Date and Time of the Query: 2019-08-20 T21:44:19 PDT
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Notes for object NGC 0931

10 note(s) found in NED.

1. 2003ApJS..148..327S
Re:Mrk 1040
5.6. Mrk 1040
The [O III] image of this Seyfert 1 galaxy is presented in the bottom
right panel of Figure 5. The [O III] emission is extended and shaped
like a cone with opening angle of 120^deg^, apex at ~0.6" NW of the
nucleus, and the axis pointing toward the SE direction, perpendicular
to the host galaxy disk. The emission along the apparent cone axis is
extended by 1.1" (350 pc) and by 1.5" (480 pc) along the
perpendicular direction. The radio emission of this galaxy is
unresolved (Schmitt et al. 2001b).

2. 2002AJ....124..675C
Re:UGC 01935
Unusually warm FIR source: alpha(25,60) = 0.76. Seyfert 1.5.

3. 1997MNRAS.286..513R
Re:MRK 1040
7.1.3 Mrk 1040
The ASCA observation of Mrk 1040 has been presented previously by Reynolds et
al. (1995a). In the present work, we model the soft complexity of this source
as a combination of neutral absorption and O VII and O VIII edges in order to
force a comparison with the classical warm absorber sources. However, due to
the small count rate and high Galactic line-of-sight absorption (7.07x10^20^
cm^-1^: Elvis et al. 1989), the exact nature of the soft complexity is unclear
and several alternative models are explored by Reynolds et al. (1995a). The
intrinsic neutral absorption is probably related to the interstellar medium
(ISM) of the host galaxy which possesses a large inclination (Amram et al.

4. 1997A&A...327..493R
Re:MRK 1040
Mrk 1040=NGC 931 is another interacting galaxy. It shows a flat-topped HI
emission line of almost 500 km/sec FWZI (Mirabel & Wilson 1984), which is quite
distinct from our gaussian shaped CO emission line profile. Solid body rotation
encompassing most of the optical disk could explain the observed 500 km/s HI
width. The differences between the HI and CO profiles reveal the differences in
the radial distribution of the HI and CO clouds.

5. 1996ApJS..105...75C
Re:NGC 0931
4.1.3. NGC 931 (Mrk 1040)
Our R-band image (Fig. 1c) shows the presence of a companion galaxy ~20" to
the north along the minor axis. Apart from emission from this companion galaxy,
we find no extended H{alpha} + [N II] emission in our long-slit spectra along
the minor axis. Fabry-Perot studies (e.g., Amram et al. 1992) show that the
kinematics of the emission-line gas are quite complex, but there is no evidence
for an outflow from the nuclear region.

6. 1996ApJ...467..551C
Re:NGC 0931
3.1.6. NGC 931 (Mrk 1040)
We did not obtain radio images of NGC 931. Rush, Malkan, & Edelson (1995) find
a flux of 6.2 mJy at 4.9 GHz (VLA, D-configuration) but do not show a map.

7. 1995ApJ...447..121W
Re:NGC 0931
NGC 931.-We find marginal evidence for a narrow spectral feature at ~7.2
keV in this galaxy.

8. 1994AJ....108.2128C
Re:PGC 009399
PGC 009399 = NGC 931. Delete B_T_, all colors, log A_e_, and m'_e_;
apertures are too small. B^o^_T_ = 12.23, HI = 1.10.

9. 1984AnTok..192.595T
Re:KUG 0225+310
Spiral with a companion to the north.

10. 1973UGC...C...0000N
Re:UGC 01935
Companion superimposed at 0.35, 353, 0.2 x 0.1

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