tifr facilities - ground, balloon,...

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)

13

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


2. Preliminary Optical Design

Optimized for K-band


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/

23

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

24

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

tifr facilities - ground, balloon,...

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