论文标题
星系的内在SFRF和SSFRF：将SDSS观察与Illustristng模拟进行比较
The intrinsic SFRF and sSFRF of galaxies: comparing SDSS observation with IllustrisTNG simulation
论文作者
论文摘要
由于对估计的SFR的不确定性，观察结果的恒星形成速率函数（SFRF）和特定的恒星形成速率函数（SSFRF）受到爱丁顿偏见的影响。我们开发了一种新的方法来纠正爱丁顿偏见，并从斯隆数字天空调查数据发行7中获得了内在的SFRF和SSFRF。内在的SFRF与文献中先前数据的测量符合UV SFRS中的先前数据的测量，这些数据依赖于UV SFRS，但其高星形形成端比这些IR和无线电磁带略低。我们证明，来自SDSS的固有SSFRF具有双模式形式，其中一个峰值在$ {\ rm SSFR \ sim 10^{ - 9.7} yr^{ - 1}} $代表星形形成对象的$ {\ rm ssfr \ rm ssfr \ sim 10^yr，而另一个峰则在$ {\ rm ssfr \ sim $ sim $ { - 12^yr}中找到。淬火人口。此外，我们将观察结果与Illustristng和Illustris模拟的预测进行了比较，并表明``TNG''模型的性能胜于其前身。但是，我们表明，TNG模拟的模拟SFRF和宇宙星形形成密度（CSFRD）高度依赖于分辨率，这反映了模型的局限性以及当今最新的模拟。我们证明，无论采用的盒子大小或分辨率如何，TNG中都不会出现双模式，两个由SDSS观测值暗示的峰值SSFRF。这种张力反映了将额外有效的淬火机制纳入TNG模型的必要性。
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.
