VCC 1250 (NGC 4476).This galaxy harbors a nuclear, clumpy, dust disk, about 11"
in radius. The clumps are clearly organized in a spiral structure. The plane of
the disk is inclined by about 20^deg^ to the line of sight; the north-west side
of the disk is the closest. This disk is similar but clumpier and smaller than
the ones seen VCC 1154 or VCC 1532. The correction for dust performs better than
in the case of VCC 1154 or VCC 1532, indicating that the change in the stellar
population embedded in the disk (relative to the one surrounding it), is not as
extreme as in those galaxies. Several blue clumps, organized in an almost
complete arc structure, are however clearly visible within the disk, and the
isophotal parameter within the inner 10" should be interpreted with caution.
There is clear indication of the presence of a nucleus from both the individual
and the color image, and from the surface brightness profiles. The color of the
nucleus cannot be assessed because of the presence of dust. The nucleus appears
to be offset by just over 1" in the north direction relative to the center of
the dust disk (the disk's major axis is aligned in the north-northeast
direction). The isophotal center is not very stable even in the outer regions,
varying by as much as 0.1" between subsequent isophotes; but it does seem to be
consistent with the location of the nucleus. The isophotes seem quite regular,
at least in the outer region.
NGC 4476. - This early-type galaxy (type SA0-), a member of the Virgo
cluster, is located in the UIT frame centered on NGC 4472. It is detected
only in the MUV image (Fig. 23b).
NGC 4476. This galaxy is one of the low luminosity companions of M 87. It
is situated at a projected distance of 12' (5.2 kpc) from M 87 and 5'
(2.2 kpc) from its nearest neighbour. The luminosity profile of NGC 4476
follows an r ^1/4^ law, with no signs of disturbances from a
gravitational interaction, except for a possible trend of increasingly
circular isophotes with increasing radius (Prugniel et al. 1987). The
stellar kinematics are normal for an elliptical galaxy, with a central
velocity dispersion of 132 km s^-1^. Dust is clearly seen on optical
photographs, showing the presence of a nuclear dust-ring. No atomic gas
has been detected. A good upper limit has been presented by Giovardini et
al. (1983). We detect CO emission in both the J = 1-0 and J = 2-1 lines,
corresponding to an H_2_ mass of ~8 x 10^7^ M_sun_. Our signal-to-noise
is not very good, but since this galaxy has been seen in the CO(J = 2-1)
line by Lees et al. (1991), we consider this as a definite detection.
E5 pec(dust); S0_3_(5)
Feb 3/4, 1979
103aO + Wr2c
NGC 4476 is classed as E5 pec(dust) in both editions of the
RSA. It is classed as S0_3_(5) in the Virgo Cluster Catalog based on
the Las Campanas plate used here, and is also classed S0 in the RC2
based on a Palomar 200-inch plate, in both cases because of the
presence of an extended envelope.
The S0_3_ subclassification is due to the presence of an internal
dust lane buried in the central image, invisible in the overexposed
print here. The dust lane is seen in the insert print in the middle
bottom illustration of panel 12.
Feb 3/4, 1979
103aO + Wr2c
The prints of NGC 4476 shown here on the facing page are from the
same plate used for the image of this galaxy at panel 11. The insert
print here shows the S0_3_-like dust ring buried in the central
NGC 4476 is the second low luminosity companion of M87. Its lies 12'
(projected) from M87 and 5' from NGC 4478 (see above). NGC 4476 is
classified SA(r)0 in the RC2, and E5pec(dust) in the RSA. This difference
arises from the presence of a dust ring in the central (a <~ 7") region,
clearly visible in the HST image in Paper I. The ring disturbs the
isophotal parameters inward of 7". Outside the ring we find a rather
constant position angle of ~25^deg^, consistent with previous studies
(Michard 1985; Prugniel et al. 1987; Caon et al. 1990), which all show
that the position angle remains nearly constant out to ~100".
NGC 4476: Only photographic data are available. The choice between the
diE and SA0 types is uncertain: the second one was adopted as in the RC2.
Non-interacting pair with NGC 4478 at 4.5 arcmin
Ap. J., 146, 28, 1966.
Paired with UGC 07645 at 4.6, 105
SA(r)0-: (de Vaucouleurs)
Very bright nucleus with a narrow, dark crescent?
Non-interacting pair with NGC 4478 at 4.5 arcmin.
Uppsala 21 and Heidelberg Veroff. Vol. 9, 1926 dimensions are for the bright
Slightly oval, 0.5' long; quite bright at center; no structure discernible.