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

Gemini 2009Gemini 2009

Gemini 2012Gemini 2012

Gemini 2012Gemini 2012

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

13

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

16

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