Date and Time of the Query: 2019-05-26 T07:19:34 PDT
Help | Comment | NED Home

Notes for object NGC 4459

17 note(s) found in NED.

1. 2007MNRAS.379.1249D
Re:NGC 4459
This S0 galaxy is in the Virgo cluster. It is the control non-active galaxy for
NGC 2655. The SAURON data presented here (Fig. 4b) are part of the SAURON
project (de Zeeuw et al. 2002) and have therefore already been published
elsewhere (Emsellem et al. 2004; Sarzi et al. 2006).
The stellar component of NGC 4459 shows roundish isophotes, and its stellar
velocity field presents a very regular rotation pattern, the major-axis of which
is parallel to the LON (PA ~77{degrees}). The velocity dispersion rises towards
the centre, reaching 200 km s^-1^ (Fig. 4b). There is almost no ionized gas
emission (our maps have been clipped at 3 {sigma}), except for the very centre
(R < 3 arcsec).The emission-line velocity field seems to be dominated by
rotation, and the velocity dispersion rises from about 80 km s^-1^ for R > 3
arcsec to 160 km s^-1^ for H{beta} (200 km s^-1^ for [O III]) inside 3 arcsec.
The [O III]/H{beta} line ratio rises regularly towards the centre.

2. 2006MNRAS.369..497K
Re:NGC 4459
This galaxy shows a central region of stronger H{beta} absorption with a
ring-like structure around it. This is consistent with the central dust ring
found in this galaxy (see Paper V and Sarzi et al. 2001). The metal lines show
relatively regular gradients.

3. 2006MNRAS.366.1151S
Re:NGC 4459
This S0 galaxy shows an extremely well-defined dust distribution and regular gas
kinematics. The H{alpha} emission peaks in a circumnuclear ring, corresponding
to the region where the dust distribution appears the most circularly symmetric
and flocculent. However, the [O III] emission very closely follows the stellar
continuum. The values of the [O III]/H{beta} ratio therefore show a very similar
radial pattern to NGC 3032, with a minimum in a circumnuclear region and
stronger [O III]/H{beta} ratios toward the centre and the edge of the gas disc.
The independently derived H{beta} kinematics shows faster rotation and smaller
velocity dispersions than the [O III] kinematics, suggesting that the H{beta}
line is tracing better than the [O III] doublet a kinematically colder component
of gas, which is currently forming stars. The detection of molecular gas by Sage
& Wrobel (1989) supports this picture.

4. 2006ApJS..164..334F
Re:VCC 1154
VCC 1154 (NGC 4459).This galaxy harbors a spectacular dust disk, similar to the
one seen, at higher inclination, in VCC 1535. The disk is about 17" across, and
its plane is inclined by ~45^deg^ to the line of sight. There are several blue
clumps in the disk, probably indicative of star formation. Several wisps and
filaments extend beyond the edge of the disk. As for the case of VCC 1535, the
correction for dust fails, and the profile can only be recovered beyond 7.5"
from the center. Unlike the case of VCC 1535, the isophotes look regular.

5. 2006A&A...460...45G
Re:NGC 4459
NGC 4459 (UGC 7614). Our morphological classification (SB candidate, see Fig. 5)
agrees with that by Satyapal et al. (2005), also based on ACIS Chandra data, who
give no additional X-ray information on this object.

6. 2006A&A...453...27C
Re:UGC 07614
UGC 7614: we estimated an upper limit to any non-thermic emission fixing the
photon index to {GAMMA} = 1.9.

7. 2005A&A...440...73C
Re:UGC 07614
UGC 7614: the presence of an inclined large scale disk induces relatively large
fluctuations in the outer profile, but the relatively unperturbed morphology at
small radii allows us a robust classification as a power-law galaxy.

8. 2004MNRAS.352..721E
Re:NGC 4459
NGC 4459: The small opening angle of the isovelocities in the central 10
arcsec corresponds to a region where h_3_ is anticorrelated with V, and
has a rather high amplitude (see Peterson 1978).

9. 2002ApJS..142..223F
Re:NGC 4459
NGC 4459. There is no NVSS detection of this source. FIRST detected a
1.8 mJy source, which together with the Wrobel & Heeschen (1991)
0.8 mJy detection at 5 GHz, 5" resolution, shows the compact and
flattish spectrum nature of the source.

10. 2002ApJ...574..740T
Re:NGC 4459
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]).

11. 1994CAG1..B...0000S
Re:NGC 4459
VCC 1154
Hubble Atlas, p. 5
Feb 1/2, 1979
103aO + Wr2c
60 min
The internal circular dust lane in NGC 4459, characteristic of
S0_3_, is prominently seen in the insert. On the original plate it can
be traced completely around the central bulge, burned out slightly in
the insert print here from a Mount Wilson 100-inch plate.
The extended envelope, showing the two-zone nature of the image,
is prominent.

12. 1994A&AS..105..481M
Re:NGC 4459
NGC 4459: This is a well known disk dominated S0, with an inner ring
of dust.

13. 1976RC2...C...0000d
Re:NGC 4459
NGC 4468 at 8.5 arcmin.
NGC 4474 at 13.5 arcmin.
Astrofizika, 1, 38, 1965.
Ap. J., 146, 28, 1966.
Bol.A.A.Argentina, No. 16, 17, 1971.
Bull. A.A.S., 5, 447, 1973.
Ap. J. (Letters), 193, L49, 1974.
Dynamics and Mass Determination:
Ap. J., 139, 284, 1964.

14. 1973UGC...C...0000N
Re:UGC 07614
SA(r)0+ (de Vaucouleurs)
Companion 2.2, 44, 0.5: x 0.5:

15. 1964RC1...C...0000d
Re:NGC 4459
Small, very bright nucleus in a smooth (r): 0.3 arcmin x 0.25 arcmin. Strong,
dark crescent.
NGC 4468 at 8.5 arcmin.
NGC 4474 at 13.5 arcmin.
Ap. J., 132, 306, 1960.
Misprint in, Zeit. fur Ap., 50, 168, 1960, are for the NGC 4559.

16. 1961Hubbl.B...0000S
Re:NGC 4459
Mar. 8/9, 1940
15 min
Enlarged 19.2X
The form of NGC 4459 is nearly identical to that of NGC 3032
(left) except that the internal absorption ring is more
regular. The ring can be traced through an entire revolution,
although it is less opaque on the south side. This
may be a projection effect where the bright central nucleus
is spherical and projects in front of the far side of the
absorption lane.

17. 1957HPh....53..275d
Re:NGC 4459
(Plate 3)
Weak ring or whorl of dark material appears in the lens close
to the large nucleus.
The envelope does not show up in this view taken with a
short exposure.
Compare with NGC 2855 (Plate 4) and NGC 1553 (Plate 7).

Back to NED Home