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首页> 外文期刊>The Astrophysical journal >CONSTRAINED SIMULATIONS OF THE REAL UNIVERSE. Ⅱ. OBSERVATIONAL SIGNATURES OF INTERGALACTIC GAS IN THE LOCAL SUPERCLUSTER REGION
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CONSTRAINED SIMULATIONS OF THE REAL UNIVERSE. Ⅱ. OBSERVATIONAL SIGNATURES OF INTERGALACTIC GAS IN THE LOCAL SUPERCLUSTER REGION

机译：真实宇宙的约束模拟。 Ⅱ。局部超群区域星际气体的观测特征

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摘要

We present results of gasdynamics+N-body constrained cosmological simulations of the Local Superclus-ter region (LSC; about 30 h~(-1) Mpc around the Virgo cluster), which closely mimic the real universe within 100 Mpc, by imposing constraints from the MARK Ⅲ catalog of galaxy peculiar velocities. The simulations are used to study the properties and possible observational signatures of intergalactic medium in the LSC region. We find that in agreement with previous unconstrained simulations, ≈30% of the gas in this region is in the warm/hot phase at T ～ 10~5-10~7 K and ≈40% in the diffuse phase at T < 10~5 K in low-density regions. The X-ray emission from the warm/hot gas may represent a small (～5%-10%) but important contribution to the X-ray background observed by the ROSAT All-Sky Survey at energies around 1 keV. The best prospects for detection of the warm/hot intergalactic medium of the LSC located in filaments and in the vicinity of viri-alized regions of groups and clusters are through absorption in resonant lines of O Ⅶ and O Ⅷ in soft X-rays and in the O Ⅵ doublet in UV. If intergalactic gas in filaments (ρ/<ρ> ～ 1-10) is enriched to typical metallicities of approx> 0.05, the column densities of O Ⅵ, O Ⅶ, and O Ⅷ along a random line of sight near the north Galactic pole, especially near the supergalactic plane, have a significant probability to be in the range detectable by current (FUSE, XMM) and future (Constellation-X) instruments.
机译：我们介绍了局部超clter-ter区域（LSC；处女座星团周围约30 h〜（-1）Mpc）的气体动力学+ N体约束宇宙模拟的结果，这些结果通过施加约束来紧密模拟100 Mpc内的真实宇宙来自MARKⅢ星系特殊速度目录。该模拟用于研究LSC区域星系间介质的性质和可能的观测特征。我们发现，与以前的无约束模拟相一致，该区域中约30％的气体在T〜10〜5-10〜7 K时处于热/热相，而在T <10〜时的扩散相则≈40％。在低密度区域为5K。在1 keV左右的能量下，来自热/热气体的X射线发射可能对ROSAT全天空测量所观察到的X射线背景产生了很小的影响（约5％-10％）。探测位于细丝中以及群和团簇的玻璃化区域附近的LSC的热/热星系间介质的最佳前景是通过在软X射线和O的共振线中吸收OⅦ和O resonant。 OⅥ在紫外光下成对存在。如果细丝中的银河系气体（ρ/ <ρ>〜1-10）富集到典型的金属含量> 0.05，则OⅥ，O and和O column的列密度沿北银河极附近的随机视线，特别是在超银河系平面附近，有很大的可能性处于当前（FUSE，XMM）和未来（Constellation-X）仪器可检测的范围内。

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