APOGEE likely binaries with estimated companion masses

This Zenodo has an assortment of data files related to Schochet, Tayar & Andrews (2024) "A Lack of Mass-Gap Compact Object Binaries in APOGEE" which sought to identify binary systems with a single stellar component that may be host to a "mass-gap" black hole/neutron star companion. These files utilize data from the Sloan Digital Sky Survey IV's (Blanton et al. 2017) Apache Point Galactic Evolution Experiment (Majewski et al. 2017) Data Release 17 (Abdurro'uf et al. 2022), including stellar abundances from the ASPCAP pipeline (Garcia Perez et al. 2016) and with spectra reduced using the Doppler (Nidever et al. 2015). Radius values used in the catalog come from Gaia + SED fitting (Yu et al. 2023).  

In this repository you will find:

Files

APOGEE_likely_binaries.csv: datafile contains basic information and IDs for the 4751 likely binary objects from our data reductions (2MASS ID, SNR, nvisits, vsini, vscatter, teff, log(g), M/H and errors for the final 3 stellar parameters).

For systems with a radius value from Yu et al. 2023 (4288/4751), we also provide:

apogee_objects_with_kiauhoku_masses.csv: this file contains masses and ages from the four grids of kiauhoku (Claytor et al. 2020) which include models from MIST (MESA Isochrones and Stellar Tracks, Choi et al. 2016 & Paxton et al. 2010), YREC (Yale Rotating stellar Evolution Code, Tayar et al. 2022 & Pinsonneault et al. 1989) Dart/DSEP (Dartmouth Stellar Evolution Program, Dotter et al. 2008), and GARSTEC/Gars (Garching Stellar Evolution Code, Serenelli et al. 2013 & Weiss & Schlattl 2008). These are in the final columns of the csv file, and other columns include Gaia IDs, APOGEE starflag and ASPCAP flags, and RA/Dec along with APOGEE Telescope and Field information for each target.

estimated_companions.csv: this file contains estimated minimum companion masses from the tidal synchronization method (CO_mass_rsync) and Joker method (CO_mass_joker) used in Schochet et al., and velocity semi-amplitude, eccentricity, and period values from the Joker (K_joker, e_joker, P_joker; Price-Whelan et al. 2017).

Programs

spectra_replotter.ipynb: This program replots spectra from the APOGEE servers when given a 2MASS ID, Field, and the telescope (APO/LCO) used for a specific observed object.  It will then print out an image of that object's spectra with the apVisit/asVisit files (pre-RV-shift reduction) plotted above the apStar/asStar files (post-RV-shift reduction) so that radial velocity shifts can be quickly identified by eye

Notes

estimated_companions.csv and apogee_objects_with_kiauhoku_masses.csv contain Fiber Dispersion in their data frames, as a reference to the observed trend that vscatter tends to be much lower for objects with 0 fiber dispersion, while objects with fiber dispersion > 0 show larger vscatters, in case there is future focus on investigating this phenomena 

Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is www.sdss4.org.

SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, Center for Astrophysics | Harvard & Smithsonian (CfA), the Chilean Participation Group, the French Participation Group, Instituto de Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU) / University of Tokyo, the Korean Participation Group, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatório Nacional / MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.

本Zenodo数据集包含与Schochet、Tayar及Andrews（2024）发表的论文《APOGEE中不存在质量间隙致密星双星系统》（*A Lack of Mass-Gap Compact Object Binaries in APOGEE*）相关的各类数据文件，该研究旨在识别可能拥有“质量间隙”黑洞/中子星伴星的单恒星成分双星系统。

本数据集使用了斯隆数字巡天第四期（Sloan Digital Sky Survey IV，Blanton et al. 2017）旗下的阿帕奇点银河演化实验（Apache Point Galactic Evolution Experiment，Majewski et al. 2017）第17次数据发布（Abdurro'uf et al. 2022）的数据，包括ASPCAP分析管道（Garcia Perez et al. 2016）得到的恒星丰度，以及经Doppler（Nidever et al. 2015）软件归约处理的光谱。本星表中使用的天体半径值来自盖亚+SED拟合分析（Yu et al. 2023）。

本仓库包含以下内容：

### 数据文件

1. APOGEE_likely_binaries.csv：该文件收录了本研究数据归约得到的4751个候选双星的基本信息与标识，包括2MASS编号、信噪比、观测次数、vsini、vscatter、有效温度、表面重力对数、金属丰度M/H及其对应误差（3项恒星参数的最终误差）。其中4288/4751个系统拥有Yu et al. 2023给出的半径值，我们额外提供了以下两个文件：
- apogee_objects_with_kiauhoku_masses.csv：该文件包含来自4套Kiauhoku演化网格（Claytor et al. 2020）的恒星质量与年龄参数，4套网格分别采用了MIST（MESA等时线与恒星轨道，Choi et al. 2016 & Paxton et al. 2010）、YREC（耶鲁旋转恒星演化代码，Tayar et al. 2022 & Pinsonneault et al. 1989）、Dart/DSEP（达特茅斯恒星演化程序，Dotter et al. 2008）以及GARSTEC/Gars（加兴恒星演化代码，Serenelli et al. 2013 & Weiss & Schlattl 2008）的恒星演化模型。该CSV文件的末列为上述质量与年龄参数，其余列则包含盖亚天体编号、APOGEE星标志与ASPCAP标志、每个目标的赤经/赤纬，以及APOGEE望远镜与观测场信息。
- estimated_companions.csv：该文件包含本研究中使用潮汐同步法（CO_mass_rsync）与Joker法（CO_mass_joker）得到的伴星最小质量估计值，以及来自Joker拟合方法的速度半振幅、偏心率与轨道周期参数（K_joker, e_joker, P_joker; Price-Whelan et al. 2017）。

### 分析程序

spectra_replotter.ipynb：该程序在输入2MASS编号、观测场信息以及对应观测所用望远镜（APO/LCO）时，可重新绘制APOGEE服务器存储的目标天体光谱。程序会将apVisit/asVisit文件（径向速度校正前的归约结果）与apStar/asStar文件（径向速度校正后的归约结果）上下并排绘制，以便研究者通过目视快速识别径向速度偏移。

### 备注

estimated_companions.csv与apogee_objects_with_kiauhoku_masses.csv的数据框中包含光纤色散（Fiber Dispersion）字段，作为观测趋势参考：光纤色散为0的天体的vscatter通常远低于光纤色散大于0的天体，后者的vscatter整体更大，该字段可供未来针对该现象开展相关研究时参考。

### 资助说明

斯隆数字巡天第四期的资助方包括阿尔弗雷德·P·斯隆基金会、美国能源部科学办公室，以及SDSS合作项目的各参与机构。SDSS感谢犹他大学高性能计算中心提供的支持与计算资源。SDSS官方网站为www.sdss4.org。

SDSS由天体物理研究联盟（Astrophysical Research Consortium）负责管理，其合作参与方包括：巴西参与小组、卡内基科学研究所、卡内基梅隆大学、哈佛与史密松天体物理中心（Center for Astrophysics | Harvard & Smithsonian, CfA）、智利参与小组、法国参与小组、加那利天体物理研究所、约翰·霍普金斯大学、东京大学Kavli物理与数学研究所（Kavli Institute for the Physics and Mathematics of the Universe, IPMU）、韩国参与小组、劳伦斯伯克利国家实验室、波茨坦莱布尼茨天体物理研究所（Leibniz Institut für Astrophysik Potsdam, AIP）、海德堡马克斯·普朗克天文研究所（Max-Planck-Institut für Astronomie, MPIA Heidelberg）、加兴马克斯·普朗克天体物理研究所（Max-Planck-Institut für Astrophysik, MPA Garching）、马克斯·普朗克地外物理研究所（Max-Planck-Institut für Extraterrestrische Physik, MPE）、中国国家天文台、新墨西哥州立大学、纽约大学、圣母大学、巴西国家天文台/MCTI、俄亥俄州立大学、宾夕法尼亚州立大学、上海天文台、英国参与小组、墨西哥国立自治大学、亚利桑那大学、科罗拉多大学博尔德分校、牛津大学、朴茨茅斯大学、犹他大学、弗吉尼亚大学、华盛顿大学、威斯康星大学、范德堡大学以及耶鲁大学。