The [CLC][ITAL]u[/ITAL][/CLC][arcmin]′[CLC][ITAL]g[/ITAL][/CLC][arcmin]′[CLC][ITAL]r[/ITAL][/CLC][arcmin]′[CLC][ITAL]i[/ITAL][/CLC][arcmin]′[CLC][ITAL]z[/ITAL][/CLC][arcmin]′ Standard-Star System

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

173 citations recorded by the source corpus.

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

View Paper: https://www.semanticscholar.org/paper/e74c1adfc2d30e55d378069509eab9a3c01a7e29

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Citations in the corpus

The host galaxies of active galactic nuclei (2003, unknown): “The imaging is conducted in the u, g, r, i and z bands (Fukugita et al. 1996; Gunn et al. 1998; Hogg et al. 2001; Smith et al. 2002), and spectra are obtained with a pair of multifibre spectrographs.”
Stellar masses and star formation histories for 105 galaxies from the Sloan Digital Sky Survey (2002, unknown): “More details concerning the SDSS photometric system may be found in Fukugita et al. (1996) and Smith et al. (2002).”
The UKIRT Infrared Deep Sky Survey ZY JHK photometric system: passbands and synthetic colours (2006, result): “These two papers, then, are similar in aim to the SDSS papers by Fukugita et al. (1996) and Smith et al. (2002).”
Protoclusters associated with z > 2 radio galaxies - I. Characteristics of high redshift protoclusters (2006, methodology): “Zero-points in the Vega system are converted to the AB system using the transformations of Bessell (1979) and Smith et al. (2002).”
The dependence of star formation history and internal structure on stellar mass for 105 low‐redshift galaxies (2002, methodology): “In order to minimize the errors in this procedure, we K-correct the magnitudes of all galaxies in our sample to z = 0.1 More details about the SDSS photometric system may be found in Fukugita et al (1996) and Smith et al (2002).”
The size distribution of galaxies in the Sloan Digital Sky Survey (2003, methodology): “…is described by Gunn et al. (1998); the filter system is roughly as described in Fukugita et al. (1996); the photometric calibration of the SDSS imaging data is described in Hogg et al. (2001) and Smith et al. (2002); and the accuracy of astrometric calibration is described in Pier et al. (2003).”
Galaxy And Mass Assembly (GAMA): the input catalogue and star–galaxy separation (2009, methodology): “Observations with a 0.5-m photometric telescope (Hogg et al. 2001) are used to calibrate the 2.5-m telescope images using theu′g′r′i′z′ standard star system (Fukugita et al. 1996; Smith et al. 2002).”
The physical properties of star-forming galaxies in the low-redshift universe (2003, methodology): “The photometry is obtained using driftscanning with a unique CCD camera (Gunn et al. 1998), allowing near-simultaneous photometry in five bands (u, g, r, i, z, Fukugita et al. 1996; Hogg et al. 2001; Smith et al. 2002).”
Resolved stellar mass maps of galaxies. I: method and implications for global mass estimates (2009, methodology): “Finally, we build a mosaic of the scans based on the previously computed astrometric solutions using SWARP (http://astromatic.iap.fr/software/swarp).6 We refer the reader to Fukugita et al. (1996), Gunn et al. (1998, 2006) and Smith et al. (2002) for a summary of the properties of the SDSS imaging.”
The shapes of galaxies in the Sloan Digital Sky Survey (2008, unknown): “The properties of all detected objects in the images are measured (Lupton, Gunn & Szalay 1999; Stoughton et al. 2002), and are calibrated astrometrically (Pier et al. 2003) and photometrically (Smith et al. 2002; Ivezić et al. 2004; Tucker et al. 2006).”
Average extinction curves and relative abundances for quasi-stellar object absorption-line systems at 1 ≤zabs < 2 (2006, unknown): “Based on precise absolute flux calibration (Hogg et al. 2001; Smith et al. 2002; Ivezic et al. 2004) of the object images in the SDSS filter system (Fukugita et al. 1996), QSOs can be reliably separated from most types of stars, and reasonably accurate photometric redshifts can be estimated for a…”
The dependence of clustering on galaxy properties (2005, methodology): “Imaging is obtained in the u, g, r, i, z bands (Fukugita et al. 1996; Smith et al. 2002; Ivezić et al. 2004) with a special purpose drift scan camera (Gunn et al. 1998) mounted on the SDSS 2.5 meter telescope at Apache Point Observatory.”
Density profiles of galaxy groups and clusters from SDSS galaxy–galaxy weak lensing (2006, methodology): “The imaging is carried out by drift-scanning the sky in photometric conditions (Hogg et al. 2001; Ivezić et al. 2004), in five bands (ugriz) (Fukugita et al. 1996; Smith et al. 2002) using a specially-designed wide-field camera (Gunn et al. 1998).”
Galaxy halo masses and satellite fractions from galaxy–galaxy lensing in the Sloan Digital Sky Survey: stellar mass, luminosity, morphology and environment dependencies (2005, methodology): “The imaging is carried out by drift-scanning the sky in photometric conditions (Hogg et al. 2001; Ivezić et al. 2004), in five bands (ugriz) (Fukugita et al. 1996; Smith et al. 2002) using a specially-designed wide-field camera (Gunn et al. 1998).”
Detection of large-scale intrinsic ellipticity—density correlation from the Sloan Digital Sky Survey and implications for weak lensing surveys (2005, methodology): “The imaging is carried out by drift-scanning the sky in photometric conditions (Hogg et al. 2001; Ivezić et al. 2004), in five bands (ugriz) (Fukugita et al. 1996; Smith et al. 2002) using a specially designed widefield camera (Gunn et al. 1998).”
The Carnegie Supernova Project: The Low‐Redshift Survey (2005, methodology): “(6)v v v v In these equations u g r i BV (left-hand side) are the published magnitudes in the standard system (Landolt 1992; Smith et al. 2002), ugribv (right-hand side) correspond to the natural-system magnitudes, ki is the extinction coefficient, xi is the effective air mass, cti is the color…”
The structure of galactic disks - Studying late-type spiral galaxies using SDSS (2006, methodology): “The Sloan Digital Sky Survey (SDSS) (York et al., 2000) will map one-quarter (∼ 104 ◦ ) of the entire sky mainly around the north galactic cap (above Galactic latitude∼ 30◦ ) in five bands, u′, g′, r ′, i′ andz′ (Fukugita et al., 1996; Smith et al., 2002).”
An absolutely calibrated T eff scale from the infrared flux method. Dwarfs and subgiants (2010, background): “Two of the CALSPEC targets are late-type main-sequence dwarfs for which accurate photometry, logg and [Fe/H] are available: the exoplanet host star HD209458 (e.g. Charbonneau et al. 2000) and the fundamental SDSS standard BD +17 4708 (e.g. Fukugita et al. 1996; Smith et al. 2002).”
Measuring the galaxy–mass and galaxy–dust correlations through magnification and reddening (2009, background): “The survey provides images in five broad optical bands (u, g, r, i, z c© 0000 RAS, MNRAS 000, 000–000 Fukugita et al. 1996; Smith et al. 2002).”