GTC instrumentation plan Science with the 8 10

GTC instrumentation plan Science with the 8 -10 meter telescopes in the era of the ELTs and the JWST La Palma, July 25 th, 2009

Background Æ Information presented here is based on: PDiscussions with the GTC science community PDiscussions and recommendations from the GTC Science Advisory Committee PAdvice and recommendations from an “ad oc” working group (S. Eikenberry, S. Arribas, J. González, A. Herrero & R. Rutten) PDiscussions and decisions taken by the GTC Steering Committee

Motivation Æ GTC user community (Spain, Mexico, and the University of Florida) is broad in its scientific interests and hence its instrumentation needs are also diverse. Æ 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. Æ 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. Æ It will be important that GTC’s instrumentation suite covers the most essential instrument capabilities. Æ GTC can position as a platform for the deployment of visiting instruments. The key reasons for hosting visiting instruments are: P fast-track execution of very specific scientific projects requiring an optimized instrument matching a narrow science goal. P A test bench of novel measuring techniques or observing methods.

OSIRIS 100000 30000 Resolution 10000 3000 OSIRIS 1000 300 100 U imaging B V R I J H K L M N Q OSIRIS 0. 3 1 2 3 Wavelength (micron) 10 20 30

OSIRIS Optical System for Imaging and low Resolution Integrated Spectroscopy Æ Developed by: IAC, IAA, IFCA, LAEFF/INTA (Spain); AAO (Aus); IA UNAM (Mex); Utexas (USA); NRO (Japan) P PI: J. Cepa Æ Wavelength range: 0. 36 - 1. 0 P 2 x 2 Kx 4 K CCD 44 -82 (Marconi) Æ Unvigneted Field of view: 7. 8’ x 8. 5’ with 0. 127 arcsec/pixel Æ Spectral Resolution: from 300 to 2500 with grisms. P Possible upgrade for R 5000 Æ Observing modes: P Broad band imaging with filters P Narrow band imaging with tuneable filters that makes OSIRIS unique amongst other instruments in 8 -10 m class telescopes P Long-slit and multi-slit spectroscopy P Fast photometry and spectroscopy, as well as powerful CCDtransfer/telescope-nodding/tunable-filter combinations Æ Status: In operation

OSIRIS Line images with TFs M 101 with broad band filter

OSIRIS Line images with TFs

OSIRIS Science driver Æ OTELO project PA deep emission line object survey. Tuneable filter tomography PIt will allow studying a clearly defined volume of the Universe at a known flux limit POTELO will produce the deepest emission line survey to date. P 104 expected emitters detected to be distributes as follows: P 10% Hα star forming emitters up to a redshift 0. 4 P 70% would be star forming emitters detected at other optical emission lines up to a redshift 1. 5 P 5% Lyα emitters at redshifts up to 6. 7 P 15% QSO and AGNs at different redshifts Pand about 0. 5% galactic emission stars.

Canari. Cam 100000 30000 Resolution 10000 3000 OSIRIS 1000 Canari. Cam 300 100 U imaging B V R I J H K L M OSIRIS 0. 3 N Q Canari. Cam 1 2 3 Wavelength (micron) 10 20 30

Canari. Cam 7 -25 Micron Imaging Spectrograph Æ Developed by the U. Florida (USA) P PI: C. Telesco Æ Wavelength range: 7 - 25 P Detector: 320 x 240 Si: As BIB (Raytheon) Æ Field of view: 25. 6” x 19. 2” with 0. 08 arcsec/pix Æ Diffraction limited above 8 m (spatial resolution: 0. 2’’) Æ Spectral resolution: 100 & 1300 Æ Sensitivity: 0. 06 m. Jy N band (10. 6 m Broadband) 1 , 1 h chopped (on plus off source) integration Æ Observing modes: P Direct imaging P Long-slit spectroscopy P Coronography and Polarimetry Æ Status: waiting for the required functionality at the telescope. P Scheduled to initiate commissioning in Autumn 2009.

Canari. Cam Science cases Æ Protoplanetary disks Æ Debris disk Æ Low mass stars (brown dwarfs, T Tauri, etc) Æ Star forming complexes Æ Luminous IR galaxies & Ultraluminous Galaxies Æ AGN Æ High redshift galaxies

CIRCE 100000 30000 Resolution 10000 3000 OSIRIS 1000 CIRCE Canari. Cam 300 100 U imaging B V R I J OSIRIS 0. 3 H K L M CIRCE 1 N Q Canari. Cam 2 3 Wavelength (micron) 10 20 30

CIRCE The Canarias Infra. Red Camera Experiment Æ Developed by the University of Florida (USA) PPI: S. Eikenberry Æ Wavelength range: 0. 9 - 2. 5 P 2 Kx 2 K Hg. Cd. Te (Rockwell) Æ Field of View: 3. 4’ x 3. 4’ with 0. 1 arcsec/pixel Æ Spectral resolution: 410 (at 1. 25 ) and 725 (at 2. 20 ) Æ Observing Modes: PBroad band imaging and polarimetry PLow resolution spectroscopy and spectropolarimetry Æ Status: under construction. Scheduled for end of 2010 PTo fill the near-IR gap prior to EMIR at the GTC

CIRCE Field of view comparison Keck+NIRC Gemini+NIRI GTC+CIRCE

CIRCE Sensitivity Æ Expected sensitivities (based on measured sensitivities with WIRC/Palomar; 5 s, 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

EMIR 100000 30000 Resolution 10000 3000 EMIR OSIRIS 1000 CIRCE Canari. Cam 300 100 U imaging B V R I J OSIRIS 0. 3 H K L M CIRCE EMIR 1 N Q Canari. Cam 2 3 Wavelength (micron) 10 20 30

EMIR Espectrógrafo Multi-objeto Infra. Rrojo Æ Developed by: PIAC, UCM, LAEFF/INTA (Spain); Toulouse (France), INAOE (Mex) Æ Wavelength range: 0. 9 - 2. 5 P 2 Kx 2 K Hg. Cd. Te (Rockwell) Æ Field of View: 6’ x 6’ with 0. 2 arcsec/pixel Æ Sensitivity: K~23. 9 in 1 h @ S/N=5 in 0. 6 arcsec aperture Æ Spectral resolution: 1000 – 5000 Æ Observing Modes: PWide Field Direct Imaging with broad and narrow band filters PMulti-object spectroscopy (50 cold configurable slitlets) Æ Status: under construction. Scheduled for 2012

EMIR Configurable Slit Unit Fundamentals Multi Slit Pattern

EMIR Configurable Slit Unit Fundamentals Long Slit Pattern: Spec. : 3% acc. for a 0. 6” slit width

EMIR Configurable Slit Unit Fundamentals 300 x 300 mm FOV

EMIR Configurable Slit Unit

UES 100000 UES 30000 Resolution 10000 3000 EMIR OSIRIS 1000 CIRCE Canari. Cam 300 100 U imaging B V R I J OSIRIS 0. 3 H K L M CIRCE EMIR 1 N Q Canari. Cam 2 3 Wavelength (micron) 10 20 30

UES Utrecht Echelle Spectrograph Æ A collaboration between ING and IAC PPI: R. García Æ Wavelength range: visible Æ Field of View: single source (fibre feed) Æ Spectral resolution: 50000 -70000 Æ Observing Modes PSingle object, high resolution spectroscopy Æ Status: under study

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

FRIDA 100000 UES 30000 Resolution 10000 FRIDA AO only 3000 EMIR OSIRIS 1000 CIRCE Canari. Cam 300 100 U imaging B V R I J OSIRIS 0. 3 H K L M CIRCE FRIDA EMIR 1 N Q Canari. Cam 2 3 Wavelength (micron) 10 20 30

FRIDA in. FRared Imager and Dissector for Adaptive optics Æ Developed by: P IA-UNAM, CIDESI (Mexico); IAC, UCM (Spain); Ud. F (USA); OMP (France) Æ Wavelength range: 0. 9 - 2. 5 P 2 Kx 2 K Hg. Cd. Te (Rockwell) Æ Field of View: P Imaging mode: 20’’ x 20’’ with 0. 01 arcsec/pixel and 40’’ x 40’’ with 0. 02 and 0. 04 arcsec/pixel P Spectroscopy mode using an IFU unit: 0. 6’’ x 0. 6’’, 1. 2’’ x 1. 2’’ and 2. 4’’ x 2. 4’’ Æ Spectral resolution: 1000 (ZJ and HK), 4000 (Z, J, H, K) and 30000 (H, K) Æ Observing Modes: P Near diffraction limited imaging with broad and narrow filters P Integral field spectroscopy Æ Status: under construction. Scheduled for 2012 P Starting with NGSAO system. Later with LGSAO for full sky coverage

FRIDA Science cases Æ Solar system an low mass objects, Æ High and Low Mass Star forming regions Æ Accretion, outflow and mass transfer phenomena in binary nuclei Æ Crowded stellar fields and stellar populations Æ High and Low mass BH Æ Active Galactic Nuclei Æ Galaxy dynamics and chemical evolution.

Mid-resolution spectroscopy Visible 100000 UES 30000 Resolution 10000 Mid-Resolution Vis 3000 EMIR OSIRIS 1000 CIRCE Canari. Cam 300 100 U imaging B V R I J OSIRIS 0. 3 H K L M CIRCE EMIR 1 N Q Canari. Cam 2 3 Wavelength (micron) 10 20 30

Mid-resolution spectroscopy Visible Æ A mid-resolution optical spectrograph (R=10000 -20000), largely demanded by the GTC community. Planed as the next GTC instrument to develop. P A workhorse, multi-purpose instrument aimed at giving support to a large number of projects. P An instrument with significant multiplexing capability Æ Now preparing a Call for Proposals

Mid-resolution spectroscopy Near-IR 100000 UES 30000 Resolution 10000 Mid-Resolution Near. IR Vis 3000 EMIR OSIRIS 1000 CIRCE Canari. Cam 300 100 U imaging B V R I J OSIRIS 0. 3 H K L M CIRCE EMIR 1 N Q Canari. Cam 2 3 Wavelength (micron) 10 20 30

Mid-resolution spectroscopy Near-IR Æ A seeing-limited, NIR instrument with R 10000 -20000, multiplexing capability of a few samples over a large patrol field of view, and broad wavelength coverage. P It would be an important workhorse instrument with large applicability P Such an instrument has not been planned or available at any other 8 to 10 -m telescope. Æ Now preparing a Call for Proposals

JWST, ALMA and GTM Æ It is expected that GTC, like other major ground-based telescopes, will complement JWST observations. PHigh spectral resolution (>3000) spectroscopy. JWST lacks this capability. PUV-Visible accessibility below 0. 6 microns. This spectral range is not covered by JWST. This will be particularly important after HST is decommissioned. PGTC+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. PAccessibility to a larger Fo. V. JWST imaging and spectroscopic (MOS) instruments have few arcminute squared Fo. V (i. e. 3’ x 3’), while GTC could take advantage of substantially larger values. PMulti-IFU observations. This capability is not provided by JWST. PUpgradeable 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 Æ GTC can be considered a part of the synergistic and follow-up facilities for ALMA. PGTC 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. Æ The Large Millimeter Telescope (LMT/GTM) in Mexico, for which INAOE plays a leading role, is another important upcoming facility in the millimeter and submillimeter bandpass. PLMT shares a similar latitude, and thus sky coverage, with GTC. PSynergies between this facility and GTC should be address.

New and long-term developments Æ Next steps will be addressed towards AO instrumentation: P Initiating feasibility studies for Multi-Conjugate Adaptive Optics capabilities, and related instrumentation capabilities. P Initiating feasibility studies for Ground Layer Adaptive Optics capabilities, and related instrumentation capabilities. P Commissioning a study to provide high-resolution measurements of the ground layer properties. P Additional instrumentation capabilities over this terms should expect to be developed. Æ 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