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Deep galaxy counts in the K band with the Keck telescope

Djorgovski, S. and Soifer, B. T. and Pahre, M. A. and Larkin, J. E. and Smith, J. D. and Neugebauer, G. and Smail, I. and Matthews, K. and Hogg, D. W. and Blandford, R. D. and Cohen, J. G. and Harrison, W. and Nelson, J. (1995) Deep galaxy counts in the K band with the Keck telescope. Astrophysical Journal, 438 (1). L13-L16. ISSN 0004-637X. doi:10.1086/187703.

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We present deep galaxy counts in the K (⋋ 2.2 micrometer) band, obtained at the W. M. Keck 10 m telescope. The data reach limiting magnitudes K approximately 24 mag, about 5 times deeper than the deepest published K-band images to date. The counts are performed in three small (approximately 1 min), widely separated high-latitude fields. Extensive Monte Carlo tests were used to derive the completeness corrections and minimize photometric biases. The counts continue to rise, with no sign of a turnover, down to the limits of our data, with the logarithmic slope of d log N/dm = 0.315 +/- 0.02 between K = 20 and 24 mag. This implies a cumulative surface density of approximately 5 x 10^5 galaxies/sq deg, or approximately 2 x 10^10 over the entire sky, down to K = 24 mag. Our counts are in good agreement with, although slightly lower than, those from the Hawaii Deep Survey by Cowie and collaborators; the discrepancies may be due to the small differences in the aperture corrections. We compare our counts with some of the available theoretical predictions. The data do not require models with a high value of Omega_0, but can be well fitted by models with no (or little) evolution, and cosmologies with a low value of Omega_0. Given the uncertainties in the models, it may be premature to put useful constrains on the value of Omega_0 from the counts alone. Optical-to-IR colors are computed, using CCD data obtaind previously at Palomar. We find a few red galaxies with (r-K) approximately greater than 5 mag, or (i-K) approximately greater than 5 mag; these may be ellipticals at z approximately 1. While the redshift distribution of galaxies in our counts is still unknown, the flux limits reached would allow us to detect unobscured L_* galaxies out to substantial redshifts (z greater than 3?)

Item Type:Article
Related URLs:
URLURL TypeDescription
Djorgovski, S.0000-0002-0603-3087
Larkin, J. E.0000-0001-7687-3965
Smith, J. D.0000-0003-1545-5078
Smail, I.0000-0003-3037-257X
Hogg, D. W.0000-0003-2866-9403
Blandford, R. D.0000-0002-1854-5506
Cohen, J. G.0000-0002-8039-4673
Additional Information:© 1995 American Astronomical Society. Received 1994 August 3; accepted 1994 October 18. The W. M. Keck Observatory is a scientific partnership between the California Institute of Technology and the University of California. It was made possible by the generous and visionary gift of the W. M. Keck foundation, and the support of its president, Howard Keck. It is a pleasure to thank the observing assistants T. Chleminiak and B. Schaefer for the expert work during our observing runs, J. R. Mould for doing the Palomar imaging of the Hercules field, and M. Wilber for the help with the models. This work was supported in part by the NSF PYI award AST-9157412 to S. D., the NSF grant AST-9223370 to R. D. B., grants from the NSF and NASA to B. T. S., G. N., and K. M., a NATO Advanced Fellowship to I. S., and an NSF graduate fellowship to D. W.H.
Funding AgencyGrant Number
W. M. Keck FoundationUNSPECIFIED
North Atlantic Treaty Organization (NATO)UNSPECIFIED
NSF Graduate Research FellowshipUNSPECIFIED
Subject Keywords:cosmology: observations galaxies: evolution galaxies: photometry
Issue or Number:1
Record Number:CaltechAUTHORS:20170228-140004588
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:74597
Deposited By: Ruth Sustaita
Deposited On:28 Feb 2017 23:05
Last Modified:11 Nov 2021 05:28

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