F. Porter, M. Eckart, M. Leutenegger, Tomomi Watanabe, C. Kilbourne, R. Kelley, Michael C. Witthoeft, R. Cumbee, M. Sawada, N. Hell, G. Brown, Y. Ishisaki, S. Yamada
{"title":"Initial ground calibration of the Resolve detector system on XRISM","authors":"F. Porter, M. Eckart, M. Leutenegger, Tomomi Watanabe, C. Kilbourne, R. Kelley, Michael C. Witthoeft, R. Cumbee, M. Sawada, N. Hell, G. Brown, Y. Ishisaki, S. Yamada","doi":"10.1117/12.2561477","DOIUrl":null,"url":null,"abstract":"The Resolve detector system is calibrated on the ground in three stages: at the focal plane assembly, at the calorimeter spectrometer insert, and at the full instrument level. We have just completed the first two stages and have measured the detailed core line shape and spectral redistribution functions, by pixel, and as a function of energy. In addition, we have measured the energy scale function that translates instrument units into spectral units, by pixel, and as a function of detector heat sink temperature. We discuss the results of the Resolve calibration program to date as well as implications for the calibration of future high resolution x-ray spectrometers.","PeriodicalId":170593,"journal":{"name":"Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray","volume":"19 1","pages":"0"},"PeriodicalIF":0.0000,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"3","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1117/12.2561477","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 3
Abstract
The Resolve detector system is calibrated on the ground in three stages: at the focal plane assembly, at the calorimeter spectrometer insert, and at the full instrument level. We have just completed the first two stages and have measured the detailed core line shape and spectral redistribution functions, by pixel, and as a function of energy. In addition, we have measured the energy scale function that translates instrument units into spectral units, by pixel, and as a function of detector heat sink temperature. We discuss the results of the Resolve calibration program to date as well as implications for the calibration of future high resolution x-ray spectrometers.