Abstract
We investigate Arp 295, a pair of interacting spirals at z = 0.023, using optical spectroscopy, Hα imaging, and H α velocity mapping with the Manchester Echelle Spectrograph. Scalelengths are rexp = 5.24 for Arp 295a and 2.52 kpc for 295b. A much smaller Im galaxy, Arp 295c, is associated with the larger spiral. Arp 295b is asymmetric with the disk more extended eastwards but with the brightest star-formation regions on its western side. The spectrum of Arp 295b shows strong emission lines with [OII]3727 equivalent width 36Å. The total Hα luminosities of Arp 295b and Arp 295c are 4.69×10^{41} and 6.76×10^{40} ergs s^{-1}, corresponding to star-formation rates 3.7 and 0.53 M_⊙ yr^{-1}. For Arp 295b, we measure the maximum disk rotation velocity as 252.6+/-9.9 kms^{-1} and find the rotation curve is very asymmetric. The east (approaching) side has a higher radial velocity than the west with the maximum difference (at r = 5 arcsec) of 88kms^{-1}, or a factor 1.675.
