The morphological classification as determined by us is indicated in
parentheses next to the galaxy name, with our "chaotic circumnuclear
dust" (C) category now not including those galaxies with obvious dust
lanes (DL). Where the classification has already been made by Martini
et al. (2003), we indicate this with "-mp."
3.27. NGC 4389
Figure 13 (bottom).
Spectra: Continuum is obvious only in OFF 1 and appears weak. H II
regions are indicated in the spectra, agreeing with Alonso-Herrero &
Knapen (2001), who find multiple H II sites in the galaxy. The
emission lines appear straight.
Image: Location of nucleus is not obvious since it is difficult to
distinguish from probable sites of star formation.
Feb 4/5, 1981
NGC 4389 has a bright bar filled with
discrete HII regions. Its spiral pattern is difficult
to trace because of the large inclination angle. Its
morphology may be similar to that of NGC 4178
(panel 311), NGC 3059 (panels 308, S9), NGC 4116
(panel 306), NGC 3319 (panel 303), and
NGC 4654 (panel 302), all of which are shown
in this SBc section and all of which have
less-steep inclination angles.
The redshift of NGC 4389 is v_o = 767 km/s.
SB(rs)... (de Vaucouleurs)
Small, bright narrow bar: 0.5 arcmin x 0.1 arcmin, crossed by a dark lane.
Pseudo (r): 1.5 arcmin x 0.65 arcmin.
An irregular spiral 1.8' x 0.8'. A bright, somewhat irregular streak lies along
the major axis in p.a. 100^deg^. Most of the nebular matter lies at the ends of
the major axis, and there is evidence of absorption on the northern side.