juliensimon/gaia-dr3-spectroscopic-binaries

--- license: cc-by-4.0 pretty_name: "Gaia DR3 Spectroscopic Binary Stars" language: - en description: "Orbital solutions for 185,957 spectroscopic binary stars (SB1 + SB2) from ESA Gaia DR3, with periods, eccentricities, and radial velocity amplitudes." task_categories: - tabular-classification tags: - space - open-data - tabular-data - parquet - gaia - esa - binary-stars - spectroscopic - stellar - astronomy size_categories: - 100K<n<1M configs: - config_name: default data_files: - split: train path: data/gaia_dr3_spectroscopic_binaries.parquet default: true --- # Gaia DR3 Spectroscopic Binary Stars <div align="center"> <img src="banner.jpg" alt="A youthful globular star cluster observed by the Hubble Space Telescope" width="400"> <p><em>Credit: NASA/ESA/Hubble</em></p> </div> *Part of the [Astronomy Datasets](https://huggingface.co/collections/juliensimon/astronomy-datasets-69c24caf2f17e36128946743) collection on Hugging Face.* ![Updated](https://img.shields.io/badge/dynamic/json?url=https://raw.githubusercontent.com/juliensimon/space-datasets/main/status.json&query=$["gaia-sb"]&label=updated&color=brightgreen) Orbital solutions for **185,957** spectroscopic binary stars from the ESA Gaia Data Release 3 non-single stars (NSS) pipeline -- **181,327** single-lined (SB1) and **4,630** double-lined (SB2) systems with full Keplerian orbital parameters. ## Dataset description Spectroscopic binaries are star systems where the binary nature is revealed not by eclipses or visual separation, but by periodic Doppler shifts in the stellar spectral lines as the stars orbit their common center of mass. In a **single-lined spectroscopic binary (SB1)**, only one star's spectrum is visible -- the companion is too faint or its lines are blended -- and the radial velocity curve of the primary yields the orbital period, eccentricity, and the mass function f(m), which places a lower limit on the companion mass. In a **double-lined spectroscopic binary (SB2)**, both stars contribute detectable spectral lines, and the two radial velocity curves provide the mass ratio directly, constraining individual masses when combined with inclination estimates. The orbital elements in this catalog -- period, eccentricity, argument of periastron, velocity semi-amplitudes (K1, K2), and systemic velocity -- are the fundamental observables for binary star physics. They enable measurements of stellar masses (the single most important parameter governing stellar evolution), tests of tidal circularization theory (short-period binaries are expected to have circular orbits due to tidal dissipation), and identification of compact companions such as white dwarfs, neutron stars, and stellar-mass black holes lurking in otherwise unremarkable systems. Gaia's contribution is transformative. The Radial Velocity Spectrometer (RVS) aboard Gaia has obtained multi-epoch radial velocities for millions of stars brighter than about G ~ 12, and the non-single stars pipeline has fitted Keplerian orbits to those showing statistically significant radial velocity variability. The resulting catalog of over 185,957 spectroscopic binary orbits is an order of magnitude larger than any previous compilation -- the Ninth Catalogue of Spectroscopic Binary Orbits (SB9) contained fewer than 4,000 systems accumulated over a century of ground-based observations. This leap in sample size enables population-level studies of binary orbital properties (period distribution, eccentricity-period relation, mass-ratio distribution) across a wide range of spectral types, metallicities, and Galactic environments that were previously inaccessible. The period-eccentricity diagram of these systems traces the physics of tidal evolution: systems with periods below roughly 10 days are expected to have been circularized by tidal friction, while longer-period systems retain the eccentricity imprinted at formation. The transition between these regimes is a sensitive probe of stellar interior structure and the efficiency of dissipative processes. Similarly, the distribution of mass functions and mass ratios encodes the initial mass function of binary companions and the physics of binary star formation -- whether companions are drawn randomly from the IMF or preferentially paired with similar-mass primaries. ## Schema | Column | Type | Description | |--------|------|-------------| | `solution_id` | int | Solution id | | `source_id` | string | Gaia DR3 unique source identifier | | `ra_deg` | float64 | Right ascension ICRS (degrees) | | `dec_deg` | float64 | Declination ICRS (degrees) | | `period_days` | float64 | Orbital period (days) | | `period_days_err` | float64 | Period days err | | `t_periastron` | float64 | Time of periastron passage (BJD) | | `t_periastron_err` | float64 | T periastron err | | `ecc` | float64 | Orbital eccentricity | | `eccentricity_err` | float64 | Eccentricity err | | `center_of_mass_velocity` | float64 | Center-of-mass velocity (km/s) | | `center_of_mass_velocity_err` | float64 | Center of mass velocity err | | `semi_amplitude_k1` | float64 | Semi amplitude k1 | | `semi_amplitude_k1_err` | float64 | Semi amplitude k1 err | | `omega` | float64 | Omega | | `omega_err` | float64 | Omega err | | `nrvp` | int | Nrvp | | `ng_rvp` | int | Ng rvp | | `nrvs` | int | Nrvs | | `ng_rvs` | int | Ng rvs | | `bit_index` | int | Bit index for solution flags | | `corvec0` | float64 | Corvec0 | | `corvec1` | float64 | Corvec1 | | `corvec2` | float64 | Corvec2 | | `corvec3` | float64 | Corvec3 | | `corvec4` | float64 | Corvec4 | | `corvec5` | float64 | Corvec5 | | `corvec6` | float64 | Corvec6 | | `corvec7` | float64 | Corvec7 | | `corvec8` | float64 | Corvec8 | | `corvec9` | float64 | Corvec9 | | `corvec10` | float64 | Corvec10 | | `corvec11` | float64 | Corvec11 | | `corvec12` | float64 | Corvec12 | | `corvec13` | float64 | Corvec13 | | `corvec14` | float64 | Corvec14 | | `obj_func` | float64 | Objective function value | | `goodness` | float64 | Goodness | | `eff` | float64 | Eff | | `signi` | float64 | Signi | | `flags` | int | Flags | | `conf_persp` | float64 | Conf persp | | `solution_type` | string | NSS solution type (SB1 = single-lined, SB2 = double-lined) | ## Quick stats - **185,957** spectroscopic binary orbital solutions - **181,327** single-lined (SB1) systems - **4,630** double-lined (SB2) systems - Period range: **0.2500** to **1451.96** days (median 118.5825) - Median eccentricity: **0.193** (24,835 near-circular with e < 0.05) - **43** columns with orbital, photometric, and astrometric parameters ## Usage ```python from datasets import load_dataset ds = load_dataset("juliensimon/gaia-dr3-spectroscopic-binaries", split="train") df = ds.to_pandas() # SB1 vs SB2 breakdown print(df["solution_type"].value_counts()) # Period-eccentricity diagram (tidal circularization) import matplotlib.pyplot as plt period_col = [c for c in df.columns if "period" in c][0] ecc_col = [c for c in df.columns if "eccentric" in c or c == "ecc"][0] valid = df.dropna(subset=[period_col, ecc_col]) plt.scatter(valid[period_col], valid[ecc_col], s=0.3, alpha=0.3) plt.xscale("log") plt.xlabel("Period (days)") plt.ylabel("Eccentricity") plt.title("Gaia DR3 Spectroscopic Binaries: Period vs Eccentricity") plt.show() # High-eccentricity systems high_ecc = df[df[ecc_col] > 0.8] print(f"{len(high_ecc):,} systems with eccentricity > 0.8") ``` ## Data source Gaia Collaboration, Arenou, F. et al. (2023), *Gaia Data Release 3: stellar multiplicity, a teaser for the hidden treasure.* Astronomy & Astrophysics, 674, A34. European Space Agency, accessed via [VizieR](https://vizier.cds.unistra.fr/) CDS Strasbourg (I/357) and/or the [Gaia Archive](https://gea.esac.esa.int/archive/). ## Update schedule Static dataset -- uploaded once from Gaia DR3. Will be updated when Gaia DR4 is released. ## Related datasets - [wds-double-stars](https://huggingface.co/datasets/juliensimon/wds-double-stars) -- Washington Double Star Catalog - [gaia-dr3-eclipsing-binaries](https://huggingface.co/datasets/juliensimon/gaia-dr3-eclipsing-binaries) -- Gaia DR3 Eclipsing Binaries - [kepler-eclipsing-binaries](https://huggingface.co/datasets/juliensimon/kepler-eclipsing-binaries) -- Kepler Eclipsing Binary Catalog - [xray-binary-catalog](https://huggingface.co/datasets/juliensimon/xray-binary-catalog) -- X-ray Binary Catalog ## Pipeline Source code: [juliensimon/space-datasets](https://github.com/juliensimon/space-datasets) ## Support If you find this dataset useful, please give it a ❤️ on the [dataset page](https://huggingface.co/datasets/juliensimon/gaia-dr3-spectroscopic-binaries) and share feedback in the Community tab! Also consider giving a ⭐️ to the [space-datasets](https://github.com/juliensimon/space-datasets) repo. ## Citation ```bibtex @dataset{gaia_dr3_spectroscopic_binaries, author = {Simon, Julien}, title = {Gaia DR3 Spectroscopic Binary Stars}, year = {2026}, publisher = {Hugging Face}, url = {https://huggingface.co/datasets/juliensimon/gaia-dr3-spectroscopic-binaries}, note = {Based on Gaia DR3 (Arenou et al. 2023, A&A 674, A34) via VizieR CDS Strasbourg} } ``` ## License [CC-BY-4.0](https://creativecommons.org/licenses/by/4.0/)license: cc-by-4.0 pretty_name: "盖亚DR3分光双星" language: - en description: 收录来自欧洲空间局（European Space Agency, ESA）盖亚第三批数据发布（Gaia Data Release 3, Gaia DR3）的185957颗分光双星（单线型分光双星SB1 + 双线型分光双星SB2）的轨道解，包含轨道周期、偏心率以及视向速度半振幅。 task_categories: - tabular-classification tags: - space - open-data - tabular-data - parquet - gaia - esa - binary-stars - spectroscopic - stellar - astronomy size_categories: - 100K<n<1M configs: - config_name: default data_files: - split: train path: data/gaia_dr3_spectroscopic_binaries.parquet default: true --- # 盖亚DR3分光双星 <div align="center"> <img src="banner.jpg" alt="哈勃空间望远镜观测的年轻球状星团" width="400"> <p><em>致谢：NASA/ESA/哈勃</em></p> </div> *本数据集属于Hugging Face平台上的[天文学数据集合集](https://huggingface.co/collections/juliensimon/astronomy-datasets-69c24caf2f17e36128946743)。* ![Updated](https://img.shields.io/badge/dynamic/json?url=https://raw.githubusercontent.com/juliensimon/space-datasets/main/status.json&query=$["gaia-sb"]&label=更新状态&color=brightgreen) 本数据集收录来自欧洲空间局盖亚第三批数据发布非单星（non-single stars, NSS）处理管道的**185957颗**分光双星轨道解，其中包含**181327颗**单线型分光双星（single-lined spectroscopic binary, SB1）与**4630颗**双线型分光双星（double-lined spectroscopic binary, SB2），均带有完整的开普勒轨道参数。 ## 数据集说明 分光双星是指其双星特性并非通过食相或视觉分离显现，而是通过两颗恒星绕共同质心运动时，其光谱线产生的周期性多普勒频移得以揭示的恒星系统。在**单线型分光双星（SB1）**中，仅能观测到一颗恒星的光谱——伴星过于暗淡或其光谱线与主星发生了混叠——通过主星的视向速度曲线可得到轨道周期、偏心率以及质量函数f(m)，该函数可限定伴星质量的下限。在**双线型分光双星（SB2）**中，两颗恒星均可产生可被探测的光谱线，两条视向速度曲线可直接给出质量比，结合倾角估算结果即可约束单颗恒星的质量。 本星表中的轨道要素——轨道周期、偏心率、近心点幅角、视向速度半振幅（K1, K2）以及系统视向速度——是双星天体物理学研究的核心可观测量。借助这些参数，研究者可测算恒星质量（决定恒星演化的最关键参数）、验证潮汐圆化理论（由于潮汐耗散，短周期双星的轨道应趋近圆形），并识别隐藏在普通恒星系统中的致密伴星，如白矮星、中子星与恒星级黑洞。 盖亚卫星的贡献具有变革性意义。盖亚搭载的**视向速度光谱仪（Radial Velocity Spectrometer, RVS）**已为约G星等亮于12等的数百万颗恒星获取了多历元视向速度数据，而非单星处理管道则为那些表现出统计显著性视向速度变化的恒星拟合了开普勒轨道。最终得到的超过185957颗分光双星轨道星表，其规模比此前所有汇编成果大一个数量级——耗时一个多世纪的地面观测积累得到的第九届分光双星轨道星表（Ninth Catalogue of Spectroscopic Binary Orbits, SB9）仅收录了不到4000个系统。样本规模的这一飞跃使得研究者能够开展群体级别的双星轨道特性研究，包括不同光谱型、金属丰度与银河环境下的周期分布、偏心率-周期关系、质量比分布等此前无法实现的研究方向。 这些系统的周期-偏心率分布图可揭示潮汐演化的物理机制：轨道周期短于约10天的系统应已通过潮汐摩擦实现轨道圆化，而长周期系统则保留了形成时的偏心率特征。这两种状态的过渡区间是研究恒星内部结构与耗散过程效率的灵敏探针。同样，质量函数与质量比的分布也蕴含了双星伴星初始质量函数以及双星形成机制的信息，例如伴星是否从初始质量函数（IMF）中随机选取，还是倾向于与质量相近的主星配对。 ## 数据模式 | 列名 | 数据类型 | 说明 | |--------|------|-------------| | `solution_id` | int | 解编号 | | `source_id` | string | 盖亚DR3唯一源标识符 | | `ra_deg` | float64 | 赤经（国际天球参考系ICRS，单位：度） | | `dec_deg` | float64 | 赤纬（国际天球参考系ICRS，单位：度） | | `period_days` | float64 | 轨道周期（单位：天） | | `period_days_err` | float64 | 周期误差（单位：天） | | `t_periastron` | float64 | 近心点通过时刻（伯尔尼儒略日BJD） | | `t_periastron_err` | float64 | 近心点时刻误差 | | `ecc` | float64 | 轨道偏心率 | | `eccentricity_err` | float64 | 偏心率误差 | | `center_of_mass_velocity` | float64 | 质心视向速度（单位：km/s） | | `center_of_mass_velocity_err` | float64 | 质心视向速度误差 | | `semi_amplitude_k1` | float64 | K1视向速度半振幅 | | `semi_amplitude_k1_err` | float64 | K1视向速度半振幅误差 | | `omega` | float64 | 近心点幅角 | | `omega_err` | float64 | 近心点幅角误差 | | `nrvp` | int | 视向速度光谱仪观测历元数 | | `ng_rvp` | int | RVS观测有效点数 | | `nrvs` | int | 视向速度测量次数 | | `ng_rvs` | int | 视向速度测量有效点数 | | `bit_index` | int | 解标志位索引 | | `corvec0` | float64 | 校正向量0 | | `corvec1` | float64 | 校正向量1 | | `corvec2` | float64 | 校正向量2 | | `corvec3` | float64 | 校正向量3 | | `corvec4` | float64 | 校正向量4 | | `corvec5` | float64 | 校正向量5 | | `corvec6` | float64 | 校正向量6 | | `corvec7` | float64 | 校正向量7 | | `corvec8` | float64 | 校正向量8 | | `corvec9` | float64 | 校正向量9 | | `corvec10` | float64 | 校正向量10 | | `corvec11` | float64 | 校正向量11 | | `corvec12` | float64 | 校正向量12 | | `corvec13` | float64 | 校正向量13 | | `corvec14` | float64 | 校正向量14 | | `obj_func` | float64 | 目标函数值 | | `goodness` | float64 | 拟合优度 | | `eff` | float64 | 效率参数 | | `signi` | float64 | 显著性水平 | | `flags` | int | 解标志位 | | `conf_persp` | float64 | 置信透视参数 | | `solution_type` | string | 非单星解类型（SB1=单线型分光双星，SB2=双线型分光双星） | ## 快速统计 - **185,957** 条分光双星轨道解 - **181,327** 颗单线型分光双星（SB1）系统 - **4,630** 颗双线型分光双星（SB2）系统 - 周期范围：**0.2500** 至 **1451.96** 天（中位数 118.5825 天） - 偏心率中位数：**0.193**（其中24,835颗为近圆轨道，偏心率e < 0.05） - 包含43个轨道、测光与天体测量参数列 ## 使用方法 python from datasets import load_dataset ds = load_dataset("juliensimon/gaia-dr3-spectroscopic-binaries", split="train") df = ds.to_pandas() # SB1与SB2系统分布统计 print(df["solution_type"].value_counts()) # 周期-偏心率分布图（潮汐圆化效应） import matplotlib.pyplot as plt period_col = [c for c in df.columns if "period" in c][0] ecc_col = [c for c in df.columns if "eccentric" in c or c == "ecc"][0] valid = df.dropna(subset=[period_col, ecc_col]) plt.scatter(valid[period_col], valid[ecc_col], s=0.3, alpha=0.3) plt.xscale("log") plt.xlabel("轨道周期（天）") plt.ylabel("轨道偏心率") plt.title("盖亚DR3分光双星：周期与偏心率关系") plt.show() # 高偏心率系统筛选 high_ecc = df[df[ecc_col] > 0.8] print(f"共找到 {len(high_ecc):,} 颗偏心率大于0.8的系统") ## 数据源 盖亚合作团队，Arenou, F. 等人（2023），*《盖亚第三批数据发布：恒星多重性，隐藏的宝藏初探》*，《天文学与天体物理学》，674卷，A34。欧洲空间局发布，通过斯特拉斯堡CDS的[VizieR](https://vizier.cds.unistra.fr/)天文台（目录编号I/357）和/或[盖亚数据档案馆](https://gea.esac.esa.int/archive/)获取。 ## 更新计划 本数据集为静态数据集，仅从盖亚DR3上传一次，将在盖亚DR4发布时进行更新。 ## 相关数据集 - [wds-double-stars](https://huggingface.co/datasets/juliensimon/wds-double-stars) —— 华盛顿双星星表 - [gaia-dr3-eclipsing-binaries](https://huggingface.co/datasets/juliensimon/gaia-dr3-eclipsing-binaries) —— 盖亚DR3食双星数据集 - [kepler-eclipsing-binaries](https://huggingface.co/datasets/juliensimon/kepler-eclipsing-binaries) —— 开普勒食双星星表 - [xray-binary-catalog](https://huggingface.co/datasets/juliensimon/xray-binary-catalog) —— X射线双星数据集 ## 数据处理管道 源代码：[juliensimon/space-datasets](https://github.com/juliensimon/space-datasets) ## 支持与反馈 如果您认为本数据集对您的研究有帮助，请前往[数据集页面](https://huggingface.co/datasets/juliensimon/gaia-dr3-spectroscopic-binaries)点赞❤️，并在社区标签页分享您的反馈！同时欢迎为[space-datasets](https://github.com/juliensimon/space-datasets)仓库点亮⭐️。 ## 引用格式 bibtex @dataset{gaia_dr3_spectroscopic_binaries, author = {Simon, Julien}, title = {Gaia DR3 Spectroscopic Binary Stars}, year = {2026}, publisher = {Hugging Face}, url = {https://huggingface.co/datasets/juliensimon/gaia-dr3-spectroscopic-binaries}, note = {基于盖亚DR3数据（Arenou等人2023，A&A 674，A34），通过斯特拉斯堡CDS的VizieR获取} } ## 许可证 [CC-BY-4.0](https://creativecommons.org/licenses/by/4.0/)