PHOTOMETRIC RESPONSE FUNCTIONS OF THE SLOAN DIGITAL SKY SURVEY IMAGER

By M. Doi, Masayuki Tanaka, M. Fukugita, James E. Gunn, N. Yasuda, Željko Ivezic´, J. Brinkmann, Ernst de Haars, S. Kleinman, J. Krzesinski and 1 more. 2010

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The monochromatic illumination system is constructed to carry out in situ measurements of the response function of the mosaicked CCD imager used in the Sloan Digital Sky Survey (SDSS). The system is outlined and the results of the measurements, mostly during the first six years of the SDSS, are described. We present the reference response functions for the five color passbands derived from these measurements, and discuss column-to-column variations and variations in time, and also their effects on photometry. We also discuss the effect arising from various, slightly different response functions of the associated detector systems that were used to give SDSS photometry. We show that the calibration procedures of SDSS remove these variations reasonably well with the resulting final errors from variant response functions being unlikely to be larger than 0.01 mag for g, r, i, and z bands over the entire duration of the survey. The considerable aging effect is uncovered in the u band, the response function showing a 30% decrease in the throughput in the short wavelength side during the survey years, which potentially causes a systematic error in photometry. The aging effect is consistent with variation of the instrumental sensitivity in the u band, which is calibrated out. The expected color variation is consistent with measured color variation in the catalog of repeated photometry. The color variation is Δ(u − g) ∼ 0.01 for most stars, and at most Δ(u − g) ∼ 0.02 mag for those with extreme colors. We verified in the final catalog that no systematic variations in excess of 0.01 mag are detected in the photometry which can be ascribed to aging and/or seasonal effects except for the secular u − g color variation for stars with extreme colors.

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Citations in the corpus

SDSS-III Baryon Oscillation Spectroscopic Survey Data Release 12: galaxy target selection and large-scale structure catalogues (2015, methodology): “…of the Northern Galactic Hemisphere and 600 deg2 of the Southern Galactic Hemisphere in the ugriz bands (Fukugita et al. 1996; Smith et al. 2002; Doi et al. 2010), using a specially designed camera (Gunn et al. 1998) on the 2.5 m Sloan telescope (Gunn et al. 2006) at the Apache Point…”
The clustering of galaxies in the sdss-iii baryon oscillation spectroscopic survey: Baryon acoustic oscillations in the data release 9 spectroscopic galaxy sample (2012, methodology): “A drift-scanning mosaic CCD camera (Gunn et al. 1998) imaged the sky in five photometric bandpasses (Fukugita et al. 1996; Smith et al. 2002; Doi et al. 2010) to a limiting magnitude of r 22.5.”
The Sloan Digital Sky Survey Reverberation Mapping Project: Hα and Hβ Reverberation Measurements from First-year Spectroscopy and Photometry (2017, methodology): “We compute g- and i-band synthetic photometry from each PrepSpec-scaled spectrum by convolving it with the corresponding SDSS filter response curves (Fukugita et al. 1996; Doi et al. 2010).”
The clustering of intermediate-redshift quasars as measured by the Baryon Oscillation Spectroscopic Survey (2012, methodology): “A drift-scanning mosaic CCD camera (Gunn et al. 1998) imaged the sky in five photometric bandpasses (Fukugita et al. 1996; Smith et al. 2002; Doi et al. 2010) to a limiting magnitude ofr ≃ 22.5.”
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: First measurement of baryon acoustic oscillations between redshift 0.8 and 2.2 (2017, methodology): “…Downloaded from https://academic.oup.com/mnras/article-abstract/473/4/4773/4443205 by University of Portsmouth Library user on 03 January 2018 bands (Fukugita et al. 1996; Smith et al. 2002; Doi et al. 2010); these data were released as part of the SDSS Data Release 7 (DR7; Abazajian et al. 2009).”
HIGH-DENSITY CIRCUMSTELLAR INTERACTION IN THE LUMINOUS TYPE IIn SN 2010jl: THE FIRST 1100 DAYS (2013, methodology): “Filter response functions for the JC and SDSS standard systems were adopted from Bessell & Murphy (2012) and Doi et al. (2010).”
SUPERNOVA CONSTRAINTS AND SYSTEMATIC UNCERTAINTIES FROM THE FIRST THREE YEARS OF THE SUPERNOVA LEGACY SURVEY (2011, methodology): “Here and elsewhere we use the mean SDSS bandpasses of Doi et al. (2010).”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Fourier space (2016, methodology): “The galaxies were selected from multicolour SDSS imaging (Fukugita et al. 1996; Gunn et al. 1998, 2006; Smith et al. 2002; Doi et al. 2010; Reid et al. 2015) over 10 252 deg2 divided in two patches on the sky and cover a redshift range of 0.2–0.75.”
The eagle simulations of galaxy formation: Public release of halo and galaxy catalogues (2015, methodology): “Magnitudes: This table contains non-dust-attenuated rest-frame broad-band magnitudes in the SDSS ugriz filters (Doi et al., 2010) and in the UKIRT Y JHK filters (Hewett et al., 2006), computed in 30 pkpc spherical apertures for all galaxies with stellar mass greater than 108.5 M as described in Tray”
The power spectrum and bispectrum of SDSS DR11 BOSS galaxies – I. Bias and gravity (2014, methodology): “The galaxies are selected from multicolour SDSS imaging (Fukugita et al. 1996; Gunn et al. 1998; Smith et al. 2002; Gunn et al. 2006; Doi et al. 2010) covering a redshift range of 0.15 < z < 0.70.”
THE Pan-STARRS1 PHOTOMETRIC SYSTEM (2012, methodology): “Doi et al. (2010) has described the evolution of the SDSS bandpasses over time, and enough change has occurred to create this level of discrepancy if the SDSS bandpasses we have adopted from the web page are not correct, since that is how we transform SDSS magnitudes onto the Pan-STARRS1 system for…”
Colours and luminosities of z = 0.1 galaxies in the eagle simulation (2015, methodology): “This factor is estimated at the effective wavelength of each filter (SDSS filter parameters taken from Doi et al. 2010, UKIRT filter parameters taken from Hewett et al. 2006), for a given dust prescription (neglecting changes in the dust opacity within a broad-band filter is a good approximation…”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Testing gravity with redshift-space distortions using the power spectrum multipoles (2013, methodology): “The galaxies are selected from multicolour SDSS imaging (Fukugita et al. 1996; Gunn et al. 1998; Smith et al. 2002; Gunn et al. 2006; Doi et al. 2010) and cover a redshift range of z = 0.15–0.7, where the survey is split into two samples called LOWZ (z = 0.15–0.43) and CMASS (z = 0.43–0.7).”
THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. V. IMPROVING THE DARK-ENERGY CONSTRAINTS ABOVE z > 1 AND BUILDING AN EARLY-TYPE-HOSTED SUPERNOVA SAMPLE (2011, background): “The Sloan Digital Sky Survey demonstrated that a 1% relative photometric calibration is possible with the current standard star network and system throughput monitoring (Doi et al. 2010).”
The one-dimensional Lyα forest power spectrum from BOSS (2013, methodology): “A mosaic CCD camera (Gunn et al. 1998) used in driftscanning mode imaged this area in five photometric bandpasses (Fukugita et al. 1996; Smith et al. 2002; Doi et al. 2010) to a limiting magnitude of g 22.8.”
The Data Release of the Sloan Digital Sky Survey-II Supernova Survey (2014, methodology): “We have followed Holtzman et al. (2008) and re-determined the absolute scale using the SDSS filter response curves (Doi et al. 2010) and the HST standard spectra (Bohlin 2007) given in the HST CALSPEC database (CALSPEC 2006).”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample (2016, background): “Details on the camera, photometry and photometric pipeline can be found in Fukugita et al. (1996), Lupton et al. (2001), Smith et al. (2002), Pier et al. (2003), Padmanabhan et al. (2008), and Doi et al. (2010).”
The SDSS-IV Extended Baryon Oscillation Spectroscopic Survey: Baryon Acoustic Oscillations at Redshift of 0.72 with the DR14 Luminous Red Galaxy Sample (2017, methodology): “Five of these maps are derived from SDSS photometry (Doi et al. 2010; Aihara et al. 2011): stellar density, i-band depth, z-band sky flux, z-FWHM and r-band extinction, while two maps are derived from WISE photometry (Wright et al. 2010; Lang et al. 2014): median number of single-exposure frames…”