Reflectivity around the gold M-edges of x-ray reflector of the Soft X-ray Telescope onboard ASTRO-H

Sho Kurashima; Akihiro Furuzawa; Toshiki Sato; Naomichi Kikuchi; Nozomi Nakaniwa; Yoshitomo Maeda; Manabu Ishida; Ryo Iizuka; Takashi Okajima; Hideyuki Mori; Hironori Matsumoto; Keisuke Tamura; Kazunori Ishibashi; Takayuki Hayashi; Takuya Miyazawa; Masato Maejima; Shun Yoshikawa

doi:10.1117/12.2231173

11 July 2016 Reflectivity around the gold M-edges of x-ray reflector of the Soft X-ray Telescope onboard ASTRO-H

Sho Kurashima, Akihiro Furuzawa, Toshiki Sato, Naomichi Kikuchi, Nozomi Nakaniwa, Yoshitomo Maeda, Manabu Ishida, Ryo Iizuka, Takashi Okajima, Hideyuki Mori, Hironori Matsumoto, Keisuke Tamura, Kazunori Ishibashi, Takayuki Hayashi, Takuya Miyazawa, Masato Maejima, Shun Yoshikawa

Author Affiliations +

Proceedings Volume 9905, Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray; 99053Y (2016) https://doi.org/10.1117/12.2231173
Event: SPIE Astronomical Telescopes + Instrumentation, 2016, Edinburgh, United Kingdom

Abstract

The X-ray astronomy satellite ASTRO-H are equipped with two equivalent soft X-ray telescopes (SXT-I and SXT-S) which cover the energy band 0.3{12 keV. The X-ray reflectors of the SXTs are coated with a gold monolayer by means of the replication technique (Okajima et al. in this volume). A series of gold M absorption edges in the 2-4 keV band causes complex structures in the energy response of the SXTs. In the same band, there are astrophysically important emission lines from Si, Ar and S. Since the SXS has unprecedentedly high spectral resolution, we have measured the reflectivity around the gold M-edges in an extremely fine energy pitch at the synchrotron radiation facility KEK PF BL11-B, with the 2 eV pitch in 2100 eV to 4100 eV band that covers the entire series of the absorption edges (M-I through M-V) at grazing incident angles to the reflectors of 0.5, 0.8, 1.0, 1.2, 1.4 degree, and with a finer pitch of 0.25 eV in the 2200 eV to 2350 eV band where the two deepest M-IV and M-V edges are included. In the resultant reflectivity curves, we have clearly identified the fine structures associated with all the M-edges. Using these data, we calculated atomic scattering factor f1 as a function of X-ray energy, with which we have built the mirror response function which can be applied to the Suzaku spectra. As a result, we have found that discrepancy of the spectral model to the Suzaku data of 4U1630-472 (a black hole transient) and the Crab nebula around the M-edges are significantly reduced from those with the official Suzaku response.

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Sho Kurashima, Akihiro Furuzawa, Toshiki Sato, Naomichi Kikuchi, Nozomi Nakaniwa, Yoshitomo Maeda, Manabu Ishida, Ryo Iizuka, Takashi Okajima, Hideyuki Mori, Hironori Matsumoto, Keisuke Tamura, Kazunori Ishibashi, Takayuki Hayashi, Takuya Miyazawa, Masato Maejima, and Shun Yoshikawa "Reflectivity around the gold M-edges of x-ray reflector of the Soft X-ray Telescope onboard ASTRO-H", Proc. SPIE 9905, Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray, 99053Y (11 July 2016); https://doi.org/10.1117/12.2231173

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