501 research outputs found
Wide-Band X-Ray Spectra and Images of the Starburst Galaxy M82
The ASCA results of the starburst galaxy M82 are presented. The X-rays in the
0.5--10 keV band exhibit a thin thermal spectrum with emission lines from
highly ionized magnesium, silicon, and sulfur, as well as a hard tail extending
to higher than 10keV energy. The soft X-rays are spatially extended, while the
hard X-rays show an unresolved point-like structure with possible a long-term
flux variability. The flux ratio of the emission lines and the spatially
extended structure in the low-energy band indicate that at least
two-temperature thin thermal plasmas are present. The abundances of the oxygen,
neon, magnesium, silicon, sulfur, and iron in the thin thermal plasmas are
found to be significantly lower than the cosmic value. Neither type-Ia nor
type-II supernova explosions can reproduce the observed abundance ratio. The
origin of the unresolved hard X-rays is uncertain, but is probably an obscured
low-luminosity AGN.Comment: 25 pages, 8 figure
Study on X-ray Spectra of Obscured AGNs based on Monte Carlo simulation - an interpretation of observed wide-band spectra
Monte Carlo simulation is one of the best tools to study the complex spectra
of Compton-thick AGNs and to figure out the relation between their nuclear
structures and X-ray spectra. We have simulated X-ray spectra of Compton-thick
AGNs obscured by an accretion torus whose structure is characterized by a
half-opening angle, an inclination angle of the torus relative to the observer,
and a column density along the equatorial plane. We divided the simulated
spectra into three components: one direct component, an absorbed reflection
component and an unabsorbed reflection component. We then deduced the
dependencies of these components on the parameters describing the structure of
the torus. Our simulation results were applied to fit the wide-band spectrum of
the Seyfert 2 galaxy Mrk 3 obtained by . The spectral analysis
indicates that we observe the nucleus along a line of sight intercepting the
torus near its edge, and the column density along the equatorial plane was
estimated to be ~10^24 cm^-2. Using this model, we can estimate the
luminosities of both the direct emission and the emission irradiating the
surrounding matter. This is useful to find the time variability and time lag
between the direct and reflected light.Comment: 25 pages, 25 figures, accepted for publication in Ap
Parameter Estimation and Confidence Regions in the Method of Light Curve Simulations for the Analysis of Power Density Spectra
The Method of Light Curve Simulations is a tool that has been applied to
X-ray monitoring observations of Active Galactic Nuclei (AGN) for the
characterization of the Power Density Spectrum (PDS) of temporal variability
and measurement of associated break frequencies (which appear to be an
important diagnostic for the mass of the black hole in these systems as well as
their accretion state). It relies on a model for the PDS that is fit to the
observed data. The determination of confidence regions on the fitted model
parameters is of particular importance, and we show how the Neyman construction
based on distributions of estimates may be implemented in the context of light
curve simulations. We believe that this procedure offers advantages over the
method used in earlier reports on PDS model fits, not least with respect to the
correspondence between the size of the confidence region and the precision with
which the data constrain the values of the model parameters. We plan to apply
the new procedure to existing RXTE and XMM observations of Seyfert I galaxies
as well as RXTE observations of the Seyfert II galaxy NGC 4945.Comment: 9 pages, 2 figures, accepted for publication in Ap
On the nature of the X-ray absorption in the Seyfert 2 galaxy NGC 4507
We present results of the ASCA observation of the Seyfert 2 galaxy NGC 4507.
The 0.5-10 keV spectrum is rather complex and consists of several components:
(1) a hard X-ray power law heavily absorbed by a column density of about 3
10^23 cm^-2, (2) a narrow Fe Kalpha line at 6.4 keV, (3) soft continuum
emission well above the extrapolation of the absorbed hard power law, (4) a
narrow emission line at about 0.9 keV. The line energy, consistent with highly
ionized Neon (NeIX), may indicate that the soft X-ray emission derives from a
combination of resonant scattering and fluorescence in a photoionized gas. Some
contribution to the soft X-ray spectrum from thermal emission, as a blend of Fe
L lines, by a starburst component in the host galaxy cannot be ruled out with
the present data.Comment: 8 pages, LateX, 5 figures (included). Uses mn.sty and epsfig.sty. To
appear in MNRA
Discovery of Bright Variable X-ray Sources in NGC 1569 with Chandra
From the analysis of a ~100 ks Chandra observation of the dwarf starburst
galaxy NGC 1569, we have found that the X-ray point sources, CXOU
043048.1+645050 and CXOU 043048.6+645058, showed significant time variability.
During this observation, the X-ray flux of CXOU 043048.1+645050 increased by 10
times in only 2 x 10^4 s. Since the spectrum in its bright phase was fitted
with a disk blackbody model with kT_in ~0.43 keV and the bolometric luminosity
is L_bol ~10^38 ergs s^-1, this source is an X-ray binary with a stellar mass
black-hole. Since the spectrum in its faint phase was also fitted with a disk
blackbody model, the time variability can be explained by a change of the
accretion rate onto the black hole. The other variable source, CXOU
043048.6+645058, had a flat spectrum with a photon index of ~1.6. This source
may be an X-ray binary with an X-ray luminosity of several x 10^37 ergs s^-1.
In addition, three other weak sources showed possible time variability. Taking
all of the variability into account may suggest an abundant population of
compact X-ray sources in NGC 1569.Comment: 15 pages including 4 Postscript figures; accepted for publication in
ApJ
Luminosity-dependent unification of Active Galactic Nuclei and the X-ray Baldwin effect
The existence of an anti-correlation between the equivalent width (EW) of the
narrow core of the iron Kalpha line and the luminosity of the continuum (i.e.
the X-ray Baldwin effect) in type-I active galactic nuclei has been confirmed
over the last years by several studies carried out with XMM-Newton, Chandra and
Suzaku. However, so far no general consensus on the origin of this trend has
been reached. Several works have proposed the decrease of the covering factor
of the molecular torus with the luminosity (in the framework of the
luminosity-dependent unification models) as a possible explanation for the
X-ray Baldwin effect. Using the fraction of obscured sources measured by recent
X-ray and IR surveys as a proxy of the half-opening angle of the torus, and the
recent Monte-Carlo simulations of the X-ray radiation reprocessed by a
structure with a spherical-toroidal geometry by Ikeda et al. (2009) and
Brightman & Nandra (2011), we test the hypothesis that the X-ray Baldwin effect
is related to the decrease of the half-opening angle of the torus with the
luminosity. Simulating the spectra of an unabsorbed population with a
luminosity-dependent covering factor of the torus as predicted by recent X-ray
surveys, we find that this mechanism is able to explain the observed X-ray
Baldwin effect. Fitting the simulated data with a log-linear L_{2-10keV}-EW
relation, we found that in the Seyfert regime (L_{2-10keV}< 10^44.2 erg s^-1)
luminosity-dependent unification produces a slope consistent with the
observations for average values of the equatorial column densities of the torus
of log N_H^T > 23.1. In the quasar regime (L_{2-10 keV}> 10^44.2 erg s^-1) a
decrease of the covering factor of the torus with the luminosity slower than
that observed in the Seyfert regime (as found by recent hard X-ray surveys) is
able to reproduce the observations for 23.2 < log N_H^T < 24.2.Comment: 9 pages, 9 figures, 1 table. Accepted for pubblication in A&
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