Date and Time of the Query: 2019-06-19 T20:32:33 PDT
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Notes for object IC 3639

16 note(s) found in NED.

1. 2009A&A...502..457G
Re:IC 3639
A.2.4 IC 3639 The intrinsic high-energy flux from this source is likely to be
completely depleted by heavy Compton-thick obscuration with N_H_ > 10^25^ cm^-2^
(e.g., Risaliti et al. 1999). Analysis is complicated by most of the <10 keV
observed X-ray flux probably being related to extended emission (Guainazzi et
al. 2005b; Ghosh et al. 2007). Using instead the [O III] {lambda}5007 emission
line (F_[O III]_ = 3.4 x 10^-12^ erg s^-1^ cm^-2^ from Lumsden et al. 2001,
corrected for extinction) as a proxy for the intrinsic power (in conjunction
with the [O III]:X-ray relation from Panessa et al. 2006) gives L_2-10_ ~ 4 x
10^43^ erg s^-1^. This also matches older [O III] measurements quoted by
Guainazzi et al. (2005b), if we correct for extinction using the prescription of
Bassani et al. (1999).

2. 2007AJ....134.1061D
Re:TOLOLO 1238-364
This object has been classified as a Seyfert 2 galaxy (NED), but there does seem
to be evidence for a broad-line region in the FUSE spectrum. We find one broad
component that shows some contamination from H_2_, Ar I, and C I. Because this
has been labeled as a Seyfert 2 galaxy, it seems this object has not been
considered as a target for intrinsic absorption studies.

3. 2007A&A...461.1209D
Re:IC 3639
IC 3639: The BeppoSAX data were not published before. The statistics are
low thus the best-fit model is simply composed of a power law plus a
Gaussian line in emission. No intrinsic absorption is required by the
data (N_H_<=5.43 x 10^22^ cm^-2^, 90% confidence). Nonetheless a huge
FeK{alpha} is detected (EW~2 keV). This line is most probably due to
cold iron (E=6.4+/-0.2). The spectra is rather flat ({GAMMA}=1.5 +/-
0.1), but not as extreme as expected for reflection-dominated sources (
{GAMMA}~0-0.5, as is the case of NGC 1068 in the 2-10 keV band, Matt et
al. 1997). The line EW, however, strongly indicates that the source is
Compton-thick but while its centroid indicates that it is produced in
cold material, the slope of the X-ray continuum indicates a possible
reflection from warm material. To conclude, as for NGC 2273 (see above),
it is not clear if the X-ray spectrum of the source below 10 keV is cold
reflection or warm scattering dominated, while its Compton-thick nature
is most probable.

4. 2002ApJS..143...47D
Re:IRAS 12381-3628
IRAS 12381-3628 (IC 3639).---This galaxy has two companions; a ring
galaxy 1<8 to the northeast, and an edge-on galaxy 2.6' to the
northwest (Morganti et al. 1999). According to our H{alpha} image, the
H{alpha} emission in IC 3639 is spread throughout the disk in numerous
knots. The H{alpha} emission in the ring galaxy occurs both in the ring
and in two knots in the nucleus. A strong H{alpha} nucleus is observed
in the edge-on galaxy. The western side of the edge-on galaxy is only
seen in the red continuum image. We classified IC 3639 previously as a
Seyfert 2 (Kewley et al. 2001b), confirming its previous classification
of Seyfert 2 by many authors including de Grijp et al. (1992), Norris
et al. (1988), and Contini & Viegas-Aldrovandi (1987). However, it is
clear that this active nucleus does not dominate the H{alpha} emission
on the large scale.

5. 2002A&A...389...68G
Re:IC 3639
IC 3639: this is a nearly face-on galaxy in a small group. The
catalog of HII regions is quite irregular and does not show any
spiral structure. We adopt the values from our second method,
which are in agreement with the PA of Hunt et al. (1999) and the
average IA of all methods. Note, however, that there is a lot of
dispersion around the mean values, which could mean that our
estimate is not very safe.

6. 2001MNRAS.327..459L
Re:IC 3639
IC3639: This galaxy has been studied in detail in the optical and
ultraviolet by Gonzalez Delgado et al. (1998) and Gonzalez Delgado,
Heckman & Leitherer (2001). They find evidence for a recent burst of star
formation in the nucleus which contributes an equal amount to the AGN
component to the overall bolometric luminosity. The starburst does not
dominate the optical continuum however, since an older population
contributes a larger fraction of the light.

7. 2001ApJS..133..269L
Re:IC 3639
5.5. IC 3639
IC 3639 has a bar (Mulchaey, Regan, & Kundu 1997) and is paired with
ESO 381-G9. We excluded the low-quality SIS1 data from the spectral
fitting. The remaining data are best fitted with a two-component model of
a power law and thermal emission. The thermal temperature is high,
kT = 2.3 keV. In this case, all the soft X-ray emission is thermal. The
three-component model, including the scattered power law, also fits the
data. In this case kT = 1.7 keV, but the improvement to the fit with
inclusion of additional parameters is not statistically significant. The
X-ray emission is extended in the HRI data, with a radius of 6.8 kpc.

8. 1999A&AS..137..457M
Re:IC 3639
TOL 1238-364 (IC 3639): In our 3 cm map the source is unresolved.
TOL 1238-364 object was observed at 20 and 6 cm by Ulvestad & Wilson
(1989). At 20 cm the source appears to have a diffuse emission around a
relatively strong core. At 6 cm only the core of the source was
detected. Ulvestad & Wilson (1989) find a 6 cm flux of 13.6 mJy which
combined with our data gives a spectral index of {alpha}_6_^3^ = -0.53.
A core of 13 mJy was detected with the PTI at 13 cm (R94).

9. 1998ApJ...505..174G
Re:IC 3639
IC 3639 has a near-IR bar aligned at P.A. = 150^deg^ (Mulchaey et
al. 1997). In the digital sky survey IC 3639 has two companions: a ring
galaxy 1.8' (22 kpc) to the northeast, and an edge-on galaxy 2.6' (33 kpc)
to the northwest. The radio map at 20 cm shows a strong core embedded in
diffuse emission, but at 6 cm only the core is detected (Ulvestad &
Wilson 1989). The excitation ratio [O III]/H{beta} is equal to 7.8
(Whittle 1992b), and conspicuous [Ne V] and He II are also present.

10. 1997ApJS..110..299M
Re:IC 3639
Bar is visible in both the ellipse fits and the K_S_image.

11. 1997ApJS..110..299M
Re:IC 3639
Bar is visible in both the ellipse fits and the K_S_image.

12. 1996ApJS..103...81C
Re:IC 3639
IC 3639.--Seyfert 2. Pair with ESO 381-G009 at optical position
{alpha} = 12h38m16.1s, {delta} = -36^deg^27'28" (van den Broek 1991) with
1.425 GHz flux density S = 10.7 mJy. Medium-resolution VLA map at 1.49 GHz in
Ulvestad & Wilson (1989).

13. 1993ApJS...86....5K
Re:IC 3639
IC 3639; SBb, Seyfert 2.
This nearby Seyfert 2 galaxy possesses a strong radio core embedded in
diffuse emission, and has a very high surface brightness, so that it
resembles NGC 1068, the prototype Seyfert 2 galaxy (Ulvestad & Wilson
1989). The narrow [O III] {lambda}5007 emission line has a blue asymmetry
similar to those seen in NLRGs (Heckman, Miley, & Green 1984), while no
such asymmetry is seen in H{beta} (Fairall 1985). The UV spectrum is
flat, with some weak emission lines (and an emission artifact at
1663 A).

14. 1985SGC...C...0000C
Re:IC 3639
Plate 2339
Overexposed center, very bright bar and (r): 0.5 x 0.45. Star 0.6 south-
preceding. 1st of 3. Interacting pair with 1238-365 1.8 north-following.
Sb:sp 2.5 north-preceding.

15. 1985SGC...C...0000C
Re:SGC 123811-3629.0
Plate 2339
Overexposed bar, many extremely bright knots; star superposed 0.4 following.
Interacting pair with IC 3639 1.8 south-preceding.

16. 1982ESOU..C...0000L
Re:ESO 123811-3629.0
=ESO 381- G 08
brightest in trio

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