The u'g'r'i'z' Standard Star Network

By J. A. Smith, Douglas L. Tucker, Stephen M. Kent, M. Richmond, M. Fukugita, Takashi Ichikawa, S. Ichikawa, Anders M. Jorgensen, A. Uomoto, James E. Gunn and 12 more. 2002

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We present the 158 standard stars that define the u'g'r'i'z' photometric system. These stars form the basis for the photometric calibration of the Sloan Digital Sky Survey (SDSS). The defining instrument system and filters, the observing process, the reduction techniques, and the software used to create the stellar network are all described. We briefly discuss the history of the star selection process, the derivation of a set of transformation equations for the UBVRcIc system, and plans for future work.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Electrical and Electronic Engineering

View Paper: https://www.semanticscholar.org/paper/052ddeb460d0506b7b53880a26d9ad9ac8562ba3

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Citations in the corpus

THE CARNEGIE SUPERNOVA PROJECT: FIRST PHOTOMETRY DATA RELEASE OF LOW-REDSHIFT TYPE Ia SUPERNOVAE (2009, methodology): “…′ syn − g ′ syn) + zpu′ , g′obs − g ′ syn = ctg′ × (g ′ syn − r ′ syn) + zpg′ , r′obs − r ′ syn = ctr′ × (r ′ syn − i ′ syn) + zpr′ , and i′obs − i ′ syn = cti′ × (r ′ syn − i ′ syn) + zpi′ , where the “obs” subscript denotes the magnitudes from the Landolt (1992) and Smith et al. (2002) catalogs.”
Distances to Galactic High-Velocity Clouds. I. Cohen Stream, Complex GCP, Cloud g1 (2007, methodology): “…1800), operating between 3900 and 9000 8, and with a CCD camera (Gunn et al. 1998) with a five-filter photometric system (Fukugita et al. 1996), calibrated on imaging nights with a 20 inch (0.5 m) Photometric Telescope (Hogg et al. 2001; Smith et al. 2002; Ivezić et al. 2004; Tucker et al. 2006).”
Photometric Properties of Void Galaxies in the Sloan Digital Sky Survey (2003, methodology): “…of the photometric camera (Gunn & et al. 1998), photometric analysis (Lupton et al. 2001), the photometric system (Fukugita et al. 1996; Smith et al. 2002), the photometric monitor (Hogg et al. 2001), astrometric calibration (Pier et al. 2003), selection of the galaxy spectroscopic…”
A CATALOG OF BROAD ABSORPTION LINE QUASARS IN SLOAN DIGITAL SKY SURVEY DATA RELEASE 5 (2008, methodology): “The survey data-processing software measures the properties of each detected object in the imaging data in all five bands, and determines and applies both astrometric and photometric calibrations (Smith et al. 2002; Pier et al. 2003; Ivezić et al. 2004).”
The Environmental Dependence of Galaxy Properties in the Local Universe: Dependences on Luminosity, Local Density, and System Richness (2004, methodology): “The imaging survey of the SDSS is made in five optical bands, u, g, r, i, and z (Fukugita et al. 1996; Hogg, Finkbeiner, Schlegel, & Gunn 2001; Smith et al. 2002).”
KEPLER INPUT CATALOG: PHOTOMETRIC CALIBRATION AND STELLAR CLASSIFICATION (2011, methodology): “The Kp are defined as AB magnitudes (Oke 1974; Smith et al. 2002), derived from each target’s calibrated g, r, i magnitudes.”
THE SLOAN DIGITAL SKY SURVEY COADD: 275 deg2 OF DEEP SLOAN DIGITAL SKY SURVEY IMAGING ON STRIPE 82 (2011, methodology): “The photometric calibration is done in two ways, by tying to photometric standard stars (Smith et al. 2002) measured by a separate 0.5 m telescope on site (the PT telescope; Tucker et al. 2006; Ivezić et al. 2004) and by using the overlap between adjacent imaging runs to tie the photometry of all…”
Large-Scale Anisotropic Correlation Function of SDSS Luminous Red Galaxies (2007, methodology): “…processing (Lupton et al. 2001; Stoughton et al. 2002; Pier et al. 2003; Ivezić et al. 2004; Tucker et al. 2006) and calibration (Hogg et al. 2001; Smith et al. 2002), the spectroscopic targets of LRGs are selected from the imaging data according to the algorithm described by Eisenstein et al.…”
The Fourth Data Release of the Sloan Digital Sky Survey (2005, methodology): “…using specialized software (Lupton et al. 2001; Lupton 2005; Stoughton et al. 2002) and are astrometrically (Pier et al. 2003) and photometrically (Tucker et al. 2005) calibrated using observations of a set of primary standard stars (Smith et al. 2002) on a neighboring 20 inch (0.5 m) telescope.”
Cosmological constraints from the clustering of the Sloan Digital Sky Survey DR7 luminous red galaxies (vol 404, pg 60, 2010) (2009, methodology): “The images were reduced (Stoughton et al. 2002; Pier et al. 2003; Ivezić et al. 2004) and calibrated (Hogg et al. 2001; Smith et al. 2002; Tucker et al. 2006; Padmanabhan et al. 2008), and galaxies were selected for follow-up spectroscopy.”
Measurement of Galaxy Cluster Sizes, Radial Profiles, and Luminosity Functions from SDSS Photometric Data (2004, background): “Seeing varies on these two stripes from 1.0” to 2.0”, and the data are photometrically uniform to within 3% (Hogg et al. 2001; Smith et al. 2002).”
The N2K Consortium. IV. New Temperatures and Metallicities for More than 100,000 FGK Dwarfs (2005, methodology): “We have produced an SDSS/2MASS overlap list of 800,000 stars, for which we have generated Johnson-Cousins B, V magnitudes with the Smith et al. (2002) conversion polynomials.”
Measuring DA and H at z = 0.35 from the SDSS DR7 LRGs using baryon acoustic oscillations (2012, methodology): “Photometric observations were taken in the ugriz bands (Fukugita et al. 1996; Smith et al. 2002) by drift scanning the sky under favourable conditions (Hogg et al. 2001).”
The Environment of Active Galactic Nuclei in the Sloan Digital Sky Survey (2003, methodology): “The data are taken from the Early Data Release of the SDSS (see Stoughton et al. 2002; see also Blanton et al. 2003; Fukugita et al. 2003; Gunn et al. 1998; Hogg et al. 2001; Pier et al. 2003; Smith et al. 2002; Strauss et al. 2002).”
Stellar and dynamical masses of ellipticals in the Sloan Digital Sky Survey (2003, methodology): “The astrometric calibration is automatically performed by a pipeline that obtains absolute positions to better than 0.1 arcsec (Pier et al. 2003), and magnitudes are calibrated to a standard star network approximately in the AB system (Smith et al. 2002).”
EFFICIENT PHOTOMETRIC SELECTION OF QUASARS FROM THE SLOAN DIGITAL SKY SURVEY. II. ∼1, 000, 000 QUASARS FROM DATA RELEASE 6 (2004, methodology): “The characterization of the photometric system is discussed by Fukugita et al. (1996), Hogg et al. (2001), Smith et al. (2002), and Stoughton et al. (2002).”
A New Milky Way Companion: Unusual Globular Cluster or Extreme Dwarf Satellite? (2004, background): “2692 (Pier et al. 2003); source identification, deblending, and photometry (Lupton et al. 2001); photometricity determination (Hogg et al. 2001); calibration (Fukugita et al. 1996; Smith et al. 2002); and spectroscopic data processing (Stoughton et al. 2002).”
The Overdensities of Galaxy Environments as a Function of Luminosity and Color (2002, methodology): “…processing: astrometry (Pier et al. 2002); source identification, deblending and photometry (Lupton et al. 2001); calibration (Fukugita et al. 1996; Smith et al. 2002); spectroscopic target selection (Eisenstein et al. 2001; Strauss et al. 2002; Richards et al. 2002); spectroscopic fiber placement…”