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Date and Time of the Query: 2019-06-18 T03:46:41 PDT
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Notes for object NGC 4968

9 note(s) found in NED.


1. 2004MNRAS.353.1151S
Re:NGC 4968
NGC 4968. Has been studied as part of a H_2_0 maser emission sample by
Greenhill et al. (2002) as well as part of a sample studying compact
radio cores in Seyfert galaxies by Roy et al. (1994). The radio
continuum of NGC 4968 has also been observed by Schmitt et al. (2001)
and Morganti et al. (1999).

2. 2003ApJS..148..327S
Re:NGC 4968
5.38. NGC 4968
Figure 11 (top right panel) presents the [O III] image of this
Seyfert 2 galaxy. The major axis of the [O III] emitting region is
extended by 2.2" (420 pc) along P.A. = 40^deg^ and 1.3" (250 pc),
along the perpendicular direction. Previous ground-based observation
did not detect any extended [O III] emission (Pogge 1989) and found
only some marginally extended radio emission (Schmitt et al. 2001b).
A more detailed description of the NLR of this galaxy is given by
Ferruit et al. (2000).

3. 2003ApJS..146..353M
Re:NGC 4968
NGC 4968 (C)
Any dust structure on the far side of the circumnuclear region is
essentially washed out, and this makes it difficult to determine if
the dust visible on the near side forms a spiral pattern. Southeast of
the nucleus is a bluer region in the color map, and this corresponds
to the extended emission observed by Ferruit et al. (2000), which may
be the ionization cone.

4. 2001ApJS..132..199S
Re:MCG -04-31-030
4.2.12. MCG -04-31-030
According to Pogge (1989) the [O III] and H{alpha} images of this
galaxy do not show extended emission. The hard X-ray spectrum can be
fitted with a double power law and has a flux
F_2-10 keV_ = 3.56 x 10^-12^ ergs cm^-2^ s^-1^ (Turner et al. 1997). The
HST F606W image (Malkan et al. 1998) shows a bright nuclear source and a
dust lane to the north of the nucleus. This galaxy shows a low flux
density linear structure extended by 480 pc along P.A. = 85^deg^.

5. 2000ApJS..128..139F
Re:NGC 4968
5.7. NGC 4968 - Seyfert 2
NGC 4968 is an inclined S0 galaxy hosting a Seyfert 2 nucleus. Our
continuum images and color maps of this galaxy are shown in Figure 14.
From the continuum images, we derive a photometric major axis P.A. of
~ 45^deg^ and an ellipticity of 0.48-0.50 (i.e., an inclination angle of
~ 60^deg^) at radii greater than 10" (2.1 kpc). The northwest side of
the galaxy is heavily obscured. Examination of the color map of the
central regions (Fig. 14, bottom right-hand panel) shows that the red
features in this map are reminiscent of the superposition of a spiral
dust feature and an inclined dusty ring similar to the one in NGC 2273
(see section 5.3). Using equation (1) and the difference in
log (F547M/F791W) between the regions northwest (~ -0.3 to -0.4) and
southeast (~ 0) of the nucleus, we infer a V-band extinction
A_V_ ~ 1.9-2.5 mag for the ring. That we observe heavy extinction of the
background stellar continuum northwest of the nucleus, while the regions
southeast of the nucleus are apparently unobscured, is consistent with
the ring lying in the plane of the (highly inclined) galaxy disk, with
the northwest side being the nearer.
The emission-line region of NGC 4968 is spatially resolved for the
first time in our [O III] and [N II] + H{alpha} images (Fig. 15, top
panels). It is extended toward the southeast side of the nucleus and the
[O III] has a wedge-shaped morphology. This could be interpreted as the
signature of an ionization cone projecting against the far side of the
galaxy disk. However, the emission-line region fills almost perfectly
the cavity inside the dusty ring (see Fig. 14, bottom right-hand panel)
and this wedge-shaped morphology could be a reddening effect. The
[O III]/([N II] + H{alpha}) map is shown in Figure 15 (bottom panel).

6. 1999A&AS..137..457M
Re:NGC 4968
NGC 4968: This object is unresolved in our observations. A core of
10 mJy has been detected with the PTI at 13 cm (R94).

7. 1997ApJS..113...23T
Re:NGC 4968
A13. NGC 4968
Our ASCA flux finds this source a factor ~5 dimmer than during the HEAO 1 A-1
survey (see Polletta et al. 1996). Unfortunately, we cannot check whether this
is due to contaminating sources close to NGC 4968 as no ROSAT observation of
this field is currently available. These ASCA data are equally well fitted by
several of our test models.

8. 1985SGC...C...0000C
Re:NGC 4968
Plate 2347
Overexposed center, very faint (R'): 1.0 x 0.6: in pretty bright lens.
3rd in group.

9. 1982ESOU..C...0000L
Re:ESO 130424-2324.7
=ESO 508- G 06
in cluster


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