Date and Time of the Query: 2019-04-21 T08:10:10 PDT
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Notes for object NGC 7679

12 note(s) found in NED.

1. 2007A&A...461.1209D
Re:NGC 7679
NGC 7679: BeppoSAX data were previously published in Risaliti (2002).
The present analysis confirms the results presented in that paper. The
X-ray spectrum of the source is almost featureless above 2 keV. Here the
marginal (~97% confidence level) detection of a FeK{alpha} emission line
at E = 7.1 +/- 0.4 keV is reported, and, if confirmed, it should arise
from ionized matter.

2. 2002AJ....124..675C
Re:UGC 12618
Seyfert 2. The 8 arcssec FWHM diffuse radio source (Condon et al.
1990) may be primarily powered by star formation.

3. 2002A&A...386..379R
Re:NGC 7679
NGC 7679: this source is peculiar within our sample, for it is
the only one with negligible X-ray absorption. The optical
classification (pure Seyfert 2) suggests that the BLR emission is
obscured by dust by at least 3-4 mag. This, assuming a galactic
dust-to-gas ratio, would imply an absorbing column density of at
least 6-7 x 10^21^ cm-2. We can explain this discrepancy in two ways:
a) the dust-to-gas ratio could be much higher than galactic, or the
dust could be associated to a warm absorber; b) there could be
a "hole'' in the absorber of the nuclear source, so that the X-ray
emission from the accretion disk is unabsorbed, but the broad lines,
emitted by the larger Broad line Region, are obscured. This scenario
is not unplausible, given the recent evidence of a complex structure
in the Seyfert 2 absorbers (Risaliti et al. 2002). Both the fits with
and without the reflected component are acceptable (see Tables 4 and
5). In our analysis the best reduced {chi}^2^ is obtained with a steep
{GAMMA}~2.1 power law plus a strong reflected component. However, in
a recent study of the same data, Della Ceca et al. (2001) propose a
best fit model in agreement with the one in Table 4, without
reflection, and with a photon index {GAMMA}~1.75.

4. 1996AJ....112..937D
Re:NGC 7679
14: NGC 7679 (S0). Arecibo fluxes of 2.5-6.1 Jy km s^-1^ were listed, while
fluxes of 9.8-10.5 Jy km s^-1^ were reported at Green Bank and Effelsberg and
14.3 Jy km s^-1^ at the Green Bank 140 foot. Two other galaxies are nearby:
NGC 7682 (Sab) at ~4', which also exhibits discrepant flux measurements, and
UGC 12628 (Sc) at ~11'. The higher flux measurements for NGC 7679 appear to be
confused primarily by NGC 7682. The profile of NGC 7679 is peculiar, and may
be somewhat confused even in the Arecibo measurements. The separation from
NGC 7682 would normally be sufficient to avoid confusion within the Arecibo
beam, however the maps suggest that the H I around NGC 7682 may be slightly
extended. The discrepancies appear to be caused mostly by confusion of the two
galaxies in the large-beam observations.

5. 1994CAG1..B...0000S
Re:NGC 7679
Sep 2/3, 1980
12 min
NGC 7679 forms a pair with NGC 7682
(SBa), at 268" separation. The direction of NGC
7682 relative to the print here is to the right and
slightly down, at about a position angle of 3:30
o'clock. The distance of NGC 7682 (not in the
RSA) from NGC 7679 is about four times the
apparent diameter of the main body plus the
plume of NGC 7679 shown in the print. However
NGC 7682 is not distorted or abnormal. It has a
symmetrical SBa(s) morphology with well-defined,
tight, relatively smooth arms.
However, NGC 7679 is abnormal. Its
smooth outer arms envelop an inner region of
high surface brightness which contains many
knots, suggesting a high, current star-formation
rate and therefore the Sb or Sc type. There are
two oppositely directed smooth plumes characteristic
of a tidal interaction.
NGC 7679 and NGC 7682 undoubtedly
form a physical pair. The redshifts are v_o(7679)
= 5397 km/s from the RSA2, and v_o(7682)
= 5333 km/s from the compilation by
Huchtmeier and Richter (1989). The redshift
distance of 107 Mpc (H = 50) gives a projected
linear separation of 139 kpc, suggesting that a
tidal interaction might have occurred in the past,
yet the form of NGC 7682 is regular. Perhaps the
plume in NGC 7679 is not caused by tides but is
endemic to the galaxy itself.
The morphology of NGC 7679 is similar to
that of NGC 4580, above; hence the mixed
classification is required for the same reasons.

6. 1994CAG1..B...0000S
Re:NGC 7679
Pair [with NGC 7682]
Sep 2/3, 1980
12 min
NGC 7679, also illustrated in the Sa section
(panel 86), forms a physical pair with NGC 7682
(SBa) at a separation of 4.5'. The redshifts are
v_o(7679) = 5397 km/s and v_o(7682) = 5333 km/s.
At the mean redshift distance of 107 Mpc
(H = 50) the projected linear separation is 139
The smooth outer arm that is pulled out on
one side of NGC 7679 may be due to a tidal
encounter with NGC 7682. However, the
morphology of NGC 4682 is undistorted.

7. 1993AJ....106.1405P
Re:NGC 7679
NGC 7679. A peculiar SB0 galaxy showing tidal distortion because of
interaction with a faint companion about 1' east, our H{alpha} image
[Fig. 4(b)] reveals a luminous nuclear star-formation complex resolved
into bright clumps of emission with an apparent spiral-like spur running
off toward the southwest to west. The brightest circumnuclear H II
complex has essentially round outer isophotes with a 3{sigma} above-
background isophote diameter of 18" (0.22 D_0_). The nucleus has a strong
H II regionlike spectrum (Dahari 1985), and like NGC 632 is an example of
a nuclear starburst with considerable circumnuclear star formation.

8. 1976RC2...C...0000d
Re:NGC 7679
= MRK 0534
In Arp 216 = VV 329
Faint extensions with brighter condensations.
Interacting (?) pair with NGC 7682 at 4.5 arcmin.

9. 1973UGC...C...0000N
Re:UGC 12618
VV 329, Arp 216
SB0 pec: (de Vaucouleurs)
In Arp's class "galaxies with adjacent loops"
Paired with UGC 12622 at 4.6, 74
"Patches north disturbed spiral, emission strong" (Arp)

10. 1964RC1...C...0000d
Re:NGC 7679
Extremely bright nucleus in a faint lens: 0.5 arcmin x 0.5 arcmin with dark
material or a faint (r). Faint bar or tidal extensions.
Non-interacting (?) pair with NGC 7682 at 4.5 arcmin.
Heidelberg Veroff. Vol. 9, 1926 dimensions are for the lens only.

11. 1959VV....C...0000V
Re:VV 329a
= NGC 7679
V = +5,378 km/sec, V = +5,278 km/sec.

12. 1956AJ.....61...97H
Re:NGC 7679
HMS Note No. 221
This highly concentrated nebula has an early-type continuum with
strong hydrogen absorption lines.
The emission lines are {lambda} 3727, H{beta}, and NI of [O III].

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