2001AJ....121.1413P

We present the results of H I mapping with the NRAO(2) VLA of one of the most metal-deficient blue compact dwarf (BCD) galaxies known, SBS 0335-052, with an oxygen abundance only 1/40 that of the Sun. We study the structure and dynamics of the neutral gas in this chemically young object with a spatial resolution of 20".5x15" (∼5.4x3.9 kpc at an assumed distance of 54.3 Mpc), a sensitivity at the 2 σ detection level of ∼2.0 K or 7.5x10¹⁹ cm^–2 and a velocity resolution of 21.2 km.s^–1. We detected a large H I complex associated with this object having an overall size of about 66 by 22 kpc and elongated in the east-west direction. There are two prominent, slightly resolved peaks visible in the integrated H I map, separated in the east-west direction 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 H I line and is identified with a faint blue compact dwarf galaxy, SBS 0335-052W, with m_B=19.4, and a metallicity close to the lowest values known for BCDs, about 1/50 that of the Sun. The radial velocities of both systems are similar, suggesting that the two BCDs, SBS 0335-052 and SBS 0335-052W, constitute a pair of dwarf galaxies embedded in a common H I envelope. Alternatively, the BCDs may be the nuclei of two distinct interacting primordial H I clouds. The estimated total dynamical mass, assuming the BCDs form a bound system, is larger than ∼6x10⁹ M_☉, compared with a total gaseous mass M_gas=2.1x10⁹ M_☉ and a total stellar mass M_star≤10⁸ M_☉. Hence, the mass of the SBS 0335-052 system is dominated by dark matter. Because of the disturbed H I velocity field and the presence of what might be tidal tails at either end of the system, we favor the hypothesis of tidal triggering of the star formation in this system. It can be due to either the nearby giant galaxy NGC 1376 or the mutual gravitational interaction of the two H I clouds.