A Photometricity and Extinction Monitor at the Apache Point Observatory

By David W. Hogg, Douglas P. Finkbeiner, David Schlegel, James E. Gunn. 2001

620 citations recorded by the source corpus.

An unsupervised software "robot" that automatically and robustly reduces and analyzes CCD observations of photometric standard stars is described. The robot measures extinction coefficients and other photometric parameters in real time and, more carefully, on the next day. It also reduces and analyzes data from an all-sky 10 μm camera to detect clouds; photometric data taken during cloudy periods are automatically rejected. The robot reports its findings to observers and data analysts via the World Wide Web. It can be used to assess photometricity and to build data on site conditions. The robot's automated and uniform site monitoring represents a minimum standard for any observing site with queue scheduling, a public data archive, or likely participation in any future National Virtual Observatory.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Electrical and Electronic Engineering

View Paper: https://www.semanticscholar.org/paper/4a04d7fb98e9f7729b6227330f02bb3212982b61

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Citations in the corpus

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).”
The Build-up of the Colour-Magnitude Relation (2005, background): “The imaging survey is performed in five optical bands, u, g, r , i , and z (Fukugita et al. 1996; Gunn et al. 1998; Hogg et al. 2001; Smith et al. 2002; Pier et al. 2003).”
Cosmological Parameters from Eigenmode Analysis of Sloan Digital Sky Survey Galaxy Redshifts (2004, methodology): “Observations are calibrated using an 0.5 m photometric telescope (Hogg et al. 2001).”
Spectroscopic Target Selection in the Sloan Digital Sky Survey: The Main Galaxy Sample (2002, positive): “The imaging data are 95% complete for point sources at r* 22.2, and the photometric calibration is accurate to about 3% in r at this writing (Hogg et al. 2001; Smith et al. 2002).”
The dependence of star formation history and internal structure on stellar mass for 105 low‐redshift galaxies (2002, methodology): “Information relating to the SDSS camera and photometric monitoring system can be found in Gunn et al (1998) and Hogg et al (2001).”
The Sloan Digital Sky Survey Quasar Catalog: Twelfth data release (2016, neutral): “These data were acquired on dark photometric nights of good seeing (Hogg et al. 2001).”
A MaxBCG Catalog of 13,823 Galaxy Clusters from the Sloan Digital Sky Survey (2007, methodology): “The imaging survey was carried out using a specially designed 2.5 m telescope (Gunn et al. 2006) in drift-scan mode in five SDSS filters (u, g, r, i, z) to a limiting magnitude of r<22.5 (Fukugita et al. 1996; Gunn et al. 1998; Lupton et al. 1999; Hogg et al. 2001; Smith et al. 2002).”
Quasars Probing Quasars. I. Optically Thick Absorbers near Luminous Quasars (2006, methodology): “The imaging data are processed by the astrometric pipeline (Pier et al. 2003) and photometric pipeline (Lupton et al. 2001) and are photometrically calibrated to a standard-star network (Smith et al. 2002; Hogg et al. 2001).”
First Measurement of the Clustering Evolution of Photometrically Classified Quasars (2005, background): “…large redshift surveys such as the Two Degree Field (2dF) Galaxy Redshift Survey (Colless et al. 2001) and the Sloan Digital Sky Survey (SDSS; Gunn et al. 1998; Lupton et al. 1999; York et al. 2000; Hogg et al. 2001; Smith et al. 2002; Stoughton et al. 2002; Pier et al. 2003; Ivezic et al. 2004).”
A Catalog of Spectroscopically Identified White Dwarf Stars in the First Data Release of the Sloan Digital Sky Survey (2004, methodology): “The SDSS photometric system is well described by Stoughton et al. (2002), Smith et al. (2002), Hogg et al. (2001), Fukugita et al. (1996), and Gunn et al. (1998).”
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).”
The C4 Clustering Algorithm: Clusters of Galaxies in the Sloan Digital Sky Survey (2005, background): “Technical details of the SDSS instrumentation and operations can be found in Gunn et al. (1998), York et al. (2000), Hogg et al. (2001), Stoughton et al. (2002), Smith et al. (2002) and Pier et al. (2003), as well as at http://www.sdss.org.”
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).”
CLUSTERING OF LOW-REDSHIFT (z ⩽ 2.2) QUASARS FROM THE SLOAN DIGITAL SKY SURVEY (2008, methodology): “The imaging data are taken on dark photometric nights of good seeing (Hogg et al. 2001) and are calibrated photometrically (Smith et al. 2002; Ivezić et al. 2004; Tucker et al. 2006; Padmanabhan et al. 2008), and astrometrically (Pier et al. 2003), and object parameters are measured (Lupton et al.…”
THE z = 5 QUASAR LUMINOSITY FUNCTION FROM SDSS STRIPE 82 (2012, background): “The quality restrictions applied to the main survey imaging (photometric and good-seeing conditions; Ivezić et al. 2004; Hogg et al. 2001) were relaxed for the Supernova Survey in order to increase the temporal coverage, resulting in a greater range of data quality.”
A Comprehensive Model for the Monoceros Tidal Stream (2004, methodology): “Drift-scan imaging in the five SDSS bandpasses (u, g, r, i, z) (Fukugita et al. 1996, Gunn et al. 1998, Hogg et al. 2001) is processed through data reduction pipelines to measure photometric and astrometric properties (Stoughton et al. 2002, Smith et al. 2002, Pier et al. 2003, Abazajian et al.…”