Статья

The Sloan Digital Sky Survey View of the Palomar-Green Bright Quasar Survey

Sebastian JesterFermi National Accelerator Laboratory, Mail Stop 127, P.O. Box 500, Batavia, IL 60510Donald P. SchneiderDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802Gordon T. RichardsPrinceton University Observatory, Peyton Hall, Princeton, NJ 08544Richard F. GreenKitt Peak National Observatory, National Optical Astronomy Observatory, P.O. Box 26732, 950 North Cherry Avenue, Tucson, AZ 85726Maarten SchmidtDepartment of Astronomy, MC 105-24, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125Patrick B. HallDepartment of Physics and Astronomy, York University, 4700 Keele Street, Toronto, ON M3J 1P3, CanadaMichael A. StraussPrinceton University Observatory, Peyton Hall, Princeton, NJ 08544D. E. vanden BerkDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802Chris StoughtonFermi National Accelerator Laboratory, Mail Stop 127, P.O. Box 500, Batavia, IL 60510James E. GunnPrinceton University Observatory, Peyton Hall, Princeton, NJ 08544J. BrinkmannApache Point Observatory, P.O. Box 59, Sunspot, NM 88349S. KentDepartment of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637J. A. SmithDepartment of Physics and Astronomy, University of Wyoming, P.O. Box 3905, Laramie, WY 82071D. L. TuckerFermi National Accelerator Laboratory, Mail Stop 127, P.O. Box 500, Batavia, IL 60510B. YannyFermi National Accelerator Laboratory, Mail Stop 127, P.O. Box 500, Batavia, IL 60510

2005en

ABI

Аннотация

The author investigates the extent to which the Palomar-Green (PG) Bright Quasar Survey (BQS) is complete and representative of the general quasar population by comparing with imaging and spectroscopy from the Sloan Digital Sky Survey. A comparison of SDSS and PG photometry of both stars and quasars reveals the need to apply a color and magnitude recalibration to the PG data. Using the SDSS photometric catalog, they define the PG's parent sample of objects that are not main-sequence stars and simulate the selection of objects from this parent sample using the PG photometric criteria and errors. This simulation shows that the effective U-B cut in the PG survey is U-B < -0.71, implying a color-related incompleteness. As the color distribution of bright quasars peaks near U-B = -0.7 and the 2-{sigma} error in U-B is comparable to the full width of the color distribution of quasars, the color incompleteness of the BQS is approximately 50% and essentially random with respect to U-B color for z < 0.5. There is however, a bias against bright quasars at 0.5 < z < 1, which is induced by the color-redshift relation of quasars (although quasars at z > 0.5 are inherently rare in bright surveys in any case). They find no evidence for any other systematic incompleteness when comparing the distributions in color, redshift, and FIRST radio properties of the BQS and a BQS-like subsample of the SDSS quasar sample. However, the application of a bright magnitude limit biases the BQS toward the inclusion of objects which are blue in g-i, in particular compared to the full range of g-i colors found among the i-band limited SDSS quasars, and even at i-band magnitudes comparable to those of the BQS objects.

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Идентификаторы

DOI: 10.1086/432466

Цитирования и источники

Цитирований: 5Использованных источников: 0

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