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AtsushiTanimoto / XClumpy

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XClumpy

Introduction

XClumpy (Tanimoto et al. 2019) is an X-ray spectral model from the clumpy torus in an Active Galactic Nucleus, using the Monte Carlo simulation for Astrophysics and Cosmology framework (MONACO: Odaka et al. 2011).

Torus Geometry

The adopted geometry of the torus is the same as that in Nenkova et al. (2008), who assumes a power-law distribution of clumps in the radial direction and a normal distribution in the elevation direction. This enables us to directly compare the results obtained from the infrared and X-ray bands. See Tanimoto et al. (2019) for more details.

Usage

We prepared an xcm file of the XClumpy model (xclumpy.xcm). Our spectral model is represented as follows in XSPEC terminology:
const*phabs*(cabs*zphabs*zcutoffpl+atable{xclumpy_v01_RC.fits}+atable{xclumpy_v01_RL.fits})

This model consists of four components:

  1. const*phabs
    The const term is a cross-normalization constant to adjust small differences in the absolute flux calibration among different instruments. The phabs term represents the Galactic absorption.

  2. cabs*zphabs*zcutoffpl
    This component represents the transmitted continuum through the torus. The zphabs and cabs terms represent the photoelectric absorption and Compton scattering by the torus, respectively. The hydrogen column density along the line of sight is determined according to Equation (1). The zcutoffpl term is the intrinsic continuum modeled by a power-law with an exponential cutoff.

  3. atable{xclumpy_v01_RC.fits}
    This component represents the reflection continuum from the clumpy torus based on the XClumpy model. This XClumpy model has six parameters: (1) hydrogen column density along the equatorial plane, (2) torus angular width, (3) inclination angle, (4) photon index, (5) cutoff energy, and (6) normalization. The photon index, cutoff energy, and normalization must be linked to those of the intrinsic continuum. We determine the line-of-sight hydrogen column density the following equation:

\begin{equation} N_{\mathrm{H}}^{\mathrm{LOS}} = N_{\mathrm{H}}^{\mathrm{Equ}} \exp\left({-\frac{(i-\pi/2)^2}{\sigma^2}}\right)\end{equation}

  1. atable{xclumpy_v01_RL.fits}
    This component represents fluorescence lines from the clumpy torus based on the XClumpy model. The hydrogen column density along the equatorial plane, torus angular width, inclination angle, photon index, cutoff energy, and normalization must be linked to those of the reflection continuum.

Parameters

The XClumpy model has six parameters.

Parameter Explanation Range Units
nh hydrogen column density along the equatorial plane 1023-1025 cm-2
sigma torus angular width 10-90 degree
incl inclination angle 20-87 degree
gamma photon index 1.0-3.0 ...
cutoff cutoff energy 10-1000 keV
norm normalization ... photons s-1 cm-2 keV-1 at 1 keV in the source frame

Example

We show the dependence of the reflection continuum on the hydrogen column density along the equatorial plane as an example. Red line is log NH/cm-2 = 23.5, orange line is log NH/cm-2 = 24.0, and blue line is log NH/cm-2 = 24.5. Here we adopt sigma = 30 degree, i = 60 degree, gamma = 2.0, cutoff = 370 keV, and norm = 1.0.

Publications

  1. XCLUMPY: X-Ray Spectral Model from Clumpy Torus and Its Application to the Circinus Galaxy
    Atsushi Tanimoto, Yoshihiro Ueda, Hirokazu Odaka, Toshihiro Kawaguchi, Yasushi Fukazawa, and Taiki Kawamuro
    The Astrophysical Journal, Volume 877, Issue 2, Eid 95, 2019.

  2. Application of Clumpy Torus Model to Broadband X-Ray Spectra of Two Seyfert 1 Galaxies: IC 4329A and NGC 7469
    Shoji Ogawa, Yoshihiro Ueda, Satoshi Yamada, Atsushi Tanimoto, and Toshihiro Kawaguchi
    The Astrophysical Journal, Volume 875, Issue 2, Eid 115, 2019.

  3. Torus Constraints in ANEPD-CXO245: A Compton-thick AGN with Double-peaked Narrow Lines Takamitsu Miyaji et al.
    The Astrophysical Journal Letters, Volume 884, Issue 1, Eid L10, 2019.

  4. NuSTAR Discovery of a Compton-thick, Dust-obscured Galaxy: WISE J0825+3002
    Yoshiki Toba et al.
    The Astrophysical Journal, Volume 888, Issue 1, Eid 8, 2020.

  5. Application of an X-Ray Clumpy Torus Model (XCLUMPY) to 10 Obscured Active Galactic Nuclei Observed with Suzaku and NuSTAR
    Atsushi Tanimoto, Yoshihiro Ueda, Hirokazu Odaka, Shoji Ogawa, Satoshi Yamada, Toshihiro Kawaguchi, and Kohei Ichikawa
    The Astrophysical Journal, Volume 897, Issue 1, Eid 2, 2020.

  6. Nature of Compton-thick Active Galactic Nuclei in "Nonmerging" Luminous Infrared Galaxies UGC 2608 and NGC 5135 Revealed with Broadband X-Ray Spectroscopy
    Satoshi Yamada, Yoshihiro Ueda, Atsushi Tanimoto, Saeko Oda, Masatoshi Imanishi, Yoshiki Toba, and Ricci Claudio
    The Astrophysical Journal, Volume 897, Issue 1, Eid 107, 2020.

  7. Systematic Study of AGN Clumpy Tori with Broadband X-Ray Spectroscopy: Updated Unified Picture of AGN Structure
    Shoji Ogawa, Yoshihiro Ueda, Atsushi Tanimoto, and Satoshi Yamada
    The Astrophysical Journal, Volume 906, Issue 2, Eid 84, 2021.

  8. X-Ray Constraint on the Location of the AGN Torus in the Circinus Galaxy
    Ryosuke Uematsu, Yoshihiro Ueda, Atsushi Tanimoto, Taiki Kawamuro, Kenta Setoguchi, Shoji Ogawa, Satoshi Yamada, and Hirokazu Odaka
    The Astrophysical Journal, Volume 913, Issue 1, Eid 17, 2021.

  9. Comprehensive Broadband X-Ray and Multiwavelength Study of Active Galactic Nuclei in 57 Local Luminous and Ultraluminous Infrared Galaxies Observed with NuSTAR and/or Swift/BAT Satoshi Yamada, Yoshihiro Ueda, Atsushi Tanimoto, Masatoshi Imanishi, Yoshiki Toba, Claudio Ricci, and George Privon The Astrophysical Journal Supplement Series, Volume 257, Issue 2, Eid 61, 2021.

  10. NuSTAR Observations of 52 Compton-thick Active Galactic Nuclei Selected by the Swift/Burst Alert Telescope All-sky Hard X-Ray Survey Atsushi Tanimoto, Yoshihiro Ueda, Hirokazu Odaka, Satoshi Yamada, and Claudio Ricci The Astrophysical Journal Supplement Series, Volume 260, Issue 2, Eid 30, 2022.

  11. Absorption variability of the highly obscured active galactic nucleus NGC 4507 Arghajit Jana et al. Monthly Notices of the Royal Astronomical Society, Volume 512, Issue 4, 2022.

Citation

If you have used the XClumpy model in a scientific publication, please cite Tanimoto et al. (2019).

Acknowledgement

Numerical computations were carried out on Cray XC50 at Center for Computational Astrophysics, National Astronomical Observatory of Japan.