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 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
LBNL CCDs Packaged at UCO/Lick C D B A F E A. 200x200 B. 2Kx2K C. 1294x4196 (12 μ m) D. 2Kx4K E. 400x690 (24 μ m) F. 470x1264
UCO/Lick Cold Wafer Probe Station
UCO/Lick Cold Wafer Probe Station
UCO/Lick Class 100 Cleanroom
Packaged 2Kx4K Packaged 2Kx4K
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.
QE comparisons of various CCDs used at Keck
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
Disadvantages of High Resistivity CCDs Worms and cosmic rays
LBNL 2Kx4K CCD 1000 s Dark
Ground-based Astronomy Applications of 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)
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
MARS observation of the 6th most distant quasar known and the most distant radio-loud source known Data courtesy of Daniel Stern (NASA/JPL)
A T4.5 brown dwarf, one of the 50 coldest stars known Data courtesy of Daniel Stern (NASA/JPL)
Dark Energy Survey Instrument Description Science Program • 3 sq-degree camera with ≥ 2.2 deg FOV ● Four Probes of Dark Energy • 62 CCDs, 2kx4k – 0.5G pixel focal plane • SDSS g,r,i,z filters covering 400 to 1100nm – Galaxy Cluster counting • 10 σ Limiting mag: 24.6, 24.1, 24.3, 23.9 ● 20,000 clusters to z=1 with M > 2x10 14 M � • Pixel size 15 microns, 0.27” /pixel • Readout time ~17 sec. – Weak lensing ● 300 million galaxies with shape measurements over 5000 sq Survey Area deg. 5000 sq. deg. – Spatial clustering of galaxies in Southern ● 300 million galaxies to z = 1 Galactic Cap and beyond with connection to – S tandard Candles SDSS stripe 82 for ● 2000 SN Ia, z = 0.3-0.8 calibration Brenna Flaugher for the DES Collaboration; DPF Meeting August 27, 2004 Riverside,CA Fermilab, U Illinois, U Chicago, LBNL, CTIO/NOAO
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- μ m pixel CCDs in HyperSuprime. E2V Technologies Prototyping up to 2Kx4K 13.5- μ m pixel CCDs.
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