UGC 1310 (NGC 694) resides in a small group of galaxies, the main other members
of which are NGC 680, 691 and 697 (Garcia 1993). The central regions of this
group were imaged in H I before by van Moorsel (1988). Apart from UGC 1310, we
also detect H I emission in NGC 691, 697 and UGC 1313, but as these are all of
later morphological type, they are not included in the present study. The H I
disk of UGC 1310 is barely resolved in our observations. As a result, the line
profiles are strongly affected by beam-smearing; the method described in Sect.
3.5 to derive the velocity field is therefore inadequate and fails to recover
the projected rotational velocities of the gas.
NGC 694 (Mrk 363). In PE87, we argued that this galaxy is a S0, but
subsequent better quality imaging suggest to us that this galaxy is truly
anomalous and is more properly classified as a peculiar late-type
starburst galaxy. We base our change in classification primarily on the
deep I-band image of this galaxy of Smith (1988) that shows faint spiral
arms extending quite far from the inner region we discussed.
= MRK 0363
= V Zw 122
In a group with NGC 0678, NGC 0680, NGC 0691, NGC 0695, NGC 0697 and IC 0167.
Classification and dimensions in RC1 refer to IC 0167,
the large spiral 5 arcmin south-following.
(= V ZW 122)
V Zw 122
Sc (de Vaucouleurs)
`Post-eruptive spiral, compact blue core and various knots' (CGPG)
NGC 697 group
V Zw 122
Member of a group.
Post-eruptive spiral, with compact blue core and various knots.
m(pg) = 13.9 [CGCG]
= V Zw 122
Elongated almost in Dec, the boundaries are sharp,
and the object is slightly condensed.
In the NGC 0678-0697 Group.
(0.5 arcmin x - ), and
Heidelberg Veroff. Vol. 9, 1926
(0.4 arcmin x 0.25 arcmin)
both rejected as they refer to the nucleus only.
A very compact, fairly bright, two-branched spiral 0.5' long.