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88 results on '"Doi, Mamoru"'

1. MUSSES2020J: The Earliest Discovery of a Fast Blue Ultraluminous Transient at Redshift 1.063

Author

World Premier International Research Center (Japan), Japan Society for the Promotion of Science, European Commission, Jiang, Ji An [0000-0002-9092-0593], Maeda, Keiichi [0000-0003-2611-7269], Tominaga, Nozomu [0000-0001-8537-3153], Ivezić, Zelijko [0000-0001-5250-2633], Yoachim, Peter [0000-0003-2874-6464], Uno, Kohki [0000-0002-6765-8988], Moriya, Takashi J. [0000-0003-1169-1954], Kumar, Brajesh [0000-0001-7225-2475], Pan, Yen Chen [0000-0001-8415-6720], Tanaka, Masayuki [0000-0002-5011-5178], Nomoto, Ken'Ichi [0000-0001-8253-6850], Jha, Saurabh W. [0000-0001-9553-0685], Ruiz-Lapuente, Pilar [0000-0001-8738-6011], Jones, David [0000-0001-9046-4420], Shigeyama, Toshikazu [0000-0003-3947-5946], Suzuki, Nao [0000-0002-4060-5931], Kokubo, Mitsuru [0000-0001-7266-930X], Furusawa, Hisanori [0000-0001-6402-1415], Miyazaki, Satoshi [0000-0002-6174-8165], Connolly, Andrew J. [0000-0002-1962-904X], Sahu, D. K. [0000-0001-5576-8189], Anupama, G. C. [0000-0003-3533-7183], Jiang, Ji An, Yasuda, Naoki, Maeda, Keiichi, Tominaga, Nozomu, Doi, Mamoru, Ivezić, Zelijko, Yoachim, Peter, Uno, Kohki, Moriya, Takashi J., Kumar, Brajesh, Pan, Yen Chen, Tanaka, Masayuki, Tanaka, Masaomi, Nomoto, Ken'Ichi, Jha, Saurabh W., Ruiz-Lapuente, Pilar, Jones, David, Shigeyama, Toshikazu, Suzuki, Nao, Kokubo, Mitsuru, Furusawa, Hisanori, Miyazaki, Satoshi, Connolly, Andrew J., Sahu, D. K., Anupama, G. C., World Premier International Research Center (Japan), Japan Society for the Promotion of Science, European Commission, Jiang, Ji An [0000-0002-9092-0593], Maeda, Keiichi [0000-0003-2611-7269], Tominaga, Nozomu [0000-0001-8537-3153], Ivezić, Zelijko [0000-0001-5250-2633], Yoachim, Peter [0000-0003-2874-6464], Uno, Kohki [0000-0002-6765-8988], Moriya, Takashi J. [0000-0003-1169-1954], Kumar, Brajesh [0000-0001-7225-2475], Pan, Yen Chen [0000-0001-8415-6720], Tanaka, Masayuki [0000-0002-5011-5178], Nomoto, Ken'Ichi [0000-0001-8253-6850], Jha, Saurabh W. [0000-0001-9553-0685], Ruiz-Lapuente, Pilar [0000-0001-8738-6011], Jones, David [0000-0001-9046-4420], Shigeyama, Toshikazu [0000-0003-3947-5946], Suzuki, Nao [0000-0002-4060-5931], Kokubo, Mitsuru [0000-0001-7266-930X], Furusawa, Hisanori [0000-0001-6402-1415], Miyazaki, Satoshi [0000-0002-6174-8165], Connolly, Andrew J. [0000-0002-1962-904X], Sahu, D. K. [0000-0001-5576-8189], Anupama, G. C. [0000-0003-3533-7183], Jiang, Ji An, Yasuda, Naoki, Maeda, Keiichi, Tominaga, Nozomu, Doi, Mamoru, Ivezić, Zelijko, Yoachim, Peter, Uno, Kohki, Moriya, Takashi J., Kumar, Brajesh, Pan, Yen Chen, Tanaka, Masayuki, Tanaka, Masaomi, Nomoto, Ken'Ichi, Jha, Saurabh W., Ruiz-Lapuente, Pilar, Jones, David, Shigeyama, Toshikazu, Suzuki, Nao, Kokubo, Mitsuru, Furusawa, Hisanori, Miyazaki, Satoshi, Connolly, Andrew J., Sahu, D. K., and Anupama, G. C.

Abstract

In this Letter, we report the discovery of an ultraluminous fast-evolving transient in rest-frame UV wavelengths, MUSSES2020J, soon after its occurrence by using the Hyper Suprime-Cam (HSC) mounted on the 8.2 m Subaru telescope. The rise time of about 5 days with an extremely high UV peak luminosity shares similarities to a handful of fast blue optical transients whose peak luminosities are comparable with the most luminous supernovae while their timescales are significantly shorter (hereafter "fast blue ultraluminous transient,"FBUT). In addition, MUSSES2020J is located near the center of a normal low-mass galaxy at a redshift of 1.063, suggesting a possible connection between the energy source of MUSSES2020J and the central part of the host galaxy. Possible physical mechanisms powering this extreme transient such as a wind-driven tidal disruption event and an interaction between supernova and circumstellar material are qualitatively discussed based on the first multiband early-phase light curve of FBUTs, although whether the scenarios can quantitatively explain the early photometric behavior of MUSSES2020J requires systematical theoretical investigations. Thanks to the ultrahigh luminosity in UV and blue optical wavelengths of these extreme transients, a promising number of FBUTs from the local to the high-z universe can be discovered through deep wide-field optical surveys in the near future.

Published
2022

3. A Very Metal-poor RR Lyrae Star with a Disk Orbit Found in the Solar Neighborhood.

Author

Matsunaga, Noriyuki, Itane, Akinori, Hattori, Kohei, Crestani, Juliana, Braga, Vittorio, Bono, Giuseppe, Taniguchi, Daisuke, Baba, Junichi, Maehara, Hiroyuki, Ukita, Nobuharu, Sakamoto, Tsuyoshi, Kobayashi, Naoto, Aoki, Tsutomu, Soyano, Takao, Tarusawa, Ken’ichi, Sarugaku, Yuki, Mito, Hiroyuki, Sako, Shigeyuki, Doi, Mamoru, and Nakada, Yoshikazu

Subjects
RR Lyrae stars, EARLY stars, STELLAR populations, OPTICAL spectroscopy, STAR formation, STELLAR orbits
Abstract

Metal-deficient stars are important tracers for understanding the early formation of the Galaxy. Recent large-scale surveys with both photometric and spectroscopic data have reported an increasing number of metal-deficient stars whose kinematic features are consistent with those of the disk stellar populations. We report the discovery of an RR Lyrae variable (hereafter RRL) that is located within the thick disk and has an orbit consistent with the thick-disk kinematics. Our target RRL (HD 331986) is located at around 1 kpc from the Sun and, with V ≃ 11.3, is among the ∼130 brightest RRLs known so far. However, this object has scarcely been studied because it is in the midplane of the Galaxy, at a Galactic latitude around â€"1°. Its near-infrared spectrum (0.91â€"1.32 ÎĽ m) shows no absorption line except hydrogen lines of the Paschen series, suggesting [Fe/H] ≲ â€"2.5. It is the most metal-deficient RRL, at least among RRLs whose orbits are consistent with the disk kinematics, although we cannot determine to which of the disk and the halo it belongs. This unique RRL would provide us with essential clues for studying the early formation of stars in the inner Galaxy with further investigations, including high-resolution optical spectroscopy. [ABSTRACT FROM AUTHOR]

Published
2022
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4. The Data Release of the Sloan Digital Sky Survey-II Supernova Survey

Author

Sako, Masao, primary, Bassett, Bruce, additional, Becker, Andrew C., additional, Brown, Peter J., additional, Campbell, Heather, additional, Wolf, Rachel, additional, Cinabro, David, additional, D’Andrea, Chris B., additional, Dawson, Kyle S., additional, DeJongh, Fritz, additional, Depoy, Darren L., additional, Dilday, Ben, additional, Doi, Mamoru, additional, Filippenko, Alexei V., additional, Fischer, John A., additional, Foley, Ryan J., additional, Frieman, Joshua A., additional, Galbany, Lluis, additional, Garnavich, Peter M., additional, Goobar, Ariel, additional, Gupta, Ravi R., additional, Hill, Gary J., additional, Hayden, Brian T., additional, Hlozek, Renée, additional, Holtzman, Jon A., additional, Hopp, Ulrich, additional, Jha, Saurabh W., additional, Kessler, Richard, additional, Kollatschny, Wolfram, additional, Leloudas, Giorgos, additional, Marriner, John, additional, Marshall, Jennifer L., additional, Miquel, Ramon, additional, Morokuma, Tomoki, additional, Mosher, Jennifer, additional, Nichol, Robert C., additional, Nordin, Jakob, additional, Olmstead, Matthew D., additional, Östman, Linda, additional, Prieto, Jose L., additional, Richmond, Michael, additional, Romani, Roger W., additional, Sollerman, Jesper, additional, Stritzinger, Max, additional, Schneider, Donald P., additional, Smith, Mathew, additional, Wheeler, J. Craig, additional, Yasuda, Naoki, additional, and Zheng, Chen, additional

Published
2018
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5. STATISTICAL PROPERTIES OF MULTI-EPOCH SPECTRAL VARIABILITY OF SDSS STRIPE 82 QUASARS.

Author

Kokubo, Mitsuru, Morokuma, Tomoki, Minezaki, Takeo, Doi, Mamoru, Kawaguchi, Toshihiro, Sameshima, Hiroaki, and Koshida, Shintaro

Subjects
ACCRETION (Astrophysics), ACCRETION disks, ACTIVE galaxies, GALACTIC nuclei, QUASARS
Abstract

We investigate the UV-optical (longward of Lyα 1216 Å) spectral variability of nearly 9000 quasars (0 < z < 4) using multi-epoch photometric data within the SDSS Stripe 82 region. The regression slope in the flux-flux space of a quasar light curve directly measures the color of the flux difference spectrum, then the spectral shape of the flux difference spectra can be derived by taking a careful look at the redshift dependence of the regression slopes. First, we confirm that the observed quasar spectrum becomes bluer when the quasar becomes brighter. We infer the spectral index of the composite difference spectrum as (in the form of ), which is significantly bluer than that of the composite spectrum . We also show that the continuum variability cannot be explained by accretion disk models with varying mass accretion rates. Second, we examine the effects of broad emission line variability on the color-redshift space. The variability of the “Small Blue Bump” is extensively discussed. We show that the low-ionization lines of Mg II and Fe II are less variable compared to Balmer emission lines and high-ionization lines, and the Balmer continuum is the dominant variable source around ∼3000 Å. These results are compared with previous studies, and the physical mechanisms of the variability of the continuum and emission lines are discussed. [ABSTRACT FROM AUTHOR]

Published
2014
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7. The Subaru/XMM-Newton Deep Survey (SXDS). II. Optical Imaging and Photometric CatalogsBased on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.

Author

Furusawa, Hisanori, Kosugi, George, Akiyama, Masayuki, Takata, Tadafumi, Sekiguchi, Kazuhiro, Tanaka, Ichi, Iwata, Ikuru, Kajisawa, Masaru, Yasuda, Naoki, Doi, Mamoru, Ouchi, Masami, Simpson, Chris, Shimasaku, Kazuhiro, Yamada, Toru, Furusawa, Junko, Morokuma, Tomoki, Ishida, Catherine M., Aoki, Kentaro, Fuse, Tetsuharu, and Imanishi, Masatoshi

Published
2008
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8. Sloan Digital Sky Survey Standard Star Catalog for Stripe 82: The Dawn of Industrial 1% Optical Photometry.

Author

Ivezić, Željko, Smith, J. Allyn, Miknaitis, Gajus, Lin, Huan, Tucker, Douglas, Lupton, Robert H., Gunn, James E., Knapp, Gillian R., Strauss, Michael A., Sesar, Branimir, Doi, Mamoru, Tanaka, Masayuki, Fukugita, Masataka, Holtzman, Jon, Kent, Steve, Yanny, Brian, Schlegel, David, Finkbeiner, Douglas, Padmanabhan, Nikhil, and Rockosi, Constance M.

Published
2007
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9. Wide-Field Survey around Local Group Dwarf Spheroidal Galaxy Leo II: Spatial Distribution of Stellar ContentBased on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.

Author

Komiyama, Yutaka, Doi, Mamoru, Furusawa, Hisanori, Hamabe, Masaru, Imi, Katsumi, Kimura, Masahiko, Miyazaki, Satoshi, Nakata, Fumiaki, Okada, Norio, Okamura, Sadanori, Ouchi, Masami, Sekiguchi, Maki, Shimasaku, Kazuhiro, Yagi, Masafumi, and Yasuda, Naoki

Published
2007
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12. Subaru Deep Survey. VI. A Census of Lyman Break Galaxies at z ≃ 4 and 5 in the Subaru Deep Fields: Clustering PropertiesBased on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.

Author

Ouchi, Masami, Shimasaku, Kazuhiro, Okamura, Sadanori, Furusawa, Hisanori, Kashikawa, Nobunari, Ota, Kazuaki, Doi, Mamoru, Hamabe, Masaru, Kimura, Masahiko, Komiyama, Yutaka, Miyazaki, Masayuki, Miyazaki, Satoshi, Nakata, Fumiaki, Sekiguchi, Maki, Yagi, Masafumi, and Yasuda, Naoki

Published
2004
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13. Subaru Deep Survey. V. A Census of Lyman Break Galaxies at z ≃ 4 and 5 in the Subaru Deep Fields: Photometric PropertiesBased on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.

Author

Ouchi, Masami, Shimasaku, Kazuhiro, Okamura, Sadanori, Furusawa, Hisanori, Kashikawa, Nobunari, Ota, Kazuaki, Doi, Mamoru, Hamabe, Masaru, Kimura, Masahiko, Komiyama, Yutaka, Miyazaki, Masayuki, Miyazaki, Satoshi, Nakata, Fumiaki, Sekiguchi, Maki, Yagi, Masafumi, and Yasuda, Naoki

Published
2004
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14. Cosmic Shear Statistics in the Suprime-Cam 2.1 Square Degree Field: Constraints on Ωm and σ8Based on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.

Author

Hamana, Takashi, Miyazaki, Satoshi, Shimasaku, Kazuhiro, Furusawa, Hisanori, Doi, Mamoru, Hamabe, Masaru, Imi, Katsumi, Kimura, Masahiko, Komiyama, Yutaka, Nakata, Fumiaki, Okada, Norio, Okamura, Sadanori, Ouchi, Masami, Sekiguchi, Maki, Yagi, Masafumi, and Yasuda, Naoki

Published
2003
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15. Subaru Deep Survey. II. Luminosity Functions and Clustering Properties of Lyα Emitters at z = 4.86 in the Subaru Deep FieldBased on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.

Author

Ouchi, Masami, Shimasaku, Kazuhiro, Furusawa, Hisanori, Miyazaki, Masayuki, Doi, Mamoru, Hamabe, Masaru, Hayashino, Tomoki, Kimura, Masahiko, Kodaira, Keiichi, Komiyama, Yutaka, Matsuda, Yuichi, Miyazaki, Satoshi, Nakata, Fumiaki, Okamura, Sadanori, Sekiguchi, Maki, Shioya, Yasuhiro, Tamura, Hajime, Taniguchi, Yoshiaki, Yagi, Masafumi, and Yasuda, Naoki

Published
2003
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16. 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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18. 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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19. 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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21. The Milky Way Tomography with SDSS. III. Stellar Kinematics

Author

Bond, Nicholas A., Ivezic, Zeljko, Sesar, Branimir, Juric, Mario, Munn, Jeffrey A., Kowalski, Adam, Loebman, Sarah, Roskar, Rok, Beers, Timothy C., Dalcanton, Julianne, Rockosi, Constance M., Yanny, Brian, Newberg, Heidi J., Allende Prieto, Carlos, Wilhelm, Ron, Lee, Young Sun, Sivarani, Thirupathi, Majewski, Steven R., Norris, John E., Bailer-Jones, Coryn A. L., Fiorentin, Paola Re, Schlegel, David, Uomoto, Alan, Lupton, Robert H., Knapp, Gillian R., Gunn, James E., Covey, Kevin R., Smith, J. Allyn, Miknaitis, Gajus, Doi, Mamoru, Tanaka, Masayuki, Fukugita, Masataka, Kent, Steve, Finkbeiner, Douglas, Quinn, Tom R., Hawley, Suzanne, Anderson, Scott, Kiuchi, Furea, Chen, Alex, Bushong, James, Sohi, Harkirat, Haggard, Daryl, Kimball, Amy, McGurk, Rosalie, Barentine, John, Brewington, Howard, Harvanek, Mike, Kleinman, Scott, Krzesinski, Jurek, Long, Dan, Nitta, Atsuko, Snedden, Stephanie, Lee, Brian, Pier, Jeffrey R., Harris, Hugh, Brinkmann, Jonathan, and Schneider, Donald P.

Subjects
Galaxy: disk, Galaxy: halo, Galaxy: kinematics and dynamics, Galaxy: stellar content, Galaxy: structure, methods: data analysis, stars: statistics
Abstract

We study Milky Way kinematics using a sample of 18.8 million main-sequence stars with r < 20 and proper-motion measurements derived from Sloan Digital Sky Survey (SDSS) and POSS astrometry, including ~170,000 stars with radial-velocity measurements from the SDSS spectroscopic survey. Distances to stars are determined using a photometric-parallax relation, covering a distance range from ~100 pc to 10 kpc over a quarter of the sky at high Galactic latitudes (|b|>20°). We find that in the region defined by 1 kpc

Published
2010
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22. The Milky Way Tomography with SDSS. II. Stellar Metallicity

Author

Ivezic, Zeljko, Sesar, Branimir, Juric, Mario, Bond, Nicholas, Dalcanton, Julianne, Rockosi, Constance M., Yanny, Brian, Newberg, Heidi J., Beers, Timothy C., Allende Prieto, Carlos, Wilhelm, Ron, Lee, Young Sun, Sivarani, Thirupathi, Norris, John E., Bailer‐Jones, Coryn A. L., Re Fiorentin, Paola, Schlegel, David, Uomoto, Alan, Lupton, Robert H., Knapp, Gillian R., Gunn, James E., Covey, Kevin R., Smith, J. Allyn, Miknaitis, Gajus, Doi, Mamoru, Tanaka, Masayuki, Fukugita, Masataka, Kent, Steve, Finkbeiner, Douglas, Munn, Jeffrey A., Pier, Jeffrey R., Quinn, Tom, Hawley, Suzanne, Anderson, Scott, Kiuchi, Furea, Chen, Alex, Bushong, James, Sohi, Harkirat, Haggard, Daryl, Kimball, Amy, Barentine, John, Brewington, Howard, Harvanek, Mike, Kleinman, Scott, Krzesinski, Jurek, Long, Dan, Nitta, Atsuko, Snedden, Stephanie, Lee, Brian, Harris, Hugh, Brinkmann, Jonathan, Schneider, Donald P., and York, Donald G.

Subjects
Galaxy: halo, Galaxy: kinematics and dynamics, Galaxy: stellar content, Galaxy: structure, methods: data analysis, stars: statistics
Abstract

Using effective temperature and metallicity derived from SDSS spectra for ~60,000 F- and G-type main-sequence stars (0.2 < g − r < 0.6), we develop polynomial models for estimating these parameters from the SDSS u − g and g − r colors. These photometric estimates have similar error properties as those determined from SDSS spectra. We apply this method to SDSS photometric data for over 2 million F/G stars and measure the unbiased metallicity distribution for a complete volume-limited sample of stars at distances between 500 pc and 8 kpc. The metallicity distribution can be exquisitely modeled using two components with a spatially varying number ratio, which correspond to disk and halo. The two components also possess the kinematics expected for disk and halo stars. The metallicity of the halo component is spatially invariant, while the median disk metallicity smoothly decreases with distance from the Galactic plane from –0.6 at 500 pc to –0.8 beyond several kiloparsecs. The absence of a correlation between metallicity and kinematics for disk stars is in a conflict with the traditional decomposition in terms of thin and thick disks. We detect coherent substructures in the kinematics-metallicity space, such as the Monoceros stream, which rotates faster than the LSR, and has a median metallicity of [Fe/H] = −0.95, with an rms scatter of only ~0.15 dex. We extrapolate our results to the performance expected from the Large Synoptic Survey Telescope (LSST) and estimate that LSST will obtain metallicity measurements accurate to 0.2 dex or better, with proper-motion measurements accurate to ~0.5 mas yr−1, for about 200 million F/G dwarf stars within a distance limit of ~100 kpc (g < 23.5)., Astronomy

Published
2008
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23. The Sixth Data Release of the Sloan Digital Sky Survey

Author

Adelman‐McCarthy, Jennifer K., Agüeros, Marcel A., Allam, Sahar S., Allende Prieto, Carlos, 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., Boroski, William N., Brinchmann, Jarle, Brinkmann, J., Brunner, Robert J., Budavári, Tamás, Carliles, Samuel, Carr, Michael A., Castander, Francisco J., Cinabro, David, Cool, R. J., Covey, Kevin R., Csabai, István, Cunha, Carlos E., Davenport, James R. A., Dilday, Ben, Doi, Mamoru, Eisenstein, Daniel James, Evans, Michael L., Fan, Xiaohui, Finkbeiner, Douglas, Friedman, Scott D., Frieman, Joshua A., Fukugita, Masataka, Gänsicke, Boris T., Gates, Evalyn, Gillespie, Bruce, Glazebrook, Karl, Gray, Jim, Grebel, Eva K., Gunn, James E., Gurbani, Vijay K., Hall, Patrick B., Harding, Paul, Harvanek, Michael, Hawley, Suzanne L., Hayes, Jeffrey, Heckman, Timothy M., Hendry, John S., Hindsley, Robert B., Hirata, Christopher M., Hogan, Craig J., Hogg, David W., Hyde, Joseph B., Ichikawa, Shin‐ichi, Ivezi?, ?eljko, Jester, Sebastian, Johnson, Jennifer A., Jorgensen, Anders M., Juric, Mario, Kent, Stephen M., Kessler, R., Kleinman, S. J., Knapp, G. R., Kron, Richard G., Krzesinski, Jurek, Kuropatkin, Nikolay, Lamb, Donald Q., Lampeitl, Hubert, Lebedeva, Svetlana, Lee, Young Sun, Leger, R. French, Lépine, Sébastien, Lima, Marcos, Lin, Huan, Long, Daniel C., Loomis, Craig P., Loveday, Jon, Lupton, Robert H., Malanushenko, Olena, Malanushenko, Viktor, Mandelbaum, Rachel, Margon, Bruce, Marriner, John P., Martínez‐Delgado, David, Matsubara, Takahiko, McGehee, Peregrine M., McKay, Timothy A., Meiksin, Avery, Morrison, Heather L., Munn, Jeffrey A., Nakajima, Reiko, Neilsen, Eric H. Jr., Newberg, Heidi Jo, Nichol, Robert C., Nicinski, Tom, Nieto‐Santisteban, Maria, Nitta, Atsuko, Okamura, Sadanori, Owen, Russell, Oyaizu, Hiroaki, Padmanabhan, Nikhil, Pan, Kaike, Park, Changbom, Peoples, Jr., John, Pier, Jeffrey R., Pope, Adrian C., Purger, Norbert, Raddick, M. Jordan, Re Fiorentin, Paola, Richards, Gordon T., Richmond, Michael W., Riess, Adam G., Rix, Hans‐Walter, Rockosi, Constance M., Sako, Masao, Schlegel, David J., Schneider, Donald P., Schreiber, Matthias R., Schwope, Axel D., Seljak, Uros, Sesar, Branimir, Sheldon, Erin, Shimasaku, Kazu, Sivarani, Thirupathi, Smith, J. Allyn, Snedden, Stephanie A., Steinmetz, Matthias, Strauss, Michael A., SubbaRao, Mark, Suto, Yasushi, Szalay, Alexander S., Szapudi, István, Szkody, Paula, Tegmark, Max, Thakar, Aniruddha R., Tremonti, Christy A., Tucker, Douglas L., Uomoto, Alan, Vanden Berk, Daniel E., Vandenberg, Jan, Vidrih, S., Vogeley, Michael S., Voges, Wolfgang, Vogt, Nicole P., Wadadekar, Yogesh, Weinberg, David H., West, Andrew A., White, Simon D. M., Wilhite, Brian C., Yanny, Brian, Yocum, D. R., York, Donald G., Zehavi, Idit, and Zucker, Daniel B.

Subjects
atlases, catalogs, surveys
Abstract

This paper describes the Sixth Data Release of the Sloan Digital Sky Survey. With this data release, the imaging of the northern Galactic cap is now complete. The survey contains images and parameters of roughly 287 million objects over 9583 deg2, including scans over a large range of Galactic latitudes and longitudes. The survey also includes 1.27 million spectra of stars, galaxies, quasars, and blank sky (for sky subtraction) selected over 7425 deg2. This release includes much more stellar spectroscopy than was available in previous data releases and also includes detailed estimates of stellar temperatures, gravities, and metallicities. The results of improved photometric calibration are now available, with uncertainties of roughly 1% in g, r, i, and z, and 2% in u, substantially better than the uncertainties in previous data releases. The spectra in this data release have improved wavelength and flux calibration, especially in the extreme blue and extreme red, leading to the qualitatively better determination of stellar types and radial velocities. The spectrophotometric fluxes are now tied to point-spread function magnitudes of stars rather than fiber magnitudes. This gives more robust results in the presence of seeing variations, but also implies a change in the spectrophotometric scale, which is now brighter by roughly 0.35 mag. Systematic errors in the velocity dispersions of galaxies have been fixed, and the results of two independent codes for determining spectral classifications and redshifts are made available. Additional spectral outputs are made available, including calibrated spectra from individual 15 minute exposures and the sky spectrum subtracted from each exposure. We also quantify a recently recognized underestimation of the brightnesses of galaxies of large angular extent due to poor sky subtraction; the bias can exceed 0.2 mag for galaxies brighter than r = 14 mag., Astronomy

Published
2008
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24. Exploring the Variable Sky with the Sloan Digital Sky Survey

Author

Sesar, Branimir, Ivezic, Zeljko, Lupton, Robert H., Juric, Mario, Gunn, James E., Knapp, Gillian R., De Lee, Nathan, Smith, J. Allyn, Miknaitis, Gajus, Lin, Huan, Tucker, Douglas, Doi, Mamoru, Tanaka, Masayuki, Fukugita, Masataka, Holtzman, Jon, Kent, Steve, Yanny, Brian, Schlegel, David, Finkbeiner, Douglas, Padmanabhan, Nikhil, Rockosi, Constance M., Bond, Nicholas, Lee, Brian, Stoughton, Chris, Jester, Sebastian, Harris, Hugh, Harding, Paul, Brinkmann, Jon, Schneider, Donald P., York, Donald, Richmond, Michael W., and Vanden Berk, Daniel

Subjects
Galaxy: halo, Galaxy: stellar content, quasars: general, stars: Population II, stars: variables: other
Abstract

We quantify the variability of faint unresolved optical sources using a catalog based on multiple SDSS imaging observations. The catalog covers SDSS stripe 82, which lies along the celestial equator in the southern Galactic hemisphere (22h24m < αJ2000.0 < 04h08m, -1.27° < δJ2000.0 < +1.27°, ~290 deg2), and contains 34 million photometric observations in the SDSS ugriz system for 748,084 unresolved sources at high Galactic latitudes (b < -20°) that were observed at least four times in each of the ugri bands (with a median of 10 observations obtained over ~6 yr). In each photometric bandpass we compute various low-order light-curve statistics, such as rms scatter, χ2 per degree of freedom, skewness, and minimum and maximum magnitude, and use them to select and study variable sources. We find that 2% of unresolved optical sources brighter than g = 20.5 appear variable at the 0.05 mag level (rms) simultaneously in the g and r bands (at high Galactic latitudes). The majority (2 out of 3) of these variable sources are low-redshift (<2) quasars, although they represent only 2% of all sources in the adopted flux-limited sample. We find that at least 90% of quasars are variable at the 0.03 mag level (rms) and confirm that variability is as good a method for finding low-redshift quasars as the UV excess color selection (at high Galactic latitudes). We analyze the distribution of light-curve skewness for quasars and find that it is centered on zero. We find that about one-fourth of the variable stars are RR Lyrae stars, and that only 0.5% of stars from the main stellar locus are variable at the 0.05 mag level. The distribution of light-curve skewness in the g - r versus u - g color-color diagram on the main stellar locus is found to be bimodal (with one mode consistent with Algol-like behavior). Using over 600 RR Lyrae stars, we demonstrate rich halo substructure out to distances of 100 kpc. We extrapolate these results to the expected performance by the Large Synoptic Survey Telescope and estimate that it will obtain well-sampled, 2% accurate, multicolor light curves for ~2 million low-redshift quasars and discover at least 50 million variable stars., Astronomy

Published
2007
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25. 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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26. 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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27. 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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28. 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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29. 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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30. 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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31. 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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32. 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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33. Optical and Radio Properties of Extragalactic Sources Observed by the FIRST Survey and the Sloan Digital Sky Survey

Author

Ivezić, Željko, Menou, Kristen, Knapp, Gillian R., Strauss, Michael A., Lupton, Robert H., Vanden Berk, Daniel E., Richards, Gordon T., Tremonti, Christy, Weinstein, Michael A., Anderson, Scott, Bahcall, Neta A., Becker, Robert H., Bernardi, Mariangela, Blanton, Michael, Eisenstein, Daniel, Fan, Xiaohui, Finkbeiner, Douglas, Finlator, Kristian, Frieman, Joshua, Gunn, James E., Hall, Pat B., Kim, Rita S. J., Kinkhabwala, Ali, Narayanan, Vijay K., Rockosi, Constance M., Schlegel, David, Schneider, Donald P., Strateva, Iskra, SubbaRao, Mark, Thakar, Aniruddha R., Voges, Wolfgang, White, Richard L., Yanny, Brian, Brinkmann, Jonathan, Doi, Mamoru, Fukugita, Masataka, Hennessy, Gregory S., Munn, Jeffrey A., Nichol, Robert C., and York, Donald G.

Subjects
galaxies: active, galaxies: photometry, quasars: general, radio continuum
Abstract

We discuss the optical and radio properties of ~30,000 FIRST (radio, 20 cm, sensitive to 1 mJy) sources positionally associated within 1farcs5 with a Sloan Digital Sky Survey (SDSS) (optical, sensitive to r* ~ 22.2) source in 1230 deg2 of sky. The matched sample represents ~30% of the 108,000 FIRST sources and 0.1% of the 2.5 × 107 SDSS sources in the studied region. SDSS spectra are available for 4300 galaxies and 1154 quasars from the matched sample and for a control sample of 140,000 galaxies and 20,000 quasars in 1030 deg2 of sky. Here we analyze only core sources, which dominate the sample; the fraction of SDSS-FIRST sources with complex radio morphology is determined to be less than 10%. This large and unbiased catalog of optical identifications provides much firmer statistical footing for existing results and allows several new findings. The majority (83%) of the FIRST sources identified with an SDSS source brighter than r* = 21 are optically resolved; the fraction of resolved objects among the matched sources is a function of the radio flux, increasing from ~50% at the bright end to ~90% at the FIRST faint limit. Nearly all optically unresolved radio sources have nonstellar colors indicative of quasars. We estimate an upper limit of ~5% for the fraction of quasars with broadband optical colors indistinguishable from those of stars. The distribution of quasars in the radio flux–optical flux plane suggests the existence of the "quasar radio dichotomy"; 8% ± 1% of all quasars with i* < 18.5 are radio-loud, and this fraction seems independent of redshift and optical luminosity. The radio-loud quasars have a redder median color by 0.08 ± 0.02 mag, and show a 3 times larger fraction of objects with extremely red colors. FIRST galaxies represent 5% of all SDSS galaxies with r* < 17.5, and 1% for r* < 20, and are dominated by red (u*-r* > 2.22) galaxies, especially those with r* > 17.5. Magnitude- and redshift-limited samples show that radio galaxies have a different optical luminosity distribution than nonradio galaxies selected by the same criteria; when galaxies are further separated by their colors, this result remains valid for both blue and red galaxies. For a given optical luminosity and redshift, the observed optical colors of radio galaxies are indistinguishable from those of all SDSS galaxies selected by identical criteria. The distributions of radio-to-optical flux ratio are similar for blue and red galaxies in redshift-limited samples; this similarity implies that the difference in their luminosity functions and resulting selection effects are the dominant cause for the preponderance of red radio galaxies in flux-limited samples. The fraction of radio galaxies whose emission-line ratios indicate an AGN (30%), rather than starburst, origin is 6 times larger than the corresponding fraction for all SDSS galaxies (r* < 17.5). We confirm that the AGN-to-starburst galaxy number ratio increases with radio flux and find that radio emission from AGNs is more concentrated than radio emission from starburst galaxies., Astronomy

Published
2002
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34. 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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35. 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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36. 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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41. A Measurement of the Rate of Type Ia Supernovae at Redshift z ≈ 0.1 from the First Season of the SDSS-II Supernova Survey.

Author

Dilday, Benjamin, Kessler, Richard, Frieman, Joshua A., Holtzman, Jon, Marriner, John, Miknaitis, Gajus, Nichol, Robert C., Romani, Roger, Sako, Masao, Bassett, Bruce, Becker, Andrew, Cinabro, David, DeJongh, Fritz, Depoy, Darren L., Doi, Mamoru, Garnavich, Peter M., Hogan, Craig J., Jha, Saurabh, Konishi, Kohki, and Lampeitl, Hubert

Published
2008
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46. THE SLOAN DIGITAL SKY SURVEY-II SUPERNOVA SURVEY: TECHNICAL SUMMARY.

Author

Frieman, Joshua A., Bassett, Bruce, Becker, Andrew, Choi, Changsu, Cinabro, David, DeJongh, Fritz, Depoy, Darren L., Dilday, Ben, Doi, Mamoru, Garnavich, Peter M., Hogan, Craig J., Holtzman, Jon, Im, Myungshin, Jha, Saurabh, Kessler, Richard, Konishi, Kohki, Lampeitl, Hubert, Marriner, John, Marshall, Jennifer L., and McGinnis, David

Published
2008
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49. Luminosity Functions of Lyman Break Galaxies at z ~ 4 and z ~ 5 in the Subaru Deep Field.

Author

Yoshida, Makiko, Shimasaku, Kazuhiro, Kashikawa, Nobunari, Ouchi, Masami, Okamura, Sadanori, Ajiki, Masaru, Akiyama, Masayuki, Ando, Hiroyasu, Aoki, Kentaro, Doi, Mamoru, Furusawa, Hisanori, Hayashino, Tomoki, Iwamuro, Fumihide, Iye, Masanori, Karoji, Hiroshi, Kobayashi, Naoto, Kodaira, Keiichi, Kodama, Tadayuki, Komiyama, Yutaka, and Malkan, Matthew A.

Published
2006
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