NGC 4350 (Pignatelli, Salucci & Danese 2001), NGC 4486B (Kormendy et al.
1997) and NGC 4594 (Kormendy et al. 1996) - Their mass measurement is
uncertain due to the lack of three-integral stellar dynamical models.
VCC 685 (NGC 4350).This is a very elongated system, with a large-scale edge-on
stellar disk typical of S0 galaxies. The presence of the disk affects the B4
coefficient, which becomes positive beyond a few arcsec. There is a nuclear,
nearly edge-on dust disk, about 4" in diameter. The dust disk is surrounded by a
blue stellar disk, extending perhaps 1.5" beyond the edge of the dust disk.
Dust, stellar, and outer disks are all aligned. In correcting for dust
absorption, the color of the region underlying the dust disk has been assumed
equal to the color of the surrounding stellar disk, although the correction is
still not entirely successful. There is no obvious evidence for the presence of
a nucleus from the color images or the surface brightness profiles (although
this is not a secure conclusion, because of the presence of the dust). The vast
majority of globular clusters are found in the equatorial plane of the galaxy
and are therefore likely associated with the large-scale disk.
This well-studied edge-on lenticular galaxy forms a pair with
NGC 4340. The surface brightness profile of this galaxy clearly
indicates the presence of bulge and disk components. The Mg2
line-strength profiles along the major and minor axes of the galaxy
differ dramatically and convincingly indicate the presence bulge and
disk components (Fisher et al. 1996). Michard & Marchal (1993)
described UGC 7473 as having a disk fully embedded in a spheroidal
halo. A disk of rapidly rotating gas is present within the inner 3";
this is decoupled from the stellar component (Fisher 1997). A
concentration of dust in the disk has been proposed by Michard &
Poulain (2000). Our B-R and B-K' color and extinction maps also
clearly reveal an inclined disk. The ellipticity rises from 0.2 to
0.61 over the observed region and the b_4_ coefficient becomes
significantly positive beyond 6", which reflects the presence of a
NGC 4350. NVSS did not detect this source. At 5 GHz, 5" resolution,
there is an upper limit of 0.5 mJy to any emission (Wrobel & Heeschen
NGC 4594 (Kormendy et al. 1996b), NGC 4486B (Kormendy et al. 1997),
NGC 4350 (Pignatelli, Salucci, & Danese 2001), NGC 3031 = M81, and
NGC 3998 (Bower et al. 2000) exhibit strong evidence from stellar
dynamics for a black hole but do not yet have three-integral dynamical
NGC 4350. The rotation curve of NGC 4350 shows a region of rapidly increasing
rotation within the inner 2" followed by a 5" long region of slowly increasing
rotation speed. The rotation curve then increases steadily before flattening
beyond 20". Two changes in the sign of the h_3_ term are observed: at 5" and
again at 10". A disk of rapidly rotating gas is present within the inner 3"
which is decoupled from the stellar component.
NGC 4350 is a member of the edge-on subsample. The surface brightness profiles
of this galaxy are well separable into r^1/4^-law and exponential disk
components. Following the region of constant Mg_2_ strength with radius
(for 10" < r < 30"), the major-axis Mg_2_ profile shows an abrupt decline in
strength with radius. The minor-axis Mg_2_ gradient is the steepest in our
entire galaxy sample. Weak [O III] 5007 A emission is present in the inner
regions (r = +/- 5") of our major-axis spectrum. The line strength profiles
along the major and minor axis of NGC 4350 differ dramatically and indicate a
convincing separation into bulge and disk components (see Figs. 4, 5). Michard
& Marchal (1993) described NGC 4350 as having a disk fully embedded in a
April 29/30, 1979
NGC 4350 forms a pair with NGC 4340
(RSB0_2_; panels 57, S7) at 5.6' projected separation.
The redshifts are similar enough, at
v_o(4340) = 775 km/s and v_o(4350) = 1085 km/s,
to suggest a physical pair. The mean redshift
Mpc, which gives the small projected linear
separation of 31 kpc.
NGC 4350 has a central bulge of high surface
brightness and a well-developed disk, which
although not as discrete as in NGC 3115 (panel
50), is more definite than simply the flattened
ellipsoid seen in E6 galaxies. The presence of the
disk, presumed to be the same as the extended
outer envelope seen in more-face-on S0's, is the
classification discriminant between highly
flattened E and highly flattened S0 types.
NGC 4350: This is the prototype of our "E - like S0's" (see-data in
Paper I and in MS93).
NGC 4350; S0.
This normal early-type (S0) galaxy has a UV spectrum consistent with its
Hubble type, as described in Section 1. NGC 4350 belongs to the Virgo
= Holm 391a
Non-interacting pair with NGC 4340 at 5.6 arcmin
(= NGC 4350)
Radial velocity = +1,122 km/sec
in the Virgo Cluster [HMS 1956].
Component of the binary system Holmberg 391.
SA0 (de Vaucouleurs)
See UGC 07467
= Holm 391a
Very small, very bright nucleus. Bright lens: 1.0 arcmin x 0.25 arcmin.
Non-interacting pair with NGC 4340 at 5.6 arcmin.
Ap. J., 132, 306, 1960.
A spindle 2' x 0.4' in p.a. 30^deg^; very bright; no spiral structure
discernible. 28 s.n.