ESO 269-G15. The observed stellar velocity is slightly asymmetric.
Simultaneously, fitting both the observed velocity and dispersion provides a
rather poor match to the data. A larger-amplitude rotation curve (by [IMAGE]10
km s^[IMAGE]1^) would improve the fit but is inconsistent with the H i and H ii
data. A slightly less steeply rising rotation curve is allowed by the data (see
Paper III). However, that would yield a very poor fit.
ESO 269-G15. The density profile is fairly symmetric. The XV diagram on
the other hand is asymmetric, the most striking being that the highest H
I densities on the approaching side do not correspond to
extreme-velocity envelope. On this side the H I appears to be in
solid-body rotation, while on the receding side the rotation curve seems
to reach a flat part. No H I was detected beyond the stellar disc.
ESO 269-G15. There is an offset of 3 arcsec (600 pc) between the optical
centre (table A1 in KKG) and the adopted dynamical centre (Table 4 in
this paper). The symmetry in the stellar velocity and velocity
dispersion curves suggests that this offset is not due to
lopsidedness. Perhaps it is caused by dust attenuation affecting the
determination of the optical centre.
NGC 4835A: strong residuals.
Similar to NGC 5907. Small SB(rs:)bc: 3.0 north-preceding.
=ESO 269- G 15
*small companion 3.0 north preceding