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Title:
B 1933+503, a dusty radio quasar at z>2. Implications for blank field sub-mm surveys?
Authors:
Chapman, Scott C.; Scott, Douglas; Lewisi, Geraint F.; Borys, Colin; Fahlman, Gregory G.
Affiliation:
AA(Department of Physics and Astronomy, University of British Columbia, Vancouver, B.C. V6T 1Z1, Canada), AB(Department of Physics and Astronomy, University of British Columbia, Vancouver, B.C. V6T 1Z1, Canada), AC(Department of Physics and Astronomy, University of Victoria, Victoria B.C. V8W 3P6, Canada), AD(Department of Physics and Astronomy, University of British Columbia, Vancouver, B.C. V6T 1Z1, Canada), AE(Department of Physics and Astronomy, University of British Columbia, Vancouver, B.C. V6T 1Z1, Canada)
Publication:
Astronomy and Astrophysics, v.352, p.406-414 (1999) (A&A Homepage)
Publication Date:
12/1999
Origin:
A&A
Astronomy Keywords:
GALAXIES: ACTIVE, GALAXIES: QUASARS: INDIVIDUAL: B 1933+503, GALAXIES: STARBURST, COSMOLOGY: OBSERVATIONS, COSMOLOGY: GRAVITATIONAL LENSING, INFRARED: GALAXIES
Bibliographic Code:
1999A&A...352..406C

Abstract

We present a detailed mm-wave and optical study of the gravitational lens system B 1933+503, discovered by Sykes et al. (1998) in the radio. This object is probably the most complex lens system known, with 10 lensed components within a radius of one arcsecond. It is potentially important as a probe of the Hubble constant, although no optical counterpart has thus far been observed down to I {=} 24.2. We have obtained new sub-millimetre detections at 450 mu m, 850 mu m and 1350 mu m. We have also constrained the possible dust emission from the proposed foreground lensing galaxy using a K-band adaptive optics image and CO(5-4) measurements. A lensing model is constructed, taking the foreground elliptical galaxy at z {=} 0.755 as the lensing mass. From this we derive a scenario from which to model the sub-millimetre emission. Several arguments then point to the source in the B 1933+503 system lying above a redshift of 2. We speculate that unlensed relatives of this source may constitute a sizable fraction of the 850 mu m source counts.

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