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Title:
Deep imaging of the field of the Z = 4.9 quasar PC 1247+3406, and faint galaxy counts in the K band with the Keck telescope
Authors:
Soifer, B. T.; Matthews, K.; Djorgovski, S.; Larkin, J.; Graham, J. R.; Harrison, W.; Jernigan, G.; Lin, S.; Nelson, J.; Neugebauer, G.; Smith, G.; Smith, J. D.; Ziomkowski, C.
Affiliation:
AA(California Inst. of Technology, Pasadena, CA, US), AB(California Inst. of Technology, Pasadena, CA, US), AC(California Inst. of Technology, Pasadena, CA, US), AD(California Inst. of Technology, Pasadena, CA, US), AE(California Inst. of Technology, Pasadena, CA, US), AF(California Inst. of Technology, Pasadena, CA, US), AG(University of California, Berkeley, CA, US), AH(University of California, Berkeley, CA, US), AI(University of California, Berkeley, CA, US), AJ(University of California, Berkeley, CA, US)
Publication:
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 420, no. 1, p. L1-L4 (ApJL Homepage)
Publication Date:
01/1994
Category:
Astronomy
Origin:
STI
NASA/STI Keywords:
Faint Objects, Galactic Evolution, Galaxies, Infrared Astronomy, Quasars, Red Shift, Astronomical Photography, Cosmology, Infrared Photography, Sky Surveys (Astronomy)
DOI:
10.1086/187148
Bibliographic Code:
1994ApJ...420L...1S

Abstract

We present deep images in the Ks band of the field of the quasar PC 1247+3406 at z = 4.897, obtained using the near-infrared camera on the W. M. Keck telescope. A number of faint sources have been detected, some of which appear to be quite red. Their nature and redshifts remain uncertain at this time. These data are combined with deep Keck infrared images of five additional fields and present galaxy counts reaching down to Ks = 22 mag, comparable to the deepest K-band surveys to date. The data presented here are in good agreement with the Hawaii Deep Survey and represent the first independent verification of those results. The slope of the log N-log S relation derived from these data agrees well with the Hawaii Deep Survey, while the counts are slightly higher, especially at the faintest levels probed here. This may be due to a presence of groups or clusters around the target objects at high redshifts.

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