5.1.2 NGC 1380 - Fig. 2 shows that the new data agree extremely well with the
previous observations, but with much improved error bounds. The new data with
their smaller errors and unfolded presentation give some indication of localized
substructure that differs between the two sides of the galaxy. An enhancement in
velocity dispersion within the central ~7 arcsec, first suggested by D'Onofrio
et al. (1995), is strongly confirmed with the new data. It is also notable from
Fig. A2 that this region also shows structure in the h_3_ skewness measure,
indicative of a distinct kinematic component. Interestingly, this feature
coincides with photometric evidence for a distinct component which comprises a
strong variation in isophotal ellipticity and position angle (Caon, Capaccioli &
NGC 1380 is a lenticular galaxy at a distance of 7.2 Mpc. ULX1 is on the edge of
NGC 1380: after masking the off-center dust lane, the brightness profile is
smooth and well fitted by a power-law. No flattening is seen before the
Feb 1/2, 1979
103aO + Wr2
NGC 1380 is a member of the Fornax
Cluster (Ferguson 1989). The spiral pattern of
the massive arms is pronounced and shows
moderately well in this reproduction. The arms
appear to attach to the bulge at position angles of
about 5 o'clock and 11 o'clock in the print here.
The sense of the spiral pattern is clockwise going
from the outside inward.
Overexposed center, bright nubs form bar. Many faint galaxies near.
=ESO 358- G 28
In the Fornax I Cluster
Star 0.85 arcmin south-preceding the nucleus.
In the Fornax I Cluster.
Very bright nucleus.
Star 0.85 arcmin [south-preceding] the nucleus.
M.N.R.A.S., 111, 526, 1951.