The ALPINE-ALMA [C ii ] survey: Investigation of 10 galaxies at z ∼ 4.5 with [O ii ] and [C ii ] line emission − ISM properties and [O ii ]−SFR relation
The ALPINE-ALMA [C ii ] survey: Investigation of 10 galaxies at z ∼ 4.5 with [O ii ] and [C ii ] line emission − ISM properties and [O ii ]−SFR relation
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ALPINE-ALMA [C-ii ] 调查：使用 [O-ii ] 和 [C-ii ] 线发射 — ISM 属性和 [O-] 调查 z ≤ 4.5 处的 10 个星系
DOI：
10.1093/mnras/stac071
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发表时间：
2022
影响因子：
4.8
通讯作者：
Silverman, J.
中科院分区：
文献类型：
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作者：
Vanderhoof, Brittany N.;Faisst, A. L.;Shen, L.;Lemaux, B. C.;Béthermin, M.;Capak, P. L.;Cassata, P.;Le Fèvre, O.;Schaerer, D.;Silverman, J.
利用Keck/MOSFIRE光谱和Subaru/MOIRCS窄带成像的光学[Oii]测量，我们呈现了10个主序星ALPINE星系（log（M/M）= 9.2−11.1和）atz = 4.5。这是在这些红移下最大的多波长样本，结合了紫外，光学和远红外的各种测量，包括阿尔马的[Cii] 158 m线发射和尘埃连续谱以及Spitzer光度法的H α发射。这是第一次，这个独特的样品使我们能够分析[Oii]和总恒星形成率（SFR）之间的关系和星际介质（ISM）的性质通过[Oii]/[Cii]和[Oii]/H α光度比atz = 4.5。[Oii]−SFR关系在4.5不能用标准的局部描述来描述，但与金属依赖关系相一致，假设金属丰度在太阳附近。为了解释我们的样品的和的测量的尘埃校正光度比，需要电离参数log（U）< −2和电子密度。前者与atz = 2−3的星系一致，但低于atz> 6。考虑到星系的特定SFR，后者可能略高于预期。这个试验样本的分析表明，典型的log（M/M）> 9的星系atz = 4.5，与它们的后代atz = 2具有大致相似的ISM特性，并表明自再电离atz> 6时代以来ISM特性的强烈演化。
We present 10 main-sequenceALPINEgalaxies (log (M/M⊙) = 9.2−11.1 and) atz∼ 4.5 with optical [Oii] measurements fromKeck/MOSFIRE spectroscopy andSubaru/MOIRCS narrow-band imaging. This is the largest such multiwavelength sample at these redshifts, combining various measurements in the ultraviolet, optical, and far-infrared including [Cii]158mline emission and dust continuum from ALMA and H α emission fromSpitzerphotometry. For the first time, this unique sample allows us to analyse the relation between [Oii] and total star-formation rate (SFR) and the interstellar medium (ISM) properties via [Oii]/[Cii] and [Oii]/H α luminosity ratios atz∼ 4.5. The [Oii]−SFR relation atz∼ 4.5 cannot be described using standard local descriptions, but is consistent with a metal-dependent relation assuming metallicities aroundsolar. To explain the measured dust-corrected luminosity ratios ofandfor our sample, ionization parameters log (U) < −2 and electron densitiesare required. The former is consistent with galaxies atz∼ 2−3, however lower than atz> 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⊙) > 9 galaxies atz∼ 4.5 to have broadly similar ISM properties as their descendants atz∼ 2 and suggest a strong evolution of ISM properties since the epoch of reionization atz> 6.