阿塔卡马大型毫米/亚毫米波阵列协同腔室II. 空洞星系中的解析标度关系
ALMA CO-CAVITY II. Resolved Scaling Relations in Void Galaxies
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中文总结 AI 辅助
研究41个位于宇宙低密度区域的空洞星系中的解析施密特-肯尼卡特关系、分子气体主序和恒星形成主序，利用高分辨率数据拟合关系，发现rMGMS最紧密且受星系间差异影响小，其可能是最稳定的关系。
中文摘要 AI 辅助
涉及恒星形成率（SFR）、分子气体质量和恒星质量的标度关系是理解星系演化的关键，此前已在解析尺度上进行过探索。然而，尚未特别强调大规模环境（LSE）来研究它们。在这项工作中，我们从41个位于宇宙最低密度区域的空洞星系（VG）样本中研究了解析的施密特-肯尼卡特关系（rSK）、分子气体主序（rMGMS）和恒星形成主序（rSFMS）。使用来自阿塔卡马大型毫米/亚毫米波阵列协同腔室和腔室调查的高分辨率干涉CO（1-0）数据和光学积分场单元数据，在2.5
英文摘要
Scaling relations involving star formation rates (SFRs), molecular gas mass, and stellar mass are key to understand galaxy evolution, and have previously been explored at resolved scales. However, they have not been examined with particular emphasis on the large-scale environments (LSEs). In this work, we study the resolved Schmidt-Kennicutt relation (rSK), molecular gas main sequence (rMGMS) and star-forming main sequence (rSFMS) from a sample of 41 void galaxies (VGs) residing in the least dense regions of the Universe. Using high-resolution interferometric CO(1-0) data and optical IFU data from the ALMA CO-CAVITY and CAVITY surveys at scales of 2.5" (0.8-2.1 kpc), we study these relations for the full sample as well as for individual galaxies in voids. We fit the relations, finding a similar parametrisation as that used for galaxies from all LSEs. However, the rMGMS is the tightest of the three relations ($σ_{rMGMS}=0.16$ dex, $σ_{rSK}=0.21$ dex, and $σ_{rSFMS}=0.24$ dex), unlike in other samples. We find that a large source of deviations in the relations comes from galaxy-to-galaxy variations. However, the rMGMS is less affected by these variations. It has been suggested that the rMGMS arises from the concentration of molecular gas within the gravitational potential set by the stellar content and dark matter. We hypothesise that deviations from the rMGMS trace changes in the gravitational potential occurring on longer time-scales, whereas deviations in the rSK and the rSFMS are driven by more rapid variations in the SFR. This distinction is particularly relevant for our sample of VGs because the 41 ALMA CO-CAVITY VGs are more isolated than galaxies in other LSEs, and therefore are less affected by events that can significantly alter the gas distribution or trigger SF on short time-scales. In this sense, the rMGMS is likely the most stable of these relations over time.
