The X-ray Evolving Universe Spectroscopy mission (XEUS)

被引：12

作者：

Bavdaz, M ^{[1
]}

Bleeker, JAM ^{[1
]}

Hasinger, G ^{[1
]}

Inoue, H ^{[1
]}

Palumbo, G ^{[1
]}

Peacock, A ^{[1
]}

Parmar, A ^{[1
]}

Turner, MJ ^{[1
]}

Truemper, J ^{[1
]}

Schiemann, J ^{[1
]}

机构：

[1] European Space Agcy, Estec, Dept Space Sci, NL-2200 AG Noordwijk, Netherlands

来源：

X-RAY OPTICS, INSTRUMENTS, AND MISSIONS II | 1999年 / 3766卷

关键词：

X-ray astrophysics; future missions; evolving universe;

D O I：

10.1117/12.363664

中图分类号：

TH7 [仪器、仪表];

学科分类号：

0804 ; 080401 ; 081102 ;

摘要：

The X-ray Evolving Universe Spectroscopy mission represents a potential follow-on mission to the ESA XMM cornerstone currently nearing completion. XEUS represents the next logical step forward in X-ray astrophysics after the current set of missions have been launched and completed their operational lives. The development and ultimate success relies heavily on the capability of the International Space Station (ISS). In this paper we describe the key characteristics of the mission including the requirements placed specifically on the ISS and discuss the significant advances in high energy astrophysics expected from such an observatory. The aim of XEUS is to study the astrophysics of some of the most distant and hence youngest known discrete objects in the universe. The specific scientific issues, which XEUS aims to address, can be summarized as follows: 1 To measure the X-ray spectra of objects with a redshift z >4 at flux levels about <10(-17) erg cm(-2) s(-1). This is at least a 100 times fainter than XMM. 2 Where possible to determine from the X-ray spectral lines the redshift and thus the age of these objects 3 To thereby establish the evolution in the distribution of matter in the early universe To achieve these demanding aims a large X-ray telescope is required. The basic features of this telescope are: 1 An X-ray mirror with an effective collecting area at I keV of 30 m(2) 2 A spatial resolution of the mirror needs to be at least 5 "(HEW) so as to avoid source confusion at above mentioned faint source levels. 3 A field of view of at least 5' is required so as to ensure that a significantly large population of high redshift x-ray sources can be observed in a single pointing. 4 Energy bandwith required is 0.05 to 30 keV, with 3m(2) at 8 keV. 5 An energy resolution of 1-10 eV is required to perform detailed plasma diagnostics on sources, such as distant galaxy clusters These are some of the most demanding requirements yet placed on any X-ray astrophysics mission and will require major technological development at an levels - optics, detectors and spacecraft.

引用

页码：82 / 93

页数：12