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102 results on '"Annis, James"'

1. Probing Galaxy Evolution in Massive Clusters Using ACT and DES: Splashback as a Cosmic Clock

Author

Adhikari, Susmita, Shin, Tae-hyeon, Jain, Bhuvnesh, Hilton, Matt, Baxter, Eric, Chang, Chihway, Wechsler, Risa H., Battaglia, Nick, Bond, J. Richard, Bocquet, Sebastian, DeRose, Joseph, Choi, Steve K., Devlin, Mark, Dunkley, Jo, Evrard, August E., Ferraro, Simone, Hill, J. Colin, Hughes, John P., Gallardo, Patricio A., Lokken, Martine, MacInnis, Amanda, McMahon, Jeffrey, Madhavacheril, Mathew S., Nati, Frederico, Newburgh, Laura B., Niemack, Michael D., Page, Lyman A., Palmese, Antonella, Partridge, Bruce, Rozo, Eduardo, Rykoff, Eli, Salatino, Maria, Schillaci, Alessandro, Sehgal, Neelima, Sif��n, Crist��bal, To, Chun-Hao, Wollack, Ed, Wu, Hao-Yi, Xu, Zhilei, Aguena, Michel, Allam, Sahar, Amon, Alexandra, Annis, James, Avila, Santiago, Bacon, David, Bertin, Emmanuel, Bhargava, Sunayana, Brooks, David, Burke, David L., Rosell, Aurelio C., Kind, Matias Carrasco, Carretero, Jorge, Castander, Francisco Javier, Choi, Ami, Costanzi, Matteo, da Costa, Luiz N., De Vicente, Juan, Desai, Shantanu, Diehl, Thomas H., Doel, Peter, Everett, Spencer, Ferrero, Ismael, Fert��, Agn��s, Flaugher, Brenna, Fosalba, Pablo, Frieman, Josh, Garc��a-Bellido, Juan, Gaztanaga, Enrique, Gruen, Daniel, Gruendl, Robert A., Gschwend, Julia, Gutierrez, Gaston, Hartley, Will G., Hinton, Samuel R., Hollowood, Devon L., Honscheid, Klaus, James, David J., Jeltema, Tesla, Kuehn, Kyler, Kuropatkin, Nikolay, Lahav, Ofer, Lima, Marcos, Maia, Marcio A. G., Marshall, Jennifer L., Martini, Paul, Melchior, Peter, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Ogando, Ricardo L. C., Paz-Chinch��n, Francisco, Malag��n, Andr��s Plazas, Sanchez, Eusebio, Santiago, Basilio, Scarpine, Vic, Serrano, Santiago, Sevilla-Noarbe, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, Suchyta, Eric, Swanson, Molly E. C., Varga, Tamas N., Wilkinson, Reese D., Zhang, Yuanyuan, Austermann, Jason E., Beall, James A., Becker, Daniel T., Denison, Edward V., Duff, Shannon M., Hilton, Gene C., Hubmayr, Johannes, Ullom, Joel N., Van Lanen, Jeff, Vale, Leila R., Collaboration, DES, Collaboration, ACT, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), Adhikari, S, Shin, T, Jain, B, Hilton, M, Baxter, E, Chang, C, Wechsler, R, Battaglia, N, Bond, J, Bocquet, S, Choi, S, Derose, J, Devlin, M, Dunkley, J, Evrard, A, Ferraro, S, Hill, J, Hughes, J, Gallardo, P, Lokken, M, Macinnis, A, Madhavacheril, M, Mcmahon, J, Nati, F, Newburgh, L, Niemack, M, Page, L, Palmese, A, Partridge, B, Rozo, E, Rykoff, E, Salatino, M, Schillaci, A, Sehgal, N, Sifon, C, To, C, Wollack, E, Wu, H, Xu, Z, Aguena, M, Allam, S, Amon, A, Annis, J, Avila, S, Bacon, D, Bertin, E, Bhargava, S, Brooks, D, Burke, D, Rosell, A, Kind, M, Carretero, J, Castander, F, Choi, A, Costanzi, M, Da Costa, L, Vicente, J, Desai, S, Diehl, T, Doel, P, Everett, S, Ferrero, I, Ferte, A, Flaugher, B, Fosalba, P, Frieman, J, Garcia-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, R, Gschwend, J, Gutierrez, G, Hartley, W, Hinton, S, Hollowood, D, Honscheid, K, James, D, Jeltema, T, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, M, Marshall, J, Martini, P, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, L. C. Ogando, R, Paz-Chinchon, F, Malagon, A, Sanchez, E, Santiago, B, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, E. C. Swanson, M, Varga, T, Wilkinson, R, Zhang, Y, Austermann, J, Beall, J, Becker, D, Denison, E, Duff, S, Hilton, G, Hubmayr, J, Ullom, J, Lanen, J, Vale, L, Adhikari, S., Shin, T. -H., Jain, B., Hilton, M., Baxter, E., Chang, C., Wechsler, R. H., Battaglia, N., Bond, J. R., Bocquet, S., Choi, S. K., Derose, J., Devlin, M., Dunkley, J., Evrard, A. E., Ferraro, S., Hill, J. C., Hughes, J. P., Gallardo, P. A., Lokken, M., Macinnis, A., Madhavacheril, M. S., Mcmahon, J., Nati, F., Newburgh, L. B., Niemack, M. D., Page, L. A., Palmese, A., Partridge, B., Rozo, E., Rykoff, E., Salatino, M., Schillaci, A., Sehgal, N., Sifon, C., C. -H., To, Wollack, E., H. -Y., Wu, Xu, Z., Aguena, M., Allam, S., Amon, A., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. C., Kind, M. C., Carretero, J., Castander, F. J., Choi, A., Costanzi, M., Da Costa, L. N., Vicente, J. D., Desai, S., Diehl, T. H., Doel, P., Everett, S., Ferrero, I., Ferte, A., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., L. C. Ogando R., Paz-Chinchon, F., Malagon, A. P., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., E. C. Swanson M., Varga, T. N., Wilkinson, R. D., Zhang, Y., Austermann, J. E., Beall, J. A., Becker, D. T., Denison, E. V., Duff, S. M., Hilton, G. C., Hubmayr, J., Ullom, J. N., Lanen, J. V., and Vale, L. R.

Subjects
Galaxy dark matter halos, 010308 nuclear & particles physics, FOS: Physical sciences, Cold dark matter, Astronomy and Astrophysics, Galaxy clusters, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology, SZ effect, Galaxy cluster, Surveys, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxy evolution, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy kinematics
Abstract

Adhikari, S., et al. (DES and ACT Collaboration), We measure the projected number density profiles of galaxies and the splashback feature in clusters selected by the Sunyaev-Zel'dovich effect from the Advanced Atacama Cosmology Telescope (AdvACT) survey using galaxies observed by the Dark Energy Survey (DES). The splashback radius is consistent with CDM-only simulations and is located at 2.4-0.4+0.3 Mpc h-1. We split the galaxies on color and find significant differences in their profile shapes. Red and green-valley galaxies show a splashback-like minimum in their slope profile consistent with theory, while the bluest galaxies show a weak feature at a smaller radius. We develop a mapping of galaxies to subhalos in simulations and assign colors based on infall time onto their hosts. We find that the shift in location of the steepest slope and different profile shapes can be mapped to the average time of infall of galaxies of different colors. The steepest slope traces a discontinuity in the phase space of dark matter halos. By relating spatial profiles to infall time, we can use splashback as a clock to understand galaxy quenching. We find that red galaxies have on average been in clusters over 3.2 Gyr, green galaxies about 2.2 Gyr, while blue galaxies have been accreted most recently and have not reached apocenter. Using the full radial profiles, we fit a simple quenching model and find that the onset of galaxy quenching occurs after a delay of about a gigayear and that galaxies quench rapidly thereafter with an exponential timescale of 0.6 Gyr., The DES Data Management System is supported by the NSF under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Unionʼs Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2)

Published
2021

2. Dust Reverberation Mapping in Distant Quasars from Optical and Mid-infrared Imaging Surveys.

Author

Yang, Qian, Shen, Yue, Liu, Xin, Aguena, Michel, Annis, James, Avila, Santiago, Banerji, Manda, Bertin, Emmanuel, Brooks, David, Burke, David, Rosell, Aurelio Carnero, Kind, Matias Carrasco, da Costa, Luiz, De Vicente, Juan, Desai, Shantanu, Diehl, H. Thomas, Doel, Peter, Flaugher, Brenna, Fosalba, Pablo, and Frieman, Josh

Subjects
QUASARS, ACTIVE galactic nuclei, OPTICAL images, DUST, DISKS (Astrophysics), ACCRETION disks
Abstract

The size of the dust torus in active galactic nuclei (AGNs) and their high-luminosity counterparts, quasars, can be inferred from the time delay between UV/optical accretion disk continuum variability and the response in the mid-infrared (MIR) torus emission. This dust reverberation mapping (RM) technique has been successfully applied to ∼70 z ≲ 0.3 AGNs and quasars. Here we present first results of our dust RM program for distant quasars covered in the Sloan Digital Sky Survey Stripe 82 region combining ∼20 yr ground-based optical light curves with 10 yr MIR light curves from the WISE satellite. We measure a high-fidelity lag between W1 band (3.4 μm) and g band for 587 quasars over 0.3 ≲ z ≲ 2 () and two orders of magnitude in quasar luminosity. They tightly follow (intrinsic scatter ∼0.17 dex in lag) the IR lag–luminosity relation observed for z < 0.3 AGNs, revealing a remarkable size–luminosity relation for the dust torus over more than four decades in AGN luminosity, with little dependence on additional quasar properties such as Eddington ratio and variability amplitude. This study motivates further investigations in the utility of dust RM for cosmology and strongly endorses a compelling science case for the combined 10 yr Vera C. Rubin Observatory Legacy Survey of Space and Time (optical) and 5 yr Nancy Grace Roman Space Telescope 2 μm light curves in a deep survey for low-redshift AGN dust RM with much lower luminosities and shorter, measurable IR lags. The compiled optical and MIR light curves for 7384 quasars in our parent sample are made public with this work. [ABSTRACT FROM AUTHOR]

Published
2020
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4. THE MULTI-OBJECT, FIBER-FED SPECTROGRAPHS FOR THE SLOAN DIGITAL SKY SURVEY AND THE BARYON OSCILLATION SPECTROSCOPIC SURVEY.

Author

SMEE, STEPHEN A., GUNN, JAMES E., UOMOTO, ALAN, ROE, NATALIE, SCHLEGEL, DAVID, ROCKOSI, CONSTANCE M., CARR, MICHAEL A., LEGER, FRENCH, DAWSON, KYLE S., OLMSTEAD, MATTHEW D., BRINKMANN, JON, OWEN, RUSSELL, BARKHOUSER, ROBERT H., HONSCHEID, KLAUS, HARDING, PAUL, LONG, DAN, LUPTON, ROBERT H., LOOMIS, CRAIG, ANDERSON, LAUREN, and ANNIS, JAMES

Published
2013
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5. THE SLOAN DIGITAL SKY SURVEY CO-ADD: CROSS-CORRELATION WEAK LENSING AND TOMOGRAPHY OF GALAXY CLUSTERS.

Author

SIMET, MELANIE, KUBO, JEFFREY M., DODELSON, SCOTT, ANNIS, JAMES T., JIANGANG HAO, JOHNSTON, DAVID, HUAN LIN, REIS, RIBAMAR R. R., SOARES-SANTOS, MARCELLE, and HEE-JONG SEO

Subjects
GALAXY clusters, GRAVITATIONAL lenses, TOMOGRAPHY, REDSHIFT
Abstract

The shapes of distant galaxies are sheared by intervening galaxy clusters. We examine this effect in Stripe 82, a 275 deg² region observed multiple times in the Sloan Digital Sky Survey (SDSS) and co-added to achieve greater depth. We obtain a mass-richness calibration that is similar to other SDSS analyses, demonstrating that the co-addition process did not adversely affect the lensing signal. We also propose a new parameterization of the effect of tomography on the cluster lensing signal which does not require binning in redshift, and we show that using this parameterization we can detect tomography for stacked clusters at varying redshifts. Finally, due to the sensitivity of the tomographic detection to accurately marginalize over the effect of the cluster mass, we show that tomography at low redshift (where dependence on exact cosmological models is weak) can be used to constrain mass profiles in clusters. [ABSTRACT FROM AUTHOR]

Published
2012
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6. THE SLOAN DIGITAL SKY SURVEY CO-ADD: A GALAXY PHOTOMETRIC REDSHIFT CATALOG.

Author

REIS, RIBAMAR R. R., SOARES-SANTOS, MARCELLE, ANNIS, JAMES, DODELSON, SCOTT, JIANGANG HAO, JOHNSTON, DAVID, KUBO, JEFFREY, HUAN LIN, HEE-JONG SEO, and SIMET, MELANIE

Subjects
GALAXIES, ARTIFICIAL neural networks, PHOTOMETRY, METAPHYSICAL cosmology, VERY large telescopes
Abstract

We present and describe a catalog of galaxy photometric redshifts (photo-z) for the Sloan Digital Sky Survey (SDSS) Co-add Data. We use the artificial neural network (ANN) technique to calculate the photo-z and the nearest neighbor error method to estimate photo-z errors for ~13 million objects classified as galaxies in the co-add with r < 24.5. The photo-z and photo-z error estimators are trained and validated on a sample of ~83,000 galaxies that have SDSS photometry and spectroscopic redshifts measured by the SDSS Data Release 7 (DR7), the Canadian Network for Observational Cosmology Field Galaxy Survey, the Deep Extragalactic Evolutionary Probe Data Release 3, the VIsible imaging Multi-Object Spectrograph--Very Large Telescope Deep Survey, and the WiggleZ Dark Energy Survey. For the best ANN methods we have tried, we find that 68% of the galaxies in the validation set have a photo-z error smaller than σ68 = 0.031. After presenting our results and quality tests, we provide a short guide for users accessing the public data. [ABSTRACT FROM AUTHOR]

Published
2012
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7. INTRINSIC ALIGNMENT OF CLUSTER GALAXIES: THE REDSHIFT EVOLUTION.

Author

HAO, JIANGANG, KUBO, JEFFREY M., FELDMANN, ROBERT, ANNIS, JAMES, JOHNSTON, DAVID E., LIN, HUAN, and MCKAY, TIMOTHY A.

Subjects
GALAXY clusters, REDSHIFT, ASTRONOMICAL photometry, ASTROPHYSICS
Abstract

We present measurements of two types of cluster galaxy alignments based on a volume limited and highly pure (≥90%) sample of clusters from the GMBCG catalog derived from Data Release 7 of the Sloan Digital Sky Survey (SDSS DR7). We detect a clear brightest cluster galaxy (BCG) alignment (the alignment of major axis of the BCG toward the distribution of cluster satellite galaxies). We find that the BCG alignment signal becomes stronger as the redshift and BCG absolute magnitude decrease and becomes weaker as BCG stellar mass decreases. No dependence of the BCG alignment on cluster richness is found. We can detect a statistically significant (≥3<δ) satellite alignment (the alignment of the major axes of the cluster satellite galaxies toward the BCG) only when we use the isophotal fit position angles (P.A.s), and the satellite alignment depends on the apparent magnitudes rather than the absolute magnitudes of the BCGs. This suggests that the detected satellite alignment based on isophotal P.A.s from the SDSS pipeline is possibly due to the contamination from the diffuse light of nearby BCGs. We caution that this should not be simply interpreted as non-existence of the satellite alignment, but rather that we cannot detect them with our current photometric SDSS data. We perform our measurements on both SDSS r-band and i-band data, but do not observe a passband dependence of the alignments. [ABSTRACT FROM AUTHOR]

Published
2011
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8. The Sixth Data Release of the Sloan Digital Sky Survey.

Author

Adelman-McCarthy, Jennifer K., Agüeros, Marcel A., Allam, Sahar S., Prieto, Carlos Allende, Anderson, Kurt S.J., Anderson, Scott F., Annis, James, Bahcall, Neta A., Bailer-Jones, C. A. L., Baldry, Ivan K., Barentine, J. C., Bassett, Bruce A., Becker, Andrew C., Beers, Timothy C., Bell, Eric F., Berlind, Andreas A., Bernardi, Mariangela, Blanton, Michael R., Bochanski, John J., and Boroski, William N.

Published
2008
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10. Observations and Theoretical Implications of the Large-Separation Lensed Quasar SDSS J1004+4112.

Author

Oguri, Masamune, Inada, Naohisa, Keeton, Charles R., Pindor, Bartosz, Hennawi, Joseph F., Gregg, Michael D., Becker, Robert H., Chiu, Kuenley, Zheng, Wei, Ichikawa, Shin-Ichi, Suto, Yasushi, Turner, Edwin L., Annis, James, Bahcall, Neta A., Brinkmann, Jonathan, Castander, Francisco J., Eisenstein, Daniel J., Frieman, Joshua A., Goto, Tomotsugu, and Gunn, James E.

Published
2004
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11. Galaxy Clustering in Early Sloan Digital Sky Survey Redshift Data.

Author

Zehavi, Idit, Blanton, Michael R., Frieman, Joshua A., Weinberg, David H., Mo, Houjun J., Strauss, Michael A., Anderson, Scott F., Annis, James, Bahcall, Neta A., Bernardi, Mariangela, Briggs, John W., Brinkmann, Jon, Burles, Scott, Carey, Larry, Castander, Francisco J., Connolly, Andrew J., Csabai, Istvan, Dalcanton, Julianne J., Dodelson, Scott, and Doi, Mamoru

Published
2002
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12. Identification of A-colored Stars and Structure in the Halo of the Milky Way from Sloan Digital Sky Survey Commissioning DataBased on observations obtained with the Sloan Digital Sky Survey and with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium.

Author

Yanny, Brian, Newberg, Heidi Jo, Kent, Steve, Laurent-Muehleisen, Sally A., Pier, Jeffrey R., Richards, Gordon T., Stoughton, Chris, Anderson, Jr. John E., Annis, James, Brinkmann, J., Chen, Bing, Csabai, István, Doi, Mamoru, Fukugita, Masataka, Hennessy, G. S., Ivezić, Željko, Knapp, G. R., Lupton, Robert, Munn, Jeffrey A., and Nash, Thomas

Published
2000
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13. The Discovery of a High-Redshift Quasar without Emission Lines from Sloan Digital Sky Survey Commissioning DataBased on observations obtained with the Sloan Digital Sky Survey and the Apache Point Observatory 3.5 m telescope, which are owned and operated by the Astrophysical Research Consortium, the Very Large Array, the Keck Telescope, and the Steward Observatory 2.3 m telescope.

Author

Fan, Xiaohui, Strauss, Michael A., Gunn, James E., Lupton, Robert H., Carilli, C. L., Rupen, M. P., Schmidt, Gary D., Moustakas, Leonidas A., Davis, Marc, Annis, James, Bahcall, Neta A., Brinkmann, J., Brunner, Robert J., Csabai, István, Doi, Mamoru, Fukugita, Masataka, Heckman, Timothy M., Hennessy, G. S., Hindsley, Robert B., and Ivezić, Željko

Published
1999
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14. The Third Data Release of the Sloan Digital Sky Survey

Author

Abazajian, Kevork, Adelman-McCarthy, Jennifer K., Agüeros, Marcel A., Allam, Sahar S., Anderson, Kurt S. J., Anderson, Scott F., Annis, James, Bahcall, Neta A., Baldry, Ivan K., Bastian, Steven, Berlind, Andreas, Bernardi, Mariangela, Blanton, Michael R., Bochanski, John J. Jr., Boroski, William N., Brewington, Howard J., Briggs, John W., Brinkmann, J., Brunner, Robert J., Budavári, Tamás, Carey, Larry N., Castander, Francisco J., Connolly, A. J., Covey, Kevin R., Csabai, István, Dalcanton, Julianne J., Doi, Mamoru, Dong, Feng, Eisenstein, Daniel James, Evans, Michael L., Fan, Xiaohui, Finkbeiner, Douglas, Friedman, Scott D., Frieman, Joshua A., Fukugita, Masataka, Gillespie, Bruce, Glazebrook, Karl, Gray, Jim, Grebel, Eva K., Gunn, James E., Gurbani, Vijay K., Hall, Patrick B., Hamabe, Masaru, Harbeck, Daniel, Harris, Frederick H., Harris, Hugh C., Harvanek, Michael, Hawley, Suzanne L., Hayes, Jeffrey, Heckman, Timothy M., Hendry, John S., Hennessy, Gregory S., Hindsley, Robert B., Hogan, Craig J., Hogg, David W., Holmgren, Donald J., Holtzman, Jon A., Ichikawa, Shin-ichi, Ichikawa, Takashi, Ivezic, Zeljko, Jester, Sebastian, Johnston, David E., Jorgensen, Anders M., Juri?, Mario, Kent, Stephen M., Kleinman, S. J., Knapp, G. R., Kniazev, Alexei Yu., Kron, Richard G., Krzesinski, Jurek, Lamb, Donald Q., Lampeitl, Hubert, Lee, Brian C., Lin, Huan, Long, Daniel C., Loveday, Jon, Lupton, Robert H., Mannery, Ed, Margon, Bruce, Martínez-Delgado, David, Matsubara, Takahiko, McGehee, Peregrine M., McKay, Timothy A., Meiksin, Avery, Ménard, Brice, Munn, Jeffrey A., Nash, Thomas, Neilsen, Eric H. Jr., Newberg, Heidi Jo, Newman, Peter R., Nichol, Robert C., Nicinski, Tom, Nieto-Santisteban, Maria, Nitta, Atsuko, Okamura, Sadanori, O, William, Owen, Russell, Padmanabhan, Nikhil, Pauls, George, Peoples, John, Pier, Jeffrey R., Pope, Adrian C., Pourbaix, Dimitri, Quinn, Thomas R., Raddick, M. Jordan, Richards, Gordon T., Richmond, Michael W., Rix, Hans-Walter, Rockosi, Constance M., Schlegel, David J., Schneider, Donald P., Schroeder, Joshua, Scranton, Ryan, Sekiguchi, Maki, Sheldon, Erin, Shimasaku, Kazu, Silvestri, Nicole M., Smith, J. Allyn, Smol?i?, Vernesa, Snedden, Stephanie A., Stebbins, Albert, Stoughton, Chris, Strauss, Michael A., SubbaRao, Mark, Szalay, Alexander S., Szapudi, István, Szkody, Paula, Szokoly, Gyula P., Tegmark, Max, Teodoro, Luis, Thakar, Aniruddha R., Tremonti, Christy, Tucker, Douglas L., Uomoto, Alan, Vanden Berk, Daniel E., Vandenberg, Jan, Vogeley, Michael S., Voges, Wolfgang, Vogt, Nicole P., Walkowicz, Lucianne M., Wang, Shu-i, Weinberg, David H., West, Andrew A., White, Simon D. M., Wilhite, Brian C., Xu, Yongzhong, Yanny, Brian, Yasuda, Naoki, Yip, Ching-Wa, Yocum, D. R., York, Donald G., Zehavi, Idit, Zibetti, Stefano, and Zucker, Daniel B.

Subjects
atlases, catalogs, surveys
Abstract

This paper describes the Third Data Release of the Sloan Digital Sky Survey (SDSS). This release, containing data taken up through 2003 June, includes imaging data in five bands over 5282 deg2, photometric and astrometric catalogs of the 141 million objects detected in these imaging data, and spectra of 528,640 objects selected over 4188 deg2. The pipelines analyzing both images and spectroscopy are unchanged from those used in our Second Data Release., Astronomy

Published
2005
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15. The Second Data Release of the Sloan Digital Sky Survey

Author

Abazajian, Kevork, Adelman-McCarthy, Jennifer K., Agüeros, Marcel A., Allam, Sahar S., Anderson, Kurt, S. J., Anderson, Scott F., Annis, James, Bahcall, Neta A., Baldry, Ivan K., Bastian, Steven, Berlind, Andreas, Bernardi, Mariangela, Blanton, Michael R., Bochanski, John J. Jr., Boroski, William N., Briggs, John W., Brinkmann, J., Brunner, Robert J., Budavári, Tamás, Carey, Larry N., Carliles, Samuel, Castander, Francisco J., Connolly, A. J., Csabai, István, Doi, Mamoru, Dong, Feng, Eisenstein, Daniel James, Evans, Michael L., Fan, Xiaohui, Finkbeiner, Douglas, Friedman, Scott D., Frieman, Joshua A., Fukugita, Masataka, Gal, Roy R., Gillespie, Bruce, Glazebrook, Karl, Gray, Jim, Grebel, Eva K., Gunn, James E., Gurbani, Vijay K., Hall, Patrick B., Hamabe, Masaru, Harris, Frederick H., Harris, Hugh C., Harvanek, Michael, Heckman, Timothy M., Hendry, John S., Hennessy, Gregory S., Hindsley, Robert B., Hogan, Craig J., Hogg, David W., Holmgren, Donald J., Ichikawa, Shin-ichi, Ichikawa, Takashi, Ivezic, Zeljko, Jester, Sebastian, Johnston, David E., Jorgensen, Anders M., Kent, Stephen M., Kleinman, S. J., Knapp, G. R., Kniazev, Alexei Yu., Kron, Richard G., Krzesinski, Jurek, Kunszt, Peter Z., Kuropatkin, Nickolai, Lamb, Donald Q., Lampeitl, Hubert, Lee, Brian C., Leger, R. French, Li, Nolan, Lin, Huan, Loh, Yeong-Shang, Long, Daniel C., Loveday, Jon, Lupton, Robert H., Malik, Tanu, Margon, Bruce, Matsubara, Takahiko, McGehee, Peregrine M., McKay, Timothy A., Meiksin, Avery, Munn, Jeffrey A., Nakajima, Reiko, Nash, Thomas, Neilsen, Eric H. Jr., Newberg, Heidi Jo, Newman, Peter R., Nichol, Robert C., Nicinski, Tom, Nieto-Santisteban, Maria, Nitta, Atsuko, Okamura, Sadanori, O, William, Ostriker, Jeremiah P., Owen, Russell, Padmanabhan, Nikhil, Peoples, John, Pier, Jeffrey R., Pope, Adrian C., Quinn, Thomas R., Richards, Gordon T., Richmond, Michael W., Rix, Hans-Walter, Rockosi, Constance M., Schlegel, David J., Schneider, Donald P., Scranton, Ryan, Sekiguchi, Maki, Seljak, Uros, Sergey, Gary, Sesar, Branimir, Sheldon, Erin, Shimasaku, Kazu, Siegmund, Walter A., Silvestri, Nicole M., Smith, J. Allyn, Smolčić, Vernesa, Snedden, Stephanie A., Stebbins, Albert, Stoughton, Chris, Strauss, Michael A., SubbaRao, Mark, Szalay, Alexander S., Szapudi, István, Szkody, Paula, Szokoly, Gyula P., Tegmark, Max, Teodoro, Luis, Thakar, Aniruddha R., Tremonti, Christy, Tucker, Douglas L., Uomoto, Alan, Vanden Berk, Daniel E., Vandenberg, Jan, Vogeley, Michael S., Voges, Wolfgang, Vogt, Nicole P., Walkowicz, Lucianne M., Wang, Shu-i, Weinberg, David H., West, Andrew A., White, Simon D. M., Wilhite, Brian C., Xu, Yongzhong, Yanny, Brian, Yasuda, Naoki, Yip, Ching-Wa, Yocum, D. R., York, Donald G., Zehavi, Idit, Zibetti, Stefano, and Zucker, Daniel B.

Subjects
atlases, catalogs, surveys
Abstract

The Sloan Digital Sky Survey (SDSS) has validated and made publicly available its Second Data Release. This data release consists of 3324 deg2 of five-band (ugriz) imaging data with photometry for over 88 million unique objects, 367,360 spectra of galaxies, quasars, stars, and calibrating blank sky patches selected over 2627 deg2 of this area, and tables of measured parameters from these data. The imaging data reach a depth of r ≈ 22.2 (95% completeness limit for point sources) and are photometrically and astrometrically calibrated to 2% rms and 100 mas rms per coordinate, respectively. The imaging data have all been processed through a new version of the SDSS imaging pipeline, in which the most important improvement since the last data release is fixing an error in the model fits to each object. The result is that model magnitudes are now a good proxy for point-spread function magnitudes for point sources, and Petrosian magnitudes for extended sources. The spectroscopy extends from 3800 to 9200 Å at a resolution of 2000. The spectroscopic software now repairs a systematic error in the radial velocities of certain types of stars and has substantially improved spectrophotometry. All data included in the SDSS Early Data Release and First Data Release are reprocessed with the improved pipelines and included in the Second Data Release. Further characteristics of the data are described, as are the data products themselves and the tools for accessing them., Astronomy

Published
2004
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16. Sloan Digital Sky Survey Imaging of Low Galactic Latitude Fields: Technical Summary and Data Release

Author

Finkbeiner, Douglas, Padmanabhan, Nikhil, Schlegel, David J., Carr, Michael A., Gunn, James E., Rockosi, Constance M., Sekiguchi, Maki, Lupton, Robert H., Knapp, G. R., Ivezic, Zeljko, Blanton, Michael R., Hogg, David W., Adelman-McCarthy, Jennifer K., Annis, James, Hayes, Jeffrey, Kinney, Ellynne, Long, Daniel C., Seljak, Uros, Strauss, Michael A., Yanny, Brian, Agüeros, Marcel A., Allam, Sahar S., Anderson, Scott F., Bahcall, Neta A., Baldry, Ivan K., Bernardi, Mariangela, Boroski, William N., Briggs, John W., Brinkmann, J., Brunner, Robert J., Budavári, Tamás, Castander, Francisco J., Covey, Kevin R., Csabai, István, Doi, Mamoru, Dong, Feng, Eisenstein, Daniel James, Fan, Xiaohui, Friedman, Scott D., Fukugita, Masataka, Gillespie, Bruce, Grebel, Eva K., Gurbani, Vijay K., de Haas, Ernst, Harris, Frederick H., Hendry, John S., Hennessy, Gregory S., Jester, Sebastian, Johnston, David E., Jorgensen, Anders M., Juric, Mario, Kent, Stephen M., Kniazev, Alexei Yu., Krzesinski, Jurek, Leger, R. French, Lin, Huan, Loveday, Jon, Mannery, Ed, Martínez-Delgado, David, McGehee, Peregrine M., Meiksin, Avery, Munn, Jeffrey A., Neilsen, Eric H. Jr., Newman, Peter R., Nitta, Atsuko, Pauls, George, Quinn, Thomas R., Rafikov, R. R., Richards, Gordon T., Richmond, Michael W., Schneider, Donald P., Schroeder, Joshua, Shimasaku, Kazu, Siegmund, Walter A., Smith, J. Allyn, Snedden, Stephanie A., Stebbins, Albert, Szalay, Alexander S., Szokoly, Gyula P., Tegmark, Max, Tucker, Douglas L., Uomoto, Alan, Vanden Berk, Daniel E., Weinberg, David H., West, Andrew A., Yasuda, Naoki, Yocum, D. R., York, Donald G., and Zehavi, Idit

Subjects
atlases, catalogs, surveys
Abstract

The Sloan Digital Sky Survey (SDSS) mosaic camera and telescope have obtained five-band optical-wavelength imaging near the Galactic plane outside of the nominal survey boundaries. These additional data were obtained during commissioning and subsequent testing of the SDSS observing system, and they provide unique wide-area imaging data in regions of high obscuration and star formation, including numerous young stellar objects, Herbig-Haro objects, and young star clusters. Because these data are outside the survey regions in the Galactic caps, they are not part of the standard SDSS data releases. This paper presents imaging data for 832 square degrees of sky (including repeats), in the star-forming regions of Orion, Taurus, and Cygnus. About 470 deg2 are now released to the public, with the remainder to follow at the time of SDSS Data Release 4. The public data in Orion include the star-forming region NGC 2068/NGC 2071/HH 24 and a large part of Barnard's loop., Astronomy

Published
2004
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17. The Three‐Dimensional Power Spectrum of Galaxies from the Sloan Digital Sky Survey

Author

Tegmark, Max, Blanton, Michael, Strauss, Michael, Hoyle, Fiona, Schlegel, David, Scoccimarro, Roman, Vogeley, Michael, Weinberg, David, Zehavi, Idit, Berlind, Andreas, Budavari, Tamás, Connolly, Andrew, Eisenstein, Daniel James, Finkbeiner, Douglas, Frieman, Joshua, Gunn, James, Hamilton, Andrew, Hui, Lam, Jain, Bhuvnesh, Johnston, David, Kent, Stephen, Lin, Huan, Nakajima, Reiko, Nichol, Robert, Ostriker, Jeremiah, Pope, Adrian, Scranton, Ryan, Seljak, Uroš, Sheth, Ravi, Stebbins, Albert, Szalay, Alexander, Szapudi, István, Verde, Licia, Xu, Yongzhong, Annis, James, Bahcall, Neta, Brinkmann, J., Burles, Scott, Castander, Francisco, Csabai, Istvan, Loveday, Jon, Doi, Mamoru, Fukugita, Masataka, Gott, J., Hennessy, Greg, Hogg, David, Ivezić, Željko, Knapp, Gillian, Lamb, Don, Lee, Brian, Lupton, Robert, McKay, Timothy, Kunszt, Peter, Munn, Jeffrey, O'Connell, Liam, Peoples, John, Pier, Jeffrey, Richmond, Michael, Rockosi, Constance, Schneider, Donald, Stoughton, Christopher, Tucker, Douglas, Berk, Daniel, Yanny, Brian, and York, Donald

Subjects
galaxies: statistics, large-scale structure of universe, methods: data analysis
Abstract

We measure the large-scale real-space power spectrum P(k) by using a sample of 205,443 galaxies from the Sloan Digital Sky Survey, covering 2417 effective square degrees with mean redshift z ≈ 0.1. We employ a matrix-based method using pseudo-Karhunen-Loève eigenmodes, producing uncorrelated minimum-variance measurements in 22 k-bands of both the clustering power and its anisotropy due to redshift-space distortions, with narrow and well-behaved window functions in the range 0.02 h Mpc-1 < k < 0.3 h Mpc-1. We pay particular attention to modeling, quantifying, and correcting for potential systematic errors, nonlinear redshift distortions, and the artificial red-tilt caused by luminosity-dependent bias. Our results are robust to omitting angular and radial density fluctuations and are consistent between different parts of the sky. Our final result is a measurement of the real-space matter power spectrum P(k) up to an unknown overall multiplicative bias factor. Our calculations suggest that this bias factor is independent of scale to better than a few percent for k < 0.1 h Mpc-1, thereby making our results useful for precision measurements of cosmological parameters in conjunction with data from other experiments such as the Wilkinson Microwave Anisotropy Probe satellite. The power spectrum is not well-characterized by a single power law but unambiguously shows curvature. As a simple characterization of the data, our measurements are well fitted by a flat scale-invariant adiabatic cosmological model with h Ωm = 0.213 ± 0.023 and σ8 = 0.89 ± 0.02 for L* galaxies, when fixing the baryon fraction Ωb/Ωm = 0.17 and the Hubble parameter h = 0.72; cosmological interpretation is given in a companion paper., Astronomy

Published
2004
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18. Early-Type Galaxies in the Sloan Digital Sky Survey. IV. Colors and Chemical Evolution

Author

Bernardi, Mariangela, Sheth, Ravi K., Annis, James, Burles, Scott, Finkbeiner, Douglas, Lupton, Robert H., Schlegel, David J., SubbaRao, Mark, Bahcall, Neta A., Blakeslee, John P., Brinkmann, J., Castander, Francisco J., Connolly, Andrew J., Csabai, István, Doi, Mamoru, Fukugita, Masataka, Frieman, Joshua, Heckman, Timothy, Hennessy, Gregory S., Ivezic, Zeljko, Knapp, G. R., Lamb, Don Q., McKay, Timothy, Munn, Jeffrey A., Nichol, Robert, Okamura, Sadanori, Schneider, Donald P., Thakar, Aniruddha R., and York, Donald G.

Subjects
galaxies: elliptical and lenticular, cD, galaxies: evolution, galaxies: fundamental parameters, galaxies: photometry, galaxies: stellar content
Abstract

The colors and chemical abundances of early-type galaxies at redshifts z < 0.3 are studied using a sample of nearly 9000 galaxies, selected from the Sloan Digital Sky Survey using morphological and spectral criteria. In this sample, redder galaxies have larger velocity dispersions: g*-r* ∝ σ0.26±0.02. Color also correlates with magnitude, g* - r* ∝ (-0.025 ± 0.003)M, and size, but these correlations are entirely due to the L-σ and Ro-σ relations: the primary correlation is color-σ. The red light in early-type galaxies is, on average, slightly more centrally concentrated than the blue. Because of these color gradients, the strength of the color-magnitude relation depends on whether or not the colors are defined using a fixed metric aperture; the color-σ relation is less sensitive to this choice. Chemical evolution and star formation histories of early-type galaxies are investigated using co-added spectra of similar objects. The resulting library of co-added spectra contains spectra that represent a wide range of early-type galaxies. Chemical abundances correlate primarily with velocity dispersion: Hβ ∝ σ-0.24±0.03, Mg2 ∝ σ0.20±0.02, Mg b ∝ σ0.32±0.03, and langFerang ∝ σ0.11±0.03. At fixed σ, the population at z ~ 0.2 had weaker Mg2 and stronger Hβ absorption compared to the population at z ~ 0. It was also bluer. Comparison of these colors and line strengths and their evolution with single-burst stellar population models suggests a formation time of 9 Gyr ago, consistent with a fundamental plane analysis of this sample. Although the fundamental plane shows that galaxies in dense regions are slightly different from galaxies in less dense regions, the co-added spectra and color-magnitude relations show no statistically significant dependence on environment., Astronomy

Published
2003
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19. Early-Type Galaxies in the Sloan Digital Sky Survey. III. The Fundamental Plane

Author

Bernardi, Mariangela, Sheth, Ravi K., Annis, James, Burles, Scott, Eisenstein, Daniel James, Finkbeiner, Douglas, Hogg, David W., Lupton, Robert H., Schlegel, David J., SubbaRao, Mark, Bahcall, Neta A., Blakeslee, John P., Brinkmann, J., Castander, Francisco J., Connolly, Andrew J., Csabai, István, Doi, Mamoru, Fukugita, Masataka, Frieman, Joshua, Heckman, Timothy, Hennessy, Gregory S., Ivezic, Zeljko, Knapp, G. R., Lamb, Don Q., McKay, Timothy, Munn, Jeffrey A., Nichol, Robert, Okamura, Sadanori, Schneider, Donald P., Thakar, Aniruddha R., and York, Donald G.

Subjects
galaxies: elliptical and lenticular, cD, galaxies: evolution, galaxies: fundamental parameters, galaxies: photometry, galaxies: stellar content
Abstract

A magnitude-limited sample of nearly 9000 early-type galaxies in the redshift range 0.01 ≤ z ≤ 0.3 was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The fundamental plane relation in this sample is Ro ∝ σ1.49±0.05I in the r* band. It is approximately the same in the g*, i*, and z* bands. Relative to the population at the median redshift in the sample, galaxies at lower and higher redshifts have evolved only a little. If the fundamental plane is used to quantify this evolution, then the apparent magnitude limit can masquerade as evolution; once this selection effect has been accounted for, the evolution is consistent with that of a passively evolving population that formed the bulk of its stars about 9 Gyr ago. One of the principal advantages of the SDSS sample over previous samples is that the galaxies in it lie in environments ranging from isolation in the field to the dense cores of clusters. The fundamental plane shows that galaxies in dense regions are slightly different from galaxies in less dense regions., Astronomy

Published
2003
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20. Early-type Galaxies in the Sloan Digital Sky Survey. II. Correlations between Observables

Author

Bernardi, Mariangela, Sheth, Ravi K., Annis, James, Burles, Scott, Eisenstein, Daniel James, Finkbeiner, Douglas, Hogg, David W., Lupton, Robert H., Schlegel, David J., SubbaRao, Mark, Bahcall, Neta A., Blakeslee, John P., Brinkmann, J., Castander, Francisco J., Connolly, Andrew J., Csabai, István, Doi, Mamoru, Fukugita, Masataka, Frieman, Joshua, Heckman, Timothy, Hennessy, Gregory S., Ivezic, Zeljko, Knapp, G. R., Lamb, Don Q., McKay, Timothy, Munn, Jeffrey A., Nichol, Robert, Okamura, Sadanori, Schneider, Donald P., Thakar, Aniruddha R., and York, Donald G.

Subjects
galaxies: elliptical and lenticular, cD, galaxies: evolution, galaxies: fundamental parameters, galaxies: photometry, galaxies: stellar content
Abstract

A magnitude-limited sample of nearly 9000 early-type galaxies, in the redshift range 0.01 ≤ z ≤ 0.3, was selected from the Sloan Digital Sky Survey using morphological and spectral criteria. The sample was used to study how early-type galaxy observables, including luminosity L, effective radius Ro, surface brightness Io, color, and velocity dispersion σ, are correlated with one another. Measurement biases are understood with mock catalogs that reproduce all of the observed scaling relations and their dependences on fitting technique. At any given redshift, the intrinsic distribution of luminosities, sizes, and velocity dispersions in our sample are all approximately Gaussian. A maximum likelihood analysis shows that σ ∝ L0.25±0.012, Ro ∝ L0.63±0.025, and Ro ∝ I-0.75±0.02 in the r* band. In addition, the mass-to-light ratio within the effective radius scales as Mo/L ∝ L0.14±0.02 or Mo/L ∝ M, and galaxies with larger effective masses have smaller effective densities: Δo ∝ M. These relations are approximately the same in the g*, i*, and z* bands. Relative to the population at the median redshift in the sample, galaxies at lower and higher redshifts have evolved only little, with more evolution in the bluer bands. The luminosity function is consistent with weak passive luminosity evolution and a formation time of about 9 Gyr ago., Astronomy

Published
2003
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21. The First Data Release of the Sloan Digital Sky Survey

Author

Abazajian, Kevork, Adelman-McCarthy, Jennifer K., Ageros, Marcel A., Allam, Sahar S., Anderson, Scott F., Annis, James, Bahcall, Neta A., Baldry, Ivan K., Bastian, Steven, Berlind, Andreas, Bernardi, Mariangela, Blanton, Michael R., Blythe, Norman, Bochanski, John J. Jr., Boroski, William N., Brewington, Howard, Briggs, John W., Brinkmann, J., Brunner, Robert J., Budavri, Tams, Carey, Larry N., Carr, Michael A., Castander, Francisco J., Chiu, Kuenley, Collinge, Matthew J., Connolly, A. J., Covey, Kevin R., Csabai, Istvn, Dalcanton, Julianne J., Dodelson, Scott, Doi, Mamoru, Dong, Feng, Eisenstein, Daniel James, Evans, Michael L., Fan, Xiaohui, Feldman, Paul D., Finkbeiner, Douglas, Friedman, Scott D., Frieman, Joshua A., Fukugita, Masataka, Gal, Roy R., Gillespie, Bruce, Glazebrook, Karl, Gonzalez, Carlos F., Gray, Jim, Grebel, Eva K., Grodnicki, Lauren, Gunn, James E., Gurbani, Vijay K., Hall, Patrick B., Hao, Lei, Harbeck, Daniel, Harris, Frederick H., Harris, Hugh C., Harvanek, Michael, Hawley, Suzanne L., Heckman, Timothy M., Helmboldt, J. F., Hendry, John S., Hennessy, Gregory S., Hindsley, Robert B., Hogg, David W., Holmgren, Donald J., Holtzman, Jon A., Homer, Lee, Hui, Lam, Ichikawa, Shin-ichi, Ichikawa, Takashi, Inkmann, John P., Ivezic, Zeljko, Jester, Sebastian, Johnston, David E., Jordan, Beatrice, Jordan, Wendell P., Jorgensen, Anders M., Juri, Mario, Kauffmann, Guinevere, Kent, Stephen M., Kleinman, S. J., Knapp, G. R., Kniazev, Alexei Y., Kron, Richard G., Krzesiski, Jurek, Kunszt, Peter Z., Kuropatkin, Nickolai, Lamb, Donald Q., Lampeitl, Hubert, Laubscher, Bryan E., Lee, Brian C., Leger, R. French, Li, Nolan, Lidz, Adam, Lin, Huan, Loh, Yeong-Shang, Long, Daniel C., Loveday, Jon, Lupton, Robert H., Malik, Tanu, Margon, Bruce, McGehee, Peregrine M., McKay, Timothy A., Meiksin, Avery, Miknaitis, Gajus A., Moorthy, Bhasker K., Munn, Jeffrey A., Murphy, Tara, Nakajima, Reiko, Narayanan, Vijay K., Nash, Thomas, Neilsen, Eric H. Jr., Newberg, Heidi Jo, Newman, Peter R., Nichol, Robert C., Nicinski, Tom, Nieto-Santisteban, Maria, Nitta, Atsuko, Odenkirchen, Michael, Okamura, Sadanori, Ostriker, Jeremiah P., Owen, Russell, Padmanabhan, Nikhil, Peoples, John, Pier, Jeffrey R., Pindor, Bartosz, Pope, Adrian C., Quinn, Thomas R., Rafikov, R. R., Raymond, Sean N., Richards, Gordon T., Richmond, Michael W., Rix, Hans-Walter, Rockosi, Constance M., Schaye, Joop, Schlegel, David J., Schneider, Donald P., Schroeder, Joshua, Scranton, Ryan, Sekiguchi, Maki, Seljak, Uro, Sergey, Gary, Sesar, Branimir, Sheldon, Erin, Shimasaku, Kazu, Siegmund, Walter A., Silvestri, Nicole M., Sinisgalli, Allan J., Sirko, Edwin, Smith, J. Allyn, Smoli, Vernesa, Snedden, Stephanie A., Stebbins, Albert, Steinhardt, Charles, Stinson, Gregory, Stoughton, Chris, Strateva, Iskra V., Strauss, Michael A., SubbaRao, Mark, Szalay, Alexander S., Szapudi, Istvn, Szkody, Paula, Tasca, Lidia, Tegmark, Max, Thakar, Aniruddha R., Tremonti, Christy, Tucker, Douglas L., Uomoto, Alan, Vanden Berk, Daniel E., Vandenberg, Jan, Vogeley, Michael S., Voges, Wolfgang, Vogt, Nicole P., Walkowicz, Lucianne M., Weinberg, David H., West, Andrew A., White, Simon D. M., Wilhite, Brian C., Willman, Beth, Xu, Yongzhong, Yanny, Brian, Yarger, Jean, Yasuda, Naoki, Yip, Ching-Wa, Yocum, D. R., York, Donald G., Zakamska, Nadia L., Zehavi, Idit, Zheng, Wei, Zibetti, Stefano, and Zucker, Daniel B.

Subjects
atlases, catalogs, surveys
Abstract

The Sloan Digital Sky Survey (SDSS) has validated and made publicly available its First Data Release. This consists of 2099 deg2 of five-band (u, g, r, i, z) imaging data, 186,240 spectra of galaxies, quasars, stars and calibrating blank sky patches selected over 1360 deg2 of this area, and tables of measured parameters from these data. The imaging data go to a depth of r ≈ 22.6 and are photometrically and astrometrically calibrated to 2% rms and 100 mas rms per coordinate, respectively. The spectra cover the range 3800–9200 Å, with a resolution of 1800–2100. This paper describes the characteristics of the data with emphasis on improvements since the release of commissioning data (the SDSS Early Data Release) and serves as a pointer to extensive published and on-line documentation of the survey., Astronomy

Published
2003
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22. The Luminosity Function of Galaxies in SDSS Commissioning Data

Author

Blanton, Michael R., Dalcanton, Julianne, Eisenstein, Daniel James, Loveday, Jon, Strauss, Michael A., SubbaRao, Mark, Weinberg, David H., Anderson, Jr., John E., Annis, James, Bahcall, Neta A., Bernardi, Mariangela, Brinkmann, J., Brunner, Robert J., Burles, Scott, Carey, Larry, Castander, Francisco J., Connolly, Andrew J., Csabai, István, Doi, Mamoru, Finkbeiner, Douglas, Friedman, Scott, Frieman, Joshua A., Fukugita, Masataka, Gunn, James E., Hennessy, G. S., Hindsley, Robert B., Hogg, David W., Ichikawa, Takashi, Ivezic, Zeljko, Kent, Stephen, Knapp, G. R., Lamb, D. Q., Leger, R. French, Long, Daniel C., Lupton, Robert H., McKay, Timothy A., Meiksin, Avery, Merelli, Aronne, Munn, Jeffrey A., Narayanan, Vijay, Newcomb, Matt, Nichol, R. C., Okamura, Sadanori, Owen, Russell, Pier, Jeffrey R., Pope, Adrian, Postman, Marc, Quinn, Thomas, Rockosi, Constance M., Schlegel, David J., Schneider, Donald P., Shimasaku, Kazuhiro, Siegmund, Walter A., Smee, Stephen, Snir, Yehuda, Stoughton, Chris, Stubbs, Christopher, Szalay, Alexander S., Szokoly, Gyula P., Thakar, Aniruddha R., Tremonti, Christy, Tucker, Douglas L., Uomoto, Alan, Vanden Berk, Dan, Vogeley, Michael S., Waddell, Patrick, Yanny, Brian, Yasuda, Naoki, and York, Donald G.

Subjects
galaxies : fundamental parameters, galaxies : photometry, galaxies : statistics
Abstract

In the course of its commissioning observations, the Sloan Digital Sky Survey (SDSS) has produced one of the largest redshift samples of galaxies selected from CCD images. Using 11,275 galaxies complete to r* = 17.6 over 140 deg2, we compute the luminosity function of galaxies in the r* band over a range -23 < M < -16 (for h = 1). The result is well-described by a Schechter function with parameters phgr* = (1.46 ± 0.12) × 10-2 h3 Mpc-3, M* = -20.83 ± 0.03, and α = -1.20 ± 0.03. The implied luminosity density in r* is j ≈ (2.6 ± 0.3) × 108h L⊙ Mpc-3. We find that the surface brightness selection threshold has a negligible impact for M < -18. Using subsets of the data, we measure the luminosity function in the u*, g*, i*, and z* bands as well; the slope at low luminosities ranges from α = -1.35 to α = -1.2. We measure the bivariate distribution of r* luminosity with half-light surface brightness, intrinsic g*-r* color, and morphology. In agreement with previous studies, we find that high surface brightness, red, highly concentrated galaxies are on average more luminous than low surface brightness, blue, less concentrated galaxies. An important feature of the SDSS luminosity function is the use of Petrosian magnitudes, which measure a constant fraction of a galaxy's total light regardless of the amplitude of its surface brightness profile. If we synthesize results for RGKC band or bj band using these Petrosian magnitudes, we obtain luminosity densities 2 times that found by the Las Campanas Redshift Survey in RGKC and 1.4 times that found by the Two Degree Field Galaxy Redshift Survey in bj. However, we are able to reproduce the luminosity functions obtained by these surveys if we also mimic their isophotal limits for defining galaxy magnitudes, which are shallower and more redshift dependent than the Petrosian magnitudes used by the SDSS., Astronomy

Published
2001
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23. Composite Quasar Spectra from the Sloan Digital Sky Survey

Author

Vanden Berk, Daniel E., Richards, Gordon T., Bauer, Amanda, Strauss, Michael A., Schneider, Donald P., Heckman, Timothy M., York, Donald G., Hall, Patrick B., Fan, Xiaohui, Knapp, G. R., Anderson, Scott F., Annis, James, Bahcall, Neta A., Bernardi, Mariangela, Briggs, John W., Brinkmann, J., Brunner, Robert, Burles, Scott, Carey, Larry, Castander, Francisco J., Connolly, A. J., Crocker, J. H., Csabai, István, Doi, Mamoru, Finkbeiner, Douglas, Friedman, Scott, Frieman, Joshua A., Fukugita, Masataka, Gunn, James E., Hennessy, G. S., Ivezic, Zeljko, Kent, Stephen, Kunszt, Peter Z., Lamb, D. Q., Leger, R. French, Long, Daniel C., Loveday, Jon, Lupton, Robert H., Meiksin, Avery, Merelli, Aronne, Munn, Jeffrey A., Newberg, Heidi Jo, Newcomb, Matt, Nichol, R. C., Owen, Russell, Pier, Jeffrey R., Pope, Adrian, Rockosi, Constance M., Schlegel, David J., Siegmund, Walter A., Smee, Stephen, Snir, Yehuda, Stoughton, Chris, Stubbs, Christopher William, SubbaRao, Mark, Szalay, Alexander S., Szokoly, Gyula P., Tremonti, Christy, Uomoto, Alan, Waddell, Patrick, Yanny, Brian, and Zheng, Wei

Subjects
quasars : emission lines, quasars : general
Abstract

We have created a variety of composite quasar spectra using a homogeneous data set of over 2200 spectra from the Sloan Digital Sky Survey (SDSS). The quasar sample spans a redshift range of 0.044 ≤ z ≤ 4.789 and an absolute r' magnitude range of -18.0 to -26.5. The input spectra cover an observed wavelength range of 3800–9200 Å at a resolution of 1800. The median composite covers a rest-wavelength range from 800 to 8555 Å and reaches a peak signal-to-noise ratio of over 300 per 1 Å resolution element in the rest frame. We have identified over 80 emission-line features in the spectrum. Emission-line shifts relative to nominal laboratory wavelengths are seen for many of the ionic species. Peak shifts of the broad permitted and semiforbidden lines are strongly correlated with ionization energy, as previously suggested, but we find that the narrow forbidden lines are also shifted by amounts that are strongly correlated with ionization energy. The magnitude of the forbidden line shifts is lesssim100 km s-1, compared with shifts of up to 550 km s-1 for some of the permitted and semiforbidden lines. At wavelengths longer than the Lyα emission, the continuum of the geometric mean composite is well fitted by two power laws, with a break at ≈5000 Å. The frequency power-law index, αν, is -0.44 from ≈1300 to 5000 Å and -2.45 redward of ≈5000 Å. The abrupt change in slope can be accounted for partly by host-galaxy contamination at low redshift. Stellar absorption lines, including higher order Balmer lines, seen in the composites suggest that young or intermediate-age stars make a significant contribution to the light of the host galaxies. Most of the spectrum is populated by blended emission lines, especially in the range 1500–3500 Å, which can make the estimation of quasar continua highly uncertain unless large ranges in wavelength are observed. An electronic table of the median quasar template is available., Astronomy

Published
2001
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24. Colors of 2625 Quasars at 0 < z < 5 Measured in the Sloan Digital Sky Survey Photometric System

Author

Richards, Gordon T., Fan, Xiaohui, Schneider, Donald P., Vanden Berk, Daniel E., Strauss, Michael A., York, Donald G., Anderson, Jr., John E., Anderson, Scott F., Annis, James, Bahcall, Neta A., Bernardi, Mariangela, Briggs, John W., Brinkmann, J., Brunner, Robert, Burles, Scott, Carey, Larry, Castander, Francisco J., Connolly, A. J., Crocker, J. H., Csabai, István, Doi, Mamoru, Finkbeiner, Douglas, Friedman, Scott D., Frieman, Joshua A., Fukugita, Masataka, Gunn, James E., Hindsley, Robert B., Ivezic, Zeljko, Kent, Stephen, Knapp, G. R., Lamb, D. Q., Leger, R. French, Long, Daniel C., Loveday, Jon, Lupton, Robert H., McKay, Timothy A., Meiksin, Avery, Merrelli, Aronne, Munn, Jeffrey A., Newberg, Heidi Jo, Newcomb, Matt, Nichol, R. C., Owen, Russell, Pier, Jeffrey R., Pope, Adrian, Richmond, Michael W., Rockosi, Constance M., Schlegel, David J., Siegmund, Walter A., Smee, Stephen, Snir, Yehuda, Stoughton, Chris, Stubbs, Christopher William, SubbaRao, Mark, Szalay, Alexander S., Szokoly, Gyula P., Tremonti, Christy, Uomoto, Alan, Waddell, Patrick, Yanny, Brian, and Zheng, Wei

Subjects
catalogs, quasars: general, surveys
Abstract

We present an empirical investigation of the colors of quasars in the Sloan Digital Sky Survey (SDSS) photometric system. The sample studied includes 2625 quasars with SDSS photometry: 1759 quasars found during SDSS spectroscopic commissioning and SDSS follow-up observations on other telescopes, 50 matches to FIRST quasars, 573 matches to quasars from the NASA Extragalactic Database, and 243 quasars from two or more of these sources. The quasars are distributed in a 2fdg5 wide stripe centered on the celestial equator covering ~529 deg2. Positions (accurate to 0farcs2) and SDSS magnitudes are given for the 898 quasars known prior to SDSS spectroscopic commissioning. New SDSS quasars, which range in brightness from i* = 15.39 to the photometric magnitude limit of the survey, represent an increase of over 200% in the number of known quasars in this area of the sky. The ensemble average of the observed colors of quasars in the SDSS passbands are well represented by a power-law continuum with αν = -0.5 (fν ∝ να) and are close to those predicted by previous simulations. However, the contributions of the "small blue (or λ3000) bump" and other strong emission lines have a significant effect upon the colors. The color-redshift relation exhibits considerable structure, which may be of use in determining photometric redshifts for quasars from their colors alone. The range of colors at a given redshift can generally be accounted for by a range in the optical spectral index with a distribution αν = -0.5 ± 0.65 (95% confidence), but there is a red tail in the distribution. This tail may be a sign of internal reddening, especially since fainter objects at a given redshift tend to exhibit redder colors than the average. Finally, we show that there is a continuum of properties between quasars and Seyfert galaxies, and we test the validity of the traditional dividing line (MB = -23) between the two classes of active galactic nuclei., Astronomy

Published
2001
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25. THE SLOAN DIGITAL SKY SURVEY COADD: 275 deg2 OF DEEP SLOAN DIGITAL SKY SURVEY IMAGING ON STRIPE 82.

Author

Annis, James, Soares-Santos, Marcelle, Strauss, Michael A., Becker, Andrew C., Dodelson, Scott, Fan, Xiaohui, Gunn, James E., Hao, Jiangang, Ivezić, Željko, Jester, Sebastian, Jiang, Linhua, Johnston, David E., Kubo, Jeffrey M., Lampeitl, Hubert, Lin, Huan, Lupton, Robert H., Miknaitis, Gajus, Seo, Hee-Jong, Simet, Melanie, and Yanny, Brian

Subjects
*GALAXY spectra, *CLASSIFICATION of stars, *REDSHIFT, *STAR colors, *ASTRONOMICAL photometry
Abstract

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. [ABSTRACT FROM AUTHOR]

Published
2014
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27. THE SDSS CO-ADD: COSMIC SHEAR MEASUREMENT.

Author

Lin, Huan, Dodelson, Scott, Seo, Hee-Jong, Soares-Santos, Marcelle, Annis, James, Hao, Jiangang, Johnston, David, Kubo, Jeffrey M., Reis, Ribamar R. R., and Simet, Melanie

Subjects
MICROWAVE reflectometry, ASTRONOMICAL photometry, GALACTIC redshift, POWER spectra
Abstract

Stripe 82 in the Sloan Digital Sky Survey was observed multiple times, allowing deeper images to be constructed by co-adding the data. Here, we analyze the ellipticities of background galaxies in this 275 deg2 region, searching for evidence of distortions due to cosmic shear. We do so using measurements of both the shear-shear correlation function and power spectrum, with the latter determined using both “quadratic” and “pseudo” estimation techniques. We show how we verified these methods using mock catalogs. We also describe our methods for modeling and correcting for the effects of the point-spread function (PSF) in our shape measurements, and we also describe our prescription for estimating photometric redshifts (photo-z's) for our galaxy sample. In particular, we assess the impact of potential systematic effects due to the PSF and to photo-z's, and show that these are under control in our analysis. We find consistent correlation function and power spectrum results, where the E-mode cosmic shear signal is detected in both real and Fourier space with >5σ significance on degree scales, while the B-mode is consistent with zero as expected. The amplitude of the signal constrains the combination of the matter density Ωm and fluctuation amplitude σ8 to be Ω0.7mσ8 = 0.252+0.032– 0.052. [ABSTRACT FROM AUTHOR]

Published
2012
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28. THE SLOAN BRIGHT ARCS SURVEY: TEN STRONG GRAVITATIONAL LENSING CLUSTERS AND EVIDENCE OF OVERCONCENTRATION.

Author

Wiesner, Matthew P., Lin, Huan, Allam, Sahar S., Annis, James, Buckley-Geer, Elizabeth J., Diehl, H. Thomas, Kubik, Donna, Kubo, Jeffrey M., and Tucker, Douglas

Subjects
OPEN clusters of stars, GALACTIC redshift, STAR clusters, GRAVITATIONAL lenses
Abstract

We describe 10 strong lensing galaxy clusters of redshift 0.26 ⩽ z ⩽ 0.56 that were found in the Sloan Digital Sky Survey. We present measurements of richness (N200), mass (M200), and velocity dispersion for the clusters. We find that in order to use the mass-richness relation from Johnston et al., which was established at mean redshift of 0.25, it is necessary to scale measured richness values up by 1.47. Using this scaling, we find richness values for these clusters to be in the range of 22 ⩽ N200 ⩽ 317 and mass values to be in the range of 1 × 1014h–1M☼ ⩽ M200 ⩽ 30 × 1014h–1M☼. We also present measurements of Einstein radius, mass, and velocity dispersion for the lensing systems. The Einstein radii (θE) are all relatively small, with 5.″4 ⩽ θE ⩽ 13″. Finally, we consider if there is evidence that our clusters are more concentrated than ΛCDM would predict. We find that six of our clusters do not show evidence of overconcentration, while four of our clusters do. We note a correlation between overconcentration and mass, as the four clusters showing evidence of overconcentration are all lower-mass clusters. For the four lowest mass clusters the average value of the concentration parameter c200 is 11.6, while for the six higher-mass clusters the average value of c200 is 4.4. ΛCDM would place c200 between 3.4 and 5.7. [ABSTRACT FROM AUTHOR]

Published
2012
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34. THE SLOAN NEARBY CLUSTER WEAK LENSING SURVEY.

Author

Kubo, Jeffrey M., Annis, James, Hardin, Frances M., Kubik, Donna, Lawhorn, Kelsey, Lin, Huan, Nicklaus, Liana, Nelson, Dylan, Reis, Ribamar R. R., Seo, Hee-Jong, Soares-Santos, Marcelle, Stebbins, Albert, and Yunker, Tony

Published
2009
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39. THE SEVENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY.

Author

Abazajian, Kevork N., Adelman-McCarthy, Jennifer K., Agüeros, Marcel A., Allam, Sahar S., Allende Prieto, Carlos, An, Deokkeun, Anderson, Kurt S. J., Anderson, Scott F., Annis, James, Bahcall, Neta A., Bailer-Jones, C. A. L., Barentine, J. C., Bassett, Bruce A., Becker, Andrew C., Beers, Timothy C., Bell, Eric F., Belokurov, Vasily, Berlind, Andreas A., Berman, Eileen F., and Bernardi, Mariangela

Published
2009
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42. A NEW SURVEY FOR GIANT ARCS.

Author

Hennawi, Joseph F., Gladders, Michael D., Oguri, Masamune, Dalal, Neal, Koester, Benjamin, Natarajan, Priyamvada, Strauss, Michael A., Inada, Naohisa, Kayo, Issha, Lin, Huan, Lampeitl, Hubert, Annis, James, Bahcall, Neta A., and Schneider, Donald P.

Published
2008
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43. The Fifth Data Release of the Sloan Digital Sky Survey.

Author

Adelman-McCarthy, Jennifer K., Agüeros, Marcel A., Allam, Sahar S., Anderson, Kurt S. J., Anderson, Scott F., Annis, James, Bahcall, Neta A., Bailer-Jones, Coryn A. L., Baldry, Ivan K., Barentine, J. C., Beers, Timothy C., Belokurov, V., Berlind, Andreas, Bernardi, Mariangela, Blanton, Michael R., Bochanski, John J., Boroski, William N., Bramich, D. M., Brewington, Howard J., and Brinchmann, Jarle

Published
2007
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44. The 2.5 m Telescope of the Sloan Digital Sky Survey.

Author

Gunn, James E., Siegmund, Walter A., Mannery, Edward J., Owen, Russell E., Hull, Charles L., Leger, R. French, Carey, Larry N., Knapp, Gillian R., York, Donald G., Boroski, William N., Kent, Stephen M., Lupton, Robert H., Rockosi, Constance M., Evans, Michael L., Waddell, Patrick, Anderson, John E., Annis, James, Barentine, John C., Bartoszek, Larry M., and Bastian, Steven

Published
2006
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46. The Fourth Data Release of the Sloan Digital Sky Survey.

Author

Adelman-McCarthy, Jennifer K., Agüeros, Marcel A., Allam, Sahar S., Anderson, Kurt S. J., Anderson, Scott F., Annis, James, Bahcall, Neta A., Baldry, Ivan K., Barentine, J. C., Berlind, Andreas, Bernardi, Mariangela, Blanton, Michael R., Boroski, William N., Brewington, Howard J., Brinchmann, Jarle, Brinkmann, J., Brunner, Robert J., Budavári, Tamás, Carey, Larry N., and Carr, Michael A.

Published
2006
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49. Andromeda IX: A New Dwarf Spheroidal Satellite of M31.

Author

Zucker, Daniel B., Kniazev, Alexei Y., Bell, Eric F., Martínez-Delgado, David, Grebel, Eva K., Rix, Hans-Walter, Rockosi, Constance M., Holtzman, Jon A., Walterbos, Rene A. M., Annis, James, York, Donald G., Ivezić, Željko, Brinkmann, J., Brewington, Howard, Harvanek, Michael, Hennessy, Greg, Kleinman, S. J., Krzesinski, Jurek, Long, Dan, and Newman, Peter R.

Published
2004
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50. A Survey of z > 5.7 Quasars in the Sloan Digital Sky Survey. III. Discovery of Five Additional Quasars.

Author

Fan, Xiaohui, Hennawi, Joseph F., Richards, Gordon T., Strauss, Michael A., Schneider, Donald P., Donley, Jennifer L., Young, Jason E., Annis, James, Lin, Huan, Lampeitl, Hubert, Lupton, Robert H., Gunn, James E., Knapp, Gillan R., Brandt, W. N., Anderson, Scott, Bahcall, Neta A., Brinkmann, Jon, Brunner, Robert J., Fukugita, Masataka, and Szalay, Alexander S.

Published
2004
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