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Redshifts for 2410 Galaxies in the Century Survey Region* **

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© 2001. The American Astronomical Society. All rights reserved. Printed in U.S.A.
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Author affiliations

1 Department of Physics and Astronomy, 6127 Wilder Laboratory, Dartmouth College, Hanover, NH 03755-3528

2 Harvard-Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138

3 Department of Astronomy and Physics, San Francisco State University, 1600 Holloway Avenue, San Francisco, CA 94132

4 Division of Astronomy and Astrophysics, Department of Physics and Astronomy, University of California, Los Angeles, 405 Hilgard Avenue, Los Angeles, CA 90095-1562

Dates

Received 2001 June 7
Accepted 2001 August 15

Citation

Gary Wegner et al 2001 AJ 122 2893

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DOI

https://doi.org/10.1086/323915

Keywords

cosmology: observations; cosmology: theory; galaxies: distances and redshifts; large-scale structure of universe

Journal RSS feed

1538-3881/122/6/2893

Abstract

The Century Survey strip covers 102 deg2 within the limits 8fh5 ≤ α ≤ 16fh5, 29fdg0 ≤ δ ≤ 30fdg0, equinox B1950.0. The strip passes through the Corona Borealis supercluster and the outer region of the Coma cluster. Within the Century Survey region, we have measured 2410 redshifts that constitute four overlapping complete redshift surveys: (1) 1728 galaxies with Kron-Cousins Rph ≤ 16.13 covering the entire strip, (2) 507 galaxies with Rph ≤ 16.4 in right ascension range 8h32m ≤ α ≤ 10 h45m, equinox B1950.0, (3) 1251 galaxies with absorption- and K-corrected RCCDc ≤ 16.2 (where "c" indicates "corrected") covering the right ascension range 8fh5 ≤ α ≤ 13fh5, equinox B1950.0, and (4) 1255 galaxies with absorption- and K-corrected VCCDc ≤ 16.7 also covering the right ascension range 8fh5 ≤ α ≤ 13fh5, equinox B1950.0. All these redshift samples are more than 98% complete to the specified magnitude limit. We derived samples 1 and 2 from scans of the POSS1 red (E) plates calibrated with CCD photometry. We derived samples 3 and 4 from deep V and R CCD images covering the entire region. We include coarse morphological types for all the galaxies in sample 1. The distribution of (V-R)CCD for each type corresponds appropriately with the classification.

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Footnotes

  • * 

    Work reported here is based partly on observations obtained at the Michigan-Dartmouth-MIT Observatory.

  • ** 

    Work reported here is based partly on observations at the Multiple Mirror Telescope, a joint facility of the Smithsonian Institution and the University of Arizona.

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