The Fifth Data Release of the Sloan Digital Sky Survey

Adelman-McCarthy, Jennifer K.; Agüeros, Marcel A.; Allam, S.; Anderson, K. S. J.; Anderson, Scott F.; Annes, James; Bahcall, Neta A.; Bailer‐Jones, C. A. L.; Baldry, I. K.; Barentine, John C.; Beers, Timothy C.; Belokurov, V.; Berlind, Andreas A.; Bernardi, Mariangela; Blanton, Michael R.; Bochanski, John J.; Boroski, William N.; Bramich, D. M.; Brewington, H.; Brenchmann, Jarle; Brinkmann, J.; Brunner, Róbert; Budavàri, Tamás; Carey, Larry N.; Carliles, Samuel; Carr, Michael; Castander, F. J.; Connolly, Andrew J.; Cool, R. J.; Cunha, C. E.; Csabai, István; Dalcanton, Julianne J.; Doi, Mamoru; Eisenstein, Daniel J.; Evans, Michael L.; Evans, N. W.; Fan, Xiaohui; Finkbeiner, Douglas P.; Friedman, S. D.; Frieman, Joshua A.; Fukugita, M.; Gillespie, Bruce; Gilmore, G.; Glazebrook, Karl; Gray, Jim; Grebel, Eva K.; Gunn, James E.; Haas, E. de; Hall, P. B.; Harvanek, Michael; Hawley, Suzanne L.; Hayes, J. J. E.; Heckman, Timothy M.; Hendry, John S.; Hennessy, G. S.; Hindsley, Robert B.; Herata, Christopher M.; Hogan, C. J.; Hogg, David W.; Holtzman, Jon A.; Ichikawa, S.; Ichikawa, Takashi; Ivezić, Željko; Jester, Sebastian; Johnston, David; Jorgensen, A. M.; Jurić, Mario; Kauffmann, Guinevere; Kent, Stephen M.; Kleinman, S. J.; Knapp, G. R.; Kniazev, A. Y.; Krön, Richard G.; Krzesiński, Jurek; Kuropatkin, N.; Lamb, D. Q.; Lampeitl, H.; Lee, Brian C.; Leger, R. French; Lema, Marcos; Lin, Huan; Long, Daneel C.; Loveday, Jon; Lupton, Robert H.; Mandelbaum, Rachel; Margon, B.; Martínez–Delgado, David; Matsubara, Takahiko; McGehee, P.; McKay, T. A.; Meiksen, Avery; Munn, Jeffrey A.; Nakajima, Reiko; Nash, T.; Neilsen, Eric H.; Newberg, Heidi Jo; Nichol, R. C.; Nieto-Santisteban, María; Nitta, A.; Oyaizu, Hiroaki; Okamura, S.; Ostriker, Jeremiah P.; Padmanabhan, Nikhil; Park, Changbom; Peoples, J.; Pier, Jeffrey R.; Pope, Adrian; Pourbaix, D.; Quinn, Thomas; Raddick, M. Jordan; Fiorenin, Paola Re; Richards, Gordon T.; Rechmond, Mechael W.; Rix, H. W.; Rockosi, Constance M.; Schlegel, David J.; Schneider, Donald P.; Scranton, Ryan; Seljak, Uroš; Sheldon, E.; Shimasaku, K.; Silvestri, Nicole M.; Smith, J. Allyn; Smolčić, Vernesa; Snedden, Stephanie A.; Stebbins, Albert; Stoughton, Chris; Strauss, Michael A.; SubbaRao, Mark; Suto, Yasushi; Szalay, Alexander S.; Szapudi, István; Szkody, Paula; Tegmark, Max; Thakar, Aniruddha R.; Tremonti, Christy; Tucker, D. L.; Uomoto, Alan; Berk, D. E. vanden; Vandenberg, Jan; Vidrih, S.; Vogeley, M.; Voges, W.; Vogt, Nicole P.; Weinberg, David H.; West, Andrew A.; White, Simon D. M.; Wilhite, Brian C.; Yanny, B.; Yocum, D. R.; York, Donald G.; Zehavi, Idit; Zibetti, S.; Zucker, D. B.

doi:10.1086/518864

Cited by 648 publications

(274 citation statements)

References 49 publications

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“…We use photometric and spectroscopic coverage from the sixth data release (DR6) of the Sloan Digital Sky Survey (SDSS; see York et al 2000;Stoughton et al 2002;Adelman-McCarthy et al 2007, and references therein). The survey, not yet finished but nearing completion, will eventually cover 10, 000 deg 2 in the northern galactic cap and a smaller region on the celestial equator.…”

Section: Optical Surveys: Sdssmentioning

confidence: 99%

A Unified Catalog of Radio Objects Detected by Nvss, First, Wenss, Gb6, and SDSS

Kimball

Ivezić

2008

The Astronomical Journal

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173

246

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We construct a catalog of radio sources detected by the Green Bank 6 cm survey GB6, Faint Images of the Radio Sky at Twenty cm (FIRST) and NRAO VLA 1 Sky Survey (NVSS) (20 cm), and Westerbork Northern Sky Survey (WENSS) (92 cm) radio surveys, and the Sloan Digital Sky Survey (SDSS) optical survey. The 2.7 million entries in the publicly-available master catalog are comprised of the closest three FIRST to NVSS matches (within 30 ) and vice versa, and unmatched sources from each survey. Entries are supplemented by data from the other radio and optical surveys, where available. All objects with even a small probability of physical association are included, such that catalog users can easily implement their own selection criteria for data analysis. We perform data analysis in the ∼3000 deg 2 region of sky where the surveys overlap, which contains 140,000 NVSS-FIRST sources, of which 64,000 are detected by WENSS and 12,000 by GB6. About one third of each sample is detected by the SDSS. An automated classification method based on 20 cm fluxes defines three radio morphology classes: complex, resolved, and compact. Radio color-magnitude-morphology diagrams for these classes show structure suggestive of strong underlying physical correlations. Complex and resolved sources tend to have a steep spectral slope (α ∼ −0.8) that is nearly constant from 6 to 92 cm, while the compact class (unresolved on ∼5 scale by FIRST) contains a significant number of flat-spectrum (α ∼ 0) sources. In the optically-detected sample, quasars dominate the flatspectrum compact sources while steep-spectrum and resolved objects contain substantial numbers of both quasars and galaxies. Differential radio counts of quasars and galaxies are similar at bright flux levels (>100 mJy at 20 cm), while at fainter levels the quasar counts are significantly reduced below galaxy counts. The optically-undetected sample is strongly biased toward steep-spectrum sources. In samples of quasars and galaxies with SDSS spectra (2885 and 1288 respectively), we find that radio properties such as spectral slope, morphology, and radio loudness are correlated with optical color and luminosity.

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Section: Optical Surveys: Sdssmentioning

confidence: 99%

A Unified Catalog of Radio Objects Detected by Nvss, First, Wenss, Gb6, and SDSS

Kimball

Ivezić

2008

The Astronomical Journal

Self Cite

173

246

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“…If an object's colors fit well to a template then it is assumed to be a star. To get the widest wavelength range of data with which to make comparisons, we compile all available PQ UBRIriz (determined using the absolute calibration), SDSS ugriz (data release 5; see Adelman-McCarthy et al 2007), Galaxy Evolution Explorer (GALEX) fn (data release 3; see Martin et al 2005), and 2MASS JHK measurements (Skrutskie et al 2006) of the variables. The spectral templates published by A. J. Pickles (Pickles 1998), which span wavelengths of 1150-12500 Å, are convolved with the transmission curves of the various surveys and fitted to the broadband measurements.…”

Section: Color Classificationmentioning

confidence: 99%

Highly Variable Objects in the Palomar-Quest Survey: A Blazar Search Using Optical Variability

Bauer

Baltay

Coppi

et al. 2009

ApJ

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We identify 3113 highly variable objects in 7200 deg 2 of the Palomar-QUEST (PQ) Survey, which each varied by more than 0.4 mag simultaneously in two broadband optical filters on timescales from hours to roughly 3.5 years. The primary goal of the selection is to find blazars by their well-known violent optical variability. Because most known blazars have been found in radio and/or X-ray wavelengths, a sample discovered through optical variability may have very different selection effects, elucidating the range of behavior possible in these systems. A set of blazars selected in this unusual manner will improve our understanding of the physics behind this extremely variable and diverse class of active galactic nucleus (AGN). The object positions, variability statistics, and color information are available using the PQ CasJobs server. The time domain is just beginning to be explored over large sky areas; we do not know exactly what a violently variable sample will hold. About 20% of the sample has been classified in the literature; over 70% of those objects are known or likely AGNs. The remainder largely consists of a variety of variable stars, including a number of RR Lyrae and cataclysmic variables.

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“…These focused on characterizing the three-dimensional topology and showed that, depending on the considered scale, topology can be useful in constraining both cosmological parameters and the galaxy formation mechanism. For example, Park et al (2005a) characterized the topology of the SDSS main galaxy sample from the New York University Value-Added Galaxy Catalog (NYU-VAGC; Blanton et al 2005), which has similar sky coverage to SDSS Data Release 4 (DR4; Adelman-McCarthy et al 2006), and presented the first clear demonstration of luminosity dependence of galaxy clustering topology (i.e., brighter galaxies show a stronger signal of meatball topology); more recently, Gott et al (2009) measured the three-dimensional LSS topology of the SDSS DR4plus luminous red galaxy (LRG) sample from the NYU-VAGC (a subsample of SDSS DR5; Adelman-McCarthy et al 2007) and found strong consistency with Gaussianity of the primordial fluctuations. In the latter case, the large available sample size allowed topology to be an important tool for testing galaxy formation models.…”

Section: Introductionmentioning

confidence: 99%

Topology of Luminous Red Galaxies From the Sloan Digital Sky Survey

Choi¹,

Kim²,

Rossi³

et al. 2013

ApJS

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We present measurements of the genus topology of luminous red galaxies (LRGs) from the Sloan Digital Sky Survey (SDSS) Data Release 7 catalog, with unprecedented statistical significance. To estimate the uncertainties in the measured genus, we construct 81 mock SDSS LRG surveys along the past light cone from Horizon Run 3, one of the largest N-body simulations to date, which evolved 7210 3 particles in a 10,815 h −1 Mpc box. After carefully modeling and removing all known systematic effects due to finite pixel size, survey boundary, radial and angular selection functions, shot noise, and galaxy biasing, we find that the observed genus amplitude reaches 272 at a 22 h −1 Mpc smoothing scale, with an uncertainty of 4.2%; the estimated error fully incorporates cosmic variance. This is the most accurate constraint on the genus amplitude to date and significantly improves on our previous results. In particular, the shape of the genus curve agrees very well with the mean topology of the SDSS LRG mock surveys in a Λ cold dark matter universe. However, comparison with simulations also shows small deviations of the observed genus curve from the theoretical expectation for Gaussian initial conditions. While these discrepancies are mainly driven by known systematic effects such as shot noise and redshift-space distortions, they do contain important cosmological information on the physical effects connected with galaxy formation, gravitational evolution, and primordial non-Gaussianity. We address the key role played by systematics on the genus curve and show how to accurately correct for their effects to recover the topology of the underlying matter. A future work will provide an interpretation of these deviations in the context of the local model of non-Gaussianity.

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The Fifth Data Release of the Sloan Digital Sky Survey

Cited by 648 publications

References 49 publications

A Unified Catalog of Radio Objects Detected by Nvss, First, Wenss, Gb6, and SDSS

A Unified Catalog of Radio Objects Detected by Nvss, First, Wenss, Gb6, and SDSS

Highly Variable Objects in the Palomar-Quest Survey: A Blazar Search Using Optical Variability

Topology of Luminous Red Galaxies From the Sloan Digital Sky Survey

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