物以类聚：利用JWST/NIRCam解析被PLCK G165.7+67.0星系团引力透镜的一对红移z~2的同类尘埃恒星形成星系的恒星质量组装过程
Birds of a Feather: Resolving Stellar Mass Assembly With JWST/NIRCam in a Pair of Kindred $z \sim 2$ Dusty Star-forming Galaxies Lensed by the PLCK G165.7+67.0 Cluster
AI总结：
本研究构建了PLCK G165.7+67.0星系团的新参数透镜模型，结合JWST等多波段观测解析了红移z~2的一对并合尘埃恒星形成星系的空间分辨恒星形成性质，并预测该天区的超新星发生率，为高红移星系质量组装研究提供新观测约束。
摘要：
我们提出了G165.7+67.0星系团的一个新参数化透镜模型，该星系团是由Planck卫星通过其明亮的亚毫米波流量发现的，辐射来自红移z≈2.2处的一对特殊尘埃恒星形成星系（DSFGs）。结合JWST观测与毫米波/射电干涉观测，我们表征了这两个DSFG的内禀物理性质：它们在源平面上仅相距约1角秒（8千秒差距），速度差ΔV≲600 km s⁻¹，因此很可能正处于主并合过程中。两个星系的内禀恒星形成率分别为SFR_IR=320±70和400±80 M☉ yr⁻¹，恒星质量分别为log[M★/M☉]=10.2±0.1和10.3±0.1，尘埃消光分别为A_V=1.5±0.3和1.2±0.3，性质极为相似。我们利用JWST/NIRCam的静止帧近紫外到近红外成像数据，对两个星系开展了空间分辨的逐像素光谱能量分布（SED）拟合，将部分恒星结构的分辨尺度下探至100秒差距。基于分辨出的比恒星形成率和UVJ颜色，两个DSFG都正在经历显著的星系级恒星形成事件。如果它们确实存在引力相互作用，这次强烈的星暴可能是气体因首次近距离交会而被扰动的标志。相比之下，近期发现的三重成像超新星SN H0pe的寄主星系的恒星形成率远低于这两个DSFG，我们还发现了证据，表明该星系正发生由内向外的恒星形成 quenching（淬熄），且即便在比恒星形成率较低的区域也存在高柱密度的尘埃。根据从紫外到远红外SED建模得到的DSFG内禀恒星形成率预测，仅这一对天体每年就会产生1.1±0.2颗可观测的核心坍缩超新星（CCSNe），使得该星系团天区非常适合开展持续监测。
英文摘要：
We present a new parametric lens model for the G165.7+67.0 galaxy cluster, which was discovered with $Planck$ through its bright submillimeter flux, originating from a pair of extraordinary dusty star-forming galaxies (DSFGs) at $z\approx 2.2$. Using JWST and interferometric mm/radio observations, we characterize the intrinsic physical properties of the DSFGs, which are separated by only $\sim 1^{\prime\prime}$ (8 kpc) and a velocity difference $ΔV \lesssim 600~{\rm km}~{\rm s}^{-1}$ in the source plane, and thus likely undergoing a major merger. Boasting intrinsic star formation rates ${\rm SFR}_{\rm IR} = 320 \pm 70$ and $400 \pm 80~ M_\odot~{\rm yr}^{-1}$, stellar masses ${\rm log}[M_\star/M_\odot] = 10.2 \pm 0.1$ and $10.3 \pm 0.1$, and dust attenuations $A_V = 1.5 \pm 0.3$ and $1.2 \pm 0.3$, they are remarkably similar objects. We perform spatially-resolved pixel-by-pixel SED fitting using rest-frame near-UV to near-IR imaging from JWST/NIRCam for both galaxies, resolving some stellar structures down to 100 pc scales. Based on their resolved specific SFRs and $UVJ$ colors, both DSFGs are experiencing significant galaxy-scale star formation events. If they are indeed interacting gravitationally, this strong starburst could be the hallmark of gas that has been disrupted by an initial close passage. In contrast, the host galaxy of the recently discovered triply-imaged SN H0pe has a much lower SFR than the DSFGs, and we present evidence for the onset of inside-out quenching and large column densities of dust even in regions of low specific SFR. Based on the intrinsic SFRs of the DSFGs inferred from UV through FIR SED modeling, this pair of objects alone is predicted to yield an observable $1.1 \pm 0.2~{\rm CCSNe~yr}^{-1}$, making this cluster field ripe for continued monitoring.
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