EDGE: Explorer of Diffuse emission and Gamma-ray burst Explosions
L. Piro, J. W. den Herder, T. Ohashi
备注：
This is a low resolution version of the proposal submitted to ESA in response to the Cosmic Vision Call. A high quality version is available at the web address reported in the cover page
How structures on various scales formed and evolved from the early Universe up to present time is a fundamental question of astrophysical cosmology. EDGE will trace the cosmic history of the baryons from the early generations of massive star by Gamma-Ray Burst (GRB) explosions, through the period of cluster formation, down to very low redshifts, when between a third and one half of the baryons are expected to reside in cosmic filaments undergoing gravitational collapse by dark matter (Warm Hot Intragalactic Medium: WHIM). In addition EDGE, with its unprecedented observational capabilities, will provide key results on several other topics. The science is feasible with a medium class mission using existing technology combined with innovative instrumental and observational capabilities on a single satellite by: a) observing with fast reaction Gamma-Ray Bursts with a high spectral resolution (R ~ 500). This enables the study of their (star-forming) environment from the Dark to the local Universe and the use of GRB as back light of large scale cosmological structures b) Observing and surveying extended sources (clusters, WHIM) with high sensitivity using two wide field of view X-ray telescopes (one with a high angular resolution and the other with a high spectral resolution).
Far Ultraviolet Spectroscopic Explorer Observations of the Supernova Remnant N49 in the Large Magellanic Cloud
本文报道了远紫外光谱探测卫星对大麦云星云中超新星遗迹N49的观测结果。使用了30“的方形孔径，速度分辨率约为100 km/s。观测的目的是检查早期工作中预期的几条明亮的发射线，并通过搜索以前在河外超新星遗迹紫外光谱中从未见过的微弱线来证明扩散源的敏感性。这两个目标都实现了。观测到O VI 1031.9 A、1037.6 A和C III 977.0 A的强发射线，多普勒展宽到+/- 225 km/s，质心红移到350 km/s，与大麦哲伦星云一致。叠加在发射谱线上的是C III和O VI 1031.9在+260 km/s的吸收，这分别归因于LMC中的温暖和高温气体。O VI 1037.6 A线受到来自LMC和我们星系的星际和H2吸收的影响更严重。N III 989.8 A是看不到的，但模型表明叠加吸收严重衰减这条线。一些来自热气体的微弱谱线也被探测到，其中许多在河外超新星遗迹光谱中从未见过。
