Date and Time of the Query: 2019-06-26 T23:28:20 PDT
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Notes for object ESO 198- G 024

4 note(s) found in NED.

1. 2007A&A...461.1209D
Re:ESO 198- G 024
ESO 198 -G24: Quadrelli et al. (2003) published the spectra of the two
observations of ESO 198-G24, adopting the same baseline model presented
here. Quadrelli et al. (2003) also considered an ionized absorber that
is not necessary to account for when data below 2 keV are not included
in the analysis.

2. 2004MNRAS.350.1049G
Re:ESO 198- G 024
9.5 ESO 198-G24 A large visual range was found for this galaxy by
Winkler et al. (1992).

3. 2004A&A...422...65B
Re:ESO 198- G 024
3.3.1 ESO198-G024 The BeppoSAX and XMM-Newton observations were analyzed
separately by Guainazzi (2003) and Porquet et al. (2004). The BMS gives
a good {chi}^2^ (103/123 d.o.f.), but some residuals redwards the iron
line are apparent in the spectrum. They can be corrected by the addition
of a second narrow Gaussian line (at about 99% confidence level), with
E=5.91+0.05-0.06 keV and EW=42^+30^_-22_ eV: the parameters in Table 2 refer
to this fit. The 6.4 keV line is unresolved and has a modest EW, as
found by Porquet et al. (2004). A previous XMM-Newton observation,
performed about two months before, showed a broad and more intense line
(Guainazzi 2003), thus suggesting a variation of both profile and
flux. However, it should be noted that an upper limit of 150 eV for the
EW of a relativistic line is found, if added to the narrow core.
The presence of the second feature is not reported by Porquet et
al. (2004), but Guainazzi (2003) found a line at 5.70^+0.07^_-0.12_ keV
in the other XMM-Newton observation. We further divided the second
XMM-Newton observation in two parts of about 10 ks each. Interestingly,
the feature is present (at the 98.3% confidence level) only in the
second half, at energy 5.96+-0.05 keV and with { EW}=64^+47^_-36_ eV. An
upper limit of 30 eV is instead found for the first half of the
observation. Even if the statistical significance of this result is
modest, it gives further support that the feature exists and is indeed
varying on a short timescale. A possible interpretation of this feature
consists of a 6.4 keV (rest-frame) iron line produced in a well-confined
region of the accretion disk. If this is the case, the line photons
suffer gravitational redshift and (relativistic) Doppler effects, as
functions of the observed orbital phase, but the integrated line width
would be in many cases narrow, because only the blue horn can be visible
in moderate signal-to-noise ratio data. We refer the reader to Dovciak
et al. (2004), for a comprehensive discussion on this possibility and
the comparison of theoretical models with data from ESO198-G024 and
other sources.

4. 1982ESOU..C...0000L
Re:ESO 023641-5224.3
=ESO 198- G 24
north following of 2
in cluster

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