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 (${\rm M_{\star}} = 10^{10} - 10^{10.5} \, {\rm M_{\odot}}$).

中文翻译：

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不同质量尺度下的特定恒星形成率函数和猝灭：宇宙学模型与SDSS的比较

我们从斯隆数字巡天数据发布 DR7 (SDSS) 的子样本中呈现了不同恒星质量尺度下的爱丁顿偏差校正特定恒星形成率函数 (sSFRF)，在恒星质量 (${ \rm M_{\star}}$) 和恒星形成率（SFR）。以上使我们能够定性和定量地研究淬灭、被动/恒星形成星系的分布，并在同一 ${\rm M_{\star}} 内与最先进的宇宙学模型的预测进行比较$ 和 SFR 限制。我们发现在低质量端 (${\rm M_{\star}} = 10^{9.5} - 10^{10} \, {\rm M_{\odot}}$) sSFRF 主要由恒星形成物体。然而，移动到两个更大的 bin (${\rm M_{\star}} = 10^{10} - 10^{10.5} \, {\rm M_{\odot}}$ 和 ${\rm M_ {\star}} = 10^{10. 5} - 10^{11} \, {\rm M_{\odot}}$) 出现具有两个峰的双峰。一个峰值代表恒星形成人口，而另一个则描述了上升的被动人口。sSFRF 的双峰形式不能通过一系列宇宙学模拟（例如 Illustris、EAGLE、Mufasa、IllustrisTNG）再现，而是主要生成恒星形成群体，而双峰形式出现在其他人中（例如 L-星系、鲨鱼、辛巴）。我们的研究结果反映了需要重新考虑最先进模型中采用的淬火方案，包括允许“淬火星系”保留少量 SF 活动的处方（sSFR $=$ ${\rm 10^ {-11} {\rm yr^{-1}}}$-${\rm 10^{-12} {\rm yr^{-1}}}$) 并产生足够的被动种群/双模态即使在中等质量 (${\rm M_{\star}} = 10^{10} - 10^{10.5} \,