The UV image of this galaxy (Fig. 16, right) shows enhanced emission along the
bar (NE-SW), as well as some emission along the inner spiral arms, which are
seen in the form of a ring, close to the borders of the image. We obtained VLA
8.46 GHz data for this galaxy, but could not detect any radio emission. Lower
resolution (~45" beam), lower frequency (1.4 GHz) observations from the NVSS
catalog (Condon et al. 1998), detected this source. Nevertheless, higher
resolution observations (~4.5" beam) at the same frequency, from the FIRST
catalog (Becker et al. 1995), did not detect it either. This suggests that the
star formation in this galaxy is faint and widespread, resulting in radio
emission below the detection threshold of our 8.46 GHz observations.
[Possible BCD] companion
March 19/20, 1982
103aO + GG385
Current star formation is occurring in the
bar; HII-region candidates exist there. The
brightest HII-region candidate in the arms is
compact, bright, and unresolved at the 1.5"
The redshift is v_o = 1304 km/s. A dwarf
(BCD?) candidate companion exists at a separation
of 6.2' which, at the redshift distance of 26
Mpc (H = 50), corresponds with a projected
linear separation of 47 kpc.
SAB(rs)cd (de Vaucouleurs)
14 29.9 +10 09 at 6.2, 294, 0.7 x 0.6, S0-a, m=15.3
Short, bright bar: 0.2 arcmin x 0.05 arcmin in a pseudo (r): 0.4 arcmin x
0.3 arcmin. 2 main, partially resolved, filamentary arms with some branches.
Lund 9 and Heidelberg Veroff. Vol. 9, 1926 dimensions are for the bright