Gaia Wide Binaries (5 kpc)

Gaia Wide Binaries Shariat, El-Badry, and Bhattacharjee (2026) Overview This page contains the catalog of resolved binaries from Gaia DR3 out to a distance of 5 kpc from the Sun. The catalog was constructed in a manner identical to El-Badry et al. (2021), but extended to a distance of 5 kpc (beyond the original 1 kpc). This adds an extra 500,000 binaries, leading to a total 1.75 million high-confidence binaries. This catalog was initially constructed for the paper "How precisely can we measure the ages of subgiant and giant stars?" by Cheyanne Shariat, Kareem El-Badry, and Soumyadeep Bhattacharjee; please cite both papers when using this catalog. The data files are: wide_binaries_5kpc.fits.gz: Table of the entire sample, where each row corresponds to one binary candidate (includes a large fraction of chance alignments). wide_binaries_5kpc_clean.fits.gz: Table of the cleaned sample; identical to above but contains only binaries that are likely bound (R_chance_align<0.1). ages_widebinaries.csv: Table of wide binaries with reported isochrone ages for both Giant stars in the binary (Table 1 of the paper). Contents For each star in the resolved binary, we provide:Gaia DR3 columns: - source_id - parallax - pmra, pmdec - ra, dec - bp_rp (color) - phot_g_mean_mag (G-band apparent magnitude) ->Data for the primary (brighter) and secondary (fainter) components are labeled with suffixes `1` and `2`, respectively. Derived quantities: - sep_AU: physical separation between binary components in astronomical units (au) - R_chance_align: chance alignment probability for the binary - binary_type: stellar type of stars in the binary. Each star can be Main-Sequence `MS`, White Dwarf `WD`, or unknown `??`, determined based on its Gaia color–magnitude diagram location Contact For any questions regarding the data or code, please email: [e-mail].# 盖亚（Gaia）宽双星数据集 Shariat、El-Badry与Bhattacharjee（2026） ## 概述 本页面收录源自盖亚DR3（Gaia DR3）、日心距离不超过5千秒差距（kpc）的已分辨双星星表。该星表的构建方法与El-Badry等人（2021）的研究完全一致，但将样本距离范围拓展至5千秒差距（远超原始的1千秒差距）。此举新增了50万个双星系统，使高置信度双星总数达到175万个。本星表最初是为Cheyanne Shariat、Kareem El-Badry以及Soumyadeep Bhattacharjee发表的论文《我们能以多高的精度测定亚巨星与巨星的年龄？》构建的；使用该星表时，请同时引用这两篇论文。 ### 数据文件 数据文件如下： 1. `wide_binaries_5kpc.fits.gz`：全样本数据表，每一行对应一个双星候选体（包含大量偶然成协的天体）。 2. `wide_binaries_5kpc_clean.fits.gz`：净化后样本数据表，与上述全样本表结构一致，但仅包含大概率为束缚态的双星系统（偶然成协概率`R_chance_align<0.1`）。 3. `ages_widebinaries.csv`：双星系统中两颗巨星均有等时线年龄（isochrone age）测定结果的宽双星数据表（对应论文中的表1）。 ## 数据内容 针对已分辨双星中的每一颗成员星，我们提供以下数据： ### 盖亚DR3原生列 - `source_id`：源标识 - `parallax`：视差 - `pmra`、`pmdec`：赤经方向自行、赤纬方向自行 - `ra`、`dec`：赤经、赤纬 - `bp_rp`（色指数）：bp-rp颜色指数 - `phot_g_mean_mag`（G星等）：G波段视星等 > 主星（更亮的成员）与伴星（更暗的成员）的数据分别以后缀`1`和`2`标注。 ### 衍生物理量 - `sep_AU`：双星成员间的物理间距，单位为天文单位（au） - `R_chance_align`：该双星系统的偶然成协概率 - `binary_type`：双星成员的恒星类型，根据盖亚色-光图位置判定，可为主序星（Main-Sequence，MS）、白矮星（White Dwarf，WD）或未知类型（??）。 ## 联系方式 若对数据或代码有任何疑问，请发送邮件至：`[e-mail]`。