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Gemini & Subaru Exchange Time: Developing Collaborations

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.

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Gemini & Subaru Exchange Time: Developing Collaborations

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  1. 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 15th January, 2009Subaru Users’ Meeting

  2. 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

  3. 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

  4. The GeminiObservatory • 7 country partnership • Northern & southernsky coverage • “One observatory, two telescopes” • Good image quality • IR optimized • Minimal support structure • Silver coating • Instruments Cass mounted • Heavily queue operated • ‘Classical’ available

  5. Gemini 2009 l

  6. Gemini 2012 l

  7. Gemini 2012 l

  8. ALTAIR+LGS • Laser system using 10-12 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 • 1st direct detection of planetary family • Discovered by ALTAIR+NIRI • Follow-up confirmation by Keck AO

  9. 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 – 2.5μm • Coronagraphic mode also available NIFS detection of gas inflow in NGC 4051 with 42km/s velocity slices along the H2 profile

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

  11. MIR Capabilities: Michelle & T-ReCS • Imaging • Filters: N, Q + NB • FOV: 28.8”x21.6”; 0.09”/pixel • 320x240 Raytheon array • 5-26μm • FWHM ~0.3” at 10μm • Diffraction limited • Polarimetry available on Michelle • Spectroscopy • T-ReCS • R~100, 1,000 at 10μm • 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

  12. Flamingos-2: Near IR Imager and MOS (GS) • General • HAWAII2 detector: 0.95 – 2.5μm • 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) • 50-80 slits per mask? Flamingos-2 Slit/Mask Wheel

  13. Multi-instrument queue observing “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 Gemini South GMOS-N Gemini North Michelle GMOS-S GNIRS NIRI Altair T-ReCS

  14. Future Instruments • MCAO • Multi-Conjugate Adaptive Optics • Nearly complete, 1st light 2009 • GPI • Gemini Planet Imager • Under construction, 1st 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

  15. 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 1-2.5μm • 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

  16. 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 • 1st light late 2009 H-band (1.6µm) Image Quality Traditional AO MCAO  More sensitive  Wider fields  New science

  17. Electronics Existing tip-tilt and translation stages Adaptive Secondary Mirror 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

  18. 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 • 1st light 2011

  19. 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

  20. 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

  21. Mapping H2 Emission of T Tauri Stars Beck, McGreger, Takami & Tae-Soo, ApJ 2007 • NIFS detection of H2 emission over 200 AU • All have H2 excitation temp ~2-3 times higher than predicted from UV or X-ray heating models • H2 line ratios most consistent with shock excitation • Emission likely associated with HH outflows • Rather than quiescent disk H2 gas stimulated by central star Extended v = 1-0 S(1) H2 emission around 6 T Tauri stars

  22. NIFS Dissects HL Tau’s JetTakami, 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 H2 (similar to CO outflow pattern) • H2 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 H2 emission [FeII] in contours, H2 at 2.122 m in blue H2 in blue, Continuum at 2.12 m as countours NIFS field 3 x 3 arcsec2 0.1 arcsec slitlets

  23. Massive Evolved Galaxy at z=1.26Matsuoka et al. 2008, ApJ • GMOS-S & GNIRS observations of TSPS J1239-0957 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* = 1011.5 Msun • Direct ancestor of brightest E and spheroidals of today • Presence of such a massive galaxy could favor hierarchical formation scenarios

  24. 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

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