CLASS B0739+366: A New Two-Image Gravitational Lens System

Creators: Marlow, D. R.; Rusin, D.; Norbury, M.; Jackson, N.; Browne, I. W. A.; Wilkinson, P. N.; Fassnacht, C. D.; Myers, S. T.; Koopmans, L. V. E.; Blandford, R. D.; Pearson, T. J.; Readhead, A. C. S.; de Bruyn, A. G.

Abstract

We present the discovery of CLASS B0739+366, a new gravitational lens system from the Cosmic Lens All-Sky Survey. Radio imaging of the source with the Very Large Array shows two compact components separated by 0."54, with a flux density ratio of ~6 : 1. High-resolution follow-up observations using the Very Long Baseline Array (VLBA) at 1.7 GHz detect weak, parity-reversed jet emission from each of the radio components. Hubble Space Telescope Near Infrared Camera and Multi-Object Spectrometer (NICMOS) F160W observations detect infrared counterparts to the lensed images, as well as an extended object between them, which we identify as the lensing galaxy. Redshifts for the galaxy and lensed source have not yet been obtained. For typical lens and source redshifts of z = 0.5 and z = 1.5, respectively, preliminary mass modeling predicts a time delay of ~7 h^(-1) days in a flat Ω_M = 1.0 universe. The small predicted time delay and weak radio components will make CLASS B0739+366 a challenging target for Hubble constant determination.

Additional Information

© 2001 The American Astronomical Society. Received 2000 March 7; accepted 2000 September 12. We thank the staffs of the VLA, MERLIN, and VLBA for their assistance during our observing runs. We also thank the anonymous referee, whose comments and suggestions led to a greatly improved draft. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. MERLIN is operated as a national facility by Nuffield Radio Astronomy Laboratories, University of Manchester, on behalf of the UK Particle Physics and Astronomy Research Council. This research used observations with the Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by Associated Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. D. R. gratefully acknowledges a fellowship from the Zaccheus Daniel Foundation. S. T. M. was supported by an Alfred P. Sloan Fellowship at the University of Pennsylvania. This research was supported in part by European Commission TMR Programme, Research Network Contract ERBFMRXCT96-0034 CERES.

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