dorsal/arxiv
View SchemaThe X-ray CCD camera of the MAXI Experiment on the ISS/JEM
| Authors | E. Miyata, H. Tsunemi, H. Ogata, D. Akutsu, K. Yoshita, Y. Hashimoto, K. Torii, M. Matsuoka, N. Kawai, A. Yoshida, T. Mihara, T. Kotani, H. Negoro, H. Kubo, H. Matsumoto, Y. Shirasaki, B. C. Rubin, I. Sakurai, M. Yamauchi |
|---|---|
| Categories | |
| ArXiv ID | physics/9904014 |
| URL | https://arxiv.org/abs/physics/9904014 |
| DOI | 10.1016/S0168-9002(99)00603-8 |
Abstract
MAXI, Monitor of All-sky X-ray Image, is the X-ray observatory on the Japanese experimental module (JEM) Exposed Facility (EF) on the International Space Station (ISS). MAXI is a slit scanning camera which consists of two kinds of X-ray detectors: one is a one-dimensional position-sensitive proportional counter with a total area of $\sim 5000 cm^2$, the Gas Slit Camera (GSC), and the other is an X-ray CCD array with a total area $\sim 200 cm^2$, the Solid-state Slit Camera (SSC). The GSC subtends a field of view with an angular dimension of 1$^\circ\times 180^\circ$ while the SSC subtends a field of view with an angular dimension of 1$^\circ$ times a little less than 180$^\circ$. In the course of one station orbit, MAXI can scan almost the entire sky with a precision of 1$^\circ$ and with an X-ray energy range of 0.5-30 keV. We have developed the engineering model of CCD chips and the analogue electronics for the SSC. The energy resolution of EM CCD for Mn K$\alpha$ has a full-width at half maximum of $\simeq$ 182 eV. Readout noise is $\simeq$ 11 e^- rms.
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"abstract": "MAXI, Monitor of All-sky X-ray Image, is the X-ray observatory on the\nJapanese experimental module (JEM) Exposed Facility (EF) on the International\nSpace Station (ISS). MAXI is a slit scanning camera which consists of two kinds\nof X-ray detectors: one is a one-dimensional position-sensitive proportional\ncounter with a total area of $\\sim 5000 cm^2$, the Gas Slit Camera (GSC), and\nthe other is an X-ray CCD array with a total area $\\sim 200 cm^2$, the\nSolid-state Slit Camera (SSC). The GSC subtends a field of view with an angular\ndimension of 1$^\\circ\\times 180^\\circ$ while the SSC subtends a field of view\nwith an angular dimension of 1$^\\circ$ times a little less than 180$^\\circ$. In\nthe course of one station orbit, MAXI can scan almost the entire sky with a\nprecision of 1$^\\circ$ and with an X-ray energy range of 0.5-30 keV. We have\ndeveloped the engineering model of CCD chips and the analogue electronics for\nthe SSC. The energy resolution of EM CCD for Mn K$\\alpha$ has a full-width at\nhalf maximum of $\\simeq$ 182 eV. Readout noise is $\\simeq$ 11 e^- rms.",
"arxiv_id": "physics/9904014",
"authors": [
"E. Miyata",
"H. Tsunemi",
"H. Ogata",
"D. Akutsu",
"K. Yoshita",
"Y. Hashimoto",
"K. Torii",
"M. Matsuoka",
"N. Kawai",
"A. Yoshida",
"T. Mihara",
"T. Kotani",
"H. Negoro",
"H. Kubo",
"H. Matsumoto",
"Y. Shirasaki",
"B. C. Rubin",
"I. Sakurai",
"M. Yamauchi"
],
"categories": [
"physics.ins-det"
],
"doi": "10.1016/S0168-9002(99)00603-8",
"title": "The X-ray CCD camera of the MAXI Experiment on the ISS/JEM",
"url": "https://arxiv.org/abs/physics/9904014"
},
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