GTC instrumentation plan Science with the 8-10 meter telescopes in the era of the ELTs and the JWST...

GTC instrumentation plan

Science with the 8-10 meter telescopes in the era of the ELTs

and the JWST

La Palma, July 25th, 2009

Background

Information presented here is based on: Discussions with the GTC science community Discussions and recommendations from the GTC Science

Advisory Committee Advice and recommendations from an “ad oc” working

group (S. Eikenberry, S. Arribas, J. González, A. Herrero & R. Rutten)

Discussions and decisions taken by the GTC Steering Committee

Motivation

GTC user community (Spain, Mexico, and the University of Florida) is broad in its scientific interests and hence its instrumentation needs are also diverse.

GTC must achieve a good balance between hosting general-use workhorse instruments and instruments optimized for a specific capability driven by a very specific science goal.

So, high quality work-horse instruments have long prospective competitive lives. Many future science programs will need basic (but high-quality) optical and near-IR spectroscopic and imaging capability that GTC should provide.

It will be important that GTC’s instrumentation suite covers the most essential instrument capabilities.

GTC can position as a platform for the deployment of visiting instruments. The key reasons for hosting visiting instruments are: fast-track execution of very specific scientific projects requiring an

optimized instrument matching a narrow science goal. A test bench of novel measuring techniques or observing methods.

Wavelength (micron)

1 2 3 10 20 300.3

100

300

imaging

100000

30000

10000

3000

1000

U B V R I J H K L M N Q

Res

olu

tio

n

OSIRIS

OSIRIS

OSIRIS

OSIRISOptical System for Imaging and low

Resolution Integrated Spectroscopy Developed by: IAC, IAA, IFCA, LAEFF/INTA (Spain); AAO

(Aus); IAUNAM (Mex); Utexas (USA); NRO (Japan) PI: J. Cepa

Wavelength range: 0.36 - 1.0 2x2Kx4K CCD44-82 (Marconi)

Unvigneted Field of view: 7.8’ x 8.5’ with 0.127 arcsec/pixel Spectral Resolution: from 300 to 2500 with grisms.

Possible upgrade for R 5000

Observing modes: Broad band imaging with filters Narrow band imaging with tuneable filters that makes OSIRIS unique

amongst other instruments in 8-10m class telescopes Long-slit and multi-slit spectroscopy Fast photometry and spectroscopy, as well as powerful

CCD-transfer/telescope-nodding/tunable-filter combinations

Status: In operation

OSIRISLine images with TFs

M101 with broad band filter

OSIRISLine images with TFs

OSIRISScience driver

OTELO project A deep emission line object survey. Tuneable filter tomography It will allow studying a clearly defined volume of the Universe at

a known flux limit OTELO will produce the deepest emission line survey to date. 104 expected emitters detected to be distributes as follows:

10% Hα star forming emitters up to a redshift 0.4 70% would be star forming emitters detected at other optical

emission lines up to a redshift 1.5 5% Lyα emitters at redshifts up to 6.7 15% QSO and AGNs at different redshifts and about 0.5% galactic emission stars.

Wavelength (micron)

1 2 3 10 20 300.3

100

300

imaging

100000

30000

10000

3000

1000


Res

olu

tio

n

OSIRIS

OSIRIS

CanariCam

CanariCam

CanariCam

CanariCam7-25 Micron Imaging Spectrograph

Developed by the U.Florida (USA) PI: C. Telesco

Wavelength range: 7 - 25 Detector: 320 x 240 Si:As BIB (Raytheon)

Field of view: 25.6” x 19.2” with 0.08 arcsec/pix Diffraction limited above 8m (spatial resolution: 0.2’’) Spectral resolution: 100 & 1300 Sensitivity: 0.06 mJy N band (10.6 m Broadband) 1, 1 h

chopped (on plus off source) integration Observing modes:

Direct imaging Long-slit spectroscopy Coronography and Polarimetry

Status: waiting for the required functionality at the telescope. Scheduled to initiate commissioning in Autumn 2009.

CanariCamScience cases

Protoplanetary disks

Debris disk

Low mass stars (brown dwarfs, T Tauri, etc)

Star forming complexes

Luminous IR galaxies & Ultraluminous Galaxies

AGN

High redshift galaxies

Wavelength (micron)

1 2 3 10 20 300.3

100

300

imaging

100000

30000

10000

3000

1000


Res

olu

tio

n

OSIRIS

OSIRIS

CanariCam

CanariCam

CIRCE

CIRCE

CIRCE

CIRCE The Canarias InfraRed Camera

ExperimentDeveloped by the University of Florida (USA)

PI: S. Eikenberry

Wavelength range: 0.9 - 2.5 2Kx2K HgCdTe (Rockwell)

Field of View: 3.4’ x 3.4’ with 0.1 arcsec/pixel

Spectral resolution: 410 (at 1.25) and 725 (at 2.20)

Observing Modes: Broad band imaging and polarimetry Low resolution spectroscopy and spectropolarimetry

Status: under construction. Scheduled for end of 2010 To fill the near-IR gap prior to EMIR at the GTC

Keck+NIRC Gemini+NIRI GTC+CIRCE

CIRCE Field of view comparison

Expected sensitivities (based on measured sensitivities with WIRC/Palomar; 5, 1-hr exposure):

Seeing (FWHM)

Band

1.0-arcsec 0.4-arcsec

J 23.8 mag 24.8 mag

H 23.2 mag 24.2 mag

Ks 22.4 mag 23.4 mag

CIRCE Sensitivity

Wavelength (micron)

1 2 3 10 20 300.3

100

300

imaging

100000

30000

10000

3000

1000


Res

olu

tio

n

OSIRIS

OSIRIS

CanariCam

CanariCam

CIRCE

CIRCE

EMIR

EMIR

EMIR

EMIREspectrógrafo Multi-objeto

InfraRrojo

Developed by: IAC, UCM, LAEFF/INTA (Spain); Toulouse (France), INAOE (Mex)


Field of View: 6’ x 6’ with 0.2 arcsec/pixel

Sensitivity: K~23.9 in 1h @ S/N=5 in 0.6 arcsec aperture

Spectral resolution: 1000 – 5000

Observing Modes: Wide Field Direct Imaging with broad and narrow band filters Multi-object spectroscopy (50 cold configurable slitlets)

Status: under construction. Scheduled for 2012

Multi Slit Pattern

EMIRConfigurable Slit Unit

Fundamentals

Long Slit Pattern:

Spec.: 3% acc. for a 0.6” slit width


Fundamentals

300 x 300 mm FOV


Fundamentals

Wavelength (micron)

1 2 3 10 20 300.3

100

300

imaging

100000

30000

10000

3000

1000


Res

olu

tio

n

OSIRIS

OSIRIS

CanariCam

CanariCam

CIRCE

CIRCE

EMIR

EMIR

UES

UES

UESUtrecht Echelle Spectrograph

A collaboration between ING and IAC PI: R. García

Wavelength range: visible

Field of View: single source (fibre feed)

Spectral resolution: 50000-70000

Observing Modes Single object, high resolution spectroscopy

Status: under study

Abundances in the ISM at large and intermediate z (L forest, Damped L systems, quasars, starbursts and star forming galaxies) and in the Local Universe

Stellar structure and atmospheres: pulsations, line asymmetries, abundances in slowly rotating stars or low density environments (chromospheres, super- and hypergiants), detection of weak lines

High precision radial velocity studies in all kind of objects, and high-order moments of velocity distributions (e.g. anisotropy, tri-axiality, etc.) in unresolved stellar systems and galaxy nuclei.

UESFields of interest

Wavelength (micron)

1 2 3 10 20 300.3

100

300

imaging

100000

30000

10000

3000

1000


Res

olu

tio

n

OSIRIS

OSIRIS

CanariCam

CanariCam

CIRCE

CIRCE

FRIDAAO only

FRIDA

EMIR

EMIR

UES

FRIDA

FRIDAinFRared Imager and Dissector for

Adaptive optics Developed by:

IA-UNAM, CIDESI (Mexico); IAC, UCM (Spain); UdF (USA); OMP (France)


Field of View: Imaging mode: 20’’ x 20’’ with 0.01 arcsec/pixel and 40’’ x 40’’ with

0.02 and 0.04 arcsec/pixel Spectroscopy mode using an IFU unit: 0.6’’ x 0.6’’, 1.2’’ x 1.2’’ and

2.4’’ x 2.4’’

Spectral resolution: 1000 (ZJ and HK), 4000 (Z,J,H,K) and 30000 (H,K)

Observing Modes: Near diffraction limited imaging with broad and narrow filters Integral field spectroscopy

Status: under construction. Scheduled for 2012 Starting with NGSAO system. Later with LGSAO for full sky coverage

FRIDAScience cases

Solar system an low mass objects,

High and Low Mass Star forming regions

Accretion, outflow and mass transfer phenomena in binary nuclei

Crowded stellar fields and stellar populations

High and Low mass BH

Active Galactic Nuclei

Galaxy dynamics and chemical evolution.

Wavelength (micron)

1 2 3 10 20 300.3

100

300

imaging

100000

30000

10000

3000

1000


Res

olu

tio

n

OSIRIS

OSIRIS

CanariCam

CanariCam

CIRCE

CIRCE

EMIR

EMIR

Mid-ResolutionVis

UES

Mid-resolution spectroscopy

Visible


Visible A mid-resolution optical spectrograph (R=10000-

20000), largely demanded by the GTC community. Planed as the next GTC instrument to develop. A workhorse, multi-purpose instrument aimed at giving support

to a large number of projects. An instrument with significant multiplexing capability

Now preparing a Call for Proposals

Wavelength (micron)

1 2 3 10 20 300.3

100

300

imaging

100000

30000

10000

3000

1000


Res

olu

tio

n

OSIRIS

OSIRIS

CanariCam

CanariCam

CIRCE

CIRCE

EMIR

EMIR

Mid-ResolutionVis

UES

Mid-ResolutionNearIR


Near-IR


Near-IR A seeing-limited, NIR instrument with R10000-

20000, multiplexing capability of a few samples over a large patrol field of view, and broad wavelength coverage. It would be an important workhorse instrument with large

applicability Such an instrument has not been planned or available at any

other 8- to 10-m telescope.

Now preparing a Call for Proposals

JWST, ALMA and GTM

It is expected that GTC, like other major ground-based telescopes, will complement JWST observations. High spectral resolution (>3000) spectroscopy. JWST lacks this

capability. UV-Visible accessibility below 0.6 microns. This spectral range is

not covered by JWST. This will be particularly important after HST is decommissioned.

GTC+AO has higher spatial resolution than JWST. In the mid infrared, under good seeing conditions GTC will approach the diffraction limit, which is also higher than JWST.

Accessibility to a larger FoV. JWST imaging and spectroscopic (MOS) instruments have few arcminute squared FoV (i.e. 3’ x 3’), while GTC could take advantage of substantially larger values.

Multi-IFU observations. This capability is not provided by JWST. Upgradeable and versatile. GTC (ground) should take full

advantage with respect to the less flexible space facilities to improve and adapt its instrumentation.

JWST, ALMA and GTM

GTC can be considered a part of the synergistic and follow-up facilities for ALMA. GTC will not be the optimal telescope for ALMA follow-up

surveys, but certainly a great tool to study selected ALMA samples and their environment, mostly through NIR spectroscopy and narrow- and broad-band imaging in the optical, NIR and mid-IR. For galactic objects, GTC can help with AO observations of the closest cold objects detected, before the ELTs become fully operational.

The Large Millimeter Telescope (LMT/GTM) in Mexico, for which INAOE plays a leading role, is another important upcoming facility in the millimeter and sub-millimeter bandpass. LMT shares a similar latitude, and thus sky coverage, with GTC. Synergies between this facility and GTC should be address.

New and long-term developments

Next steps will be addressed towards AO instrumentation: Initiating feasibility studies for Multi-Conjugate Adaptive Optics

capabilities, and related instrumentation capabilities. Initiating feasibility studies for Ground Layer Adaptive Optics

capabilities, and related instrumentation capabilities. Commissioning a study to provide high-resolution

measurements of the ground layer properties. Additional instrumentation capabilities over this terms should

expect to be developed.

In a longer-term, we need to be open to fundamentally re-assessing our direction and mission in a time of multiple ground-based ELTs.

Thank you for coming

GTC instrumentation plan Science with the 8-10 meter telescopes in the era of the ELTs and the JWST...

Documents

Transcript of GTC instrumentation plan Science with the 8-10 meter telescopes in the era of the ELTs and the JWST...