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Notes for object NGC 7674

16 note(s) found in NED.


1. 2007AJ....134..648M
Re:NGC 7674
NGC 7674 (Figs. 7.70, 8.10, 9.70, 20.70): This is an obvious spiral structure
with many star-forming regions. The nucleus is very bright and embedded in
extended diffuse emission and surrounded by an arc of star formation.

2. 2007A&A...461.1209D
Re:NGC 7674
NGC 7674: The X-ray spectrum of the source is reflection dominated as
reported in Malaguti et al. (1998) with the reflection component
dominating at energies above ~2 keV. The FeK{alpha} emission line
(EW ~ 360 eV) is not as extreme as in other Compton-thick sources where
it reaches ~ 1. 0 keV. Nonetheless, the broadband (2-100 keV) continuum
is significantly better described by the reflection continuum rather
than a power law ({DELTA}{chi}^2^ ~ 40 for two extra parameters of
interest).

3. 2006A&A...457...61R
Re:NGC 7674
NGC 7674. Classified as a Seyfert 2 (Osterbrock & Dahari 1983), NGC
7674 is a CfA galaxy (Huchra & Burg 1992) in interaction with UGC 12608
(Levenson et al. 2001). NGC 7674 displays broad emission in polarized
lines, which were first detected in this object by Miller & Goodrich
(1990). The extremely bright nuclear point source compared to the other
Seyfert 2 galaxies (with the exception of NGC 1068) reinforces its
interpretation as an obscured Seyfert 1. Our NIR spectrum is ambiguous
regarding the classification of this source. It is a Seyfert 2 because
of the absence of O I and Fe II. However, most H I lines display a
conspicuous broad component, particularly strong in Pa{alpha} and
Br{gamma}, where it reaches an FWHM of ~3000 km s^-1^. This width is
similar to the one detected in polarized light for H{beta} (Tran 1995).
Note that the peak of the broad component is blueshifted relative to
the systemic velocity of the galaxy by ~480 km s^-1^ in Pa{alpha} and
~300 km s^-1^ in Br{gamma}. Such a shift, of lower value (~100 km
s^-1^), is also found in the polarized broad component reported by Tran
(1995). Veilleux et al. (1997) suggests that the broad component is not
associated to the classical BLR because it is similar in width to the
one found in [O III] 5007 Angstrom. We checked the [S III] 9531 line,
and indeed it has a blue wing, well-fitted by a broad component of
~1550 km s^-1^, half the value found in Pa{beta}. Other lines, such as
[Fe II] 1.257 microns, display a similar component to that of sulfur.
We therefore conclude that we are looking at a genuine BLR feature in
NGC 7674. The continuum emission of this object is peculiar. It is
nearly flat from the blue end up to ~1.2 microns. Redwards, it
increases with wavelength, with a shape very similar to that found in
Mrk 1239 and Mrk 766. In addition, NGC 7674 shows large polarization,
supporting the hypothesis that the excess of NIR continuum emission in
H and K are very likely du e to hot dust.

4. 2003ApJS..148..327S
Re:NGC 7674
5.60. NGC 7674
This Seyfert 2 galaxy was observed to have polarized broad emission
lines by Miller & Goodrich (1990). The radio emission was studied by
Unger (1988), Neff & Hutchings (1992), and Kukula et al. (1995), who
found a double source separated by ~0.5" along P.A. = 117^deg^ and a
smaller component to the east of the nucleus. Ground-based
spectroscopy shows young stars around the nucleus of this galaxy
(Gonzalez Delgado, Heckman, & Leitherer 2001). The HST [O III] image,
presented in the bottom right panel of Figure 14, is extended by 4.4"
(2480 pc) along P.A. = 120^deg^, which is a direction similar to that
of the extended radio emission, and 2.7" (1520 pc) along the
perpendicular direction. One can also see in this image, at 1.3" to
the NW of the nucleus, along the host galaxy major axis, a small loop
and a hole in the emission.

5. 2003ApJS..146..353M
Re:NGC 7674
NGC 7674 (GD)
There are two clear dust lanes entering the circumnuclear region from
the large-scale bar, yet the great distance and bright nuclear point
source make it difficult to resolve dust lanes in the central
kiloparsec, although they appear to have a slight curve at the
smallest radii observable.

6. 2002AJ....124..675C
Re:UGC 12608
Seyfert 2.

7. 2001ApJS..133..269L
Re:NGC 7674
5.14. NGC 7674
NGC 7674 is interacting with UGC 12608, located 17 kpc (32") toward the
northeast. This galaxy exhibits broad lines in polarized light (Miller &
Goodrich 1990; Tran 1995a). NGC 7674 was observed with the PSPC for only
3 ks. The best fit to these limited data is a power law, with
{GAMMA} = 2.0_-1.3_^+0.72^. Although the measurement errors do not
constrain the extended fraction of soft X-ray emission well, this galaxy
is resolved, with R_kpc_ = 45.

8. 2001ApJ...562..139M
Re:NGC 7674
NGC 7674. - Polarized, broad emission lines were first detected in this
object by Miller & Goodrich (1990). The extremely bright nuclear point
source compared to the other Seyfert 2 galaxies (with the exception of
NGC 1068) reinforces its interpretation as an obscured Seyfert 1. The
elliptical isophotes are a reasonable match to the surface brightness
distribution of this galaxy outside the immediate influence of the nuclear
source.

9. 2000MNRAS.318..173M
Re:NGC 7674
2.5 NGC 7674
This source has been analysed and discussed by Malaguti et al. (1998). As
for NGC 1068, the nucleus is completely hidden at all energies, which
implies a column density >~ 10^25^ cm^-2^. The emission above a few keV is
dominated by a cold-reflection component, and the evidence for ionized
reflection is scanty. The apparently broad iron line can actually be
fitted by a blend of K{alpha} and K{beta} fluorescent lines.

10. 1999ApJ...516...97N
Re:Mrk 0533
Mrk 533 (NGC 7674): RC3 lists log R_25_ = 0.04 and does not give a
major axis P.A. A major axis P.A. of 150^deg^, which appears to be the
P.A. of the brighter isophotes, is derived by G. Paturel & C. Petit
(private communication to LEDA). The fainter isophotes are more circular
and are affected by a nearby companion to the northeast.

11. 1997ApJ...477..631V
Re:MRK 0533
MRK 533 = NGC 7674 - Spectropolarimetry of NGC 7674 reveals broad
H{alpha} emission with FWHM = 2830 km s^-1^ in polarized light (Miller &
Goodrich 1990; Tran 1995a). The optical emission lines of this object are
well known to present remarkable blue wings extending up to velocities of
2000 km s^-1^ with respect to the peak velocity (see, e.g., Veilleux
1991a). Our infrared spectra of this object are presented in Figures 2h
and 2i. The profiles of both Pa{beta} and Br{gamma} are characterized by
a narrow core superposed on a broad base blueshifted with respect to the
narrow core. Ruiz et al. (1994) arrived at a qualitatively similar result
for He I{lambda}1.083 and Pa{beta}.
To disentangle the true origin of the broad base in the infrared line
profiles, it is important to note that the profiles of Pa{beta} and
Br{gamma} are similar to that of [O III]{lambda}5007 (Veilleux 1991a,
1991b). These results suggest that the broad component in the profiles of
Pa{beta} and Br{gamma} represents emission from a NLR rather than from a
genuine high-density BLR (in which [O III]{lambda}5007 is collisionally
de-excited). Veilleux (1991c) has argued that the spectacular blue wing
in the line profiles of Mrk 533 is produced by gas of high ionization.
This explanation is also consistent with the fact that the extended blue
wing is not apparent in the profiles of the low-excitation lines
[Fe II]{lambda}1.2567 and H_2_{lambda}2.121.
The fluxes listed in Table 3 were derived by fitting the profiles with
the sum of a Gaussian and a Lorentzian, both with the same FWHM and the
same peak strength. The NLR reddenings determined from Pa{beta}/H{beta}
and Br{gamma}/H{beta} are larger than the reddening determined from the
Balmer decrement, perhaps a sign that the infrared lines are probing
deeper column depths than the Balmer lines.

12. 1996ApJ...465..191M
Re:NGC 7674
3.9. NGC 7674
Images of NGC 7674 at 11.7 microns and 8.8 microns are shown in Figures 15 and
16, respectively. The galaxy is unresolved at both wavelengths (Fig. 19).
The radio map by CHSS with a 1.5" beam may be slightly resolved at the 0.5"
(360 kpc) level, although this may be pushing the limits of the observation.
Optical maps show the galaxy to be interacting with UGC 12608, located 32"
(17 kpc) to the northeast. The galaxy has an asymmetric spiral structure with
a tail (Hutchings & Neff 1991; Fig. 1).

13. 1996AJ....111..712H
Re:MRK 0533
2325+085 (Mkn 533). This is another higher redshift object, comparable with
0148+223. The galaxy is a face-on spiral with asymmetrical arms, and a tidal
connection to a nearby compact elliptical galaxy. The elliptical has a red
"shell" on the side nearest to the main spiral. The galaxy has a weak and
slightly extended nuclear radio source. There are a few bright knots inside
the disk, and even fewer outside it. The background is smooth and the knots do
not have any blending.
DAOPHOT found very few faint objects to measure in this galaxy, unlike the
other high redshift object (0148+223). The objects measured lie within the
distributions seen in the H-R diagrams of the other galaxies, but only along
the upper luminosiry edge.

14. 1995MNRAS.276.1262K
Re:MRK 0533
Markarian 533: (NGC 7674, VV343, Arp 182). Type 2. Host galaxy: SBb
(UGC). Radio: the slightly extended C-array object is resolved into a
0.5-arcsec double source by the A-array image, consistent with the
structure seen at 20 cm with MERLIN (Unger et al. 1986).

15. 1976RC2...C...0000d
Re:NGC 7674
= MRK 0533
= Arp 182
= VV 343
Compact elliptical companion attached at 0.5 arcmin north-following.
NGC 7675 is 2.2 arcmin following.
Spectrum:
Astrofizika, 10, 485, 1974 (possibly a weak Seyfert).
Radio Observations:
M.N.R.A.S., 167, 251, 1974.

16. 1973UGC...C...0000N
Re:UGC 12608
VV 343
Listed as NGC 7675 in MCG, which is incorrect
Paired with b) at 0.6, 64, 0.20 x 0.15
23 25.5 +08 29 = NGC 7675 at 2.5, 105, 0.5 x 0.3, E, m=14.8
Companion 3.7, 250, 0.4 x 0.2


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