Did VV 29 collide with a dark Dark-Matter halo?

Westerbork Radio Synthesis Telescope observation of the galaxy VV 29 = Arp 188 = UGC 10214 shows that there are at least three distinct dynamical comp onents whose kinematics can be traced in 21 cm line emission. The system ap pears to be the result of a galaxy-galaxy interaction. We identify a suffic ient number of dynamical elements containing baryons (stars and neutral gas ) that there is no compelling reason to postulate the presence of an additi onal dark matter halo that is devoid of detectable baryons. The central gal axy VV 29a is massive (V-rot similar to 330 km s(-1)) and gas rich (M-HI si milar to 6 x 10(9) h(-2) M-.). The distinctive optical plume (VV 29b), whic h extends eastward from the main galaxy, is also gas rich (M-HI similar to 3 similar to 10(9) h(-2) M-.) and has a very low gradient in line of sight velocity (<30 km s(-1)) over <similar to>70 h(-1) kpc. On the western side, there is an HI feature of M-HI similar to 4 x 10(8) h(-2) M-. that partici pates strongly in orbital motion about the host in the same sense of rotati on as the VV 29a itself. A blue, less massive, gas-rich galaxy "VV 29c" (M- HI similar to 9 x 10(8) h(-2) M-.) appears clearly in the HI maps as an sim ilar to 170 km s(-1) wide spectral feature, seen in projection against or, more likely, behind the west side of the host disk. Its high recessional ve locity is counter to the host rotation direction. The optical images of Tre ntham et al. (2001) show signs of this blue dwarf against the redder VV 29a disk. The companion galaxy CGCG 27-021 = MGC 09-26-54 (at projected distan ce similar to 115 h(-1) kpc) is not detected in 21 cm line emission (M-HI < 10(9) h(-2) M-.).