X-Ray Spectral Model from Clumpy Torus and Its Application to Circinus Galaxy. (arXiv:1904.08945v1 [astro-ph.HE])

X-Ray Spectral Model from Clumpy Torus and Its Application to Circinus Galaxy. (arXiv:1904.08945v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Tanimoto_A/0/1/0/all/0/1">Atsushi Tanimoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ueda_Y/0/1/0/all/0/1">Yoshihiro Ueda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Odaka_H/0/1/0/all/0/1">Hirokazu Odaka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kawaguchi_T/0/1/0/all/0/1">Toshihiro Kawaguchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fukazawa_Y/0/1/0/all/0/1">Yasushi Fukazawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kawamuro_T/0/1/0/all/0/1">Taiki Kawamuro</a>

We construct an X-ray spectral model from the clumpy torus in an active
galactic nucleus (AGN), designated as “XCLUMPY”, utilizing the Monte Carlo
simulation for Astrophysics and Cosmology framework (MONACO: Odaka et al. 2011,
2016). The adopted geometry of the torus is the same as that in Nenkova et al.
(2008), who assume a power law distribution of clumps in the radial direction
and a normal distribution in the elevation direction. We investigate the
dependence of the X-ray continuum and Fe K$alpha$ fluorescence line profile on
the torus parameters. Our model is compared with other torus models: MYTorus
model (Murphy & Yaqoob 2009), Ikeda model (Ikeda et al. 2009), and CTorus model
(Liu & Li 2014). As an example, we also present the results applied to the
broadband X-ray spectra of the Circinus galaxy observed with XMM-Newton,
Suzaku, and NuSTAR. Our model can well reproduce the data, yielding a hydrogen
column density along the equatorial plane $N_{mathrm{H}}^{mathrm{Equ}} =
9.08_{-0.08}^{+0.14} times 10^{24}$ cm$^{-2}$, a torus angular width $sigma =
14.7_{-0.39}^{+0.44}$ degree, and a 2–10 keV luminosity $log
L_{2-10}/mathrm{erg s^{-1}} = 42.8$. These results are discussed in
comparison with the observations in other wavelengths.

We construct an X-ray spectral model from the clumpy torus in an active
galactic nucleus (AGN), designated as “XCLUMPY”, utilizing the Monte Carlo
simulation for Astrophysics and Cosmology framework (MONACO: Odaka et al. 2011,
2016). The adopted geometry of the torus is the same as that in Nenkova et al.
(2008), who assume a power law distribution of clumps in the radial direction
and a normal distribution in the elevation direction. We investigate the
dependence of the X-ray continuum and Fe K$alpha$ fluorescence line profile on
the torus parameters. Our model is compared with other torus models: MYTorus
model (Murphy & Yaqoob 2009), Ikeda model (Ikeda et al. 2009), and CTorus model
(Liu & Li 2014). As an example, we also present the results applied to the
broadband X-ray spectra of the Circinus galaxy observed with XMM-Newton,
Suzaku, and NuSTAR. Our model can well reproduce the data, yielding a hydrogen
column density along the equatorial plane $N_{mathrm{H}}^{mathrm{Equ}} =
9.08_{-0.08}^{+0.14} times 10^{24}$ cm$^{-2}$, a torus angular width $sigma =
14.7_{-0.39}^{+0.44}$ degree, and a 2–10 keV luminosity $log
L_{2-10}/mathrm{erg s^{-1}} = 42.8$. These results are discussed in
comparison with the observations in other wavelengths.

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