The Second Data Release of the Sloan Digital Sky Survey

Abazajian, Kevork N.; Adelman-McCarthy, Jennifer K.; Agüeros, Marcel A.; Allam, S.; Severance, Kurt; Anderson, Scott F.; Annis, J.; Bahcall, Neta A.; Baldry, I. K.; Bastian, Steven; Berlind, Andreas A.; Bernardi, Mariangela; Blanton, Michael R.; Bochanski, John J.; Boroski, William N.; Briggs, John W.; Brinkmann, J.; Brunner, Róbert; Budavàri, Tamás; Carey, Larry N.; Carliles, Samuel; Castander, F. J.; Connolly, Andrew J.; Csabai, István; Doi, Mamoru; Dong, Feng; Eisenstein, Daniel J.; Evans, Michael L.; Fan, Xiaohui; Finkbeiner, Douglas P.; Friedman, S. D.; Frieman, Joshua A.; Fukugita, M.; Gal, R. R.; Gillespie, Bruce; Glazebrook, Karl; Gray, Jim; Grebel, Eva K.; Gunn, James E.; Gurbani, Vijay K.; Hall, Patrick B.; Hamabe, M.; Harris, Frederick H.; Harris, Hugh C.; Harvanek, Michael; Heckman, Timothy M.; Hendry, John S.; Hennessy, G. S.; Hindsley, Robert B.; Hogan, Craig J.; Hogg, David W.; Holmgren, D.; Ichikawa, S.; Ichikawa, Takashi; Ivezić, Željko; Jester, Sebastian; Johnston, David; Jorgensen, A. M.; Kent, Stephen M.; Kleinman, S. J.; Knapp, G. R.; Kniazev, A. Y.; Krön, Richard G.; Krzesiński, Jurek; Kunszt, Péter Z.; Kuropatkin, N.; Lamb, D. Q.; Lampeitl, H.; Lee, Brian C.; Leger, R. French; Li, Nolan; Lin, Huan; Loh, Y. S.; Long, Daniel C.; Loveday, Jon; Lupton, Robert H.; Malik, Tanu; Margon, B.; Matsubara, Takahiko; McGehee, P.; McKay, Timothy A.; Meiksin, Avery; Munn, Jeffrey A.; Nakajima, Reiko; Nash, T.; Neilsen, Eric H.; Newberg, Heidi Jo; Newman, Peter R.; Nichol, R. C.; Nicinski, Tom; Nieto-Santisteban, María; Nitta, A.; Okamura, S.; O’Mullane, W.; Ostriker, Jeremiah P.; Owen, Russell; Padmanabhan, Nikhil; Peoples, J.; Pier, Jeffrey R.; Pope, Adrian; Quinn, Thomas; Richards, Gordon T.; Richmond, M.; Hans-Rix, Walter; Rockosi, Constance M.; Schlegel, David J.; Schneider, Donald P.; Scranton, Ryan; Sekiguchi, M.; Seljak, Uroš; Sergey, G.; Sesar, Branimir; Sheldon, E.; Shimasaku, K.; Siegmund, Walter A.; Silvestri, Nicole M.; Smith, J. Allyn; Smolčić, Vernesa; Snedden, Stephanie A.; Stebbins, Albert; Stoughton, Chris; Strauss, Michael A.; Subba, Mark Rao; Szalay, Alexander S.; Szapudi, István; Szkody, Paula; Szokoly, G.; Tegmark, Max; Teodoro, L. F. A.; Thakar, Aniruddha R.; Tremonti, Christy; Tucker, D. L.; Uomoto, Alan; Berk, D. E. vanden; Vandenberg, Jan; Vogeley, Michael S.; Voges, W.; Vogt, Nicole P.; Walkowicz, Lucianne M.; Wang, Shu I.; Weinberg, David H.; West, Andrew A.; White, Simon D. M.; Wilhite, Brian C.; Xu, Y.; Yanny, B.; Yasuda, Naoki; Yip, C. W.; Yocum, D. R.; York, Donald G.; Zehavi, Idit; Zibetti, S.; Zucker, D. B.

doi:10.1086/421365

Cited by 1,016 publications

(499 citation statements)

References 40 publications

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“…The best linear combination of the exponential and de Vaucouleurs models is stored in a parameter called fracDeV (Abazajian et al 2004). An axial ratio (b/a) is given by this fitting procedure.…”

Section: The Datamentioning

confidence: 99%

Boxy Hα emission profiles in star-forming galaxies

Chen

Tremonti

et al. 2016

Mon. Not. R. Astron. Soc.

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We assemble a sample of disk star-forming galaxies from the Sloan Digital Sky Survey Data Release 7, studying the structure of Hα emission lines, finding a large fraction of this sample contains boxy Hα line profiles. This fraction depends on galaxy physical and geometric parameters in the following way: (1) it increases monotonically with star formation rate per unit area (Σ SFR ), and stellar mass (M * ), with the trend being much stronger with M * , from ∼0% at M * = 10 10 M ⊙ to about 50% at M * = 10 11 M ⊙ ; (2) the fraction is much smaller in face-on systems than in edge-on systems. It increases with galaxy inclination (i) while i < 60 • and is roughly a constant of 25% beyond this range; (3) for the sources which can be modeled well with two velocity components, blueshifted and redshifted from the systemic velocity, these is a positive correlation between the velocity difference of these two components and the stellar mass, with a slope similar to the Tully-Fisher relation; (4) the two components are very symmetric in the mean, both in velocity and in amplitude. The four findings listed above can be understood as a natural result of a rotating galaxy disk with a kpc-scale ring-like Hα emission region.

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Section: The Datamentioning

confidence: 99%

Boxy Hα emission profiles in star-forming galaxies

Chen

Tremonti

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The sharp drop in the number of systems with g > 23 is however a feature of the CV population rather than a limit to the survey sensitivity. SDSS photometry is available for the whole of the Legacy footprint, complete to a depth of 22.2 in the g band (Abazajian et al 2004). Slightly deeper photometry is available in areas observed under good seeing and low-sky-brightness conditions.…”

Section: Completeness Of the Crts CV Samplementioning

confidence: 99%

1000 cataclysmic variables from the Catalina Real-time Transient Survey

Breedt

Gänsicke

Drake

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Over six years of operation, the Catalina Real-time Transient Survey (CRTS) has identified 1043 cataclysmic variable (CV) candidates -the largest sample of CVs from a single survey to date. Here, we provide spectroscopic identification of 85 systems fainter than g ≥ 19, including three AM Canum Venaticorum binaries, one helium-enriched CV, one polar and one new eclipsing CV. We analyse the outburst properties of the full sample and show that it contains a large fraction of low-accretion-rate CVs with long outburst recurrence times. We argue that most of the high-accretion-rate dwarf novae in the survey footprint have already been found and that future CRTS discoveries will be mostly low-accretion-rate systems. We find that CVs with white-dwarf-dominated spectra have significantly fewer outbursts in their CRTS light curves compared to disc-dominated CVs, reflecting the difference in their accretion rates. Comparing the CRTS sample to other samples of CVs, we estimate the overall external completeness to be 23.6 per cent, but show that as much as 56 per cent of CVs have variability amplitudes that are too small to be selected using the transient selection criteria employed by current ground-based surveys. The full table of CRTS CVs, including their outburst and spectroscopic properties examined in this paper, is provided in the online materials.

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“…A compendium of technical details about individual pipelines and data processing can be found in Stoughton et al (2002), Abazajian et al (2003Abazajian et al ( , 2004, and on the SDSS web site (www.sdss.org).…”

Section: Data Processing Factorymentioning

confidence: 99%

SDSS data management and photometric quality assessment

et al. 2004

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Abstract. We summarize the Sloan Digital Sky Survey data acquisition and processing steps, and describe runQA, a pipeline designed for automated data quality assessment. In particular, we show how the position of the stellar locus in color-color diagrams can be used to estimate the accuracy of photometric zeropoint calibration to better than 0.01 mag in 0.03 deg 2 patches. Using this method, we estimate that typical photometric zeropoint calibration errors for SDSS imaging data are not larger than ∼ 0.01 mag in the g, r, and i bands, 0.02 mag in the z band, and 0.03 mag in the u band (root-mean-scatter for zeropoint offsets).

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The Second Data Release of the Sloan Digital Sky Survey

Cited by 1,016 publications

References 40 publications

Boxy Hα emission profiles in star-forming galaxies

Boxy Hα emission profiles in star-forming galaxies

1000 cataclysmic variables from the Catalina Real-time Transient Survey

SDSS data management and photometric quality assessment

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