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W. M. Keck Observatory Update

W. M. Keck Observatory Update. Randy Campbell. Photo Credit: Subaru Telescope 28 May 2005 UT. Outline Keck Highlights. Recent Projects LRIS, Low Resolution Imager / Spectrometer NGWFC, Next generation wavefront controller. Current Projects

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W. M. Keck Observatory Update

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

  2. OutlineKeck 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 R. Campbell

  3. Photo credit: Ed Stevens 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 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 R. Campbell

  6. LRIS-R Read Noise, Dark Currentand Radiation Trails Average channel * Upper Limit R. Campbell

  7. LRIS-R R-Band ImageBefore and after flat fielding QE variations About 1% residual after flattening 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 R. Campbell

  9. NGWFC Block Diagram R. Campbell

  10. Image QualityStrehl vs. Magnitude NGSAO NGSAO LGSAO FWHM 49mas LGSAO 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 R. Campbell

  12. OutlineKeck 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 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 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 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 R. Campbell

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

  17. MOSFIRE R. Campbell

  18. NIRCTo 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 R. Campbell

  19. OutlineKeck 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 R. Campbell

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

  21. NGAO Conceptual Design 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 R. Campbell

  23. KCWI: Keck Cosmic Web ImagerChris Martin, Anna Moore, M. Matteuzski, P. Morrissey, D. Chang, S. Rahman 3D, Low Surface Brightness Spectroscopy at Keck • Low mass/surface brightness universe • Galaxy kinematics & stellar pops • Strong lens systems • GRB/SNe host properties • Galactic superwinds/feedback • Integral Field Spectrograph: (8-30) arcsec x 20 arcsec • R~1000-20,000 spectrograph • 2 channels, 0.35-1.0 μm 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 Science Applications (examples) • Map circum-galactic medium 2<z<7 • Map circum-QSO medium • Map z~6 reionization bubbles • Composition & age of stellar remnants (halos, intracluster light) 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 R. Campbell

  25. Thank You R. Campbell

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