Date and Time of the Query: 2019-05-23 T09:48:14 PDT
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Notes for object NGC 4365

16 note(s) found in NED.

1. 2006ApJS..164..334F
Re:VCC 0731
VCC 731 (NGC 4365).The galaxy is a member of the W-cloud, at a distance of ~23
Mpc (S. Mei et al. 2006, in preparation). A resolved, slightly elongated nucleus
is clearly visible in the color image, as well as in the individual frames. The
nucleus is bluer than the surrounding galaxy and clearly affects the surface
brightness profiles, in particular in the g band. The isophotes appear quite

2. 2006ApJ...639..136H
Re:NGC 4365
NGC 4365. We extracted a spectrum from a 2' (11 kpc) aperture. We found
that two hot gas components (0.36 and 0.93 keV) were required by the data,
and the resulting Z_Fe_ was poorly constrained. Sivakoff et al. (2003)
reported similarly poorly constrained abundances for a similar region,
using Chandra data. These authors also report some evidence of an
abundance gradient. However, given the challenges of background
subtraction in such a low surface brightness regime and the few available
photons, we did not find compelling evidence.

3. 2006ApJ...639...95P
Re:VCC 0731
VCC 731.Appears to have significantly more GCs than other galaxies of comparable
luminosity. The excess appears to be due to an large number of red GCs.

4. 2001AJ....121.2974L
Re:NGC 4365
NGC 4365: Probably located slightly behind the Virgo Cluster, this large
elliptical galaxy contains a kinematically distinct core (Bender 1988),
which may indicate a past merger event. The first HST study was that of
Forbes et al. (1996). From a short-exposure central pointing they detected
328 GCs but no obvious bimodality. Here we use longer exposure images of
the galaxy center and a region directly to the north. We find a broad color
distribution for 323 clusters brighter than V = 24, although most GCs seem
to belong to a peak with the same color as the blue population in most
large elliptical galaxies.

5. 1997ApJ...481..710C
Re:NGC 4365
The nucleus of this galaxy is very diffuse, i.e., the surface
brightness profile increases toward the center with a shallow slope.
However, it shows a weak (bumplike) excess of brightness in the very
center (V ~ 23, M_V_ ~ -7) which might be unresolved. Visual inspection
of the V image confirms the rounding of the isophotes in the very center
(r <= 0.3") shown by the ellipticity profile in this passband. The I
image shows a weak disklike feature, which explains the larger
ellipticity of the I profile at those radii. A ~40^deg^ isophote twist is
also observed there. In our V - I color map, this central tilted
structure has a radius of about 0.14" and is bluer by about 0.05 mag than
the surrounding regions. It seems unlikely that this feature is an
artifact of an imperfect matching of the V and I PSFs, since its size is
a factor of 4 larger than the FWHM of both Tinytim PSFs. At larger radii,
a stellar disk (not seen by van den Bosch et al. 1994, but detected by
Forbes 1994) is clearly visible between 1" and 3". At these radii, the
ellipticity and the C_4_ show the typical bump, where C_4_ reaches 0.01.
There is a hint that this disk is slightly redder than the outer

6. 1997A&A...321..765B
Re:NGC 4365
3.2. NGC 4365
The ^12^CO(2-1) emission in NGC 4365 nearly reaches the 3{sigma} level but was
clearly not detected in CO(1-0) (see Table 2). The ^12^CO(2-1) "line" is not at
the optical velocity of 1227 km s^-1^ but at v~1115 km s^-1^. NGC 4365 was not
detected in HI. We do not consider this to he a CO detection.

7. 1995AJ....109.1988F
Re:NGC 4365
NGC 4365: This Virgo galaxy reveals a complex kinematic structure with
a counter-rotating core (Bender 1988; Surma 1992) There is evidence for a
small-scale disk from both spectroscopic line analysis (Surma 1992) and
PC imaging (Forbes 1994; see also Jaffe et al 1994). This disk can be
seen as a positive fourth cosine term in Fig.3 between 1" and 3",
Compared to the other galaxies described here, it is interesting that
NGC 4365 shows no evidence for dust and has a remarkably flat core
({alpha} = -0.17) for a relatively faint galaxy (M_B_ = 20.88).

8. 1994CAG1..B...0000S
Re:NGC 4365
VCC 731
March 8/9, 1953
103aD + GG11
30 min
NGC 4365, a bright member of the Virgo Cluster near subcluster B,
is also shown on panel 7. Although the globular cluster population is
high, as seen in the print here, the specific frequency (the number
per unit M_B_ = -15 luminosity) is not as high as in M87 (Harris

9. 1994CAG1..B...0000S
Re:NGC 4365
VCC 731
Feb 23/24, 1979
103aO + Wr2c
55 min
NGC 4365, one of the brighter members of the Virgo Cluster, is
associated with the Virgo subcluster B centered on NGC 4472. The blue
magnitude of NGC 4365 is B_T_ = 10.6, which is 1.3 mag fainter than
B_T_ = 9.3 of NGC 4472, the brightest galaxy in the cluster (Binggeli,
Sandage, and Tammann 1985).
Globular clusters are evident, the few brightest of which are at
the same apparent magnitude as the brightest globular clusters in NGC
4486 (panel 17), although bright clusters are much fewer in NGC 4365
than in NGC 4486.

10. 1994AJ....108.1579v
Re:NGC 4365
NGC 4365 is a radio quiet giant elliptical. Surma (1993) found clear
evidence for two kinematically distinct components within this object: a
hot "bulge"-like component plus a cold "disk-like subsystem. Surma finds
the cos 4{theta} term to become positive ("disky") inside ~4", consistent
with our results. However, the isophotes become boxy again at a < 1.2",
where Surma's data is unreliable. The ellipticity and position angle
remain rather constant over the entire radial range, while the isophotes
are almost perfectly elliptical (except for the small positive
cos 4{theta}-bump around 2"-3"). While we found no dust by visual
inspection, this galaxy is a far-infrared emitter (cf. Paper 1) and a
small amount of dust may influence the 3{theta} and 4{theta} components at
small radii. Additionally the bumpy profiles might also originate from
weak H{alpha},+[N II] emission detected by Kennicut & Kent (1983). We
therefore argue that there is no conclusive photometric dependence for a
decoupled core.

11. 1994A&AS..106..199C
Re:NGC 4365
NGC 4365. This galaxy is surrounded by a luminous X-ray halo (Forman et
al. 1985), and shows peculiar core kinematic and Mg_2_ increasing inwards
in the center (Bender & Surma 1992).

12. 1994A&AS..105..481M
Re:NGC 4365
NGC 4365: This giant boE develops a somewhat asymmetric and elongated
envelope, well above the r^1/4^ law.

13. 1994A&AS..104..179G
Re:NGC 4365
Boxy isophotes. Detected by IRAS at 100 microns. X-ray source.

14. 1976RC2...C...0000d
Re:NGC 4365
Non-interacting pair with NGC 4370 at 10 arcmin
Dynamics and Mass Determination:
Ap. J., 139, 284, 1964.

15. 1973UGC...C...0000N
Re:UGC 07488
E3 (de Vaucouleurs)

16. 1964RC1...C...0000d
Re:NGC 4365
Very bright center. Smooth nebulosity. Many globular clusters.
Non-interacting pair with NGC 4370 at 10 arcmin.
A.J., 132, 306, 1960.
A.J., 61, 97, 1956.
Zwicky, F., Morphological Astronomy, p.154, 1957.

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