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Notes for object IC 4329A

19 note(s) found in NED.

1. 2009ApJ...690.1322W
Re:IC 4329A
IC 4329A. This source has complex absorption, studied most recently in
the XMM-Newton spectrum analyzed in Steenbrugge et al. (2005). They find
signatures from seven different absorbing systems.

2. 2008A&A...484..341R
Re:ESO 445- G 050
For this Seyfert I galaxy we measure 352 mJy at 11.9 micron. A 10.4 micron flux
of 640 mJy can be found at Siebenmorgen et al. (2004).

3. 2007A&A...461.1209D
Re:IC 4329a
IC 4329a: The source has been observed five times by BeppoSAX. Analysis
of the first (1996) and last (2000) observations may be found in Perola
et al. (1999), and in Gondoin et al. (2001) and Bianchi et al. (2004)
respectively. The other observations were published in Cappi et al.
(2001). Bianchi et al. (2004) speculated that a Compton-shoulder is
visible in the data collected simultaneously by BeppoSAX and XMM-Newton
in 2000. Overall, the spectrum of the source is almost steady,
independently of the flux state that varied by a factor of ~2 in the
period sampled by the observations. In few cases (see figures), the
FeK{alpha} emission line is best fitted with a mildly broad line (width
FWHM ~ 0.13), as was previously noted by Perola et al. (1999).

4. 2006ApJ...638..642B
Re:IC 4329A
IC 4329A - This source (Seyfert 1.2; z = 0.016) is well represented by a
power law (GAMMA = 1.5^+0.4^_-0.4_) with exponential cutoff (E_C_ =
104^+344^_-48_ keV; see Fig. 6). The results are consistent on a 2-3 s
level with the spectrum measured by BeppoSAX (GAMMA = 1.90 +- 0.05, E_C_
~= 300 keV; Perola et al. 2002).

5. 2004MNRAS.350.1049G
Re:IC 4329A
9.20 IC 4329A This has a partially obscured nucleus, very faint at
visible wavelengths (Winkler et al. 1992). There is a suggestion of a
delay of between 33 and 85 d between J and L.

6. 2004ApJ...613..682P
Re:IC 4329A
IC 4329A. This object and NGC 3227 were both observed in the CTIO
monitoring program (Winge et al. 1995, 1996). These observations
employed a Reticon detector, which yielded poorer quality spectra than
obtained with the CCDs used in virtually every other ground-based
campaign. We attempted to improve the original light curves by rescaling
the original spectra in flux by using the van Groningen & Wanders (1992)
algorithm and remeasuring the continuum and emission-line fluxes. This
did improve light curves and rms spectra, but only marginally. The light
curves are very poor, and the time-lag measurements should be regarded
with caution. The FWHM measurement is very poor (note the large
uncertainty yielded by our measurement algorithm). We have little
confidence in the mass determination for this object.

7. 2004A&A...422...65B
Re:IC 4329A
3.3.6 IC 4329A The simultaneous observation was already analyzed by
Gondoin et al. (2001). However their results are affected by an
incorrect value of the normalization factor between the MECS and the
PDS. The BMS gives an acceptable fit ({chi}^2^=263/207 d.o.f.), with
the inclusion of an edge at 0.72+-0.02 keV, this source being one of
those whose soft X-ray spectrum has been analyzed. The line width is
resolved, but its value is lower and only marginally consistent with
that measured by BeppoSAX (Perola et al. 1999,2002), while inconsistent
with the one found by ASCA (Done et al. 2000).
A Chandra observation, even if not simultaneous, was also analyzed to
better constrain the iron line width. Indeed, the HEG spectrum reveals
the presence of a double-peaked feature at 6.31^+0.02^_-0.01_ and
6.40+-0.02 keV, with EWs of around 20 eV each and detected at 2.5{sigma}
confidence level (see Fig. 3). The total flux of the two lines is
consistent with that found by XMM-Newton for the neutral iron line. If
this is the case, the only fully resolved iron line of our sample could
be the result of a blend of two lines. The line around 6.31 keV can be
one more example of relativistic features arising from an orbiting spot,
as already mentioned for ESO198-G024. Deferring the reader to Dovciak et
al. (2004) for details on the model, this feature could be the blue horn
of a r ~=10 annulus profile, provided an inclination angle slightly
smaller than 30deg. Note, however, that this is not the only
interpretation consistent with these data: McKernan & Yaqoob (2004)
suggested other possibilities, such as a single broad Gaussian line or a
relativistic feature arising in a nearly face-on disk. A line at
6.94^+0.05^_-0.06_ keV, consistent with emission from Fe XXVI, is also
present in the data, with an EW of ~= 30 eV and at a 2{sigma} confidence
level. This feature was also reported by McKernan & Yaqoob (2004).

8. 2002A&A...389..802P
Re:IC 4329A
IC 4329A. Observation (1) was published by Perola et al. (1999).
The average flux of observation (2) is 20% lower, yet there
are no statistically significant differences between the two
sets of parameters (the same holds for the three pointings
merged, when fitted individually, despite a 25% difference
between the lowest and the highest of their flux levels).
The mean values of the absorbers are:
N_s_ = (2.7 +/- 1.0) x 10^21^ cm^-2^,
N_W_ = (2.8 ^+1.2^_-1.0_) x 10^21^ cm^-2^ with
X_i_ ~ 5 erg cm s^-1^. The iron line is resolved. Given the
strength of the source (the brightest of the sample) and the
correspondingly good statistics, Perola et al. (1999) attempted
a fit with a narrow Gaussian plus a relativistic disk profile,
and obtained marginal evidence for the existence of the narrow
component. Another marginal detection of the narrow component
in a simultaneous ASCA and RossiXTE observation is presented
by Done et al. (2000). In a XMM-Newton observation with the
EPIC instrument (Gondoin et al. 2001), at a flux level 25%
higher than in observation (1), the narrow ({sigma} less
than 0.06 keV) line is detected, with W_{alpha} = 43 +/- 1 eV;
a broad component is seemingly absent, but unfortunately the
authors do not provide an upper limit on its equivalent
width. A simultaneous and relatively short (34 000 s in the
MECS) BeppoSAX observation is used, together with the EPIC
data, by Gondoin et al. (2001) to estimate {GAMMA} = 1.93 +/- 0.03
and R = 1.1 +/- 0.3: we believe that the estimate of R is
incorrect, because obtained with a PDS to MECS normalization
factor equal to an improbable value of 0.7; by fitting the
BeppoSAX data, as retrieved from the public archive, with this
factor equal to 0.86 (for FRT selection, see Sect. 2), we
obtain best fit values of R=0.54 and {GAMMA}=1.91, fully
consistent with those in Table 2.

9. 2001ApJ...550..261W
Re:IC 4329A
3.3.10. IC 4329a
This target has been observed on five occasions. The 2-10 keV flux
changes by ~25% (Fig. 8j). The line energy changes by less than 4%, but the
data are not sensitive enough to comment on changes in the EW or line flux.

10. 1999ApJS..120..209N
Re:IC 4329A
IC 4329A (type 1.2; Fig. 13) - The extension in P.A. ~75^deg^ in
the 20cm map is present before the self-calibration process. Higher
resolution 20 and 6cm maps of this source (Unger et al. 1987a) show a
diffuse 6" extension in P.A. ~285^deg^. There is another source in the
same field (8 mJy at 20cm) at {alpha} = 13^h^46^m^25.94^s^, {delta} =
-30^deg^02'25.4" (B1950.0). The source is suspected to be variable
(Unger et al. 1987a). The printed edition of RC3 lists an erroneous
host galaxy P.A. of 63^deg^, while the updated on-line version
(available at NED) lists the correct P.A. of 45^deg^.

11. 1998ApJS..114...73G
Re:IC 4329A
Section A12. IC 4329A
This Seyfert 1.0 galaxy was first detected in X-rays by Ariel V (Elvis et al.
1978). In our analysis of the data from ASCA observation performed in 1993
August, we find no model in Section 5 that satisfies our formal criteria for
acceptability. However, we do find a significant improvement in the fits for
models including ionized gas, with U_X_ ~ 0.02-0.04, N_H, z_ ~ 2 x 10^21^
cm^-2^, and {GAMMA} ~ 1.9 for all models B(i)-C(ii). A substantial column
density of neutral gas is also required for this source N_H_, 0 ~ 4 x 10^21^
cm^-2^, far in excess of N^gal^_H,0_, but consistent with previous findings
and the edge-on orientation of the host galaxy. Cappi et al. (1996) and R97
have both performed independent analyses of this ASCA data set. Both find the
addition of two edges to a single-power-law model ({GAMMA} ~ 1.9)
significantly improved the goodness of fit over the 0.6-1.0 keV band. R97
fixed the edge energies to those appropriate for O VII and O VIII and found
{tau}_O7_ ~ 0.6 and {tau}_O8_ ~ 0.1. Cappi et al. allowed the line energies
to be free and obtained a different ratio of optical depths but otherwise
similar results. Both Cappi et al. and R97 also fitted the data with a
similar photoionization model and obtained {{xi} ~ 10 (=U^R97^_X_ ~ 0.02),
N_H, z_ ~ 3 x 10^21^ cm^-2^, and N_H_, 0 ~ 3 x 10^21^ cm^-2^. These results
are consistent with those found in a ROSAT PSPC observation (Madejski et al.
We also found evidence for a strong Compton-reflection component in this
source with F~4 (Section 6.4.1), similar to that found by Cappi et al. This
hard tail was also found in HEAO 1 (W95) and Ginga (Miyoshi et al. 1988;
Piro, Yamauchi, & Matsuoka 1990) observations and offers an explanation the
CGRO OSSE spectrum of this source (Madejski et al. 1995).
None of the models quoted by Cappi et al. (1996) and R97 formally satisfy our
criteria for acceptability (though some of the fits described by Cappi et al.
are considered acceptable to those workers). We consider it likely that the
poverty of the various fits to the ASCA data is a combination of unaccounted
for systematics errors in the calibration and additional spectral complexity
in the soft X-ray band. As can be seen from Table 10, even we applied the
Compton-reflection fit, an excess of counts remains <0.6 keV. A similar
effect was reported by Cappi et al. This may be the result of a real
steepening of the intrinsic emission from IC 4329A or the result of
contamination of the ASCA data by emission from the nearby elliptical galaxy,
IC 4329 (see Madejski et al. 1995).
NP94 found evidence for absorption by ionized gas in Ginga observations, with
N_H, z_ ~ 10^22^ cm^-2^.

12. 1997MNRAS.286..513R
Re:IC 4329A
7.1.10 IC 4329a
The Seyfert 1 galaxy IC 4329a displays a strong unmodelled high-energy excess
after fitting with model B. Cappi et al. (1996) model this hard excess as the
onset of a very strong Compton reflection continuum. Time lag effects have to
be invoked to obtain such a reflection component. As shown in Cappi et al., the
iron line is weak (W_Fe_~90+/-30 eV) once the reflection continuum has been
included. If this is the correct spectral model, such a weak line requires an
iron underabundance and/or an ionized disc. This is in contrast to many other
well-studied Seyfert galaxies.

13. 1996ApJS..105...75C
Re:IC 4329A
4.1.12. IC 4329A
A bi-symmetric halo of emission-line gas can be seen in our H{alpha} + [N II]
image (Fig. 1j) extending along the minor axis, ~10" (3 kpc) on both sides of
the nucleus. The H{alpha} + [N II] luminosity of the extended emission on
either side is ~2.5 x 10^39^ ergs s^-1^. Unger et al. (1987) show that radio
emission extends ~6" west from the nucleus and suggest that it is from
material lying out of the plane. The H{alpha} halo we observe here is probably
produced by an outflow from the nuclear region, and we consider IC 4329A a good
candidate for a large-scale galactic outflow.

14. 1996ApJS..102..309M
Re:IC 4329A
The host galaxy of this well-studied Seyfert 1 is essentially edge-on. The
[O III] emission is extended along the major axis of the galaxy. H{alpha} is
extended along both the major axis of the galaxy and perpendicular to it. The
perpendicular extension in H{alpha} could represent a superwind as is commonly
seen in edge-on infrared-luminous galaxies (e.g. McCarthy, Heckman &
van Breugel 1987; Armus, Heckman & Miley 1990). The dust in the disk of the
galaxy is apparent in the color map. There are also two large patches of
apparent reddening on either side of the nucleus, which could be responsible
for the peculiar emission-line isophotes in the nuclear region (i.e. the
"multiple nuclei").

15. 1996ApJ...467..551C
Re:IC 4329A
3.1.15. IC 4329A
We did not obtain new radio images of IC 4329A. As far as we know, the only
published radio maps of this galaxy are those in Unger et al. (1987; see Fig.
1k). Diffuse radio structure extends westward ~6" (1.9 kpc) in P.A. ~285^deg^,
in the general direction of the galaxy minor axis.

16. 1995ApJ...447..121W
Re:IC 4329A
IC 4329A.-We confirm the spectral complexity observed by Ginga. Piro et
al. (1990) find that the Ginga data can be described either by
reflection, having a ratio of the reflected to direct component of
1.53 +/- 0.32, or by partial covering with f_c_~ 0.3 and N_H_ ~1.5 x
10^24^ cm^-2^. The upper limit on N_HFe_ is consistent with Ginga (NP94).

17. 1985SGC...C...0000C
Re:IC 4329A
Plate 494
Overexposed bulge, very strong dark lane. Possible Sa?

18. 1982ESOU..C...0000L
Re:ESO 134628-3003.7
=ESO 445- G 50
absorption lane
in cluster

19. 1976RC2...C...0000d
Re:IC 4329A
At 3.1 arcmin from IC 4329.
In a group with A1345-30, IC 4327, NGC 5302, and IC 4329 (brightest).
Type 1 Seyfert nucleus.
Photograph, Photometry, and Spectrum:
Ap. J. (Letters), 181, L55, 1973.
Photometry (10.6 microns):
Ap. J. (Letters), 191, L19, 1974.
M.N.R.A.S., 168, 109, 1974.
Radio Observations:
Ap. J. (Letters), 181, L55, 1973 (possible detection)

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