The Sloan Digital Sky Survey COADD: 275 deg{sup 2} of deep Sloan Digital Sky Survey imaging on stripe 82

Journal Article · Mon Oct 20 00:00:00 EDT 2014 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/794/2/120· OSTI ID:22370421

Annis, James; Soares-Santos, Marcelle; Dodelson, Scott; Hao, Jiangang; Jester, Sebastian; Johnston, David E.; Kubo, Jeffrey M.; Lampeitl, Hubert; Lin, Huan; Miknaitis, Gajus; Yanny, Brian ^[1]; Strauss, Michael A.; Gunn, James E.; Lupton, Robert H. ^[2]; Becker, Andrew C.; Ivezić, Željko ^[3]; Fan, Xiaohui; Jiang, Linhua ^[4]; Seo, Hee-Jong ^[5]; Simet, Melanie ^[6]

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1. Center for Particle Astrophysics, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510 (United States)
2. Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544 (United States)
3. Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195 (United States)
4. Steward Observatory, 933 North Cherry Avenue, Tucson, AZ 85721 (United States)
5. Berkeley Center for Cosmological Physics, LBL and Department of Physics, University of California, Berkeley, CA 94720 (United States)
6. Kavli Institute for Cosmological Physics, Chicago, IL USA (United States)

We present details of the construction and characterization of the coaddition of the Sloan Digital Sky Survey (SDSS) Stripe 82 ugriz imaging data. This survey consists of 275 deg{sup 2} of repeated scanning by the SDSS camera over –50° ≤ α ≤ 60° and –1.°25 ≤ δ ≤ +1.°25 centered on the Celestial Equator. Each piece of sky has ∼20 runs contributing and thus reaches ∼2 mag fainter than the SDSS single pass data, i.e., to r ∼ 23.5 for galaxies. We discuss the image processing of the coaddition, the modeling of the point-spread function (PSF), the calibration, and the production of standard SDSS catalogs. The data have an r-band median seeing of 1.''1 and are calibrated to ≤1%. Star color-color, number counts, and PSF size versus modeled size plots show that the modeling of the PSF is good enough for precision five-band photometry. Structure in the PSF model versus magnitude plot indicates minor PSF modeling errors, leading to misclassification of stars as galaxies, as verified using VVDS spectroscopy. There are a variety of uses for this wide-angle deep imaging data, including galactic structure, photometric redshift computation, cluster finding and cross wavelength measurements, weak lensing cluster mass calibrations, and cosmic shear measurements.

• OSTI ID: 22370421
• Journal Information: Astrophysical Journal, Vol. 794, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ACCURACY
AMINO ACIDS
CALCULATION METHODS
CALIBRATION
CATALOGS
COLOR
EQUATOR
GALAXIES
IMAGE PROCESSING
MASS
PHOTOMETRY
RED SHIFT
SIMULATION
SKY
SPECTROSCOPY
STARS