论文标题
$ z \ sim $ 0.62在黎明调查中对H $α$发射器的全面研究：对深层和宽区域的需求
A comprehensive study of H$α$ emitters at $z \sim$ 0.62 in the DAWN survey: the need for deep and wide regions
论文作者
论文摘要
我们介绍了h $α$选择的样本，以$ z \ sim0.62 $从深和宽狭窄的波段（黎明）调查中选择样品的亮度函数（LF）和恒星形成速率密度（SFRD）的新估计值。我们的结果是基于扩展宇宙区域中新的H $α$样品（与Coughlin等人2018相比），其中包括侧翼场，导致总面积覆盖率为$ \ sim $ 1.5 $^2 $。基于使用Spectro-Photomportric Redshifts和宽带色彩分类的强大选择标准选择了总共241 h $α$发射器。我们通过使用恒定的粉尘消光校正来计算LF和SFRD来探索不同的灰尘校正处方的效果，A {$ _ {\ textrm {h}α} = 1 $} mag，依赖于亮度的校正和出色的依赖性依赖性依赖性。使用具有最佳参数的Schechter函数：L $^*= 10^{42.24} $ erg s $^{ - 1} $，$ ϕ^*= 10^*= 10^{ - 2.85} $ MPC $^{ - 3} $，$ n = -1.3} $，$α= -1.3} $，$α= - 3} $，$ a = -1.3} $，$α= 10^{ - 2.85} $ mpc $^{ - 3} $，$ n = -3} $，$α= -1.62 l $^*= 10^{42.31} $ erg s $^{ - 1} $，$ ϕ^*= 10^{ - 2.8} $ mpc $^{ - 3} $，$α= -1.39 $，用于光度互动的粉尘校正，以及l $^*= 10^*= 10^$ er^$ er s $ er^$ erg s $ er $ ϕ^*= 10^{ - 2.91} $ mpc $^{ - 3} $，$α= -1.48 $，用于恒星质量依赖的尘埃校正。黎明调查的深度和广泛的性质有效地在广泛的亮度范围内采样了h $α$发射器，从而在LF的微弱和明亮的端提供了更好的限制。另外，SFRD估计$ρ_ {\ textrm {sfr}} = 10^{ - 1.39} $ m $ _ {\ odot} $ yr $^{ - 1} $ mpc $^{ - 3} $ m $ _ {\ odot} $ yr $^{ - 1} $ mpc $^{ - 3} $（与光度相关的灰尘校正）和$ρ_ {\ textrm {sfr}} = 10^10^{ - 1.49} （恒星质量依赖的尘埃校正）与从以前的H $α$调查中看到的红移（$ 0 <z <2 $）的SFRD的演变非常吻合。
We present new estimates of the luminosity function (LF) and star formation rate density (SFRD) for an H$α$ selected sample at $z\sim0.62$ from the Deep And Wide Narrow-band (DAWN) survey. Our results are based on a new H$α$ sample in the extended COSMOS region (compared to Coughlin et al. 2018) with the inclusion of flanking fields, resulting in a total area coverage of $\sim$1.5 deg$^2$. A total of 241 H$α$ emitters were selected based on robust selection criteria using spectro-photometric redshifts and broadband color-color classification. We explore the effect of different dust correction prescriptions by calculating the LF and SFRD using a constant dust extinction correction, A{$_{\textrm{H}α}=1$} mag, a luminosity-dependent correction, and a stellar-mass dependent correction. The resulting H$α$ LFs are well fitted using Schechter functions with best-fit parameters: L$^*=10^{42.24}$ erg s$^{-1}$, $ϕ^*=10^{-2.85}$ Mpc$^{-3}$, $α= -1.62$ for constant dust correction, L$^*=10^{42.31}$ erg s$^{-1}$, $ϕ^*=10^{-2.8}$ Mpc$^{-3}$, $α=-1.39$ for luminosity-dependent dust correction, and L$^*=10^{42.36}$ erg s$^{-1}$, $ϕ^*=10^{-2.91}$ Mpc$^{-3}$, $α= -1.48$, for stellar mass-dependent dust correction. The deep and wide nature of the DAWN survey effectively samples H$α$ emitters over a wide range of luminosities, thereby providing better constraints on both the faint and bright end of the LF. Also, the SFRD estimates $ρ_{\textrm{SFR}}=10^{-1.39}$ M$_{\odot}$yr$^{-1}$Mpc$^{-3}$ (constant dust correction), $ρ_{\textrm{SFR}}=10^{-1.47}$ M$_{\odot}$yr$^{-1}$Mpc$^{-3}$ (luminosity-dependent dust correction), and $ρ_{\textrm{SFR}}=10^{-1.49}$ M$_{\odot}$yr$^{-1}$Mpc$^{-3}$ (stellar mass-dependent dust correction) are in good agreement with the evolution of SFRD across redshifts ($0 < z < 2$) seen from previous H$α$ surveys.
