1 / 23

Peter Wizinowich W. M. Keck Observatory AOSC May 31, 2004

Keck Observatory Overview. Peter Wizinowich W. M. Keck Observatory AOSC May 31, 2004. Presentation Sequence. Brief Chronology Telescopes & Optics Science Instruments Science at Keck Adaptive Optics Interferometer The People. The People.

sora
Download Presentation

Peter Wizinowich W. M. Keck Observatory AOSC May 31, 2004

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Keck Observatory Overview Peter Wizinowich W. M. Keck Observatory AOSC May 31, 2004

  2. Presentation Sequence • Brief Chronology • Telescopes & Optics • Science Instruments • Science at Keck • Adaptive Optics • Interferometer • The People

  3. The People • Science Community (Caltech, UC, NASA, UH, NOAO) • Astronomers (~ 300 users) • Graduate Students • Instrument Builders • CARA (~120 staff) • Support Astronomers • Observing Assistants • Engineers & Techicians (Electronics, Facilities, Mechanical, Optical, Software) • Administrative Support (Human Resources, Financial, Administrative Assistants, Janitors, Maintenance) • Public Outreach

  4. WMKO: A Brief Chronology • Early 1980s – University of California and Caltech begin discussions to build “TMT” • 1985 - W.M. Keck Foundation provides $70M grant for Keck I • CARA established as a non-profit organization to build & operate the Keck telescopes. • 1990 - Keck Foundation provides grant for 80% of Keck II actual construction cost (that grant eventually totals $63M)

  5. WMKO Chronology (cont.) • 1991 - 5-m Keck I first light • 1992 - 10-m Keck I first light • 1993 - Keck I science operations begin • 1996 - Keck II first light • 1996 - Keck II science operations begin • 1996 - NASA joins Keck partnership • 1999 - Keck II Adaptive Optics (AO) 1st light • 2001 - Keck-Keck first fringes • 2003 - Keck II Laser Guide Star AO 1st light

  6. Mauna Kea Summit

  7. Keck Telescopes

  8. Primary Mirror

  9. Primary Mirror Segments

  10. Keck Telescope

  11. Enclosure with roof removed Elevation Ring AO Optics Bench NIRC2 NIRSPEC or Dual Star Module Nasmyth Platform Rails to deck Electronics Racks Nasmyth Platform

  12. Wavefront Sensor Path Field Steering Mirrors (2 gimbals) Sodium dichroic/beamsplitter AOA Camera Video Display AOA Camera Camera Focus Wavefront Sensor Focus Wavefront Sensor Optics: field stop, pupil relay, lenslet, reducer optics

  13. Science Instruments

  14. Science Instruments • K1&2: • Interferometer (AO): Visibility, Nulling, Differential Phase • K1: • HIRES HIgh Resolution Echelle Spectrometer • LRIS Low Resolution Imaging Spectrometer • LWS Long Wavelength Spectrometer • NIRC Near InfraRed Camera • K2: • DEIMOS DEep Imaging Multi-Object Spectrograph • ESI Echellette Spectrograph and Imager • NIRC2 (AO) Near InfraRed Camera • NIRSPEC (/AO) Near InfraRed Spectrometer • OSIRIS OH Suppression InfraRed Integral field Spectrometer http://www2.keck.hawaii.edu/inst/

  15. D = 10m!

  16. L dwarf companion to HR7672 (Liu et al, ApJ 571, 2002) NIRSPEC K-band image & spectra Closest ultracool companion around a main sequence star m = 8.6 mag FWHM = 50 milli-arcsec

  17. Galactic: Galactic Center (Ghez et al.) K-band

  18. First LGS Results

  19. Keck Interferometer Characteristics • The two 10-m Keck telescopes + 4 proposed 1.8-m telescopes • 85-meter K-K baseline • Wavelength: 2 m & 10 m • Imaging resolution: 5 mas at 2 m • Astrometric accuracy: 30 as • First light • Two-element: March 2001 Objectives • High sensitivity fringe visibility measurements • Measurement of zodiacal dust around nearby stars using nulling (TPF) • Direct detection of brown dwarfs & warm Jupiters (Jupiter-mass planets in close orbits) • Indirect detection of Uranus-mass planets via astrometry • High-resolution imaging of disks in which planets may be forming

  20. Keck Basement

  21. Subaru 8 m Keck I&II 10 m UKIRT 4 m Gemini 8 m IRTF 3 m -> 6,50m CFHT 3,60 m OHANA: The Mauna Kea Observatory • Largest optical astronomical site of quality in the world • 3 4m-class telescopes and 4 8-10m-class telescopes with adaptive optics Unique opportunity to build the most resolving and sensitive interferometer with no competitor for more than a decade if telescopes are combined using single-mode fibers

More Related