THE SLOAN DIGITAL SKY SURVEY COADD: 275 deg2 OF DEEP SLOAN DIGITAL SKY SURVEY IMAGING ON STRIPE 82

By James Annis, M. Soares-Santos, M. Strauss, A. Becker, Scott Dodelson, Xiaohui Fan, James E. Gunn, Jiangang Hao, Željko Ivezic´, S. Jester and 10 more. Astrophysical Journal, 2011

161 citations recorded by the source corpus.

We present details of the construction and characterization of the coaddition of the Sloan Digital Sky Survey (SDSS) Stripe 82 ugriz imaging data. This survey consists of 275 deg2 of repeated scanning by the SDSS camera over −50° ⩽ α ⩽ 60° and −1.°25 ⩽ δ ⩽ +1.°25 centered on the Celestial Equator. Each piece of sky has ∼20 runs contributing and thus reaches ∼2 mag fainter than the SDSS single pass data, i.e., to r ∼ 23.5 for galaxies. We discuss the image processing of the coaddition, the modeling of the point-spread function (PSF), the calibration, and the production of standard SDSS catalogs. The data have an r-band median seeing of 1.″1 and are calibrated to ⩽1%. Star color–color, number counts, and PSF size versus modeled size plots show that the modeling of the PSF is good enough for precision five-band photometry. Structure in the PSF model versus magnitude plot indicates minor PSF modeling errors, leading to misclassification of stars as galaxies, as verified using VVDS spectroscopy. There are a variety of uses for this wide-angle deep imaging data, including galactic structure, photometric redshift computation, cluster finding and cross wavelength measurements, weak lensing cluster mass calibrations, and cosmic shear measurements.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/1e114ef4adbad4776d5fc50be4f84b20421d9c1e

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Citations in the corpus

The Hyper Suprime-Cam Software Pipeline (2017, methodology): “Annis et al. (2014) followed a similar approach, but coadded the PSF at predefined positions on a grid and then fit a smoothly-varying PSF model to these (despite the fact that the PSF being modeled may contain discontinuities).”
THE FINAL SDSS HIGH-REDSHIFT QUASAR SAMPLE OF 52 QUASARS AT z > 5.7 (2016, methodology): “The multi-epoch data have been used to construct coadded images that can reach two magnitudes deeper than the SDSS single-epoch images (e.g., Annis et al. 2014; Jiang et al. 2014; Fliri & Trujillo 2016).”
SDSS-III Baryon Oscillation Spectroscopic Survey Data Release 12: galaxy target selection and large-scale structure catalogues (2015, methodology): “To investigate this issue, we combined the deep co-added SDSS Stripe82 imaging (Abazajian et al. 2009; Annis et al. 2014) with near-infrared J- and K-band imaging from the UKIDSS Large Area Survey Data Release 4 (Hewett et al. 2006; Casali et al. 2007; Lawrence et al. 2007; Hambly et al. 2008) in…”
THE ELEVENTH AND TWELFTH DATA RELEASES OF THE SLOAN DIGITAL SKY SURVEY: FINAL DATA FROM SDSS-III (2015, background): “Both fields have 3–4 times as many PS1 epochs as does SDSS Stripe 82 (Annis et al. 2014), and PS1 continued monitoring these fields at the time the BOSS spectroscopy of these plates was carried out.”
THE BARYON OSCILLATION SPECTROSCOPIC SURVEY OF SDSS-III (2012, methodology): “For Stripe 82, the color criteria used for prioritizing targets were slightly relaxed, owing to the coadded ugriz photometry available from Annis et al. (2011), which greatly reduced the initial stellar contamination from the riz selection.”
Lensing is Low: Cosmology, Galaxy Formation, or New Physics? (2016, background): “The coaddition of these data reaches r ∼ 23.5, about 2 mag fainter than the SDSS single pass data (Annis et al. 2014) but has an r-band median seeing of 1.1 arcsec.”
Dark Energy Survey Year 1 results: weak lensing mass calibration of redMaPPer galaxy clusters (2018, background): “The two noncontiguous areas are the ‘SPT’ area (1321 deg2), which overlaps the footprint of the South Pole Telescope Sunyaev-Zel’dovich Survey (Carlstrom et al. 2011), and the ‘S82’ area (116 deg2), which overlaps the Stripe-82 deep field of the Sloan Digital Sky Survey (SDSS; Annis et al. 2014).”
The Atacama Cosmology Telescope: Sunyaev-Zel'dovich selected galaxy clusters at 148 GHz from three seasons of data (2013, methodology): “The Equatorial survey area, on which we report in this work, was chosen to overlap the deep (r ≈ 23.5 mag) optical data from the Sloan Digital Sky Survey (SDSS; Abazajian et al. 2009) Stripe 82 region (S82 hereafter; Annis et al. 2011).”
THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY: THE QUASAR LUMINOSITY FUNCTION FROM DATA RELEASE NINE (2012, methodology): “The fluxes are transferred to observed values via empirical relations for the photometric uncertainties derived from single-epoch observations of stars on Stripe 82, using the coadded fluxes (Annis et al. 2011) as the reference system.”
Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). V. Quasar Luminosity Function and Contribution to Cosmic Reionization at z = 6 (2018, unknown): “The remaining 13 quasars with zAB ≤ 22 mag were discovered in the SDSS Stripe 82 on the celestial equator, which was repeatedly scanned 70 – 90 times (Annis et al. 2014; Jiang et al. 2014).”
The number and size of subhalo-induced gaps in stellar streams (2016, background): “For example, for the Pal 5 stream, they estimated ∼ 5 close flybys 1 Note, however, an increasingly erratic behaviour of the rms scatter in completeness estimate at r = 21 in Figure 8 of Annis et al. (2014) for subhaloes with masses in the range of 107 − 108 M .”
Galaxy Alignments: Observations and Impact on Cosmology (2015, methodology): “…used this new formalism, extended to allow for full photometric redshift probability distributions, p(z), to place constraints on intrinsic alignments of a deeper sample of source galaxies in the SDSS stripe 82 region (using coadds from Huff et al. 2014 and coadd photometry from Annis et al. 2014).”