论文标题
Minijpas调查：排放线星系的识别和表征降至$ z <0.35 $
The miniJPAS survey: Identification and characterization of the emission line galaxies down to $z < 0.35$ in the AEGIS field
论文作者
论文摘要
预计加速宇宙天体物理调查（J-PAS）的Javalambre物理预计将在未来几年用56个窄带过滤器绘制数千个北方天空的平方度。与光谱或窄带调查相比，这将使J-PAS成为非常具竞争力和公正的排放线调查。 Minijpas调查覆盖了1度$^2 $，并且使用了与J-PAS相同的光度系统，但是使用Pathfinder J-PAS摄像头进行了观测值。在这项工作中，我们识别并表征了从红移低于$ 0.35 $的Minijpas的排放线星系（ELG）样本。使用基于人工神经网络的方法，我们检测到ELG群体并测量$Hα$，$Hβ$，[OIII]和[NII]发射线的等效宽度和通量。我们使用图[oiii]/h $β$对[nii]/h $α$（bpt）和ew（h $α$）与[nii]/h $α$（whan）探索电离机制。我们从AEGIS领域的父样本（2154个星系）中识别出1787 ELG（$ 83 $％）。对于可以放置在Whan图中的可靠EW值的星系（总共2000个星系），我们获得了$ 72.8 \ pm 0.4 $ 0.4 $％，$ 17.7 \ pm 0.4 $％\ pm 0.4 $％，$ 9.4 \ pm 0.2 $ 0.2 $ 0.2 $ 0.2 $％是星形型（sf），活跃的星座核（Seyfert）和quiescenties and quiescenties，quiescenties and quiescenties siectiessies siqecencecencecencesies siqe cysendsiessiessiessies sysectiessies。基于$hα$的通量，我们发现星形组主序列被描述为$ \ log $ sfr $ [m_ \ mathrm {\ odot} \ mathrm {yr}^{ - 1} = 0.90^{+ 0.90^{+ 0.02} {+ 0.02} [m_ \ mathrm {\ odot}] -8.85^{+ 0.19} _ { - 0.20} $，并具有$ 0.20^{+ 0.01} _ { - 0.01} $的内在散布。 The cosmic evolution of the SFR density ($ρ_{\text{SFR}}$) is derived at three redshift bins: $0 < z \leq 0.15$, $0.15 < z \leq 0.25$, and $0.25 < z \leq 0.35$, which agrees with previous results that were based on measurements of the $Hα$ emission line.
The Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) is expected to map thousands of square degrees of the northern sky with 56 narrowband filters in the upcoming years. This will make J-PAS a very competitive and unbiased emission line survey compared to spectroscopic or narrowband surveys with fewer filters. The miniJPAS survey covered 1 deg$^2$, and it used the same photometric system as J-PAS, but the observations were carried out with the pathfinder J-PAS camera. In this work, we identify and characterize the sample of emission line galaxies (ELGs) from miniJPAS with a redshift lower than $0.35$. Using a method based on artificial neural networks, we detect the ELG population and measure the equivalent width and flux of the $Hα$, $Hβ$, [OIII], and [NII] emission lines. We explore the ionization mechanism using the diagrams [OIII]/H$β$ versus [NII]/H$α$ (BPT) and EW(H$α$) versus [NII]/H$α$ (WHAN). We identify 1787 ELGs ($83$%) from the parent sample (2154 galaxies) in the AEGIS field. For the galaxies with reliable EW values that can be placed in the WHAN diagram (2000 galaxies in total), we obtained that $72.8 \pm 0.4$%, $17.7 \pm 0.4$% , and $9.4 \pm 0.2$% are star-forming (SF), active galactic nucleus (Seyfert), and quiescent galaxies, respectively. Based on the flux of $Hα$ we find that the star formation main sequence is described as $\log$ SFR $[M_\mathrm{\odot} \mathrm{yr}^{-1}] = 0.90^{+ 0.02}_{-0.02} \log M_{\star} [M_\mathrm{\odot}] -8.85^{+ 0.19}_{-0.20}$ and has an intrinsic scatter of $0.20^{+ 0.01}_{-0.01}$. The cosmic evolution of the SFR density ($ρ_{\text{SFR}}$) is derived at three redshift bins: $0 < z \leq 0.15$, $0.15 < z \leq 0.25$, and $0.25 < z \leq 0.35$, which agrees with previous results that were based on measurements of the $Hα$ emission line.
