Gemini & Subaru Exchange Gemini & Subaru Exchange Time: Time: Developing CollaborationsDeveloping Collaborations
Chris PackhamUniversity of Florida
Chair of the US Gemini Science Advisory CommitteeMember of the International Gemini Science Committee
15th January, 2009Subaru Users’ Meeting
Presentation GoalsPresentation GoalsDiscussion 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 BiasMy Personal BiasLinking 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 GeminiThe GeminiObservatoryObservatory7 country partnershipNorthern & southern
sky coverage◦ “One observatory, two telescopes”
Good image qualityIR optimized
◦ Minimal support structure◦ Silver coating◦ Instruments Cass mounted
Heavily queue operated◦ ‘Classical’ available
ALTAIR+LGSALTAIR+LGSLaser system using 10-12 W laser
◦ Equivalent magnitude V~9-10Tip/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 2009Started LGS science in 2007A1st direct detection of planetary
family◦ Discovered by ALTAIR+NIRI◦ Follow-up confirmation by Keck AO
NIFS: Near-IR Integral Field NIFS: Near-IR Integral Field SpectrometerSpectrometer
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
GNIRS: Gemini Near-InfraRed GNIRS: Gemini Near-InfraRed Spectrograph (GN)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
MIR Capabilities: Michelle & MIR Capabilities: Michelle & T-ReCST-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
Flamingos-2: Near IR Imager and Flamingos-2: Near IR Imager and MOS (GS)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
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Multi-instrument queue Multi-instrument queue observingobserving
Gemini South
T-ReCS
GNIRSGMOS-S
Michelle
GMOS-N
NIRIAltair
Gem
ini N
orth
“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 InstrumentsFuture InstrumentsMCAO
◦ Multi-Conjugate Adaptive Optics◦ Nearly complete, 1st light 2009
GPI◦ Gemini Planet Imager◦ Under construction, 1st light 2011, ‘Aspen’
instrumentGLAO
◦ Ground Layer Adaptive Optics◦ Proposed – ‘Aspen’ instrument
WFMOS◦ Wide Field Multi-Object Spectrograph◦ Proposed, top rated ‘Aspen’ instrument
AO at GeminiAO at GeminiAltair (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
Multi-Conjugate AOMulti-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
MCAO
Traditional A
O
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More sensitive Wider fields New science
H-band (1.6µm) Image Quality
GLAO (Possible Future GLAO (Possible Future Capability)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-tiltand translation
stages
Adaptive Secondary
Mirror
GPI OverviewGPI 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
Large Scale View 1/2Large Scale View 1/2Many Gemini & Subaru instruments have
similar science goals & tech. driversShould be careful to avoid duplicating too
many capabilities◦Repetition of future instruments unlikely to
provide efficient next scientific stepsSpecialization of telescopes offers
perhaps the best science return on investment◦Sharing observatory resources maintains
broad range of instruments & science
Large Scale View 2/2Large Scale View 2/2Pooling of resources for future can
strengthen both communities30m class telescopes will be necessarily
internationalUse 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) H2 emissionaround 6 T Tauri stars
Mapping H2 Emission of T Tauri StarsBeck, 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
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] incontours,H2 at 2.122 min blue
H2 in blue,Continuum at2.12 m ascountours
NIFS field 3 x 3 arcsec2
0.1 arcsec slitlets
Massive Evolved Galaxy at z=1.26Matsuoka et al. 2008, ApJMatsuoka 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
ConclusionsConclusionsCollaborations 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