FIRST TIER Stoughton Lupton Bernardi Blanton Burles Castander Connolly Eisenstein Frieman Hennessy Hindsley Ivezic Kent Kunszt Lee Meiksin Munn Newberg Nichol Pier Richards Richmond Schlegel Smith Strauss SubbaRao Szalay Thakar Tucker VandenBerk Yanny SECOND TIER Adelman AndersonJ AndersonS Annis BahcallN Bakken Bartelmann Bastian Bauer Berman Bohringer Boroski Bracker Briegel Briggs Brinkmann Brunner Carey Carr Chen Christian Colestock Crocker Csabai Czarapata Dalcanton Davidsen Davis Dehnen Dodelson Doi Dombeck Donahue Elms Ellman Evans Eyer Fan Federwitz Friedman Fukugita Gal Gunn Gillespie Glazebrook Gray Grebel Greene Greenawalt Haas Haiman Haldeman Hall Hamabe Hansen HarrisF HarrisH Harvanek Hawley Hayes Heckman Helmi Henden Hogan Hogg Holmgren Holtzman Huang Hull IchikawaS IchikawaT Johnston Kauffmann Kim Kimball Kinney Klaene KleinmanS Klypin Knapp Korienek Krolik Kron Krzesinski Lamb Leger Limmongkol Lindenmeyer Long Loomis Loveday MacKinnon Mannery Mantsch Margon McGehee McKay Mclean Menou Merelli Mo Monet Nakamura Narayanan Nash Neilsen Newman Nitta Odenkirchen Okada Okamura Ostriker Owen Pauls Peoples Peterson Petravick Pope Pordes Postman Prosapio Quinn Rechenmacher Rivetta Rix Rockosi Rosner Ruthmansdorfer Sandford Schneider Scranton Sekiguchi Sergey Sheth Shimasaku Smee Snedden Stebbins Stubbs Szapudi Szkody Szokoly Tabachnik Tsvatenov Uomoto Vogeley Voges Waddell Walterbos Wang Watanabe Weinberg White White_S Wilhite Wolfe Yasuda York Zehavi Zheng
The Sloan Digital Sky Survey (SDSS) is an imaging and spectroscopic
survey which will eventually cover 
one-quarter of the
Celestial Sphere and collect spectra of 
galaxies,
100,000 quasars, 30,000 stars, and 30,000 serendipity targets. In
June 2001, the SDSS released to the general astronomical community its
Early Data Release (EDR), roughly 462 square degrees of imaging data
including almost 14 million detected objects,
and 54,008 followup spectra. The imaging data was collected in drift
scan mode in five bandpasses (u, g, r, i, and z);
our 95% completeness limits for stars are 22.0, 22.2, 22.2, 21.3, and
20.5, respectively. The photometric calibration is reproducible to
(5, 3, 3, 3, 5)%, respectively. The spectra are flux- and
wavelength-calibrated, with 4096 pixels from 3800Å to 9200Å at
. We present the means by which these data are
distributed to the astronomical community, descriptions of the
hardware used to obtain the data, the software used for processing the
data, the measured quantities for each observed object, and an
overview of the properties of this dataset.
surveys -- catalogs -- atlases