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Date and Time of the Query: 2019-08-25 T16:21:14 PDT
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Notes for object NGC 5371

13 note(s) found in NED.


1. 2005MNRAS.360.1201H
Re:NGC 5371
NGC 5371. In this galaxy, there is no evidence of H{alpha} emission in the
centre.

2. 2002ApJS..143...73E
Re:NGC 5371
NGC 5371.---SBbc: Nuclear point source embedded in an elliptical
bulge. Bulge is threaded by a prominent bar with a P.A. skewed ~45deg
from that of the bulge. On the west side of the bar, a doubled arm
emerges offset behind the end of the bar. The outer part of the
doubled arm can be traced through ~400deg before it fades into the
sky. After ~270deg it becomes smooth and LSB. On the east end of the
bar a single arm emerges from the bar end, with no offset. The arm can
be traced through ~90deg before it merges with the inner part of the
doubled west arm. The merged feature can be traced through another
~300deg after this. For the last ~120deg, it is smooth and LSB. The
disk is full of knots, with the brightest knots in the arms. There are
clear dust lanes especially on the southern side of the disk.

3. 2002AJ....124..675C
Re:UGC 08846
Extended, asymmetric radio source. F13535+4042 is the identification,
despite the large optical/FSC offset.

4. 2002A&A...389...68G
Re:NGC 5371
NGC 5371: the galaxy was too big to fit in the CCD frame
used by Gonzalez-Delgado et al. (1997), so that, the PA values
found using this catalog can not be very reliable. We thus
adopt for this galaxy an average of the photometric values.

5. 2001A&A...378..370V
Re:NGC 5371
NGC 5371: this SAB(rs)bc with a LINER spectrum, was mapped in H I at
Westerbork (Wevers et al. 1986). Its optical luminosity profile shows a
sharp edge at a radius of about 100", beyond which the surface brightness
drops rapidly and the disk becomes redder. Its H I distribution is
ring-shaped with a maximum surface density of 80" radius, and having an
outer edge coinciding with the optical edge. Its velocity field shows
signs of a mild warp, and a flat rotation curve was derived from it with
a V_rot,max_ of 300 km s^-1^.

6. 2001A&A...368...16M
Re:NGC 5371
40. NGC 5371 is an Sb/SBb spiral of low inclination. The faint bar (e.g.
Martin 1995) is no problem for our fit (Fig. 6 in on-line version).

7. 1999A&A...349...88K
Re:NGC 5371
4.7. NGC 5371
The galaxy was classified as a LINER by Rush et al. (1993).
Elfhag et al. (1996) presented CO measurements and suggested NGC 5371
to be a good candidate for a post-starburst galaxy (Koorneef 1993). The
rotation curve was measured by, e.g., Zasov & Sil'chenko (1987).
Gonzalez Delgado et al. (1997) studied the HII region population.
The X-ray lightcurve does not show short-timescale variability (the
countrate in individual bins falls slightly outside the 1{sigma} error,
occasionally, but this is most likely due to the closeness of the source
to the PSPC support grid structure).
The source appears to be extended or double. Thus, photons from the
total emission region were first extracted for analysis. A spectrum was
fit to this 'double' source (since their contributions cannot be
disentangled from each other safely; it is these results that are listed
in Table 2). In that case, a powerlaw of index {GAMMA}_X_ ~ -1.6 yields
a successful X-ray spectral fit. The cold absorption, if treated as free
parameter, underpredicts the Galactic value, and even more so if a RS
model is applied. The latter type of model only provides an acceptable
fit if the metal abundances are depleted below 0.01 x solar.
Secondly, since the optical position of NGC 5371 falls on the
northernmost of the two sources, source photons centered on the optical
position of the galaxy were extracted within a circular region of
diameter 250". In this case, the X-ray spectrum is dominated by the
northernmost source, but the second one contributes to some extent. The
spectral analysis then yields a best fit in terms of a powerlaw with
{GAMMA}_X_ ~ -1.96({chi}_red_^2^ = 0.5), and N_H_ recovers the Galactic
value if treated as free parameter. Again, RS emission can only
successfully describe the spectrum for heavily depleted abundances.
The source appears double, or extended. No HRI observation is
available for a more detailed study of the spatial extent.

8. 1997ApJS..108..155G
Re:NGC 5371
NGC 5371 shows a beautiful spiral structure drawn by most of the 100 H II
regions detected in the disk; the nearest to the nucleus is at 3.5 kpc,
and the brightest ones are in the outskirts of the spiral arm, which goes
to the south. The nucleus extends 9" at P.A. = 22^deg^.

9. 1996A&AS..115..439E
Re:NGC 5371
NGC 5371 is a grand design spiral galaxy (Elmegreen & Elmegreen 1990) with a
rising H I rotation curve in the outer regions (Begeman 1987). It has also
been classified as a LINER by Rush et al. (1993). It has a low dust
temperature but substantial far-infrared luminosity and may be a good
candidate for a post-starburst galaxy (Koorneef 1993). It is interesting that
the strongest observed CO profile is at the 30"-position to the north along
the major axis. Significant CO emission is also observed at the 15"-positions
along the east-west bar.

10. 1994CAG1..B...0000S
Re:NGC 5371
Sb(rs)I/SBb(rs)I
H-654-H
April 17/18, 1926
E40
60 min
The print of NGC 5371 here is made from a very weak early Mount
Wilson 100-inch plate, increased in contrast by control in the
darkroom. The suggestion of a bar is evident but not prominent. The
arms are thin and well formed, and contain many apparent HII regions.

11. 1976RC2...C...0000d
Re:NGC 5371
= NGC 5390
Photometry:
Bull. Ap. Inst. Duschambe, No. 46, 25, 1966.
HI 21cm:
M.N.R.A.S., 150, 337, 1970.

12. 1973UGC...C...0000N
Re:UGC 08846
SAB(rs)bc (de Vaucouleurs)

13. 1964RC1...C...0000d
Re:NGC 5371
= NGC 5390
Very small, bright, diffuse nucleus. Weak bar. Pseudo (r): 1.0 arcmin x
0.7 arcmin. Several knotty, filamentary, regular arms with some branches.


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