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Wide band filter @ 700nm Narrow band filter @1000nm
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
Lawrence Berkeley National Laboratory High Resistivity CCDs in - - PowerPoint PPT Presentation
Lawrence Berkeley National Laboratory High Resistivity CCDs in - - PowerPoint PPT Presentation
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
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- A. 200x200 B. 2Kx2K C. 1294x4196 (12μm) D. 2Kx4K E. 400x690 (24 μm) F. 470x1264
A B C D E F
LBNL CCDs Packaged at UCO/Lick
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UCO/Lick Cold Wafer Probe Station
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UCO/Lick Cold Wafer Probe Station
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UCO/Lick Class 100 Cleanroom
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Packaged 2Kx4K Packaged 2Kx4K
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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.
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QE comparisons of various CCDs used at Keck
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A Keck LRIS spectrograph flat-field spectrum obtained by I. M. Hook processed to illustrate the interference patterns produced in the CCD
~5%
Image courtesy Don Groom, LBNL
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Disadvantages
- f
High Resistivity CCDs
Worms and cosmic rays
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LBNL 2Kx4K CCD
1000 s Dark
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Ground-based Astronomy Applications
- f
High-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)
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Results from the NOAO Multi Aperture Red Spectrometer (MARS)
- n 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
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MARS observation of the 6th most distant quasar known and the most distant radio-loud source known
Data courtesy of Daniel Stern (NASA/JPL)
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A T4.5 brown dwarf, one of the 50 coldest stars known
Data courtesy of Daniel Stern (NASA/JPL)
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Dark Energy Survey
- 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
- 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
- 10σ Limiting mag: 24.6, 24.1, 24.3, 23.9
- Pixel size 15 microns, 0.27” /pixel
- Readout time ~17 sec.
Science Program Instrument Description 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
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