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Lawrence Berkeley National Laboratory High Resistivity CCDs in Ground Based Astronomy

Lawrence Berkeley National Laboratory High Resistivity CCDs in Ground Based Astronomy Richard Stover, Mingzhi Wei, William Brown University of California Observatories/Lick Observatory The University of California Santa Cruz, California September, 2006. Orion Nebula.

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Lawrence Berkeley National Laboratory High Resistivity CCDs in Ground Based Astronomy

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  1. Lawrence Berkeley National LaboratoryHigh Resistivity CCDs in Ground Based Astronomy Richard Stover, Mingzhi Wei, William Brown University of California Observatories/Lick Observatory The University of California Santa Cruz, California September, 2006

  2. Orion Nebula First astronomical images with QE>60% at 1000nm. Using UCO/Lick 1-m Nickel Telescope and LBNL 200x200 backside-illuminated high-resistivity CCD. 4 December, 1996 Wide band filter @ 700nm Narrow band filter @1000nm

  3. LBNL CCDs Packaged at UCO/Lick C D B A F E A. 200x200 B. 2Kx2K C. 1294x4196 (12μm) D. 2Kx4K E. 400x690 (24 μm) F. 470x1264

  4. UCO/Lick Cold Wafer Probe Station

  5. UCO/Lick Cold Wafer Probe Station

  6. UCO/Lick Class 100 Cleanroom

  7. Packaged 2Kx4K

  8. Advantages of High Resistivity CCDs The LBNL high resistivity CCDs offer three advantages for ground-based astronomical imaging compared to previous CCDs. 1. Very high quantum efficiency at wavelengths greater than about 700nm. 2. No internal interference fringes. 3. Reduced charge diffusion.

  9. QE comparisons of various CCDs used at Keck

  10. A Keck LRIS spectrograph flat-field spectrum obtained by I. M. Hookprocessed to illustrate the interference patterns produced in the CCD ~5% Image courtesy Don Groom, LBNL

  11. DisadvantagesofHigh Resistivity CCDs Worms and cosmic rays

  12. LBNL 2Kx4K CCD 1000 s Dark

  13. Ground-based Astronomy ApplicationsofHigh-Resistivity CCDs UCO/Lick Hamilton echelle spectrograph (one 2Kx2K CCD) UCO/Lick Kast Cassegrain spectrograph (planned) UCO/Lick Nickel Telescope direct camera (planned) UCO/Lick guide cameras (4 cameras) (one 400x690 or 470x1264 CCD) NOAO MARS spectrograph (one 1980x800 CCD) NOAO RC spectrograph (one 1980x800 CCD) Keck LRIS spectrograph (red-side) (planned, 2 2Kx4K CCDs) Fermilab DES camera for Cerro Tololo 4-m Blanco telescope (planned, 62 2Kx4K CCDs) Non-LBNL high resistivity CCD projects: HyperSuprime Camera for Subaru telescope (planned, 176 2Kx4K Hamamatsu CCDs)

  14. Results from the NOAO Multi Aperture Red Spectrometer (MARS) on the Kitt Peak 4-m Telescope Data courtesy of Xiaohui Fan from a study of SDSS-identified high- redshift quasars. Originally pub- lished in NOAO newsletter

  15. MARS observation of the 6th most distant quasar known and the most distant radio-loud source known Data courtesy of Daniel Stern (NASA/JPL)

  16. A T4.5 brown dwarf, one of the 50 coldest stars known Data courtesy of Daniel Stern (NASA/JPL)

  17. Dark Energy Survey Instrument Description Science Program • 3 sq-degree camera with ≥ 2.2 deg FOV • 62 CCDs, 2kx4k – 0.5G pixel focal plane • SDSS g,r,i,z filters covering 400 to 1100nm • 10 Limiting mag: 24.6, 24.1, 24.3, 23.9 • Pixel size 15 microns, 0.27” /pixel • Readout time ~17 sec. • Four Probes of Dark Energy • Galaxy Cluster counting • 20,000 clusters to z=1 with M > 2x1014 M • Weak lensing • 300 million galaxies with shape measurements over 5000 sq deg. • Spatial clustering of galaxies • 300 million galaxies to z = 1 and beyond • Standard Candles • 2000 SN Ia, z = 0.3-0.8 Survey Area 5000 sq. deg. in Southern Galactic Cap with connection to SDSS stripe 82 for calibration Brenna Flaugher for the DES Collaboration; DPF Meeting August 27, 2004 Riverside,CA Fermilab, U Illinois, U Chicago, LBNL, CTIO/NOAO

  18. High Resistivity CCD Sources LBNL – Natalie Roe, Steven Holland, etc. Hamamatsu Photonics K.K. Subaru Telescope, N.O.A. Japan will use up to 176 2Kx4K 15-μm pixel CCDs in HyperSuprime. E2V Technologies Prototyping up to 2Kx4K 13.5-μm pixel CCDs.

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