paper

HI study of extremely metal-deficient dwarf galaxies. I. The Nancay Radio Telescope observations of twenty-two objects

arXiv:astro-ph/0701505 · doi:10.1051/0004-6361:20066137

Abstract

The goal of this study is to measure parameters of the integrated HI emission for twenty-two dwarf galaxies with oxygen abundance 12+log(O/H) in the range of 7.42 to 7.65, which are representatives of the eXtremely Metal-Deficient (XMD) galaxy group. Some of them are expected to be similar to the well-known candidates for local young galaxies, IZw18 and SBS 0335-052 that have most of their baryon mass in the form of neutral gas. Therefore, the HI 21-cm line observations are crucial to understanding their group and individual properties. The Nancay Radio Telescope (NRT) with the upgraded focal receiver was used for observations of the 21-cm HI-line. This permitted the detection of the faintest sources with rms of ~1 mJy per 10.5 km/s resolution element. For eighteen detected galaxies we present the parameters of their integrated HI line emission and describe the data on individual objects in more detail. For four undetected XMD galaxies, we give upper limits on their M$(HI). For 70% of the twenty studied non low surface brightness XMD galaxies, we find evidence (both from HI and optical data) for their interaction with neighboring objects. In the brief discussion of the group HI properties of the observed subsample (the total O/H range is of 0.23 dex, or a factor of 1.7), we underline the broad distributions of the HI mass (range is of 2 orders of magnitude), of the ratio M(HI)/L_B (of 1 order of magnitude), and of the blue luminosity (range is of 2 orders of magnitude). We also obtained HI parameters of six galaxies that do not belong to the XMD sample. These data increase the number of XMD galaxies with known integrated HI parameters (or upper limits) by a factor of two. This allows us to address statistical properties of this group, which will be presented in a forthcoming paper. (Abridged).

11 pages, including 2 tables and 2 postscript figures. Accepted to Astronomy and Astrophysics

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