论文标题
自从$ z \ sim4 $从fuv+ir亮度函数起
The star-forming main sequence and the contribution of dust-obscured star formation since $z\sim4$ from the FUV+IR luminosity functions
论文作者
论文摘要
提出了一种分析方法，以研究恒星形成星系（SFG）主序列（MS）的演变和灰尘刺激的SF的比例最高为$ z \ sim4 $。 Far-Ultraviolet（FUV）和红外（IR）星形形成率SFRS被描述为$ M _ {\ ast} $的条件概率函数。我们将它们与SFG的星系恒星质量函数（GSMF）相连，以得出FUV和IR LFS。 2 SF模式形式主义用于描述星际星系。通过拟合观察到的fuv和ir lfs，sfr $ _ {\ rm fuv} -m _ {\ ast} $和sfr $ _ {\ rm ir} -m _ {\ ast} $的参数化受到约束。与其他观察性推断相比，我们派生的SFR $ _ {\ rm fuv+ir} -m _ {\ ast} $重现了MS的演变。在任何红移时，我们都会发现SSFR $ _ {\ rm fuv+ir} -m _ {\ ast} $的关系，MS SFGS的关系接近高质量端的权力定律。在较低的质量下，它弯曲，最终在非常低的质量下从负向正变为正变化。在$ z \ sim0 $上，这种标志的更改为$ m _ {\ ast} \ sim5 \ times10^{8} {8} {\ rm m} _ {\ odot} $接近dust-obscured sf sf sfemime，$ m_ m} _ {\ odot} $。斜率标志的变化与FUV LF的膝盖有关。我们派生的尘埃刺激的分数与先前的确定$ 0 \ leq z \ leq2.5 $一致。尘埃刺激的分数在很大程度上取决于质量，而在$ z \ gtrsim1.2 $的红移几乎没有依赖性。与高红移同行相比，在$ z \ lyssim0.75 $高质量的星系变得更加“透明”。在相反的情况下，低质量和中间质量的星系已被灰尘遮盖。 GSMF和FUV和IR LFS的关节演化是研究质量生长和尘埃形成/破坏机制的有前途的方法。
An analytical approach is proposed to study the evolution of the star-forming galaxy (SFG) main sequence (MS) and the fraction of dust-obscured SF up to $z\sim4$. Far-ultraviolet (FUV) and infrared (IR) star formation rates, SFRs, are described as conditional probability functions of $M_{\ast}$. We convolve them with the galaxy stellar mass function (GSMF) of SFGs to derive the FUV and IR LFs. The 2 SF modes formalism is used to describe starburst galaxies. By fitting observed FUV and IR LFs, the parametrization of SFR$_{\rm FUV}-M_{\ast}$ and SFR$_{\rm IR}-M_{\ast}$ are constrained. Our derived SFR$_{\rm FUV+IR}-M_{\ast}$ reproduces the evolution of the MS as compared to other observational inferences. At any redshift, we find that the sSFR$_{\rm FUV+IR}-M_{\ast}$ relation for MS SFGs approaches to a power law at the high-mass end. At lower masses, it bends and eventually the slope sign changes from negative to positive at very low masses. At $z\sim0$, this change of sign is at $M_{\ast}\sim5\times10^{8}{\rm M}_{\odot}$ close to dust-obscured SF regime, $M_{\ast}\sim6\times10^{8}{\rm M}_{\odot}$. The slope sign change is related to the knee of the FUV LF. Our derived dust-obscured fractions agree with previous determinations at $0\leq z\leq2.5$. Dust-obscured fractions depend strongly on mass with almost no dependence with redshift at $z\gtrsim1.2$. At $z\lesssim0.75$ high-mass galaxies become more "transparent" compared to their high redshift counterparts. On the opposite, low- and intermediate-mass galaxies have become more obscured by dust. The joint evolution of the GSMF and the FUV and IR LFs is a promising approach to study mass growth and dust formation/destruction mechanisms.
