<title>Soft x-ray response of the prototype CCD camera (XIS) for Astro-E</title>

Abstract

The X-ray Imaging Spectrometers (XIS) are X-ray CCD cameras on-board the Astro-E satellite launched in 2000. The XIS consists of 4 cameras, each of them will be installed on a focal plane of the Astro-E X-ray Telescope(XRT). The XIS not only have a higher sensitivity, which comes from a larger effective area of the XRT and thicker depletion layers of the XIS CCDs, than ASCA 515, but also have several features that will overcome the radiation damage effects anticipated in the orbit. The calibration experiment at Osaka focuses on the soft X-ray response of the XIS. The calibration system employs a grating spectrometer which irradiates the CCD with dispersed X-rays. We have obtained preliminary results on the XIS proto model, including the energypulse-height relation, the energyresolution relation, and the quantum efficiency at the energy range of 0.25 -2.2 keV.

Soft x-ray response of x-ray CCD camera XIS onboard Astro-E2

“…There found a deviation from the straight line at around and above the Si K-edge. Similar deviation was found in the XIS for Astro-E1, but the amount of deviation was reduced if we refine the data reduction, for example, taking into account of the detailed pulse profile including the tail structure 1,2 . Further examination of such effect for the Astro-E2 XIS results is needed The slope of the Ex-PH relation represents the gain of the XIS system.…”

“…The design of Astro-E2 XIS is basically the same as that for Astro-E1 described in Hayashida et al 1,2 The system consists of four X-ray CCD cameras, analog electronics (AE), and digital electronics (DE). Each CCD camera has one frame-transfer type CCD chip manufactured by MIT Lincoln Laboratory.…”

“…The soft X-ray calibration system and its usage for Astro-E1 XIS calibrations were described in series of papers 1,2,5,6 . The system consists of a soft X-ray source, Manson model 2 ultra soft X-ray source, and a grating spectrometer by Hetrick Science, and a chamber in which a CCD camera and/or a gas proportional counter are installed.…”

Ultra-high energy neutrinos: A review of theoretical and phenomenological issues

“…At higher energies, indirect methods involving detection of secondaries produced by interaction of the primaries in the atmosphere is necessary. The most widely used indirect method has been the deployment of Extensive Air Shower (EAS) arrays (for example Yakutsk [21] and AGASA [22]). These sample a lateral cross-section of the multi-particle shower initiated by a CR primary high up in the atmosphere.…”