标题： 星系的固有SFRF和sSFRF：比较SDSS观测与IllustrisTNG模拟 显示英文标题

标题： The intrinsic SFRF and sSFRF of galaxies: comparing SDSS observation with IllustrisTNG simulation

摘要： 恒星形成率函数（SFRF）和特定恒星形成率函数（sSFRF）由于对估计的恒星形成率存在不确定性，会受到埃丁顿偏差的影响。我们开发了一种新的方法来校正这种偏差，并从斯隆数字巡天数据释放版7（SDSS DR7）中获得了内在的SFRF和sSFRF。内在的SFRF与之前依赖于紫外光SFR的文献测量值很好地吻合，但其高恒星形成端略低于红外和射电示踪剂的结果。我们证明了来自SDSS的内在sSFRF呈现双峰形式，其中一个峰值位于${\rm sSFR \sim 10^{-9.7} yr^{-1}}$表示恒星形成物体，另一个峰值位于${\rm sSFR \sim 10^{-12} yr^{-1}}$表示被淬灭的群体。此外，我们将观测结果与IllustrisTNG和Illustris模拟的预测进行了比较，显示“TNG”模型比其前身表现更好。然而，我们表明TNG模拟中的SFRF和宇宙恒星形成密度（CSFRD）高度依赖于分辨率，这反映了该模型及其当前最先进的模拟的局限性。我们演示了由SDSS观测暗示的双模态、双峰sSFRF无论采用何种盒子大小或分辨率，在TNG中均未出现。这一矛盾反映了需要在TNG模型中加入一种额外有效的淬灭机制。 显示英文摘要

摘要： The star formation rate function (SFRF) and specific star formation rate function (sSFRF) from the observation are impacted by the Eddington bias, due to the uncertainties on the estimated SFR. We develop a novel method to correct the Eddington bias and obtained the intrinsic SFRF and sSFRF from the Sloan Digital Sky Survey Data Release 7. The intrinsic SFRF is in good agreement with measurements from previous data in the literature that relied on UV SFRs but its high star-forming end is slightly lower than those IR and radio tracers. We demonstrate that the intrinsic sSFRF from SDSS has a bi-modal form with the one peak found at ${\rm sSFR \sim 10^{-9.7} yr^{-1}}$ representing the star-forming objects while the other peak is found at ${\rm sSFR \sim 10^{-12} yr^{-1}}$ representing the quenched population. Furthermore, we compare our observations with the predictions from the IllustrisTNG and Illustris simulations and show that the ``TNG'' model performs much better than its predecessor. However, we show that the simulated SFRF and cosmic star formation density (CSFRD) of TNG simulations are highly dependent on resolution, reflecting the limitations of the model and today state-of-the-art simulations. We demonstrate that the bi-modal, two peaked sSFRF implied by the SDSS observations does not appear in TNG regardless of the adopted box-size or resolution. This tension reflects the need for inclusion of an additional efficient quenching mechanism to the TNG model.