Mr. Takashi Hanasaka Profile

Takashi Hanasaka

at Osaka Univ

SPIE Involvement:

Author

Publications (4)

Proceedings Article | 18 December 2020 Presentation + Paper

Sub-arcseconds to micro-arcsecond x-ray imaging with multi image x-ray interferometer method (MIXIM): concept and scalabe mission plans

Kiyoshi Hayashida, Kazunori Asakura, Ayami Ishikura, Shotaro Sakuma, Takashi Hanasaka, Tomoki Kawabata, Tomokage Yoneyama, Hirofumi Noda, Koki Okazaki, Maho Hanaoka, Kengo Hattori, Kenmei Sawagami, Wataru Kamogawa, Hiroshi Nakajima, Yusuke Matsuhita, Taisei Mineta, Marina Yoshimoto, Tomohiko Hakamata, Yuichi Ode, Hironori Matsumoto, Hiroshi Tsunemi, Hisamitsu Awaki, Yuichi Terashima, Toshihiro Kawaguchi

Proceedings Volume 11444, 114441C (2020) https://doi.org/10.1117/12.2562193

KEYWORDS: X-ray imaging, X-rays, Interferometers, Diffraction gratings, Sensors, Image resolution, Spatial resolution, Satellites, Astronomy, Visibility

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Proceedings Article | 13 December 2020 Presentation + Paper

Subsub-arcseconds x-ray imaging with multi-image x-ray interferometer module (MIXIM): experimental results

Kazunori Asakura, Kiyoshi Hayashida, Takashi Hanasaka, Tomoki Kawabata, Tomokage Yoneyama, Hirofumi Noda, Shotaro Sakuma, Koki Okazaki, Ayami Ishikura, Maho Hanaoka, Shuntaro Ide, Kengo Hattori, Hironori Matsumoto, Hiroshi Tsunemi, Hisamitsu Awaki, Hiroshi Nakajima, Junko Hiraga

Proceedings Volume 11444, 114441D (2020) https://doi.org/10.1117/12.2560772

KEYWORDS: X-rays, X-ray imaging, X-ray detectors, Interferometers, CMOS sensors, Diffraction gratings, X-ray astronomy, Sensors, Spatial resolution, Astronomy

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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, 035002, (June 2019) https://doi.org/10.1117/12.10.1117/1.JATIS.5.3.035002

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 | 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

Proceedings Volume 10699, 106990U (2018) https://doi.org/10.1117/12.2314181

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

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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.

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