Date and Time of the Query: 2018-12-12 T21:46:51 PST
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Notes for object NGC 4654

10 note(s) found in NED.

1. 2006MNRAS.366..812C
Re:NGC 4654
The stellar and gaseous morphologies are very asymmetric. The H{alpha} velocity
field is strongly perturbed. Alternating patterns of (decreasing and increasing)
solid body and constant velocity are observed through the field, which is well
illustrated by the PV diagram. In the approaching half, the transition region
between the central solid-body part and the outer decrease occurring at an
offset of ~1 arcmin leaves a remarkable imprint in the velocity field. In
addition, streaming motions are evidenced along the spiral arms. A solid-body
rotation is partly associated with the very thin and elongated H{alpha} bar-like
structure in the central parts. According to Vollmer (2003), a scenario mixing
effects of a tidal interaction with NGC 4639 ~500 Myr ago and RPS could be
responsible for the perturbed stellar and gaseous distributions of NGC 4654.
There is a large difference of distance between the two galaxies, ~22 and ~25
Mpc for NGC 4639 as estimated from the Tully-Fisher relation (Yasuda et al.
1997) and the Cepheids method (Saha et al. 1997), respectively, and ~14 Mpc for
NGC 4654 (Tully-Fisher relation, Yasuda et al. 1997). This inconsistency of
distance points out that the Tully-Fisher distance of NGC 4654 must be highly
erroneous if the Vollmer's scenario is valid.

2. 2003PASJ...55...59S
Re:NGC 4654
4.11 NGC 4654 CO distribution is highly distorted and lopsided. The PVD
shows rigid-body ridge, and the RC is also gradually rising at
r < 2kpc. Accordingly, the SMD comprises only disk and bulge components
with slight enhancement due to a possible core component near the

3. 2003PASJ...55...17S
Re:NGC 4654
6.14 NGC 4654 This galaxy is known for its lopsided structure in the
optical as well as HI disks, most likely due to the rampressure effect of
the intracluster gas, blowing from the northwest (Phookun and Mundy
1995). The CO distribution is also lopsided, in the same direction as
that of the HI and optical image tail. The lopsided CO distribution
suggests that the ram pressure effect is not negligible even in such a
central molecular disk. Moreover, the CO distribution is more elongated
than the optical/HI disks. The velocity structure is rigid body-like
with mildly increasing rotation velocity with the radius. Such rotation
characteristics is exceptional among the presently observed PVDs.

4. 2002ApJS..143...73E
Re:NGC 4654
NGC 4654.---SBcd: No real bulge. Nucleus is threaded by a short, thin,
HSB bar. Two prominent spiral arms emanate from the ends of the bar.
The arm emanating from the SE end of the bar and wrapping around the
north side of the disk is the more prominent. It is rich in
star-forming knots for the first ~180deg and becomes smooth and
diffuse thereafter. It can be traced for nearly a full 360deg. The
inner part of the NW arm is also rich in star-forming knots but
becomes broad and diffuse after ~150deg. It can be traced only ~270deg
before fading from view.

5. 1994CAG1..B...0000S
Re:NGC 4654
VCC 1987
March 28/29, 1982
50 min
NGC 4654 is among the 15 largest spirals
considered to be members of the Virgo Cluster.
Its isophotal diameter is large at D_25_ = 4.7'. A
comparison of its angular size with other large
spirals in the cluster can be seen in the atlas of
Virgo Cluster spirals (Sandage, Binggeli, and
Tammann 1985a, panel 6).
As with the other large spirals in the cluster,
NGC 4654 is in the outskirts of the cluster, away
from either subcluster A or B (compare Binggeli,
Tammann, and Sandage 1987). It is located 3.3^deg^
east (and slightly north) of NGC 4486, which is
associated with Virgo subcluster A.
HII regions are present in the bar. The
nucleus is brilliant and starlike at the 1" level.
The brightest HII regions in the arms are abundant
and have a heterochromatic blue magnitude
of about B = 20. The galaxy is a good candidate
for resolution into individual stars using a
high-resolution telescope.
The redshift is v_o = 926 km/s but, being in
the Virgo Cluster, this is as much a virial velocity
as a distance indicator.

6. 1993A&AS...97..887B
Re:NGC 4654
NGC 4654 was detected by KY at about the same intensity as NGC 4651. Our
observations, however, show clear, strong CO(1-0) lines out to 60" from
the center and these spectra are nearly an order of magnitude stronger
than the NGC 4651 spectra making the IRAM and FCRAO spectra incompatible.

7. 1976RC2...C...0000d
Re:NGC 4654
= IC 3708
Photometry (10 microns):
Ap. J. (Letters), 176, L95, 1972.
Ap. J. Suppl., 26, No. 230, 1973.

8. 1973UGC...C...0000N
Re:UGC 07902
SAB(rs)cd (de Vaucouleurs), Sc- (Holmberg)

9. 1964RC1...C...0000d
Re:NGC 4654
= IC 3708
Short, knotty bar: 0.35 arcmin x 0.08 arcmin. Pseudo (r?): 1.1 arcmin x
0.5 arcmin. Several partially resolved filamentary, branching arms with many
dark lanes. Slightly asymmetric.
Lick 13 and Uppsala 21 dimensions are for the bright part only.

10. 1918PLicO..13....9C
Re:NGC 4654
A very faint, somewhat irregular spiral 3' x 1.2' in p.a. 125^deg^ Faint,. small
nucleus. Most of the matter is in -one whorl.

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