Dynamical masses for two M1 + mid-M dwarf binaries monitored during the SPHERE-SHINE survey
Dynamical masses for two M1 + mid-M dwarf binaries monitored during the SPHERE-SHINE survey
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SPHERE-SHINE 巡天期间监测到的两颗 M1 中 M 矮双星的动态质量
DOI：
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发表时间：
2021
影响因子：
6.5
通讯作者：
A. Roux
中科院分区：
文献类型：
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作者：
B. Biller;A. Grandjean;S. Messina;S. Desidera;P. Delorme;A. Lagrange;F. Hambsch;D. Mesa;M. Janson;R. Gratton;V. D’Orazi;M. Langlois;A. Maire;J. Schlieder;T. Henning;A. Zurlo;J. Hagelberg;S. Brown;C. Romero;M. Bonnefoy;G. Chauvin;M. Feldt;M. Meyer;A. Vigan;A. Pavlov;C. Soenke;D. LeMignant;A. Roux
我们提出了HIP 113201 AB和HIP 36985 AB的轨道拟合和动力学质量，这两个M1 +中M矮双星系统是SPHERE-SHINE调查的一部分。为了通过陀螺年代学确定这两个系统的年龄，我们使用40厘米的阿塔卡马沙漠远程天文台望远镜对HIP 113201和GJ 282 AB进行了光度监测活动，HIP 36985的两颗宽K星星同伴。基于这种监测和陀螺年代学关系，我们采用HIP 113201 AB的年龄为1.2 ± 0.1 Gyr，HIP 36985 AB的年龄为750 ± 100 Myr。这些系统足够古老，我们期望这些二进制文件的所有组件都已经到达主序列。为了获得HIP 113201 AB和HIP 36985 AB系统所有组件的动力学质量，我们使用并行回火马尔可夫链蒙特卡罗采样来拟合径向速度，直接成像以及盖亚和HIPPARCOS天体测量的组合。拟合HIP 113201的直接成像和径向速度数据，得到0.54 ± 0.03 M（cid：12）的初级质量，与其M1光谱类型完全一致，以及0.145 ± M（cid：12）的次级质量。在有和没有包括HIPPARCOS-Gaia数据的情况下得出的次级质量都比从伴星的测光估计的0.1 M（cid：12）质量大得多。因此，这颗伴星的动力学影响表明它的质量比测光所预期的要大。HIP 113201 B的一颗未被发现的褐矮星伴星可能是这种明显差异的自然解释。当年龄大于1陀螺时，HIP 113201 B的30 M木星伴星对系统光度的贡献可以忽略不计（< 1%），但可能会产生强烈的动力学影响。拟合HIP 36985 AB的直接成像、径向速度和HIPPARCOS-Gaia自行异常，我们发现其主质量为0.54 ± 0.01 M（cid：12），次质量为0.185 ± 0.001 M（cid：12），这与测光估计的组分质量、M矮星的M K -质量关系估计的质量以及文献中以前的动力学质量非常一致。
We present orbital fits and dynamical masses for HIP 113201AB and HIP 36985AB, two M1 + mid-M dwarf binary systems monitored as part of the SPHERE-SHINE survey. To robustly determine the age of both systems via gyrochronology, we undertook a photometric monitoring campaign for HIP 113201 and GJ 282AB, the two wide K star companions to HIP 36985, using the 40 cm Remote Observatory Atacama Desert telescope. Based on this monitoring and gyrochronological relationships, we adopt ages of 1.2 ± 0.1 Gyr for HIP 113201AB and 750 ± 100 Myr for HIP 36985AB. These systems are sufficiently old that we expect that all components of these binaries have reached the main sequence. To derive dynamical masses for all components of the HIP 113201AB and HIP 36985AB systems, we used parallel-tempering Markov chain Monte Carlo sampling to fit a combination of radial velocity, direct imaging, and Gaia and H IPPARCOS astrometry. Fitting the direct imaging and radial velocity data for HIP 113201 yields a primary mass of 0.54 ± 0.03 M (cid:12) , fully consistent with its M1 spectral type, and a secondary mass of 0.145 ± M (cid:12) . The secondary masses derived with and without including H IPPARCOS - Gaia data are all considerably more massive than the 0.1 M (cid:12) mass estimated from the photometry of the companion. Thus, the dynamical impacts of this companion suggest that it is more massive than expected from its photometry. An undetected brown dwarf companion to HIP 113201B could be a natural explanation for this apparent discrepancy. At an age > 1 Gyr, a 30 M Jup companion to HIP 113201B would make a negligible ( < 1%) contribution to the system luminosity but could have strong dynamical impacts. Fitting the direct imaging, radial velocity, and H IPPARCOS - Gaia proper motion anomaly for HIP 36985AB, we find a primary mass of 0.54 ± 0.01 M (cid:12) and a secondary mass of 0.185 ± 0.001 M (cid:12) , which agree well with photometric estimates of component masses, the masses estimated from M K – mass relationships for M dwarf stars, and previous dynamical masses in the literature.