Date and Time of the Query: 2019-06-24 T16:37:22 PDT
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Notes for object MCG -03-34-064

6 note(s) found in NED.

1. 2009ApJ...690.1322W
Re:MCG -03-34-064
MCG-03-34-064. The spectrum also has a significant ({DELTA}{chi}^2^ =
34) soft component, which we fit with an apec model with kT = 0.82^+0.11^
_-0.09_ keV. A more complete analysis of this source is presented in
Miniutti et al. (2007), where they model the spectra as
reflection-dominated with thermal plasmas, a broad Fe K line, and
additional Fe emission lines.

2. 2007A&A...461.1209D
Re:IRAS 13197-1627
IRAS 13197-1627: The source was first detected in X-rays by ASCA (Ueno
1995). The X-ray spectrum of the source is dominated by a complex
absorber (Dadina & Cappi 2004) that hides a QSO-like nucleus. Here, the
absorber has been modeled with a partial covering model (N_H_ ~2.6 +/-
0.9 x 10^24^ cm^-2^, c_f_ = 0.90 +/- 0.05) that is in agreement with what
was reported in Dadina & Cappi (2004). Another interesting property of
the source is its steep continuum {GAMMA} ~ 2.4 - 3, depending on the
modelization of the absorber). This value is not typical of a Seyfert
galaxy or a QSO ({GAMMA} ~ 1.7 - 2, Smith and Done 1996, Turner et al.
1997) and is more similar to what observed in NLSy1 (Brandt et al.

3. 2002ApJ...564..650C
Re:IRAS 13197-1627
5. IRAS 13197-1627 is a known Seyfert galaxy (de Grijp et al. 1985)
and is classified as a Seyfert 1.8 by Aguerro et al. (1994). It has
a tentative classification in NED as an SB galaxy morphology. A compact
core of 26 mJy has been detected previously using the PTI
(resolution 0.1"; Heisler et al. 1997), and VLA observations at 3.6 cm
by Kinney et al. (2000) have revealed a linear structure extending about
278 pc from the core, believed to be a synchrotron jet. We detect a
compact core of 8.9 mJy at 0.05" resolution. IRAS 13197-1627 exhibits
one of the largest radio excesses of our sample with the 4.8 GHz flux
almost an order of magnitude larger than the predicted value. This
excess remains after subtraction of the compact core emission and is
probably due, at least in part, to emission from the ~300 pc scale radio

4. 2001ApJS..132..199S
Re:MCG -03-34-064
4.2.13. MCG -03-34-064
According to Roy et al. (1998), this galaxy has a compact nuclear radio
source with a flux of 26 mJy at 2.3 GHz. The optical and ultraviolet
spectra show narrow emission lines with blueward asymmetries and possibly
a broad C IV {lambda}1550 A line (De Robertis, Hutchings, & Pitts 1988).
The radio emission is extended by 280 pc. It starts as a linear structure
to the southwest (P.A. = 219^deg^), and after ~100 pc it bends to the
south, along P.A. ~ 180^deg^. Kay (1994) spectropolarimetric data showed
that the nuclear spectrum of this galaxy is polarized by 7.4% at 4400 A,
along P.A. = 109^deg^, approximately perpendicular to the extended radio
emission. We adopt the innermost P.A. as the direction of the jet.

5. 1996ApJS..103...81C
Re:MCG -03-34-063
MCG-03-34-063.--Seyfert 2. Pks B1319-164. VLA D-configuration map at 4.86 GHz
in Condon et al. (1995).

6. 1996ApJ...467..551C
Re:MCG -03-34-064
THE SEYFERT GALAXY IRAS 13197-1627 IS MCG -3-34-64
In Figure 5, we show contour maps of the 4.9GHz radio emission from the
two galaxies MCG -3-34-63 and MCG -3-34-64. We find total radio fluxes of
93.4 mJy (5.0x10^22^ W Hz^-1^ at an assumed distance of 67.2 Mpc) and 1.3 mJy
(7.1x10^20^ W Hz^-1^) for MCG -3-34-63 and MCG -3-34-64, respectively. {NED
note: this should read "MCG -3-34-64 and MCG -3-34-63, respectively".} The
central source in MCG -3-34-63 has a flux of 0.6 mJy (3.4x10^20^ W Hz^-1^),
and the source positioned ~15" (4.9 kpc) northeast of the nucleus has a
flux of 0.15 mJy (8.1x10^19^ W Hz^-1^). The radio source in MCG -3-34-64 is
slightly resolved along P.A. 135^degrees^.
Our complete sample of edge-on Seyfert galaxies was constructed by
cross-referencing various Seyfert catalogs with RC3 (de Vaucouleurs et al.
1991; see Paper I). One of the objects selected by this process was the
warm FIR galaxy IRAS 13197-1627, which is listed in the Seyfert catalog of
Huchra (1995). This object was first identified as a Seyfert galaxy by
de Grijp et al. (1985). Several workers have associated this IRAS source with
MCG -3-34-63, and edge-on galaxy with axial ratio 3.2 (RC3). We have since
found that IRAS 13197-1627 is not associated with MCG -3-34-63 but is
instead associated with the galaxy MCG -3-34-64, positioned ~1.8' southeast
of MCG -3-34-63.
We suspected this to be the case when we found a large disagreement between
our observed radio fluxes for MCG -3-34-63 and those listed in the literature
from previous radio observations (which were undoubtedly measurements of the
stronger radio source MCG -3-34-64). The IRAS fluxes listed for IRAS 13197-1627
(which probably include emission from both galaxies) also implied excessively
large values of {mu} (i.e., the FIR flux was comparatively very large). We
later learned (M. de Robertis 1995, private communication) that the nuclear
spectrum which identified the Seyfert galaxy IRAS 13197-1627 is a spectrum of
MCG -3-34-64, not MCG -3-34-63.
Authors of future catalogs of Seyferts should note that this error has
progressed into many published catalogs and papers.

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