Semi‐analytic modelling of galaxy evolution in the IR/submm range
Semi‐analytic modelling of galaxy evolution in the IR/submm range
复制标题
红外/亚毫米范围内星系演化的半解析建模
DOI：
10.1046/j.1365-8711.1998.01308.x
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发表时间：
1997
影响因子：
4.8
通讯作者：
B. Maffei
中科院分区：
文献类型：
--
作者：
B. Guiderdoni;E. Hivon;F. Bouchet;B. Maffei
本文提出了一种新的红外/亚毫米波长范围内星系特性的半解析模型，该模型明确地设置在宇宙学框架中。我们从描述原始扰动的非耗散和耗散坍缩开始，加入恒星形成，恒星演化和反馈，以及尘埃对星光的吸收及其在红外和亚毫米波中的再发射。这种方法在再现星系的光学特性方面取得了一些成功。我们随后提出了一个简单的红外/亚毫米范围的扩展。结构的增长是按照标准的冷暗物质模型进行的。我们假设恒星形成要么以“静止”模式进行，例如在圆盘中，要么以“爆发”模式进行，其时间尺度缩短了10倍。为了重现当前关于宇宙恒星形成速率和气体密度演化的数据，我们需要引入一个与“爆发”模式相关的质量分数，该质量分数随着红移而强烈增加，可能反映了相互作用和合并活动的增加。我们估计了这些“温和星暴”和“发光紫外/红外星系”的红外/亚毫米光度，并通过设计一系列与当前“宇宙约束”状态一致的进化场景，以及IRAS 60 μm光度函数和微弱计数，探索了多少恒星形成可能隐藏在严重熄灭的“超发光红外星系”中，但具有不同的高z红外光度密度。然而，这些场景产生的宇宙红外背景，其光谱落在Puget等人探测到的各向同性红外成分的±1σ范围内，Guiderdoni等人重新研究了这一范围。我们给出了在红外和亚毫米波段的微弱星系数量和红移分布的预测。亚毫米范围对进化情景的细节非常敏感。因此，ISO和SCUBA（以及后来的SIRTF， SOFIA， FIRST和PLANCK）正在进行和即将进行的观测将对z ~ 1及以后的星系演化施加强有力的限制。
This paper proposes a new semi-analytic modelling of galaxy properties in the IR/submm wavelength range, which is explicitly set in a cosmological framework. We start from a description of the non-dissipative and dissipative collapses of primordial perturbations, and add star formation, stellar evolution and feedback, as well as the absorption of starlight by dust and its re-emission in the IR and submm. This type of approach has had some success in reproducing the optical properties of galaxies. We hereafter propose a simple extension to the IR/submm range. The growth of structures is followed according to the standard cold dark matter model. We assume that star formation proceeds either in a ‘quiescent’ mode, e.g., as in discs, or in a ‘burst’ mode with 10 times shorter time-scales. In order to reproduce the current data on the evolution of the comoving cosmic star formation rate and gas densities, we need to introduce a mass fraction involved in the ‘burst’ mode strongly increasing with redshift, probably reflecting the increase of interaction and merging activity. We estimate the IR/submm luminosities of these ‘mild starburst’ and ‘luminous UV/IR galaxies’, and we explore how much star formation could be hidden in heavily extinguished, ‘ultraluminous IR galaxies’ by designing a family of evolutionary scenarios which are consistent with the current status of the ‘cosmic constraints’, as well as with the IRAS 60-μm luminosity function and faint counts, but with different high-z IR luminosity densities. However, these scenarios generate a cosmic infrared background whose spectrum falls within the ±1σ range of the isotropic IR component detected by Puget et al. and revisited by Guiderdoni et al. We give predictions for the faint galaxy counts and redshift distributions at IR and submm wavelengths. The submm range is very sensitive to the details of the evolutionary scenarios. As a result, the ongoing and forthcoming observations with ISO and SCUBA (and later with SIRTF, SOFIA, FIRST and PLANCK) will put strong constraints on the evolution of galaxies at z∼1 and beyond.