Date and Time of the Query: 2019-04-25 T15:56:42 PDT
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Notes for object NGC 4478

10 note(s) found in NED.

1. 2006ApJS..164..334F
Re:VCC 1279
VCC 1279 (NGC 4478).This galaxy is generally well behaved on large scales. There
is no hint of the existence of a large-scale disk, but the isophotes become more
elongated in the very innermost region. The color image betrays the existence of
a small (less than 1" in radius) blue stellar disk, which is seen almost edge-on
and oriented along the major axis of the galaxy. The presence of a disk is also
reflected in the B4 coefficient. From the surface brightness profile, it is
possible that a compact nucleus exists, affecting the profile within the inner
1" or so, although the feature seen could also be attributable to the disk.

2. 2001MNRAS.326..473H
Re:NGC 4478
A11 NGC 4478
NGC 4478 is a member of the Virgo cluster. While classified as E2 in both
RC3 and RSA, this elliptical is classified as a compact elliptical by
Prugniel, Nieto & Simien (1987). They argue that NGC4478 had been tidally
truncated by its nearby neighbour M87. NGC 4478 has been studied with HST
by vdB94. In Fig. A11 we show their measurements along the major axis of
{epsilon}, PA and a_4_ (kindly supplied by F. C. van den Bosch). Also
shown are the measurements of {epsilon} and PA taken from P90.
In Fig. A12, measurements of rotation, {sigma}, h_3_ and h_4_ for
|r| < 10 arcsec provide strong indications of a central component,
decoupled from the surrounding galaxy. Measurements of {sigma} and h_4_
for this range of radii are asymmetric, and rotation and h_3_ are not
point-symmetric about the galaxy centre, most notably along the major axis.
This could be the result of considerable isophote twisting measured by
vdB94 for |r| < 5 arcsec, such that the measured PA deviated by up to
10^deg^ from that of our major axis observation (i.e. PA 145^deg^)
(see Fig. A11). Observations obtained for the photometric axes of the main
galaxy therefore may not coincide with the similar axes of a distinct
component. A central decrease in is measured for both, minor and major
axes. For the major axis, a significantly non-zero value of h_3_ is
measured for |r| < 5 arcsec, and h_4_ is positive for 0 <~ r <~ 3 arcsec.
For the minor axis, h_3_ is slightly non-zero for |r| < 2 arcsec, and h_4_
becomes slightly negative outside r = 3 arcsec.
Two additional interesting features of the photometry of vdB94
(Fig. A11) are the significant measurement of disciness for the inner
2 arcsec and the sharp increase in ellipticity for |r| <~ 1.5 arcsec.
These two results offer strong support to the idea that a disc component
resides at the galaxy centre. From the study of residual maps of their
photometry, vdB94 were unable, however, to state conclusively that such a
component was observed.
The asymmetric LOSVDs along the major axis (i.e. non-zero measurement
of h_3_), together with the positive measurement of h_4_ for both axes
close to the galaxy centre, are consistent with the detection of a separate
kinematical component with orbital motion across the line of sight. The
central dip in {sigma}, for similar radii, suggests that this component is
more rotationally supported than the surrounding bulge component. Taken
together these results may be consistent with the detection of a central
disc population.
The kinematics of this galaxy are clearly complex. Two-dimensional maps
of the velocity field, available using integral field unit spectroscopy
would greatly enhance the study of its dynamics.

3. 2001ApJS..132..129M
Re:NGC 4478
NGC 4478. - This elliptical, a member of the Virgo cluster and located
in the UIT frame centered on NGC 4472, is faintly detected in the MUV
(Fig. 23b) as a point source. Due to a large number of point source-like
artifacts in this image (for example, note the bright source to the east),
caution should be exercised in using this detection or associated

4. 1994CAG1..B...0000S
Re:NGC 4478
VCC 1279
Feb 3/4, 1979
103aO + Wr2c
60 min
NGC 4478 in the Virgo Cluster is the nearest bright galaxy to NGC
4486 (M87), which is the dominant galaxy in Virgo subcluster A
(Binggeli, Tammann, and Sandage 1987). It is a moderately compact E2
galaxy, 2.5 mag fainter than M87.

5. 1994AJ....108.1579v
Re:NGC 4478
This galaxy is, like NGC 4476, a companion of M87; its projected
separation from M87 is 8.5". It is classified E2 in both RC2 and RSA. The
lack of extended envelope indicates that NGC 4478 might be tidally
truncated by M87. Prugniel et al. (1987) therefore classify NGC 4478 as a
compact elliptical (cE). Previous studies on the photometry of NGC 4478
(Michard 1985; Prugniel et al. 1987; Bender et al. 1988; Peletier et al.
1990; Nieto et al. 1991a) all show a large isophote twist of ~30^deg^
between 30" and 60" (in agreement with what one might expect to find in
the outer regions of a tidally truncated galaxy) plus a slow, constant
change of position angle going inwards from 30". We find that this change
of position angle continues down to 0.5". Outside 6" the isophotes are
slightly boxy, consistent with previous studies. Inside ~1.5" we find a
strong increase in ellipticity and diskiness with a negative cos 3
{theta} term. The residual map [Fig. 7(b)] reveals a spot with slightly
enhanced surface brightness at 1.8" (~130 pc) from the center plus a
string-like feature at the other side of the nucleus. This feature might
represent ionized gas (none detected by Roberts et at 1991), or a bright
nuclear disk seen at an intermediate inclination angle. High resolution
images in other colors and kinematic data are necessary to study this
"photometrically distinct nucleus" in more detail.

6. 1994A&AS..105..481M
Re:NGC 4478
NGC 4478: This is another example of a boE "satellite" of a massive
galaxy (see NB89). The light profile deviates from the r^1/4^ law as is
often the case for these minor objects. Farther than l = 30 arcsec,
appears an envelope of low SuBr strongly twisted from the main body, with
perhaps some evidence of a spiral pattern. NGC 4478 might well be a two-
component object with a significant disk.

7. 1976RC2...C...0000d
Re:NGC 4478
Non-interacting pair with NGC 4476 at 4.5 arcmin
Astrofizika, 1, 38, 1965.
Photometry (10 Color):
Ap. J., 179, 731, 1973.

8. 1973UGC...C...0000N
Re:UGC 07645
E2 (de Vaucouleurs)
See UGC 07637
UGC 07654 at 8.6, 65

9. 1964RC1...C...0000d
Re:NGC 4478
Extremely bright center. Smooth nebulosity with a steep gradient.
Non-interacting pair with NGC 4476 at 4.5 arcmin.
Lick 13 and Heidelberg Veroff. Vol. 9, 1926 dimensions are for the bright
part only.

10. 1918PLicO..13....9C
Re:NGC 4478
Nearly round; 0.5' in diameter; bright, almost stellar nucleus. A star of magn.
15 is distant 11" in p.a. 352^deg^. Structureless.

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