NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-05-22 T03:47:00 PDT
Help | Comment | NED Home

Notes for object NGC 4536

16 note(s) found in NED.


1. 2012ApJ...754...67F
Re:NGC 4536
NGC 4536 .SXT4..-A strong dust spiral extends into the very center. Fisher &
Drory (2008) classify the bulge as pseudobulge. The bulge radius is 10.1". The
major axis rotational velocity flattens well inside bulge radius at around 2".
The velocity dispersion profile is slightly asymmetric but mostly constant
within the bulge region. The h_3_ moments are anti-correlated with velocity
inside the bulge region and reach values of about 0.1. The h_4_ profile is
asymmetric. The minor axis velocities show slight asymmetric rotation (~=25 km
s^-1^). The velocity dispersion profile rises centrally but stays relatively
flat within +/- 10". The minor axis h_3_ moments are somewhat noisy but seem to
show a central depression.

2. 2008ApJ...677..926S
Re:NGC 4536
NGC 4536 is a barred late-type spiral (SABbc; de Vaucouleurs et al. 1976) that,
based on HST imaging, shows no evidence of a classical bulge but instead has a
surface brightness profile consistent with a pseudobulge that seems to exhibit
spiral structure (Fisher 2006). This galaxy is optically classified by H97 as an
H II galaxy. We detected the [Ne V] 14.3 micron line in this galaxy from an ~580
x 580 pc region (adopting the distance to NGC 4536 from H97) approximately 10"
northeast of the optical nucleus of the galaxy. This is the only galaxy in our
sample for which the [Ne V] emission seems to originate from a location that
does not coincide with the optical nucleus as listed in the NASA/IPAC
Extragalactic Database (NED). The [O IV] 26 micron and [Ne III] 15.5 micron
emission, however, are centrally concentrated with a peak that is offset from
the location of the [Ne V] emission and is closer to the optical nucleus than
defined in NED, as can be seen from Figure 4. The [O IV] 26 {mu}m line was not
detected in the same aperture in which the [Ne v] 14.3 micron line was detected;
the [O IV] flux is therefore listed as an upper limit in Tables 3 and 4 but is
displayed in Figure 4. We note that the sensitivity of the current mapping
observation of NGC 4536 is insufficient to conduct a full exploration of the
spatial morphology of the [Ne V] emission in this galaxy. Deeper IRS mapping
observations are critical to confirm the exact peak of the [Ne V] emission in
this galaxy. Apart from the [Ne V] detection reported in this work, to the best
of our knowledge, there is only one previously published observation of NGC 4536
that hints at the possibility of nuclear activity in this galaxy. The optical
line ratios obtained using recent high spatial resolution Space Telescope
Imaging Spectrograph spectroscopy suggest the presence of a weak AGN (Hughes et
al. 2005). There is abundant evidence for powerful nuclear star formation in NGC
4536.

3. 2008ApJ...677..926S
Re:NGC 4536
Its high far-infrared luminosity and strong H{alpha} (Pogge 1989), Br{gamma}
(Puxley et al. 1988), and 10.8 micron (Telesco et al. 1993) emission suggest
vigorous star formation in the central ~20" x 30" region. The radio emission
shows a diffuse morphology with three separate peaks (Vila et al. 1990; Laine et
al. 2006), possibly representing an annular ring of star formation surrounding
the nucleus. However, Laine et al. (2006) suggest, based on HST data, that the
radio clumps are close to the nucleus in projection but that none correspond to
the nucleus itself. This morphology is similar to that seen at 10.8 microns
(Telesco et al. 1993), as well as in the 1-0 S(1) molecular hydrogen line
(Davies et al. 1997). We note that the variable resolution of most published
observations, coupled with the fact that this galaxy is nearly edge-on and has
an intricate central complex of emission at various wavelengths, makes it very
difficult to confirm the spatial coincidence of the various sources. The galaxy
was detected by Einstein (Fabbiano et al. 1992). ROSAT High Resolution Imager
data reveal two ultraluminous X-ray sources, one of which may be coincident with
the optical nucleus (Liu & Bregman 2005). It is not possible, based on existing
X-ray observations, to determine whether this source is consistent with an AGN.
The galaxy was not observed by Chandra. Our observations provide strong
motivation to conduct an extensive high spatial resolution investigation at
infrared and X-ray wavelengths of NGC 4536 to determine the exact location of
the peak of the [Ne V] emission and to confirm its association with an AGN in
this galaxy. The central stellar velocity dispersion in this galaxy is 84 +/- 1
km s^-1^ (Batcheldor et al. 2005).

4. 2006MNRAS.366.1265B
Re:NGC 4536
Streaming motions along the spiral arms and a Z shape of the velocities in the
central parts are observed in this barred galaxy. As in the CO data (Sofue et
al. 2003), a steep velocity gradient is observed in the H{alpha} data.

5. 2006MNRAS.366..812C
Re:NGC 4536
This large barred galaxy displays two main prominent spiral arms and additional
spiral-like structures. The only kinematical perturbations are seen in the Z
shape of the velocities in the central parts and streaming motions along the
arms. As in the CO data (Sofue et al. 2003a), a steep velocity gradient is
observed in the H? data in the galaxy core.

6. 2005ApJS..160...76B
Re:NGC 4536
Significant discordance and very low S/N. Steep rotation and centrally peaked
{sigma}_*_ field. Steep centrally peaked curve of growth. High inclination
(~{degree}) and obscuring dust present (Hughes et al. 2003). See
Figures 27 and 30b.

7. 2003PASJ...55...59S
Re:NGC 4536
4.8 NGC 4536 This is also a single-CO peak galaxy with a typical spider
velocity field. The PVD comprises two ridges, a central steeply rising
component and a rigid-body like disk component. The RC rises extremely
steeply in the central 100 pc, reaching a maximum followed by a flat
RC. SMD shows clearly distinguishable three components of the core,
bulge and disk.

8. 2003PASJ...55...17S
Re:NGC 4536
6.9 NGC 4536 This is also a typical "single-peak" type galaxy with the
molecular gas being concentrated in the nuclear disk of ~10" radius
and an unresolved compact core exists at the nucleus. The velocity
field shows a spider diagram, and the PV diagram indicates that the
rotation velocity rises to 200 kms ^-1^ within the central 2". There
appears no strong non-circular streaming motion.

9. 2003AJ....126..742H
Re:NGC 4536
The morphological classification as determined by us is indicated in
parentheses next to the galaxy name, with our "chaotic circumnuclear
dust" (C) category now not including those galaxies with obvious dust
lanes (DL). Where the classification has already been made by Martini
et al. (2003), we indicate this with "-mp."
.
3.29. NGC 4536 (C)
Figure 14 (top).
Spectra: Strong continuum and emission lines and clear evidence of
rotation.
Images: Obscuring dust to the northeast of the nucleus in both STIS
and NICMOS images.

10. 1999AJ....118.2331V
Re:NGC 4536
The site of this well-studied SN Ia is not in the deep Sandage
et al. HST Cepheid images (Saha et al. 1996b) of NGC 4536, but instead
is in shallower F555W, F675W, F814W, and F658N exposures taken for
another project. SN 1981B occurred well beyond the galaxy's spiral arms,
near several faint H II regions (Fig. 20). We have performed PSF-fitting
photometry of the stars in the three broadband images within about 10"
of the SN site. Unfortunately, the resulting CMDs do not go sufficiently
deep to constrain the progenitor population for this SN Ia, since the
oldest population detected is apparently only about 20 Myr.
After the stars were subtracted away from the broadband images, we
estimated the colors and magnitude of the environment within the error
circle. We find that F555W - F675W ~ 1.6 mag, F555W - F814W ~ 0.83 mag,
and m_F555W_ ~ 28.45 mag. The F555W - F675W color almost certainly must
be contaminated by H{alpha} emission in the environment. The F555W -
F814W color is consistent with late F-type stars, indicating a possible
mixture of older red and younger blue stars in the environment.

11. 1994CAG1..B...0000S
Re:NGC 4536
VCC 1562
Sbc(s)I-II
CD-2139-S
March 22/23, 1982
103aO
50 min
NGC 4536 is one of the largest spirals in the
Virgo Cluster region. It is located about 6^deg^ south
of the center of Virgo subcluster B around NGC 4472,
and is near the beginning of what was once
called the southern extension of the Virgo
Cluster, now known as the Virgo Cluster envelope
along the supergalactic plane. The redshift of
NGC 4536 is v_o = 1646 km/s.
The spiral pattern is dominated by the two
principal spiral arms, clearly of the grand design
type. Many HII regions exist in the arms, the
largest of which are resolved into disks with core
diameters of about 3".

12. 1976RC2...C...0000d
Re:NGC 4536
Non-interacting pair with NGC 4533 at 8.2 arcmin
SPTM Observatory, 88, 239, 1968.

13. 1973UGC...C...0000N
Re:UGC 07732
SAB(rs)bc (de Vaucouleurs), Sc- (Holmberg)
See UGC 07721

14. 1964RC1...C...0000d
Re:NGC 4536
Very small, extremely bright nucleus. Foreshortened bar with strong dark lane.
Pseudo (r): 2.9 arcmin x 1.0 arcmin. 2 main, filamentary, regular arms with
knots.
Non-interacting pair with NGC 4533 at 8.2 arcmin.
Unusual increase of (B-V) with log A/D(0), interpolated value.
Photometry:
M.N.R.A.S., 94, 806, 1934.

15. 1956AJ.....61...97H
Re:NGC 4536
HMS Note No. 142
Slit on nucleus and emission patch. Redshift is for nucleus only,
since rotation may affect the result for the emission patch.
HMS Note No. 143
Emission patch approximately 75 arcsec [east] of nucleus.

16. 1918PLicO..13....9C
Re:NGC 4536
Vol. VIII, Plate 38. A fine bright spiral 7' x 1.8' in p.a. 122^deg^. Bright
nucleus; two main whorls, with several condensations; evidence of a short curved
absorption lane near the nucleus. See Abs. Eff. 25 s.n.


Back to NED Home