The Third Data Release of the Sloan Digital Sky Survey

Abazajian, Kevork N.; Adelman-McCarthy, Jennifer K.; Agüeros, Marcel A.; Allam, S.; Anderson, K. S. J.; 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.; Brewington, H.; Briggs, John W.; Brinkmann, J.; Brunner, Róbert; Budavàri, Tamás; Carey, Larry N.; Castander, F. J.; Connolly, Andrew J.; Covey, Kevin R.; Csabai, István; Dalcanton, Julianne J.; Doi, Mamoru; Dong, Feng; Eisenstein, Daniel J.; Evans, Michael L.; Fan, Xiaohui; Finkbeiner, Douglas P.; Friedman, S. D.; Frieman, Joshua A.; Fukugita, M.; Gillespie, Bruce; Glazebrook, Karl; Gray, Jim; Grebel, Eva K.; Gunn, James E.; Gurbani, Vijay K.; Hall, Patrick B.; Hamabe, M.; Harbeck, Daniel; Harris, Frederick H.; Harris, Hugh C.; Harvanek, Michael; Hawley, Suzanne L.; Hayes, J. J. E.; Heckman, Timothy M.; Hendry, John S.; Hennessy, G. S.; Hindsley, Robert B.; Hogan, Craig J.; Hogg, David W.; Holmgren, D.; Holtzman, Jon A.; Ichikawa, S.; Ichikawa, Takashi; Ivezić, Željko; Jester, Sebastian; Johnston, David; Jorgensen, A. M.; Jurić, Mario; Kent, Stephen M.; Kleinman, S. J.; Knapp, G. R.; Kniazev, A. Y.; Krön, Richard G.; Krzesiński, Jurek; Lamb, D. Q.; Lampeitl, H.; Lee, Brian C.; Lin, Huan; Long, Daniel C.; Loveday, Jon; Lupton, Robert H.; Mannery, Edward J.; Margon, B.; Martínez–Delgado, David; Matsubara, Takahiko; McGehee, P.; McKay, Timothy A.; Meiksin, Avery; Ménard, Brice; Munn, Jeffrey A.; 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.; Owen, Russell; Padmanabhan, Nikhil; Pauls, George; Peoples, J.; Pier, Jeffrey R.; Pope, Adrian; Pourbaix, D.; Quinn, Thomas; Raddick, M. Jordan; Richards, Gordon T.; Richmond, M.; Hans-Rix, Walter; Rockosi, Constance M.; Schlegel, David J.; Schneider, Donald P.; Schroeder, Joshua J.; Scranton, Ryan; Sekiguchi, M.; Sheldon, E.; Shimasaku, K.; Silvestri, Nicole M.; Smith, J. Allyn; Smolić, 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:10.1086/427544

Cited by 654 publications

(308 citation statements)

References 23 publications

(9 reference statements)

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“…The galaxy pairs were selected from cross-matches between the 2MASS K s Extended Source Catalog (XSC; Jarrett et al 2000) and the galaxy catalog of SDSS-DR3 (Abazajian et al 2005). This sample includes all spectroscopically confirmed spiralspiral (S-S) and spiral-elliptical (S-E) pairs in a parent sample that is complete for primaries brighter than K = 12.5 mag, projected separations between 5 h −1 kpc and 20 h −1 kpc, and mass ratio ≤2.5.…”

Section: Pair Selectionmentioning

confidence: 99%

An investigation of star formation and dust attenuation in major mergers using ultraviolet and infrared data

Yuan

Takeuchi

Matsuoka

et al. 2012

A&A

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Merger processes play an important role in galaxy formation and evolution. To study the influence of merger processes on the evolution of dust properties and cosmic star formation rate, we investigate a local sample of major merger galaxies and a control sample of isolated galaxies using GALEX ultraviolet (UV) and Spitzer infrared (IR) images. Through a statistical study, we find that dust attenuation in merger galaxies is enhanced with respect to isolated galaxies. We find this enhancement is contributed mainly by spiral galaxies in spiral-spiral (S-S) pairs, and increases with the increasing stellar mass of a galaxy. Combining the IR and UV parts of star formation rates (SFRs), we then calculated the total SFRs and specific star formation rates (SSFRs). We find the SSFRs to be enhanced in merger galaxies. This enhancement depends on galaxy stellar mass and the companion's morphology, but depends little on whether the galaxy is a primary or secondary component or on the separation between two components. These results are consistent with a previous study based only on IR images. In addition, we investigate the nuclear contributions to SFRs. SFRs in paired galaxies are more concentrated in the central part of the galaxies than in isolate galaxies. Our studies of dust attenuation show that the nuclear parts of pairs most resemble ULIRGs. Including UV data in the present work not only provides reliable information on dust attenuation, but also refines analyses of SFRs.

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Section: Pair Selectionmentioning

confidence: 99%

An investigation of star formation and dust attenuation in major mergers using ultraviolet and infrared data

Yuan

Takeuchi

Matsuoka

et al. 2012

A&A

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“…Their catalog contained 9316 WDs, nearly 3.6 times the number of WDs found in the first SDSS WD catalog ) based on DR1 (Abazajian et al 2003) data, consistent with the ratio of spectroscopic sky coverage (4783 / 1360 square degrees) in DR4 vs. DR1. Harris et al (2006) have constructed a reduced propermotion based WD LF using the photometric sample from SDSS DR3 (Abazajian et al 2005) and proper motions from Monet et al (2003). The large data set available from SDSS enabled them to sample the LF within a magnitude range of ∼7 < M bol < 14 using 0.5 mag bins, with each bin containing hundreds of stars for quite excellent statistics.…”

Section: Introductionmentioning

confidence: 99%

A hot white dwarf luminosity function from the Sloan Digital Sky Survey

Krzesiński¹,

Kleinman²,

Nitta³

et al. 2009

A&A

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Aims. We present a hot white dwarf (WD) luminosity function (LF) using data taken from the Sloan Digital Sky Survey (SDSS) Data Release 4. We present and discuss a combined LF, along with separate DA and non-DA as LFs. We explore the completeness of our LFs and interpret a sudden drop in the non-DA LF near 2 M bol as a transition of the non-DA WD atmosphere into the DA one during WD evolution. Our LF extends roughly between −0.5 < M bol < 7 or equivalently, ∼120 000 K > T eff > ∼25 000 K. Our LF should now be useful for estimates of recent star formation and for studies of neutrino and other potential particle emission losses in hot WDs. Methods. To create a sample whose completeness can be characterized fully, we used stars whose spectra were obtained via the SDSS's "hot standard" target selection criteria. The hot standard stars were purposefully targeted to a high level of completeness by the SDSS for calibration purposes. We are fortunate that many of them are hot white dwarfs stars. We further limited the sample to stars with fitted temperatures exceeding 23 500 K and log g > 7.0. We determined stellar distances for our sample based on their absolute SDSS g filter magnitudes, derived from WD stellar atmosphere model fits to the SDSS stellar spectra. Results. We compared our LF with those of other researchers where overlap occurs; however, our LFs are unique in their extension to the most luminous/hottest WDs. The cool end of our LF connects with the hot end of previously determined SDSS WD LFs and agreement here is quite good. It is also good with previous non-SDSS WD LFs. We note distinct differences between the DA and non-DA LFs and discuss the reliability of the DA LF at its hot end. We have extended the range of luminosities covered in the most recent WD LFs. The SDSS sample is understood quite well and its exploration should contribute to a number of new insights into early white dwarf evolution.

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“…Here, we extend our DR1 results using SDSS Data Release 3 (DR3; Abazajian et al 2005 Nestor et al (2003) and Rao & Turnshek (2000) (see Rao et al 2005, these proceedings, for an updated discussion). We remove clearly spurious candidates by visually inspecting each Mg II spectrum.…”

Section: Resultsmentioning

confidence: 58%

Measuring the halo mass of Mg II absorbers from their cross-correlation with Luminous Red Galaxies

et al. 2005

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Abstract. We study the cross-correlation between 716 Mg II quasar absorption systems and ∼ 100,000 Luminous Red Galaxies (LRGs) selected from the Sloan Digital Sky Survey Data Release 3 in the redshift range 0.4 z 0.8. The Mg II systems were selected to have λλ2796 & 2803 rest-frame equivalent widths 1.0Å and identifications confirmed by the Fe II λ2600 or Mg I λ2852 lines. Over co-moving scales 0.2-13h −1 Mpc, the Mg II-LRG cross-correlation has an amplitude 0.69 ± 0.09 times that of the LRG-LRG auto-correlation. Since LRGs have halo-masses of 10 13 M⊙, this strong cross-correlation signal implies that the absorber host-galaxies have halo-masses 1-2 × 10 12 M⊙.

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The Third Data Release of the Sloan Digital Sky Survey

Cited by 654 publications

References 23 publications

An investigation of star formation and dust attenuation in major mergers using ultraviolet and infrared data

An investigation of star formation and dust attenuation in major mergers using ultraviolet and infrared data

A hot white dwarf luminosity function from the Sloan Digital Sky Survey

Measuring the halo mass of Mg II absorbers from their cross-correlation with Luminous Red Galaxies

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