1. 1 W. M. Keck Observatory Update Randy Campbell Photo Credit: Subaru Telescope 28 May 2005 UT

2. Detectors for Astronomy 12 Oct 2009 R. Campbell 2 Outline Keck Highlights Recent Projects LRIS, Low Resolution Imager / Spectrometer NGWFC, Next generation wavefront controller Current Projects MOSFIRE, Muliti Object Spectrometer for InfraRed Exploration K1 Laser Guide Star AO Future projects NGAO, Next Generation Adaptive Optics KCWI, Keck Cosmic Web Imager

3. Detectors for Astronomy 12 Oct 2009 R. Campbell 3 Photo credit: Ed Stevens

4. Detectors for Astronomy 12 Oct 2009 R. Campbell 4 Instrumentation 8 science instruments –Optical and infrared imagers, spectrometers –6 seeing limited –3 adaptive optics (AO) assisted Keck-Keck Interferometer –Multiple configurations –AO assisted

5. Detectors for Astronomy 12 Oct 2009 R. Campbell 5 LRIS – R Upgrade Instrument age: 16 years, –Blue side age (Two 2kX4k Marconi CCDs): 7 years June 2009, new red side, mosaic of two LBNL 2k×4k high- resistivity CCDs QE improvement No Fringing New dewar, focus mechanism, CCD electronics & software Smooth LRIS-Red operations during several science runs

6. Detectors for Astronomy 12 Oct 2009 R. Campbell 6 LRIS-R Read Noise, Dark Current and Radiation Trails Read NoiseDark Current [DN][e-][e-/px/hr] ~4.1~4.01.7* Average channel * Upper Limit

7. Detectors for Astronomy 12 Oct 2009 R. Campbell 7 LRIS-R R-Band Image Before and after flat fielding QE variationsAbout 1% residual after flattening

8. Detectors for Astronomy 12 Oct 2009 R. Campbell 8 Next Generation WaveFront Controller, NGWFC Commissioned in 2006 –KI and KII Based on the CCD-39 –upgrade path to the CCID-56 SciMeasure camera –Maximum 2.4 kHz frame rate MicroGate Real-time Controller Significant improvement in performance and reliability –Frame rate –Dark current –Read Noise –Charge Diffusion (MTF) Interface to existing AO system

9. Detectors for Astronomy 12 Oct 2009 R. Campbell 9 NGWFC Block Diagram

10. Detectors for Astronomy 12 Oct 2009 R. Campbell 10 Image Quality Strehl vs. Magnitude NGSAO LGSAO FWHM 49mas NGSAO LGSAO

11. Detectors for Astronomy 12 Oct 2009 R. Campbell 11 Key LGSAO Performance Areas Wave Front Controller –1 kHz BW with laser –20x20 sub-apertures STRAP, R < 19mag Truth sensor (LBWFS) –20x20 Shack-Hartman Laser brightness ~9-10 Rmag –Spot elongation, manageable problem –Typical spot 2.0 x 2.2 arcsec –Good up tip tilt (UTT) performance Regular Calibrations –Once per run –Daily afternoon check On Sky Optimization Continuous Improvements to the System Side Projected Spot Elongation

12. Detectors for Astronomy 12 Oct 2009 R. Campbell 12 Outline Keck Highlights Recent Projects LRIS, Low Resolution Imager / Spectrometer NGWFC, Next generation wavefront controller Current Projects K1 Laser Guide Star AO MOSFIRE, Muliti Object Spectrometer for InfraRed Exploration Future projects NGAO, Next Generation Adaptive Optics KCWI, Keck Cosmic Web Imager

13. Detectors for Astronomy 12 Oct 2009 R. Campbell 13 Keck I LGSAO Motivation –Improved performance –Greater flexibility –LGSAO with IF Brighter LGS AO spot –Laser: 20W (K1) vs. 14W (K2) –Mode-locked quasi-CW –Improved Na coupling Fiber beam transport (Mitsubishi) Center projection (Galileo Avionica) –Spot elongation reduced by 2x –LGS aberrations symmetric & not a function of pupil angle Science Instrument: –The IR integral field spectrometer, OSIRIS, moved from Keck II Science operation expected fall 2010 LMCTI solid state laser

14. Detectors for Astronomy 12 Oct 2009 R. Campbell 14 MOSFIRE: Multi-Object Spectrometer for Infra-Red Exploration PIs: Chuck Steidel, CIT, Ian McLean, UCLA Wide field (6’x6’) Multiplex –Configurable Slit Unit – 46 slits Each 7.3" long. Delivery: summer 2010 Keck I Cas focus

15. Detectors for Astronomy 12 Oct 2009 R. Campbell 15 MOSFIRE Detector 2048 x 2048 Teledyne Scientific Hawaii-2RG and ASIC; 18 μm pixels, long-wavelength cutoff @2.5 μm Guiding Optical CCD guider Wavelength coverage 0.975 to 2.40 μm; Y, J, H, K Spectral Resolution Rθ=2290 ⇒ R=3270 w/0.7" slit, (2.9 pixels) Pixel Scale 0.18" in imaging mode Field Size 6.12' slit length, 6.14' field for imaging

16. Detectors for Astronomy 12 Oct 2009 R. Campbell 16 Cryogenic Configurable Slit mask Unit (CSU): Swiss Centre for Micro- Electronics (CSEM). Masking Bars Indexing Stage

17. Detectors for Astronomy 12 Oct 2009 R. Campbell 17 MOSFIRE

18. Detectors for Astronomy 12 Oct 2009 R. Campbell 18 NIRC To be decommissioned in Feb 2010 Keck I First Light instrument 256^2 InSb (SBRC) 38” x 38” FOV Most sensitive Near IR instrument for 17 years PI: Keith Matthews, Caltech

19. Detectors for Astronomy 12 Oct 2009 R. Campbell 19 Outline Keck Highlights Recent Projects LRIS, Low Resolution Imager / Spectrometer NGWFC, Next generation wavefront controller Current Projects K1 Laser Guide Star AO MOSFIRE, Muliti Object Spectrometer for InfraRed Exploration Future projects NGAO, Next Generation Adaptive Optics KCWI, Keck Cosmic Web Imager

20. Detectors for Astronomy 12 Oct 2009 R. Campbell 20 NGAO Next Generation AO Key new capabilities 1.Improved near-IR performance Strehls  80% at K) Lower backgrounds  improved sensitivity Improved PSF stability & knowledge  improved photometry, astrometry & companion sensitivity 2.AO correction at red wavelengths Strehl of 15 - 25% at 750 nm  highest angular resolution of any existing filled aperture telescope 3.Increased sky coverage Improved tip/tilt correction  improved sky coverageImproved tip/tilt correction  improved sky coverage Broader range of science programs Broader range of science programs

21. Detectors for Astronomy 12 Oct 2009 R. Campbell 21 NGAO Conceptual Design

22. Detectors for Astronomy 12 Oct 2009 R. Campbell 22 NGAO Detectors The system is envisioned to have four types of wavefront sensors (WFS), namely, –1 NGS WFS –7 LGS WFS’s, –3 Low Order IR WFS’s (2TTs and 1 TT Focus and Astig), –1 High Order truth sensor –Acquisition and diagnostic cameras –Plus science instruments

23. Detectors for Astronomy 12 Oct 2009 R. Campbell 23 KCWI: Keck Cosmic Web Imager Chris Martin, Anna Moore, M. Matteuzski, P. Morrissey, D. Chang, S. Rahman Science Applications (examples) ① Map circum-galactic medium 2<z<7 ② Map circum-QSO medium ③ Map z~6 reionization bubbles ④ Composition & age of stellar remnants (halos, intracluster light) Integral Field Spectrograph: (8-30) arcsec x 20 arcsec R~1000-20,000 spectrograph 2 channels, 0.35-1.0 μ m coverage Flexible sampling, FOV, resolution High efficiency system (~30%) Designed for low surface brightness emission Designed for precision sky subtraction Keck II Nasmyth (likely) LBL High Resistivity CCDs ⑤ Low mass/surface brightness universe ⑥ Galaxy kinematics & stellar pops ⑦ Strong lens systems ⑧ GRB/SNe host properties ⑨ Galactic superwinds/feedback 3D, Low Surface Brightness Spectroscopy at Keck

24. Detectors for Astronomy 12 Oct 2009 R. Campbell 24 Acknowledgements Jim Lyke, WMKO Erik Johannson, WMKO Paul Stomski, WMKO Marcos VanDam, WMKO Marc Kassis, WMKO Chris Martin, Caltech Connie Rockosi, UCSC James Larkin, UCLA Chuck Steidel, CIT Ian MacLean, UCLA Thomas Stalcup, WMKO Peter Wizinowich, WMKO www.keckobservatory.org

25. Detectors for Astronomy 12 Oct 2009 R. Campbell 25 Thank You