发表机构
School of Physics, Trinity College Dublin, the University of Dublin; Center for Astrophysics, Harvard & Smithsonian; Department of Astronomy and Steward Observatory, University of Arizona; UK Astronomy Technology Centre, Royal Observatory Edinburgh（都柏林三一学院物理学院，都柏林大学; 哈佛-史密森尼天体物理中心; 亚利桑那大学天文系和斯图尔德天文台; 英国天文学技术中心，爱丁堡皇家天文台）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究利用 ALMA 观测重新分析 ε Eridani 碎片盘，发现其外带近乎圆形且动力学冷，并约束了额外行星的质量与轨道范围。
AI 中文摘要
邻近（3.2 pc）的 K2V 恒星 ε Eridani 拥有最近探测到的碎片盘和一颗类木星系外行星（ε Eridani b）。在本工作中，我们重新分析了 ε Eridani 的 ALMA 波段 6（1.29 mm）观测数据，以评估其外部碎片带是否具有非零偏心率，这可能由行星-盘相互作用引起。考虑两种模型，一种考虑盘的受迫偏心率（e_f），另一种考虑固有偏心率（e_p），我们给出了严格的（99.7 百分位）上限分别为 e_f < 2.6% 和 e_p < 6.8%，并发现了非零受迫偏心率 e_f = 1.62^{+0.39}_{-0.40}% 的初步证据，置信度为 4σ。这是迄今为止任何碎片盘受迫偏心率的最低毫米波导出的上限，加上固有偏心率的低上限，表明外带近乎圆形且动力学上冷。我们进一步结合 Spitzer/IRAC、JWST/NIRCam F444W 和 JWST/MIRI F2550W 数据，探索与这些 ALMA 结果一致的行星系统架构。总之，这些分析为这个邻近系统中的潜在行星-盘相互作用提供了见解，将 ε Eridani b 之外的任何额外行星的质量限制在约 2×10^{-4} 至 0.3 M_Jup 范围内，轨道间隔约 6-60 au。
英文摘要
The nearby (3.2 pc) K2V star $ε$ Eridani hosts the closest detected debris disk and an exo-Jupiter analog ($ε$ Eridani b). In this work, we reanalyse ALMA Band 6 (1.29 mm) observations of $ε$ Eridani to assess whether its outer debris belt exhibits a non-zero eccentricity, potentially induced by planet-disk interactions. Considering two models, one that accounts for the disk's forced eccentricity ($e_\mathrm{f}$) and another that accounts for a proper eccentricity ($e_\mathrm{p}$), we place stringent (99.7th-percentile) upper limits of $e_\mathrm{f} < 2.6\%$ and $e_\mathrm{p} < 6.8\%$, respectively, and find tentative evidence for a non-zero forced eccentricity of $e_\mathrm{f} = 1.62^{+0.39}_{-0.40}\%$ at the $4σ$ level. This corresponds to the lowest millimeter-derived upper limit on the forced eccentricity of any debris disk to date, which, together with the low upper limit on the proper eccentricity, suggests that the outer belt is nearly circular and dynamically cold. We further explore planetary system architectures that are consistent with these ALMA-based results in combination with Spitzer/IRAC, JWST/NIRCam F444W, and JWST/MIRI F2550W data. Together, these analyses provide insight into potential planet-disk interactions in this nearby system, constraining any additional planet beyond $ε$ Eridani b to masses ranging from $\sim 2\times10^{-4}$ to $0.3\,M_\mathrm{Jup}$ at orbital separations of $\sim 6$-$60$ au.
Comments22 pages, 10 figures, 1 table, accepted for publication in ApJ
