W M Keck Observatory Instrumentation Adaptive Optics and

W. M. Keck Observatory: Instrumentation, Adaptive Optics and Scientific Productivity Taft Armandroff Director W. M. Keck Observatory 25 July 2009 La Palma, Canary Islands, Spain

Outline • • Recent Science Highlights Current Instrumentation Keck Adaptive Optics Future Enhancements to Instrumentation & Adaptive Optics • Keck Observatory Scientific Productivity • Future Strategy 2

Recent Science Highlights 3

Mike Liu et al. measure masses of brown dwarfs using Keck-AO-assisted astrometry • Angular separations: 0. 1 -0. 2 arcsec • Periodic images reveal orbits, which give masses • Compare mass, luminosity and temperature with 4

Simon/Geha Program to Measure Mass-to-Light Ratios of Faintest Galaxies in Local Group • “Missing Dwarfs” Problem from CDM Cosmology • Spectra from DEIMOS & HIRES give velocity dispersion & abundances • Most dark matter-dominated galaxies ever found 5

Marois, Macintosh et al. Discovery of Three Planetary Companions to HR 8799 • Three planets, roughly 10, 10 and 7 times mass of Jupiter 6

Current Instrumentation 7

Name Acronym Tel. & Pos. Type / FOV Wavelength range Detector LRIS Keck I Cass. Imager 6' x 8' Spectrograph: Long slit; Multi-slit (≤ 30) R = 500 – 3, 000 310 ‑ 1000 nm Red ‑ mosaic of two 2048 x 4096 LBNL CCDs Blue ‑ mosaic of two 2048 x 4096 E 2 V CCDs High Resolution Echelle Spectrometer HIRES Keck I RNAS Echelle Spectrograph: R = 30, 000 – 80, 000 350 ‑ 1000 nm Mosaic of three 2048 x 4096 MIT/LL MBE CCDs (2 blue, 1 red) Near Infrared Camera NIRC Keck I Cass. Imager 38" x 38" Spectrograph: R = 164 0. 8 – 5. 5 µm Hughes/SBRC 256 x 256 In. Sb detector NIRSPEC Keck II LNAS AO RNAS Imager 46" x 46" Spectrograph: R = 2, 000 & 25, 000 0. 95 ‑ 2. 5 µm 0. 95 ‑ 5. 5 µm Rockwell Hg. Cd. Te 256 x 256 and Aladdin-III 1024 x 1024 In. Sb (Raytheon) ESI Keck II Cass. Imager 2' x 8' Spectrograph: Echellette R up to 32, 000 Low dispersn R = 6, 000 to 1, 000 390 ‑ 1100 nm 2048 x 4096, 15 µm pixel MIT/LL CCD NIRC 2 Keck II LNAS AO Imager: 10" x 10" (narrow camera) 20" x 20" (medium camera) 40" x 40" (wide camera) Spectrograph: R = 5, 000 0. 9 - 5. 3 µm Aladdin-III 1024 x 1024 In. Sb (Raytheon) DEIMOS Keck II RNAS Imager 17' x 5' Spectrograph: Multi-slit (up to 130 slitlets with 1. 5" gaps) R = 6, 000 400 ‑ 1050 nm 410 ‑ 1100 nm Mosaic of eight 2048 x 4096, 15 µm pixel MIT/LL CCD Keck II LNAS AO Imager 0. 02“ pixel scale 20”x 20” field IFU sampling: 0. 02" to 0. 1" plate scales Broadband 16 x 64 elements Narrowband 48 x 64 elements Spectrograph: R = 3, 900 0. 95 ‑ 2. 5 µm Imager: Hawaii-I 1024 x 1024 Hg. Cd. Te Spectrograph: 8 Hawaii-II 2048 x 2048 Hg. Cd. Te Low Resolution Imager / Spectrograph Near Infrared Spectrometer Echellette Spectrograph and Imager Near Infrared Camera 2 Deep Extragalactic Imaging and Multi. Object Spectrograph OH Suppressing Infra. Red Imaging Spectrograph OSIRIS

LRIS Red Channel Detector Upgrade • Upgrade to a mosaic of two 2 K x 4 K high resistivity, thick substrate detectors (LBNL) • Significant QE improvement • No fringing • Typically 25% more spectral coverage • New dewar, focus mechanism & red channel electronics • First light 6 June 2009 9

Keck Adaptive Optics 10

LGS AO Science Galactic Center KBO’s Bipolar Jet 11 Methane brown dwarfs

Keck AO Science Capabilities Future 12

Future Enhancements to Instrumentation & Adaptive Optics 13

MOSFIRE Multi-Object Spectrometer For Infra. Red Exploration • Near-IR Multi-Object Imaging Spectrometer – 0. 97 to 2. 45 m • At Cass focus of Keck I, MOSFIRE will provide: – R = 3, 270 for a slit width of 0. 7" – 46 slits over 6. 1' x 3' FOV using a remotely configurable slit mask unit – Imaging FOV 6. 14' diameter with 0. 18" pixels • Cold testing underway • First light in June 2010 14

Keck I LGS AO • LGS AO for Keck I telescope (2010) – Higher performance than Keck II LGS AO • Higher power laser • Center launch telescope – OSIRIS at fixed location with one less reflection – LGS AO for Keck Interferometer & redundancy of key science capability 15

ASTRA overview Based on NASA investments in Keck Interferometer Based on K 2 and K 1 LGS AO capabilities July 2006 ~ July 2010 1 Self Phase Referencing Young Stellar Objects Chemical Composition at R~1800 K<8 limit R~1800 2 Dual Field Phase Referencing K<8. 5 reference K<15 science 3 Active Galactic Nuclei Chemical Composition Increased Sample Astrometry Galactic Center Stellar Population BH mass and GR effects 30μ˝ for 30˝ separation Three new operating modes Four science cases Exoplanets Reflex Motion of Multiple Planet Systems 16

NGAO - Next Generation AO Key Science Goals Understanding the Formation and Evolution of Today’s Galaxies Measuring Dark Matter in our Galaxy and Beyond Testing the Theory of General Relativity in the Galactic Center Understanding the Formation of Planetary Systems around Nearby Stars Exploring the Origins of Our Solar System Key New Science Capabilities Near Diffraction-Limited in Near-IR (K-Strehl ~80%) AO correction at Red Wavelengths (0. 65 -1. 0 m) Increased Sky Coverage Improved Angular Resolution, Sensitivity and Contrast Improved Photometric and Astrometric Accuracy Imaging and Integral Field Spectroscopy 17

How is NGAO different from Keck AO today? 18

NGAO System Architecture Key Features: 1. Fixed narrow field laser tomography 2. AO corrected NIR TT sensors 3. Cooled AO enclosure smaller 4. Cascaded relay 5. Combined imager/IFU instrument 19

NGAO in the world of 8 -10 m telescopes: Uniqueness is high spatial resolution, shorter ’s, AO-fed NIR IFS • Most 8 -10 m telescopes plan either high contrast or wide field 20 AO

Keck Observatory Scientific Productivity 21

Number of Publications per Year Number of refereed publications increasing over time 22

Papers per Telescope 23

Keck AO Science Product 217 refereed science papers (thru May/09) 10% 26% 64% 29% 52% 19% 24

LGS-AO Refereed Science Papers M. Liu Compiled by Michael Liu (U. Hawaii) 25

Future Strategy 26

Scientific Strategic Plan Mission Statement • High angular resolution astrophysics • Faint object, high-precision & highlymultiplexed spectroscopy from UV through K • Highly efficient operations • Flexibility to exploit emerging opportunities • Training the future leaders of the field 27

Strategies for Keck in the ELT Era (1) • Organizational – Nimbleness re new opportunities – Preserve strong relationship with our user community • Observing programs – More large programs – Programs that study sample of objects with Keck, then ELT follow-up of the most interesting objects – Greater exploitation of time domain – Exploit new wide-field imaging surveys • Imbalance between resources dedicated to new imaging surveys and follow-up capability 28

Strategies for Keck in the ELT Era (2) • Instrumentation & adaptive optics – Must continue to invest in compelling new instrumentation & adaptive optics systems – Higher-risk, high-reward instruments & AO • ELTs do not have appetite for risk in instrumentation • 8 -10 m telescopes will be proving ground for new, innovative instrument concepts • More specialized instruments than might be selected as 1 st generation ELT instruments – Interferometry 29

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