Searching for C ii Emission from the First Sample of z ∼ 6 O i Absorption-associated Galaxies with the Atacama Large Millimeter/submillimeter Array

IF 4.8 2区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS
Yunjing Wu, Zheng Cai, Jianan Li, Kristian Finlator, Marcel Neeleman, J. Xavier Prochaska, Bjorn H. C. Emonts, Shiwu Zhang, Feige Wang, Jinyi Yang, Ran Wang, Xiaohui Fan, Dandan Xu, Emmet Golden-Marx, Laura C. Keating, Joseph F. Hennawi
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Abstract

Abstract We report the first statistical analyses of [C ii ] and dust continuum observations in six strong O i absorber fields at the end of the reionization epoch obtained by the Atacama Large Millimeter/submillimeter Array (ALMA). Combined with one [C ii ] emitter reported in Wu et al., we detect one O i -associated [C ii ] emitter in six fields. At redshifts of O i absorbers in nondetection fields, no emitters are brighter than our detection limit within impact parameters of 50 kpc and velocity offsets between ±200 km s −1 . The averaged [C ii ]-detection upper limit is <0.06 Jy km s −1 (3 σ ), corresponding to the [C ii ] luminosity of L [C II ] < 5.8 × 10 7 L ⊙ and the [C ii ]-based star formation rate of SFR [C II ] <5.5 M ⊙ yr −1 . Cosmological simulations suggest that only ∼10 −2.5 [C ii ] emitters around O i absorbers have comparable SFR to our detection limit. Although the detection in one out of six fields is reported, an order of magnitude number excess of emitters obtained from our ALMA observations supports that the contribution of massive galaxies that caused the metal enrichment cannot be ignored. Further, we also found 14 tentative galaxy candidates with a signal-to-noise ratio of ≈4.3 at large impact parameters (>50 kpc) and having larger outflow velocities within ±600 km s −1 . If these detections are confirmed in the future, then the mechanism of pushing metals at larger distances with higher velocities needs to be further explored from the theoretical side.
用阿塔卡马大型毫米/亚毫米阵列搜索z ~ 6 O i吸收相关星系首个样本的C ii发射
摘要本文首次对阿塔卡马大型毫米波/亚毫米波阵列(ALMA)获得的6个强毫米波吸收场再电离期末的[C ii]和尘埃连续体观测数据进行了统计分析。结合Wu等人报道的一个[C ii]发射器,我们在六个领域检测到一个O i相关的[C ii]发射器。在非检测场的O - i吸收体的红移中,在撞击参数为50 kpc和速度偏移在±200 km s - 1之间的范围内,没有发射体比我们的检测极限更亮。平均[C ii]探测上限为0.06 Jy km s−1 (3 σ),对应于L [C ii] <的[C ii]光度;5.8 × 10.7 L⊙和SFR [Cⅱ]<5.5 M⊙yr−1的基于[Cⅱ]的恒星形成速率。宇宙学模拟表明,只有O i吸收器周围的~ 10−2.5 [C ii]发射器具有与我们的检测极限相当的SFR。虽然在六分之一的磁场中被发现,但从我们的ALMA观测中获得的发射器数量超过了数量级,这支持了导致金属富集的大质量星系的贡献是不可忽视的。此外,我们还发现了14个暂定的候选星系,它们在大撞击参数(>50 kpc)下的信噪比为≈4.3,并且在±600 km s−1以内具有较大的流出速度。如果这些探测在未来得到证实,那么在更大的距离上以更高的速度推动金属的机制需要从理论方面进一步探索。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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来源期刊
Astrophysical Journal
Astrophysical Journal 地学天文-天文与天体物理
CiteScore
8.40
自引率
30.60%
发文量
2854
审稿时长
1 months
期刊介绍: The Astrophysical Journal is the foremost research journal in the world devoted to recent developments, discoveries, and theories in astronomy and astrophysics.
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