论文标题
恒星形成速率功能在电离时期的早期生长：一种带有静止框架光学排放的方法
Early Growth of the Star Formation Rate Function in the Epoch of Reionization: an Approach with Rest-frame Optical Emissions
论文作者
论文摘要
我们根据恒星形成率（SFRS（SFR）（SFRS），通过光谱能量分布（SED）拟合在烛台紫外线到烛台商品 - 南部和北面的星系的光学波长的数据中，以$ z \ sim6 $的形式提出了星形形成率函数（SFRF）。与先前的估计相比，通过使用对尘埃衰减校正的静止紫外线光度函数（LFS）相比，所得的SFRF表现出了过量，并且与远红外LF估计的估计值可比。这表明，$ z \ sim6 $的尘埃刺激性星系的数量密度仅基于REST-FRAME UV观测值，在以前的方法中被低估了。我们使用Schechter函数对SFRF进行参数化，并在固定微弱的斜率和特征数密度时获得特征SFR（$ {\ rm sfr}^*$）的最佳拟合参数。当宇宙恒星形成活动达到峰值时，最佳拟合$ {\ rm sfr}^*$ at $ z \ sim6 $与$ z \ sim2 $相当。连同使用REST-FRAME UV到光学数据的SFRF估计，$ {\ rm sfr}^*$从$ z \ sim2 $到$ z \ sim6 $大致恒定，并且可能会降低$ z \ sim6 $。由于$ {\ rm sfr}^*$对SFRF的高-SFR端敏感，因此$ {\ rm sfr}^*$的这种演变表明，SFRF的High-Sfr末端在re否时迅速生长，并在$ z2 $ \ sim2 $中观察到类似的水平。
We present a star formation rate function (SFRF) at $z\sim6$ based on star formation rates (SFRs) derived by spectral energy distribution (SED) fitting on data from rest-frame UV to optical wavelength of galaxies in the CANDELS GOODS-South and North fields. The resulting SFRF shows an excess compared to the previous estimations by using rest-frame UV luminosity functions (LFs) corrected for the dust attenuation, and is comparable to that estimated from a far-infrared LF. This suggests that the number density of dust-obscured intensively star-forming galaxies at $z\sim6$ has been underestimated in the previous approach based only on rest-frame UV observations. We parameterize the SFRF with using the Schechter function and obtain the best-fit parameter of the characteristic SFR (${\rm SFR}^*$) when the faint-end slope and characteristic number density are fixed. The best-fit ${\rm SFR}^*$ at $z\sim6$ is comparable to that at $z\sim2$, when the cosmic star formation activity reaches its peak. Together with SFRF estimations with similar approach using rest-frame UV to optical data, the ${\rm SFR}^*$ is roughly constant from $z\sim2$ to $z\sim6$ and may decrease above $z\sim6$. Since the ${\rm SFR}^*$ is sensitive to the high-SFR end of the SFRF, this evolution of ${\rm SFR}^*$ suggests that the high-SFR end of the SFRF grows rapidly during the epoch of reionization and reaches a similar level observed at $z\sim2$.
