Hubble Space Telescope images of submillimeter sources: large, irregular galaxies at high redshift

Details Hubble Space Telescope images of submillimeter sources: large, irregular galaxies at high redshift Hubble Space Telescope images of submillimeter sources: large, irregular galaxies at high redshift

2003-08-11

arxiv.org/abs/astro-ph/0308197v2

Astrophys.J.599:92-104,2003

Astronomy and Astrophysics

Astrophysics

16 pages, 6 figures, scheduled for ApJ, v599, Dec10, 2003. Minor edits. For version with higher resolution figures, see http

Scientific paper

10.1086/379120

We present new Hubble Space Telescope STIS, high-resolution optical imaging of a sample of 13 submillimeter (submm) luminous galaxies, for which the optical emission has been pinpointed either through radio-1.4 GHz or millimeter interferometry. We find a predominance of irregular and complex morphologies in the sample, suggesting that mergers are likely common for submm galaxies. The component separation in these objects are on average a factor two larger than local galaxies with similarly high bolometric luminosities. The sizes and star formation rates of the submm galaxies are consistent with the maximal star formation rate densities of 20 Msun kpc^{-2} in local starburst galaxies (Lehnert & Heckman 1996). We derive quantitative morphological information for the optical galaxies hosting the submm emission; total and isophotal magnitudes, Petrosian radius, effective radius, concentration, aspect ratio, surface brightness, and asymmetry. We compare these morphological indices with those of other galaxies lying within the same STIS images. Most strikingly, we find ~70% of the submm galaxies to be extraordinarily large and elongated relative to the field population, regardless of optical magnitude. Comparison of the submm galaxy morphologies with those of optically selected galaxies at z~2-3 reveal the submm galaxies to be a morphologically distinct population, with generally larger sizes, higher concentrations and more prevalent major-merger configurations.

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