Gemini & Subaru Exchange Time: Developing Collaborations Chris Packham University of Florida Chair of the US Gemini Science Advisory Committee Member of the International Gemini Science Committee 15 th January, 2009 Subaru Users’ Meeting

Presentation Goals Discussion of the attractions of a Subaru-Gemini partnership ◦ Good and bad points to partnership (from Subaru point of view)  Positives  Access to Gemini’s instruments & IR optimization  Access to southern skies  Collaborative with Gemini international community  Negatives  Less time on Subaru for Subaru community (but time on Gemini)  Increased complexities due to more partners involvement  Need to investigate the role of instrumentation development Increase awareness of Gemini’s capabilities ◦ Subaru-Gemini exchange time

My Personal Bias Linking of observatories maximizes scientific return from our limited resources world ◦ Improved science has got to be the result of any change  In both the respect of PI- and ‘system-’ science output ◦ Duplication of capabilities on observatories cannot be the optimal path ◦ Continuation of process underway  ALMA  TMT & GMT  Space-based  ESO Any change must be “win-win” & equitable for the communities

The Gemini Observatory 7 country partnership Northern & southern sky coverage ◦ “One observatory, two telescopes” Good image quality IR optimized ◦ Minimal support structure ◦ Silver coating ◦ Instruments Cass mounted Heavily queue operated ◦ ‘Classical’ available

Gemini 2009 Gemini North GMOS ALTAIR + LGS NIRI NIFS GNIRS Michelle Gemini South GMOS Phoenix NICI Flamingos-2 T-ReCS

Gemini 2012 Gemini North GMOS ALTAIR + LGS NIRI NIFS GNIRS GLAO Michelle Gemini South GMOS NICI Flamingos-2 MCAO GSAOI GPI T-ReCS

Gemini 2012 Gemini North GMOS ALTAIR + LGS NIRI NIFS GNIRS GLAO Michelle Gemini South GMOS NICI Flamingos-2 MCAO GSAOI GPI T-ReCS

ALTAIR+LGS Laser system using W laser ◦ Equivalent magnitude V~9-10 Tip/tilt guide stars ◦ Tip/tilt guide stars to R~18 mag ◦ Patrol field ~1 arcmin diameter Now feeds ◦ NIFS & NIRI imaging & spectroscopy Expect to feed GNIRS later in 2009 Started LGS science in 2007A 1 st direct detection of planetary family ◦ Discovered by ALTAIR+NIRI ◦ Follow-up confirmation by Keck AO

NIFS: Near-IR Integral Field Spectrometer Integral Field Unit ◦ Image slicer w/ 29 slices ◦ 3”x3” field ◦ ~70 detector pixels along each slice ◦ Spaxels ~0.1”x0.04” Spectroscopy ◦ R ~ 5000 ◦ z,J,H, K bands HAWAII-2RG detector ◦ 2048x2048 pixels ◦ 0.9 – 2.5 μm Coronagraphic mode also available NIFS detection of gas inflow in NGC 4051 with 42km/s velocity slices along the H 2 profile

GNIRS: Gemini Near-InfraRed Spectrograph (GN) Long Slit ◦ 0.9 – 2.5 μ m, R~5,900,18,000 ◦ 1.1 – 2.5 μ m, R~1,700 ◦ 2.9 – 5.5 μ m, R~1,700, 5,900, 18,000 ◦ ∆ λ : R1700: 0.3* λ ; R5900: 0.09* λ ; R18000: 0.03* λ Cross-Dispersed ◦ 0.9 – 2.5 μ m, R=1,700 full coverage ◦ R=5,900, partial coverage ALADDIN III detector ◦ 1024x1024 pixels ◦ 0.9 – 5.5 μ m Seeing-limited and Altair NGS/LGS AO (soon) GNIRS spectra of Z~6 QSOs

MIR Capabilities: Michelle & T-ReCS Imaging ◦ Filters: N, Q + NB ◦ FOV: 28.8”x21.6”; 0.09”/pixel ◦ 320x240 Raytheon array ◦ 5-26 μ m ◦ FWHM ~0.3” at 10 μ m ◦ Diffraction limited ◦ Polarimetry available on Michelle Spectroscopy ◦ T-ReCS ◦ R~100, 1,000 at 10 μ m ◦ Slits: 0.21”-1.32” x 21.6” ◦ Michelle ◦ R ~100 – 3,000 long slit ◦ R ~10,000 – 30,000 echelle ◦ Slits 0.36”-1.3” wide x 43.2” HST/NICMOS, T-ReCS & Spitzer images of LIRGS

Flamingos-2: Near IR Imager and MOS (GS) General HAWAII2 detector: 0.95 – 2.5 μ m Commissioning mid-2009 Seeing limited and MCAO ready Imaging ◦ 6.1’ ∅ FOV; 0.18”/pixel ◦ ~2’ ∅ FOV; 0.09”/pixel MCAO ◦ Y-K filters + NB + F2T2 Spectroscopy ◦ R ~ 1,200 – 3,000 ◦ FOV: 2'x6' ◦ Long-slit or custom multi-slit masks (9 held at once) ◦ slits per mask? Flamingos-2 Slit/Mask Wheel

13 Multi-instrument queue observing Gemini South T- ReCS GNIRS GMOS- S Michelle GMOS-N NIRI Altair Gemini North “Queue” is versatile  Optimized execution of programs for conditions  High completion rate of high priority programs  High shutter open efficiency: rapid switch of programs and/or instruments  Fast response programs enabled

Future Instruments MCAO ◦ Multi-Conjugate Adaptive Optics ◦ Nearly complete, 1 st light 2009 GPI ◦ Gemini Planet Imager ◦ Under construction, 1 st light 2011, ‘Aspen’ instrument GLAO ◦ Ground Layer Adaptive Optics ◦ Proposed – ‘Aspen’ instrument WFMOS ◦ Wide Field Multi-Object Spectrograph ◦ Proposed, top rated ‘Aspen’ instrument Aspen was the community (bottom- up), science driven, definition of the next generation of Gemini instruments

AO at Gemini Altair (GN) ◦ LGS/NGS modes ◦ 177 element DM ◦ 10W, 589nm laser ◦ Strehls of 20-40% NGS; 10-20% LGS in H-K MCAO (GS) ◦ Mutli-conjugate AO ◦ Strehls ~45-80% over 1-2' FOV at μ m ◦ GSAOI imager: 1.4’x1.4’ FOV; 0.02”/pixel; 4 H2RG detectors. ◦ Commissioning expected 2009 GLAO (GN) (possible future capability) ◦ Ground Layer AO ◦ Expected to deliver IQ20 80% of the time

Multi-Conjugate AO MCAO corrects multiple layers of turbulence and overcomes the cone-effect Traditional AO systems produce image quality that degrades off- axis; MCAO’s image quality is much more uniform, even over several square arcmin VLT technology demonstration system (MAD) showed that MCAO works using natural guide stars 1 st light late 2009 MCAO Traditional AO 16  More sensitive  Wider fields  New science H-band (1.6µm) Image Quality

GLAO (Possible Future Capability) A GLAO system on MK should produce 20-percentile seeing 80% of the time The GLAO conceptual design ◦ “Backwards compatible” with current instrument support structure and instruments ◦ Includes adaptive secondary mirror ◦ Uses modified MCAO laser projection system ◦ Includes a new acquisition and guidance system that incorporates all the necessary wavefront sensors ◦ Works with the existing Altair system Electronics Existing tip-tilt and translation stages Adaptive Secondary Mirror

GPI Overview GPI uses combination of optical systems to permit high contrast imaging <0.2” from bright stars ◦ High-Order Adaptive Optics System  Combination “Woofer/Tweeter” AO system that has >10x actuators than ALTAIR and will yield Strehls of 80-90% ◦ Interferometer  Measure and compensate for “super speckles” ◦ Advanced coronagraph  Rejects light from the bright central star ◦ Integral Field Spectrometer  Multi-wavelength image of planets in the field 1 st light 2011

Large Scale View 1/2 Many Gemini & Subaru instruments have similar science goals & tech. drivers Should be careful to avoid duplicating too many capabilities ◦ Repetition of future instruments unlikely to provide efficient next scientific steps Specialization of telescopes offers perhaps the best science return on investment ◦ Sharing observatory resources maintains broad range of instruments & science

Large Scale View 2/2 Pooling of resources for future can strengthen both communities 30m class telescopes will be necessarily international Use of shared time between telescopes very exciting ◦ Gemini-Subaru and Gemini-Keck exchange time well used & loved ◦ Currently Subaru-Gemini time is rather limited (5 nights per semester)  Could discourage potential applicants? ◦ Help available for applications

Extended v = 1-0 S(1) H 2 emission around 6 T Tauri stars Mapping H 2 Emission of T Tauri Stars Beck, McGreger, Takami & Tae-Soo, ApJ 2007 NIFS detection of H 2 emission over 200 AU All have H 2 excitation temp ~2-3 times higher than predicted from UV or X-ray heating models H 2 line ratios most consistent with shock excitation –Emission likely associated with HH outflows –Rather than quiescent disk H 2 gas stimulated by central star

NIFS Dissects HL Tau’s Jet Takami, Beck, Tae-Soo et al. 2007, ApJL ALTAIR/NIFS focus on HL Tau jet “central engine” <0.2” spatial resolution [Fe II] highly collimated –Compared to more extended H 2 (similar to CO outflow pattern) –H 2 outflow over a scale of only 150 pc Arc-like bipolar features predicted to change over a few years –Monitoring will provide dynamical age Consistent with jet surrounded by unseen wide-angled wind –Wind interaction with ambient gas produces bipolar cavity and shocked H 2 emission

Matsuoka et al. 2008, ApJ Massive Evolved Galaxy at z=1.26 Matsuoka et al. 2008, ApJ GMOS-S & GNIRS observations of TSPS J at z = 1.26 –Wide spectrum optical & IR coverage of southern object –Typically other work uses optical spectra and NIR broad-band photometry Bright ERO formed when universe was 2-3 Gyr, then passively evolved –M * = M sun Direct ancestor of brightest E and spheroidals of today Presence of such a massive galaxy could favor hierarchical formation scenarios

Conclusions Collaborations between Subaru & Gemini potentially very attractive and complimentary for both communities ◦ Subaru’s world leading optical observations - SC, HSC & WFMOS ◦ Drive for IR image quality, NIR & MIR at Gemini ‘Guiding light’ must be ‘win-win’ & equitable for partners ◦ Need to consider carefully instrument development options  Collaborative instrument development teams?  Upcoming Gemini next generation instrument workshop Timing seems appropriate as  Three mature telescopes  Instruments growing in complexity & expense  Move to internationally based science (i.e. TMT) Early science results promising, but much more potential