2009 Gemini Highlights Jean-René Roy SOCHIAS Annual Meeting - Santiago, Chile, January 2009

Since 1993, Gemini: an international partnership  Gemini members are: United States (50%), United Kingdom (25%), Canada (15%), Australia (5%) Argentina (2.5%) and Brazil (2.5%) - Hosts: Chile, Hawaii Two 8 m telescopes optimized for visible/infrared wavelengths –GN on Mauna Kea (4200 m), Hawaii –GS on Cerro Pachon (2700 m), Chile Current Gemini International Agreement ends on 31 Dec Negotiations for post-2012 have started.

… Gemini : one observatory, two telescopes Since 2000 Gemini North, Hawaii Mauna Kea 4200 m

Gemini South, Chile Cerro Pachón 2900 m Since 2001

Instrument suite at Cass Gemini South T-ReCS GNIRS GMOS-S Michelle GMOS-N NIRI Altair Gemini North  Optimized execution of programs  High completion rate of programs  High shutter open efficiency

Two sites 11,000 km apart + Gemini archive in Canada Mauna Kea Cerro Pachon CADC-archive Total staff ~185 GN = 55% GS= 45% ~1/3 Eng ~1/3 Sci ~1/3 Admin + NGOs

A brief history of exo-planet imaging at Gemini

2001: Two ultracool companions to the young star HD Gravitationally bound pair Very low mass ultracool objects –Pair separation = / ” –~7% of the Sun mass Binary = 1.13 M sun total –Semi-major axis = 2.4 AU –period ~ 10 yr Primary < 1 Gyr Potter et al. ApJ, 2001

2002: Crossing the BD desert in 15 Sge 0.06 M sun (48 M jup ) L dwarf companion HR 7672; 14 AU from star Gemini/Hokupa’a. BD can exist that close to the main star (Liu et al. AJ, 2002)

…but Brown Dwarfs are NOT planets. Young Jovian planets are 100 – 1000 times fainter The race for imaging the first extrasolar planet is on. Gemini, Keck, Subaru, VLT or HST? Gemini N CFHT Keck Subaru Slides from 2/17/02

11 Gemini Deep Planet Survey* Deepest and Largest Exo-planet Imaging Survey NIRI/ALTAIR AO search for giant planets and brown dwarfs around 86 stars –1.6  m 5  sensitivity to  > 0.5”  m = 9.5 at 0.5”  m = 12.9 at 1” –or 2 M jup for 100 Myr old K0 star at d ~ 22 pc at AU separation Second epoch observations of 48 stars confirm all candidates as unrelated background stars 95% upper limit of fractions of star with at least one planet of M Jup are –0.28 for AU –0.13 for AU Lafrenière et al. 2007, ApJ Jovian planets are rare around late- and Sun-like stars ==> chance of young Jovians to be in the AU zone is max ~20% Angular differential imaging demo Final ADI

“low hanging fruit”: large Jovian “companion” of IRXS J… Gemini North ALTAIR NIRI discovery of 8 M Jup “companion” to K7-type solar mass star (d ~ 150 pc) –In ~5 Myr-old Upper Scorpio association –At r = 2.22” or 330 AU orbit? Spectroscopy of Jovian planet –L4-type with T eff ~ 1800 K Needs proper motion measurements over next 2- 3 yrs to establish whether planet is bound to star of chance superposition. After 10 years of trials, first imaging of a self-luminous Jovian planet ‘around’ a normal star, I.e. lowest mass companion Imaged around normal star so far. Lafrenière et al. 2008, ApJL

HR 8799: Three More Planets! HR 8799: ~60 Myr, F-type C. Marois et al., 2008, Science First images of “planetary Family” M~3 to 13 M Jup

Models of Young Planet Luminosity Marley et al Age Planet Luminosity (L sun ) 5 Myr, 8 M Jup planet! (Lafreniere et al. 2008)

In 3rd quarter of 2008: a beautiful crop of exoplanets!

2009+: NICI at Gemini South NICI AO performance as good or better than expected at radii less than ~1.4 arcsec Contrast at larger radii is limited by array controller issues, read noise, and short exposure times used for these tests (ADI)

Super Gemini Planet Imager at GS in 2011

Other recent science accomplishments

19 BBQ Temperature Brown Dwarf* CFBDS0059 found by i’-z’ imaging on CFHT and spectral characterization by Gemini (NIRI) and VLT –Coolest BD with T eff ~ 625 K and log g ~ 4.75 –Evolutionary models indicate age of 1-5 Gyr and M Jup –CFBDS0059 and ULAS J0034 could be the first Y0 dwarfs detected Delorme et al. 2008, A&A Spectral indices defining T dwarf saturate below 700 K. New index of NH 3 absorption in the H band introduced.

20 SN2008d: A Unique Opportunity  3 SN in NGC 2770 over ~10 years  SN 2008d discovered at the moment of explosion Jan 10  Rapid Gemini-GMOS spectroscopy follow-up Gemini North-GMOS g’, r’, I’ and H , March 6, 2008 Soderberg et al. 2008, Nature

21 Present at the Birth of SN 2008d Birth of SN 2008d (SN Ibc) signaled by extremely luminous X-ray outburst –First ever event detected so early (10 Jan 2008) - Swift –NGC 2770 at d = 27 Mpc Almost daily monitoring with GN/GMOS from the first day (GN-2007B-DD-9) up to the end of Jan, and weekly spectroscopy from Feb. 1st until mid May 2008 –Clear evolution from featureless continuum to broad absorption lines, and finally to deep absorption features of moderate widths Soderberg et al. 2008, Nature SN 2008d shows emergence of strong He I features of He-rich SN Ibc, unlike GRB-Supernovae.

22 Massive “Dead” Galaxies at z >2 “Dead” massive galaxies at z > 2 –Previous deep GNIRS spectroscopy had revealed 45% of the small sample to have low or no SF –New very deep GNIRS spectrum of one “dead” object at z ~ 2.2 confirms very low SF Most massive galaxies formed early And nuclear/black hole driven winds may act as “birth control” High z galaxy research enabled by efficient and versatile X-dispersed mode of GNIRS Kriek et al. 2006, 2008, ApJ

23 GN LGS AO: Ops highlights Successfully (and somewhat painfully) operating Laser Guide Star Adaptive Optics (LGS-AO) at Gemini North –Demand: 200h in queue per semester, leading to scheduled nights per semester –Gaining experience that will help with deployment of LGS-AO at GS Laser AO use requires cloudless sky and seeing better than ~ 0.8” in the optical –Occurs ~25% of the time –Schedule times as many LGS nights in queue as approved queue science time Operating under the Laser Clearing House rules for clearance to propagate the laser –Target positions need to be pre-approved –Each target has clearance only in specific time intervals Mix LGS AO programs with non-LGS queue to make optimal use of telescope time

24 Deep into the core of NGC 4244 with Gemini North NIFS

25 A Rotating Nuclear Stellar Cluster ALTAIR/NIFS LGS AO spectroscopy of flattened nuclear star cluster in edge-on spiral NGC 4244 –Multiple components –Strong rotation +/-30 km/s within the central 10 pc Both young disk and spheroidal components rotate Rotation is in same direction as normal disk 1.7 x 10 6 solar mass located < 8 pc from core Primary formation of NSC through episodic accretion of material from the disk, gas or young star clusters. Seth et al. 2008, ApJ

Mauna KeaCerro Pachón GMOSGMOS T-ReCST-ReCS PhoenixPhoenix NICI*NICI* FLAMINGOS-2*FLAMINGOS-2* MCAO/Canopus*MCAO/Canopus* GSAOI*GSAOI* GPI*GPI* GMOSGMOS ALTAIR+LGS*ALTAIR+LGS* NIRI*NIRI* MICHELLEMICHELLE NIFS*NIFS* GNIRS*GNIRS* GLAO*GLAO* WFMOSWFMOS 2009: Current deployment of instruments on GN & GS * AO instrumentation

FLAMINGOS-2: Near IR MOS for Gemini South mm FOV 6’x6’ for imaging FOV 2’x6’ for MOS We “hope” To deploy F-2 in 2009A

GLAO MK Modeling Results Improvements in FWHM are consistent, about 0.2 arcsec at H Ensquared energy improvements between 50% and 100% in 0.2 arcsec Current 20percentile IQ would be achieve 80% of the time.

Summary Coming very soon: GNIRS “reborn” – recommissioning 2009A NICI –Planet survey has started –Available for all type of science, not only planet search FLAMINGOS-2 –Acceptance tests being analyzed GMOS-N CCD replacement in 2009; GMOS-S to follow New development: GPI –In construction; completion in 2011 WFMOS –designs studies under way; end date Feb –Gemini negotiation with Subaru on-going GLAO –Site survey data imply excellent GLAO performance on MK

Na Kilo Hoku o Mauna Kea