Date and Time of the Query: 2022-01-23 T02:02:24 PST
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Notes for object NGC 4150

17 note(s) found in NED.

1. 2007MNRAS.382.1552L
Re:NGC 4150
NGC 4150: Fig. 2 shows central structures in the B/I image, with a red nucleus
consistent with the dust structures seen in the HST images (Lauer et al. 1995).
The nuclear spectrum is dominated by absorption features with some weak emission
lines. The X-ray source X1 in Paper I (source 2 in Fig. 2) has a position
consistent with a knot of optical emission 15 arcsec away from the nucleus. Its
spectrum reveals that it is in fact a background quasar at redshift 0.52. Its
X-ray luminosity corresponds to 2-3 x 10^44^ erg s^-1^ in the 2-10 keV energy
range (Appendix B).

2. 2006MNRAS.369..497K
Re:NGC 4150
NGC 4150. Notable obscuration from dust is visible in the central parts of this
galaxy (Quillen, Bower & Stritzinger 2000). A KDC resides in the central few
arcsec of this galaxy (see Paper III), coincident with a strong drop in the Mg b
absorption strength and a corresponding peak in H{beta} absorption strength,
which itself is globally enhanced. The iron line maps are relatively featureless
by comparison, with no strong central features. The core is therefore dominated
by a young stellar population, as found by other authors (e.g. Fernandes et al.

3. 2006MNRAS.366.1151S
Re:NGC 4150
This object displays extremely smooth EW maps, exemplifying how closely the gas
emission can follow the stellar continuum in early-type galaxies. Despite heavy
binning, the V_gas_ and {sigma}_gas_ maps suggest fairly regular gas motions in
a dynamically cold disc. A complex dust structure in the central 3 arcsec
corresponds to the region where the stellar kinematics reveal counter-rotating
structure (Paper III) and to a minimum in the [O III]/H{beta} distribution.
Outside these central features, the gas and stellar kinematics are mildly
misaligned by 20^deg^.

4. 2006ApJS..166..154P
Re:NGC 4150:[PCV2006] ULX29
ULX29 is found in NGC 4150, a lenticular galaxy (T = -2). The only Association
image available was an I band exposure in which no counterparts were found.

5. 2004MNRAS.352..721E
Re:NGC 4150
NGC 4150: The dispersion map exhibits a double-peaked structure along
the major axis, which corresponds to a region where the velocity
gradient flattens out. A closer look at the central 5 arcsec reveals the
presence of a counter-rotating structure.

6. 2003A&A...398..467K
Re:NGC 4150
NGC 4150. The core of this lenticular galaxy is crossed by a curved
dusty furrow (see insert in Fig. 2). In spite of its low radial
velocity, V_LG_ = 198 km s^-1^ , NGC 4150 appears unresolved into stars
on the WFPC2 images. Its TRGB magnitude appears to exceed I_lim_ = 25
mag (beyond our detection limit), yielding a lower limit of 6.3 Mpc
for its distance. We suggest that NGC 4150 belongs to the Virgo
cluster outskirts, and not to the CVn I cloud. Most of the objects seen
in the galaxy body seem to be slightly extended and diffuse with
integrated colors of V - I = 0.8-1.6, which raises the possibility that
they are globular clusters. If they are indeed globular clusters, we
can use the turnover magnitude of the globular cluster luminosity
function (GCLF), V ~24 mag, as a distance indicator (Ferrarese et al.
2000). With this assumption we derive a rough distance estimate of ~20
Mpc consistent with the Virgo cluster distance.

7. 2002ApJS..142..223F
Re:NGC 4150
NGC 4150. This source was not detected in the NVSS. 1.4 GHz 15"
resolution observations (Condon et al. 1998b) show a weak 0.8 mJy
source. The high-resolution, 5 GHz observations of Wrobel & Heeschen
(1991) establish a 0.5 mJy upper limit to any radio emission.

8. 2001AJ....122..653R
Re:NGC 4150
NGC 4150: A strong nuclear dust lane causes considerable obscuration of
the central region, both in the optical and in the NIR. The dust lane was
carefully masked while doing the two-dimensional fit.

9. 2000MNRAS.319...17L
Re:NGC 4150
NGC 4150: A strong point-like source coincident with this galaxy was
detected in the ROSAT All-Sky Survey with
F_X_ = 6 x 10^-13^ erg s^-1^ cm^-2^ and a photon index {GAMMA} = 1.41.
The emission was assumed to be from the nucleus of NGC 4150
(Boller et al. 1992; Moran, Halpern & Helfand 1996). The high-resolution
image seen in Fig. 17 shows, however, that the X-ray
source is more than 15 arcsec away from the galactic nucleus, and has a
position consistent with a knot of optical emission. Spectroscopy of the
optical counterpart shows that the source is a background quasar at
redshift 0.52 (Fig. 32).
Fig. 17 shows that the X-ray contours of the source are elongated in
the north-west direction, suggesting that some emission might be coming
from the nuclear region of the galaxy. An estimate of the nuclear emission
was obtained using a 10-arcsec-radius aperture, located as shown in
Fig. 33. Although the observed counts have an S/N ratio of ~2.6 (and so
would be considered a significant detection by the criteria defined in
Section 3.2.2), the measurement will be treated as an upper limit because
of contamination from the nearby quasar.

10. 2000A&AS..141..211B
Re:UGC 07165
UGC 7165: has a SBP that is close to an exponential, and also has a
bright nuclear part. The color is almost constant over the whole radius
range, apparently including the central part. But the resolution of our
data is insufficient to discuss the center in any detail. The galaxy as
a whole has a smooth elliptical appearance.

11. 1999ApJ...519...89C
Re:NGC 4150
NGC 4150.-NGC 4150 is a nearby, small lenticular galaxy. We found a
compact X-ray source offset by 16.3" (767 pc) from the galaxy nucleus.

12. 1998ApJS..117..319A
Re:[ATZ98] D062
NGC 4150 = IRAS 12080+3040.

13. 1994CAG1..B...0000S
Re:NGC 4150
Hubble Atlas, p. 4
May 16/17, 1958
103aO + GG13
20 min
NGC 4150 has a typical S0 bulge and disk,
showing the extended outer envelope characteristic
of the S0 class. The print here is made to
show the inner dust lane rather than the faint
and extended outer envelope. This envelope can
be traced on the original plate to at least twice
the distance from the center of the bright star at
the lower right of the major axis. The envelope
can be seen best by viewing the print from a
The non-circular dust pattern threading the
inner third of the disk is the reason for the Sa
classification. If the lane were smoother and
more circular, the classification would be S0_3_.
However, a spiral pattern exists in the dust,
opening outward from the lower right part of this
print. The dust lane is seen much better here
than in the print in the Hubble Atlas (p. 4) made
from an early 100-inch Mount Wilson plate. The
galaxy was classed S0_1_ from that plate.

14. 1976RC2...C...0000d
Re:NGC 4150
Photometry (12 Color):
Ap. J., 145, 36, 1966.

15. 1973UGC...C...0000N
Re:UGC 07165
SA(r)0/a? (de Vaucouleurs)

16. 1964RC1...C...0000d
Re:NGC 4150
Very small, very bright nucleus with a faint dark crescent on one side.

17. 1961Hubbl.B...0000S
Re:NGC 4150
Jan. 31/Feb. 1, 1925
35 min
Enlarged 8.3X
The three zones mentioned in the description of NGC 1201 are
well marked here. The outer envelope of NGC 4150 is very
extensive. This places NGC 4150 later in the S01 classification
than NGC 1201. Microphotometer tracings should be
made of these galaxies to find the real difference in the
luminosity gradients of E and S01 galaxies. At present the
classification depends entirely on subjective impressions
gained from visual inspection of photographic plates.

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