IN-SYNC VI. Identification and Radial Velocity Extraction for 100+ Double-Lined Spectroscopic Binaries in the APOGEE/IN-SYNC Fields
M. A. Fernandez, Kevin R. Covey, Nathan De Lee, S. Drew Chojnowski, David Nidever, Richard Ballantyne, Michiel Cottaar, Nicola Da Rio, Jonathan B. Foster, Steve… 展开作者
M. A. Fernandez, Kevin R. Covey, Nathan De Lee, S. Drew Chojnowski, David Nidever, Richard Ballantyne, Michiel Cottaar, Nicola Da Rio, Jonathan B. Foster, Steven R. Majewski, Michael R. Meyer, A. M. Reyna, G. W. Roberts, Jacob Skinner, Keivan Stassun, Jonathan C. Tan, Nicholas Troup, Gail Zasowski
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Accepted for publication in PASP, 17 pages, 11 figures
We present radial velocity measurements for 70 high confidence, and 34 potential binary systems in fields containing the Perseus Molecular Cloud, Pleiades, NGC 2264, and the Orion A star forming region. 18 of these systems have been previously identified as binaries in the literature. Candidate double-lined spectroscopic binaries (SB2s) are identified by analyzing the cross-correlation functions (CCFs) computed during the reduction of each APOGEE spectrum. We identify sources whose CCFs are well fit as the sum of two Lorentzians as likely binaries, and provide an initial characterization of the system based on the radial velocities indicated by that dual fit. For systems observed over several epochs, we present mass ratios and systemic velocities; for two systems with observations on eight or more epochs, and which meet our criteria for robust orbital coverage, we derive initial orbital parameters. The distribution of mass ratios for multi-epoch sources in our sample peaks at q=1, but with a significant tail toward lower q values. Tables reporting radial velocities, systemic velocities, and mass ratios are provided online. We discuss future improvements to the radial velocity extraction method we employ, as well as limitations imposed by the number of epochs currently available in the APOGEE database. The Appendix contains brief notes from the literature on each system in the sample, and more extensive notes for select sources of interest.
Double-lined spectroscopic binaries in the APOGEE DR16 and DR17 data
在测量恒星径向速度（RV）时，远地点辐射谱提供了$\lesssim$ 1 km s $^{-1}$的精度。即使当多颗恒星被捕获在同一光谱中时，这也是成立的，就像双线光谱联星（SB 2）最常见的情况一样，尽管也可能发生不相关恒星的随机视线对准。我们开发了一个代码，自主识别SB2和高阶多次波的APOGEE光谱，导致7273候选SB2，813 SB3和19 SB4。我们估计的质量比的二进制文件，并为这些系统的一个子集，有足够数量的测量，我们执行一个完整的轨道拟合，确认大多数系统周期$<$ 10天循环。总的来说，我们在主序星矮星中发现了一个SB2分数（$F_{SB2}$）$\sim$ 3，并且$F_{SB2}$随恒星温度的变化没有明显的趋势.我们还能够在金属丰度较低的来源中恢复较高的$F_{SB2}$，但存在一些观测偏差。我们还检查了TESS的光变曲线，以确定这些光谱双星中哪些也是日食。这样的系统，特别是那些也是主序前后的系统，是进行后续分析以确定其质量和温度的良好候选者。
Spectroscopic Binary Detection as Agent-Callable Tools: Detecting 40,000+ Main-Sequence Binary Candidates from SDSS DR19 APOGEE Spectra
The Ohio State University（俄亥俄州立大学）；Center for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University（俄亥俄州立大学宇宙学与天体粒子物理中心）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）
The Chemical Homogeneity of Single-Lined Spectroscopic Binaries in Open Clusters
University of Utah（犹他大学）；Texas Christian University（德克萨斯基督教大学）；Johns Hopkins University（约翰斯·霍普金斯大学）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Observatório Nacional（国家天文台）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Center for Computational Astrophysics, Flatiron Institute（平顿院计算天体物理中心）；American Museum of Natural History（美国自然历史博物馆）
Discovery of a Candidate Black Hole - Giant Star Binary System in the Galactic Field
我们报告的发现，第一个可能的黑洞在一个非相互作用的双星系统与外地红巨星。通过将来自阿帕奇点天文台星系演化实验（APOGEE）的径向速度测量与来自超新星全天空自动巡天（ASAS-SN）的光度变化数据相结合，我们确定了明亮的快速旋转巨星2 MASS J 05215658 +4359220是一个带有巨大的看不见的伴星的双星系统。随后的径向速度测量揭示了一个轨道周期为83天，离心率接近零的系统。这颗巨星的光度变化周期与轨道周期一致，表明恒星黑子和潮汐同步。根据光度、表面重力和温度对这颗巨星的质量和半径的限制，意味着它有一颗质量为$3.3^{+2.8}_{-0.7}$ M $_\odot$的伴星，这意味着它是一颗低质量的黑洞或质量极大的中子星。通过{ \it Gaia}对天体测量双星运动的测量将进一步表征该系统。这一发现证明了像APOGEE这样的大规模光谱测量和像ASAS-SN这样的全天空高节奏光度测量的潜力，以彻底改变我们对紧凑物体质量函数的理解，并测试双星演化和超新星机制的理论。
Binarity at LOw Metallicity (BLOeM): Projected rotational velocities
Instituto de Astrofísica de Canarias（加那利天体物理研究所）；Universidad de La Laguna（拉各纳大学）；Centro de Astrobiologìa (CSIC–INTA)（天体生物学中心（西班牙高等科学研究理事会-国家航空航天技术研究所））；Royal Observatory of Belgium（比利时皇家天文台）；Astrophysics Research Centre, School of Mathematics & Physics, Queen’s University, Belfast（贝尔法斯特女王大学数学与物理学院天体物理研究中心）；Argelander-Institut für Astronomie, Universität Bonn（波恩大学阿尔冈德天文学研究所）；Max-Planck-Institute for Astrophysics（马克斯·普朗克天体物理学研究所）
