1 small telescopes and the photometric calibration of the sloan digital sky survey (sdss) douglas...
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Small Telescopes and the Photometric Calibration of
the Sloan Digital Sky Survey (SDSS)
Douglas Tucker
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Sloan Digital Sky Survey (SDSS)
• SDSS I: 2000-2005
• SDSS II: 2005-2008
• 2.5m telescope
• Imaged one-quarter of the sky in ugriz down to r~22.2
• Obtained > 1 million spectra– ~800K galaxies– ~100K quasars– ~300K stars
Credit: SDSS, APO
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SDSS 2.5m Imaging Camera
• 30 SITe 2kx2k CCDs– 6 x 5 mosaic
• 6 camera columns• 5 filters (ugriz)
– 2.5° FOV
• Time Delay Integration (TDI), or “drift-scanning”– Large swaths of sky along
Great Circles
• Gaps between camera columns– 2 interleaved “strips” make
a “stripe”From SDSS
website
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Photometric Calibration of the SDSS Imaging Camera Data
• All-sky photometry requirement: 2% rms in gri, 3% rms in u,z
• Problem: – The 2.5m imaging camera saturates for stars brighter than r ~ 14.5.
• Due to drift scanning, exposure time pretty much set by the Earth’s rotation rate.
– Standard stars typically brighter than r ~ 12.– Furthermore, before SDSS, no standard stars had ever been calibrated
to the SDSS ugriz filter system.
• Solution: use smaller telescopes to calibrate primary standard stars to the ugriz filter system and to establish a set of secondary transfer fields faint enough for the 2.5m to observe.
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QuickTime™ and aTIFF (Uncompressed) decompressor
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Primary Standard Stars
• 157 bright non-variable stars calibrated against synthetic u’g’r’i’z’ photometry of the sdF star BD+17° 7808– 8.5 < r’ < 15– -0.6 < g’-r’ < 1.6
• Two-year observing campaign by J. A. Smith on the USNO-1m telescope at Flagstaff Station, Arizona (3/1998-12/1999)
• Smith, Tucker, Kent, et al. 2002, AJ, 123, 2121
USNO-1m at Flagstaff Station.Credit: USNO.
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Primary Standard Stars
USNO-1m at Flagstaff Station.Credit: USNO.
Tucker, Kent, Richmond, et al. 2006; Smith, Allam, Tucker, et al (submitted)
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Secondary (Transfer) Patches
• Primaries too bright for the 2.5m to observe
• 1520 Secondary Patches
• 40 arcmin x 40 arcmin fields
• 4 patches per “patch group” which spans the width of an SDSS stripe (2.5°)
• Patch groups are spaced roughly every 15° along the length of an SDSS stripe
• 11 < r < 17 (faint enough)
USNO-1m at Flagstaff Station.Credit: USNO.
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From SDSS Project Book
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SDSS 0.5m Photometric Telescope (“PT”)
PT
2.5m
• The PT…– Observes Primaries
to obtain nightly extinctions and zeropoints
– Observes Secondary Patches to calibrate against Primaries
• The SDSS 2.5m…– Scans over
Secondary Patches during normal course of operations
– Uses extinctions measured by PT
– Does not waste time observing Primaries itself
Apache Point Observatory
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Summary, Plus a Caveat
Summary:• The SDSS used small telescopes (smaller than about 1m) to:
– Establish primary standard stars and secondary transfer patch fields– Measure nightly extinctions
Caveat: • Going from USNO-1m (primaries) to PT (primaries,
secondaries) to SDSS 2.5m (secondaries) adds a level of complexity in the absolute calibration of the 2.5m ugriz system.– Useful to be able to measure moderately bright (V~13) HST
spectrophotometry standards directly; will will be able to do this with DECam.
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Extra Slides
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The Photometric Telescope (“PT”)
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Credit: Brian C. Lee
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12Courtesy: NOAO/AURA/NSF
SDSS 0.5m Photometric Telescope
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Secondary Patches (North Galactic Cap)
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• Smith, Allam, Tucker, Stute, Rodgers, Stoughton
• 13.5' x 13.5' fields, typically tens of stds. per field
• r = 9 - 18, ~60 fields, ~16,000 standards
• stars as bright as r≈13 can likely be observed by DECam with 5+ second exposures under conditions of poor seeing or with de-focusing (FWHM=1.5”).
Southern u’g’r’i’z’ Standards
http://www-star.fnal.gov/Southern_ugriz/
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• Already part of the DES survey strategy.
• Readily observable at a range of airmasses throughout most nights during the DES program.
• 2.5° wide (compares favorably with DECam's FOV (≈2.2°).
• Good star/galaxy classification to r ≈ 21.
• Value-added catalogue of tertiary standards is being made
– Area of Stripe 82 has been observed by SDSS > 10x under photometric conditions
– ~ 1 million tertiary SDSS ugriz standards (r = 14.5 - 21)!
– ~ 4000 per sq deg (on average)– Ivezic et al. 2006
(Others: VST OmegaCam stds (Verdoes Kleign)? SkyMapper stds (Bessell)?)
SDSS Stripe 82 ugriz Standards