Date and Time of the Query: 2019-06-15 T16:47:13 PDT
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Notes for object ESO 033- G 002

4 note(s) found in NED.

1. 2007A&A...461.1209D
Re:ESO 033- G 002
ESO33-G02: The BeppoSAX data were unpublished. Previous X-ray
observations of the source were carried out by Ginga (Smith & Done 1996)
and ASCA (Vignali et al. 1998). In the MECS FOV, other sources are
present, one of which is known to be a bright KIII peculiar star that is
not expected to significantly contribute to the PDS counts. The
continuum is absorbed (as was previously observed) by a column with
N_H_ ~ 2 x 10^22^ cm^-2^. This value is in good agreement with what was
observed by Ginga (N_H_ ~ 2 x 10^22^ cm^-2^, Smith & Done 1996) and
slightly above the measurements by ASCA (N_H_ ~10^22^ cm^-2^,
Vignali et al. 1998). The shape of the continuum, as measured by
BeppoSAX, is typical of Seyfert galaxies and significantly steeper
({GAMMA} = 2.0 +/- 0.2) than that measured by ASCA ({GAMMA} = 1.5 +/- 0.2,
Vignali et al. 1998), although it is similar to what was measured by
Ginga ({GAMMA} = 2.1 +/- 0.2, Smith & Done 1996). The 2-10 keV flux of
the source (F_2-10 keV_ ~ 6 x 10^-12^ erg s^-1^ cm^-2^) is half of what
was previously measured by ASCA and Ginga. An iron emission line is
detected at ~6.4 keV with EW 110 eV which is consistent with Ginga and
ASCA results. A reflection component is also observed (R = 0.6 +/- 0.5,
90% confidence), while the energy of E_c_ is unconstrained (E_c_ >= 52 keV).
As previously noted by Vignali et al. (1998), the absorber is complex and
the best fit reported here includes a partial covering component that
hides ~70% of the primary emission with a N_H_ ~ 4 x 10^24^ cm^-2^ column.
On the contrary, Vignali et al. (1998) reported a reprocessor covering ~35%
of the primary continuum and with a much lower column (N_H_ ~ 10^23^ cm^-2^).
Once corrected for the partial absorption, the 2-10 keV flux is
F_2-10 keV_ ~ 2.5 x 10^-11^ erg s^-1^ cm^-2^, that is ~2 times above the
Ginga and ASCA values, thus indicating that absorption is leading the flux
dimming. The overall scenario is that ESO33-G02 seems to be a high luminosity
Seyfert galaxy (with intrinsic L_2-10 keV_ ~ 2 x 10^43^ erg s^-1^) that
displays two different absorber: a) a stable one with approximatively the
same column measured in a ~10-year-long sparse monitoring, and b) a variable
and probably cloudy one that showed strong variations between the the
ASCA and BeppoSAX observations.

2. 2006ApJ...638..642B
Re:ESO 033- G 002
ESO 33-2 - Several sources may have been marginally suspected in the
INTEGRAL data. They either were targets of dedicated observations or were
detected in some single science windows. We performed the same analysis as
for the other sources presented here, but found only spurious source
candidates that result from image reconstruction problems such as ghosts
and mask patterns. Among those sources are Mrk 231, ESO 33-2, PKS 0637-75,
MCG -05-23-16, QSO 1028+313, NGC 4736, NGC 4418, 3C 353, and QSO

3. 2003ApJS..148..327S
Re:ESO 033- G 002
5.17. ESO 33-G02
The [O III] image of this Seyfert 2 galaxy is presented in the bottom
left panel of Figure 7. The emission is distributed in a more or less
homogeneous way around the nucleus, extended by 1" x 1.45" (350 x 510
pc), with the major axis along the N-S direction, perpendicular to
the host galaxy major axis. Some diffuse emission can be seen to the
NE of the nucleus. The ground-based [O III] images published by
Mulchaey et al. (1996a) show only slightly resolved emission.

4. 1996ApJS..102..309M
Re:ESO 033- G 002
ESO 33-G2 is only slightly resolved in our [O III] image. The H{alpha}
emission is extended along the direction of the galactic bar and presumably
indicates on-going star formation. The continuum peak appears to be very red
based on the color map.

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