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Notes for object IC 0342

21 note(s) found in NED.


1. 2008ApJ...679..310G
Re:IC 0342
The morphology of the PAH emission (Fig. 21) follows the ^12^CO(J = 1 ->
0)_2.6mm_ emission, which traces out the nuclear ring and ridge associated with
the stellar bar (Sakamoto et al. 1999). The spectra of this galaxy are much
noisier than those of M82. The correlations are very well defined, with a linear
correlation coefficient of ~= 0.8 (Table 2). The deviation of the relation
involving the 8.6 micron feature with the Lorentzian method (Fig. 19, middle
right panel), compared to the general correlation, is due to a systematic
overestimation of the attenuation in the central region. The average centroid of
the 7.7 {mu}m feature is identical for IC 342 and M82 ({lambda}_7.7_) ~= 7.68
microns;Table 2).

2. 2007MNRAS.382.1552L
Re:IC 0342
IC 342: NIR and molecular gas observations show a young nuclear stellar cluster,
a small-scale nuclear stellar bar, and a star-forming ring at the Inner Lindblad
Resonance (ILR) of the bar with a radius of only 50 pc (Boker et al. 1997; Meier
& Turner 2001). The nuclear star-forming ring is partially seen in our V/I
image. A nuclear stellar cluster lies at the centre of the ring and is clearly
seen in Fig. 2. In the optical we also see two bright blue regions to the north
and south of the nucleus which are located within the stellar bar. The positions
of the three central radio peaks marked in Fig. 2 were measured from the 6-cm
map in fig. 1 of Turner & Ho (1983), as positions are not given in the paper.
Spectra were acquired of the nucleus and the southern blue region. After
correcting for foreground extinction, the spectra appear very blue. Our
population-synthesis analysis shows that the nuclear stellar cluster is not
older than 100 Myr and the blue southern region is only 1 Myr old. The Balmer
decrement suggests significant intrinsic extinction. This is confirmed by IR
observations (Boker et al. 1997).

3. 2005MNRAS.360.1201H
Re:IC 0342
IC 0342. This large SAB(rs)cd nearby galaxy is nearly face-on so its
photometrical PA is uncertain. A strong difference between its kinematical and
photometrical inclination is noted. Observations in CO and H i (Crosthwaite et
al. 2000) suggest that its kinematical PA is 37{degrees}. The kinematical data
from CO, H i and H{alpha} are comparable. An H{alpha} spiral structure near the
centre can be seen.

4. 2005ApJS..157...59L
Re:IC 0342
PGC 13826 (IC 342) is a face-on Scd spiral at a distance of 3.9 Mpc with a
very bright nucleus and weak surface brightness spiral arms. Three ULXs are all
on spiral arms. ULX1 is close to but not the second nuclear source. ULX2 was
highly variable during the 2 day HRI observation. ULX3 (IXO 22) is coincident
with a tooth-shaped nebula (PM2002) and is quite variable and showed spectral
state transitions reminiscent of black hole candidates during ASCA observations
(Kobuta et al. 2001).

5. 2005A&A...436...75H
Re:IC 0342
3.5 IC 342 and NGC 2146
We also observed the previously detected H_2_O maser sources IC 342 and
NGC 2146. IC 342 was not detected in June 2001 and March 2002,
indicating that the flaring component observed at V_LSR_ ~ 16 km s^-1^
(Tarchi et al. 2002a) has been quiescent since June 2001. Spectra from
NGC 2146, obtained in March 2002, show no significant variations with
respect to profiles observed two years earlier (see Tarchi et al.
2002b).

6. 2004MNRAS.349.1193R
Re:IC 0342
4.2.1 CXOU J034555.7+680455 (IC 342 X-1) This ULX showed a fairly
constant X-ray spectrum between the two observations, with an absorbed
power-law continuum providing a good fit to the data from both
epochs. In each case the absorption was roughly twice the foreground
value (cf. Table 2), with the additional absorption of 2-3 x 10^21^ atom
cm^-2^ in excess of the integrated column through IC 342 at the ULX
position (~8 x 10^20^ atom cm^-2^; Crosthwaite, Turner & Ho 2000). This
implies a source of additional absorption intrinsic to, or in the
environment of, CXOU J034555.7+680455. This may originate in the nebula
surrounding this ULX described by Roberts et al. (2003). The Chandra
spectra are consistent with the low/hard spectral state observed by ASCA
in 2000 February 24-March 1, described by an absorbed power-law
continuum with NH= 0.64+-0.07 x 10^22^ atom cm^-2^ and {GAMMA}=
1.73+-0.06 (Kubota et al. 2001). This state has also been interpreted as
an anomalous/very high state (Kubota, Done & Makishima 2002), which we
discuss further in Section 5.1. The luminosity also appears little
changed at ~5 x 10^39^ erg s^-1^ (versus 6 x 10^39^ erg s^-1^ in ASCA)
when extrapolated to the 0.5-10 keV band. Hence, it appears that this
ULX has been in a constant spectral state in three separate observations
over 2.5 yr.

7. 2004MNRAS.349.1193R
Re:IC 0342
A1 IC 342 X-1 (CXOU J034555.7+680455) This ULX was first detected in an
Einstein IPC observation of IC 342, with a 0.2-4 keV X-ray luminosity of
3 x 10^39^ erg s^-1^ (Fabbiano & Trinchieri 1987). A subsequent ROSAT
HRI observation detected IC 342 X-1 in a similarly luminous state
(Bregman, Cox & Tomisaka 1993; RW2000) . An early ASCA observation
showed IC 342 X-1 to be in a very luminous, highly variable state in
which its average 0.5-10 keV luminosity surpassed 10^40^ erg s^-1^ and
it displayed large-amplitude variability on ~1000 s time-scales (Okada
et al. 1998). In this state its X-ray spectrum was well fitted by the
multicolour disc blackbody model describing an accretion disc around a
black hole in a high/soft state (Makishima et al. 2000). However, a
follow-up observation obtained late in the ASCA mission showed the ULX
to have dimmed to a luminosity of 6 x 10^39^ erg s^-1^ and undergone a
spectral transition to a low/hard state, similar to the behaviour
observed in many Galactic and Magellanic black hole X-ray binary systems
(Kubota et al. 2001; Mizuno et al. 2001). However, the low/hard spectral
state has recently been reinterpreted as a high/anomalous state where
the X-ray spectrum is described by a strongly Comptonized optically
thick accretion disc, as observed in many Galactic black hole X-ray
binaries experiencing a high mass accretion rate (Kubota et
al. 2002). Finally, recent William Herschel Telescope integral field
unit observations have revealed that this ULX lies at the centre of a
large nebula, probably a supernova remnant shell (Roberts et al. 2003,
and references therein). The inferred initial energy input to the
supernova remnant is consistent with a hypernova event and highly
excited (O III) emission-line regions on the inner edge of the shell
suggest that the ULX is photoionizing its inner regions to produce an
X-ray ionized nebula.

8. 2004A&A...419..501F
Re:IC 0342
IC342 - We adopted an aperture of 17" x 17" corresponding to the size
of the Br{gamma} line map provided by Boker et al. (1997), which
encompasses the circumnuclear starburst ring. This aperture is close to
the intrinsic size of the mid-IR source fitted on the surface brightness
profiles, between 19" and 22". The areas agree to within 30%, and the
MIR fluxes to within 9% in the different apertures. We combined the
Br{gamma} flux integrated over the map with the Br{alpha} flux of Verma
et al. (2003) obtained in the 14" x 20" SWS beam (excluding their
Br{beta} measurement because of possible contribution from the H2 1-0
O(2) line and Pf{alpha} because of larger uncertainties on the
extinction law near 7 {micron}). Fits assuming a UFS and a mixed model
are both well constrained, and the derived extinctions imply nearly
identical Q_Lyc_ (within 1%).

9. 2002AJ....124.2581S
Re:IC 0342
IC 342 (see Fig. 6): IC 342 has a small, oval stellar bar.
The bar ellipse shown in Figure 6 is at a P.A. of 28^deg^.
The CO emission appears to be in the center of the bar
with a P.A. of ~0^deg^-10^deg^. This central distribution
of gas is unusual because it is expected only when the bar
is extremely strong and inner Lindblad resonances are
absent (Athanassoula 1992b). Such a situation is extremely
short-lived in the models. It is more likely that the bar
parameters for this galaxy are misidentified because the
bar resides in a bright starburst circumnuclear region. A
recent study by (Crosthwaite et al. 2001) suggests that,
although the bar is most prominent in the central 2', CO
kinematics indicate a gaseous bar as long as 4.7' with
P.A. 0^deg^. In that case the CO emission would be on the
leading edge of the bar.
As in other bars the CO emission along both dust
lanes decreases in intensity outward from the circumnuclear
region, toward C2 to the north and C4 to the south. In the
northern half of the bar there is an extension of CO,
labeled "C1," toward the trailing side. A few arcseconds
north of it is an H II region, labeled "H1," which also
lies along the leading edge of the CO emission. Farther
north near the bar end there is a CO emission peak,
labeled "C3." A few arcseconds north and east of C3 is
another H{alpha} peak, labeled "H2."
In the southern half of the bar there is a
concentration of CO emission, labeled "C5," on the
trailing side of the main lane of CO emission. There is
also a ridge of CO emission that extends southeast of the
nucleus toward the bar end, ending in a CO peak,
labeled "C6." In the bar there is a lot of diffuse H{alpha}
emission, but the few H II regions (H3 and H4) are on the
leading side of the CO ridge.

10. 2002AJ....124..675C
Re:UGC 02847
Very extended and lumpy radio source; the 1.4 GHz flux density is from
Condon & Broderick (1988).

11. 2001ApJS..137..139S
Re:IC 0342
The IC 342/Maffei 1 Group. - Krismer, Tully, & Gioia (1995) derive
Tully-Fisher distances to NGC 1560 and UGCA 105. The mean of these
measures gives a group distance of 3.6 Mpc. The best distance estimate for
NGC 1569 is that of Karachentsev et al. (1997), who derive a distance of
1.7 Mpc from bright stars. Krismer et al. (1995) find that NGC 1569
does not yield a plausible Tully-Fisher distance.

12. 2000MNRAS.319...17L
Re:IC 0342
IC 342: We have re-analysed the ROSAT HRI data already discussed by
(Bregman, Cox & Tomisaka 1993). They found evidence for a diffuse nuclear
component that could be explained as a hot interstellar medium generated by
a very young nuclear starburst.
Fig. 7 shows that three sources lie within the limits of the optical JKT
image of the galaxy. The brightest source is coincident with the nucleus,
and visual inspection of the image suggests that it is marginally resolved.
A comparison of the azimuthally averaged profile of the source and the HRI
model PSF can be seen in Fig. 30, and a clear deviation from the model PSF
is visible at a radius of between 7 and 13 arcsec from the centre. For
comparison, an off-nuclear source is also shown, which is in good agreement
with the model PSF, confirming the diffuse nuclear component.
X3 is located close to a faint knot of optical emission, while X1 has no
obvious optical counterpart. Notice, however, that only one source was used
to check the astrometry of this observation (Section 3.2.2). X1 has an S/N
ratio of 2.3 (see Table 4), but is included here because it was reported by
Bregman et al. (1993) (they found an S/N ratio of 2.8, probably due to a
different background estimate).
Fabbiano & Trinchieri (1987) analysed Einstein IPC observations of the
nuclear region in IC 342, and argued that the emission is consistent with
starburst activity. Unfortunately, the IPC was not able to resolve the
three sources detected with the HRI.

13. 1999ApJS..124..403S
Re:IC 0342
5.1. IC 342
The data for IC 342 are taken from Ishizuki et al. (1990a), which
contains channel maps in addition to the moment maps. The ridges of
molecular gas caused by a stellar bar, and a nuclear ring associated
with a starburst ring, are discussed in their paper. The central gas
ring of ~ 100 pc diameter is a good example of small gas holes at
galactic centers. The central gas hole would not be evident if IC 342,
the nearest galaxy in our sample, were as distant as other galaxies in
the sample (D ~ 15 Mpc). This galaxy has been observed by several groups
in various molecular lines (Lo et al. 1984; Ho et al. 1990;
Turner & Hurt 1992; Downes et al. 1992; Wright et al. 1993;
Turner, Hurt, & Hudson 1993).

14. 1999ApJ...519...89C
Re:IC 0342
IC 342.-IC 342 is a large, face-on spiral galaxy with a normal
galaxy nucleus. We found several compact X-ray sources in IC 342, one of
which was coincident with the galaxy nucleus. ASCA observations of IC
342 are unable to isolate the central X-ray source seen in the ROSAT HRI
image from other surrounding X-ray sources in the galaxy (Okada et al.
1994). However, Okada et al. (1998) suggest that another X-ray source
(not the most central one) in the central regions of IC 342 may be an
accreting BH of mass ~100 M_sun_.

15. 1996ApJS..103...81C
Re:IC 0342
IC 0342.--Maps at 0.327, 1.49, and 10.7 GHz in Hummel & Grave (1990).

16. 1996ApJ...458..120S
Re:IC 0342
IC 342
This is an almost face-on (i = 25^deg^) Sc galaxy at 3.9 Mpc distance. It has
been extensively studied in the CO line, and various PV diagrams have been
obtained (Young & Scoville 1982; Hayashi et al. 1987; Sage & Solomon 1991). A
rotation curve in the H I line has been obtained by Rogstad & Shostak (1972).
In this paper, we make use of PV diagrams observed with the NRO 45 m telescope
at a resolution of 15" (284 pc; Hayashi et al. 1987) and a 4" resolution
millimeter array PV diagram (Ishizuki et al. 1990a; Ishisuki 1994, private
communication). Figure 3 shows the obtained rotation curve for IC 342 using
the PV diagrams.
The rotation velocity increases almost rigidly in the innermost region at
R < 10" = 190 pc, and reaches V_rot_ ~ 130 km s^-1^ at R ~ 15" (280 pc). Then
it increases gradually to reach a maximum of 190 km s^-1^ at R ~ 2'-3'
(2-3 kpc), followed by a flat H I rotation at 195 km s^-1^ (at 8 kpc) to
190 km s^-1^ (at 20 kpc).

17. 1994AJ....108.2128C
Re:PGC 013826
PGC 013826 = IC 342. A_g = 3.05, B^o^_T_ = 6.04, HI = 2.20.

18. 1976RC2...C...0000d
Re:IC 0342
Brightest in the UMa-Cam Cloud,
possibly with Maffei 1 (= A0232+59) and Maffei 2 (A0238+59).
Photograph:
Publ. U.S. Naval Obs., XX, Part IV, 1971.
Astr. Ap., 29, 249, 1973.
Ap. J., 194, 559, 1974.
Photometry:
Publ. U.S. Naval Obs., XX, Part IV, 1971.
HII Regions:
Ap. J., 194, 559, 1974.
Distance Modulus:
Nature, 231, 35, 1971.
Ap. J., 194, 559, 1974.
HI 21cm:
Ap. J., 176, 315, 1972.
Astr. Ap., 22, 111, 1973.
IAU Symp. No. 58, 122, 1974.
Radio Observations:
Ap. J., 142, 1333, 1965.
Astr. Ap., 29, 249, 1973.
Possible Supernova Remnant:
Astr. Ap., 26, 105, 1973.
"Supernovae & SN Remnants", Ap. & Space Sc. Lib., Vol. 45, p.56, 1974.

19. 1973UGC...C...0000N
Re:UGC 02847
SAB(rs)cd (de Vaucouleurs)

20. 1964RC1...C...0000d
Re:IC 0342
Very bright nucleus. Weak pseudo (r): 4.1 arcmin x 3.7 arcmin. Extensive,
well resolved arms. Very similar to M101.
See also H[RC1] A105, 229, 1937.
Monograph:
H.B., 899, 16, 1935.
Photograph:
Hubble, Realm of the Nebulae, Plate 12, 1936.
L'Astronomie, 50, 26, 1936.
Spectrum:
A.J., 61, 97, 1956.
Zwicky, F., Morphological Astronomy, 153, 1957.
Radio Emission:
P.A.S.P., 72, 368, 1960.
M.N.R.A.S., 122, 479, 1961.
HI Emission:
A.J., 67, 313, 1962.

21. 1956AJ.....61...97H
Re:IC 0342
HMS Note No. 025
Early-type continuous nuclear spectrum with H{beta} in emission
and absorption lines nearly invisible.
The plate listed is the only one of four suitable for
measurement of redshift. The others are:
1941 Sept. 29.4, 4h, Ilf, 6 arcsec x 1 arcmin, 90 degrees.
Nuclear continuous spectrum that shows only H{beta} in weak emission.
1941 Nov. 19.3 8h, Ilf, 6 arcsec x 3 arcmin, 98 degrees.
1941 Nov. 22.3, 6h, Ilf, 6 arcsec x 6 arcmin, 35 degrees.
Slit on nucleus and oriented to cover several condensations
in the spiral. No emission lines show on these plates.
The probable absence of condensations having strong emission lines is
also indicated by a slitless grating spectrogram, kindly taken by
G. H. Herbig, which included the whole of this unusually large spiral
(Shapley, H., and Seyfert, C.K. 1935,
Bull. Astr. Obs. Harvard, No. 899, 16).


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