Light and motion in SDSS Stripe 82: The catalogues

By D. Bramich, S. Vidrih, L. Wyrzykowski, J. Munn, Huan Lin, N. Evans II, M. Smith, V. Belokurov, G. Gilmore, D. Zucker and 12 more. 2008

133 citations recorded by the source corpus.

We present a new public archive of light-motion curves in Sloan Digital Sky Survey (SDSS) Stripe 82, covering 99° in right ascension from a = 20 h 7 to 3 h .3 and spanning 2.°52 in declination from δ = -1°.26 to 1°.26, for a total sky area of ∼249 deg 2 . Stripe 82 has been repeatedly monitored in the u, g, r, i and z bands over a seven-year baseline. Objects are cross-matched between runs, taking into account the effects of any proper motion. The resulting catalogue contains almost 4 million light-motion curves of stellar objects and galaxies. The photometry are recalibrated to correct for varying photometric zero-points, achieving ∼20 and 30 mmag rms accuracy down to 18 mag in the g, r, i and z bands for point sources and extended sources, respectively. The astrometry are recalibrated to correct for inherent systematic errors in the SDSS astrometric solutions, achieving ∼32 and 35 mas rms accuracy down to 18 mag for point sources and extended sources, respectively. For each light-motion curve, 229 photometric and astrometric quantities are derived and stored in a higher level catalogue. On the photometric side, these include mean exponential and point spread function (PSF) magnitudes along with uncertainties, rms scatter, Χ 2 per degree of freedom, various magnitude distribution percentiles, object type (stellar or galaxy), and eclipse, Stetson and Vidrih variability indices. On the astrometric side, these quantities include mean positions, proper motions as well as their uncertainties and Χ 2 per degree of freedom. The light-motion curve catalogue presented here is complete down to r ∼ 21.5 and is at present the deepest large-area photometric and astrometric variability catalogue available.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/23b4e390bc1407973452a204f84b2f7729186e8e

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Citations in the corpus

THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY: THE QUASAR LUMINOSITY FUNCTION FROM DATA RELEASE NINE (2012, background): “…two reasons: (i) the improved photometry of the deeper data better defines the stellar locus (Ivezić et al. 2007) and (ii) quasars can be selected based on their variability (Sesar et al. 2007; Bramich et al. 2008; Schmidt et al. 2010; MacLeod et al. 2011; Palanque-Delabrouille et al. 2011, 2012).”
The Milky Way stellar halo out to 40 kpc: squashed, broken but smooth (2011, methodology): “We use the light curve catalogue compiled by Bramich et al. (2008) and classify variable stars according to the criteria outlined in Sesar et al. (2007).”
QUANTIFYING QUASAR VARIABILITY AS PART OF A GENERAL APPROACH TO CLASSIFYING CONTINUOUSLY VARYING SOURCES (2009, methodology): “To our knowledge, there are the quasars in the SDSS equatorial strip, with roughly 60 epochs over ∼six years (Sesar et al. 2007; Bramich et al. 2008), the QUEST survey (Rengstorf et al. 2004b), whose light curves are not publicly available, and any quasars lying in the microlensing survey regions.”
Kinematics of SDSS subdwarfs: structure and substructure of the Milky Way halo (2009, methodology): “The full Bramich et al. (2008) catalogue contains proper motions, µ, for ∼ 1 million stars down to magnitudes of r ∼ 21.5.”
THE SEVENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY (2008, methodology): “…in the CAS; rms variations of more than 0.1 mag are an indication of considerable variable cloud cover, and a value of more than 1 magnitude suggests that the approximate calibration procedure of Bramich et al. (2008) breaks down, and the resulting photometry should be regarded with caution.”
THE BARYON OSCILLATION SPECTROSCOPIC SURVEY OF SDSS-III (2012, methodology): “• HPM consists of ∼ 100 high proper motion stars also selected from the catalogs of Bramich et al. (2008) and Ivezić et al. (2007) with an emphasis on faint objects with high proper motions (µ > 0.1 mas yr−1).”
OPTICAL DISCOVERY OF PROBABLE STELLAR TIDAL DISRUPTION FLARES (2010, background): “Selecting flares in SDSS observations The ∼ 300 deg2 Sloan Digital Sky Survey (SDSS; York et al. 2000) multi-epoch imaging data Stripe 82 (Sesar et al. 2007; Bramich et al. 2008; Frieman et al. 2008; Abazajian et al. 2009) was the starting point of our search.”
THE MILKY WAY TOMOGRAPHY WITH SDSS. III. STELLAR KINEMATICS (2009, methodology): “In Bramich et al. (2008), proper motions are computed using only SDSS data, and thus they are expected to have different, and probably smaller, systematic errors than the SDSS–POSS proper motions (random errors for the stripe 82 proper motions are larger by about a factor of 2).”
THE SLOAN DIGITAL SKY SURVEY COADD: 275 deg2 OF DEEP SLOAN DIGITAL SKY SURVEY IMAGING ON STRIPE 82 (2011, methodology): “The runs were calibrated following the prescription of Bramich et al. (2008), which builds a catalog-level coadd of bright stars to match stars in the frames and compute a zero-point shift.”
Substructure revealed by RR Lyraes in SDSS Stripe 82 (2009, methodology): “In this paper, we select first the variable objects in Stripe 82 and then the subset of RR Lyraes, using the Bramich et al. (2008) Light-Motion Curve Catalogue (LMCC) and Higher-Level Catalogue (HLC).”
LIGHT CURVE TEMPLATES AND GALACTIC DISTRIBUTION OF RR LYRAE STARS FROM SLOAN DIGITAL SKY SURVEY STRIPE 82 (2009, methodology): “It was the largest source of multi-epoch data during the first phase of the SDSS (SDSS-I), with a median of 10-20 observations per source (S07, Bramich et al. 2008) and it remains so thanks to additional imaging runs obtained during the SDSS-II Supernova (SN) survey (Frieman et al. 2008).”