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Date and Time of the Query: 2019-05-21 T03:47:47 PDT
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Notes for object NGC 4371

9 note(s) found in NED.


1. 2012ApJ...754...67F
Re:NGC 4371
NGC 4371 .LBR+..-Strongly barred galaxy. Erwin & Sparke (1999) find a bright
stellar ring that is notable by adjusting the contrast of the HST F606W image
carefully or through unsharp masking. While free of obvious dust or spiral
structures the ring with a radius of about 5" falls within the bulge radius
which lets Fisher & Drory (2010) classify this as a pseudobulge. The major axis
rotational velocity starts to flatten out at a radius of 8"-well inside the
bulge radius or 22.9"-with a weak shelf around 3-8". The velocity dispersion
rises from about 105 km s^-1^ at the bulge radius to about 130 km s^-1^ at 7".
Inside of 7" the velocity dispersion stays relatively constant. The h_3_ moments
are somewhat asymmetric but generally anti-correlated with velocity within the
bulge. The h_4_ moments are compatible with zero in the center but rise
gradually to values of about 0.05 at 10". The minor axis velocity dispersion
stays mostly constant within the covered radial range. The minor axis h_3_
moments remain com patible with zero while the h_4_ moments rise from zero at
the center to values of about 0.05 at +/-9".

2. 2006ApJS..164..334F
Re:VCC 0759
VCC 759 (NGC 4371).This galaxy has a small dust disk at the center, only about
1.6" across. The disk is inclined by about 26^deg^ to the line of sight, and its
major axis seems to coincide with the major axis of the galaxy (which is aligned
in the east-west direction). The structure beyond is not easily interpretable.
There seems to be a thin (less than 1" across) blue nuclear stellar ring
centered on the galaxy's center, with a radius just below 11". The inclination
and orientation of the stellar ring are the same as those of the nuclear dust
disk. Within this ring, there seems to be at least one additional blue arc. Just
beyond the stellar ring, there seems to be a second, this time redder, stellar
ring, about 6" across. Farther out, at a distance of about 34", a ring
rests at the end of a kpc-scale bar. The presence of the rings makes the A4 and
B4 coefficients nonzero. The position angle, ellipticity and the surface
brightness profile are also irregular. There does not appear to be a stellar
nucleus, although the presence of the dust makes this statement hard to
quantify.

3. 2005MNRAS.364..283E
Re:NGC 4371
NGC 4371. Bar measurements are from WIYN R-band images measurements, but the
outer-disc inclination and scalelength are from deeper INT-WFC r-band images
(Erwin et al., in preparation).

4. 2004A&A...415..941E
Re:NGC 4371
NGC 4371: Wozniak et al. (1995) suggested this galaxy might be triply barred (it
is listed as such by Moiseev 2001), but pointed out that high inclination and
alignment of inner two "bars" with outer disk could mean that they were
projected axisymmetric structures; Kormendy (1979) noted a possible secondary
bar in this galaxy, which corresponds to the middle of W95's three ellipticity
peaks. Erwin & Sparke (1999) showed that the middle ellipticity peak was due to
a bright, stellar ring; the apparent inner peak was produced by the effects of
superimposing a ring on a rounder bulge profile, accompanied by circularizing of
the inner isophotes by seeing (see Fig. 5 and Erwin et al. 2001).

5. 1997A&AS..124...61B
Re:NGC 4371
This galaxy has been classified SB0(r)+ by RC3 and SB0_2/3_(r)3 by RSA. The bar
is clearly visible along the apparent minor axis of the disk. It has been
studied also by Kormendy (1982a) by means of a spectrum at PA=90^deg^ (5^deg^
from major axis). He found a central velocity dispersion {sigma}=106 km s^-1^
and a maximum of rotation of 125 km s^-1^. From our data, taken at PA=95^deg^,
we measure a higher rotational velocity V_max_~190 km s^-1^ and also a slightly
higher velocity dispersion {sigma}=139+/-2 km s^-1^.

6. 1994CAG1..B...0000S
Re:NGC 4371
VCC 759
SB0_2/3_(r)(3)
CD-1318-S/Br
March 12/13, 1980
103aO
75 min
The two regions of enhanced luminosity in
NGC 4371 at the end of the bar at the rim of the
inner disk are well shown in this negative print.
As in NGC 3892 to the lower left and NGC 4340
below, this luminosity enhancement of the rim
can be traced for about 5 deg on either side of each
termination of the bar.

7. 1976RC2...C...0000d
Re:NGC 4371
Photometry:
Astrofizika, 2, 53, 1966.
Isodensitometry:
Ap. J. Suppl., 26, No. 230, 1973.

8. 1973UGC...C...0000N
Re:UGC 07493
SB(r)0+ (de Vaucouleurs), S0 (Holmberg)

9. 1964RC1...C...0000d
Re:NGC 4371
Very bright nucleus: 0.6 arcmin x 0.3 arcmin on a smooth bar: 1.1 arcmin x
0.4 arcmin. Weak (r): 1.9 arcmin x 1.1 arcmin., stronger near the
extremities of the bar.


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