Hard x-ray imaging polarimeter for PolariS

Hayashida, Kentaro; Juyong, Kim; Sadamoto, M.; Yoshinaga, Keinosuke; Gunji, Shuichi; Mihara, T.; Kishimoto, Y.; Kubo, H.; Mizuno, T.; Takahashi, H.; Dotani, Tadayasu; Yonetoku, Daisuke; Nakamori, Takeshi; Yoneyama, T.; Ikeyama, Yuki; Kamitsukasa, Fumiyoshi

doi:10.1117/12.2232472

Cited by 5 publications

(3 citation statements)

References 6 publications

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“…MF of GMAX0505 is not as high as other x-ray polarimeters; 20% to 65% for the gas photoelectron tracking polarimeter at 2 to 8 keV 12 and 30% to 50% for the hard x-ray and soft γ-ray scattering polarimeters above 20 keV. 6,9,30 However, the energy range of 10 to 20 keV is the valley of these two classes of x-ray polarimeters, and there is a room for the small-sized pixel CMOS sensors such as GMAX0505. Combining with a future high-quality x-ray mirror of 10-m focal lengths, we would obtain the spatial resolution of ∼0.05 arcsec.…”

Section: Discussionmentioning

confidence: 92%

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

Asakura

Hayashida

Hanasaka

et al. 2019

J. Astron. Telesc. Instrum. Syst.

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X-ray polarimetry in astronomy has not been exploited well, despite its importance. The recent innovation of instruments is changing this situation. We focus on a complementary MOS (CMOS) pixel detector with small pixel size and employ it as an x-ray photoelectron tracking polarimeter. The CMOS detector we employ is developed by GPixel Inc., and has a pixel size of 2.5 µm × 2.5 µm. Although it is designed for visible light, we succeed in detecting x-ray photons with an energy resolution of 176 eV (FWHM) at 5.9 keV at room temperature and the atmospheric condition. We measure the x-ray detection efficiency and polarimetry sensitivity by irradiating polarized monochromatic x-rays at BL20B2 in SPring-8, the synchrotron radiation facility in Japan. We obtain modulation factors of 7.63% ± 0.07% and 15.5% ± 0.4% at 12.4 keV and 24.8 keV, respectively. It demonstrates that this sensor can be used as an x-ray imaging spectrometer and polarimeter with the highest spatial resolution ever tested.

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Section: Discussionmentioning

confidence: 92%

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

Asakura

Hayashida

Hanasaka

et al. 2019

J. Astron. Telesc. Instrum. Syst.

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“…• X-ray -g-ray Polarimetry Satellite (Polaris) 11 , a JAXA small satellite series mission that will use a 6m mast and include spacecraft rotation at ~0.1 rpm.…”

Section: Discussionmentioning

confidence: 99%

GettingNuSTARon target: predicting mast motion

Madsen

Miyasaka

Craig³

et al. 2016

Observatory Operations: Strategies, Processes, and Systems VI

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The Nuclear Spectroscopic Telescope Array (NuSTAR) is the first focusing high energy (3-79 keV) X-ray observatory operating for four years from low Earth orbit. The X-ray detector arrays are located on the spacecraft bus with the optics modules mounted on a flexible mast of 10.14m length. The motion of the telescope optical axis on the detectors during each observation is measured by a laser metrology system and matches the pre-launch predictions of the thermal flexing of the mast as the spacecraft enters and exits the Earths shadow each orbit. However, an additional motion of the telescope field of view was discovered during observatory commissioning that is associated with the spacecraft attitude control system and an additional flexing of the mast correlated with the Solar aspect angle for the observation. We present the methodology developed to predict where any particular target coordinate will fall on the NuSTAR detectors based on the Solar aspect angle at the scheduled time of an observation. This may be applicable to future observatories that employ optics deployed on extendable masts. The automation of the prediction system has greatly improved observatory operations efficiency and the reliability of observation planning.

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“…PolariS (Polarimetry Satellite) [111] is a proposed small mission (JAXA) designed to perform polarimetry in the 10-80 keV energy band. The main scientific objective of PolariS mission is the hard X-ray polarimetry of bright SNRs, BHs and NSs.…”

Section: Polarismentioning

confidence: 99%

Instrumentation and Future Missions in the Upcoming Era of X-ray Polarimetry

Fabiani

2018

Galaxies

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The maturity of current detectors based on technologies that range from solid state to gases renewed the interest for X-ray polarimetry, raising the enthusiasm of a wide scientific community to improve the performance of polarimeters as well as to produce more detailed theoretical predictions. We will introduce the basic concepts about measuring the polarization of photons, especially in the X-rays, and we will review the current state of the art of polarimeters in a wide energy range from soft to hard X-rays, from solar flares to distant astrophysical sources. We will introduce relevant examples of polarimeters developed from the recent past up to the panorama of upcoming space missions to show how the recent development of the technology is allowing reopening the observational window of X-ray polarimetry.

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Hard x-ray imaging polarimeter for PolariS

Cited by 5 publications

References 6 publications

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

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

GettingNuSTARon target: predicting mast motion

Instrumentation and Future Missions in the Upcoming Era of X-ray Polarimetry

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