NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-04-24 T04:48:00 PDT
Help | Comment | NED Home

Notes for object NGC 4596

11 note(s) found in NED.


1. 2008MNRAS.386.2242H
Re:NGC 4596
NGC 4596 has a relatively exponential bulge with Sersic index n= 1.4
(Laurikainen, Salo & Buta 2005), but the bulge kinematics (Bettoni &
Galletta 1997) is ellipsoidal.

2. 2008MNRAS.386.2242H
Re:NGC 4596
NGC 4596 has a relatively exponential bulge with Serisic index n=1.4
(Laurikainen,Salo & Buta 2005), but the bulge kinematics (Bettoni & Galletta
1997) is ellipsoidal.

3. 2006MNRAS.369..529F
Re:NGC 4596
NGC 4596 is a non-interacting strongly barred galaxy (Gerssen, Kuijken &
Merrifield 1999). The SAURON stellar velocity field displays regular rotation
along an axis misaligned with respect to the photometric major axis. There is
evidence for a disc-like component in the inner 5-arcsec region, that it is also
apparent in the velocity dispersion and h_3_ maps. The distribution and
kinematics of both H{beta} and [O III] are aligned with the stellar kinematic
major axis. Gerssen et al. (1999), using the Tremaine-Weinberg method, reported
that NGC 4596 has a fast bar.

4. 2006A&A...460...45G
Re:NGC 4596
NGC 4596 (UGC 7828). This galaxy is very faint at X-ray frequencies, showing
diffuse X-ray morphology in all the spectral bands (Fig. 5). Information on its
spectral properties cannot be obtained based on the present data due to the lack
of sufficient counts in the hard band (4.5-8.0* keV). No previous X-ray data
have been reported for this galaxy.

5. 2005MNRAS.364..283E
Re:NGC 4596
NGC 4596. All measurements are from BARS Project R-band images (taken with the
Prime Focus Camera of the INT), except for the outer-disc orientation and
inclination, which are from a deeper I-band image.

6. 2002ApJ...574..740T
Re:NGC 4596
NGC 2787, NGC 4459, NGC 4596.
The black hole masses are based on Space Telescope Imaging
Spectrograph (STIS) measurements of ionized-gas disks by
Sarzi et al. (2001). The disk inclinations are determined from
dust-lane morphology. Note that the distance and dispersion for
NGC 2787, 7.5 Mpc and 140 km s^-1^, are much smaller than the
values assumed by Sarzi et al. (2001). Our distance is from
Tonry et al. (2001), and the dispersion was measured by one
of us (Gebhardt). For NGC 4459 and NGC 4596, we have used the
dispersions {sigma}'_8_ from Sarzi et al. (2001), since on average
these are close to {sigma}_1_ (eq. [16]).

7. 1997A&AS..124...61B
Re:NGC 4596
This is a well known example of SB0 galaxy; SB0(r)+ in RC3. It has been yet
classified as SBa(very early) in RSA. Photometry and kinematics of the bar have
been studied by Kent (1990), who found that the bar in this galaxy is roughly
rectangular, and that the kinematics of the bar do not differ from the mean
rotation of the disk of the galaxy. The rotation curve along the bar shows a
peak of velocity near the center, followed by a decrease and by a new rise
outward. This shape is confirmed by our measurements and it appears to be
another case of the waving rotation curve phenomenon observed in the bars of
many SB0s (Bettoni 1989). The velocity dispersion is almost constant along all
the observed PAs and our value (Table 2) is in very good agreement with
previous published data (Mcelroy 1995).

8. 1994CAG1..B...0000S
Re:NGC 4596
VCC 1813
SBa (very early)
(VE,L,0)
CD-1319-S/Br
March 12/13, 1980
103aO
75 min
The images of the four galaxies on this panel have been printed
to a contrast showing the pattern of the bar and the inner disk at the
place where the ansae of the bar terminate on the rim of the disk. The
best example of the form is NGC 4596, which is one of the earliest SBa
galaxies in the RSA.
The bar is well defined. The flared ansae end abruptly on the rim
of the disk, which, however, is not elliptically symmetrical but is
broken at the bar termini where the massive smooth spiral pattern that
covers the outer disk begins.
There are no external arms as in the galaxies on the preceding
panel. The SBa classification rests solely on the internal massive
spiral pattern of the disk at the ends of the bar. A structure of this
kind will be generally missed on plate material of low spatial
resolution.
The classification of SB0 in the RC2, based on a Mount Wilson
yellow plate, is not appropriate.

9. 1976RC2...C...0000d
Re:NGC 4596
Non-interacting pair with NGC 4608 At 19 arcmin
Spectrophotometry:
Observatory, 88, 239, 1968.

10. 1973UGC...C...0000N
Re:UGC 07828
SB(r)0+ (de Vaucouleurs), Sa (Holmberg)
Paired with UGC 07842 at 18.9, 94

11. 1964RC1...C...0000d
Re:NGC 4596
Very bright, diffuse nucleus in a strong bar with blobs. Faint (r):
1.8 arcmin x 1.3 arcmin.
Non-interacting pair with almost identical twin NGC 4608 at 19 arcmin.
Lund 9 dimensions are for the bright part only.


Back to NED Home