Post on 30-Jul-2020
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TIFR Facilities - Ground, Balloon, Space
Devendra K. OjhaTata Institute of Fundamental Research
(TIFR), Mumbai
Workshop on Science with Subaru: An Indian Perspective 20 December 2019TIFR, Mumbai
Instrumentation related work (TIFR-DAA)
X-ray:
● Three instruments (LAXPC, SXT and CZTI) being fabricated for ASTROSAT satellite. ASTROSAT was launched on 28 September 2015.
Infrared:
● Development of the Laboratory Model of Infrared Spectroscopic Imaging Survey (IRSIS) payload for an Indian Satellite is successfully completed and the final reports have been submitted to ISRO.
● Science observations with TIFR Near Infrared Imaging Camera-II(TIRCAM2) on 3.6m Devasthal Optical Telescope (DOT).
● TIFR Near Infrared Imager and Spectrometer (TIRSPEC) for 2-meter HCT at Hanle (Ladakh) was developed and thrown open to general astronomical community from May 2014.
● Fabrication of TIFR-ARIES Near Infrared Spectrograph (TANSPEC) is completed and first light with 3.6m DOT was achieved on 12 April 2019.
Scientific Ballooning:
● TIFR Balloon Facility at Hyderabad has been conducting stratospheric balloon flights for research in Astronomy for more than five decades.
X-ray Astronomy - ASTROSAT (Launch: 2015 September 28)
Laboratory and POCs -both engaged in helping students and post-docs to analyze AstroSat data and to write proposals –directly and via IUCAA.
AstroSat Results (LAXPC, CZTI, SXT, UVIT) (Calibration, GRBs, HMXBs, BHs, SNR, GCs..…)
Since launch several refereed and conference proceedingspapers have been published; many more under review / submitted / under preparation
Four years of AstroSat (28 September 2019) - Data from AstroSat have resulted in so far 85 scientific papers (02 Dec 2019) in refereed journals
IR Astronomy Activity @ TIFRBalloon based Ground based
Satellite based5
Ground-based IR Astronomy Space-based IR Astronomy
TIRCAM2
@ 3.6m DOT
TIRSPEC
@ 2m HCT
TANSPEC
@ 3.6m DOT
Science
observations
in progress
Science
observations
are continuing
and plans to
upgrade the
FPA during
2020 – 21
Commissioned
on 3.6m DOT
in the second
quarter of
2019
Ongoing Ongoing Exploratory
IRSIS
Lab Model
T100
Balloon
Borne +
FPS
IR payload
for L2 orbit
Completed
and report
is submitted
to ISRO in
April 2018.
PDR is
scheduled in
early 2020
[C II] 158
µm line +
[Si II] 34.8
µm line
survey
using
5 x 5 Si:Sb
array
(future)
Overview - IR Instrumentation
Proposal
(MISS) is
submitted
to ISRO in
April 2018.
Concept
design is in
progress.
Development of Multi-Object Infrared
Spectrometer (MOIS, 2017+) – MP (PI)
Infrared Astronomy from Space
Spectroscopic Survey at 1.7-6.4 µm covering > 50% ofthe full sky (within 2 years) including the Galactic plane;(to shallow but uniform depth; low resolution R ~ 100);
Infra-Red Spectroscopic Imaging Survey (IRSIS) Experiment - a payload for an Indian Satellite
Key Science Goals for IRSIS:
(1) Detection of several broad spectral features & strong lines due to the Interstellar Gas and Dust components of the Interstellar Medium (ISM) of our Galaxy(PAH, H2O, CO2, …; Hydrogen recombination lines, ….)
(2) Classification of stellar populations in the Galaxy(based on seamless infrared spectra)
(3) Complete census of Low Mass objects in the Solar neighbourhood (~30 pc) (BDs characterized by molecular bands)
Target of Opportunity (ToO) class of studies (Time Critical Phenomena : Nova outburst spectra; etc)
Summary of the proposed instrument (IRSIS):(driven by ISRO’s constraints on size, mass, power)
Wavelength coverage : 1.7- 6.4 µm [2 channels]Sky coverage : ~ 70% (ecliptic latitude, |β| > 45 deg) Angular resolution : 18”Spectral resolution, R = (λ/∆λ) ~ 100-120 [Moderate]
Medium size telescope : ~ 30 cm (dia) @~100KInstantaneous FoV : 15’ x 15’
(9 sub-fields - 5’x5’, each feeding one slit)
Survey Sensitivity (3-σ, 10 sec) –Point source : @ K (2.2 µm) = 14 mag. (@L ~ 13)Diffuse emission :
SW (1.7-3.4 µm) ~ 0.4 MJy/SrLW (3.2-6.4 µm) ~ 1.5 MJy/Sr
Confusion limit : 2,500 stars/sq. deg.
Spectroscopic Imaging : Topology -Telescope focal plane Slit detector array
Simultaneous spectra from all sub-areas (fibers) of sky !
(no moving parts !)
Telescope
Spectrometer
Micro-lenses + Infrared fiber-bundles couple Focal Plane to multiple slits of 2-channel spectrometer :
Channel SW : 1.7—3.4 µm;Channel LW : 3.2 – 6.4 µm;
Optical components for dispersion (Grating)
Cooled (~ 80 K) detector arrays :1024x1024 (2k x 2k in LM) HgCdTe (H1RG x 2)
IRSIS Lab ModelComponents
IRSIS Laboratory Model (test setup) ….
IRSIS PDR planned in early 2020
Mid-Infrared IFU Spectroscopy Satellite (MISS) for the L2 Orbit
Department of Astronomy and Astrophysics, TIFR
Concept Design
we also plan this design as a path finder for an actively cooled future larger L2mission.
2018+ (After IRSIS)
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To conduct a comprehensive mid-IR (2.5 to 5 µm) spectroscopic survey of selected star forming regions to study the evolution of protostars, protoplanetary discs, formation of planetary systems and the origin of Oort cloud and icy comets, as well as the interstellar medium.
To obtain the largest catalog of mid-IR, multi-epoch medium resolution (R ~ 1200) spectra of young stars in star forming regions.
The 2.5 to 5 µm band not only contains numerous water and methanol ice bands, but also contains strong absorption bands of CO, CO2, OCN etc - all these molecules trace fundamental chemistry of the ISM and more specifically of protostellarenvelopes and protoplanetary discs
Complementary information on the gas chemistry from ALMA observations and TMT.
Scientific Objectives (Summary)
MISS Spectrograph (Overall Concept Design)
Wavelength coverage (λ): 2.5 - 5.0 µm
R ~ 1200 (target) Field of View (FOV) ~
6’ X 6’ Spatial resolution ~
2” (target)
We now have designs for both 50 cm as well as 150 cm primary which can be further developed depending on the availability of the platform for the L2 mission.
Spectroscopic Capabilities AKARI Spitzer
Imaging
Spectroscopy
5
AKARI (68.5 cm) – 2006 - 2011
Spitzer (85 cm) – 2003 – 2018 cont [now in “warm” mission – MIR Imaging (3.6 µm and 4.5 µm) by passive cooling @35K]
IRSIS
MISS: R ~1200 (2.5 – 5 µm)
---MISS---
MISS Status - Presentation made during review meeting held in ISRO HQ during July 05-06, 2018. Close-out report submitted on 15 Oct 2018. Submitted as inputs for "VISION DOCUMENT" for Space Sciences in India (ISRO) (Nov 2019)
Infrared Astronomy from Ground
TIRCAM2 on 3.6m DOT(2018+) 1 – 3.6 µm
512 x 512 InSb
TIRCAM2 on 2m IGO (2004+)
TIRSPEC on 2m HCT(2014+)
1 – 2.5 µm1024x1024 HgCdTe(HAWAII-1) PACE
TANSPEC on 3.6m DOT(2019+) 0.55 – 2.5 µm(simultaneous coverage from optical to NIR)H2RG (2048 x 2048)
Multi-Object Infrared Spectrometer (MOIS)IR group @DAA, TIFR
To initiate developmental activities (concept development, design and fabrication of sub-assemblies) toward building a multi-object (multi-slit) spectrometer for a large aperture telescope such as 10-meter class national large optical/IR telescope (NLOT) and the TMT
First build a prototype for the 3.6 m DOT
P. Manoj (PI)
Multi-Object Infrared Spectrometer (MOIS)
1. Configurable multiple slits
Testing out Peizo walking drives to control slit movements at cryogenic temperatures
Courtesy: MOSFIRE
Piezo Walker movements under test
Multi-Object Infrared Spectrometer (MOIS)
2. Preliminary Optical Design
Optimized for K-band
Multi-Object Infrared Spectrometer (MOIS)
3. Detector & associated electronics
• H2RG IR array as detector. • Plan to develop the readout electronics ourselves• Currently running various tests on ARC controllers &
video cards• Procured an H2RG ROIC for further tests.
Teledyne H2RG Focal Plane
Array
TIFR-Japan Collaboration
Space-based (Balloon-borne & Satellite) – since 1996
Prof. Hidehiro Kaneda (Nagoya University)Dr. Shinki Oyabu (Tokushima University)Dr. Toyoaki Suzuki (Nagoya University)Dr. Takehiko Wada (ISAS-JAXA)Prof. Takao Nakagawa (ISAS-JAXA)
Ground-based (2.2m UH, 1.4m IRSF, 8.2m Subaru, KISO Schmidt) - since early 2000
Prof. Motohide Tamura (ABC/NAOJ & Univ. of Tokyo)Prof. Katsuo Ogura (Kokugakuin University)Prof. Suji Sato (Nagoya University)Prof. Naoto Kobayashi (University of Tokyo & KISO)
TIFR 100 cm
Balloon Borne
Far Infrared
Telescope
Primary : 100 cm
aluminium ;
Mass ~ 850 Kg
No. of launches
: 26 (since 1983)
“T100” payload on Launch Arm
Final map
resolution
~ 1.0 arc min
(@ 200 mm)
Robust signal
processing & image
processing scheme
FIR Astronomy using balloons (TIFR-Japan Joint Collaboration)
http://web.tifr.res.in/~bf/
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India-Japan collaborative research based on [C II] balloon-borne experiments using the TIFR telescope & Japanese spectrometer
Fabry Perot Spectrometer (FPS)(Developed at ISAS & Nagoya Univ, Japan & adapted for T100)
Spectral Resolution (R) ~ 1800 (~170 km/s)Spectral scanning range ~ 63.2 – 63.5 cm^-1(157.41 µm – 158.57 µm)
Stressed Ge:Ga photoconductor(Spectral Response)
Scanning Fabry Perot
Basic configurationof the FPS
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Tuned to [CII] line at 157.7 µm
Spatial Resolution - 1.0’
Detection Limit (3-σ) –~ 1 x 10-4 ergs s-1 cm-2 sr-1
TIFR-BF, Hyderabad
TIFR 100-cm + FPS ([C II] 158 µm) (25-Nov-1999,25-Nov-2001, 30-Mar-2003, 15-Nov-2004, 21-Nov-2006,05-Feb-2009)Last 4 T100+FPS flights(18-Feb-2017, 30-Nov-2017, 18-Mar-2018 and 28-Oct-2018)Next IR balloon Campaign: March-April 2020
(W3, RCW36, NGC2024, Mon-R2,
Carina, NGC6334, NGC6357, W31,
RCW106, W40)
Scientific Outcomes
W31
Herschel T100-FPS Herschel T100-FPS
Carina NGC 6334
Herschel T100-FPS
“Large-scale mapping of the massive star-forming region RCW38 in the [CII] and PAH emission”, H. Kaneda, T. Nakagawa, S.K. Ghosh, D.K. Ojha, et al., Astronomy & Astrophysics, Volume 556, id.A92, 9 pp (2013)
[CII] map of RCW36
Contours: [CII]
• Large-area [CII] maps of Galactic star-forming regions
“[CII] emission properties of the massive star-forming region RCW 36 in a filamentary molecular cloud”, T. Suzuki, S. Oyabu, S.K. Ghosh,
D.K. Ojha, et al., Astron. & Astroph. (Under Review) (2019)
Good spatialcorrelations
Images: dust emission froma) Very cold dust,b) Cold dust,c) Warm dust,d) PAHs
(a) (b)
(c) (d)
30 arcmin 30 arcmin
Future T100-FPS experiments・Background
IR: filamentary gas structures connecting star-forming regions.Radio: gas collisions for massive star formation.
・Science goalStudy of gas geometry and dynamics probed with [CII] in star-forming regions to directly reveal the relation between gas collisions and star formation and thus to answer the long-standing question.
→ No direct evidence of gas collision induced star formation.
How are dense gas clouds collected to form massive stars?
Gutermuth+2008
Filament-filament gas collisions?Serpens South
NIR+MIR Sub-mmHill+2012
Nakamura+2014
Upgraded FPS aboard T100・Requirements from the science goal
2) Measure gas dynamics due to collisions → Spectral resolutions of R≧10,000
1) Resolve filamentary gas geometries → Spatial resolution of ≦40”
Tra
nsm
itta
nce
New Fabry-Perot spectrometerwith R=10,000
State-of-art FIR detector array (25 pixels)
First practical application in the world
・Development of key components
Upgraded T100(electronics)
BIB-TypeGe detectorArray
UH 2.2m / IRSF 1.4m + SIRIUS/SIRPOL
Ojha, Tamura, et al., ApJ, Volume 608, Issue 2, pp. 797-808 (2004)
Ojha, Tamura, et al., ApJ, Volume 616, Issue 2, pp. 1042-1057 (2004)
Ojha (+Tamura), et al., PASJ, Vol.57, No.1, pp. 203-210 (2005)
Sanchawala (+Ojha, Tamura), et al., ApJ, Volume 667, Issue 2, pp. 963-979 (2007)
Samal (+Ojha, Tamura), et al., ApJ, Volume 714, Issue 2, pp. 1015-1036 (2010)
Ojha (+Tamura), et al., ApJ, Volume 738, Issue 2, article id. 156, 18 pp. (2011)
Mallick (+Ojha, Tamura), et al., ApJ, Volume 759, Issue 1, article id. 48, 19 pp. (2012)
Vig (+Ojha, Tamura), et al., MNRAS, Volume 440, Issue 4, p.3078-3090 (2014)
Mallick (+Ojha, Tamura), et al., MNRAS, Volume 447, Issue 3, p.2307-2321 (2015)
Multi-wavelength studies of Galactic star-forming regions (with Motohide Tamura)
Since August 2003 and continuing……
Subaru 8.2m + CISCO (Cooled Infrared Spectrograph and Camera for OHS)
Subaru Press Release (January 29, 2009)
“Subaru Head Count of Low-mass Stars in W3 Main”https://subarutelescope.org/Pressrelease/2009/01/29/index.html
● Ojha, Tamura, et al., ApJ, 693, 634 (2009) – W3 Main
● Mallick, Ojha, Tamura, et al., MNRAS, 443, 3218 (2014) – NGC 7538
Young Brown Dwarfs in the Core of Star-Forming Regions
with Motohide Tamura
Summary● The IR group at TIFR has active IR instrumentation and observation programs. Access to SUBARU telescope will greatly complement and expand the scope of these programs.
● TIFR may contribute by technical development (in-kind contribution)
-IR detector readout electronics-Detector characterisations - CCDs as well as NIR H2RGs -Fabrication of opto-mechanical components-Optical fibre related expertise, like polishing, splicing, FRD measuring, testing etc..-Optical design, Cryogenic systems
● Some data reduction techniques might be common among IRD-Subaru and TIFR IR spectrometers (e.g. TANSPEC).
The above expertise can naturally be extended to TMT instrumentation
Hands-on experiences for students & young researchers to develop instrumentations
Developing IR spectrometers for balloon-borne & ground-based telescopes (e.g. Subaru). Testing satellite-borne instruments. Experiments & observations in the international environments.
FPS100 in India
SUBARU (future……….)
● Large number of Japanese students were trained for T100-FPS and J50 balloon programs
● Similarly, training of Indian students can be achieved using Subaru
Thank You