Date and Time of the Query: 2019-06-20 T05:12:48 PDT
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Notes for object NGC 1667

16 note(s) found in NED.

1. 2006ApJS..164...52S
Re:NGC 1667
The nucleus of this galaxy hosts a low-luminosity Seyfert 2 (Ho et al. 1997).
The images (Fig. 2, left) show that the AGN contributes very little to the
overall UV, H{alpha}, and radio emission. Less than 1% of the UV emission
originates from the nucleus of this galaxy (inner 2"), where the emission may in
part be due to nuclear radiation scattered in our direction, or to circumnuclear
star formation. Most of the emission in this band comes from star-forming
regions along the spiral arms of the galaxy. The H{alpha} image shows
significantly stronger emission at the nucleus, related to the Seyfert 2 nucleus
of this galaxy. It also shows emission from the star-forming regions along the
spiral arms. The radio image shows strong emission related to the galaxy;
however, because this emission is weak, we were not able to self-calibrate this
image, and some closure errors can still be seen.

2. 2004A&A...418..465L
Re:NGC 1667
NGC 1667 is likely another example of a fading "fossil" AGN (Bassani et
al. 1999), introducing additional uncertainty on the AGN contribution
at different wavelengths. For example, if the AGN is turning off the
apparently high N_ H may be an artifact of the reflected component
remaining visible longer.

3. 2004A&A...415..941E
Re:NGC 1667
NGC 1667: Suggested as double-barred by Laine et al. (2002). Inspection of the
K-band image of Mulchaey et al. (1997), the NICMOS2 F160W image, and the WFPC2
F606W image all indicate that "outer bar" is really a pair of spiral arms (as
noted by Mulchaey et al.); see Fig. 6. In this case, it is the "inner" bar which
is evidently the genuine (and only) bar in this galaxy; isophote twists interior
to it are due to strong dust lanes.

4. 2003ApJS..146..353M
Re:NGC 1667
NGC 1667 (LW)
The star-forming ring at approximately 2 kpc is composed of many
spiral arm fragments intermixed with young star clusters. Inside of
the ring the circumnuclear disk is substantially smoother and the few
spiral dust lanes present do not fill the disk.

5. 2002A&A...389...68G
Re:NGC 1667
NGC 1667: this galaxy has a small apparent size, with a catalog
with a low number of HII regions. Nevertheless, as the galaxy is
quite inclined, the two methods are in reasonable agreement and
we give the mean of both methods.

6. 2001ApJS..133...77H
Re:NGC 1667
NGC 1667 (S2). - Ulvestad & Wilson (1989) detected a core at 6 and 20 cm
with flux densities comparable to ours, and Thean et al. (2000) give a
similar value of S_6_ = 1.5 mJy ({DELTA}{theta} = 0.3"). Our tapered 6 cm
map shows, in addition, a low surface brightness two-armed spiral feature,
with a total linear extent of 14.5 kpc along P.A. ~ 0^deg^. The tapered
20 cm image only shows the central core and the high-surface brightness
region of the southern spiral arm.

7. 1999AJ....117.2676R
Re:NGC 1667
The HST color map of NGC 1667 (Fig. 2h) reveals a complex but
relatively ordered dust morphology with a nuclear spiral morphology. The
overall extinction is stronger to the northeast of the nucleus. From the
southwest a relatively straight dust lane approaches the nuclear region
until it intersects a nuclear ring. Here it curves around until it joins
the opposite dust lane approaching the ring from the north. The ring
then continues around until it is south of the nucleus where it then
becomes hard to trace. Inside the ring a multiarmed spiral pattern is
seen near the nucleus. These two arms are only roughly symmetrical and
the center of symmetry does not appear to be the nucleus. Blue,
presumably star-forming, regions are also visible in the map as clumps
to the west of the western dust lane and about 7" southeast of the
nucleus near where the eastern dust lane intersects the dust ring.

8. 1997ApJS..113...23T
Re:NGC 1667
A4. NGC 1667
This Seyfert nucleus is surrounded by extended H II regions, the ionization of
which is only weakly influenced by the central engine. Radovich & Rafanelli
1996) find evidence for intense star formation activity in the inner 10 kpc of
this source, and they estimate 700-3000 O V stars reside within this region. No
ROSAT image is currently available to check for spatial extent. Historically,
the source has varied by a factor 6 in 2-10 keV flux (Polletta et al. 1996).

9. 1997ApJS..112..391H
Re:NGC 1667
NGC 1667.--The narrow-line profiles have extended, non-Gaussian wings that are
slightly asymmetric to the red (Fig. 8a), giving the false impression that
there might be a broad H{alpha} line in this Seyfert 2 nucleus. Both H{alpha}
and [N II] have similar profiles, but [S II] is slightly narrower.

10. 1997ApJS..110..299M
Re:NGC 1667
Inner bar is visible in both ellipticity fits and the K_S_image. Second
increase in ellipticity beyond about ~10" is probably due to inclined
spiral arms. Unbarred in the RSA.

11. 1997ApJS..108..155G
Re:NGC 1667
This is an S2 nucleus in an Sc host galaxy. The disk is a strong H{alpha}
emitter; the H II regions are mainly clumped along the spiral arms and an
inner ring. The nucleus is compact, and its emission represents only 5%
of the total emission.

12. 1994CAG1..B...0000S
Re:NGC 1667
Nov 6/7, 1980
12 min
The three main spiral arms begin tangent to
a high-surface-brightness inner ring similar to
the pattern in NGC 309 (panel 221).
The redshift is v_o = 4562 km/s.

13. 1994AJ....108.1987A
Re:NGC 1667
NGC 1667. The ellipse fitting results were not satisfactory with bigger
errors. The extrapolated magnitude was not accurate enough to be used in the

14. 1976RC2...C...0000d
Re:NGC 1667
Pair with NGC 1666 at 15 arcmin.

15. 1964RC1...C...0000d
Re:NGC 1667
Very small, bright nucleus.
Weak bar.
Knotty (r): 0.33 arcmin x 0.24 arcmin.
Several knotty arms with branchings.
Non-interacting pair with NGC 1666 at 15 arcmin.

16. 1963MCG3..C...0000V
Re:MCG -01-13-013
According to vB - Sb*II:.

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