Date and Time of the Query: 2018-11-15 T15:01:01 PST
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Notes for object NGC 4435

12 note(s) found in NED.

1. 2006ApJS..164..334F
Re:VCC 1030
VCC 1030 (NGC 4435).There is a small dust disk, about 8" across, centered
on the galaxy's center. The disk is inclined ~16^deg^ to the line of sight.
Although similar, this disk is smaller and less structured than those in VCC
1154 and VCC 1532. Several regions within the disk are quite blue, probably due
to star formation. This prevents an accurate dust correction, and the isophotes
are not recovered within the inner 2". Because of the dust, it is also
impossible to assess the presence of a nucleus. The isophotes are visibly boxy
in the inner ~10", switching to disky further out.

2. 2006A&A...453...27C
Re:UGC 07575
UGC 7575: Machacek et al. (2004) analysed the total emission from the galaxy
(within 32" of the nucleus). The data were described by a
thermal MEKAL plasma plus a power-law component. Fixing the absorbing column at
the Galactic value (2.64 x 10^22^ cm^-2^) and the MEKAL model abundance
at 0.1 Z_{odot}_, the data are well fitted with a photon index {GAMMA = 1.22.

3. 2005MNRAS.364..283E
Re:NGC 4435
NGC 4435. Bcause this galaxy is apparently interacting with its neighbour NGC
4438 and possibly edge-on as well (e.g. Kenney et al. 1995), I excluded it from
the sample.

4. 2005A&A...440...73C
Re:UGC 07575
UGC 7575: the situation for this object is similar to that of UGC 7614, with a
large scale disk but little dust in the innermost 1", leading to a clear
power-law classification.

5. 2002ApJS..142..223F
Re:NGC 4435
NGC 4435. NVSS did not detect this source, while FIRST shows a 2.2 mJy
detection. 5 GHz, 5" resolution observations (Wrobel & Heeschen 1991)
detect a weak 1.2 mJy source. However, the 15 GHz, 0.2" resolution
observations of Nagar et al. (2000) give an upper limit of 1.1 mJy to
any small-scale radio emission.

6. 1994CAG1..B...0000S
Re:NGC 4435
VCC 1030
Feb 3/4, 1979
103aO + Wr2c
60 min
NGC 4435 forms an optical pair with NGC
4438 (Sb tides; shown below and on panel 153)
near the center of Virgo Cluster subcluster A
associated with NGC 4486.
The central bulge in NGC 4435 has an
elongated image whose major axis makes an angle
of about 70 deg to the major axis of the disk, as
shown in the insert. The difference in the tilt of
the isophotes of the bulge and the extended outer
envelope is the classification criterion for the SB

7. 1994CAG1..B...0000S
Re:NGC 4435
Pair [with NGC 4438]
Feb 3/4, 1979
103aO + Wr2c
60 min
NGC 4438 has a set of smooth luminous
plumes that may or may not define a highly
distorted plane. If so, the plane is disturbed and
the type is Sb(tides) from the existence of a plane
and the large central bulge. The presence of the
dust patches asymmetrically placed across the
image suggests that a plane exists and that the
form is not simply a bulge with tidal plumes.
Tidal distortion (Toomre and Toomre 1972)
caused by a close encounter is suggested by the
morphology. The obvious candidate for the
perturber is NGC 4435 [SB0(7)] at a separation of
only 4.3', also seen on the print here. However,
two points militate against a tidal perturbation:
(1) NGC 4435 shows no evidence of tidal effects,
and (2) the redshifts of the two galaxies are
widely different. The redshifts are v_o(4435) =
753 km/s and v_o(4438) = -115 km/s. An
encounter velocity as high as 868 km/s may not
produce strong tidal effects because the event is
too rapid.
The second-closest large galaxy to this pair
is NGC 4406 (S0/E3; panel 27), at a separation
of 18', whose redshift is v_o = 367 km/s. Its
morphology is as undisturbed as that of NGC 4435.
A possible explanation of the morphology of
NGC 4438 is that a merger is in progress having
nothing to do with NGC 4435, and that the
merged parents are not individually visible now.
Very short exposures of NGC 4438 show no sign
of two components; only a single nucleus exists at
the center of the bulge.
A prototype dE,N nucleated dwarf elliptical
is to the right of the major axis of NGC 4438 in
the print here, very close to the bulge. It is not
listed in the VCC probably because of its close
proximity to the main body of NGC 4438 where
it evidently was missed in the Virgo Cluster
Survey (Binggeli, Sandage, and Tammann 1985).

8. 1994A&AS..105..481M
Re:NGC 4435
NGC 4435: This object is presented in Fig. 4 as an example of an S0
with an embedded disk in a spheroidal halo. It is classified SB0 in both
the RC2 and RSA. There is indeed an inner boxy feature twisted by 9^deg^.
Here the type SAB0 has been adopted.

9. 1993A&AS...97..887B
Re:NGC 4435
NGC 4435/4438 are separated by about 5' (13 kpc). NGC 4438 has strong CO
emission (Combes et al. 1988) but we did not detect NGC 4435 in CO.

10. 1976RC2...C...0000d
Re:NGC 4435
= Arp 120
= VV 188
= Holm 409b.
Interacting pair with NGC 4438 at 4.3 arcmin
A.J., 79, 671, 1974.
Astrofizika, 1, 38, 1965.
Ap. J., 146, 28, 1966.
Bol. A. A. Argentina, No. 16, 17, 1971.
Ap. J. Suppl., 26, No. 230, 1973.
A.J., 79, 671, 1974.
Observatory, 88, 239, 1968.

11. 1973UGC...C...0000N
Re:UGC 07575
VV 188 (b), Arp 120 b
SB(s)0/a (de Vaucouleurs), S0 (Holmberg)
See UGC 07574, UGC 07494

12. 1964RC1...C...0000d
Re:NGC 4435
= Holm 409b
Very bright nucleus in a bright bar with a spherical envelope.
Interacting pair with NGC 4438 at 4.3 arcmin.
Ap. J., 138, 876, 1963.

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