miniJPAS巡天：在AEGIS场中直到$z < 0.35$的发射线星系的识别和特征
The miniJPAS survey: Identification and characterization of the emission line galaxies down to $z < 0.35$ in the AEGIS field
摘要：
加速宇宙天体物理调查（J-PAS）的Javalambre物理学预计将在未来几年内使用56个窄带滤波器绘制数千平方度的北方天空。这将使J-PAS成为一个非常有竞争力和公正的发射线调查相比，光谱或窄带调查与更少的过滤器。miniJPAS测量覆盖1 deg $^2$，它使用与J-PAS相同的测光系统，但观测是用探路者J-PAS相机进行的。在这项工作中，我们确定和表征的样本的发射线星系（ELG）的红移低于$0.35$的迷你JPAS。使用基于人工神经网络的方法，我们检测ELG人口和测量的$Hα$，$Hβ$，[OIII]，和[NII]发射线的等效宽度和通量。我们使用[OIII]/H $β$与[NII]/H $α$（BPT）和EW（H $α$）与[NII]/H $α$（WHAN）图探索电离机制。我们确定了1787 ELG（$83$ %）的母样本（2154星系）在神盾局领域。对于具有可靠EW值的星系（总共2000个星系），我们得到$72.8 \pm 0.4$ %、$17.7 \pm 0.4$ %和$9.4 \pm 0.2$ %分别是恒星形成星系（SF）、活动星系核星系（Seyfert）和静止星系。基于$Hα$的流量，我们发现恒星形成主序被描述为$\log$ SFR $[M_\mathrm{\odot} \mathrm{yr}^{-1}] = 0.90^{+ 0.02}_{-0.02} \log M_{\star} [M_\mathrm{\odot}] -8.85^{+ 0.19}_{-0.20}$，并具有$0.20^{+ 0.01}_{-0.01}$的内禀散射。在三个红移仓：$0 < z \leq 0.15$，$0.15 < z \leq 0.25$，和$0.25 < z \leq 0.35$，这与以前的结果是一致的，基于测量的$Hα$发射线的SFR密度（$ρ_{\text{SFR}}$）的宇宙演化。
英文摘要：
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.
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