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2009 Gemini Highlights

2009 Gemini Highlights. Jean-Ren é Roy. SOCHIAS Annual Meeting - Santiago, Chile, 14-16 January 2009. Gemini members are: United States (50%), United Kingdom (25%), Canada (15%), Australia (5%) Argentina (2.5%) and Brazil (2.5%) - Hosts: Chile, Hawaii

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2009 Gemini Highlights

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  1. 2009 Gemini Highlights Jean-René Roy SOCHIAS Annual Meeting - Santiago, Chile, 14-16 January 2009

  2. 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. 2012. Negotiations for post-2012 have started. Since 1993, Gemini: an international partnership

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

  4. Gemini South, ChileCerro Pachón 2900 mSince 2001

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

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

  7. A brief history of exo-planet imaging at Gemini A brief history of exo-planet imaging at Gemini

  8. 2001: Two ultracool companions to the young star HD130948 • Gravitationally bound pair • Very low mass ultracool objects • Pair separation = 0.134+/-0.002” • ~7% of the Sun mass • Binary = 1.13 Msun total • Semi-major axis = 2.4 AU • period ~ 10 yr • Primary < 1 Gyr Potter et al. ApJ, 2001

  9. 2002: Crossing the BD desert in 15 Sge 0.06 Msun (48 Mjup) 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)

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

  11. Gemini Deep Planet Survey*Deepest and Largest Exo-planet Imaging Survey Final ADI • 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 Mjup for 100 Myr old K0 star at d ~ 22 pc at 40-200 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 0.5 - 13 MJup are • 0.28 for 10-25 AU • 0.13 for 25-50 AU Jovian planets are rare around late- and Sun-like stars ==> chance of young Jovians to be in the 10-50 AU zone is max ~20% Angular differential imaging demo Lafrenière et al. 2007, ApJ

  12. “low hanging fruit”: large Jovian “companion” of IRXS J… Gemini North ALTAIR NIRI discovery of 8 MJup “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 Teff ~ 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

  13. 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 MJup

  14. Models of Young Planet Luminosity Planet Luminosity (Lsun) 5Myr, 8 MJup planet! (Lafreniere et al. 2008) Marley et al. 2006 Age 14

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

  16. 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)

  17. Super Gemini Planet Imager at GS in 2011

  18. 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 Teff ~ 625 K and log g ~ 4.75 • Evolutionary models indicate age of 1-5 Gyr and 15-30 MJup • CFBDS0059 and ULAS J0034 could be the first Y0 dwarfs detected Spectral indices defining T dwarf saturate below 700 K. New index of NH3 absorption in the H band introduced. Delorme et al. 2008, A&A

  20. SN2008d: A Unique Opportunity Soderberg et al. 2008, Nature • 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

  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 SN 2008d shows emergence of strong He I features of He-rich SN Ibc, unlike GRB-Supernovae. Soderberg et al. 2008, Nature

  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 50-60 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 3.5-4 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 23

  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 106 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

  26. GMOS T-ReCS Phoenix NICI* FLAMINGOS-2* MCAO/Canopus* GSAOI* GPI* GMOS ALTAIR+LGS* NIRI* MICHELLE NIFS* GNIRS* GLAO* WFMOS 2009: Current deployment of instruments on GN & GS Mauna Kea Cerro Pachón *AO instrumentation

  27. FLAMINGOS-2: Near IR MOS for Gemini South 1-2.5 mm FOV 6’x6’ for imaging FOV 2’x6’ for MOS We “hope” To deploy F-2 in 2009A

  28. 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.

  29. 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. 2009 Gemini negotiation with Subaru on-going GLAO Site survey data imply excellent GLAO performance on MK

  30. Na Kilo Hoku o Mauna Kea

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