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April 8/9, 2003 Green BankGBT PTCS Conceptual Design Review
John Ford
September 28, 2009
Casper Instrumentation at Green Bank
The NRAO is operated for the National Science Foundation (NSF)
by Associated Universities, Inc. (AUI), under a cooperative
agreement.
2
Outline
• NRAO
• Configurable Instrument Collection for Agile Data Acquisition (CICADA)– Green Bank Ultimate Pulsar Processing Instrument
(GUPPI)– West Virginia University Pulsar Processing Instrument
(WUPPI)– GUPPI - 2– Future instruments
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NRAO Mission
The (US) National Radio Astronomy Observatory enables forefront research into the Universe at radio wavelengths.
• In partnership with the scientific community, we:– provide world leading telescopes,
instrumentation and expertise,– train the next generation of scientists and
engineers, and– promote astronomy to foster a more scientifically
literate society.
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Aperture Synthesis Telescopes
• Very Long Baseline Array (VLBA)– Network of 10 telescopes spread over
United States– Resolution of a 5000 mile diameter
telescope• Highest Resolution of any telescope on
earth or in space– Sometimes the GBT becomes part of this
array• (E) Very Large Array (VLA)
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Green Bank Facilities
• 2700 Acre site in Pocahontas County– 8 Radio Telescopes on site– National Radio Quiet Zone
• 150 mile rectangle centered around Green Bank and Sugar Grove
• Provides protection for the sensitive receivers on the telescopes
– Green Bank Science Center
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Panoramic View of Green Bank Telescopes
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CICADA
• Configurable Instrument Collection for Agile Data Acquisition– FPGA based data acquisition and
processing– Uses CASPER tools and hardware
• Umbrella program for organizing FPGA projects– Purchase/obtain boards, software, development systems– 3 ROACH, 2 BEE2, 5 iBOB, 6 ADC, 3 ADC-2, 10 GbE
switches, servers, etc.
CICADA People
• GUPPI– Randy McCullogh, Jason Ray , Patrick Brandt, Ron Duplain,
Paul Demorest, Scott Ransom• WUPPI/43 meter stuff
– Shilpa Bollineni, Glen Langston, Paul Demorest– WVU Folks
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CICADA Projects
• Spectrometer Proposals– KFPA backend– Replacement for GBT Spectrometer
• Event capture machines– Used for transient events
• Pulsar machines– Incoherent machine (GUPPI, WUPPI)– Coherent dedispersion machine GUPPI-2
GUPPI
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Sampler( iBOB)
GUPPI BEE2 XAUI alignment
GUPPI BEE2 XAUI alignment
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GUPPI BEE2 signal processing design
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GUPPI BEE2 signal combining FPGA
beef.gb.nrao.edu
*.nrao.edu
GUPPI command prompt
Python SOAP client
GUPPI GBT M&C Manager
C++ SOAP client
GUPPI Software Overview
100 MbE 10 GbE
Ethernet
XAUIout-of-bandcontrol bits
equipment
BEE2
runs guppi controller on Debian + BORPH O/S
IBOBs
no custom controller software
ADCs
Clock Synthesizer
Power Strip
clock input
power
XAUIGBT IF
telnet over Ethernet
telnet over Ethernet
systems control signals data streams notes/comments .
guppi_daq
threads:• net• disk• fold (for folding mode)will also run on GPU nodes in GUPPI Phase II
guppi controller
modules:• DAQ• POWER• SYNTH• BEE2 guppi_statusd
gets GBTStatus
shared memory
Unix socket
shared memory
GUPPI Status
• Currently available GUPPI Modes– 128 to 4096 channels– 2 polarizations– 100 to 800 MHz bandwidth– Full Stokes or Total Intensity Only– Decimation in frequency and time in CPU– Records up to ~250 MB/S continuously– Disk space is a considerable problem
• Fully integrated into the GBT Observing System
GUPPI's Advantages
Searching: 800MHz of BW, 4096 chan, and RFI-resistance (from polyphase filterbank) will make GUPPI a “Super-Spigot” that will be unbeatable for searches from 1-5 GHz (previously the BCPM and Spigot)
High Dynamic-Range Studies: 8-bit sampling, high spectral resolution and Full Stokes will make GUPPI perfect for scintillation studies, HI absorption, Faraday rotation measurements, polarization studies, and singlepulse studies (previously the Spectral Processor)
Ultra-High Precision Timing: 8-bit sampling, 800MHz of BW, and RFI resistance will allow unprecedented timing precision from 1-3 GHz for millisecond pulsars (i.e. the NANOGrav project and the search for nHz gravitational waves; previously GASP/CGSR2)
GUPPI-2
• Uses GUPPI to feed a 9-machine cluster of GPU’s via 4 10 GbE ports.
• 128, 256, or 512 coarse channels will be supported• 100 MHz processed per GPU at “reasonable” DM’s.• Only modification to GUPPI is a new output FPGA
personality and software to control the nodes
GUPPI-2 experiments
GUPPI-2 Experiments
WUPPI Crab Pulsar Data
Future Projects
• Not funded, but…– K band Array receiver spectrometer– GBT Spectrometer Replacement– Transient searches on old telescopes (like fly-eye, with bigger
and fewer dishes)– Lunar Neutrino project
• Several 43m projects:– WUPPI– Receiver project
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K band Feedhorn Array Spectrometer
• 7 pixels, dual polarization– 21 ROACH boards, 14 ADC's – Needs to be in receiver room
• 3 GHz bandwidth• Cross correlation between polarizations on a single
pixel• “Zoom” mode for multiple narrow windows in a
bandpass• Fast dump mode for pulsar use on a few polarizations• Normal dump times of 1 ms
Array Spectrometer design
Reconfigurable Open
ArchitectureComputingHardware
Reconfigurable Open
ArchitectureComputingHardware
Front-endElectronics
Reconfigurable Open
ArchitectureComputingHardware
IF 0
Pixel 0
Pixel 1
Pixel 7Pixel 6
Pixel 5Pixel 4
Pixel 3Pixel 2
Front-endElectronics
IF 1
10 Gb Switch
10 GB X 210 GB X 2
10 Gb Switch
32 Core Pipeline Processor
Disk Controller
Disk Controller
Dual10 GbLinks
Fibers FromGBT
40 TB
40 TB
Up to 500 MB/sec to disks,
sustained
Fibers To Jansky Lab Equipment
Room
Signal Processors
Signal Combiner/Accumulator
To existing GB Network infrastructure
43m Receiver and Spectrometer
The End
• Summary:– GUPPI is working well
• Designs available for distribution in unadorned form now (version 7.1 right now)
• Plan to submit the FPGA designs, software, and hardware designs to the CASPER wiki