Computer Science
Scientific paper
Nov 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000ign..confe...5b&link_type=abstract
Ionized Gaseous Nebulae. Mexico City November 21- 24, 2000, meeting abstract
Computer Science
Scientific paper
We present VLA HI observations of one of the most metal-deficient blue compa ct dwarf (BCD) galaxies known, SBS 0335-052, which sports an oxygen abundance of only 1/40th that of the Sun. We study the structure and dynamics of the neutral gas in this chemically young object at a spatial resolution of 20'' x 15'' (5.4 x 3.9 kpc at an assumed distance of 54 Mpc), and a velocity resolution of 21.2 km/s. We detected a large HI complex associated with this object with an overall size of about 64 x 21 kpc and elongated in the East-West direction. There are two prominent, slightly resolved peaks visible which are separated by 22 kpc (84''). The eastern peak is nearly coincident with the position of the optical galaxy SBS 0335-052. The western peak is about a factor of 1.3 brighter in the HI line and is identified with a faint blue compact galaxy, SBS 0335-052W, which has an mV = 19, and a metallicity close to the lowest values known for BCDs, about 1/50th that of the Sun. The radial velocities of both systems are similar, suggesting that the two BCDs form a pair of dwarf galaxies embedded in a common HI envelope. Alternatively, the BCDs could be the nuclei of two distinct interacting primordial HI clouds. The estimated total dynamical mass, assuming the BCDs form a bound system, is larger than 7 x 109 Mo. This is to be compared to a total gaseous mass Mgas = 2.0 x 109 Mo, and a total stellar mass Mstar < 108 Mo. Hence, the mass of the SBS 0335-052 system is dominated by dark matter. Because of the disturbed HI velocity field and the presence of what might be tidal tails at either end of the system, we favor the hypothesis that the star formation trigger in this system was provided by a tidal interaction, either with the nearby giant galaxy NGC 1376 or as a result of the mutual gravitational interaction of the two HI clouds proper.
Brinks Elias
Izotov Yu. I.
Lipovetsky Valentin
Pustilnik Simon
Thuan Trinh Xuan
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