The Faint Sub-mm Galaxy Population: HST Morphologies and Colors

Details The Faint Sub-mm Galaxy Population: HST Morphologies and Colors The Faint Sub-mm Galaxy Population: HST Morphologies and Colors

1998-06-04

arxiv.org/abs/astro-ph/9806061v1

Astronomy and Astrophysics

Astrophysics

5 pages, LaTeX, 2 figures, uses emulateapj.sty, submitted to ApJL

Scientific paper

We present optical morphologies obtained from deep HST and ground-based images for galaxies selected from the first sub-millimeter survey of the distant Universe. Our sample comprises galaxies detected in deep 850-micron continuum maps of seven massive clusters, obtained using SCUBA, the new bolometer camera on the JCMT. The survey covers a total area of 0.01 square degrees to 1-sigma noise levels of about 2 mJy/beam. We detect a total of 25 sources at 850 microns, of which 17 and 10 are brighter than the respective 50% and 80% completeness limits. Optical counterparts are identified for 14 of the 16 sources in the f(50%) sample and for 9 of the 10 sources in the f(80%) sample that lie within our optical fields. The morphologies of those galaxies for which we have HST imaging fall into three broad categories: faint disturbed galaxies and interactions; faint galaxies too compact to classify reliably; and dusty, star-forming galaxies at intermediate redshifts. The disturbed and interacting galaxies constitute the largest class, which suggests that interactions remain an important mechanism for triggering star formation and the formation of ultraluminous galaxies in the distant Universe. The faint, compact galaxies may represent a later evolutionary stage in these mergers, or more centrally-concentrated starbursts. It is likely that some of these will host AGN. Analysis of the colors of our sample allow us to estimate a crude redshift distribution: >75% have z<5.5 whilst >50% lie at z<4.5, suggesting that the luminous sub-mm population is coeval with the more modestly star-forming galaxies selected by UV/optical surveys of the distant Universe. This imposes important constraints on models of galaxy formation and evolution.

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