arXiv 2406.035442024-06astro-ph.GA

基于JWST和ALMA的大质量恒星形成星系的结构：多尘埃的高红移盘状星系

The Structure of Massive Star-Forming Galaxies from JWST and ALMA: Dusty, High Redshift Disk Galaxies

Steven Gillman, Ian Smail, Bitten Gullberg, A. M. Swinbank, Aswin P. Vijayan, Minju Lee, Gabe Brammer, U. Dudzevičiūtė, Thomas R. Greve, Omar Almaini, Malte Bri… 展开作者

Steven Gillman, Ian Smail, Bitten Gullberg, A. M. Swinbank, Aswin P. Vijayan, Minju Lee, Gabe Brammer, U. Dudzevičiūtė, Thomas R. Greve, Omar Almaini, Malte Brinch, Scott C. Chapman, Chian-Chou Chen, Soh Ikarashi, Yuichi Matsuda, Wei-Hao Wang, Fabian Walter, Paul P. van der Werf

备注：: 23 pages, 13 figures. Accepted for publication in A&A
发表信息：: A&A 691, A299 (2024)
DOI：: 10.1051/0004-6361/202451006

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AI总结：

本研究利用JWST和ALMA分析80个大质量多尘埃恒星形成星系，发现多数并非晚期主并合，而是与普通星系共享盘状结构，但其较弱的核球导致动力学稳定性低，微小扰动引发更高活动性。

摘要：

我们分析了JWST PRIMER项目观测的80个大质量（$\log_{10}(M_\ast[M_{\odot}])$=11.2$\pm$0.1）多尘埃恒星形成星系的JWST NIRCam和MIRI形态学性质，这些星系位于$z$$=$2.7$^{+1.2}_{--0.7}$，由ALMA认证为亚毫米星系（SMGs）。为了将这些大质量活动星系的结构与较典型、活动性较低的恒星形成星系进行比较，我们定义了两个对比样本：第一个是比恒星形成率和红shift匹配的850个场星系，第二个是恒星质量匹配的80个场星系。我们确认20$\pm$5%的SMGs为候选晚期主并合，另有40$\pm$10%为潜在次并合，40$\pm$10%具有相对未受扰动的盘状形态且无明显的巨大邻星。这些比例与场样本相当，表明大多数亚毫米探测到的星系并非晚期主并合，其相互作用率与$z$$\sim$2-3处活动性较低的种群相似。我们确定SMGs的近红外尺寸与活动性较低的种群相当，但Sérsic指数较低，与无核球的盘状结构一致，且在2$\mu$m处的形态比4$\mu$m处更有结构。我们发现证据表明尘埃红化是种群间形态差异的起源，并确认F200W$-$F444W像素颜色与870$\mu$m表面亮度之间存在强相关性。我们得出结论，同一时期的SMGs和活动性较低的星系共享盘状结构，但SMGs较弱的核球成分导致较低的动力学稳定性。因此，由内部或外部微小扰动触发的不稳定性导致SMGs比典型恒星形成星系具有更高的活动性（和尘埃含量）。

英文摘要：

We present an analysis of the JWST NIRCam and MIRI morphological properties of 80 massive ($\log_{10}(M_\ast[M_{\odot}])$=11.2$\pm$0.1) dusty star-forming galaxies at $z$$=$2.7$^{+1.2}_{-0.7}$, identified as sub-millimetre galaxies (SMGs) by ALMA, that have been observed as part of the JWST PRIMER project. To compare the structure of these massive, active galaxies to more typical less actively star-forming galaxies, we define two comparison samples. The first of 850 field galaxies matched in specific star-formation rate and redshift and the second of 80 field galaxies matched in stellar mass. We identify 20$\pm$5% of the SMGs as candidate late-stage major mergers, a further 40$\pm$10% as potential minor mergers and 40$\pm$10% which have comparatively undisturbed disk-like morphologies, with no obvious massive neighbours. These rates are comparable to those for the field samples and indicate that the majority of the sub-millimetre-detected galaxies are not late-stage major mergers, but have interaction rates similar to the less-active population at $z$$\sim$2-3. We establish that SMGs have comparable near-infrared sizes to the less active populations, but exhibit lower Sérsic indices, consistent with bulge-less disks and have more structured morphologies at 2$μ$m relative to 4$μ$m. We find evidence for dust reddening as the origin of the morphological differences between the populations, identifying a strong correlation between the F200W$-$F444W pixel colour and the 870$μ$m surface brightness. We conclude that SMGs and less active galaxies at the same epochs share a common disk-like structure, but the weaker bulge components of the SMGs results in a lower dynamical stability. Consequently, instabilities triggered either secularly or by minor external perturbations result in higher levels of activity (and dust content) in SMGs compared to typical star-forming galaxies. [Abridged]

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