论文标题
特定的星形形成率在不同的质量尺度和淬火下的功能：宇宙学模型与SDS之间的比较
The specific star formation rate function at different mass scales and quenching: A comparison between cosmological models and SDSS
论文作者
论文摘要
我们介绍了从斯隆数字天空调查数据发行DR7（SDSS）的子样本的不同恒星质量尺度上的Eddington偏差校正了特定的星形形成速率函数（SSFRF），这在恒星质量（$ {\ rm m _ {\ star}}} $）和星形组合率（$ {\ rm m _ {\ rm m _ {\ rm m _ {\ rm m _ {\ rm m _ {\ rm m _ {\ rm m _ {\ rm m _ {\ rm m _ {\ rm m _ {\ rm m _ {\ rm m _ {\ rm m _ {以上使我们能够进行定性和定量淬火，被动/星形形成星系的分布，并与最先进的宇宙学模型的预测进行比较，并在相同的$ {\ rm m _ {\ star}}} $和SFR限制内进行比较。我们发现在低质量端（$ {\ rm m _ {\ star}} = 10^{9.5} -10^{10} \，{\ rm m _ {\ odot}} $）SSFRF最多由星形对象主导。但是，移至两个更大的垃圾箱（$ {\ rm m _ {\ star}} = 10^{10} - 10^{10.5} \，{\ rm m _ {\ odot}}} $ M _ {\ odot}} $）出现了两个峰值的双模式。一个峰代表着恒星形成的人群，而另一个峰描述了被动种群的上升。 SSFRF的双模式形式并非由一系列宇宙学模拟（例如Illustris，Eagle，Mufasa，Illustristng）复制，这些模拟主要产生恒星形成的种群，而在其他人中则出现双模式（例如，L-Galaxies，Shark，Shark，Shark，Shark，Shark，Shark，Shark，Shark）。我们的发现反映了需要重新考虑的最先进模型中使用的淬火方案的必要性，涉及允许“淬火星系”的处方，以保留少量的SF活动（SSFR $ = $ = $ = $ {\ rm 10^{-11}}}} { - 11} {\ rm yr yr yr yr yr yr^{ - 1}}}} {\ rm yr^{ - 1}}} $）即使在中间群众（$ {\ rm m _ {\ rm m _ {\ star}} = 10^{10} -10} -10^{10.5} {10.5} \，，{10.5} \，，{\ rm m m _ {\ odot）。
We present the eddington bias corrected Specific Star Formation Rate Function (sSFRF) at different stellar mass scales from a sub-sample of the Sloan Digital Sky Survey Data Release DR7 (SDSS), which is considered complete both in terms of stellar mass (${\rm M_{\star}}$) and star formation rate (SFR). The above enable us to study qualitatively and quantitatively quenching, the distribution of passive/star-forming galaxies and perform comparisons with the predictions from state-of-the-art cosmological models, within the same ${\rm M_{\star}}$ and SFR limits. We find that at the low mass end (${\rm M_{\star}} = 10^{9.5} - 10^{10} \, {\rm M_{\odot}}$) the sSFRF is mostly dominated by star-forming objects. However, moving to the two more massive bins (${\rm M_{\star}} = 10^{10} - 10^{10.5} \, {\rm M_{\odot}}$ and ${\rm M_{\star}} = 10^{10.5} - 10^{11} \, {\rm M_{\odot}}$) a bi-modality with two peaks emerges. One peak represents the star-forming population, while the other describes a rising passive population. The bi-modal form of the sSFRFs is not reproduced by a range of cosmological simulations (e.g. Illustris, EAGLE, Mufasa, IllustrisTNG) which instead generate mostly the star-forming population, while a bi-modality emerges in others (e.g. L-Galaxies, Shark, Simba). Our findings reflect the need for the employed quenching schemes in state-of-the-art models to be reconsidered, involving prescriptions that allow "quenched galaxies" to retain a small level of SF activity (sSFR $=$ ${\rm 10^{-11} {\rm yr^{-1}}}$-${\rm 10^{-12} {\rm yr^{-1}}}$) and generate an adequate passive population/bi-modality even at intermediate masses (${\rm M_{\star}} = 10^{10} - 10^{10.5} \, {\rm M_{\odot}}$).
