Prof. Hironori Matsumoto Profile

Prof. Hironori Matsumoto

Professor at Osaka Univ

SPIE Involvement:

Conference Program Committee | Author

Publications (62)

SPIE Journal Paper | 8 October 2019

Effect of barrier layer on moisture absorption of thin carbon-fiber-reinforced plastic mirror substrates

Hisamitsu Awaki, Tessei Yoshida, Chisato Oue, Nozomi Aida, Hironori Matsumoto, Tomohiro Kamiya

JATIS Vol. 5 Issue 04

KEYWORDS: Absorption, Mirrors, Coating, Diffusion, X-rays, Humidity, X-ray telescopes, Telescopes, Spatial resolution, Aluminum

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SPIE Journal Paper | 6 June 2019

X-ray imaging polarimetry with a 2.5-μm pixel CMOS sensor for visible light at room temperature

Kazunori Asakura, Kiyoshi Hayashida, Takashi Hanasaka, Tomoki Kawabata, Tomokage Yoneyama, Koki Okazaki, Shuntaro Ide, Hirofumi Noda, Hironori Matsumoto, Hiroshi Tsunemi, Hisamitsu Awaki, Hiroshi Nakajima

JATIS Vol. 5 Issue 03

KEYWORDS: X-rays, Polarimetry, X-ray detectors, Sensors, X-ray imaging, CMOS sensors, Polarization, Visible radiation, X-ray astronomy, Charge-coupled devices

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Proceedings Article | 20 July 2018 Presentation + Paper

The spectral response of X-ray CCDs in the energy band around Si-K edge: a solution to the Si-K edge problem for the XIS onboard Suzaku

Koki Okazaki, Kiyoshi Hayashida, Hiroshi Nakajima, Riku Shomura, Tomokage Yoneyama, Hironori Matsumoto, Hiroshi Tsunemi, Koji Mori, Masahiro Tsujimoto, Yoshitomo Maeda, Ken Ebisawa

Proc. SPIE. 10709, High Energy, Optical, and Infrared Detectors for Astronomy VIII

KEYWORDS: Cameras, Sensors, Calibration, Matrices, X-rays, Quantum efficiency, Charge-coupled devices, X-ray imaging, X-ray astronomy, Absorption

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X-ray Imaging Spectrometers (XIS) are the X-ray CCD cameras onboard Suzaku. They were operated in orbit from 2005 to 2015 and produced lots of findings with their good energy resolution and low non X-rat background. Precise calibration including the 10 eV accuracy in the energy scale reinforced them. Nevertheless, there has been a unresolved calibration issue in the spectral response around the Si-K edge (1.839 keV) appearing as systematic residuals up to 10%. The residual is negative peaking at 1.85 keV in the front illuminated (FI) sensors and positive peaking at 1.8 keV in the back illuminated (BI) sensor for X-ray sources dominated by continuum X-ray emission. Various attempts to eliminate these residuals by changing response parameters or quantum efficiency models have been insufficient. In this paper, we revisit this problem by focusing on the relation between incident X-ray energy and pulse height. We introduce a jump in that relation at the Si-K edge by modifying the , and optimize its value so as to minimize the residuals in the fit of the X-ray spectra for the black hole binary LMC X-3, a source dominated by continuum emission. We find the introduction of a jump significantly reduces the residuals. The optimized jump values are +4:2 channel, +4:0 channel, and -3:1 channel, corresponding to 15.3 eV, -11:3 eV, and 14.6 eV, for XIS0, XIS3 (FI), and XIS1 (BI), respectively. The direction of the jump is opposite for the FI and for the BI. We revise the response matrices generator so as to include the jump for each XIS sensor, and apply it to the X-ray spectra of the Perseus cluster of galaxies which has various emission lines in the spectra, and the blazar PKS2155-304 which was observed various epoch in the Suzakuoperation. We confirm the residuals are significantly reduced for these sources, too. We finally suggest the jump at Si-K edge in the energy and pulse height relation is qualitatively explained, if some of charges are lost in course of charger collection to the electrode of the CCD in the depletion later, and its amount is large for larger travel length in the depletion layer. If this explanation is correct, the Si-K edge problem and its solution presented in this paper is not specific only for the SuzakuXIS but also for other X-ray CCDs.

Proceedings Article | 10 July 2018 Presentation + Paper

Sub-arcsecond imaging with multi-image x-ray interferometer module (MIXIM) for very small satellite

Kiyoshi Hayashida, Tomoki Kawabata, Takashi Hanasaka, Kazunori Asakura, Tomokage Yoneyama, Koki Okazaki, Shuntaro Ide, Hironori Matsumoto, Hiroshi Nakajima, Hisamitsu Awaki, Hiroshi Tsunemi

Proc. SPIE. 10699, Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray

KEYWORDS: CMOS sensors, Interferometers, Sensors, Satellites, X-rays, X-ray sources, Interferometry, Collimators, X-ray imaging, X-ray detectors

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We have proposed a new type of X-ray interferometer called Multi Image X-ray Interferometer Module (MIXIM) consisting simply of a grating and an X-ray spectral imaging detector. The baseline concept of MIXIM is a slit camera to obtain the profile of X-ray sources, but aim to get a sub-arcsecond resolution. For that purpose, to avoid blurring of the image by diffraction is a key, and we select X-ray events of which energy satisfies the interferometric condition called Talbot effect. Stacking the images (X-ray interferometric fringes) with the period of the grating is another point of the method, which provides the self image of a grating slit convolved with the profile of the X-ray source. We started an experiment with a micro focus X-ray source, 4.8 μm pitch grating, and an SOI type X-ray detector XRPIX2b with a pixel size of 30 μm. The stacked self image was obtained with a magnification factor of 4.4. We, however, need finer positional resolution for the detector to obtain the self image to a parallel beam, for which the magnification factor must be 1. We thus focused on small pixel size CMOS sensors developed for visible light. We irradiated X-rays to one of such CMOS sensors GSENSE5130 with a pixel size of 4.25 μm, and found enough capability to detect X-rays, i.e., FWHM of 207 eV at 5.9 keV at room temperature. We then employed this sensor and performed an experiment at a 200 m beam line of BL20B2 in the synchrotron facility SPring8. Using a grating with a pitch of 4.8 µm and an opening fraction of f=0.5, we obtained the self image of the grating at the detector distance from the grating of 23 cm and 46 cm and the X-ray energy of 12.4 keV. We also performed an experiment using a 9.6 μm f = 0.2 grating with a detector-grating distance of 92 cm, and obtained higher contrast image of the grating. Note that the slit width of 2.4 μm at 46 cm corresponds to 1.1′′, while that of 1.9 μm at 92 cm does 0.43′′. We suggest several format of possible MIXIM missions, including MIXIM-S for very small satellite of 50cm size, MIXIM-P for parasite use of nominal X-ray observatory employing grazing X-ray telescopes with a focal length of 10 m, and MIXIM-Z in which the grating-detector distance of 100 m is acquired by formation flight or free fryers to yield 0.01” level resolution.