Complete list of the ASTRO-H Science Working Group

Complete list of the ASTRO-H Science Working Group

Tadayuki Takahashi Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Kazuhisa Mitsuda Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Richard Kelley NASA/Goddard Space Flight Center, MD 20771, USA Felix Aharonian Astronomy and Astrophysics Section, Dublin Institute for Advanced Studies, Dublin 2, Ireland Hiroki Akamatsu SRON Netherlands Institute for Space Research, Utrecht, The Netherlands Fumie Akimoto Department of Physics, Nagoya University, Aichi 338-8570, Japan Steve Allen Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, CA 94305, USA Naohisa Anabuki Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan Lorella Angelini NASA/Goddard Space Flight Center, MD 20771, USA Keith Arnaud Department of Astronomy, University of Maryland, MD 20742, USA Marc Audard Université de Genève, Genève 4, Switzerland Hisamitsu Awaki Department of Physics, Ehime University, Ehime 790-8577, Japan Aya Bamba Department of Physics and Mathematics, Aoyama Gakuin University, Kanagawa 229-8558, Japan Marshall Bautz Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, MA 02139, USA Roger Blandford Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, CA 94305, USA Laura Brenneman NASA/Goddard Space Flight Center, MD 20771, USA Greg Brown Lawrence Livermore National Laboratory, CA 94550, USA Edward Cackett Institute of Astronomy, Cambridge University, CB3 0HA, UK Maria Chernyakova Astronomy and Astrophysics Section, Dublin Institute for Advanced Studies, Dublin 2, Ireland Meng Chiao NASA/Goddard Space Flight Center, MD 20771, USA Paolo Coppi Yale Center for Astronomy and Astrophysics, Yale University, CT 06520-8121, USA Elisa Costantini SRON Netherlands Institute for Space Research, Utrecht, The Netherlands Jelle de Plaa SRON Netherlands Institute for Space Research, Utrecht, The Netherlands Jan-Willem den Herder SRON Netherlands Institute for Space Research, Utrecht, The Netherlands Chris Done Department of Physics, University of Durham, DH1 3LE, UK Tadayasu Dotani Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Ken Ebisawa Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Megan Eckart NASA/Goddard Space Flight Center, MD 20771, USA Teruaki Enoto RIKEN, Saitama 351-0198, Japan Yuichiro Ezoe Department of Physics, Tokyo Metropolitan University, Tokyo 192-0397, Japan Andrew Fabian Institute of Astronomy, Cambridge University, CB3 0HA, UK Carlo Ferrigno Université de Genève, Genève 4, Switzerland Adam Foster Harvard-Smithsonian Center for Astrophysics, MA 02138, USA Ryuichi Fujimoto Faculty of Mathematics and Physics, Kanazawa University, Ishikawa 920-1192, Japan Yasushi Fukazawa Department of Physical Science, Hiroshima University, Hiroshima 739-8526, Japan Stefan Funk Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, CA 94305, USA Akihiro Furuzawa Department of Physics, Nagoya University, Aichi 338-8570, Japan Massimiliano Galeazzi Physics Department, University of Miami, FL 33124, USA Luigi Gallo Department of Astronomy and Physics, Saint Mary’s University, Nova Scotia B3H 3C3, Canada Poshak Gandhi Department of Physics, University of Durham, DH1 3LE, UK Matteo Guainazzi European Space Agency (ESA), European Space Astronomy Centre (ESAC), Madrid, Spain Yoshito Haba Department of Physics and Astronomy, Aichi University of Education, Aichi 448-8543, Japan Kenji Hamaguchi Department of Astronomy, University of Maryland, MD 20742, USA Isamu Hatsukade Department of Applied Physics, University of Miyazaki, Miyazaki 889-2192, Japan Takayuki Hayashi Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Katsuhiro Hayashi Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Kiyoshi Hayashida Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan Junko Hiraga Department of Physics, University of Tokyo, Tokyo 113-0033, Japan Ann Hornschemeier NASA/Goddard Space Flight Center, MD 20771, USA Akio Hoshino Department of Physics, Rikkyo University, Tokyo 171-8501, Japan John Hughes Department of Physics and Astronomy, Rutgers University, NJ 08854-8019, USA Una Hwang Department of Physics and Astronomy, Johns Hopkins University, MD 21218, USA Ryo Iizuka Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Yoshiyuki Inoue Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Hajime Inoue Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Kazunori Ishibashi Department of Physics, Nagoya University, Aichi 338-8570, Japan Manabu Ishida Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Kumi Ishikawa RIKEN, Saitama 351-0198, Japan Yoshitaka Ishisaki Department of Physics, Tokyo Metropolitan University, Tokyo 192-0397, Japan Masayuki Ito Faculty of Human Development, Kobe University, Hyogo 657-8501, Japan Naoko Iyomoto Kyushu University, Fukuoka 819-0395, Japan Jelle Kaastra SRON Netherlands Institute for Space Research, Utrecht, The Netherlands Timothy Kallman NASA/Goddard Space Flight Center, MD 20771, USA Tuneyoshi Kamae Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, CA 94305, USA Jun Kataoka Research Institute for Science and Engineering, Waseda University, Tokyo 169-8555, Japan Satoru Katsuda Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Junichiro Katsuta Department of Physical Science, Hiroshima University, Hiroshima 739-8526, Japan Madoka Kawaharada Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Nobuyuki Kawai Department of Physics, Tokyo Institute of Technology, Tokyo 152-8551, Japan Dmitry Khangulyan Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Caroline Kilbourne NASA/Goddard Space Flight Center, MD 20771, USA Masashi Kimura Tsukuba Space Center (TKSC), Japan Aerospace Exploration Agency (JAXA), Ibaraki 305-8505, Japan Shunji Kitamoto Department of Physics, Rikkyo University, Tokyo 171-8501, Japan Tetsu Kitayama Department of Physics, Toho University, Chiba 274-8510, Japan Takayoshi Kohmura Department of Physics, Tokyo University of Science, Chiba 278-8510, Japan Motohide Kokubun Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Saori Konami Department of Physics, Tokyo Metropolitan University, Tokyo 192-0397, Japan Katsuji Koyama Department of Physics, Kyoto University, Kyoto 606-8502, Japan Hans Krimm NASA/Goddard Space Flight Center, MD 20771, USA Aya Kubota Department of Electronic Information Systems, Shibaura Institute of Technology, Saitama 337-8570, Japan Hideyo Kunieda Department of Physics, Nagoya University, Aichi 338-8570, Japan Stephanie LaMassa Yale Center for Astronomy and Astrophysics, Yale University, CT 06520-8121, USA Philippe Laurent IRFU/Service d’Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette Cedex, France François Lebrun IRFU/Service d’Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette Cedex, France Maurice Leutenegger NASA/Goddard Space Flight Center, MD 20771, USA Olivier Limousin IRFU/Service d’Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette Cedex, France Michael Loewenstein NASA/Goddard Space Flight Center, MD 20771, USA Knox Long Space Telescope Science Institute, MD 21218, USA David Lumb European Space Agency (ESA), European Space Research and Technology Centre (ESTEC), 2200 AG Noordwijk, The Netherlands Grzegorz Madejski Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, CA 94305, USA Yoshitomo Maeda Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Kazuo Makishima Department of Physics, University of Tokyo, Tokyo 113-0033, Japan Maxim Markevitch NASA/Goddard Space Flight Center, MD 20771, USA Hironori Matsumoto Department of Physics, Nagoya University, Aichi 338-8570, Japan Kyoko Matsushita Department of Physics, Tokyo University of Science, Tokyo 162-8601, Japan Dan McCammon Department of Physics, University of Wisconsin, WI 53706, USA Brian McNamara University of Waterloo, Ontario N2L 3G1, Canada Jon Miller Department of Astronomy, University of Michigan, MI 48109, USA Eric Miller Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, MA 02139, USA Shin Mineshige Department of Astronomy, Kyoto University, Kyoto 606-8502, Japan Ikuyuki Mitsuishi Department of Physics, Nagoya University, Aichi 338-8570, Japan Takuya Miyazawa Department of Physics, Nagoya University, Aichi 338-8570, Japan Tsunefumi Mizuno Department of Physical Science, Hiroshima University, Hiroshima 739-8526, Japan Koji Mori Department of Applied Physics, University of Miyazaki, Miyazaki 889-2192, Japan Hideyuki Mori Department of Physics, Nagoya University, Aichi 338-8570, Japan Koji Mukai NASA/Goddard Space Flight Center, MD 20771, USA Hiroshi Murakami Department of Information Science, Faculty of Liberal Arts, Tohoku Gakuin University, Miyagi 981-3193, Japan Toshio Murakami Faculty of Mathematics and Physics, Kanazawa University, Ishikawa 920-1192, Japan Richard Mushotzky Department of Astronomy, University of Maryland, MD 20742, USA Ryo Nagino Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan Takao Nakagawa Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Hiroshi Nakajima Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan Takeshi Nakamori Department of Physics, Faculty of Science, Yamagata University, Yamagata 990-8560, Japan Shinya Nakashima Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Kazuhiro Nakazawa Department of Physics, University of Tokyo, Tokyo 113-0033, Japan Masayoshi Nobukawa Department of Physics, Kyoto University, Kyoto 606-8502, Japan Hirofumi Noda RIKEN, Saitama 351-0198, Japan Masaharu Nomachi Laboratory of Nuclear Studies, Osaka University, Osaka 560-0043, Japan Steve O’ Dell NASA/Marshall Space Flight Center, AL 35812, USA Hirokazu Odaka Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Takaya Ohashi Department of Physics, Tokyo Metropolitan University, Tokyo 192-0397, Japan Masanori Ohno Department of Physical Science, Hiroshima University, Hiroshima 739-8526, Japan Takashi Okajima NASA/Goddard Space Flight Center, MD 20771, USA Naomi Ota Department of Physics, Faculty of Science, Nara Women’s University, Nara 630-8506, Japan Masanobu Ozaki Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Frits Paerels Department of Astronomy, Columbia University, NY 10027, USA Stéphane Paltani Université de Genève, Genève 4, Switzerland Arvind Parmar European Space Agency (ESA), European Space Astronomy Centre (ESAC), Madrid, Spain Robert Petre NASA/Goddard Space Flight Center, MD 20771, USA Ciro Pinto Institute of Astronomy, Cambridge University, CB3 0HA, UK Martin Pohl Université de Genève, Genève 4, Switzerland F. Scott Porter NASA/Goddard Space Flight Center, MD 20771, USA Katja Pottschmidt NASA/Goddard Space Flight Center, MD 20771, USA Brian Ramsey NASA/Marshall Space Flight Center, AL 35812, USA Rubens Reis Department of Astronomy, University of Michigan, MI 48109, USA Christopher Reynolds Department of Astronomy, University of Maryland, MD 20742, USA Claudio Ricci Department of Astronomy, Kyoto University, Kyoto 606-8502, Japan Helen Russell Institute of Astronomy, Cambridge University, CB3 0HA, UK Samar Safi-Harb Department of Physics and Astronomy, University of Manitoba, MB R3T 2N2, Canada Shinya Saito Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Hiroaki Sameshima Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Goro Sato Research Institute for Science and Engineering, Waseda University, Tokyo 169-8555, Japan Kosuke Sato Department of Physics, Tokyo University of Science, Tokyo 162-8601, Japan Rie Sato Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Makoto Sawada Department of Physics and Mathematics, Aoyama Gakuin University, Kanagawa 229-8558, Japan Peter Serlemitsos NASA/Goddard Space Flight Center, MD 20771, USA Hiromi Seta Department of Physics, Saitama University, Saitama 338-8570, Japan Aurora Simionescu Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Randall Smith Harvard-Smithsonian Center for Astrophysics, MA 02138, USA Yang Soong NASA/Goddard Space Flight Center, MD 20771, USA Łukasz Stawarz Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Yasuharu Sugawara Department of Physics, Chuo University, Tokyo 112-8551, Japan Satoshi Sugita Department of Physics, Ehime University, Ehime 790-8577, Japan Andrew Szymkowiak Yale Center for Astronomy and Astrophysics, Yale University, CT 06520-8121, USA Hiroyasu Tajima Department of Physics, Nagoya University, Aichi 338-8570, Japan Hiromitsu Takahashi Department of Physical Science, Hiroshima University, Hiroshima 739-8526, Japan Hiroaki Takahashi Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan Yoh Takei Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Toru Tamagawa RIKEN, Saitama 351-0198, Japan Takayuki Tamura Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Keisuke Tamura Department of Physics, Nagoya University, Aichi 338-8570, Japan Takaaki Tanaka Department of Physics, Kyoto University, Kyoto 606-8502, Japan Yasuo Tanaka Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Yasuyuki Tanaka Department of Physical Science, Hiroshima University, Hiroshima 739-8526, Japan Makoto Tashiro Department of Physics, Saitama University, Saitama 338-8570, Japan Yuzuru Tawara Department of Physics, Nagoya University, Aichi 338-8570, Japan Yukikatsu Terada Department of Physics, Saitama University, Saitama 338-8570, Japan Yuichi Terashima Department of Physics, Ehime University, Ehime 790-8577, Japan Francesco Tombesi NASA/Goddard Space Flight Center, MD 20771, USA Hiroshi Tomida Tsukuba Space Center (TKSC), Japan Aerospace Exploration Agency (JAXA), Ibaraki 305-8505, Japan Yohko Tsuboi Department of Physics, Chuo University, Tokyo 112-8551, Japan Masahiro Tsujimoto Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Hiroshi Tsunemi Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan Takeshi Tsuru Department of Physics, Kyoto University, Kyoto 606-8502, Japan Hiroyuki Uchida Department of Physics, Kyoto University, Kyoto 606-8502, Japan Yasunobu Uchiyama Department of Physics, Rikkyo University, Tokyo 171-8501, Japan Hideki Uchiyama Science Education, Faculty of Education, Shizuoka University, Shizuoka 422-8529, Japan Yoshihiro Ueda Department of Astronomy, Kyoto University, Kyoto 606-8502, Japan Shutaro Ueda Department of Earth and Space Science, Osaka University, Osaka 560-0043, Japan Shiro Ueno Tsukuba Space Center (TKSC), Japan Aerospace Exploration Agency (JAXA), Ibaraki 305-8505, Japan Shinichiro Uno Faculty of Social and Information Sciences, Nihon Fukushi University, Aichi 475-0012, Japan Meg Urry Yale Center for Astronomy and Astrophysics, Yale University, CT 06520-8121, USA Eugenio Ursino Physics Department, University of Miami, FL 33124, USA Cor de Vries SRON Netherlands Institute for Space Research, Utrecht, The Netherlands Shin Watanabe Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Norbert Werner Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, CA 94305, USA Dan Wilkins Department of Astronomy and Physics, Saint Mary’s University, Nova Scotia B3H 3C3, Canada Shinya Yamada Department of Physics, Tokyo Metropolitan University, Tokyo 192-0397, Japan Hiroya Yamaguchi NASA/Goddard Space Flight Center, MD 20771, USA Kazutaka Yamaoka Department of Physics, Nagoya University, Aichi 338-8570, Japan Noriko Yamasaki Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan Makoto Yamauchi Department of Applied Physics, University of Miyazaki, Miyazaki 889-2192, Japan Shigeo Yamauchi Department of Physics, Faculty of Science, Nara Women’s University, Nara 630-8506, Japan Tahir Yaqoob NASA/Goddard Space Flight Center, MD 20771, USA Yoichi Yatsu Department of Physics, Tokyo Institute of Technology, Tokyo 152-8551, Japan Daisuke Yonetoku Faculty of Mathematics and Physics, Kanazawa University, Ishikawa 920-1192, Japan Atsumasa Yoshida Department of Physics and Mathematics, Aoyama Gakuin University, Kanagawa 229-8558, Japan Takayuki Yuasa RIKEN, Saitama 351-0198, Japan Irina Zhuravleva Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, CA 94305, USA Abderahmen Zoghbi Department of Astronomy, University of Maryland, MD 20742, USA John ZuHone NASA/Goddard Space Flight Center, MD 20771, USA
Abstract

X-ray observations provide a powerful tool to probe the central engines of active galactic nuclei (AGN). A hard X-ray continuum is produced from deep within the accretion flow onto the supermassive black hole, and all optically thick structures in the AGN (the dusty torus of AGN unification schemes, broad emission line clouds, and the black hole accretion disk) “light up” in response to irradiation by this continuum. This White Paper describes the prospects for probing AGN physics using observations of these X-ray reflection signatures. High-resolution SXS spectroscopy of the resulting fluorescent iron line in type-2 AGN will give us an unprecedented view of the obscuring torus, allowing us to assess its dynamics (through line broadening) and geometry (through the line profile as well as observations of the “Compton shoulder”). The broad-band view obtained by combining all of the ASTRO-H instruments will fully characterize the shape of the underlying continuum (which may be heavily absorbed) and reflection/scattering, providing crucial constraints on models for the Cosmic X-ray Background with a subsequent impact on understanding of supermassive black hole evolution. ASTRO-H will also permit the relativistically broadened reflection spectrum from the inner accretion disk to be robustly studied, even in complex systems with, for example, warm absorption and composite soft excesses. Finally, the HXI will allow the detection and study of reverberation delays between the continuum and the Compton reflection hump from the inner disk.

ASTRO-H Space X-ray Observatory

White Paper

AGN Reflection

C. Reynolds (University of Maryland), Y. Ueda (Kyoto University), H. Awaki (Ehime University),

L. Gallo (Saint Mary’s University), P. Gandhi (University of Durham111Also at University of Southampton),

Y. Haba (Aichi University of Education), T. Kawamuro (Kyoto University), S. LaMassa (Yale University), A. Lohfink (University of Maryland222Also at University of Cambridge), C. Ricci (Kyoto University), F. Tazaki (Kyoto University333Also at National Astronomical Observatory of Japan),

and A. Zoghbi (University of Maryland444Also at University of Michigan)

on behalf of the ASTRO-H Science Working Group

Figure Credit: ESA / V. Beckmann (NASA)

1 General Introduction

After over four decades of study, active galactic nuclei (AGN) continue to be of great interest to astrophysicists. With the realization that supermassive black holes (SMBHs) are ubiquitous, being present at the center of essentially every galaxy, a tremendous amount of attention is focused on the co-evolution of SMBHs and galaxies. The tight correlation between the mass of the SMBH in a galactic center and the velocity dispersion of the stellar budge (Gebhardt et al. , 2000; Ferrarese & Merritt , 2000) found in the local universe strongly suggests that SMBHs and host galaxies co-evolved. In the extreme (probably realized in massive galaxies), a SMBH can dramatically suppress baryonic cooling and star formation in the galaxy, all-but truncating any further growth of the galaxy. AGN are also interesting in their own right, providing one of the most accessible laboratories for studying the extremes of physics found close to the horizon of a black hole (BH).

Figure 1: The anatomy of an AGN as according to the standard unified model. Figure from Urry & Padovani (1995)

Any study of AGN must start by characterizing their “engineering blueprint”, i.e., the properties of the SMBH (mass and spin), the distribution of circumnuclear matter, the (inward and outward) flow of matter, and the forms taken by the liberated energy as it leaves the AGN. Our current understanding is summarized in Figure 1. At its heart, an AGN consists of a SMBH fed by an accretion disk. Powerful winds can be produced from the accretion disk which probably produce the optical broad line region (BLR) with characteristic velocities of 2,000–20,000 . These broad optical lines are the defining characteristic of the classical unabsorbed (type-1) AGN. Further out, we know that many AGN possess a cold and dusty structure (the “dusty torus”) that can, depending upon viewing angle, obscure the BLR and the central accretion disk, leading to a classification as an obscured (type-2) AGN. The nature (and even the location) of this important structure is unclear. The torus may be the reservoir for the accretion disk, being fed by cold gas flows from the ISM of the galaxy — in other words, it is gas on the way in. Alternatively, it may be the colder/outer regions of the disk wind — gas on the way out. Both possibilities may be realized across the AGN population. In either case, “the torus” is the interface of the AGN with the rest of the galaxy, and understanding its basic nature is crucial if we are to understand the AGN-galaxy link.

Figure 2: Example of an X-ray reflection spectrum, assuming a slab of matter irradiated by a power-law spectrum with a photon index (red dashed line). The surface of the slab is assumed to have an ionization parameter of . Figure produced using the xillver code of Garcia et al. (2013)

X-ray spectroscopy is a powerful tool for determining the engineering blueprint of an AGN. X-rays are produced deep within the heart of the AGN, within a few gravitational radii (, where is the mass of the SMBH) of the black hole. Any optically-thick structures in the AGN (the accretion disk, BLR clouds, and the torus) will then be irradiated by the X-ray continuum and respond by producing an “X-ray reflection spectrum”. An example of an X-ray reflection spectrum is shown in Figure 2. The classic signatures of X-ray reflection are a strong iron-K emission line (at energies 6.4–6.97 keV depending upon the ionization state of the reflector) and a broad hard X-ray hump peaking at 20 keV where Compton reflection dominates over photoelectric absorption (at lower energies) and Compton recoil losses (at higher energies). If the reflector has a moderate-to-high ionization parameter, as is the case for the inner accretion disk, the reflection spectrum also possesses a forest of soft X-ray radiative-recombination features.

The iron line is a crucial diagnostic of AGN structure; iron is an abundant element and possess strong emission/absorption features that are relatively isolated from other spectral complexities. The iron line is to AGN/X-ray astronomers what the CO rotational lines are to star-formation/mm-wave astronomers. Detailed studies of reflection spectra allow us to study the distribution and kinematics of gas flowing in, out and around the SMBH; with this tool, we can start to determine the blueprint of the AGN central engine.

This White Paper (WP) discusses the impact of ASTRO-H on studies of AGN structure using X-ray reflection. The WP is divided into two parts. We start (Sections 2 and 3) by discussing the ability of ASTRO-H to map out the structures that are distant from the SMBH. Section 2 discusses the impact of ASTRO-H on studies of photoionized winds and the torus in general type-2 AGN, whereas Section 3 focuses on the particularly interesting case of Compton-Thick AGN. The superior spectral resolution of the ASTRO-H/SXS and the superior bandbass achieved by combining SXS and HXI data will transform our knowledge of these systems. As already mentioned, an understanding of AGN winds and the torus is crucial if we wish to truly understand how the AGN is fueled and how it feeds back on its host galaxy. The second part of this WP (Section 4) discusses the ability of ASTRO-H to study X-ray reflection from the inner accretion disk, where relativistic Doppler and gravitational redshifts can strongly skew the observed spectrum. Reflection from the inner disk is a broad-band phenomenon, resulting in a soft excess (as the radiative recombination lines are smeared into a pseudo-continuum), the broadened iron line, and the Compton reflection hump. ASTRO-H will be the first observatory capable of simultaneously observing and characterizing in detail all three aspects of disk reflection. This energy reach represents an important advance.

2 Mapping the structure of obscured AGN

2.1 The X-ray View of Type-2 AGN

The basic nature of dusty tori in AGN remains unclear. We are ignorant about many of their most basic characteristics, including their location, size, total mass, clumpiness, dynamics, and relation to the accretion disk and BLR. Even the “definition” of the torus is ambiguous, and it is not entirely clear whether it is distinct structure or just a smooth continuation from the BLR. A particularly curious fact is that they must typically subtend a large solid angle as seen from the SMBH in order to produce the observed fraction of type-2 AGN. Theoretical studies suggest that it is not easy to stably sustain such a cold but large scale-height () structure. This implies that the torus is not just static structure but may be a sequence of dynamic phenomena like nuclear starburst (e.g., Hopkins et al., 2012; Wada, 2012). The total mass of a torus may be an important parameter reflecting the evolutional stage of the galaxy (Kawakatu & Wada, 2008).

High quality broad-band X-ray spectra give unique insights into the anatomy of an AGN. Hard X-rays have strong penetrating power against obscuration, enabling us to study the properties of the obscuring matter and surrounding gas. Type-2 AGN are particularly well suited for a study of AGN structure; (1) information on the line-of-sight material can be obtained through X-ray absorption, (2) photoionized gas located outside the torus (in the narrow line region; NLR) can be observed in emission and scattering lines that gives definite probes on its physical state, (3) the equivalent widths of iron-K lines from the obscuring torus become large thanks to the attenuated continuum level and hence are more readily characterized, and (4) the high inclination angles make it easier to measure Keplerian motion of line emitting matter.

The typical X-ray spectrum of a type-2 AGN is characterized by the combination of a heavily absorbed primary power-law, Compton reflection with fluorescence lines from the cold torus (with additional reflection possible from the BLR and accretion disk), and soft X-ray emission dominated by the emission lines from highly ionized gas (Turner et al., 1997). The soft emission lines can provide diagnostic tools to reveal the temperature, density, and ionization state of the gas surrounding the supermassive black hole.

Figure 3: Left panel : The spectrum of Mrk 3 as observed by the Suzaku/XIS in 2005. The continuum (direct/absorbed an scattered/unabsorbed) is shown as dotted orange line. A strong cold reflection component is marked as a solid orange line. The complex soft spectrum is described as coming from three different photoionized plasmas (light blue; 0.01, 1.010 cm, green; 1.8, 1.410 cm, blue; 2.9, 2.010 cm) and an optically-thin thermal plasma (magenta; apec in XSPEC) with temperature of 1.0 keV. Right panel : The simulated SXS spectrum of Mrk 3 for a 200 ksec exposure based on the spectral model for Mrk 3. We employ the redistribution matrix function (RMF) with 5 eV resolution, the current best-estimated (file ah_sxs_5ev_basefilt_20100712.rmf), and the ancillary response file (ARF) for the point source (file sxt-s_120210_ts02um_of_intallpxl.arf).

As an illustration, Figure 3 (left panel) shows the Suzaku spectrum of the prototypical Seyfert-2 galaxy Mrk 3 (), one of the brightest objects among the class (Cappi et al., 1999). Despite having an absorption column that is marginally Compton-Thick, we can see still see the direct (absorbed) power-law continuum at high-energies. We also see that some fraction of this continuum is scattered around the the torus. A cold X-ray reflection component from, presumably, Compton-Thick regions of the torus out of our line of sight produces a strong 6.4 keV iron fluorescence line and contributes significantly to the continuum above 5 keV. The soft-band is very complex (Sako et al., 2000; Pounds & Page, 2005; Awaki et al., 2008), requiring photoionized emitters with at least three different ionization parameters as well as a collisionally ionized thermal plasma component (see figure caption).

2.2 Astro-H/SXS studies of type-2 AGN

The superior resolution of the ASTRO-H/SXS will permit a giant leap forward in the study of these line-rich AGN. For example, Figure 3 (right panel) shows a simulation of a 200 ks SXS observation of Mrk 3. Comparing with the Suzaku/XIS spectrum, we can see that the forrest of soft X-ray emission lines is resolved, allowing us to employ the full machinery of line ratio diagnostics for density, temperature, and excitation mechanism. The K-triplet lines from helium-like ions are particularly useful (Gabriel & Jordan, 1969; Porquet & Dubau, 2000). While these soft X-ray lines have already been seen at such resolutions by the grating instruments on Chandra and XMM-Newton, ASTRO-H/SXS provides significantly more sensitivity at soft energies (permitting the full spectral resolution to be realized in realistic exposure times) and, simultaneously, unprecedented resolution of the iron line complex.

The ability to resolve and characterize the velocity profile of the fluorescent iron line will permit the first study of the dynamics of the X-ray reflecting torus. At the same time, the resolution of the SXS will greatly facilitate our ability to centroid the K line as well as detect the K line — both of these observables are sensitive to the ionization state of the gas. Putting this information together will permit us to determine the location (), size () and density () of the torus material — the velocity broadening gives us the location from Keplerian arguments (), the dominant ionization states of iron tell us the ionization parameter (, where is the ionizing luminosity) and the combination of these two yields the density. Comparing the density with the line of sight column density (which can be measured from the continuum absorption, provided that the AGN is Compton-thin) gives the size of the torus .

While detailed dynamical and ionization models will be needed to interpret the real results, we can obtain a first look at the impact of ASTRO-H/SXS results by assuming that the torus has a single ionization parameter and the form of a disk-like structure in Keplerian motion about the SMBH. For this exercise, we use the XSTAR photoionization code to model the scattered and emitted spectrum of a torus with a density of cm, a column density of cm irradiated by a Seyfert-like X-ray source (luminosity of erg s (0.01–10 keV) and a power-law spectrum of ). We adopt three different distances for the torus, 1 pc, 0.1 pc, and 0.01 pc, which we designate the “far torus”, “near torus”, and “BLR” cases, respectively. These tori spectra are then convolved with the Doppler broadening appropriate for a disk in Keplerian motion (using the diskline model with an emissivity profile ) assuming an inclination of 45.

Figure 4: Simulated spectra of NGC 4388 with the SXS, assuming 300 ks exposure. Three cases shown are the far torus (left), near torus (middle) and BLR (right).

Figure 4 shows a simulated 300 ks SXS spectra in the iron-K band for NGC 4388, the brightest obscured Compton-thin AGN with a 14–195 keV flux of (Baumgartner et al., 2013). It is clearly seen that details of the 6.4 keV line profile are resolved, in this case revealing the double-peak structure characteristic of the (assumed) keplerian disk. We can use the centroid and K/K line ratios to constrain the dominant ionization state of the iron; for the near torus case, we obtain the range Fe II–Fe VI, consistent with the XSTAR model that is dominated by Fe II. In this simulated case, we can also constrain the inner radius of the torus to better than 3%, and measure mean bulk motion with a precision of km s.

While the parameters of this simulation are clearly simplistic, it highlights the fact that ASTRO-H will open a new window on AGN tori.

2.3 Broadband Continuum studies of Type-2 AGN with Astro-H

The Cosmic X-ray Background (CXB) results from the integrated X-ray emissions of all the AGN in the Universe, and the spectrum, normalization and spatial fluctuations of the CXB are important constraints on models for the cosmological evolution of SMBHs. While it is spectrally smooth, the CXB has a substantially harder spectrum than any known unabsorbed AGN and, in fact, absorbed AGN are crucial components any CXB model. A good knowledge of the reflection and continuum parameters of AGN is fundamental for the creation of such models. Especially important but ill-constrained are the cut-off energies for the power-law continua from AGN resulting from the finite temperatures of the X-ray emitting coronae. This is another area where ASTRO-H will make a major impact, this time due to its ability to simultaneously determine the parameters of the primary continuum, scattering of that continuum, reflection, and the continuum cut-off.

Again, we illustrate this with the example of NGC 4388. A broad-band study of this source performed combining XMM-Newton EPIC/PN, INTEGRAL IBIS/ISGRI and Swift/BAT data shows an absorbed continuum with a photon index of and moderate levels of reflection (Ricci et al. in prep). However, even with this array of data, the high-energy cutoff of the power-law could not be determined.

To appreciate the importance of the high-energy cut-off, it is necessary to consider the physical processes responsible for producing the primary X-ray continuum. The primary X-ray continuum is thought to be produced through Comptonization of the thermal optical/UV photons from the accretion disk by hot electrons in a magnetically energized corona (e.g., Haardt & Maraschi, 1993). The most basic parameters that we need to know about the corona if we wish to understand its nature and origin are its temperature and optical depth . Now, the resulting spectrum is approximated as an exponentially cut-off power-law, with a cut-off energy at . If we only have knowledge of the photon index of the power-law, we can only constrain the combination (proportional to the so-called Compton -parameter). Only if we measure the high-energy cutoff we can break the degeneracy between these fundamental coronal parameters.

Figure 5: Left panel: 100 ks simulation of the broad-band ASTRO-H spectrum of NGC 4388. Shown here are data from the SXS (red), SXI (black), HXI (blue and green), and SGD (magenta). Right panel: contour plot of the reflection component versus the energy of the cutoff obtained by fitting the simulated 100 ks ASTRO-H observation of NGC 4388. The cross represents the best set of parameters obtained by the fit, while the three contours are the 68%, 90% and the 99% confidence regions.

Very recent NuSTAR results are already demonstrating the dramatic impact that a focusing hard X-ray telescope is having on our abilities to measure cut-off energies in AGN spectra (see study of IC4329A; Brenneman et al. in prep). ASTRO-H will take these studies to the next level, providing NuSTAR quality spectra from the HXI with simultaneous soft X-ray data from the SXI/SXS and harder data from the SGD. Figure 5 (left) illustrates this with a 100 ks multi-instrument simulation of an ASTRO-H observation of NGC 4388. In a single observation, the spectral shape can be determined with high precision from 0.5–80 keV, and the SGD detection gives us an important lever-arm out to  keV on our ability to determine cut-off energies. In this simulation, we assumed a reflection strength (measured relative to that obtained from a source above an infinite slab) of , and cut-off energy of  keV. As can be seen in Figure 5 (right), the ASTRO-H multi-instrument dataset allows us to break any degeneracy between and , and measure each to a high precision; and  keV. The constraints on the cut-off energy are systematically improved as that energy is lowered and more of the curvature is placed into the HXI band, with 12% errors if  keV and 7% errors for  keV. However, even for  keV, we can still detect the cut-off and measure its energy to %.

Figure 6: Extract of the spectrum obtained by a 100ks ASTRO-H observation of NGC 4388 simulated using a Comptonization model for the continuum ( keV, ). The simulated spectrum was fitted using a cutoff power-law to account for the primary X-ray emission, which, as it can be seen from the bottom panel, overestimates the flux above 150 keV.

An exponentially cutoff power-law is only a first approximation to the X-ray continuum of AGN. The precise form of the spectrum produced by a physical thermal Comptonization model can be crudely approximated by an exponential power-law across a certain range of energies, but will deviate significantly from that simple model for . Once we are sensitive to these deviations, we have opened a new window on the geometry and structure of the corona. Here, the combination of the HXI and SGD on ASTRO-H will make a qualitative advance. We illustrate this for the case of NGC 4388 in Figure 6; we simulate a 100 ks multi-instrument spectrum using a physical Comptonization model (compPS, Poutanen & Svensson, 1996) but fit the simulated data with an exponential powerlaw. Assuming a coronal temperature of  keV, we can see that dramatic and easily measurable deviations from the exponential cutoff power-law model are seen above 150 keV.

3 The Nature of Compton-Thick AGNs

3.1 The Importance of Compton-Thick AGN

The shape of the CXB requires that a significant population of highly obscured AGN must exist. At the extreme end of the distribution lies the Compton-Thick AGN (CTAGN), those for which the electron scattering optical depth to the central engine exceeds unity implying gas column densities exceeding cm. For obvious reasons, this makes them difficult to find — we must either look in the highest energy X-ray bands (some fraction of which can still penetrate the obscurer unless ) where sensitivity has historically been challenging or search for secondary/reprocessed signatures. Their unknown prevalence represents the most important remaining factor affecting our understanding of the composition of the CXB (Ueda et al., 2003; Gilli et al., 2007), and is a major uncertainty in our understanding of the coevolution of galaxies with their SMBHs. To put it bluntly, our knowledge of up to half of the accretion energy budget of the universe remains hidden from view, with our current knowledge being extrapolations from biased data.

Being extreme objects, CTAGN are also interesting in their own right. It is unknown whether they are a disjoint population, possibly corresponding to some given phase in the life of a merger-driven AGN, or simply one end of the distribution of normal AGN. Neither do we know their cosmological evolution. Hierarchical growth models posit that the nuclei of all large galaxies develop under large (probably Compton-Thick) columns of gas that feed as well as obscure the growing SMBH (Fabian, 1999; Hopkins et al. , 2006). This implies that the CTAGN abundance ought to evolve positively with redshift, and recent results appear to support this (e.g., Brightman & Ueda, 2012). Changing preliminary evidence into proof requires secure identification of statistically-significant samples of CT AGN, as well as detailed spectral follow-up to measure physical parameters such as their covering factor.

Here, we discuss the impact of ASTRO-H on our understanding of the physical nature of CTAGN. Again, this comes both from the high-spectral resolution of the SXS and the remarkable broad-band capabilities of ASTRO-H.

3.2 The Compton Shoulder as a Probe of the Obscurer

Figure 7: Monte Carlo simulations of Compton shoulders for various column densities. A torus geometry is assumed following Ikeda et al. (2009), with a half opening angle of and a viewing angle of (i.e., grazing the edge of the torus). For simplicity, the scatters are assumed to be cold free electrons.

As explained in Section 1, iron fluorescence results when cold matter is irradiated by a hard X-ray continuum. If the irradiated structure is Compton-Thick, iron line photons that are produced heading into the interior can be Compton scattered back towards the surface and, with some probability, to the observer. Due to Compton-recoil, these scattered iron line photons are downshifted in energy by and form a “Compton shoulder” sitting redwards of the main line. In fact, there is a series of Compton shoulders corresponding to iron line photons that have been once-scattered, twice-scattered etc., each becoming successively downshifted and broadened compared with the previous (see Figure 7).

The detailed strength and shape of the main shoulder is a novel probe of the geometry and conditions of the reflector. Its detailed shape can be used to determine if the scattering electrons are bound in atoms/molecules or free (see also White Paper 17), and whether the observed iron line does in fact come from a Compton-Thick structure, even if the line-of-sight absorption is Compton-thin. Calculations of the type shown in Figure 7 reveal that the relative strength of the Compton shoulder decreases with increasing the half opening angle of the Compton thick torus. Thus we can tell whether an AGN is deeply buried, i.e. almost surrounded by Compton-Thick material, by looking for a strong Compton shoulder.

While hints of the Compton shoulder have been seen in Chandra grating data, the ASTRO-H/SXS is the first instrument capable of truly utilizing this diagnostic. Figure 8 shows a simulated SXS spectrum from a 100 ks observation of the Circinus galaxy, assuming a spectral model with a Compton-Thick torus, and a half opening angle of 30. Thanks to the intense iron line in this confirmed CTAGN, the Compton shoulder will be clearly observed.

Figure 8: Simulated SXS spectrum of the Compton-Thick Circinus galaxy in the iron-K band. The exposure is 100 ks.

3.2.1 Broadband Continuum Studies of CTAGN

For understanding the nature of a CTAGN, it is critical to accurately constrain the column density and its intrinsic luminosity. With its unique combination of broad band-pass and sensitivity, ASTRO-H will permit unprecedented studies of the continuum in CTAGN. We illustrate this with the case of NGC 4945, a bright AGN with a line-of-sight column of which completely extinguishes any primary continuum below 10 keV. Prior studies have shown that the X-ray spectrum is dominated by scattered continuum (below 10 keV) and a reflection component (above 10 keV), with the absorbed primary continuum remaining subdominant out beyond 50 keV (see Figure 9, left).

Figure 9 (right) shows simulated SXS/SXI/HXI spectra from a 10 ks ASTRO-H observation of NGC 4945. It is clear that the continuum shape can be defined even in such a short observation; the photon index can be measured to and the column density can be constrained with 20% errors. While NGC 4945 is very local () and extremely bright, similar constraints can be obtained for a typical CTAGN at with a 200 ks exposure.

Figure 9: Left: Spectral model for NGC 4945. Right: Simulated SXS (red), SXI (black) and HXI (green) spectra of NGC 4945, with a 10 ks exposure.

4 Probes of the Relativistic Accretion Disk and SMBH

4.1 Into the Heart of the AGN

Figure 10: Effects of relativistic Doppler and gravitational redshift effects on an ionized reflection spectrum assuming a viewing inclination of , irradiation index of , and a rapidly spinning BH (; black line) or non-spinning (; blue line) BH. Figure from Reynolds (2013).

In order to understand the AGN phenomenon, we must ultimately understand the physics within a few gravitational radii of the black hole where the vast majority of the energy is released. X-ray irradiation of the ionized inner regions of the accretion disk, and the associated X-ray reflection, gives us our cleanest probe to date of this region. As illustrated in Figure 10 Spectral features in the reflected X-ray emission are strongly broadened and skewed by the Doppler effect from the accretion flow’s orbital motion as well as gravitational redshifts as the photons climb out of the deep potential well (Tanaka et al., 1995; Fabian et al., 2000; Reynolds & Nowak, 2003). In addition to producing the well-known broad iron line, ionized reflection from the inner disk can also produce at least some part of the soft excess as well as a broadened Compton reflection hump.

To study the inner accretion disk, we must disentangle these spectral features from other complexity. Even in sources where the line-of-sight to the inner disk is Compton-thin, there may still be significant absorption features imprinted into the spectrum from partially photoionized material (the so-called warm absorber). As discussed in the first part of this WP, emission signatures from scattering/reflection of X-rays by distant (low velocity) matter can further contribute to and complicate the spectra. As we will describe below, ASTRO-H will provide powerful new ways of disentangling these complexities from the accretion disk features.

The primary X-ray source is highly variable. So, in addition to the spectrum, timing provides another way to probe the heart of the AGN. Particularly exciting is the discovery of reverberation time delays in the XMM-Newton and Suzaku data of some bright AGN. It has long been predicted that, since the X-ray source is external to the accretion disk, there will be light travel induced time-lags between the observed continuum changes and the observed response of the reflection (Reynolds et al., 1999). Using XMM-Newton and Suzaku, these reverberation delays have now been seen in the (soft) reflection spectrum of several narrow line Seyfert 1 galaxies (Zoghbi et al., 2010; De Marco et al., 2013), as well as in the broad iron line of several hard X-ray bright AGN (Zoghbi et al., 2012).

4.2 Disentangling the Accretion Disk Spectrum From Other Complexities

The disk reflection spectrum is a broad-band component, producing a soft excess, a broad iron line and a hard X-ray bump. When extracting accretion disk (or SMBH spin) parameters from an X-ray spectrum, it is crucial to know the X-ray continuum that is superposed on this disk reflection spectrum as well as the effects of any absorption. ASTRO-H is a powerful observatory for disentangling even complex AGN spectra. The SXI and HXI provide a high signal-to-noise and broad-band view of the spectrum, allowing us to simultaneously study the continuum, soft excess and Compton hump. For bright objects or long exposures, the SXS provides a high-fidelity view of narrow emission and absorption lines, removing any influence that such features may have on the modeling of the underlying broadened disk features. Taken all together, ASTRO-H will give us our best ability to date to study broad iron lines and relativistic disk reflection in a manner that is robust to the other spectral complexities.

Figure 11: The spectral model adopted for the simulations is similar to that of Mrk 335 in the intermediate flux state. The model is composed of a power law continuum, a blurred reflection component (blue line), and a distant reflector. The broad-band continuum is modified by a three-zone warm absorber and a Galactic column density.

Figure 12: A power law plus distant reflector model is fitted to the 200 ks simulated spectra of an AGN with . The residuals in each instrument are shown on the left. The broad component becomes visible in all detectors and the SXS begins to reveal the structure of the warm absorber. A blurred reflector and warm absorber are then added to the model. The residuals from the final fit are shown on the right.

We illustrate the ability of ASTRO-H to disentangle warm absorption, torus reflection and disk reflection by adopting the spectrum of Mrk 335 () as a representative of the “typical” type-1 Seyfert population. Using XMM-Newton data, Gallo et al. (2013) find that this object displays a complex warm absorber (i.e. multiple zones of photoionized absorption) and reflection from a torus, in addition to the relativistically blurred reflection from the central regions of a moderately ionized, , accretion disk (see Figure 11). We simulate a 200k̇s ASTRO-H observation of this spectrum, assuming a 2–10 keV source flux of ; this is brighter than is typical for Mrk 335, but well within the flux range for many other similar type-1 Seyfert galaxies.

Figure 12 (left panels) shows the residuals that remain when we fit the  keV spectrum with a model consisting of the power-law and torus reflection but does not include the warm absorber or the accretion disk. The unmodelled broad iron line can be clearly seen in both the SXI and SXS residuals, and the unmodelled Compton reflection from the accretion disk is apparent in the HXI residuals. Furthermore, sharp narrow absorption lines in the SXS result from the unmodelled warm absorption. When the full spectral model is used, the residuals are flat as expected (Figure 12, right) and we can obtain excellent constraints on the parameters of the relativistic disk — we recover the inner edge of the disk to (input ), the inclination to (input ), the irradiation index to (input ) and the disk iron abundance to (input ). The disk parameters can be recovered despite the presence of the highly ionized absorber that affects the iron band.

An interesting point to note is the relative roles played by the SXI, SXS and HXI. While contributing significant signal-to-noise in the detection of broad features in the 3–10 keV band, the principal role of the SXS is to detect and characterize absorption features, thereby removing any remaining degeneracies in the fits to the disk reflection arising from uncertainties in absorption. Using just the soft X-ray detectors (the SXI and SXS), we can detect the presence of blurred reflection but cannot statistically distinguish the actual blurring parameters () from some default set (). It is only with the inclusion of the HXI data that the blurring parameters can be constrained in detail. This follows from the modest effective areas of the SXI and SXS compared with the HXI.

The uncertain nature of the soft excess can also be a source of uncertainty when attempting to constrain the accretion disk parameters. For example, Lohfink et al. (2012) examined multi-epoch XMM-Newton and Suzaku data for the unabsorbed Seyfert nucleus in Fairall 9 and found that, while the presence of relativistically blurred disk reflection was robust, the inferred black hole spin and disk iron abundance depended strongly upon whether the soft excess was model as an additional ionized blurred reflection (beyond that needed to probe the iron line) or thermal Comptonization from lukewarm material. Part of the issue is that the broad line in Fairall 9 is not particularly strong compared to sources such as MCG–6-30-15 or NGC3783 — however, it may be representative of “normal” sources with regards to its broad line strength.

Figure 13: Simulated 150 ks spectra of the Seyfert I galaxy Fairall 9, assuming a model with cold and ionized reflection, as well as a Comptonization soft excess. Shown here is the fit to the SXS [blue], SXI [black], HXI [red] spectra with a double ionized-disk-reflection scenario but no luke warm Comptonization component. The precise form of the residuals clearly shows that the two scenarios can be distinguished.

ASTRO-H will be able to slice through the degeneracies responsible for the current ambiguities in a Fairall 9 like source. To explicitly demonstrate this, we have adopted the “Comptonization soft excess” scenario for Fairall 9 and simulated 150 ks exposures with the SXI, SXS and HXI, assuming a typical 0.5–10 keV flux level of . To maximize realism, we also redshift the spectrum to , the redshift of Fairall 9 (and quite typical for many Seyfert galaxies that we will wish to study). Figure 13 shows a fit to these simulated spectra with the “wrong” soft-excess model, namely an additional blurred ionized disk component on top of that needed to produce the iron line. Residuals clearly remain at the softest and hardest energies, showing that ASTRO-H can resolve this tough degeneracy.

4.3 X-ray Reverberation from the Inner Disk

Figure 14: Recovered time-lags in simulated HXI data. The input simulation assumes a 1 ks time lag (constant for all Fourier frequencies) between the continuum band (7–10 keV) and the hard band containing the time-delayed Compton hump (20–50 keV). The simulation includes gaps in the lightcurve appropriate for a low-Earth satellite, and the quoted exposure time is the “on source” time. The time lags are recovered using Fourier techniques that incorporate a maximum likelihood technique to handle the data gaps (Zoghbi et al. in prep).

As discussed in §4.1, XMM-Newton and Suzaku studies of bright AGN have recently opened an exciting new frontier in the study of reverberation effects from the inner accretion disk. Here, we assess the impact that ASTRO-H will have on these studies.

The total number of detected photons, and hence the effective area of the ASTRO-H instruments, is key to whether reverberation lags can be detected. To formally assess detectability, we have simulated pairs of light curves assuming a standard spectral shape (Figure 11) with a fixed time-delay between the direct power-law and the reflected disk emission. For definiteness, we assume 1 ks time lags at all temporal frequencies. We have considered two average BAT-band flux levels ( and ), two levels of variability (10% and 20% rms flux variability), and three observation lengths (100 ks, 200 ks and 400 ks “on-source” exposure time). For each pair of light curves, we add Poisson noise appropriate for the SXI, SXS and HXI. We also introduce gaps in the lightcurve appropriate to a satellite in low Earth orbit. We then conduct an analysis of the light curves in order to recover the time lags using the Fourier techniques laid out in Zoghbi et al. (2010), treating the gaps with a maximum likelihood method described in Zoghbi et al. (2013).

We find that, for these parameters, the SXI and SXS cannot detect lags — the count rates are simply insufficient. However, lags in the Compton bump are readily detectable with the HXI. Using simulated light curves in the 7–10 keV and 20–50 keV bands (i.e., a continuum dominated band and a band with a significant Compton-reflection contribution), Figure 14 shows the recovered lags as a function of Fourier frequency. In the bright source scenario, we see that lags can be detected at an intermediate Fourier frequency in a 100 ks observation, but a 200 ks lightcurve is required in order to detect the lag across the Fourier spectrum. This is important since, in real sources, the lags will change as a function of Fourier frequency, and these changes are crucial for disentangling reverberation delays from hard-lags that are intrinsic to the physics of the X-ray continuum emission. In the faint source scenario, lags are detectable but a long (400 ks) observation will be required to gain even crude information on the frequency dependence.

5 Summary of Top Science

We end this WP with a brief summary of the “whys and hows” of our top science goals.

  1. OBJECTIVE : Characterization of the “torus” and other high column density obscuring structures in AGN.
    WHY : The basic nature of the torus is unclear; is it the reservoir for the accretion disk (inflow) or the outer parts of an AGN wind (outflow). In many ways, the torus is the “interface” between the AGN and the rest of the galaxy, so understanding its nature is important for understanding the AGN-galaxy connection. We also see to understand the basic nature of CTAGN, poorly understood objects that are crucial in models of the CXB and SMBH evolution.
    HOW : We will use a combination of detailed iron line diagnostics (profile, shifts, Compton shoulder) enabled by the ASTRO-H/SXS as well as the broad-band/hard coverage of ASTRO-H to characterize transmission and reflection from the torus, even in cases where it may be Compton-Thick.

  2. OBJECTIVE : Define the X-ray continuum shape of AGN, from the softest energies observable to energies beyond their high-energy cutoff.
    WHY : A broad-band characterization of the continuum, correcting for absorption and reflection effects, is crucial for understanding the energetics of the AGN population and the true nature of the CXB. Robust determinations of the high-energy cutoff are needed to access the physics of the corona.
    HOW : Using the combination of all four instruments, ASTRO-H can cover the range 0.5–200 keV with unprecedented sensitivity. The SGD in particular will enable us to go beyond the exponentially-cutoff powerlaw approximation for the Comptonized high-energy spectrum.

  3. OBJECTIVE : Robust characterization of the inner accretion disk reflection even in cases with complex absorption and composite soft excesses.
    WHY - We wish to probe accretion disk inclination, disk abundances, and black hole spin even in sources that are “complicated”, i.e., have complex warm absorbers or highly variable spectral shapes. Only then can we use disk reflection as a tool to undercover the true demographics of these properties.
    HOW - ASTRO-H/SXI+HXI will be the first observatory capable of, in a single observation, probing all three aspects of the disk reflection spectrum (the soft excess, broad iron line, and Compton hump). SXS spectroscopy will be important for characterizing and allowing us to remove the effects of absorption. Long SXI+HXI observations of bright and variable sources will allow us to see reverberation effects across the full spectrum.

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