The Sloan Digital Sky Survey monitor telescope pipeline

By Douglas L. Tucker, S. Kent, M. Richmond, James Annis, J. A. Smith, Sahar Allam, C. Rodgers, J. Stute, J. Adelman-McCarthy, J. Brinkmann and 24 more. 2006

290 citations recorded by the source corpus.

The photometric calibration of the Sloan Digital Sky Survey (SDSS) is a multi-step process which involves data from three different telescopes: the 1.0-m telescope at the US Naval Observatory (USNO), Flagstaff Station, Arizona (which was used to establish the SDSS standard star network); the SDSS 0.5-m Photometric Telescope (PT) at the Apache Point Observatory (APO), New Mexico (which calculates nightly extinctions and calibrates secondary patch transfer fields); and the SDSS 2.5-m telescope at APO (which obtains the imaging data for the SDSS proper). In this paper, we describe the Monitor Telescope Pipeline, MTPIPE, the software pipeline used in processing the data from the single-CCD telescopes used in the photometric calibration of the SDSS (i.e., the USNO 1.0-m and the PT). We (a)

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Improved cosmological constraints from a joint analysis of the SDSS-II and SNLS supernova samples (2014, methodology): “SNLS calibration relied on observations of the BD +17 4708 primary standard in the Landolt photometric system (Landolt & Uomoto 2007), while in SDSS, the tertiary stars were compared to the HST solar analog standard stars using a dedicated monitor telescope (Tucker et al. 2006).”
The WiggleZ Dark Energy Survey: Direct constraints on blue galaxy intrinsic alignments at intermediate redshifts (2009, methodology): “All of the data were processed by completely automated pipelines that detect and measure photometric properties of objects, and astrometrically calibrate the data (Lupton et al. 2001; Pier et al. 2003; Tucker et al. 2006).”
COLORS AND KINEMATICS OF L DWARFS FROM THE SLOAN DIGITAL SKY SURVEY (2010, background): “The SDSS (York et al. 2000; Stoughton et al. 2002; Pier et al. 2003; Ivezić et al. 2004) is a multicolor (ugriz Fukugita et al. 1996; Gunn et al. 1998; Hogg et al. 2001; Smith et al. 2002; Tucker et al. 2006) photometric and spectroscopic survey centered on the northern Galactic cap.”
THE SLOAN DIGITAL SKY SURVEY QUASAR CATALOG. V. SEVENTH DATA RELEASE (2010, background): “The details of the SDSS photometric calibration are described in Smith et al. (2002), Tucker et al. (2006), and Padmanabhan et al. (2008).”
PHOTOMETRIC RESPONSE FUNCTIONS OF THE SLOAN DIGITAL SKY SURVEY IMAGER (2010, methodology): “The brightness of stars in the secondary patches was measured with respect to the USNO brightness for the set of standard stars that define the zero point of SDSS photometry (Smith et al. 2002; Tucker et al. 2006), originally denoted as primed magnitudes (FS96).”
The Sloan Digital Sky Survey Quasar Catalog: Twelfth data release (2016, methodology): “Objects were detected and their properties were measured by the photometric pipeline (Lupton et al. 2001; Stoughton et al. 2002) and calibrated photometrically (Smith et al. 2002; Ivezić et al. 2004; Tucker et al. 2006; Padmanabhan et al. 2008), and astrometrically (Pier et al. 2003).”
An Improved Photometric Calibration of the Sloan Digital Sky Survey Imaging Data (2007, background): “These patches are what finally calibrate the data from the 2.5m survey telescope (Tucker et al. 2006).”
MAPPING THE STELLAR STRUCTURE OF THE MILKY WAY THICK DISK AND HALO USING SEGUE PHOTOMETRY (2009, background): “…and photometric measurements for all detected objects (Lupton, Gunn, & Szalay 1999; Stoughton et al. 2002; Smith et al. 2002; Pier et al. 2003; Ivezić et al. 2004; Tucker et al. 2006), reaching a photometric accuracy of 2% down to g ≃22.5 and r ≃22 (Ivezić et al. 2004; Sesar et al. 2007).”
Baryon Acoustic Oscillations in the Sloan Digital Sky Survey Data Release 7 Galaxy Sample (2009, methodology): “The images were reduced (Lupton et al. 2001; Stoughton et al. 2002; Pier et al. 2003; Ivezic et al. 2004) and calibrated (Lupton, Gunn & Szalay 1999; Hogg et al. 2001; Smith et al. 2002; Tucker et al. 2006), and galaxies were selected in two ways for follow-up spectroscopy.”
Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems (2014, methodology): “Primed magnitudes should thus be transformed into the unprimed system before comparing and/or using them with the synthetic photometry published here (see e.g., Tucker et al. 2006).”
SUPERNOVA CONSTRAINTS AND SYSTEMATIC UNCERTAINTIES FROM THE FIRST THREE YEARS OF THE SUPERNOVA LEGACY SURVEY (2011, methodology): “Instead, they were calibrated by transferring observations from the SDSS monitor telescope (Tucker et al. 2006) using linear magnitude and color transformations derived from standard stars.”
MULTI-ELEMENT ABUNDANCE MEASUREMENTS FROM MEDIUM-RESOLUTION SPECTRA. II. CATALOG OF STARS IN MILKY WAY DWARF SATELLITE GALAXIES (2010, methodology): “Therefore, we transformed CFHT gri magnitudes to SDSS gri magnitudes following the prescription of Tucker et al. (2006).”
A systematic search for changing-look quasars in SDSS (2015, methodology): “…are taken on dark photometric nights of good seeing (Hogg et al. 2001) and are calibrated photometrically (Smith et al. 2002; Ivezić et al. 2004a; Tucker et al. 2006; Padmanabhan et al. 2008), and astrometrically (Pier et al. 2003) before object parameters are measured (Lupton et al. 2001;…”
A CATALOG OF QUASAR PROPERTIES FROM SLOAN DIGITAL SKY SURVEY DATA RELEASE 7 (2010, methodology): “The imaging data are taken on dark photometric nights of good seeing (Hogg et al. 2001), are calibrated photometrically (Smith et al. 2002; Ivezić et al. 2004; Tucker et al. 2006) and astrometrically (Pier et al. 2003), and object parameters are measured (Lupton et al. 2001; Stoughton et al. 2002).”
GALAXY CLUSTERING IN THE COMPLETED SDSS REDSHIFT SURVEY: THE DEPENDENCE ON COLOR AND LUMINOSITY (2010, methodology): “The imaging data were processed through a series of pipelines that perform astrometric calibration (Pier et al. 2003), photometric reduction (Lupton et al. 1999, 2001) and photometric calibration (Hogg et al. 2001; Ivezić et al. 2004; Tucker et al. 2006; Padmanabhan et al. 2008).”
The Sloan Digital Sky Survey Quasar Catalog. IV. Fifth Data Release (2007, methodology): “Photometric calibration is provided by simultaneous observations with a 20 inch (0.51 m) telescope at the same site (see Hogg et al. 2001; Smith et al. 2002; Stoughton et al. 2002; Tucker et al. 2006).”
The Milky Way’s Circular Velocity Curve to 60 kpc and an Estimate of the Dark Matter Halo Mass from the Kinematics of ~2400 SDSS Blue Horizontal-Branch Stars (2008, methodology): “Photometric calibration is provided by simultaneous observations with a 20-inch telescope at the same site (Hogg et al. 2001; Smith et al. 2002; Stoughton et al. 2002; Tucker et al. 2006).”
SEGUE: A SPECTROSCOPIC SURVEY OF 240,000 STARS WITH g = 14–20 (2009, methodology): “Except in regions of high stellar density, the processing and calibration of the SEGUE imaging data are the same as that of the SDSS imaging data (Blanton et al. 2003a; Fukugita et al. 1996; Hogg et al. 2001; Pier et al. 2003; Smith et al. 2002; Stoughton et al. 2002; Tucker et al. 2006).”
QUASAR CLUSTERING FROM SDSS DR5: DEPENDENCES ON PHYSICAL PROPERTIES (2008, methodology): “The imaging data are taken on dark photometric nights of good seeing (Hogg et al. 2001), are calibrated photometrically (Smith et al. 2002; Ivezić et al. 2004; Tucker et al. 2006) and astrometrically (Pier et al. 2003), and object parameters are measured (Lupton et al. 2001; Stoughton et al. 2002).”