AI 中文总结
本研究利用JWST和ALMA数据对宇宙正午主序星系进行空间分辨SED建模，发现加入MIRI/ALMA可减少尘埃光度高估，并揭示恒星质量面密度与气体调控及恒星形成的关联。
AI 中文摘要
我们展示了从ALMA光谱巡天（ASPECS）在哈勃超深场中选出的35个主序星系在$z \approx 0.5-3.7$、恒星质量$\log(M_*/M_\odot) \sim 9.7-11.7$、恒星形成率$\mathrm{SFR} \sim 1.4-280\\,\mathrm{M_\odot\\,yr^{-1}}$的kpc尺度（$0.2''-0.5''$）物理性质图。利用独特的HST、JWST（NIRCam和MIRI）和ALMA观测，我们在紫外到远红外波段进行了空间分辨的光谱能量分布（SED）建模。我们发现，加入MIRI和/或ALMA数据可将尘埃光度的高估降低最多约$\sim0.8$ dex，而ALMA观测进一步缓解了年龄-尘埃简并。在缺乏此类数据的情况下，基于观测到的未分辨颜色限制SED模型库可以部分缓解这些偏差。从分辨和未分辨建模得到的恒星质量（$M_{*}$）在$\sim0.05$ dex内一致，这表明当包含静止系近红外（NIR；例如$\sim1-3\\,\mu\mathrm{m}$）数据时，质量差异（归因于外耀）对宇宙正午主序星系不那么显著。在归一化到相同参考后，我们样本的复合SED与局部星暴星系（如M82）非常相似，表明类似的尘埃消光和再辐射特性。最后，我们发现分子气体比例和耗尽时间与有效恒星质量面密度（$\Sigma_{\rm eff,*} = M_{*}/2\pi R_{\rm eff,M_*}^2$）的相关性与局部星系中观测到的相似。这些结果为恒星引力势如何影响局部宇宙之外星系中的气体调控和恒星形成提供了首个定性视角。
英文摘要
We present kpc-scale ($0.2''-0.5''$) physical property maps of 35 main-sequence galaxies at $z \approx 0.5-3.7$, with stellar masses of $\log(M_*/M_\odot) \sim 9.7-11.7$ and star formation rates of $\mathrm{SFR} \sim 1.4-280\,\mathrm{M_\odot\,yr^{-1}}$, selected from the ALMA Spectroscopic Survey (ASPECS) in the Hubble Ultra Deep Field. Leveraging the unique HST, JWST (NIRCam and MIRI), and ALMA observations, we perform spatially resolved spectral energy distribution (SED) modeling across the UV-to-FIR regime. We find that incorporating MIRI and/or ALMA data reduces the overestimation of dust luminosity (by up to $\sim0.8$ dex), while ALMA observations further mitigate the age-dust degeneracy. In the absence of such data, restricting the SED model library based on the observed unresolved colors can partially mitigate these biases. The stellar masses ($M_{*}$) derived from resolved and unresolved modeling are consistent within $\sim0.05$ dex, suggesting that mass discrepancies (attributed to outshining) are less significant for cosmic noon main-sequence galaxies when rest-frame near-infrared (NIR; e.g., $\sim1-3\,μ\mathrm{m}$) data are included. After normalization to the same reference, the composite SED of our sample closely resembles that of local starburst galaxies such as M82, suggesting similar dust attenuation and re-emission properties. Finally, we find that the molecular gas fraction and depletion time correlate with the effective stellar mass surface density ($Σ_{\rm eff,*} = M_{*}/2πR_{\rm eff,M_*}^2$) similarly to that observed in local galaxies. These results provide a first qualitative view of how the stellar gravitational potential influences gas regulation and star formation in galaxies beyond the local Universe.
Comments25 pages, 15 figures, 5 tables. Accepted for publication in MNRAS
