Modeling and Reproducibility of Suzaku HXD PIN/GSO Background

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dc.creatorFukazawa, Yasushi
dc.creatorMizuno, Tsunefumi
dc.creatorWatanabe, Shin
dc.creatorKokubun, Motohide
dc.creatorTakahashi, Hiromitsu
dc.creatorKawano, Naomi
dc.creatorNishino, Sho
dc.creatorSasada, Mahito
dc.creatorShirai, Hirohisa
dc.creatorTakahashi, Takuya
dc.creatorYamasaki, Tomonori
dc.creatorYasuda, Tomonori
dc.creatorBamba, Aya
dc.creatorOhno, Masanori
dc.creatorTakahashi, Tadayuki
dc.creatorUshio, Masayoshi
dc.creatorEnoto, Teruaki
dc.creatorKitaguchi, Takao
dc.creatorMakishima, Kazuo
dc.creatorNakazawa, Kazuhiro
dc.creatorUehara, Yuichi
dc.creatorYamada, Shin'ya
dc.creatorYuasa, Takayuki
dc.creatorIsobe, Naoki
dc.creatorKawaharada, Madoka
dc.creatorTanaka, Takaaki
dc.creatorTashiro, Makoto
dc.creatorTerada, Yukikatsu
dc.creatorYamaoka, Kazutaka
dc.date2009-01-05
dc.date.accessioned2026-07-07T12:31:57Z
dc.date.available2026-07-07T12:31:57Z
dc.descriptionSuzaku Hard X-ray Detector (HXD) achieved the lowest background level than any other previously or currently operational missions sensitive in the energy range of 10--600 keV, by utilizing PIN photodiodes and GSO scintillators mounted in the BGO active shields to reject particle background and Compton-scattered events as much as possible. Because it does not have imaging capability nor rocking mode for the background monitor, the sensitivity is limited by the reproducibility of the non X-ray background (NXB) model. We modeled the HXD NXB, which varies with time as well as other satellites with a low-earth orbit, by utilizing several parameters, including particle monitor counts and satellite orbital/attitude information. The model background is supplied as an event file in which the background events are generated by random numbers, and can be analyzed in the same way as the real data. The reproducibility of the NXB model depends on the event selection criteria (such as cut-off rigidity and energy band) and the integration time, and the 1sigma systematic error is estimated to be less than 3% (PIN 15--40 keV) and 1% (GSO 50--100 keV) for more than 10 ksec exposure.
dc.description29 pages, 45 figures, will appear on the PASJ 61, Suzaku 3rd issue
dc.identifierhttps://arxiv.org/abs/0901.0419
dc.identifierhttp://arxiv.org/abs/0901.0419
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/216624
dc.subjectInstrumentation and Methods for Astrophysics
dc.titleModeling and Reproducibility of Suzaku HXD PIN/GSO Background
dc.typetext

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