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Date and Time of the Query: 2019-04-26 T07:19:18 PDT
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Notes for object NGC 4117

8 note(s) found in NED.


1. 2003ApJS..146..353M
Re:NGC 4117
NGC 4117 (LW)
The main, prominent dust lane parallel to the semimajor axis dominates
the circumnuclear dust, yet at low contrast this arm appears to make
an entire revolution about the nucleus. This galaxy is relatively
highly inclined.

2. 2000ApJS..128..139F
Re:NGC 4117
5.6. NGC 4117 - Seyfert 2
NGC 4117 is a highly inclined S0 galaxy hosting a Seyfert 2
nucleus. The continuum images and color maps of this galaxy are shown in
Figure 12. The photometric major axis P.A. and the isophote ellipticity
of the galaxy, as measured beyond 10" (750 pc) from the nucleus, are
~ 22^deg^ and 0.55-0.60 (i.e., an inclination angle of ~ 65^deg^),
respectively. There is a strong dust lane southeast of the nucleus,
running roughly parallel to the photometric major axis of the galaxy
(see also M96). As no significant extinction feature is seen on the
other side of the galaxy (northwest side), this suggests that the near
side of the galaxy is its southeast side. Using equation (1) and the
difference in log (F547M/F791W) between the region northwest of the
nucleus and the dust lane area, we infer an V-band extinction
A_V_ ~ 1.5-2 mag for the dust lane.
The [O III] and [N II] + H{alpha} images of NGC 4117 are shown in
Figure 13. The [O III] emission is the most compact in our sample. It is
dominated by an unresolved nuclear core, with only a hint of diffuse
[O III] emission to the west of the nucleus. M96 reported extended
[O III] emission along the major axis of the galaxy. We do not detect
it, likely because of our much lower sensitivity to diffuse emission.
The [N II] + H{alpha} image shows an arc of emission west of the nucleus
and weak, diffuse emission to the north of the nucleus, which is better
seen in M96's image. The extended line emission along the disk of this
galaxy is probably related to star formation.

3. 1999ApJS..120..209N
Re:NGC 4117
NGC 4117 (type 2; Fig. 10) - There is a large confusing "stripe" on
the 20cm map, but no confusing source could be found within a radius of
a degree. The maps are therefore noisy. The source is quite weak, and
the structure would normally be considered unreliable. However, the 20
cm map of Paper VII shows a similar north-south extension. We therefore
classify the radio morphology as "(L)" at 20cm in P.A. 177^deg^. The
galaxy is not detected at 3.6cm. Paper VII lists a 20cm flux of 2.8 mJy
for this object, which is marginally higher than the present value, and
a flux upper limit of 0.6 mJy at 6 cm, so that our nondetection at
3.6cm is not surprising.

4. 1996ApJS..105...75C
Re:NGC 4117
4.2.5. NGC 4117
Our H{alpha} + [N II] image (Fig. 2e) of this galaxy shows emission from the
inner disk but no extended emission along the minor axis. We did not find
double-peaked line profiles or any evidence for ELRs extending out of the disk
in our minor axis spectra.

5. 1996ApJS..102..309M
Re:NGC 4117
Both [O III] and H{alpha} are extended roughly along the major axis of this
inclined galaxy. The high excitation gas is confined mainly to the southwest
of the continuum peak. NGC 4117 may have a weak extended component north of
the nucleus at 20cm (Ulvestad & Wilson 1989). This radio component would be
offset from the emission-line axis, but this needs to be verified with a
higher quality radio map. There is evidence for a large-scale dust lane in the
color map.

6. 1976RC2...C...0000d
Re:NGC 4117
= Holm 334a
Pair with NGC 4118 at 1.6 arcmin

7. 1973UGC...C...0000N
Re:UGC 07112
12 05.3 {+43 23} = NGC 4118 at 1.5, 137, 0.6 x 0.3, m=15.7
In a subgroup with UGC 07103 brightest at 8.5, 245
{UGC incorrectly notes: "+43 24". H. Corwin}

8. 1964RC1...C...0000d
Re:NGC 4117
= Holm 334a
Pair with NGC 4118 at 1.6 arcmin.


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