低z环银河系和银河系间介质的可观测特征：模拟中的UV线发射
Observable Signatures of the low-z Circum-Galactic and Inter-Galactic Medium : UV Line Emission in Simulations
摘要：
我们提出了第一次预测的紫外线发射的星系际和环星系气体的自适应网格分辨率（AMR）大尺度结构（LSS）模拟在红移0.3<z<1.2，特别强调与当前和不久的将来紫外仪器的可观测性。在三个感兴趣的转变（Lya，OVI和CIV）中，物体的类型存在明显的双峰性：绝大多数通量来自离散的紧凑源，而更大的体积分数则由更稀薄的气体填充。我们对这两种天体类型的数量密度、物理大小和形状、亮度、光度、速度结构、质量、温度、电离状态和金属含量进行了分析。将AMR网格降级为可用（如FIREBall）或可预见仪器的特征分辨率，可以评估从当前可能的观测中可以得出哪些推论，并为未来任务的观测策略奠定基础。一般来说，IGM和附属结构的微弱发射仍然超出了仅具有短时间暴露潜力的仪器的能力（平流层气球），即使是对Lya的乐观假设，而这些结构的较弱金属线转变对于长时间暴露仍将具有挑战性（天基望远镜），主要是由于低金属量推动它们的亮度比Lya辐射低三个数量级。对于环银河系介质（CGM）的情况是更有希望的，可以预见的是，在不久的将来，我们不仅会检测到这样的来源，但所有三条线的组合，除了速度信息将产生有价值的洞察力的物理过程，照亮重要的机制，在星系的形成和他们的反作用到IGM从那里他们形成。（abrigded）
英文摘要：
We present for the first time predictions for UV line emission of intergalactic and circumgalactic gas from Adaptive Mesh Resolution (AMR) Large Scale Structure (LSS) simulations at redshifts 0.3<z<1.2, with specific emphasis on observability with current and near-future UV instrumentation. In three transitions of interest (Lya, OVI and CIV) there is a clear bimodality in the type of objects : the overwhelming majority of flux stems from discrete, compact sources, while a much larger volume fraction is filled by more tenuous gas. We characterise both object types with regard to number density, physical size and shape, brightness, luminosity, velocity structure, mass, temperature, ionisation state, and metal content. Degrading AMR grids to characteristic resolutions of available (such as FIREBall) or foreseeable instrumentation, allows to assess which inferences can be drawn from currently possible observations, and set foundations to prepare observing strategies for future missions. In general, the faint emission of the IGM and filamentary structure remains beyond capabilities of instruments with only short duration exposure potential (stratospheric balloons), even for optimistic assumptions for Lya, while the yet fainter metal line transitions for these structures will remain challenging for long duration exposures (space-based telescopes), mostly due to low metallicity pushing them more than three orders of magnitudes in brightness below Lya radiation. For the circum-galactic medium (CGM) the situation is more promising, and it is foreseeable that in the near future we will not only just dectect such sources, but the combination of all three lines in addition to velocity information will yield valuable insight into the physical processes at hand, illuminating important mechanisms during the formation of galaxies and their backreaction onto the IGM from whence they formed. (abrigded)
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