Date and Time of the Query: 2019-06-26 T17:45:57 PDT
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Notes for object NGC 4235

16 note(s) found in NED.

1. 2006MNRAS.369..529F
Re:NGC 4235
NGC 4235 is a nearly edge-on Seyfert 1 galaxy (Jimenez-Benito et al. 2000) in a
non-interacting pair with NGC 4246 at 12 arcmin. The stellar velocity field
displays regular rotation and evidence for the presence of a smaller stellar
disc in the inner parts. This is supported by a decrease in velocity dispersion
and h_3_ anticorrelation in the centre of the galaxy. The [O III] emission is
much more extended along the main disc of the galaxy than the H{beta} emission,
which is mainly confined near the centre of the galaxy. The [O III]/H{beta}
ratio is high in the centre, consistent with its classification as a Seyfert
galaxy. The ionized-gas velocity maps of both H{beta} and [O III], although
patchy, are consistent with the stellar velocity field. Near-infrared surface
photometry of this galaxy is presented in Peletier et al. (1999). Long-slit
kinematics can be found in Corsini et al. (2003).

2. 2005ApJ...627..674A
Re:NGC 4235
NGC 4235.Essentially unresolved in the VLBA imaging of A04, this galaxy shows
modest variability in the September VLA data.

3. 2005A&A...429..439G
Re:VCC 0222
VCC 222: We did not detect this galaxy, with an rms noise level of 0.60 mJy. Its
optical redshift, 2298+/-122 km s^-1^, is not well determined. An Effelsberg H I
detection was reported by Huchtmeier (1982) at 2410 km s^-1^, with W_50_ = 273
km s^-1^ and I_HI_ = 4.4+/-1.5 Jy km s^-1^, with an average line signal of 16
mJy. Although Magri (1994) reported a tentative detection at 2596 km s^-1^, its
low signal-to-noise ratio makes it appear spurious. Two published (Krumm &
Salpeter 1979; Mirabel & Wilson 1984) estimated upper limits to its line flux
are 2.4 and 3.4 Jy km s^-1^, respectively. We conclude that the line signal
reported by Huchtmeier is spurious and due to RFI.

4. 2003A&A...406..505R
Re:NGC 4235
NGC 4235 NGC 4235 has been classified as a Seyfert galaxy of type 1
(Weedman 1978), and has no physical companion (Dahari 1984). Pogge
(1989a) has studied the nuclear environment using narrowband imaging of
H{alpha} and [O III]. He found a bright nucleus with an extended
region towards the NE direction at PA ~48deg, which extends ~4.4".
Neither disk H II regions were detected, nor ionized gas above the
plane. Radio continuum observations (Hummel et al. 1991) also did not
find evidence for extended emission. In the X-ray regime the strong
nuclear region is detected with a luminosity of 1.55x10^42^~ erg~ s^-1^
(Fabbiano et al. 1992). In a study of large-scale outflows in edge-on
Seyfert galaxies Colbert et al. (1996b) found no double peaked line
profiles, or any evidence for extended line regions, and no minor axis
emission, too. However, on radio continuum images obtained with the VLA
at 4.9 GHz there was a diffuse, bubble-like, extended structure (~9
kpc) found in addition to the unresolved nucleus (Colbert et al.
1996a). Our H{alpha} image reveals a bright nucleus with a faint
extended layer, which is restricted to the circumnuclear part. NE of
the nucleus a depression is visible, possibly due to absorbing dust, as
already noted by Pogge (1989a), and easily visible in the broad band
HST image by Malkan et al. (1998). This is one of the very few Seyfert
galaxies that appear in our survey. The role of minor axis outflows in
Seyfert galaxies, and thus the contribution to the IGM enrichment and
heating still has to be explored.

5. 2002AJ....124..675C
Re:UGC 07310
Seyfert 1.

6. 2001ApJS..133...77H
Re:NGC 4235
NGC 4235 (S1.2). - The unresolved core has a flat or slightly inverted
spectrum ({alpha}_6_^20^ = 0.09), consistent with previously reported flux
densities from 2 to 20 cm (Ulvestad & Wilson 1984b, 1989; Kukula et al.

7. 2000MNRAS.317..907J
Re:NGC 4235
3.1 NGC 4235
NGC 4235 is classified as a Seyfert 1 galaxy in the literature (Abell,
Eastmond & Jenner 1978; Morris & Ward 1988). It is a nearly edge-on
spiral galaxy and its nuclear emission is strongly reddened by the dust
in the spiral arms of the galaxy (Abell et al. 1978). It has a spatially
resolved nucleus, bisected by a dust lane (Malkan, Gorjian & Tam 1998),
and extended radio emission spread on both sides of the galaxy
(Colbert et al. 1996a) with a compact radio core
(Ulvestad & Wilson 1984b; Kukula et al. 1995). The galaxy presents
optical emission lines extended along the major axis (Pogge 1989;
Colbert et al. 1996b).

8. 1998ApJ...500..685P
Re:NGC 4235
7. NGC 4235.--NGC 4235 has a Seyfert 1 type nucleus hosted by an SAa galaxy. The
disk shows prominent dust lanes. For this object, we have not included the
120 {mu}m flux value in the inversion, since this measurement is very noisy and
not very secure. The result of the inversion shows three components at 11, 42,
and 151 K, with widths of 11, 15, and 120 K, respectively. Although the
temperature spectrum (see Fig. 1) rises a bit at the ends of the temperature
range, to fit the SED we have only taken the three temperature components
described above, totally neglecting the contribution of those features at the
ends. We believe that these edge features are due to the boundary conditions
used in solving the numerical problem, and they do not influence the final
result. For this galaxy the warm component at 151 K is the more intense one,
the very cold component at 11 K being very dim.

9. 1997ApJS..112..391H
Re:NGC 4235
NGC 4235.--The broad H{alpha} profile of this Seyfert 1 nucleus (Abell,
Eastmond, & Jenner 1978) has a peculiar secondary hump redward of [N II]
{lambda}6583, resembling that of NGC 7213 (Filippenko & Halpern 1984). The
narrow-line profile, as judged by modeling [S II], requires a superposition of
three Gaussians to reproduce its irregular shape (Fig. 6e). The profile of
[N II] {lambda}6583 appears to have additional structure not present in [S II],
but, for the present purposes, we neglect this subtlety. A very prominent broad
component is visible at H{beta}.

10. 1997A&A...319...33A
Re:NGC 4235
NGC 4235 This is the pair which involves the strongest pair of X-ray sources,
C=268 and 119 as shown in Fig. 9. The brighter source coincides almost exactly
with a V_est_~17mag., compact galaxy. This might, for example, turn out to be
an object like the Seyfert 1 companion near NGC 3516 (see Fig. 11 and Table 2).
There are apparent BSO's about 1' on either side of the brighter, C=268, X-ray
source. The C=119 source lies close to a BSO: (V_est_~16.5mag.) with apparent
jet connection in the blue to a BSO: ~45"NW. Both of these represent unusual
configurations and should be investigated with deep, high resolution direct
imaging and spectra. Finding charts are given in the Appendix.
One unresolved puzzle is that a Seyfert 1, MSS 12170+07, V=16.29, Z=.080 is
catalogued at the position of the + sign in Fig. 9. The Einstein, X-ray
position is 36" E of the optical object, a somewhat large disparity. But only
14" SE of the MSS position is a faint BSO (only on the blue plate with O=21.59
mag., O-E<1.59 mag.) which could be the source of the X-rays. The puzzle is
that the ROSAT observation does not register the MSS source but does register a
C=119 source 5.6' SE of the reported MSS source. The ROSAT source is completely
free of web or detector support structure.

11. 1996ApJ...467..551C
Re:NGC 4235
3.1.11. NGC 4235
In Figure 1g, we show contour maps of the radio emission from NGC 4235. Diffuse
structures extend out ~1' (9.3 kpc) from the nucleus, both eastward and
westward from the nuclear region. The morphology of the extraplanar emission
appears diffuse and bubble-like, especially toward the west. At large radii,
the eastern source may be slightly more extended toward the galaxy minor axis
(see low-resolution 20 cm map).
The nuclear radio source is unresolved in small-scale VLA maps (Ulvestad &
Wilson 1984; Kukula et al. 1995).

12. 1995MNRAS.276.1262K
Re:NGC 4235
NGC 4235: Type 1. Host galaxy: Sa (UGC). Radio: a single compact
component, unresolved in both images. Ulvestad & Wilson (1984b) report a
flat radio spectrum.

13. 1994CAG1..B...0000S
Re:NGC 4235
VCC 222
March 24/25, 1980
75 min
NGC 4235 is in the Virgo region but is
probably in the W cloud (Sandage, Binggeli, and
Tammann 1985b), a notion that is supported by
the high velocity of v_o = 2527 km/s.
Intricate dust lanes pervade the disk, only a
few of which are visible in the print. As in NGC
5689 above and NGC 7377 on panels 75 and
S14, the multiple arms are made entirely of dust
lanes. No evidence of HII regions is on the plates,
either in the smooth disk or associated with the
dust arms.

14. 1976RC2...C...0000d
Re:NGC 4235
= IC 3098
= Holm 359a
Non-interacting pair with NGC 4246 at 12 arcmin.
NGC 4247 at 13 arcmin.

15. 1973UGC...C...0000N
Re:UGC 07310
SA(s)a (de Vaucouleurs), Sa (Holmberg)

16. 1964RC1...C...0000d
Re:NGC 4235
= IC 3098
= Holm 359a
Small, very bright diffuse nucleus in a bright bulge. Smooth spiral arms
with a dark lane on one side.
Lund 9 dimensions are for the bright part only.
Yerkes 1 classification: or DG
Non-interacting pair with NGC 4246 at 12 arcmin.
Non-interacting pair with NGC 4247 at 13 arcmin.

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