THE GALAXY UV LUMINOSITY FUNCTION BEFORE THE EPOCH OF REIONIZATION
THE GALAXY UV LUMINOSITY FUNCTION BEFORE THE EPOCH OF REIONIZATION
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DOI：
10.1088/0004-637x/813/1/21
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发表时间：
2015-08
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影响因子：
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通讯作者：
C. Mason;M. Trenti;T. Treu
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文献类型：
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作者：
C. Mason;M. Trenti;T. Treu
我们提出了一个模型的星系紫外线（UV）光度函数（LF）在宇宙时间的星星的形成与组装的暗物质晕的假设下的质量依赖，但红移无关，效率的演变。我们介绍了一个新的自洽治疗晕星星形成的历史，这使我们能够在z > 10（回顾时间为500万年），当增长迅速的预测。通过在单个红移处进行校准以设置恒星与晕的质量比，并且没有进一步的自由度，我们的模型捕获了所有可用观测（0 z 10）的UV LF的演化。目前可探测到的z 108以上星系光度密度的显著下降可以用星星形成向质量较小、较暗的星系转移来解释。假设星星的形成过程是原子冷却晕，我们得到再电离光学深度τ = 0.056 - 0.010 + 0.007，？>与最新的普朗克测量结果完全一致，这意味着宇宙在z = 7.84 − 0.98 + 0.65处完全重电离。?>此外，我们的模型自然地产生平稳上升的星星形成历史的星系与L L * 与观测和流体动力学模拟。在z > 10的再电离时期之前，我们预测LF仍然可以用谢克特函数很好地描述，但有一个越来越陡的暗端斜率（在z = 16时α = −3.5）。最后，我们构建了詹姆斯·韦伯空间望远镜（JWST）和宽视场红外巡天望远镜（WFIRST）巡天的预测，并预测将观测到z 14的星系。在z > 15处的Galerkin只有在强透镜放大的帮助下才可能被JWST和WFIRST所接近。
We present a model for the evolution of the galaxy ultraviolet (UV) luminosity function (LF) across cosmic time where star formation is linked to the assembly of dark matter halos under the assumption of a mass-dependent, but redshift-independent, efficiency. We introduce a new self-consistent treatment of the halo star formation history, which allows us to make predictions at z > 10 (lookback time ≲500 Myr), when growth is rapid. With a calibration at a single redshift to set the stellar-to-halo mass ratio, and no further degrees of freedom, our model captures the evolution of the UV LF over all available observations (0 ≲ z ≲ 10). The significant drop in luminosity density of currently detectable galaxies beyond z ∼ 8 is explained by a shift of star formation toward less massive, fainter galaxies. Assuming that star formation proceeds down to atomic cooling halos, we derive a reionization optical depth τ = 0.056 − 0.010 + 0.007 , ?> fully consistent with the latest Planck measurement, implying that the universe is fully reionized at z = 7.84 − 0.98 + 0.65 . ?> In addition, our model naturally produces smoothly rising star formation histories for galaxies with L ≲ L * in agreement with observations and hydrodynamical simulations. Before the epoch of reionization at z > 10 we predict the LF to remain well-described by a Schechter function, but with an increasingly steep faint-end slope (α ∼ −3.5 at z ∼ 16). Finally, we construct forecasts for surveys with James Webb Space Telescope (JWST) and Wide-field Infrared Survey Telescope (WFIRST) and predict that galaxies out to z ∼ 14 will be observed. Galaxies at z > 15 will likely be accessible to JWST and WFIRST only through the assistance of strong lensing magnification.