Characterization of a Hard X-ray Telescope at Synchrotron Facility SPring-8

Ogasaka, Yasushi; Tamura, Kouichi; Shibata, Ryo; Furuzawa, Akihiro; Miyazawa, Tatsuo; Shimoda, Kenta; Fukaya, Yoshihiro; Iwahara, Tomonaga; Nakamura, Tadahisa; Naitou, Masataka; Kanou, Yasuhiko; Sasaki, Naoki; Ueno, Daisuke; Okajima, Takashi; Miyata, Emi; Tawa, Noriaki; Mukai, Kenji; Ikegami, Kentaro; Aono, Michihiko; Uesugi, Kentaro; Suzuki, Yoshio; Takeuchi, Satoshi; Futamura, Taku; Takahashi, Rika; Sakashita, Mitsuo; Sakai, Chiaki; Nonoyama, Masayuki; Yamada, Nobuaki; Onishi, Katsuhiko; Miyauchi, Takuya; Maeda, Yoshitomo; Okada, Shunsaku; Serlemitsos, P. J.; Soong, Yang; Chan, Kai-Wing; Rohrbach, Scott; Berendse, Fred; Tueller, J.; Tsunemi, H.; Kunieda, H.; Yamashita, Koujun

doi:10.1143/jjap.47.5743

Cited by 25 publications

(12 citation statements)

References 30 publications

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“…The mirror shell was initially measured in full illumination at the PANTER facility (Burwitz et al 2013) at 1 to 40 keV. Subsequently, the PSF at 15 to 63 keV was measured sector-by-sector at the beamline BL20B2 of the SPring-8 radiation facility (Ogasaka et al 2008). The mirror shell with the details of the manufacturing process is described in Basso et al (2011).…”

Section: Experimental Verificationmentioning

confidence: 99%

Mirrors for X-ray telescopes: Fresnel diffraction-based computation of point spread functions from metrology

Raimondi¹,

Spiga

2014

A&A

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Context. The imaging sharpness of an X-ray telescope is chiefly determined by the optical quality of its focusing optics, which in turn mostly depends on the shape accuracy and the surface finishing of the grazing-incidence X-ray mirrors that compose the optical modules. To ensure the imaging performance during the mirror manufacturing, a fundamental step is predicting the mirror point spread function (PSF) from the metrology of its surface. Traditionally, the PSF computation in X-rays is assumed to be different depending on whether the surface defects are classified as figure errors or roughness. This classical approach, however, requires setting a boundary between these two asymptotic regimes, which is not known a priori. Aims. The aim of this work is to overcome this limit by providing analytical formulae that are valid at any light wavelength, for computing the PSF of an X-ray mirror shell from the measured longitudinal profiles and the roughness power spectral density, without distinguishing spectral ranges with different treatments. Methods. The method we adopted is based on the Huygens-Fresnel principle for computing the diffracted intensity from measured or modeled profiles. In particular, we have simplified the computation of the surface integral to only one dimension, owing to the grazing incidence that reduces the influence of the azimuthal errors by orders of magnitude. The method can be extended to optical systems with an arbitrary number of reflections -in particular the Wolter-I, which is frequently used in X-ray astronomy -and can be used in both near-and far-field approximation. Finally, it accounts simultaneously for profile, roughness, and aperture diffraction. Results. We describe the formalism with which one can self-consistently compute the PSF of grazing-incidence mirrors, and we show some PSF simulations including the UV band, where the aperture diffraction dominates the PSF, and hard X-rays where the X-ray scattering has a major impact on the PSF degradation. The results are validated with ray-tracing simulations, or by comparison with the analytical computation of the half-energy width based on the known scattering theory, where these approaches are applicable. Finally, we validate this by comparing the simulated PSF of a real Wolter-I mirror shell with the measured PSF in hard X-rays.

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Section: Experimental Verificationmentioning

confidence: 99%

Mirrors for X-ray telescopes: Fresnel diffraction-based computation of point spread functions from metrology

Raimondi¹,

Spiga

2014

A&A

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“…An energy resolution E∕ΔE of ∼10 4 is provided by a Si double-crystal monochrometer. The details are described by Ogasaka et al 16 The performance of the reflectors for the Hitomi's HXT was also measured in the SPring-8 facility. Figure 13 shows the measured reflectivity of the HXT reflector designed for nominal grazing angle of 0.09 deg at the energy of 30 keV.…”

Section: Multilayer Evaluationmentioning

confidence: 99%

Supermirror design for Hard X-Ray Telescopes on-board Hitomi (ASTRO-H)

Tamura

Kunieda

Miyata

et al. 2018

J. Astron. Telesc. Instrum. Syst.

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Abstract. We designed depth-graded multilayers, so-called supermirrors, with platinum/carbon (Pt/C) layer pairs for the Hard X-Ray Telescope (HXT) that was on-board the sixth Japanese X-Ray Astronomy Satellite Hitomi (ASTRO-H). The HXT has multinested thin foil optics, and the grazing angles of the x-ray mirrors are 0.07 to 0.27 deg. Supermirrors for HXTs are designed to provide a broad energy response (up to 80 keV) for astronomical requests. Under practical boundary conditions, we establish a block method applying empirical rules to maximize the integrated reflectivity. We fabricated Pt/C supermirrors using a DC magnetron sputtering system. The reflectivity of the mirrors was measured in a synchrotron radiation facility, SPring-8. We describe the design method for the supermirrors and our results.

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“…The ground calibration of past hard X-ray optics for balloon missions has been conducted at existing synchrotron and long-beam facilities. 13,14,15 Here we describe the ground calibration approach for the NuSTAR optics for which a dedicated calibration facility was used.…”

Section: Optics Ground Calibrationmentioning

confidence: 99%

First results from the ground calibration of the NuSTAR flight optics

Koglin

Barrière

et al. 2011

SPIE Proceedings

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NuSTAR is a hard X-ray satellite experiment to be launched in 2012. Two optics with 10.15 m focal length focus Xrays with energies between 5 and 80 keV onto CdZnTe detectors located at the end of a deployable mast. The FM1 and FM2 flight optics were built at the same time based on the same design and with very similar components, and thus the performance of both is expected to be very similar. We provide an overview of calibration data that is being used to build an optics response model for each optic and describe initial results for energies above 10 keV from the ground calibration of the flight optics. From a preliminary analysis of the data, our current best determination of the overall HPD of both the FM1 and FM2 flight optics is 52", and nearly independent of energy. The statistical error is negligible, and a preliminary estimate of the systematic error is of order 4". The as-measured effective area and HPD meet the toplevel NuSTAR mission sensitivity requirements.

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Characterization of a Hard X-ray Telescope at Synchrotron Facility SPring-8

Cited by 25 publications

References 30 publications

Mirrors for X-ray telescopes: Fresnel diffraction-based computation of point spread functions from metrology

Mirrors for X-ray telescopes: Fresnel diffraction-based computation of point spread functions from metrology

Supermirror design for Hard X-Ray Telescopes on-board Hitomi (ASTRO-H)

First results from the ground calibration of the NuSTAR flight optics

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