either at our own initiative or because they are mandated. Some projects come with deadlines that are tied to real world relevance – an article associated with an astronomical event that will happen on a certain date, for example. Other projects have evergreen value, and can be interrupted if a better opportunity for immediate impact presents itself; this increasingly happens as organizations with their own public/student user bases come to see NRAO as a valuable resource.

6.4.1 STEM Education National deficiencies and needs in STEM education are well-documented, as is the need to attract students to STEM careers. Efforts are underway on a national scale to address these issues, and it is a crucial component of NRAO’s commitment to the betterment of society to contribute to them on both local and national scales. For FY 2014, NRAO’s EPO department, with supplemental resources provided by NSF grant funds and AUI corporate funds, will focus on the following major STEM activity themes:

a) Providing authentic research experiences for learners and teachers b) Providing standards-aligned curriculum materials to STEM teachers nationally c) Developing a cadre of STEM role models and an associated integrated program to attract

students to STEM careers d) Providing stimulating informal learning opportunities for lifelong learners via our visitor

centers and community events These activity themes map well to STEM Education Investment Areas identified in the recently released five year Federal STEM Education Strategic Plan.


Continuous Level-of-Effort Programs NRAO will:

• Operate the Green Bank Science Center and VLA Visitor Center public exhibits and tours program. (Tours are ordinarily self-guided at the VLA, and have been recently enhanced via the installation of a new introductory film and new walking tour signage.)

• Provide special Green Bank tours to educational and tourist groups • Provide a minimum of four special community events in Green Bank, plus a regular schedule of

special scheduled activities (planetarium shows, lab tours, etc.) • Provide an Overnight Educational Field Trip program for schools, universities, and scouts in

Green Bank, featuring student-conducted research using the 40-Foot Telescope. • Provide local astronomy teaching resources (and training in their use), including the use of

StarLab portable planetariums, in NM and WV. • Provide professional development opportunities for teachers through the Chautauqua Short

Course program (subject to enrollment). • Provide a monthly series of public events at the VLA, featuring guided tours. • Provide an annual or bi-annual Open House event at the VLA, subject to the cooperation of the

Trinity site. Planned Projects Pulsar Search Collaboratory (PSC): NSF funding for this program, which empowers high school students to search for and discover pulsars in GBT data, has elapsed and not been renewed. The PSC will not cease to exist, however. During FY 2014 the following activities will be carried out: (a) in cooperation with West Virginia University (WVU), seek funding to continue and expand the PSC; (b) maintain the existing PSC website and offer online courses to PSC students and teachers via Skype; (c) organize and conduct a two-day PSC capstone event at WVU (subject to funding which we believe can be raised); organize and conduct a seven-day summer PSC workshop for new students and teachers (subject to funding which we believe can be raised). Skynet Jr. Scholars (SJS): NRAO is a partner with the University of North Carolina, Chapel Hill; The University of Chicago Yerkes’s Observatory, 4H Clubs, and the Astronomical Society of the Pacific in an NSF-funded program to develop educational activities in which 4H youth nationwide will conduct experiments and observations using Skynet robotic telescopes, one of which—and the only radio telescope—is NRAO’s recently refurbished and automated 40 Meter Telescope. During FY 2014 NRAO will lead the effort, via a series of workshops with professional educators, to develop and pilot-test the curriculum for SJS youth activities, as well as create a series of development workshops for 4H leaders. WV Governor’s School: NRAO Green Bank will, once again, host a cohort of rising 8th grade students for an intense, two week educational experience. VLA Visitor Center Improvements: During FY 2013 EPO purchased some display hardware for the VLA Visitor Center using EVLA construction funds. This year we will create an informative large-screen info-graphic display for the large screen, and an interactive “kiosk” version of the VLA Explorer Virtual Tour to populate that hardware and provide an enhanced visitor experience. Vision & Feasibility Workshop for new VLA Visitor Center: It is a long-term goal for NRAO to replace the current Visitor Center with a new, and much better facility. To that end, EPO will conduct


in October, 2013 a professionally facilitated workshop to develop a vision, assess feasibility of success, and generate a list of next steps. STEM Role Models Program: Attracting the next generation of science practitioners involves more than just helping students succeed in their STEM-related classes. Exposure to role models, the work they do, and the rich environments in which they function, can give students, who are wondering just what it is that they’re going to be, a model to emulate. NRAO has scientists, engineers, and technicians who are naturals for interacting with kids, but they’re also busy, and asking them to develop their own presentations can be daunting. EPO will develop a pilot program to get great STEM role models in front of impressionable students. This will be an integrated program involving background media, live and internet-based appearances, and participation in several STEM career development days sponsored by community organizations in Charlottesville, all designed to minimize the barrier to participation by our staff volunteers, and maximize the impact for the students. If successful, this model could be propagated from NRAO to other FFRDCs. A related pilot program to train West Virginia undergraduate students to become STEM presenters to younger-age students, will be undertaken in Green Bank, subject to anticipated funding from the WV Space Grant Consortium. ALMA Operations Online Interactive Role Playing Game: Most of NRAO’s EPO effort pertains to our science and technology, but the technology only delivers the science if the telescopes are well managed, with appropriate choices made about how much time to invest (and when) in observing vs. repair and maintenance. Getting the most science output from a telescope is the name of the game, and speaking of games, middle school kids love them. In collaboration with a contracted outside educational game developer, and in consultation with NRAO’s experts in ALMA operations, we will continue work begun late in FY 2013 to develop an online role playing game in which players will be challenged to make real-time choices that determine the scientific success of the telescope. 6.4.2 News and Public Information NRAO operates four telescopes, each of which are the best of their kind in the world. So naturally, scientists use them to make a lot of interesting discoveries. Conveying those discoveries, and the technical and scientific contexts in which they occur, is the task of our News and Public Information team. Continuous Level-of-Effort Programs Social Media Engagement: Today’s young audiences are not only more tolerant of a higher level of “background noise” than their predecessors, they actually thrive in high-noise environment, seeking immersion in continuous streams of informative tidbits, and comfortable with extracting what they wish, commenting where they desire, and synthesizing their own ultimate understandings. Via social media (principally Facebook and Twitter, plus Youtube and Vimeo where video is involved, but also via other channels as time allows), NRAO is enjoying impressive, continuous audience growth. The key is continuous postings; we will continue to research and post material from the profound and informative to the downright quirky, nearly every business day (and many holidays). Public Website Maintenance, User Support, and Improvements: It is simply an ongoing effort to maintain a website such as public.nrao.edu. Not only is more material being posted all the time, but new browser releases and new software releases are forever inducing unanticipated changes to how pages render. In addition, users suggest new ways to make existing content more accessible (for


example, via enriched metatags and searching capabilities); we will implement good suggestions as resources permit. Public Inquiry Response: NRAO receives hundreds of public inquiries every year. We allocate staff resources to answer them, and will in FY 2013 develop an enhanced mechanism for tracking inquiries to make sure they are routed to the appropriate party for answer, and that they are responded to. Press Release Development, Distribution, and Monitoring: The ‘press release’ or ‘news release’ is the way we generally announce our most newsworthy science results to the public. In hopeful anticipation of a bumper crop of interesting results from our newest telescopes, we are allocating sufficient PIO (Public Information Officer) resources to handle as many as 30 press releases in FY 2014. Since releases are more effective when accompanied by an image, and even more so when accompanied by a video, we will allocate significant resources from the EPO media team to create images and videos to accompany press releases. We will enhance our press release distribution via a select email list and via the Newswise wire service; we will enhance our ability to monitor and report impact by use of the Ciscion press reporting service. News Tip Development, Distribution, and Monitoring: An NRAO News Tip is generally a short (~300 word) story about a topic that falls below the threshold of significance for a press release, but which is yet of interest to certain members of the journalism community. Typical topics include superlative, record-setting observations, achievement of milestones, and receipt of funding awards. We generally bundle two or three tips into a “tipsheet” before sending out. We will produce at minimum one tipsheet per quarter. Media Inquiry and Request Response: NRAO receives many requests annually for support from the media, from recommendations for a picture to accompanying a broadcast crew to ALMA. Sufficient PIO resources will be allocated to respond to predicted demand. Planned Projects NRAO Homepage Re-Design and Re-Program: With science.nrao.edu the site for users and public.nrao.edu the site for the public, the nrao.edu home page will be redesigned as a portal to those other domains, also providing access to places where visitors may wish to conduct business, such as HR. “What NRAO Telescopes Are Observing; smartphone app, website display, and NRAO lobby display: Recommended by several successive User Committees, this project, to begin in FY 2014 and conclude in FY 2015, will entail establishing webcams at the VLA and GBT, tapping into databases of telescope observing schedules, writing interpretive content to explain approved science programs, displaying accurate information in real time, learning the Objective C language for iOS app development and/or appropriate languages for Android device development, and designing a legacy compilation display so that the accumulating value of NRAO observations can be appreciated. During FY 2014 we will get the webcams and website/lobby displays working; the smartphone app will be developed in 2015, subject to planning priorities identified for that year. ALMA Info-graphics/Edu-graphics: Per efforts to support a TEDx talk on ALMA, EPO will refine and post a collection of graphics for use by NRAO/NSF/AUI staff and science users giving public presentations about ALMA.


NRAO Display for Virginia Air and Space Center Museum, Hampton, Virginia: This museum has dedicated a wall in their astronomy gallery for NRAO. We will design and fabricate a 4x8 ft. exhibit panel, and also provide a video screen with looping NRAO videos. NRAO Public Brochure: We will produce a new, public-level brochure that summarizes NRAO. VLA Booklet: We will produce a new booklet about the VLA, for sale in the VLA Visitor Center gift shop, but also available online. Milky Way Explorer for public website: We will produce a new online virtual tour of the Milky Way that features "tour stops" where particular contributions of radio astronomy to our understanding of the Galaxy and Local Group are displayed and explained. Just in time for the G2 Cloud encounter with the black hole at the galaxy’s core. This will be produced in consultation with our STEM team for possible additional use in education, and will be mapped to the Next Generation Science Standards. 6.4.3 EPO Major Milestones

FY 2014


News & Public Information

NRAO Homepage Re-Design & Re-Program + “Main Site” Cleanup and Archive 1 2 3

“What NRAO Telescopes are Observing” NRAO Lobby Display (note: this project is a prerequisite to developing smartphone app in FY15

4, 5, 6

Milky Way Explorer for NRAO Public Website 7 8

STEM Education

Skynet Jr. Scholars (grant funded program) 9 10 11

WV Governor’s School 12 Educational Annotation of Existing NRAO EPO Assets 13 14

Milestones: 1. Specify, Develop, and Review Design 2. Program, implement design, test, correct, migrate

to live server. 3. Archive and houseclean deprecated web content 4. Define and specify project. Design digital signage

display 5. Programming and graphical implementation 6. Procure digital signage software system, program

digital signage display, publish to network 7. Design and specify project. Develop design. 8. Produce scripts, narrations, graphics, videos,

program and implement 9. Conduct online course for first cohort of Skynet Jr.

Scholars educators 10. Skynet science and education workshop II 11. Educational Module Set II Development workshop 12. Conduct Governor’s School Program in GB 13. Review existing inventory of assets and annotate in

accordance with appropriate STEM-related teaching standards

14. Create thematic STEM assets database/catalog/clusters and publish to NRAO public website

Deliverables: [1] Design document for new homepage [2] Functioning new NRAO home page [3] Reduced “clutter” on www.nrao.edu server [4] Design document for new display [5] Functioning automated scripts that harvest data from various telescope operational databases, feeding necessary information to EPO database from which the digital signage display will draw [6] Scala Infochannel software system up and running, lobby display up and running [7] Design document and script for Milky Way Explorer [8] Produced media elements for Milky Way Explorer, implemented and running. [9] Educators trained in use of Skynet Jr. Scholars-developed educational materials [10] Scientists edit module set one for scientific accuracy, develop outlines for module set II, provide feedback on telescope interfaces and image processing tools. [11] Second set of Skynet Educational modules development underway [12] WV Governor School program completed. [13] Document showing annotated assets. [14] Online catalog available

http://www.nrao.edu/


6.5 Administration The Observatory Administration Services department provides administrative management, human resources management and non-programmatic services to NRAO and ALMA. Administration activities are headquartered in Charlottesville in Stone Hall on Edgemont Road (ER) at the University of Virginia. Other administrative offices are at the Central Development Lab (CDL) on Ivy Road; in Green Bank in the Jansky Building; and in Socorro in the Domenici Science Operations Center (DSOC). 6.5.1 Business Services Succession Planning: The Associate Director of Administration will solicit and review recommendations from Observatory Administrative Services division heads for how their division would best be managed in their absence. Lease Negotiations: Two VLBA sites are currently undergoing lease renegotiations. Owens Valley expired 5/2013 and is being negotiated by Cal Tech with the LA water authority that owns the land. St. Croix expires 3/31/2014. NRAO is actively working this with an end goal of January. 6.5.2 Contracts and Procurement Export Management: As a follow-through to the approved Export Management & Compliance Program Manual, the following actions will be accomplished:

• create a process to label controlled items identified at NRAO sites as either “ITAR Controlled” or “EAR Controlled,” and include both the ECCN number and Schedule B number on said label;

• Develop on-line training presentation for new employees and post on NRAO web site; • Develop process to insure that either the terms “ITAR Controlled” or “EAR controlled” are

clearly shown on the outside of all export packages. Grants Management: Develop a Grants Lifecycle training program (from submission to award to closeout) for all Principal Investigators (PI’s) to enhance NRAO compliance with contracting policies. 6.5.3 Environmental, Safety & Security Safety Training: Develop a comprehensive safety training plan that catalogues all available training sessions, required frequencies will be identified, and the training program then published into an annual calendar for planning and scheduling. Work Order System: Develop a safety work order system to track and export on the progress of implementation of corrective safety actions. Safety Policy: Develop a physical security policy for personnel safety. 6.5.4 Management Information Systems Indirect Cost Allocation: Implement new Indirect Cost Allocation system. Based upon revised calculation method, program the distribution of overhead/indirect costs to the funding sources. Software upgrades: Upgrade of J.D. Edwards to tools release 9.1.3. Upgrade J.D. Edwards tools


operating system that will allow for enhanced and future capabilities with the web and portal interfaces. This will additionally keep the AUI/NRAO J.D. Edwards tools release software on a more current, up-to-date version. Automated Performance Evaluation Plan (PEP) Process: This item is a joint effort of MIS and HR to investigate and implement a replacement to the current paper form evaluation. A system has been identified through an RFP and implementation will begin in Q1 2014. 6.5.5 Technology Transfer Office Cooperative Research Agreements: Form at least one cooperative research agreement (CRADA with industry. 6.5.6 Administration Major Milestones

FY 2014

Program Project Q1 Q2 Q3 Q4 Business Services Succession planning documentation for OAS divisions 1

CAP

Create a process to label controlled items as “ITAR Controlled” or “EAR Controlled” 2

Develop on-line Export Compliance training 3 Develop labeling for “ITAR Controlled” and “EAR Controlled” shipments. 4

Develop Grants Lifecycle training program 5

ES&S Develop a comprehensive safety training plan 6 Develop a safety work order system 7 Develop a security policy 8

MIS

Implementation of new cost allocation system. 9 Upgrade of J.D. Edwards to tools release 9.1.x 10 Investigation and implementation of automated Personnel Evaluation Process (PEP) system 11

TTO Form at least one Cooperative Research Agreement with industry. 12

Milestones: 1. Succession planning 2. Create labeling process for ITAR and EAR controlled items 3. Develop on-line Export Compliance training 4. Develop labeling for ITAR and EAR controlled shipments 5. Develop Grant Lifecycle training program 6. Develop a comprehensive safety training plan 7. Develop a safety work order system 8. Develop a security policy 9. Implementation of a new cost allocation system 10. Upgrade J.D. Edwards to tools release 9.1.3 11. Investigation and Implementation of automated Performance

Evaluation Process. 12. Form at least one Cooperative Research Agreement (CRADA)

with industry.

Deliverables: [1] Succession planning document prepared [2] ITAR and EAR controlled items identified and labeled [3] Export Compliance training loaded on NRAO Intranet and availability announced. [4] Labels and labeling procedures in place [5] Grant Lifecycle training program delivered to al l PIs [6] Comprehensive Safety Training plan [7] Safety work order system installed [8] Security policy written and disseminated [9] New cost allocation system tested and loaded in MIS [10] J.D. Edwards upgrades [11] Automated Personnel Evaluation Process [12] CRADA in place and active.


6.6 Human Resources Human Resources support the HR needs of NRAO’s domestic and international (ISM) staff. HR staff are stationed in Charlottesville, VA (5.75 FTE), Green Bank (1 FTE) and Socorro (2 FTE). There are eight core areas of responsibility for NRAO’s Human Resources Department that are allocated among the staff: Compensation, Diversity, Employment, Employee Relations, HRIS, Training, and support of AUI benefits for NRAO staff. 6.6.1 Human Resources Major Milestones Human Resources have five major initiatives planned for FY 2014 and supports major milestones identified in Section 6.7 (Diversity).

FY 2014


Compensation Electronic PEP Process 1 Salary Review Process 2

Policy NRAO HR Policies 3 Training Management Training 4 Employment Applicant Tracking System 5 Milestones: 1. Complete the FY 2013 performance review process

on time using a new performance software system. 2. Provide managers with the information and guidance

to complete the FY 2014 Salary Review Process. 3. Complete update and consolidation of NRAO HR

policies. 4. Develop new management training courses. 5. Review the feasibility of replacing the existing

applicant tracking system (PeopleAdmin) thru the use of an add-on tracking module to the performance management system.

Deliverables: [1] Transition all performance evaluations from the paper PEP forms to the electronic performance management system. [2] Complete the FY 2014 Salary Review process on time and within budget. [3] Consolidated HR Policies document approved by NRAO and AUI management. [4] Deliver two new courses to NRAO managers and supervisors. [5] Complete transition to new applicant tracking system, if decision to change is made.


6.7 Diversity NRAO has developed a comprehensive Diversity Strategic Plan that will provide specific guidance on diversity initiatives across the Observatory. Diversity efforts across the Observatory for FY 2014 will focus on the following key areas; broader impact, new/on-going pipeline initiatives, workforce hiring (process and policies), retention, training, workplace culture. Continued integration of programs within and amongst Science Support and EPO will enable us to leverage existing talent and coordinate existing resources. The need to effectively communicate and actively engage and encourage increased participation in diversity efforts at the sites will be a key goal in ensuring that the diversity milestones are met. Management will have a key role in ensuring that diversity and broadening participation is encouraged at all levels. 6.7.1 Diversity Major Milestones

FY 2014


Communication Develop new strategies to increase participation in broader impact and diversity efforts at all sites, at all levels.

1

New Initiatives Diversity Review Panel Report 2 Training Observatory Wide Diversity Training 3 International Outreach Building Bridges to South Africa, China, and Chile 4

Domestic Outreach

Howard University, Hampton University, University of Maryland, BC. 5

Employment Implement Recruitment Guidelines 6 Milestones: 1. Clarify and communicate the Diversity Mission. 2. Develop action plan for Diversity Review Panel report. 3. Continue diversity training – cultural workplace topics, gender, ADA, Veterans, etc. 4. Continue to build International relationships to create pipeline for next generation of scientists and engineers. Investigate alternative funding streams to sustain partnerships. 5. Continue domestic outreach partnerships to maintain pipeline. Partner with EPO and SSR to maximize existing programs and funding. 6. Implement recruitment guide and provide training that focuses on diversity focus.

Deliverables: [1] Communication from Director’s Office to all staff stating that diversity is critical to NRAO’s future. Buy-in and participation in diversity efforts is a shared responsibility. Increased engagement and participation is an expectation. Establish clear expectations, with accountability and training. Diversity goals incorporated into manager’s performance review. Establish mechanism to charge diversity/broader impact activities. [2] Implement FY 2014 initiatives identified in the 2013 Diversity Review Panel report. [3] Conduct quarterly diversity training at all sites [4] Create solid partnerships with the faculty at the Universities, create student cohorts, joint collaborations, and conduct workshops. NRAO to host Post Doc/students. [5] Continue partnership with Howard University. Establish metrics. Cultivate partnership with Hampton University for pipeline opportunities. [6] Disseminate recruitment guide to hiring managers and provide diversity training to search committee members. Create and monitor diversity recruitment metrics.


6.8 Computing & Information Services Overview Computing and Information Services (CIS) staff has been successfully matrixed into the new DMS Department during FY 2013. This has enabled transparent sharing of highly skilled Information Services resources to be available for both telescope supporting science responsibilities (tracked under DMS), as well as general staff IT support duties (CIS). CIS is responsible for:

• Staff Helpdesk (tracking Service and Change Requests as well as Incidents) • Documented Service Catalog (https://inside.nrao.edu/computing) • Support for Desktop platforms (Windows, Mac, and Unix) • Client services: E-mail, browser, 3rd party productivity/engineering applications • Standard core services such as E-mail/printing/file sharing/backups • Commodity data networks (Intranet, Internet, secure VPN) • NRAO Phone/voicemail systems • Video-conference systems (room and desktop) • Meeting room and NRAO science event audio/visual support • Mobile, satellite and smartphone services • Licensing, maintenance, and support for commercial software • Maintenance contracts for computer/communication hardware • Web platform stability to support content and software development • Collaboration solutions (wiki, Plone, WebEx) • Audio/Visual for key NRAO sponsored events • Monitoring and alerting of key services • Coordinating Add/Move/Change requests for staff and visitors • Staff login account management • Staff training (onboarding, documentation and annual security update) • IT Audit compliance, in conjunction with MIS

As part of the observatory-wide alignment of CIS resources, a unified staff helpdesk will be implemented in Q2 FY 2014 with simplified priority scheme (4 instead of 100 levels) and intuitive Urgency (time) vs. Impact (scope) mapping. Clear Service Level Objectives for request response and resolution will be consistently adopted between sites, with transparent and communicated Change Control and Root Cause investigation. CIS is focused on supporting OAS operations by leveraging the structure of the Common Computing Environment (CCE) to ensure that all standard NRAO computers have a common system image and that the expertise available for supporting servers is also leveraged for desktop and laptop systems to ensure a consistent end-point security model and user experience. This consistency of oversight extends from hardware to software and on to supported applications and training. This oversight includes planning, policy, standards (for software, hardware, and system administration), computer security, allocation of the CIS budget, computer staff training, inter-site computing-related travel, procurements, and ongoing maintenance contracts. CIS also manages the telecommunications infrastructure (voice, video, data and mobile communications) within the observatory. In addition, CIS


covers the cost of upgrading Computing Infrastructure for desktop and servers as well as printers and the storage systems. The following sections outline the activities and milestones coordinated by CIS, to ensure an optimum computing, storage, and communications environment for staff and users of NRAO telescopes as well as providing agile service support for an active research and development program. 6.8.1 Common Computing Environments The CCE coordinates and prioritize NRAO-wide computing projects and initiatives between the sites, facilitated by the annual system-administrators meeting and staff skills improvement via computing conferences and training events. A major objective for FY 2014 is the work to implement computer inventory and patch management solutions for all platforms: Windows (System Center), Macintosh (Munki) and Red Hat Linux (Kickstart/Puppet) with reliable testing and release management practices. The experience gained from the shift to site centralized HPC solutions for both storage and computing will be shared throughout the observatory through Data Management and Science Software divisions and deployed within the standard CCE framework. Leveraging the insight from this, CIS will evaluate these storage devices with open source Network Attached Storage (NAS) software in Q3 for business needs to replace the current proprietary and expensive NAS solutions used for user storage. 6.8.2 Communications and Network The final fiber segment build for the 10Gigabit/sec link to the Green Bank site will be available by Q1 FY 2014 with substantial effort required to ensure secure, transparent and reliable access service is provided at this revolutionary speed. Particular focus will be given to key GBT projects such as NANOGrav via SIS with stable service in Q2. In order to better support staff directory information and access, the legacy LDAP service will be retired and Active Directory will be leveraged for authentication and contact information in Q1. As the importance of international partnerships and the cost of travel continue to increase, NRAO will be investing in a desktop collaboration and on-line training solutions, with a new solution being evaluated in Q1 FY 2014, and released throughout the year as acceptance grows. 6.8.3 Computing Security CIS will continue to shift to emphasize a holistic risk management strategy in which the users of NRAO computing resources are educated and engaged in the mitigation of cyber-attacks and malicious targeting particularly when on travel. These attack vectors increasingly depend on social engineering vulnerabilities with risks mitigated through a manifold of prompt patch management, user education, bulletins and proactive engagement of staff. To mitigate the risk of malicious network activity over increasingly high capacity links, the Bro Network Security Monitoring solution will also be evaluated in FY 2014, with a sustained effort on “securing the human” with multi-tier staff training enforced. 6.8.4 Site Specific Facilities Infrastructure With the advent of increased visibility of service at the Charlottesville location in support of the NAASC and Observatory-wide services, a natural gas generator will be installed in support of the Edgemont


Road computer room for x10 improved reliability and availability in Q1 FY 2014. Work will be carried out in FY 2014 on standardization of physical access key-card systems to replace the legacy solution in Socorro (currently requires manual unlocking during workday), aligning it with the policy-based card technology used at the other sites. 6.8.5 CIS Major Milestones

FY 2014


CIS

Unified Staff Helpdesk 1 Standardize inventory and Patch management solutions 2

Evaluation of NAS with open source option 3 GBT network 4 Consolidation of Staff Directory Service 5 Collaboration solution 6 7 Security training and Network Monitoring evaluation 8 9

Reliable power for Edgemont Road 10 Installation of Archive systems in UVa data center 11 Swipe Card access for Socorro 12

Milestones: 1. Installation of staff Helpdesk solution 2. Standardization of platform patch solutions 3. Evaluate Open Source NAS 4. Installation of 10Gbps network equipment 5. Retirement of leagacy LDAP 6. Evaluation of interactive Web collaboration tool 7. Installation and training for collaboration tool 8. Evaluation of Bro tool 9. Update to staff security training curriculum 10. Specification and installation of ER generator 11. Installation of archive servers in UVa Data Center 12. Prox-card solution for Socorro doors

Deliverables: [1] Unified staff helpdesk service [2] Aligned OS and software update service [3] Design proposal for general user network storage [4] High speed science network solution for GB [5] Single directory service for NRAO staff information [6] Implementation plan for collaboration tool [7] Widespread (~40) adoption of collaboration service [8] Network security monitoring service with alerts [9] In-person and online mandatory security training [10] Power availability at 99.9% level for ER [11] Colocation service for public archive data in UVa [12] Standard key-card solution at all major sites


6.9 Director’s Office Overview The FY 2014 program operating plan and milestones for the NRAO Communications Office (6.9.1), New Initiatives Office (6.9.2), and the National and International Spectrum Management Office (6.9.3) follow. The NRAO staff member who leads each of these offices reports to the NRAO Director. 6.9.1 Communications The Communications Office (COM) collaborates with scientific staff and the Director’s Office to communicate NRAO science, vision, accomplishments, and plans to the science community, NRAO/AUI staff, and key external stakeholders, including NRAO advisory committees, the NSF, and the U.S. Congress. COM will collaborate with scientific staff and the Director’s Office to organize an effective Observatory presence at major FY 2014 science community meetings, including the 5-9 January 2014 and 1-5 June 2014 AAS meetings in National Harbor, MD and Boston, MA, respectively. A COM proposal for an NRAO Town Hall has been accepted for the January 2014 AAS meeting, and a proposal is pending for a Workshop at the January AAS to communicate and discuss a NRAO VLA Sky Survey (VLASS) initiative that will explore the science and technical opportunities of a new centimeter-wavelength survey. At least one Splinter Session designed to assist the community with NRAO proposal and observing preparation will be proposed for the winter and summer AAS meetings. COM plans to redesign the NRAO exhibit for the January 2014 AAS. To help communicate NRAO science to the broader scientific community, two science symposia proposals were submitted by COM in April 2013 for the 2014 AAAS Annual Meeting (13-17 February 2014, Chicago). Both proposals were peer-reviewed and accepted. A symposium titled From Dust and Gas to Disks and Planets will feature six speakers who will explore how the new generation of radio telescopes is revolutionizing our understanding of protoplanetary disk and planet formation. A symposium titled New Millimeter-wavelength Insights into Galaxy Evolution in the Early Universe will feature three speakers who will describe recent progress in the study of galaxy kinematics, structure, and evolution in the early Universe that has been enabled by ALMA, Jansky VLA, and the South Polar Telescope. COM and CIS will organize an NRAO exhibition and technical presence at the International Conference for High Performance Computer Networking, Storage, and Analysis (SC13) that will be held 17-22 November 2013 in Denver, CO. COM will design and publish a 2013 NRAO Annual Report in FY 2014. This Report will feature 2013 science highlights from the community and NRAO scientific staff; major accomplishments at NRAO operational facilities; construction project status; R&D progress for next-generation facilities; community support activities; and public outreach and diversity highlights. This Report will be widely distributed to observatories and universities in the U.S. and abroad, as well as NSF and the U.S. Congress. In collaboration with the SSR team and scientific staff across the Observatory, COM will continue to design, manage, and improve the high-level content of the NRAO science web site in FY 2014. COM will also continue to edit, improve, publish, and expand the subscription base for the Observatory’s monthly


electronic newsletter, NRAO eNews, and the periodic electronic announcements series, NRAO Announcements, which enter FY 2014 with 6,000+ subscribers in North American and around the world. Improving internal communication will continue to be a priority. COM will continue to work with the management team to develop and implement more effective, timely, and accurate communication across the Observatory. Content and tools for the NRAO Intranet will be further developed to improve internal communication. 6.9.2 New Initiatives Strategic Mission: The NIO pursues, develops, and manages strategic partnerships and collaborations with academic, government, and non-profit organizations. Among the core NIO activities envisioned for FY 2014 are to continue managing and further expanding the partnerships to sustain the scientific operations and unique technical capabilities of the VLBA and GBT. 6.9.3 Spectrum Management The NRAO participates heavily in spectrum management in order to protect and improve observing conditions for all astronomers and has done so since its inception. Domestic Activities: The NRAO monitors FCC actions and is the most frequent commenter during the public processes that unfold when the Commission proposes and implements new rules regarding use of the radio spectrum. Much attention now is on reorganization of the TV broadcast bands below 700 MHz, with ramifications for the channel 37 radio astronomy band at 608-614 MHz. NRAO also interacts with domestic commercial interests, for instance an upcoming round of negotiations with Iridium, LLC to ensure that operation of their next generation of satellites adequately protects observations of the 1612 MHz OH maser line. NRAO liaises with NSF Electromagnetic Spectrum Management at monthly telephone meetings and attends annual meetings of the National Academy of Sciences Committee on Radio Frequencies (CORF). NRAO staff members serve as CORF members and consultants. International Activities: On behalf of radio astronomy, and in the belief that success in these activities will flow back to their own countries, the NRAO and a few other major observatories promote an international agenda that is coordinated at bi-yearly ITU-R sessions in Geneva and at triennial URSI, IAU and COSPAR General Assemblies. ITU-R issues of importance to radio astronomy now being studied in preparation for the 2015 World Radio Conference include: 76 – 81 GHz car radars; allocations of new spectrum for pilotless drone flight in commercial airspace; prospective allocations to satellite-phones for broadband use; and possible world-wide designation of bands for increased allocations to broadband cell phone use, among others. The current NRAO Spectrum Manager is the vice-chair of IUCAF, an international committee funded by IAU, URSI and COSPAR that works to coordinate radio astronomy spectrum management activities world-wide. ALMA: The NRAO spectrum manager informally represents ALMA interests abroad and liaises with the ALMA JAO and with SUBTEL, the Chilean national telecommunications authority that administers the radio quiet and coordination zones that it created around the ALMA core. The NRAO Spectrum Manager is also working toward implementation of self-sustaining spectrum management activities within the ALMA operations plan.


6.9.4 Director’s Office Major Milestones

FY 2014


Communications Annual Report 1 Exhibit Design 2 Science Symposium Proposals 3

Milestones: 1. Publish NRAO 2013 Annual Report 2. Complete NRAO exhibit re-design for January 2014 American Astronomical Society meeting 3. Submit science symposium proposal(s) for 2015 American Association for the Advancement of Science Annual Meeting

Deliverables: [1] 2013 NRAO Annual Report document, hardcopy and on-line. [2] NRAO exhibit for major science meetings. [3] Science symposium proposal(s).


6.10 Observatory-wide Services Financial/FTE Projections

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*

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en0

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0.00

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1420

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ifica

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0.00

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0.00

00.

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0.00

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0.00

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0.00

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*

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& E

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0.00

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*

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000

0.00

00.

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0.00

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4.65

00.

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00.

000

0.00

00.

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nce

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rati

ons

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091

3.95

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ific

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r Se

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1,47

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112

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4,41

317

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1,70

4,98

611

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00.

000

0.00

3,99

9,39

928

.55

3620

Scie

nce

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a Pr

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*34

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0.00

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000

0.00

1,18

1,55

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3621

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a Pr

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8,83

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00.

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6,06

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2,81

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421

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0.00

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ent

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Observatory-wide Services Financial/FTE Projections (Part 2 of 2)

WB

SE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

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xpen

ses

FTE

'sE

xpen

ses

FTE

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xpen

ses

FTE

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ses

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ses

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dmin

istr

ativ

e Se

rvic

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000

0.00

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000

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ness

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000

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mun

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ities

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5,95

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00

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tral

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0.00

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0.00

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)*

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ms

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ce H

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0.00

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00(1

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548)

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000

0.00

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0.00

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00.

000

0.00

00.

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*

4500

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agem

ent

00.

000

0.00

00.

000

0.00

486,

381

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1*

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ead

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1,49

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mun

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ions

00.

000

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00.

000

0.00

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6,01

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00.

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6,20

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trat

ion

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0.00

00.

000

0.00

00.

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0.00

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3.75

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and

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nd T

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49.7

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93.5

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73

* n<

3

GR

AN

D T

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al, C

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tory

Cen

tral

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rvic

esC

SA-1

NR

AO

Ops

GB

TE

VLA

VLB

AC

DL

Non

-Tel

esco

pe


APPENDIX A: PRELIMINARY FINANCIAL PLAN & WORK BREAKDOWN STRUCTURE

Table 1: Observatory Financial/ FTE Projection by Site (Part 1 of 3)

WB

SE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

's10

00T

eles

cope

Ope

rati

ons

55,0

34*

5,99

4,00

216

.60

68,1

57*

00.

000

0.00

6,11

7,19

317

.36

1100

Mai

nten

ance

00.

001,

748,

234

9.55

00.

000

0.00

00.

001,

748,

234

9.55

1200

Ope

ratio

ns55

,034

*3,

375,

768

6.55

00.

000

0.00

00.

003,

430,

802

6.98

1300

Spec

trum

Man

agem

ent

00.

000

0.00

68,1

57*

00.

000

0.00

68,1

57*

1400

Infr

astr

uctu

re M

ods

& U

pgra

des

00.

0087

0,00

00.

000

0.00

00.

000

0.00

870,

000

0.00

1500

Man

agem

ent

00.

000

*0

0.00

00.

000

0.00

0*

2000

Dev

elop

men

t P

rogr

ams

2,11

9,38

025

.68

5,02

8,84

55.

6598

8,51

44.

200

0.00

00.

008,

136,

739

35.5

321

00Bu

sine

ss D

evel

opm

ent

00.

000

0.00

704,

023

3.30

00.

000

0.00

704,

023

3.30

2200

Tec

hnol

ogy

Dev

elop

men

t1,

553,

258

21.5

64,

866,

860

5.15

00.

000

0.00

00.

006,

420,

117

26.7

1

2300

R&

D S

uppo

rt38

7,51

94.

130

0.00

00.

000

0.00

00.

0038

7,51

94.

13

2400

Soft

war

e D

evel

opm

ent

00.

000

0.00

00.

000

0.00

00.

000

0.00

2500

Man

agem

ent

178,

603

0.00

161,

985

*28

4,49

2*

00.

000

0.00

625,

080

*

3000

Scie

nce

Ope

rati

ons

1,50

4,23

511

.85

4,78

8,25

530

.92

1,38

4,71

07.

6740

,000

0.00

182,

404

0.00

7,89

9,60

350

.43

3100

Obs

erva

tory

Tim

e A

lloca

tion

59,3

87*

00.

000

0.00

00.

000

0.00

59,3

87*

3200

Ref

eren

ce12

0,00

00.

0055

,081

0.00

496,

168

*0

0.00

00.

0067

1,24

9*

3300

Broa

der

Impa

cts

475,

355

3.60

772,

941

*0

0.00

00.

0018

2,40

40.

001,

430,

700

3.90

3400

Scie

ntifi

c St

aff

187,

340

3.00

336,

232

4.00

00.

0040

,000

0.00

00.

0056

3,57

27.

00

3600

Scie

ntifi

c U

ser

Serv

ices

662,

152

4.75

3,05

1,85

724

.17

00.

000

0.00

00.

003,

714,

009

28.9

1

3500

Man

agem

ent

00.

0057

2,14

4*

888,

542

4.87

00.

000

0.00

1,46

0,68

67.

32

4000

Adm

inis

trat

ive

Serv

ices

11,0

59,1

50*

3,53

9,23

2*

(7,6

82,6

91)

26.0

60

0.00

00.

006,

915,

692

27.8

141

00Bu

sine

ss S

ervi

ces

295,

096

*45

,065

*4,

046,

699

25.0

60

0.00

00.

004,

386,

861

26.8

1

4200

Faci

litie

s0

0.00

00.

002,

480,

463

*0

0.00

00.

002,

480,

463

*

4300

Aux

iliar

ies

00.

000

0.00

00.

000

0.00

00.

000

0.00

4500

Man

agem

ent

78,9

540.

000

0.00

00.

000

0.00

00.

0078

,954

0.00

4800

NR

AO

Ove

rhea

d10

,685

,100

0.00

3,49

4,16

70.

00(1

4,20

9,85

3)0.

000

0.00

00.

00(3

0,58

6)0.

00

5000

Dir

ecto

r's

Off

ice

2,90

3,16

83.

062,

901,

004

5.70

1,66

0,28

58.

270

0.00

6,79

60.

007,

471,

253

17.0

351

00Pr

ogra

m M

anag

emen

t0

0.00

00.

0044

5,05

03.

500

0.00

00.

0044

5,05

03.

50

5200

Publ

ic O

utre

ach

364,

977

*66

9,56

54.

800

0.00

00.

000

0.00

1,03

4,54

27.

03

5300

Com

mun

icat

ions

198,

191

*24

1,99

5*

126,

014

*0

0.00

00.

0056

6,20

0*

5500

Adm

inis

trat

ion

00.

000

0.00

1,08

9,22

13.

750

0.00

00.

001,

089,

221

3.75

5800

AU

I Fee

and

IDC

2,34

0,00

00.

001,

989,

444

0.00

00.

000

0.00

6,79

60.

004,

336,

240

0.00

Gra

nd T

otal

17,6

40,9

6642

.07

22,2

51,3

3759

.57

(3,5

81,0

24)

46.5

340

,000

0.00

189,

200

0.00

36,5

40,4

8014

8.17

CSA

-1 N

RA

O O

psC

SA-2

ALM

A O

psO

bser

vato

ry C

entr

al

Serv

ices

Sola

r B

urst

CSA

-4 R

EU

RIT

Tot

al, C

harl

otte

svill

e

* n<

3 FT

E

Cha

rlot

tesv

ille


Observatory Financial/ FTE Projection by Site (Part 2 of 3)

WB

SE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

's10

00T

eles

cope

Ope

rati

ons

16,6

75,3

177.

004,

974,

181

44.7

60

0.00

446,

673

3.94

00.

005,

420,

854

48.7

011

00M

aint

enan

ce0

0.00

1,14

7,48

25.

700

0.00

00.

000

0.00

1,14

7,48

25.

70

1200

Ope

ratio

ns43

1,54

2*

2,93

8,40

933

.24

00.

000

0.00

00.

002,

938,

409

33.2

4

1300

Spec

trum

Man

agem

ent

00.

0015

,336

*0

0.00

446,

673

3.94

00.

0046

2,00

94.

09

1400

Infr

astr

uctu

re M

ods

& U

pgra

des

00.

0047

,922

0.00

00.

000

0.00

00.

0047

,922

0.00

1500

Man

agem

ent

16,2

43,7

756.

0082

5,03

35.

670

0.00

00.

000

0.00

825,

033

5.67

2000

Dev

elop

men

t P

rogr

ams

00.

000

0.00

00.

000

0.00

750,

000

*75

0,00

0*

2100

Busi

ness

Dev

elop

men

t0

0.00

00.

000

0.00

00.

000

0.00

00.

00

2200

Tec

hnol

ogy

Dev

elop

men

t0

0.00

00.

000

0.00

00.

0075

0,00

0*

750,

000

*

2300

R&

D S

uppo

rt0

0.00

00.

000

0.00

00.

000

0.00

00.

00

2400

Soft

war

e D

evel

opm

ent

00.

000

0.00

00.

000

0.00

00.

000

0.00

2500

Man

agem

ent

00.

000

0.00

00.

000

0.00

00.

000

0.00

3000

Scie

nce

Ope

rati

ons

00.

0094

5,44

85.

3418

,836

*62

,442

*0

0.00

1,02

6,72

65.

9731

00O

bser

vato

ry T

ime

Allo

catio

n0

0.00

00.

000

0.00

50,4

42*

00.

0050

,442

*

3200

Ref

eren

ce0

0.00

00.

000

0.00

00.

000

0.00

00.

00

3300

Broa

der

Impa

cts

00.

0053

,013

0.00

00.

000

0.00

00.

0053

,013

0.00

3400

Scie

ntifi

c St

aff

00.

0019

,205

0.00

00.

000

0.00

00.

0019

,205

0.00

3600

Scie

ntifi

c U

ser

Serv

ices

00.

0087

3,23

05.

3418

,836

*0

0.00

00.

0089

2,06

65.

59

3500

Man

agem

ent

00.

000

0.00

00.

0012

,000

0.00

00.

0012

,000

0.00

4000

Adm

inis

trat

ive

Serv

ices

1,01

7,00

0*

1,50

5,81

526

.77

00.

002,

312,

731

14.4

80

0.00

3,81

8,54

641

.25

4100

Busi

ness

Ser

vice

s1,

017,

000

*17

8,27

5*

00.

001,

430,

001

12.7

00

0.00

1,60

8,27

614

.70

4200

Faci

litie

s0

0.00

1,02

0,50

913

.65

00.

0067

3,95

0*

00.

001,

694,

458

14.4

3

4300

Aux

iliar

ies

00.

0068

,968

9.77

00.

000

0.00

00.

0068

,968

9.77

4500

Man

agem

ent

00.

0023

8,06

4*

00.

0020

8,78

0*

00.

0044

6,84

4*

4800

NR

AO

Ove

rhea

d0

0.00

00.

000

0.00

00.

000

0.00

00.

00

5000

Dir

ecto

r's

Off

ice

51,0

61*

214,

878

3.39

00.

000

0.00

00.

0021

4,87

83.

3951

00Pr

ogra

m M

anag

emen

t0

0.00

00.

000

0.00

00.

000

0.00

00.

00

5200

Publ

ic O

utre

ach

51,0

61*

214,

878

3.39

00.

000

0.00

00.

0021

4,87

83.

39

5300

Com

mun

icat

ions

00.

000

0.00

00.

000

0.00

00.

000

0.00

5500

Adm

inis

trat

ion

00.

000

0.00

00.

000

0.00

00.

000

0.00

5800

AU

I Fee

and

IDC

00.

000

0.00

00.

000

0.00

00.

000

0.00

Gra

nd T

otal

17,7

43,3

787.

157,

640,

322

80.2

518

,836

*2,

821,

846

18.8

075

0,00

0*

11,2

31,0

0410

2.27

Chi

leO

bser

vato

ry C

entr

al

Serv

ices

CSA

-2 A

LMA

Ops

* n<

3 FT

E

CSA

-1 N

RA

O O

psC

SA-2

ALM

A O

psIn

tern

al S

ourc

esG

reen

Ban

kT

otal

, Gre

en B

ank


Observatory Financial/ FTE Projection by Site (Part 3 of 3)

WB

SE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

's10

00T

eles

cope

Ope

rati

ons

12,9

83,7

5713

2.23

1,34

4,31

68.

754,

097

*14

,332

,169

141.

0242

,545

,534

214.

0811

00M

aint

enan

ce5,

780,

871

65.5

458

5,82

23.

750

0.00

6,36

6,69

369

.29

9,26

2,40

884

.54

1200

Ope

ratio

ns3,

580,

696

37.8

175

8,49

45.

004,

097

*4,

343,

287

42.8

511

,144

,039

84.0

8

1300

Spec

trum

Man

agem

ent

00.

000

0.00

00.

000

0.00

530,

167

4.42

1400

Infr

astr

uctu

re M

ods

& U

pgra

des

919,

976

8.51

00.

000

0.00

919,

976

8.51

1,83

7,89

88.

51

1500

Man

agem

ent

2,70

2,21

420

.36

00.

000

0.00

2,70

2,21

420

.36

19,7

71,0

2132

.53

2000

Dev

elop

men

t P

rogr

ams

128,

511

*41

6,62

10.

000

0.00

545,

132

*9,

431,

871

39.7

021

00Bu

sine

ss D

evel

opm

ent

00.

000

0.00

00.

000

0.00

704,

023

3.30

2200

Tec

hnol

ogy

Dev

elop

men

t0

0.00

416,

621

0.00

00.

0041

6,62

10.

007,

586,

738

29.6

7

2300

R&

D S

uppo

rt0

0.00

00.

000

0.00

00.

0038

7,51

94.

13

2400

Soft

war

e D

evel

opm

ent

128,

511

*0

0.00

00.

0012

8,51

1*

128,

511

*

2500

Man

agem

ent

00.

000

0.00

00.

000

0.00

625,

080

*

3000

Scie

nce

Ope

rati

ons

2,70

2,48

721

.50

1,05

6,91

99.

5349

6,33

7*

4,25

5,74

333

.93

13,1

82,0

7290

.33

3100

Obs

erva

tory

Tim

e A

lloca

tion

00.

000

0.00

38,8

59*

38,8

59*

148,

688

*

3200

Ref

eren

ce0

0.00

00.

000

0.00

00.

0067

1,24

9*

3300

Broa

der

Impa

cts

197,

476

*0

0.00

00.

0019

7,47

6*

1,68

1,19

04.

90

3400

Scie

ntifi

c St

aff

546,

272

4.65

192,

652

*0

0.00

738,

924

5.65

1,32

1,70

112

.65

3600

Scie

ntifi

c U

ser

Serv

ices

1,95

8,73

815

.85

864,

267

8.53

00.

002,

823,

005

24.3

87,

429,

080

58.8

8

3500

Man

agem

ent

00.

000

0.00

457,

478

*45

7,47

8*

1,93

0,16

49.

92

4000

Adm

inis

trat

ive

Serv

ices

3,26

9,09

714

.20

00.

002,

904,

166

25.2

36,

173,

263

39.4

317

,924

,501

108.

5941

00Bu

sine

ss S

ervi

ces

00.

000

0.00

1,79

6,50

621

.69

1,79

6,50

621

.69

8,80

8,64

263

.30

4200

Faci

litie

s3,

093,

185

13.0

00

0.00

775,

757

*3,

868,

942

14.0

08,

043,

863

29.4

3

4300

Aux

iliar

ies

6,54

8*

00.

000

0.00

6,54

8*

75,5

1710

.97

4500

Man

agem

ent

169,

363

0.00

00.

0033

1,90

3*

501,

267

*1,

027,

064

4.89

4800

NR

AO

Ove

rhea

d0

0.00

00.

000

0.00

00.

00(3

0,58

6)0.

00

5000

Dir

ecto

r's

Off

ice

189,

796

*0

0.00

00.

0018

9,79

6*

7,92

6,98

822

.28

5100

Prog

ram

Man

agem

ent

00.

000

0.00

00.

000

0.00

445,

050

3.50

5200

Publ

ic O

utre

ach

189,

796

*0

0.00

00.

0018

9,79

6*

1,49

0,27

712

.28

5300

Com

mun

icat

ions

00.

000

0.00

00.

000

0.00

566,

200

*

5500

Adm

inis

trat

ion

00.

000

0.00

00.

000

0.00

1,08

9,22

13.

75

5800

AU

I Fee

and

IDC

00.

000

0.00

00.

000

0.00

4,33

6,24

00.

00

Gra

nd T

otal

19,2

73,6

4717

0.94

2,81

7,85

618

.28

3,40

4,60

028

.17

25,4

96,1

0321

7.39

91,0

10,9

6547

4.97

* n<

3 FT

E

Soco

rro

(Inc

l VLB

A)

Tot

al, S

ocor

roG

rand

Tot

al, A

ll Si

tes

CSA

-1 N

RO

A O

psC

SA-2

ALM

A O

psO

bser

vato

ry C

entr

al

Serv

ices


Table 2: NRAO Observatory Central Services, By Location

WBS Expenses FTE's Expenses FTE's Expenses FTE's Expenses FTE's1000 Telescope Operations 68,157 * 446,673 3.94 4,097 * 518,927 4.311200 Operations 0 0.00 0 0.00 4,097 * 4,097 *

1210 Scheduling 0 0.00 0 0.00 4,097 * 4,097 *

1300 Spectrum Management 68,157 * 446,673 3.94 0 0.00 514,830 4.27

1310 Interference Suppression 0 0.00 346,229 * 0 0.00 346,229 *

1320 NRQZ Management 0 0.00 100,445 * 0 0.00 100,445 *

1340 Internation Spectrum Managemen 68,157 * 0 0.00 0 0.00 68,157 *

2000 Development Programs 988,514 4.20 0 0.00 0 0.00 988,514 4.202100 Business Development 704,023 3.30 0 0.00 0 0.00 704,023 3.30

2110 Partnerships 533,183 * 0 0.00 0 0.00 533,183 *

2120 Commercialization 170,840 * 0 0.00 0 0.00 170,840 *

2500 Management 284,492 * 0 0.00 0 0.00 284,492 *

3000 Science Operations 1,384,710 7.67 62,442 * 496,337 * 1,943,489 10.953100 Observatory Time Allocation 0 0.00 50,442 * 38,859 * 89,301 *

3120 Proposal Review & Time Allocat 0 0.00 50,442 * 38,859 * 89,301 *

3200 Reference 496,168 * 0 0.00 0 0.00 496,168 *

3210 Library 372,859 * 0 0.00 0 0.00 372,859 *

3220 Historical Archives 38,090 * 0 0.00 0 0.00 38,090 *

3230 Metrics & Statistics 85,219 * 0 0.00 0 0.00 85,219 *

3500 Management 888,542 4.87 12,000 0.00 457,478 * 1,358,020 7.47

4000 Administrative Services (7,682,691) 26.06 2,312,731 14.48 2,904,166 25.23 (2,465,793) 65.774100 Business Services 4,046,699 25.06 1,430,001 12.70 1,796,506 21.69 7,273,206 59.45

4110 Business Office 1,187,598 5.50 314,529 3.00 739,675 8.49 2,241,803 16.99

4120 CIS 1,531,425 8.71 230,006 * 510,494 6.20 2,271,924 16.61

4130 CAP 490,815 5.00 41,135 * 151,871 3.00 683,821 9.00

4140 MIS 0 0.00 516,243 3.50 92,891 0.00 609,134 3.50

4150 ESS 80,735 0.00 231,562 * 151,754 * 464,050 4.50

4160 HR 756,126 5.85 96,525 * 149,823 * 1,002,474 8.85

4200 Facilities 2,480,463 * 673,950 * 775,757 * 3,930,170 *

4210 Plant Maintenance 0 0.00 462,429 0.00 368,000 0.00 830,429 0.00

4220 Communication 519,711 0.00 0 0.00 0 0.00 519,711 0.00

4230 Utilities 0 0.00 176,031 0.00 307,000 0.00 483,031 0.00

4240 Leases 1,943,106 * 0 0.00 0 0.00 1,943,106 *

4260 Vehicles 17,646 0.00 35,491 * 100,757 * 153,894 *

4800 NRAO Overhead (14,209,853) 0.00 0 0.00 0 0.00 (14,209,853) 0.00

4500 Management 0 0.00 208,780 * 331,903 * 540,683 3.54

5000 Director's Office 1,660,285 8.27 0 0.00 0 0.00 1,660,285 8.275100 Program Management 445,050 3.50 0 0.00 0 0.00 445,050 3.50

5300 Communications 126,014 * 0 0.00 0 0.00 126,014 *

5800 Administration 1,089,221 3.75 0 0.00 0 0.00 1,089,221 3.75

Grand Total (3,581,024) 46.53 2,821,846 18.80 3,404,600 28.17 2,645,422 93.50

*n < 3 FTE

Charlottesville Green Bank Socorro GRAND TOTALObservatory Central Services


Table 3: FY 2014 Projected Budget by Expense Object

Telescope Operations

Development Programs

Science Operations

Administrative Services

Director's Office Grand Total

% of Total Expenditures

NSF AST CSA-1 NRAO Ops Salary & Benefits 15,873,213 2,083,356 4,071,405 2,357,649 759,005 25,144,628 56.4%

Materials & Supplies 1,142,612 - 246,589 12,579,222 2,233,500 16,201,923 36.4%

Equipment 833,587 126,735 575,707 878,026 255,037 2,669,092 6.0%

Travel 163,560 37,800 258,468 19,166 60,300 539,294 1.2%

Total 18,012,972 2,247,891 5,152,169 15,834,062 3,307,842 44,554,936 100.0%

NSF AST CSA-2 ALMA Ops Salary & Benefits 3,288,797 766,769 4,290,650 672,750 596,498 9,615,464 22.4%

Materials & Supplies - 612,000 - - - 612,000 1.4%

Equipment 20,474,327 4,040,197 1,065,894 3,810,482 2,313,327 31,704,226 74.0%

Travel 250,511 26,500 507,466 73,000 42,240 899,717 2.1%

Total 24,013,635 5,445,466 5,864,010 4,556,232 2,952,065 42,831,407 100.0%

NSF CSA-4 REU/RIT Salary & Benefits

Materials & Supplies 131,168 6,796 137,964 72.9%

Equipment 51,236 51,236 27.1%

Travel

Total 182,404 6,796 189,200 100.0%

Internal Funding Sources Salary & Benefits 519,169 519,169 69.2%

Materials & Supplies - -

Equipment 243,840 243,840 32.5%

Travel - -

Total 750,000 750,000 100.0%

Observatory Central Services Salary & Benefits 462,090 909,510 1,652,633 6,364,871 1,425,694 10,814,797

Materials & Supplies - - - 4,046,968 17,500 4,064,468

Equipment 45,120 56,840 147,756 (13,002,384) 102,797 (12,649,871)

Travel 11,716 22,164 143,100 124,752 114,295 416,028

Total 518,927 988,514 1,943,489 (2,465,793) 1,660,285 2,645,422

NSF SPO-4 Solar Burst Spect. Salary & Benefits 37,928 37,928 94.8%

Materials & Supplies 2,072 2,072 5.2%

Equipment

Travel

Total 40,000 40,000 100.0%

TOTAL, Salaries & Benefits 19,624,100 4,278,804 10,052,616 9,395,269 2,781,197 46,131,986 50.7%TOTAL M&S 1,142,612 612,000 379,829 16,626,190 2,257,796 21,018,426 23.1%TOTAL Equipment 21,353,034 4,467,611 1,840,593 (8,313,876) 2,671,160 22,018,523 24.2%TOTAL Travel 425,787 86,464 909,034 216,918 216,835 1,855,038 2.0%GRAND TOTAL 42,545,534 9,431,871 13,182,072 17,924,501 7,926,988 91,010,965 100.0%


Table 4: Observatory Work Breakdown Structure (Part 1 of 2)

WB

SE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

's

1000

Tel

esco

pe O

pera

tion

s4,

997,

827

44.8

98,

209,

526

81.8

14,

691,

843

49.9

216

,052

*0

0.00

97,7

24*

18,0

12,9

7217

7.42

24,0

13,6

3532

.35

1100

Mai

nten

ance

1,13

1,93

05.

553,

883,

140

44.2

11,

897,

731

21.3

315

,552

*0

0.00

00.

006,

928,

352

71.2

42,

334,

056

13.3

0

1200

Ope

ratio

ns2,

992,

943

33.6

71,

637,

367

14.6

71,

943,

329

23.1

450

00.

000

0.00

00.

006,

574,

139

71.4

94,

565,

804

12.5

5

1300

Spec

trum

Man

agem

ent

00.

000

0.00

00.

000

0.00

00.

0015

,336

*15

,336

*0

0.00

1400

Infr

astr

uctu

re M

ods

& U

pgra

des

47,9

220.

0063

7,77

36.

9428

2,20

3*

00.

000

0.00

00.

0096

7,89

88.

5187

0,00

00.

00

1500

Man

agem

ent

825,

033

5.67

2,05

1,24

715

.99

568,

579

3.87

00.

000

0.00

82,3

88*

3,52

7,24

626

.03

16,2

43,7

756.

50

2000

Dev

elop

men

t P

rogr

ams

00.

000

0.00

00.

000

0.00

2,11

9,38

025

.68

128,

511

*2,

247,

891

26.8

85,

445,

466

5.65

2100

Busi

ness

Dev

elop

men

t0

0.00

00.

000

0.00

00.

000

0.00

00.

000

0.00

00.

00

2200

Tec

hnol

ogy

Dev

elop

men

t0

0.00

00.

000

0.00

00.

001,

553,

258

21.5

60

0.00

1,55

3,25

821

.56

5,28

3,48

15.

15

2300

R&

D S

uppo

rt0

0.00

00.

000

0.00

00.

0038

7,51

94.

130

0.00

387,

519

4.13

00.

00

2400

Soft

war

e D

evel

opm

ent

00.

000

0.00

00.

000

0.00

00.

0012

8,51

1*

128,

511

*0

0.00

2500

Man

agem

ent

00.

000

0.00

00.

000

0.00

178,

603

0.00

00.

0017

8,60

30.

0016

1,98

5*

3000

Scie

nce

Ope

rati

ons

699,

091

3.95

88,2

08*

34,8

32*

00.

000

0.00

4,33

0,03

833

.69

5,15

2,16

938

.68

5,86

4,01

040

.70

3100

Obs

erva

tory

Tim

e A

lloca

tion

00.

000

0.00

00.

000

0.00

00.

0059

,387

*59

,387

*0

0.00

3200

Ref

eren

ce0

0.00

00.

000

0.00

00.

000

0.00

120,

000

0.00

120,

000

0.00

55,0

810.

00

3300

Broa

der

Impa

cts

00.

000

0.00

00.

000

0.00

00.

0072

5,84

54.

6072

5,84

54.

6077

2,94

1*

3400

Scie

ntifi

c St

aff

00.

000

0.00

00.

000

0.00

00.

0075

2,81

77.

6575

2,81

77.

6552

8,88

45.

00

3600

Scie

ntifi

c U

ser

Serv

ices

699,

091

3.95

88,2

08*

34,8

32*

00.

000

0.00

2,67

1,98

920

.94

3,49

4,12

025

.93

3,93

4,96

032

.95

3500

Man

agem

ent

00.

000

0.00

00.

000

0.00

00.

000

0.00

00.

0057

2,14

4*

4000

Adm

inis

trat

ive

Serv

ices

125,

120

0.00

2,24

7,90

612

.55

653,

279

*0

0.00

00.

0012

,807

,757

29.0

215

,834

,062

42.0

24,

556,

232

*41

00Bu

sine

ss S

ervi

ces

00.

000

0.00

00.

000

0.00

00.

0047

3,37

13.

0547

3,37

13.

051,

062,

065

*

4200

Faci

litie

s12

5,12

00.

002,

247,

906

12.5

565

3,27

9*

00.

000

0.00

1,08

7,38

913

.65

4,11

3,69

326

.65

00.

00

4300

Aux

iliar

ies

00.

000

0.00

00.

000

0.00

00.

0075

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10.9

775

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10.9

70

0.00

4500

Man

agem

ent

00.

000

0.00

00.

000

0.00

00.

0048

6,38

1*

486,

381

*0

0.00

4800

NR

AO

Ove

rhea

d0

0.00

00.

000

0.00

00.

000

0.00

10,6

85,1

000.

0010

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,100

0.00

3,49

4,16

70.

00

5000

Dir

ecto

r's

Off

ice

00.

000

0.00

00.

000

0.00

00.

003,

307,

842

8.26

3,30

7,84

28.

262,

952,

065

5.75

5100

Prog

ram

Man

agem

ent

00.

000

0.00

00.

000

0.00

00.

000

0.00

00.

000

0.00

5200

Publ

ic O

utre

ach

00.

000

0.00

00.

000

0.00

00.

0076

9,65

17.

4376

9,65

17.

4372

0,62

64.

85

5300

Com

mun

icat

ions

00.

000

0.00

00.

000

0.00

00.

0019

8,19

1*

198,

191

*24

1,99

5*

5500

Adm

inis

trat

ion

00.

000

0.00

00.

000

0.00

00.

000

0.00

00.

000

0.00

5800

AU

I Fee

and

IDC

00.

000

0.00

00.

000

0.00

00.

002,

340,

000

0.00

2,34

0,00

00.

001,

989,

444

0.00

Gra

nd T

otal

5,82

2,03

848

.84

10,5

45,6

4095

.10

5,37

9,95

450

.67

16,0

52*

2,11

9,38

025

.68

20,6

71,8

7372

.82

44,5

54,9

3629

3.26

42,8

31,4

0785

.25

NE

T(6

26,0

36)

(0

)

Oth

erT

otal

, CSA

-1 N

RA

O O

psN

on-T

eles

cope

* n<

3 FT

E

CSA

-1 N

RA

O O

psC

DL

CSA

-2 A

LMA

Ops

GB

TE

VLA

VLB

A

42,8

31,4

07

43,9

28,9

00

16

0,00

0

Tot

al R

even

ues

Rev

enue

sN

SF A

lloca

tion

NSF

Car

ryfo

rwar

d Fu

nds,

Inc

Prio

r Y

ear

Com

mitm

ents

CC

R

GB

Fees

WFO

in S

cope

(V

LBA

& G

BT E

xter

nal S

uppo

rt)

WFO

Net

Rev

enue

Oth

er R

even

ue

6,42

1,40

7

36,4

10,0

00

CSA

-2 A

LMA

Ops

1,59

3,90

0

100,

000

1,07

5,00

0

41

,000

,000

CSA

-1 N

RA

O O

ps


Observatory Work Breakdown Structure (Part 2 of 2)

WB

SE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

'sE

xpen

ses

FTE

's

1000

Tel

esco

pe O

pera

tion

s0

0.00

518,

927

4.31

518,

927

4.31

00.

000

0.00

00.

000

0.00

00.

0042

,545

,534

214.

0811

00M

aint

enan

ce0

0.00

00.

000

0.00

00.

000

0.00

00.

000

0.00

00.

009,

262,

408

84.5

4

1200

Ope

ratio

ns0

0.00

4,09

7*

4,09

7*

00.

000

0.00

00.

000

0.00

00.

0011

,144

,039

84.0

8

1300

Spec

trum

Man

agem

ent

00.

0051

4,83

04.

2751

4,83

04.

270

0.00

00.

000

0.00

00.

000

0.00

530,

167

4.42

1400

Infr

astr

uctu

re M

ods

& U

pgra

des

00.

000

0.00

00.

000

0.00

00.

000

0.00

00.

000

0.00

1,83

7,89

88.

51

1500

Man

agem

ent

00.

000

0.00

00.

000

0.00

00.

000

0.00

00.

000

0.00

19,7

71,0

2132

.53

2000

Dev

elop

men

t P

rogr

ams

284,

492

*70

4,02

33.

3098

8,51

44.

200

0.00

00.

0028

4,00

0*

466,

000

*75

0,00

0*

9,43

1,87

139

.70

2100

Busi

ness

Dev

elop

men

t0

0.00

704,

023

3.30

704,

023

3.30

00.

000

0.00

00.

000

0.00

00.

0070

4,02

33.

30

2200

Tec

hnol

ogy

Dev

elop

men

t0

0.00

00.

000

0.00

00.

000

0.00

284,

000

*46

6,00

0*

750,

000

*7,

586,

738

29.6

7

2300

R&

D S

uppo

rt0

0.00

00.

000

0.00

00.

000

0.00

00.

000

0.00

00.

0038

7,51

94.

13

2400

Soft

war

e D

evel

opm

ent

00.

000

0.00

00.

000

0.00

00.

000

0.00

00.

000

0.00

128,

511

*

2500

Man

agem

ent

284,

492

*0

0.00

284,

492

*0

0.00

00.

000

0.00

00.

000

0.00

625,

080

*

3000

Scie

nce

Ope

rati

ons

00.

001,

943,

489

10.9

51,

943,

489

10.9

540

,000

0.00

182,

404

0.00

00.

000

0.00

00.

0013

,182

,072

90.3

331

00O

bser

vato

ry T

ime

Allo

catio

n0

0.00

89,3

01*

89,3

01*

00.

000

0.00

00.

000

0.00

00.

0014

8,68

8*

3200

Ref

eren

ce0

0.00

496,

168

*49

6,16

8*

00.

000

0.00

00.

000

0.00

00.

0067

1,24

9*

3300

Broa

der

Impa

cts

00.

000

0.00

00.

000

0.00

182,

404

0.00

00.

000

0.00

00.

001,

681,

190

4.90

3400

Scie

ntifi

c St

aff

00.

000

0.00

00.

0040

,000

0.00

00.

000

0.00

00.

000

0.00

1,32

1,70

112

.65

3600

Scie

ntifi

c U

ser

Serv

ices

00.

000

0.00

00.

000

0.00

00.

000

0.00

00.

000

0.00

7,42

9,08

058

.88

3500

Man

agem

ent

00.

001,

358,

020

7.47

1,35

8,02

07.

470

0.00

00.

000

0.00

00.

000

0.00

1,93

0,16

49.

92

4000

Adm

inis

trat

ive

Serv

ices

00.

00(2

,465

,793

)65

.77

(2,4

65,7

93)

65.7

70

0.00

00.

000

0.00

00.

000

0.00

17,9

24,5

0110

8.59

4100

Busi

ness

Ser

vice

s0

0.00

7,27

3,20

659

.45

7,27

3,20

659

.45

00.

000

0.00

00.

000

0.00

00.

008,

808,

642

63.3

0

4200

Faci

litie

s0

0.00

3,93

0,17

0*

3,93

0,17

0*

00.

000

0.00

00.

000

0.00

00.

008,

043,

863

29.4

3

4300

Aux

iliar

ies

00.

000

0.00

00.

000

0.00

00.

000

0.00

00.

000

0.00

75,5

1710

.97

4500

Man

agem

ent

00.

0054

0,68

33.

5454

0,68

33.

540

0.00

00.

000

0.00

00.

000

0.00

1,02

7,06

44.

89

4800

NR

AO

Ove

rhea

d0

0.00

(14,

209,

853)

0.00

(14,

209,

853)

0.00

00.

000

0.00

00.

000

0.00

00.

00(3

0,58

6)0.

00

5000

Dir

ecto

r's

Off

ice

00.

001,

660,

285

8.27

1,66

0,28

58.

270

0.00

6,79

60.

000

0.00

00.

000

0.00

7,92

6,98

822

.28

5100

Prog

ram

Man

agem

ent

00.

0044

5,05

03.

5044

5,05

03.

500

0.00

00.

000

0.00

00.

000

0.00

445,

050

3.50

5200

Publ

ic O

utre

ach

00.

000

0.00

00.

000

0.00

00.

000

0.00

00.

000

0.00

1,49

0,27

712

.28

5300

Com

mun

icat

ions

00.

0012

6,01

4*

126,

014

*0

0.00

00.

000

0.00

00.

000

0.00

566,

200

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APPENDIX B: MAJOR MILESTONES SUMMARY

POP Section Number

POP Milestone Task Name

Completion Date

OBSERVATORY SCIENCE OPERATIONS 3.1 Science Support and Research

Telescope Time Allocation (TTA) 1 SSR review of TTA 12/31/2013 2 CfP for semester 2014B 03/31/2014 3 CfP for semester 2015A 09/30/2014 4 SRP & tech review process, semester 2014B 03/31/2014 5 SRP & tech review process, semester 2015A 09/30/2014 6 TAC meeting for semester 2014A 12/31/2013 7 TAC meeting for semester 2014B 06/30/2014 8 Update SW tools requirements for TAC support 2014A 12/31/2013 9 Update SW tools requirements for PST 2014B 03/31/2014 10 Update SW tools requirements for TAC support 2014B 06/30/2014 11 Update SW requirements tools for PST 2015A 09/30/2014 12 Update documentation for CfP & tools 2014B 03/31/2014 13 Update documentation for CfP & tools 2015A 09/30/2014 Science User Services (SUS) 14 HD 4.5 documentation 12/31/2013 15 Update ALMA Cycle 2 proposal preparation documentation 12/31/2013 16 Update CASAGUIDES 12/31/2013 17 Update CASAGUIDES 06/30/2014 18 IAU Symposium 303 – The Galactic Center 12/31/2013 19 NRAO/China Science Workshop 06/30/2014 20 8th NAASC sponsored science workshop 09/30/2014 21 AAT/ASA science requirements 12/31/2013 22 Manual reduction of ALMA science data and QA2 12/31/2013 23 Manual reduction of ALMA science data and QA2 03/31/2014 24 ALMA pipeline tests complete between manual and pipeline products 06/30/2014 25 Requirements for integrated science portal 06/30/2014 26 Manual reduction of ALMA science data and QA2 06/30/2014 27 Reprocessing pipeline interface tested 09/30/2014 28 Manual reduction of ALMA science data and QA2 09/30/2014 Science & Academic Affairs 29 Jansky Fellow selection 12/31/2013 30 NRAO summer student selection 03/31/2014 31 SOS program selection for ALMA Cycle 2 06/30/2014 32 Summer student program begins 06/30/2014


POP Section Number


Completion Date

33 Summer Student program concludes 09/30/2014 Science Support and Research Services 34 Renegotiate electronic journals 03/31/2014 OBSERVATORY TELESCOPE OPERATIONS

4.1 Atacama Large Millimeter/submillimeter Array (ALMA) Construction 1 ALMA Construction Completion and Operations Readiness Review 03/31/2014 2 Acceptance of Optical Pointing Telescopes 12/31/2013 3 Complete installation of 400V cables and fuse disconnects at AOS 12/31/2013 4 Complete delivery of FE Thermal Interlock Modules 03/31/2014 5 Complete delivery of NAOJ Band 4, 8, and 10 multipliers 03/31/2014 6 Delivery of first Front End Handling Vehicle (FEHV) 03/31/2014 7 Delivery of three remaining FEHVs 09/30/2014 Operations NAASC/NA ARC 8 ALMA Construction Completion and Operations Readiness Review 03/31/2014 9 ALMA C1 User Survey 03/31/2014 10 C2 Phase 2 Software Tests 06/30/2014 11 Start of C2 observing season 06/30/2014 12 C1 Data Delivery Closeout 09/30/2014 Offsite HW 13 Establish long-term maintenance contracts for vendor bulk modules 06/30/2014

4.2 Very Large Array (VLA) Scientific Support for Operations 1 Support the 2014B semester (2014 Feb 1) Call for Proposals 03/31/2014 2 Support the 2015A semester (2014 Aug 1) Call for Proposals 09/30/2014 3 Support reconfiguration to B-config 12/31/2013 4 Support reconfiguration to BnA and A-configs 03/31/2014 5 Support reconfiguration to D-config 06/30/2014 6 Support reconfiguration to DnC-config 09/30/2014 7 Stabilize VLA capabilities: Y27, sub-arrays, & fast dumps 06/30/2014 Array Operations 8 Re-configurations to B config 12/31/2013 9 Re-configurations to BnA and A configs 03/31/2014 10 Re-configuration to D config 06/30/2014 11 Re-configuration to DnC config 09/30/2014

12 Complete evaluation of whether evening and nighttime array operations can be moved to Socorro 06/30/2014

VLA Prototype ACU


POP Section Number


Completion Date

13 Critical Design Review of ACU prior to 2nd installation 12/31/2013 14 Install 2nd ACU 03/31/2014 15 Scientific evaluation of ACU performance 06/30/2014 16 Install 3rd ACU 09/30/2014 VLA Thermal Gap Retrofit 17 Install thermal gap on 3 VLA C-Band receivers. 09/30/2014 18 Install thermal gap on 6 VLA L-Band receivers. 09/30/2014 VLA Card Cage Upgrade 19 Install 48 card cage upgrades for VLA front ends 09/30/2014 VLA 3-Bit Sampler Upgrade 20 Install 3-bit sampler PCB in 2 VLA DTS modules 03/31/2014 21 Present performance analysis to NRAO staff 06/30/2014 VLA API Upgrade 22 Install final 2 API dishes 12/31/2013 23 Incorporate API output into VLA dynamic scheduler 06/30/2014 Capability Enhancements 24 Define and demonstrate new SR and general capabilities for 2014B 12/31/2013 25 Define and demonstrate new SR and general capabilities for 2015A 06/30/2014 Operational Enhancements 26 Improved referenced pointing 09/30/2014 27 Tipping scans implemented 03/31/2014 28 Improved switched power calibration 06/30/2014 29 Pipeline heuristic development 09/30/2014

Infrastructure Maintenance and Renewal 30 Overhaul total of 6 antennas 12/31/2013 31 Overhaul total of 6 antennas 03/31/2014 32 Overhaul total of 6 antennas 06/30/2014 33 Overhaul total of 6 antennas 09/30/2014 34 Replace azimuth bearing on one antenna (probably EA21) 09/30/2014 35 Replace 2500 ties 09/30/2014 36 Replace 3 intersections 09/30/2014 37 Develop proposal for VLA VAX building 09/30/2014 38 Replace VLA Activity Center transformer 06/30/2014 39 Preventive maintenance on 90 VLA site transformers 09/30/2014 40 Preventive maintenance on hatch gear 03/31/2014 41 Preventive maintenance on hatch gear 09/30/2014


POP Section Number


Completion Date

4.3 Very Long Baseline Array (VLBA) Scientific Support for Operations 1 Support the 2014B semester (2014 Feb 1) Call for Proposals 03/31/2014 2 Support the 2015A semester (2014 Aug 1) Call for Proposals 09/30/2014 3 Complete verification tests of VLBA dual RDBE system 03/31/2014 4 Define and document calibration procedures for VLBA dual RDBEs 09/30/2014 5 Stabilize VLBA + Y27/GBT operations 03/31/2014 Retirement of VLBA VMEs

6 Design, build, and install VLBA Control Computer Interface Box in laboratory 12/31/2013

7 Test VLBA interface box in VLBA antenna 09/30/2014 Retirement of Legacy Recording System 8 Complete transition of projects using legacy system to DDC 06/30/2014 9 Re-integrate Mark 5A recorders from sites into correlator 06/30/2014 C-Band Receivers 10 Complete construction of spare VLBA C-Band receiver 03/31/2014 11 Upgrade two pre-production VLBA C-Band receivers 09/30/2014 Capability Enhancements 12 Define and demonstrate new SR and general capabilities for 2014B 12/31/2013 13 Define and demonstrate new SR and general capabilities for 2015A 06/30/2014 Infrastructure Maintenance and Renewal 14 Tiger Team maintenance visit to North Liberty 06/30/2014 15 Tiger Team maintenance visit to Hancock 09/30/2014

4.4 Green Bank Telescope (GBT) GBT Maintenance 1 Beginning of summer painting 06/30/2014 2 End of summer painting 09/30/2014 3 GBT track inspection will take place, any needed repairs completed 09/30/2014 Antenna Performance 4 A new pointing model for the GBT will be developed 12/31/2013 GBT Operations

5 A retirement plan for the GBT spectrometer and spectral processor will be put in place 09/30/2014

OBSERVATORY DEVELOPMENT PROGRAMS

5.1 CDL Development

Phased Array Feeds

1 Design improved low-noise amplifier with lower noise and improved reliability 03/31/2014

2 Design balanced low-noise amplifier for PAF integration 09/30/2014

3 Complete study on cryogenic efficiency, new window and IR filter materials, and modular cryogenic architectures for large PAFs 09/30/2014


POP Section Number


Completion Date

4 Demonstrate single L-Band prototype integrated downconverter digital photonic link 03/31/2014

5 Integrate and test digital downconverter photonic links on existing PAF 09/30/2014

6 Demonstrate single-FPGA narrowband beamformer prototype 03/31/2014

7 Demonstrate three-FPGA intermediate-bandwidth beamformer prototype 09/30/2014

8 Demonstrate and verify PAF optimization algorithm with impedance matching network and feed geometry as input parameters 09/30/2014

9 Complete design study on optimum wideband antenna elements for a PAF 06/30/2014

10 Implement version control and document existing PAF software 12/31/2013

11 Demonstrate new release of PAF software with improved user interface and real-time analysis capability 06/30/2014

Advanced Receiver Technologies 12 Test triangular Digital OMT (DOMT) on the sky 12/31/2013 13 Demonstrate polarization isolation of DOMT using FPGA 03/31/2014 14 Measure W-Band phase stability of the LO distribution network 03/31/2014

15 Demonstrate printed circuit flexible thermal transition with low loss up to 40 GHz 06/30/2014

16 Build multi-channel digital back end for testing of digital photonic links 03/31/2014 5.2 ALMA Development

Band 5 Local Oscillator

1 Unit production; WCA No. 04 - 05 12/31/2013



4 Unit production; WCA No. 51 - 75 09/30/2014 5.3 GBT Developments

1 ARGUS Cryostat Complete 03/31/2014 2 ARGUS Module delivery complete 06/30/2014 3 ARGUS IF/LO complete 06/30/2014 4 ARGUS Warm electronics complete 03/31/2014 5 ARGUS Feeds complete 09/30/2014

6 MUSTANG 1.5 Science commissioning begins 12/31/2013

7 MUSTANG 1.5 project complete 06/30/2014

OBSERVATORY-WIDE SERVICES

6.1 Central Development Lab 1 Complete repairs of VLA L-Band LNAs 09/30/2014 2 Complete production of eight spare Band 6 SIS mixers 09/30/2014 3 Demonstrate 4-12 GHz balanced IF LNA with low power dissipation 03/31/2014


POP Section Number


Completion Date

4 Demonstrate balanced 2SB SIS mixer with 4-12 GHz IF that exceeds noise performance of current Band 6 mixer 09/30/2014

5 Demonstrate Nb/Al-AlN/NbTiN SIS mixer with low noise up to 900 GHz 06/30/2014

6 Demonstrate low-loss hybrid for 800-950 GHz 09/30/2014 7 Complete design of reflective Band 2 optics 03/31/2014 8 Build and measure Band 2 feed 09/30/2014 9 Produce prototype data acquisition upgrade for PAPER 03/31/2014

10 Characterize beam pattern of MWA tiles and PAPER antennas using ORBCOMM satellite 03/31/2014

11 Deploy upgraded low-frequency antenna on Green Bank solar radio burst monitor 06/30/2014

12 Deploy improved data acquisition system on Green Bank solar radio burst monitor 06/30/2014

13 Deploy DARE engineering prototype in Green Bank 09/30/2014 6.2 Data Management & Software

Software Development Archive Access Tool 1 Develop initial design of ALMA Archive Tool 03/31/2014 2 Develop ALMA Archive Tool prototype 09/30/2014 CASA Pipeline 3 Develop CASA pipeline for ALMA Cycle 1 Early Science 12/31/2013 4 Integrate VLA Scripted Pipeline 12/31/2013 5 Develop CASA pipeline for ALMA Cycle 2 Early Science 03/31/2014 CASA 6 Release CASA version 4.2 12/31/2013 7 Release CASA version 4.3 06/30/2014

8 Develop CASA version 4.4

12/31/2013 03/31/2014 06/30/2014 09/30/2014

9 Develop CASA VO support 09/30/2014 Observing Preparation Tool 10 Implement OPT updates for Semester 2014A VLA observing 03/31/2014 11 Implement OPT updates for Semester 2014B VLA observing 09/30/2014 Proposal Handling Tool 12 Implement PHT updates for Semester 2014A TAC meeting 12/31/2013 13 Implement PHT updates for Semester 2014B TAC meeting 06/30/2014 Proposal Submission Tool 14 Implement PST updates for Semester 2014B Call for Proposals 12/31/2013 15 Implement PST updates for Semester 2015A Call for Proposals 06/30/2014


POP Section Number


Completion Date

Reprocessing 16 Complete Reprocessing interface 09/30/2014

ALMA Systems Software


17 Deploy Dynamic Scheduling software 03/31/2014

18 Deploy Quick-look improvements software 12/31/2013

19 Incorporate TelCal calibrations in scan sequences 03/31/2014


20 Implement correlator improvements 09/30/2014

VLBI Modifications

21 Deploy ALMA phasing project correlator software 09/30/2014

VLA/VLBA System

22 Deploy software to support Semester 2013B observing 12/31/2013

23 Deploy software to support Semester 2014A commissioning 12/31/2013

24 Deploy software to support Semester 2014A observing 06/30/2014

25 Deploy software to support Semester 2014B commissioning 06/30/2014

26 Deploy hardware & software to support Full On-The-Fly Mosaics for VLA Resident Shared Risk Observing use 09/30/2014

27 Conduct observations with new, non-VME hardware 09/30/2014

28 Demonstrate quasi-real time spacecraft tracking 03/31/2014

29 Demonstrate wideband observing stabilization 09/30/2014

GBT System

WVSys-Archive

30 GBT Data in NRAO Archive 03/31/2014

WVSys - M&C

31 Core infrastructure changes complete 12/31/2013

32 M&C system modified to use new infrastructure 06/30/2014

33 Deliver Astrid modifications & commission on-site 09/30/2014

GBTPP - Pipeline

34 Deliver GBT imaging capability in CASA 12/31/2013

35 VEGAS supports highest data rates 03/31/2014

36 Complete GBT Pipeline parallelization 06/30/2014

Scientific Information Services

Archive & Cluster

37 Draft computer access policy for external users 12/31/2013

38 Enable early access to cluster resources 03/31/2014

XSEDE/Cloud

39 Install Grid/Cloud Middleware 03/31/2014

40 Prototype access available to non-NRAO computing cycles 09/30/2014


POP Section Number


Completion Date

Network Performance

41 Enable improved monitoring of Internet 2 links 03/31/2014

42 Release remote link test procedures to users 06/30/2014

Cluster Performance

43 Complete cluster performance characterization 09/30/2014

Co-location at UVa

44 Install 10 Gigabit/s link to UVa Data Center 12/31/2013

45 Install storage at UVa 03/31/2014

Green Bank data

46 Install 10 Gigabit network hardware 12/31/2013

47 GB link go-live 03/31/2014

48 Condition access to PSC Data Supercell 06/30/2014

DMSD Administration

49 Complete Data Management & Services Department formation 12/31/2013

50 Organize and hold a Data Management & Services Review 06/30/2014

6.3 Program Management Department

1 PMD SOP Development complete 09/30/2014

2 Audit complete – proposal development 12/31/2013

3 Audit complete – project management 03/31/2014

4 Audit complete – Documentation 06/30/2014

5 Audit complete – Analytics and Decision Support 09/30/2014

6 PMD F2F complete 12/31/2013

6.4 Education and Public Outreach

News & Public Information

1 Specify, Develop, and Review Design NRAO Homepage 12/31/2013

2 Program, implement design, test, correct, migrate Homepage to live server 03/31/2014

3 Archive and houseclean deprecated web content 06/30/2014

4 NRAO lobby display: Define and specify project. Design digital signage display 12/31/2013

5 NRAO lobby display: Programming and graphical implementation 12/31/2013

6 NRAO lobby display: Procure digital signage software system, program digital signage display, publish to network 12/31/2013

7 Milky Way Explorer for public website: Design and specify project. Develop design 03/31/2014

8 Milky Way Explorer for public website: Produce scripts, narrations, graphics, videos, program and implement 06/30/2014

STEM Education

9 Conduct online course for first cohort of Skynet Jr. Scholars educators 12/31/2013

10 Skynet science and education workshop II 06/30/2014


POP Section Number


Completion Date

11 Educational Module Set II Development workshop 09/30/2014

12 Conduct Governor’s School Program in GB 09/30/2014

13 Review existing inventory of assets and annotate in accordance with appropriate STEM-related teaching standards 06/30/2014

14 Create thematic STEM assets database/catalog/clusters and publish to NRAO public website 09/30/2014

6.5 Administration

Business Services

1 Succession planning documentation for OAS divisions 12/31/2013

CAP

2 Create a process to label controlled items as “ITAR Controlled” or “EAR Controlled” 03/31/2014

3 Develop on-line Export Compliance training 03/31/2014

4 Develop labeling for “ITAR Controlled” and “EAR Controlled” shipments 06/30/2014

5 Develop Grants Lifecycle training program 06/30/2014

ES&S

6 Develop a comprehensive safety training plan 12/31/2013

7 Develop a safety work order system 09/30/2014

8 Develop a security policy 06/30/2014

MIS

9 Implementation of new cost allocation system 12/31/2013

10 Upgrade of J.D. Edwards to tools release 9.1.3 03/31/2014

11 Investigation and implementation of automated Personnel Evaluation Process 12/31/2013

TTO

12 Form at least one Cooperative Research Agreement with industry 09/30/2014

6.6 Human Resources

Compensation

1 Complete the FY 2013 performance review process on time using a new performance software system 06/30/2014

2 Provide managers with the information and guidance to complete the FY 2014 Salary Review Process 06/30/2014

Policy

3 Complete update and consolidation of NRAO HR policies 12/31/2013

Training

4 Develop new management training courses 09/30/2014

Employment

5

Review the feasibility of replacing the existing applicant tracking system (PeopleAdmin) thru the use of an add-on tracking module to the performance management system

09/30/2014

6.7 Diversity

Communication


POP Section Number


Completion Date

1 Clarify and communicate the Diversity Mission 12/31/2013

New Initiatives

2 Develop action plan for Diversity Review Panel report 09/30/2014

Training

3 Continue diversity training – cultural workplace topics, gender, ADA, Veterans, etc 09/30/2014

International Outreach

4

Continue to build International relationships to create pipeline for next generation of scientists and engineers. Investigate alternative funding streams to sustain partnerships

09/30/2014

Domestic Outreach

5 Continue domestic outreach partnerships to maintain pipeline. Partner with EPO and SSR to maximize existing programs and funding 03/31/2014

Employment

6 Implement recruitment guide and provide training that focuses on diversity focus 12/31/2013

6.8 Computing & Information Services

1 Installation of staff Helpdesk solution 03/31/2014

2 Standardization of platform patch solutions 06/30/2014

3 Evaluate Open Source NAS 06/30/2014

4 Installation of 10Gbps network equipment 03/31/2014

5 Retirement of leagacy LDAP 12/31/2013

6 Evaluation of interactive Web collaboration tool 12/31/2013

7 Installation and training for collaboration tool 09/30/2014

8 Evaluation of Bro tool 03/31/2014

9 Update to staff security training curriculum 09/30/2014

10 Specification and installation of ER generator 12/31/2013

11 Installation of archive servers in UVa Data Center 12/31/2013

12 Prox-card solution for Socorro doors 09/30/2014

6.9 Director’s Office

Communication

1 Publish NRAO 2013 Annual Report 09/30/2014

2 Complete NRAO exhibit re-design for January 2014 American Astronomical Society meeting 12/31/2013

3 Submit science symposium proposal(s) for 2015 American Association for the Advancement of Science Annual Meeting 06/30/2014


APPENDIX C: FY 2014 NRAO INFRASTRUCTURE MAINTENANCE & RENEWAL SUMMARY

The NRAO takes seriously its role of protecting and assuring that the physical assets needed for the functioning of the Observatory are maintained and renewed as required. Infrastructure systems include fixed assets, control systems, and software required to operate, manage and monitor the systems. Infrastructure also includes accessory buildings, roads, communications systems, energy, waste, and water management facilities, and site vehicle and maintenance equipment that are an essential part of the overall system. Although the NRAO sites are responsible for infrastructure performance, prioritization of site infrastructure maintenance and repair needs is both a site responsibility and an Observatory-wide activity. The site prioritizes and performs routine maintenance and repair. Extraordinary maintenance and repair requirements are prioritized and funded at the Observatory-wide level. As not all infrastructure needs can be funded at the present allocation levels, NRAO maintains a prioritized list of infrastructure initiatives in case funds become available and as a reminder of issues and opportunities pending. Full details for these projects are maintained outside this document. As described within the document text, and compiled here in this appendix in summary, the FY 2013 Program Operating Plan includes the following routine maintenance and infrastructure renewal activities: ALMA Maintenance Plans and Schedules North American ALMA Offsite Maintenance provides technical support and maintenance services for ALMA devices and instrumentation by agreement with the JAO. In most cases, the NRAO NA ALMA offsite group is responsible for the repair and maintenance of the same devices that it developed and manufactured during the construction project. The ALMA maintenance plan is divided into tiers, with the JAO staff responsible in most cases for Tier 1 and Tier 2 maintenance on site, and the regional (offsite) labs responsible for Tier 3 maintenance, which involve component-level diagnostics and repairs. NRAO Offsite Hardware Maintenance consists of several groups in Charlottesville including: FE components plus the Band 6 cold cartridge; Local Oscillator (LO)- warm cartridge assembly and cryogenic multipliers; Photonics - central LO modules and antenna articles; Correlator; and Antenna; as well as the BE group in Socorro (antenna articles, data receiver articles, and some of the central LO articles). Front End support for the Band 3 cold cartridges is provided by our Canadian partners at NRC-Herzberg. Through the hardware expertise and experience of NRAO technical staff, efficient use of resources, and the coordination with onsite Chilean staff and offsite support staff from our international ALMA partners, the Offsite Hardware Maintenance Division helps to ensure that the ALMA Observatory operates at its maximum scientific potential. Specific ongoing operational activities of the NRAO hardware maintenance groups in support of this mission include:

• Planning the level and type of hardware maintenance support based on available resources and a continuous analysis of operational failure rate data

• Assisting with onsite troubleshooting and repair through regular coordination with Chilean maintenance staff and hardware support staff from our international partners

• Troubleshooting and repair of items returned to NRAO that require NRAO expertise and facilities

• Coordination and oversight of maintenance contracts for vendor-built modules supplied by NRAO during construction


• Troubleshooting and maintenance, including software support, of test systems used by Chilean maintenance staff designed and/or delivered by NRAO as part of the Construction project

• Training of Chilean maintenance staff in troubleshooting and repair of both ALMA hardware deliverables and the systems to test them

• Procurement, assembly, and testing of spare components to maintain an appropriate stock consistent with observed failure rates

• Continued improvement of testing and repair procedures in collaboration with onsite Chilean staff

• Serving as a technical knowledge resource for the ALMA project (such as serving on design reviews for ALMA development projects)

• Supporting the ICT in implementing new Correlator modes • Shipping and receiving of equipment between NRAO, vendors, and Chile

Specific FY 2014 initiatives include (i) commissioning of a front end test cryostat by the FE maintenance group in Charlottesville, which will greatly enhance maintenance and optimization of the two onsite front end test systems, as well as allow for complete qualification of repaired and newly constructed assemblies; (ii) establishing long-term maintenance contracts for vendor-built modules, such as the BE Intermediate Frequency (IF) Downconverters; (iii) conducting onsite training visits by each major hardware group (BE, FE, LO, and photonics); and (iv) quantifying actual MTBFs (Mean Time Between Failures) for each major component based on observed failure rates in the initial years of ALMA operations, allowing for greater accuracy in planning maintenance support in future years. NA ALMA Offsite Software support is described in the Data Management and Software section of the Program Operating Plan. VLA Maintenance Plans and Schedules New Mexico Operations also supports over 3,300 modules, power supplies, and receivers for the VLA, VLBA, and the ALMA BE, as well as all mechanical parts in the antennas, such as motors, gears, and structural elements. Support work includes addressing the over 3000 maintenance forms generated yearly and requires engineers and technicians to investigate, diagnose, trouble shoot and ultimately resolve these reports. To this end, there is a daily maintenance meeting attended by the group leads of all electronics and engineering service personnel to review all new problem reports to assure all problems are assigned to the proper group. Older forms are reviewed to avoid stagnation of those issues and to identify recurring issues that may require an improvement or redesign of a module or procedure. Technicians are also available for after-hours callouts to address problems that seriously impact the safety of the array, such power failures, electrical problems, antennas stuck in un-safe positions. Callouts also occur if there are more than three antennas unusable for astronomy due to problems that may not be safety related, such as warmed receivers following a power glitch. Specific maintenance activities are described further below. Antennas: VLA antennas are routinely cycled through the Antenna Assembly Building for checkout and overhaul throughout the year. Under normal maintenance circumstances, up to eight antennas per year could be cycled through the assembly building. In FY 2014, several antennas will be upgraded with new control circuitry (ACU), and as such each will require roughly double the period of time given that these will be the first antennas which undergo this retrofit. In FY 2014, we plan to perform overhauls on six antennas. In addition to the mechanical work associated with the ACU upgrade, the overhaul process includes (1) structural inspections that may reveal existing and potential problems; (2) the installation of upgrades to mechanical parts, electrical systems and electronic equipment; (3) addressing maintenance


issues that require the Antenna Assembly Building resources, such as azimuth gear and bearing replacement; (4) inspecting and changing oil in gear boxes; (5) carrying out touch-up painting on the structure; and (6) repairing and replacing parts as needed. After a one year hiatus, the process of replacing one antenna azimuth bearing per year will resume in FY 2014. Preventive maintenance is conducted in the field to inspect, clean, and lubricate each antenna’s Focus Rotation Mount (FRM) and azimuth and elevation bearings. Antenna mechanics routinely check grease for metal chips on all antennas in the field so as to be alerted for potential failure of moving parts. This is especially important for the sustainability of the azimuth gears. The goal is for each antenna to undergo this maintenance every six months. The antenna mechanics will continue to respond to mechanical/structural problems that occur regularly, such as inoperative motors, water leaks into the antenna, equipment rooms, broken anemometers located on the dish lip, realigning misaligned FRMs, and addressing other antenna issues brought to their attention. The two transporters used to move the antennas during reconfigurations undergo maintenance and repair between move periods. Maintenance on the almost forty year old transporters includes servicing the motors, checking the generators that keep critical power to the antenna during a move, lubricating the moving parts, checking on the twenty-four wheel axles and wheels and maintaining electrical and hydraulic systems. Antenna mechanics also inspect the 72 concrete antenna pads to ensure their structural integrity and to measure for signs of shifting. If the tripod legs of the pad were to shift too far apart, the antenna would not be able to be bolted to the pad. Track: During FY 2014, inspection of the VLA railroad tracks will continue, checking for problems that could compromise the safety of the transporters that carry the antennas during array reconfigurations and other antenna moves. These inspections also guard against problems that could jeopardize the safety of the maintenance rail vehicles that are used by technicians to service the antennas. Maintaining track integrity requires specialized railroad repair vehicles and equipment, as well as ballast, rails and track sections. The supply of ballast purchased with ARRA stimulus funding in FY 2010 is quickly being exhausted, so a line item for this has been added back into the operations budget. The VLA track contains approximately 200,000 ties. With a nominal life expectancy of 25 years for pine railroad tie, ideally we would replace on the order of 8000 ties per year, or more given the dry conditions at the site. This task alone would require the constant attention of seven FTE over the course of a year. Given that the track crew comprises of six FTE, and that there exists other necessary maintenance tasks to keep the tracks in reasonable shape, our goal is to locate and replace only 2500 ties along the approximate 44 miles of track in FY 2014. Seventy-three intersections to antenna pads are included in the VLA Wye. As with the track cross-ties, the ties which make up these intersections must be replaced on a regular basis. Due to the complexity of rebuilding an intersection, the decision was made to replace failing intersections with fabricated concrete ties rather than wooden ones. This requires more time to accomplish than working with wooden ties, but the payoff is extended life and less maintenance. To date, approximately 10 of the 73 intersections have been replaced. Another 3 will be fabricated and replaced in FY 2014. Site Infrastructure: The VLA site buildings, utility systems, and grounds will continue to undergo routine annual inspection and preventive maintenance in FY 2014. This includes annual road grading; roof repairs; heating and cooling systems maintenance; pest and weed control; fire brigade and emergency medical response team training; and the routine servicing of gas pumps, sewer and water


supply systems, backup generator power, electrical lines, switches, and transformers, and other related systems.

In FY 2014 a plan will be developed to recommend the best course of action to take for the site’s original VAX building, which used to host the VLA VAX computing resources. This building, also referred to as the Scientist and Library office building, also held the VLA library books and some scientific staff offices. After the DSOC was built in 1988, this building was repurposed for storage and the track crew, and later the fiber group. These two groups now have new homes in the cold storage bldg (track) and the VLA control bldg (fiber), leaving this building empty. Also, a campaign will be carried out to replace the failing transformer which supplies the VLA Activity Center, Visitor’s Center, and soon to be decommissioned ALMA Test Facility.

In addition to the telescope facilities on site and managed from Scocorro, New Mexico hosts a number of other facilities such as an instrument shop which provides support for all NRAO telescopes and projects. A small motel-like lodging, operated by NRAO on the New Mexico Technical University campus, is available for use both by all site visitors. The NRAO VLA Visitors’ Center, is located at the VLA site and contains an exhibit hall, auditorium, and gift shop open to the general public. Vehicle Support: The VLA continues to operate more than 50 vehicles and heavy equipment items, such as forklifts, cranes, loaders, tampers, backhoes, trenchers, and buses. Many of these are used daily and will continue to be routinely serviced and repaired to remain in safe, efficient working condition through FY 2014 and on. Electronics Division Support: In addition to the upgrade projects described above, the New Mexico Electronics Division is responsible for maintaining all VLA electronic components and the WIDAR Correlator. Routine work for FY 2014 will consist of the following:

• Overhaul at least 30 receiver cold heads per quarter to keep FEs operating. • Replace Low Noise Amplifiers (LNAs) in 12 L-Band receivers (one per month) to correct wire

bond breakage problem. • Recondition and replace receiver desiccant in each of 240 units twice per year. • Perform preventive maintenance on 25 VLA compressor lines twice per year. • Overhaul two EVLA compressors due to normal wear-and-tear. • Perform preventive maintenance on four helium circuits to maintain cryogenic performance. • Repair and replace 24 FE receivers per year. • Perform checks on the Correlator boards, replace as needed. • Perform checks of the fiber optics system to ensure proper operations, reset as needed. • Build 20 fiber optic cables for the Computing Division and replace 20 fiber optic cables on the

EVLA antenna infrastructure per quarter. • Investigate issues with locking, fringing, output power, and general communication dropouts. • Perform routine power supply and battery maintenance. • Retrofit upgrades or additions to enhance equipment safety. • Perform bench work on modules for repair or assembly. • Monitor modules responsible for array timing, adjusting as needed. • Perform maintenance on ACUs and FRM controllers. • Replace 10 SCR driver cards in the VLA antenna servo cabinet. • Maintain monitor for local radio frequency interference (RFI) at the VLA site. • Swap out the site weather station twice yearly for preventive maintenance.


RFI Mitigation: Plans for reducing and mitigating RFI for FY 2014 include:

• Reduce or eliminate high frequency and very high frequency RFI originating from Transporter Building florescent lighting. Current lighting interferes with the VLA low band observing and Long Wavelength Array (LWA) observing.

• Re-enable the W8, L-Band automated spectrum monitor. The legacy W8 monitor was found to produce ripples in the L-Band spectrum during early EVLA observations and was disconnected.

VLBA Maintenance Plans and Schedules The VLBA is approaching the twentieth anniversary of the end of its construction phase. Some critical components are becoming more problematic as they reach the end of their normal lifespan. These items include the masers, the azimuth track and the grouting, elevation bearings, and rust problems at the Hancock and Saint Croix sites. Maser issues are likely to continue in 2014 – two masers failed in FY 2013. Symmetricom, the supplier of these masers, will only consider repair of the newer models, and not the older ones. We are currently renting one maser and will probably rent another in FY 2014. One of the two failed masers is repairable, but the other cannot be repaired. The Saint Croix and Hancock sites, due to their local weather conditions, will soon require extensive re-painting to control rust on the structure. The local technicians perform spot painting on areas showing signs of rust, but more extensive painting is likely to be needed at some point. The grout on the rails of the azimuth track deteriorates with time and typically one antenna per year has needed re-grouting, patching of the concrete, and/or replacement of the rail, making it probable that this may be needed in FY 2014. Other electronic components are also on the verge of becoming unsupportable due to obsolete repair parts and/or incompatibility with recent electronic updates. Those potential failures that pose the most serious risk to operations are being addressed through upgrade projects. Antennas: In FY 2014, the North Liberty and Hancock VLBA stations are scheduled to receive major maintenance visits by the VLBA Tiger Team comprising personnel from the antenna mechanics and servo groups. The number of visits will remain at two per year for FY 2014 (compared with three per year in FY 2012 and earlier) in order to reduce operations costs. We will continue to monitor the impact of the reduced Tiger Team visits to VLBA stations. The Tiger Team will inspect, repair, and upgrade mechanical and electronic components, as needed. Gears will be greased and checked for early signs of potential failure, and elevation bearings checked. Most, if not all, of the VLBA antennas will likely need both elevation bearings replaced over the next five years. Detailed descriptions of past VLBA Tiger team tasks are documented in the Antenna memo series available on the VLBA web site. Electronics Division Support: Each VLBA antenna contains eight cooled receivers, two compressors and numerous other electronics components. Although some of these components are supported in the Socorro labs, for efficiency, many are sent to the 20 VLBA site technicians for repair and maintenance. In FY 2014 sites technicians will continue to carry out the bulk of the routine maintenance tasks of:

• Inspection and lubrication of FRM, Az/El drive motors, encoder and pintle bearings, elevation gears, elevation hoist, change gearbox oil, etc.

• Check/test encoder motor tachometers, servo limits, ACU, vacuum pumps, all HVAC systems, dry air system, weather station equipment, etc.

• Ensure safety equipment such as UPS’s and generators, emergency power, fire alarm systems, fire extinguishers, security systems, etc. are operating normally.


• Ensure all other preventive maintenance tasks such as checking motor brushes and commutators are checked and replaced, check of Azimuth wheel position, check for metal in grease samples, cable wrap maintenance, replace oil filters, etc., completed in a timely fashion.

• Repair some VLBA specific modules to relieve some of this task from the technical staff at the DSOC and the VLA sites.

• Maintain the grounds and building infrastructure. • Other diagnostic and repair tasks as needed.

Other tasks performed by the Electronic Division personnel include support for the FEs. Because some of the VLBA receivers still use old-style LNAs (e.g., S-Band) that are no longer serviced by CDL, occasionally an entire receiver may have to be rebuilt with new LNAs in order to maintain full operational functionality. The Division is also responsible for the repair of 24 VLBA recording and playback modules, and repairs 100 Mark 5 disk packs per year. The maser lab is also part of the Electronics Division. It is currently in need of modernization, and NRAO will develop a plan for addressing the long-term support of the VLBA and VLA masers during FY 2014. RFI Mitigation: RFI mitigation efforts in FY 2014 will address the Brewster, WA 6cm RFI problem by working with the “USEI-Teleport” engineers to reduce the effects of their 6676 MHz satellite uplink signal on VLBA-BR C-Band Methanol line observing. GBT Maintenance Plans and Schedules Track replacement/repair: The GBT track is now ten years old and is showing signs of wear. Beginning in FY 2014 NRAO will, on an annual basis, be replacing those GBT track pieces which show significant wear. Telescope painting: Painting of the GBT is necessary to preserve the overall integrity of the structure. In FY 2014 we will continue our annual painting efforts at roughly the same levels as in FY 2013 and FY 2012. Green Bank Radio Frequency Interference Mitigation: Working with colleagues from the federal Sugar Grove, WV facility, NRAO will continue to administer all FCC applications within the National Radio Quiet Zone. NRAO also monitors the West Virginia Radio Zone, a ten mile radius around the GBT. NRAO will continue looking for potentially harmful interference and working with the community to find solutions for their needs which do not impinge upon GBT observers. Finally, in FY 2014 NRAO will be increasing efforts to eliminate internally created RFI on the Green Bank site, bringing an additional engineer into the interference protection group. Digital Servo Replacement: The original analog servo system for the GBT is out-dated and difficult to maintain. It is being replaced by a digital servo system that will provide the platform for model-based servo control, allowing for significantly improved telescope pointing and motion. The servo replacement is being run as part of operations and will continue in FY 2014. GBT and other telescopes: Ongoing telescope front-end and back-end maintenance will continue routinely in FY 2012, including cold-head and compressor maintenance for the cryogenic receivers, repair of failed parts in the front ends, servo and LO-IF systems, and the maintenance and repair of fiber optic connections. Antenna mechanics also check grease for metal chips, on the GBT and all other


antennas, in the field to be alerted for potential failure of moving parts, especially azimuth truck bearings and elevation gears and bearings. Other telescopes: The 43m telescope is operational and being prepped for the RadioAstron contract, which will operate through 2015. The 20m telescope is operational and supports the University of North Carolina's SKYNet project through 2013. The 45' is operational and supports the Solar Radio Burst Spectrometer through 2013. The 40' is operational, supporting education. Big Horn is operational and needs repair but is only used for special events. Reber and Jansky are both operational and only used for special events. PAPER is operational, funded from an NSF grant. The Magnetometer is operational, funded by WVU. The following telescopes are in stasis: 85-1, 85-2, 85-3. Site Infrastructure: The GB site buildings and grounds will continue to undergo routine annual inspection and maintenance in FY 2012. This includes annual road repair and winter plowing; roof repairs; heating and cooling systems maintenance; pest and weed control; servicing of sewer systems, water supply, backup generator power, HVAC systems, electrical lines and related systems. Road repair, maintenance, and plowing (as needed): The GB site owns and maintains all roads within its boundary, and is therefore responsible to repair all damage and keep the roads clear for proper use and, most importantly, for the passage of emergency vehicles when necessary. To that end, the maintenance group is responsible to repair all road damage caused by accident or weather extreme, and plow the roads of snow in the winter. Proper maintenance of the roads has kept them in outstanding shape over the course of the last 50 years with minimal outlay of funds for replacement. These activities are required to ensure the GB site and the GBT remain in a current state of repair. Vehicle Support: The GB site continues to operate more than 65 vehicles and heavy equipment items, such as loaders, dozers, backhoes, trenchers, tractors, mowers, fleet vehicles, and buses. All of these are used daily and will continue to be routinely serviced and repaired to remain in safe, efficient working condition through FY 2012 and onward. CDL & HQ Maintenance Plans and Schedules The Edgemont Road facilities are leased from University of Virginia (UVa) and therefore all maintenance and repair is handled by their internal facilities engineering department. They follow a preventative maintenance schedule and respond to emergency requests as needed. The NRAO Technology Center (NTC), where the Coordinated Development Laboratory and NRAO production is housed, is leased and maintained through a private leaseholder agreement and maintenance and repairs are subject to the provisions of the agreement.


APPENDIX D: FY 2013 ANNUAL PROGRESS SUMMARY

Quarterly Status Update (April – June 2013) Table 1of 6


Quarterly Status Update (April – June 2013) Table 2 of 6










Quarterly Status Update (April – June 2013)

FY13 YTD by Major WBS Category ALMA Ops

FY13 POP Budget

FY13 YTD Expenses YTD %

Telescope Ops 20,263 18,092 89.3

Development 2,992 3,008 100.6

Science Ops 5,363 3,902 72.8

Admin Services 5,045 3387 67.1

Director’s Office 2,291 1,635 71.4

Total 35,954 30,024 83.5

FY13 YTD by Major WBS Category NRAO Ops

FY13 POP Budget

FY13 YTD Expenses

YTD %

Telescope Ops 16,793 13,445 80.1

Development 4,056 3,802 93.8

Science Ops 6,414 5,240 81.7

Admin Services 13,944 9,643 69.2

Director’s Office 4,545 3,282 72.2

Total 45,752 35,413 77.4


APPENDIX E: WORK FOR OTHERS

Green Bank Operations RadioAstron Earth Station: In FY 2013 the 43m diameter telescope was refitted for operation as a down link (Earth) station for the Lebedev Institute’s RadioAstron science satellite. Operation as an Earth Station continues through FY 2014. Staffing for this project is primarily through staff would otherwise not be funded through the AUI-NSF cooperative agreement. PAPER: The Green Bank facility is the Northern site for the PAPER telescope, the HERA prototype run by a partnership that includes UC Berkeley and the University of Virginia, which also operates an identical array in the Karoo desert of South Africa. This project is staffed and run through the University of Virginia. Low Frequency All-Sky Monitor Project: LoFASM is a University of Texas, Brownsville project to which will consist of four phased dipole arrays, separated by several thousand kilometers. One of its first arrays was installed on the Green Bank site in FY 2013 and the instrument is now operational. This project is staffed and run through the University of Texas. MEASURE: West Virginia University has installed a magnetometer on site as part of the University of California led Magnetometers along the Eastern Atlantic Seaboard for Undergraduate Research and Education (MEASURE) project to study magnetosphere dynamics. This project is staffed and run through the West Virginia University. West Virginia Geospatial Information Network: A reference GPS sensor for the West Virginia Geospatial Information Network is installed on site. This project is staffed and run through the State of West Virginia. Central Development Laboratory Components for ALMA Band 1 Construction: East Asia is leading the construction of the full complement of Band 1 (35-52 GHz) receivers for ALMA. As part of an ALMA Downselect Review in January 2013, it was decided that the Band 1 receivers should use the low-noise amplifiers and local oscillator subsystem developed by the CDL. The construction of these items is being treated as a work for others contract with the Academia Sinica Institute of Astronomy and Astrophysics (ASIAA) as the customer. Full production of the LNAs is planned to begin in FY 2014 and extend through FY 2016. ALMA Phasing Project: This is a continuation of a MIT Haystack Observatory led project to demonstrate the use of ALMA as a millimeter-wave VLBI station. The CDL is responsible as a subcontractor to Haystack to provide a set of upgrades to the ALMA correlator to phase and sum inputs from all basebands of up to 64 antennas. The CDL digital group has also accepted some system-level assignments as part of the initiative including system level documentation and hosting the integration tests. During the past year, the project successfully passed both PDR and CDR. During the coming year the plan is to produce the required hardware, microprocessor software and FPGA personalities required to complete the project. NRAO will also lead the system integration effort in Charlottesville. The hardware will likely be assembled and tested by the second quarter of FY 2014 and the integration tests in Charlottesville will likely be complete by the third quarter of FY 2014. This effort has been underway since 2012 and uses a portion of the CDL Digital Group’s resources not allocated toward Program Plan activities.


Data Management & Software Department ALMA Phasing Project: The APP funding has been applied in such a way (additional personnel employed for a term position) in such a way that it will have no net impact on the ALMA System (M&C) groups available effort. That is, the effort expended by existing staff members will be replaced through the addition of a term position. USNO DiFX correlator: USNO has contracted with NRAO to supply an additional 32 node extension to the delivered Phase-I 32 node DiFX correlator to be delivered in Q1 FY 2014 with maintenance and support provided through Q2 FY 2014. A request to extend support through Q4 FY 2014 is expected. In FY14 the support for this project is expected to be low, and will not affect any deliverables enumerated in this document.


APPENDIX F: ACRONYMS

Acronym Definition AAAS American Association for the Advancement of Science AAS American Astronomical Society AAT Archive Access Tool ACCOR ALMA Construction Completion and Operations Readiness Review ACU Antenna Control Unit AD Assistant Director ADSC ALMA Development Steering Committee ALMA Atacama Large Millimeter/submillimeter Array AOD Astronomer on Duty AOS Array Operations Site (ALMA, Chile) API Atmospheric Phase Interferometer APP ALMA Phasing Project ARC ALMA Regional Center ARRA American Recovery and Reinvestment Act ASA ALMA Science Archive ASAC ALMA Science Advisory Committee ASIAA Academia Sinica Institute for Astronomy and Astrophysics ASKAP Australian SKA Pathfinder ATI Advance Technologies and Instrumentation AU Astronomical Unit AUI Associated Universities, Incorporated BE Back End BYU Brigham Young University CAP Contracts and Procurement CARMA Combined Array for Research in Millimeter-wave Astronomy CASA Common Astronomy Software Applications CBI Cosmic Background Imager (CBI) CCA Cold Cartridge Assembly CCB Caltech Continuum Backend CCE Common Computing Environment CDE Community Day Events CDL Central Development Laboratory CDR Critical Design Review CfP Call for Proposals CIS Computing and Information Services cm Centimeter C0, C1, C2, C3 ALMA Cycles CoDR Conceptual Design Review COM NRAO Communications Office CORF Committee on Radio Frequencies COSPAR Joint Committee on Space Research CSA Cooperative Support Agreement CSIRO Australia’s Commonwealth Science and Industrial Research Organization CSSC CASA Science Steering Committee CSV Commissioning and Science Verification (ALMA) CV Charlottesville, VA DA Database Administrator or Data Analyst DARE Dark Ages Radio Explorer DASI Degree Angular Scale Interferometer


Acronym Definition dB Decibel DCR Digital Continuum Receiver DDC Digital Downconverter DI Digital Infrastructure DiFX Distributed FX correlator DM Data Management DMS Data Management and Software Department DO Director’s Office DOMT ultra-low-loss triangular digital OMT DOS Department of State DSO Division of Science Operations- ALMA DSOC Domenici Science Operations Center DSP Digital Signal Processing EAR Export Administration Regulations ECCN Export Control Classification Number EOP Earth Orientation Parameters EoR Epoch of Reionization EPO Education and Public Outreach ESO European Southern Observatory ES&S Environment, Safety, and Security EVLA Expanded Very Large Array Project EVN European VLBI Network FASR Frequency-Agile Solar Radiotelescope FAST Five hundred meter Aperture Spherical Telescope FCC Federal Communications Commission FE Front End FEHV Front End Handling Vehicles FEIC Front End Integration Center FET Field Effect Transistors FETIM FE Thermal Interlock Modules FFRDC Federally Funded Research and Development Centers FFT Fast Fourier Transform FIAN Lebedev Institute of the Russian Academy of Sciences FITS Flexible Image Transport System FPGA Field-programmable Gate Array FRM Focus Rotation Mount FTE Full-Time Equivalent FY Fiscal Year (1 October through 30 September) F2F Face to Face GARD Group for Advanced Receiver Development GB Green Bank, WV Gbps Giga-bits per second GBSE Green Bank Session Editor GBSO Green Bank Science Operations Center GBT Green Bank Telescope GBTIDL Interactive package for reduction and analysis of spectral line data taken at the GBT GHz Gigahertz GPU Graphics Processing Unit GUI Graphical User Interface GUPPI Green Bank Ultimate Pulsar Processing Instrument HERA Hydrogen Epoch of Reionization Array


Acronym Definition HFET Heterojunction Field-Effect Transistor HPC High Performance Computing HR Human Resources HRIS Human Resource Information System HSA High Sensitivity Array HST Hubble Space Telescope IAU International Astronomical Union ICT Integrated Computing Team IF Intermediate Frequency IFP IF Processor InP Indium Phosphide IPG Green Bank Interference Protection Group IPT Integrated Product Team ITAR International Traffic in Arms Regulations ITU-R International Telecommunication Union-Radio communications Sector IR Infrared IR (CDL) Integrated Receivers IT Information Technology IUCAF Scientific Committee on Frequency Allocations for Radio Astronomy and Space Science JAO Joint ALMA Office JD Job Description JPL Jet Propulsion Laboratory k 1,000 kHz kiloHertz KIDS Kinetic inductance detectors LAN Local Area Network LEDA NSF-funded LEDA experiment at LWA1 LIGO Laser Interferometer Gravitational-Wave Observatory LISA Laser Interferometer Space Antenna LNA Low Noise Amplifier LoFASM Low Frequency All-Sky Monitor Project LO Local Oscillator LO/IF Local Oscillator/Intermediate Frequency LRP Long Range Plan LSST Large Synoptic Survey Telescope LWA Long Wavelength Array m meter M&S Materials and Supplies Mbps Mega-bits per second

MEASURE Magnetometers along the Eastern Atlantic Seaboard for Undergraduate Research and Education

MeerKAT Meer Karoo Array Telescope MHz Megahertz MIC Microwave Integrated Circuit MIS Management Information Services MIT Massachusetts Institute of Technology mm millimeter mm/submm Millimeter/submillimeter MMIC Monolithic Millimeter-wave Integrated Circuit MOA Memorandum of Agreement MOU Memorandum of Understanding


Acronym Definition MPIfR Max Planck Institut für Radioastronomie MREFC Major Research Equipment and Facility Construction MRI Major Research Instrumentation MTBF Mean Time Between Failures MUSTANG 32-feedhorn bolometer camera MWA Murchison Wide-field Array µas Micro-arcsecond µJy microJansky MUSTANG Multiplexed SQUID/TES Array for Ninety Gigahertz NA North American NAASC North American ALMA Science Center NANOGrav North American Nanohertz Observatory for Gravitational Waves NAOJ National Astronomical Observatory of Japan NASA National Aeronautics and Space Administration Nb Niobium nHz nanohertz, a frequency of one cycle per 109 seconds (about 32 years) NIO New Initiatives Office NIST National Institute of Standards and Technology NOVA Netherlands Research School for Astronomy NRAO National Radio Astronomy Observatory NRC-HIA National Research Council of Canada - Herzberg Institute of Astrophysics NRL Naval Research Laboratory NRQZ National Radio Quiet Zone NSF National Science Foundation NSF-MRI National Science Foundation – NSF-AST National Science Foundation – Division of Astronomical Sciences NSF-ATI National Science Foundation - Advanced Technologies and Instrumentation NTC NRAO Technology Center (Charlottesville, VA) NVO National Virtual Observatory NWNH 2010 Decadal Survey “New World New Horizons” OCA Office of Chile Affairs ODP Observatory Development Programs OMT OrthoMode Transducer OPT (OSO) Observation Preparation Tool OPT (ALMA) Optical Pointing Telescope OSF Operations Support Facility (ALMA, Chile) OSO Observatory Science Operations OT Observing Tool OTO Observatory Telescope/Array Operations PA Product Assurance PAF Phased Array Feed PAPER Precision Array to Probe the Epoch of Reionization pc parsec PDR Preliminary Design Review PEP Performance Evaluation Process PF 1, 2 Prime Focus PFB Polyphase Filterbank system Ph2 SBs Phase two scheduling blocks (related to software development) PHT Proposal Handling Tool PI Principle Investigator PMD Program Management Department

http://en.wikipedia.org/wiki/Hertz


Acronym Definition POP Program Operating Plan PSC Pulsar Search Collaboratory PST Proposal Submission Tool PT Pie Town Q Fiscal Quarter QA Quality Assurance QA2 Quality Assurance, Level 2 (related to software development) R&D Research and Development RDBE ROACH Digital Backend REU Research Experiences for Undergraduates RF Radio Frequency RFI Radio-Frequency Interference RISC RadioAstron International Science Council RMS Radio, Millimeter and Submillimeter? ROACH Reconfigurable Open Architecture Computing Hardware RPI Pipeline Reprocessing Interface RSRO Resident Shared Risk Observing SAA Science and Academic Affairs SADC Strasbourg Astronomical Data Center SASPO South African SKA Project Office SB Scheduling Block SE Systems Engineering SCO Santiago Central Office SCR Silicon Controlled Rectifier SEI Systems Engineering and Integration SHAO Shanghai Astronomical Observatory SIS Superconductor–Insulator–Superconductor SKA Square Kilometre Array SMBH Supermassive Black Hole SMT Submillimeter Telescope on Mt. Graham SNR Signal to Noise Ratio SOP Standard Operating Procedure SOS Student Observing Support SPDO SKA Program Development Office SPO Special Program Office SQUID Superconducting Quantum Interference Device SRBS Solar Radio Burst Spectrometer SRO Shared Risk Observing SRP Science Review Panel SSR Science Support and Research STEM Science, Technology, Engineering, and Mathematics Sub-kpc Sub-kiloparsec submm submillimeter SUBTEL Subsecretaria de Telecomunicaciones (Chile) SUS Science User Support TAC Time Allocation Committee TBytes Terabytes THz TeraHertz TTA Telescope Time Allocation TTO Technology Transfer Office UNM University of New Mexico


Acronym Definition URSI International Union of Radio Science U.S. United States of America USEI U.S. Electrodynamics Inc USML U.S. Munitions List USNO United States Naval Observatory UTI/UTC Earth's Rotation and Reference Frames UVML University of Virginia Microfabrication Laboratory v Volt VA Virginia VEGAS VErsatile GBT Astronomical Spectrometer VLA Very Large Array VLASS VLA Sky Survey VLBA Very Long Baseline Array VLBI Very Long Baseline Interferometry WBS Work Breakdown Structure WCA Warm Cartridge Assembly WFO Work for Others (non-NSF CSA, SPO grants) WIDAR Wideband Interferometric Digital ARchitecture WMAP Wilkinson Microwave Anisotropy Probe WRC World Radiocommunication Conference WV West Virginia WVRAZ West Virginia Radio Astronomy Zoning Act WVU West Virginia University XAO Xinjiang Astronomical Observatory

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