ASTRO-H Hard X-ray Telescope (HXT)

Awaki, Hisamitsu; Kunieda, H.; Furuzawa, Akihiro; Haba, Yoshito; Hayashi, Takayuki; Iizuka, Ryo; Ishibashi, Koji; Ishida, M.; Itoh, M.; Kosaka, Tatsuro; Maeda, Yoshitomo; Matsumoto, Hironori; Miyazawa, Tatsuo; Mori, Hajime; Nagano, Hosei; Namba, Yoshiharu; Ogasaka, Yasushi; Ogi, Keiji; Okajima, Takashi; Sugita, S.; Suzuki, Yoshio; Tamura, Kouichi; Tawara, Yuzuru; Uesugi, Kentaro; Yamashita, Koujun; Yamauchi, Shigeo

doi:10.1117/12.2054633

Cited by 12 publications

(19 citation statements)

References 4 publications

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“…The soft X-ray spectrum of Mkn 3 is extremely complex, but the spectral resolution of the XIS is significantly worse (at all energies) than the gratings aboard Chandra and XMM-Newton (∼ 1−2 orders of magnitude worse than the medium-energy Chandra grating, depending on the energy). Previous studies of Mkn 3 using Chandra and XMM-Newton gratings have shown numerous atomic features, indicative of a predominantly photoionized spectrum originating in material with a wide range in ionization states (Sako et al 2000;Pounds et al 2005;Bianchi et al 2005;Awaki et al 2008). Thus, when grating spectra are available, CCD data cannot contribute substantially new understanding of the origin of the soft X-ray spectrum since many emission and absorption features are blended together.…”

Section: Model Setupmentioning

confidence: 98%

“…1 that above ∼ 2 keV the spectrum is very flat due to absorption and reflection, and there is complex structure around the Fe Kα emission line in the ∼ 6−8 keV Fe K band. The spectrum steepens towards low energies and below ∼ 3 keV there are many emission and absorption features, which have been well-studied with both CCD and higher spectral resolution instrumentation (Sako et al 2000;Pounds et al 2005;Bianchi et al 2005;Awaki et al 2008).…”

Section: Analysis Strategy and Spectral Fittingmentioning

confidence: 99%

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A Compton-thin solution for theSuzakuX-ray spectrum of the Seyfert 2 galaxy Mkn 3

Yaqoob

Tatum

Scholtes

et al. 2015

Mon. Not. R. Astron. Soc.

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Mkn 3 is a Seyfert 2 galaxy that is widely regarded as an exemplary Comptonthick AGN. We study the Suzaku X-ray spectrum using models of the X-ray reprocessor that self-consistently account for the Fe Kα fluorescent emission line and the associated Compton-scattered, or reflection, continuum. We find a solution in which the average global column density, 0.234 +0.012 −0.010 × 10 24 cm −2 , is very different to the line-of-sight column density, 0.902 +0.012 −0.013 × 10 24 cm −2 . The global column density is ∼ 5 times smaller than that required for the matter distribution to be Compton-thick. Our model accounts for the profiles of the Fe Kα and Fe Kβ lines, and the Fe K edge remarkably well, with a solar abundance of Fe. The matter distribution could consist of a clumpy medium with a line-of-sight column density higher than the global average. A uniform, spherically-symmetric distribution alone cannot simultaneously produce the correct fluorescent line spectrum and reflection continuum. Previous works on Mkn 3, and other AGN, that assumed a reflection continuum from matter with an infinite column density could therefore lead to erroneous or "puzzling" conclusions if the matter out of the line-of-sight is really Compton-thin. Whereas studies of samples of AGN have generally only probed the line-of-sight column density, with simplistic, one-dimensional models, it is important now to establish the global column densities in AGN. It is the global properties that affect the energy budget in terms of reprocessing of X-rays into infrared emission, and that constrain population synthesis models of the cosmic X-ray background.

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Section: Model Setupmentioning

confidence: 98%

Section: Analysis Strategy and Spectral Fittingmentioning

confidence: 99%

A Compton-thin solution for theSuzakuX-ray spectrum of the Seyfert 2 galaxy Mkn 3

Yaqoob

Tatum

Scholtes

et al. 2015

Mon. Not. R. Astron. Soc.

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“…2 The others are hard X-ray telescopes (HXTs) covering up to ∼ 80 keV. 3 One SXT is for soft X-ray spectroscopy (SXS : X-ray micro-calorimeter detector) with a high resolution spectroscopy. The FOV is 3.05 arcmin with the pixels of 6 × 6.…”

Section: Introductionmentioning

confidence: 99%

Ground-based x-ray calibration of the Astro-H soft x-ray telescopes

et al. 2014

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The X-ray astronomy satellite Astro-H, planed to be launched in 2015, will have several instruments for covering a wide energy band from a few hundreds eV to 600 keV. There are four X-ray telescopes, and two of them are soft X-ray telescopes (SXTs) covering up to about 15 keV. One is for an X-ray micro-calorimeter detector (SXS) and the other is for an X-ray CCD detector (SXI). The design of the SXTs is a conical approximation of the Wolter Type-I optics, which is also adopted for the telescopes on the previous mission Suzaku launched in 2005. It consists 203 thin-foil reflectors coated with gold monolayer (2000Å) on the aluminum substrate (101.6 mm length) with the thickness of 0.15, 0.23 and 0.31 mm. These are nested confocally within the radius of 58 to 225 mm. The focal length of SXTs is 5.6 m. The weight is as light as ∼ 43 kg per telescope.We present the current status of the calibration activity of two SXTs (SXT-1 and SXT-2). The developments of two SXTs were completed by NASA's Goddard Space Flight Center (GSFC). First X-ray measurements with a diverging beam at the GSFC 100m beamline found an angular resolution at 8.0 keV to be 1.1 and 1.0 arcmin (HPD) for SXT-1 and SXT-2, respectively. The full characterization of the X-ray performance has been now continuously calibrated with the 30m X-ray beamline facility at the Institute of Space and Astronautical Science (ISAS) of Japan Aerospace eXploration Agency (JAXA) in Japan. We adopted a raster scan method with a narrow X-ray pencil beam with the divergence of ∼ 15". X-ray characterization of the two SXTs has been measured from May and December 2013, respectively.In the case of SXT-1, the on-axis effective area was approximately 580, 445, 370, 270, 185 and 90 cm 2 at energies of 1. 5, 4.5, 8.0, 9.4, 11.1 and 12.9 keV respectively. The effective area of SXT-2 is 2% larger than that of SXT-1 irrespective to X-ray energy. The on-axis angular resolution of SXT-1 was evaluated as 1.3 -1.5 arcmin (HPD) in the 1.5 -13 keV band. The resolution was slightly got worse at higher energies by ∼ 0.3 arcmin. Otherwise, the resolution of SXT-2 is 1.2 arcmin, almost irrespective to X-ray energy. The field of view (FOV) was ∼ 16 arcmin at 1.5 keV, decreasing with increasing X-ray energy, and became ∼ 8 arcmin at 13 keV. The FOV is defined here as the full-width at half-maximum (FWHM) of the vignetting curve.The X-ray performance of SXT-1 and SXT-2 meets the system requirements. Because all the parameters of the SXT-2 is slightly better that of SXT-1, we adopted the SXT-2 telescope for the SXS detector of the Astro-H primary instrument with the narrow FOV.

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“…ASTRO-H will mount three kinds of X-ray detectors: an X-ray micro-calorimeter (SXS 2 ), a Soft X-ray Imager (SXI 3,4 ) a hard X-ray imager (HXI 5 ), and a soft Gamma-ray Detector (SGD 6 ). The SXS, SXI and HXI are mounted on ASTRO-H as the focal plane detectors of two Soft X-ray telescope (SXT1 and SXT2 7 respectively) and the Hard X-ray telescope (HXI) 8 , respectively. Our team has developed the X-ray CCD's (SXI; Soft X-ray Imager) onboard ASTRO-H (Tsunemi et al 2013; Hayashida et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Soft x-ray transmission of contamination blocking filter for SXI onboard ASTRO-H

Kohmura¹,

Kaneko²,

Tsunemi³

et al. 2014

SPIE Proceedings

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X-ray CCD operated onboard satellite are contaminated by outgas from organic material used in satellites. This contamination causes a significant reduction in the detection sensitivity of X-ray detectors.In order to prevent such contamination to the Back-IlluminatedCCD (BI-CCD) of the Soft X-ray Imager (SXI) onboard ASTRO-H, we have developed a Contamination Blocking Filter (CBF), which consists of ∼30nm thick Aluminum and ∼200nm thick Polyimide. The CBF is be placed on the top of the CCD camera hood and is required to have a high X-ray transmission in order to take advantage of the high detection efficiency of BI-CCD.We measured the X-ray transmission of three fight candidates of the CBF last October at the SPring-8 and obtained the X-ray transmission of three CBFs in the soft X-ray energy from 0.2 to 1.8 keV which covers the absorption edges around C-K, N-K, O-K, and Al-K including X-ray absorption fine structure (XAFS). In these measurements, we found three CBFs have high X-ray transmission below 2ke V, e.g. ∼70% at around 0.5 keV, and determined the thickness of Al and Polyimide to be 220 nm and ∼50 nm, respectively. We will calculate the response function of SXI including these results.

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ASTRO-H Hard X-ray Telescope (HXT)

Cited by 12 publications

References 4 publications

A Compton-thin solution for theSuzakuX-ray spectrum of the Seyfert 2 galaxy Mkn 3

A Compton-thin solution for theSuzakuX-ray spectrum of the Seyfert 2 galaxy Mkn 3

Ground-based x-ray calibration of the Astro-H soft x-ray telescopes

Soft x-ray transmission of contamination blocking filter for SXI onboard ASTRO-H

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