arXiv 2501.165542025-01-27astro-ph.EPastro-ph.SR

搜寻GEMS：两颗围绕M矮星的褐矮星的发现与表征

Searching for GEMS: Discovery and Characterization of Two Brown Dwarfs Around M Dwarfs

Alexander Larsen, Tera N. Swaby, Henry A. Kobulnicky, Caleb I. Canas, Shubham Kanodia, Jessica Libby-Roberts, Andrew Monson, Arvind Gupta, William Cochran, Suvr… 展开作者

Alexander Larsen, Tera N. Swaby, Henry A. Kobulnicky, Caleb I. Canas, Shubham Kanodia, Jessica Libby-Roberts, Andrew Monson, Arvind Gupta, William Cochran, Suvrath Mahadevan, Chad Bender, Scott A. Diddams, Samuel Halverson, Andrea S. J. Lin, Maxwell Moe, Joe Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gudmunder Stefansson

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AI总结：

本研究利用天基与地基测光及近红外视向速度，发现并表征了两颗围绕早期M矮星运行的凌星褐矮星TOI-5389Ab和TOI-5610b，并首次揭示短周期M矮星系统缺乏特定质量范围的褐矮星伴星。

摘要：

褐矮星填补了恒星与行星之间的空白，为行星和恒星形成机制提供了宝贵见解。然而，凌星褐矮星伴星的普查，特别是围绕M矮星的伴星，仍然不完整。我们报告了利用天基和地基测光以及近红外视向速度，发现两颗围绕低质量宿主恒星的凌星褐矮星。我们表征了TOI-5389Ab（$68.0^{+2.2}_{-2.2} \\ \mj$）和TOI-5610b（$40.4^{+1.0}_{-1.0} \\ \mj$），它们是围绕早期M矮星宿主（$\teff = 3569 \pm 59 \\ K$和$3618 \pm 59 \\ K$）运行的两颗中等质量褐矮星。对于TOI-5389Ab，最佳拟合参数为周期$P=10.40046 \pm 0.00002$天，半径$R_{\rm BD}=0.824^{+0.033}_{-0.031}$~\rj，低偏心率$e=0.0962^{+0.0027}_{-0.0046}$。特别是，这构成了最极端的亚恒星-恒星伴星与宿主质量比之一，$q=0.150$。对于TOI-5610b，最佳拟合参数为周期$P=7.95346 \pm 0.00002$天，半径$R_{\rm BD}=0.887^{+0.031}_{-0.031}$ \rj，中等偏心率$e=0.354^{+0.011}_{-0.012}$。预计两个目标的次凌星都很浅但可能可观测：两者在Johnson K波段均$\lesssim 500$ ppm。对M矮星/BD系统的统计分析首次揭示，与轨道稍宽的系统相比，短轨道周期（$P < 13$天）的系统缺乏$13 \mj < M_{\rm BD} < 40 \mj$的伴星（$q$ $<$ 0.1）。

英文摘要：

Brown dwarfs bridge the gap between stars and planets, providing valuable insight into both planetary and stellar formation mechanisms. Yet the census of transiting brown dwarf companions, in particular around M dwarf stars, remains incomplete. We report the discovery of two transiting brown dwarfs around low-mass hosts using a combination of space- and ground-based photometry along with near-infrared radial velocities. We characterize TOI-5389Ab ($68.0^{+2.2}_{-2.2} \ \mj$) and TOI-5610b ($40.4^{+1.0}_{-1.0} \ \mj$), two moderately massive brown dwarfs orbiting early M dwarf hosts ($\teff = 3569 \pm 59 \ K$ and $3618 \pm 59 \ K$, respectively). For TOI-5389Ab, the best fitting parameters are period $P=10.40046 \pm 0.00002$ days, radius $R_{\rm BD}=0.824^{+0.033}_{-0.031}$~\rj, and low eccentricity $e=0.0962^{+0.0027}_{-0.0046}$. In particular, this constitutes one of the most extreme substellar-stellar companion-to-host mass ratios of $q=0.150$. For TOI-5610b, the best fitting parameters are period $P=7.95346 \pm 0.00002$ days, radius $R_{\rm BD}=0.887^{+0.031}_{-0.031}$ \rj, and moderate eccentricity $e=0.354^{+0.011}_{-0.012}$. Both targets are expected to have shallow but potentially observable secondary transits: $\lesssim 500$ ppm in Johnson K band for both. A statistical analysis of M-dwarf/BD systems reveals for the first time that those at short orbital periods ($P < 13$ days) exhibit a dearth of $13 \mj < M_{\rm BD} < 40 \mj$ companions ($q$ $<$ 0.1) compared to those at slightly wider separations.

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