论文标题
Alpine-Alma [CII]调查：使用[OII]和[CII]线排放$ - $ ISM Properties和[OII] $ - $ SFR关系对10个星系的调查
The ALPINE-ALMA [CII] Survey: Investigation of 10 Galaxies at $z\sim4.5$ with [OII] and [CII] Line Emission $-$ ISM Properties and [OII]$-$SFR Relation
论文作者
论文摘要
我们提出$ 10 $主序列高山星系（log（$ m/m _ {\ odot} $）= 9.2-11.1和$ {\ rm sfr} = 23-190 \，{\ rm m _ {\ odot} Keck/Mosfire光谱和Subaru/Moirir窄带成像。这是这些红移处最大的此类多波长样本，结合了超紫外线，光学和远红外的各种测量结果，包括[CII] $ _ {158 {\ rmμm}} $线发射和来自Alma和H $α$α$α$α$α$α$α$α$α$α$α$α$α$α$α$α$α$α$α$α$α$α$α$。这个独特的样本首次使我们能够通过[OII]/[CII]和[OII]/\ HALPHA亮度比率分析[OII]和总星体形态率（SFR）（SFR）和星际介质（ISM）属性之间的关系。无法使用标准本地描述来描述[oii] $ - $ SFR关系，$ z \ sim4.5 $无法描述，但与金属依赖关系的关系是一致的，假设金属含量约为$ 50 \％$ $ solar。 To explain the measured dust-corrected luminosity ratios of $L[OII]/L[CII] \sim 0.98^{+0.21}_{-0.22}$ and $L[OII]/LHa \sim -0.22^{+0.13}_{-0.15}$ for our sample, ionization parameters $\log(U)< -2$ and electron密度$ \ log（\ rm n_e / {\ rm [cm^{ - 3}]}）\ sim 2.5-3 $。前者与$ z \ sim2-3 $的星系一致，但是低于$ z> 6 $。考虑到星系的特定SFR，后者可能略高于预期。对该试验样本的分析表明，典型的日志（$ m/m _ {\ odot}）$> 9个星系$ z \ sim4.5 $，具有与$ z \ sim2 $的后代相似的ISM属性，并暗示了自$ z> 6 $ ivioniation以来的ISM属性的强大进化。
We present $10$ main-sequence ALPINE galaxies (log($M/M_{\odot}$) = 9.2-11.1 and ${\rm SFR}=23-190\,{\rm M_{\odot}\,yr^{-1}}$) at $z\sim4.5$ with optical [OII] measurements from Keck/MOSFIRE spectroscopy and Subaru/MOIRCS narrow-band imaging. This is the largest such multi-wavelength sample at these redshifts, combining various measurements in the ultra-violet, optical, and far-infrared including [CII]$_{158{\rm μm}}$ line emission and dust continuum from ALMA and H$α$ emission from Spitzer photometry. For the first time, this unique sample allows us to analyze the relation between [OII] and total star-formation rate (SFR) and the interstellar medium (ISM) properties via [OII]/[CII] and [OII]/\halpha luminosity ratios at $z\sim4.5$. The [OII]$-$SFR relation at $z\sim4.5$ cannot be described using standard local descriptions, but is consistent with a metal-dependent relation assuming metallicities around $50\%$ solar. To explain the measured dust-corrected luminosity ratios of $L[OII]/L[CII] \sim 0.98^{+0.21}_{-0.22}$ and $L[OII]/LHa \sim -0.22^{+0.13}_{-0.15}$ for our sample, ionization parameters $\log(U)< -2$ and electron densities $\log(\rm n_e / {\rm [cm^{-3}]}) \sim 2.5-3$ are required. The former is consistent with galaxies at $z\sim2-3$, however lower than at $z>6$. The latter may be slightly higher than expected given the galaxies' specific SFR. The analysis of this pilot sample suggests that typical log($ M/M_{\odot})$ > 9 galaxies at $z\sim4.5$ to have broadly similar ISM properties as their descendants at $z\sim2$ and suggest a strong evolution of ISM properties since the Epoch of Reionization at $z>6$.
