HI in the field of the dwarf spheroidal/irregular galaxy Phoenix

New results are presented for a mosaic mapping of the H I in the field of the Local Group dwarf galaxy Phoenix. The observations, obtained with the Australia Telescope Compact Array, cover an area of similar to 2 degrees x 2 degrees. Four velocity components are identified, at heliocentric velocities of -23, 7, 59, and 140 km s(-1). While the gas at 7 km s(-1) is of Galactic origin and the gas at 140 km s(-1) is most likely associated with the Magellanic Stream, the situation for the two other components is unsure. However, it is suggested that the component at -23 km s(-1) is probably associated with Phoenix because: (1) it has a compact structure and is only slightly offset from the optical image, (2) its H I mass of similar to 10(5) M. is what can be expected in such a system, 3) it has a definite velocity gradient, (4) its location west of Phoenix is compatible with the already suspected self-propagation from east to west of the last star formation episode. Because of the large mass (similar to 5 x 10(6) M.) implied if at the distance of Phoenix and also because of its large extent, the component at +59 km s(-1) is most likely not associated. Optical velocities are still needed to confirm or not those possible associations.