Orbital and Mass Constraints of the Young Binary System IRAS 16293-2422 A,The Astrophysical Journal

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Orbital and Mass Constraints of the Young Binary System IRAS 16293-2422 A
The Astrophysical Journal ( IF 4.8 ) Pub Date : 2020-07-02 , DOI: 10.3847/1538-4357/ab960b
Mara Jos Maureira ₁ , Jaime E. Pineda ₁ , Dominique M. Segura-Cox ₁ , Paola Caselli ₁ , Leonardo Testi ₂ , Giuseppe Lodato ₃ , Laurent Loinard _{4,

5} , Antonio Hernndez-Gmez _{4,

6,

7}

Affiliation

We present 3 mm ALMA continuum and line observations at resolutions of 6.5 au and 13 au respectively, toward the Class 0 system IRAS 16293-2422 A. The continuum observations reveal two compact sources towards IRAS 16293-2422 A, coinciding with compact ionized gas emission previously observed at radio wavelengths (A1 and A2), confirming the long-known radio sources as protostellar. The emission towards A2 is resolved and traces a dust disk with a FWHM size of ~12 au, while the emission towards A1 sets a limit to the FWHM size of the dust disk of ~4 au. We also detect spatially resolved molecular kinematic tracers near the protostellar disks. Several lines of the J=5-4 rotational transition of HNCO, NH2CHO and t-HCOOH are detected, with which we derived individual line-of-sight velocities. Using these together with the CS (J=2-1), we fit Keplerian profiles towards the individual compact sources and derive masses of the central protostars. The kinematic analysis indicates that A1 and A2 are a bound binary system. Using this new context for the previous 30 years of VLA observations, we fit orbital parameters to the relative motion between A1 and A2 and find the combined protostellar mass derived from the orbit is consistent with the masses derived from the gas kinematics. Both estimations indicate masses consistently higher (0.5< M1

中文翻译：

年轻双星系统 IRAS 16293-2422 A 的轨道和质量约束

我们分别针对 0 类系统 IRAS 16293-2422 A 以 6.5 au 和 13 au 的分辨率呈现 3 mm ALMA 连续谱和线观测。连续谱观测揭示了 IRAS 16293-2422 A 的两个紧凑源，与致密电离气体发射一致之前在射电波长（A1 和 A2）上观察到，证实了众所周知的射电源是原恒星。向 A2 的发射被解析并追踪一个 FWHM 大小约为 12 au 的尘埃盘，而向 A1 的发射对尘埃盘的 FWHM 大小设置了一个限制，约为 4 au。我们还在原恒星盘附近探测到空间分辨的分子运动示踪剂。检测到 HNCO、NH2CHO 和 t-HCOOH 的 J=5-4 旋转跃迁的几条线，我们从中得出了单独的视线速度。将这些与 CS (J=2-1) 一起使用，我们将开普勒剖面拟合到各个致密源并推导出中央原恒星的质量。运动学分析表明 A1 和 A2 是一个有界二元系统。在 VLA 之前 30 年的观测中使用这种新背景，我们将轨道参数拟合到 A1 和 A2 之间的相对运动，并发现从轨道导出的组合原恒星质量与从气体运动学导出的质量一致。两种估计都表明质量始终较高（0.5< M1 我们将轨道参数拟合到 A1 和 A2 之间的相对运动，发现从轨道导出的组合原恒星质量与从气体运动学导出的质量一致。两种估计都表明质量始终较高（0.5< M1 我们将轨道参数拟合到 A1 和 A2 之间的相对运动，并发现从轨道导出的组合原恒星质量与从气体运动学导出的质量一致。两种估计都表明质量始终较高（0.5< M1

更新日期：2020-07-02

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