Properties Of Galaxies Found In A Deep Blind Neutral Hydrogen Survey
Creators: name: Minchin, Robert Frank
Publisher: name: Zenodo
Year: 2001
Subjects: Astronomy
Telescopes: Parkes Observatory
Radio lines: Galaxies
Surveys

description: p&gt;The DEEP survey used the Parkes neutral hydrogen (Hi) multibeam system to observe a 4ordm; xnbsp;8ordm; region to a noise level of 4 mJy per 13.2 km/snbsp;channel, or 3.5 times the column-density sensitivity of previous surveys. A blind Hi survey like DEEP avoids optical selection-e ects such as discrimination against low surface-brightness (LSB) galaxies in de ning the sample. Hi parameters are presented for 69 galaxies found within this region. A deep optical image (eight 1-hour tech pan plates) was obtained, centred on the same position as the Hi survey. Optical parameters from this data are presented for 54 galaxies uniquely identi ed as optical counterparts of the Hi sources. No evidence was found for a population of low column-density galaxies that would be undetected in shallower surveys./p&gt;

p&gt;No high-luminosity, LSB galaxies have been found, however high Hi mass, LSB galaxies were seen. That LSB galaxies make up more than 12% of the total population of high-luminosity galaxies can be ruled out with 95% con dence, however LSB galaxies could, to the same con dence level, contribute up to 46% of high Hi mass galaxies. Luminosity is not a good guide to the total baryon content of LSB galaxies. The surface-brightness distribution and the luminosity function have been found for the DEEP galaxies./p&gt;

p&gt;The surface-brightness distribution is truncated at the high surface-brightness end, with the down-turn occuring near the #39;Freeman-law#39;nbsp;value while it is slowly increasing towards lower surface-brightnesses. The luminosity function is fairly at, consistent with faint-end slopes for eld galaxies from the literature. Further analysis of this data shows that low surface-brightness galaxies could make a signi cant contribution to the cosmic baryon density (19% to 71% at 1sigma;) and to the dynamical mass density of the Universe (27% to 90% at 1sigma;).nbsp;/p&gt;
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