论文标题
GAIA数据版本3：APSIS II-恒星参数
Gaia Data Release 3: Apsis II -- Stellar Parameters
论文作者
论文摘要
第三个GAIA数据释放包含超出天文学和光度法，从Gaia Prism Spectra（BP和RP）和光谱仪（RVS）中分散了数亿源的光。该数据发布为我们的星系中恒星的化学动力特性打开了一个新窗口，这是了解银河系的结构，形成和演变的基本知识。 To provide insight into the physical properties of Milky Way stars, we used these data to produce a uniformly-derived, all-sky catalog of stellar astrophysical parameters (APs): Teff, logg, [M/H], [$α$/Fe], activity index, emission lines, rotation, 13 chemical abundance estimates, radius, age, mass, bolometric luminosity, distance, and dust extinction.我们开发了APSIS管道来通过分析其天体，光度法，BP/RP和RVS光谱来推断Gaia对象的AP。我们对其他文献作品进行了验证，包括基准恒星，干涉法和星号学。在这里，我们从统计学上评估了APSIS的出色分析性能。我们描述了我们获得的数量，包括我们的结果的基本假设和局限性。我们提供指导，并确定我们的参数应和不应使用的制度。尽管有一些局限性，但这是迄今为止最广泛的恒星参数目录。这些包括Teff，Logg和[M/h]（使用BP/RP的4.7亿，600万使用RVS），半径（4.7亿），弥撒（1.4亿），年龄（1.2亿），化学丰度（500万），差异跨性别频带分析（1/200万），活动指数（200万），$ $ $ a}（$ $ $}（$ $}（$ $}（$）光谱类型（2.2亿）和排放线星（5万）。下一个GAIA数据发布计划，基于Epoch BP，RP和RV的更精确和详细的天体物理参数。
The third Gaia data release contains, beyond the astrometry and photometry, dispersed light for hundreds of millions of sources from the Gaia prism spectra (BP and RP) and the spectrograph (RVS). This data release opens a new window on the chemo-dynamical properties of stars in our Galaxy, essential knowledge for understanding the structure, formation, and evolution of the Milky Way. To provide insight into the physical properties of Milky Way stars, we used these data to produce a uniformly-derived, all-sky catalog of stellar astrophysical parameters (APs): Teff, logg, [M/H], [$α$/Fe], activity index, emission lines, rotation, 13 chemical abundance estimates, radius, age, mass, bolometric luminosity, distance, and dust extinction. We developed the Apsis pipeline to infer APs of Gaia objects by analyzing their astrometry, photometry, BP/RP, and RVS spectra. We validate our results against other literature works, including benchmark stars, interferometry, and asteroseismology. Here we assessed the stellar analysis performance from Apsis statistically. We describe the quantities we obtained, including our results' underlying assumptions and limitations. We provide guidance and identify regimes in which our parameters should and should not be used. Despite some limitations, this is the most extensive catalog of uniformly-inferred stellar parameters to date. These comprise Teff, logg, and [M/H] (470 million using BP/RP, 6 million using RVS), radius (470 million), mass (140 million), age (120 million), chemical abundances (5 million), diffuse interstellar band analysis (1/2 million), activity indices (2 million), H{$α$} equivalent widths (200 million), and further classification of spectral types (220 million) and emission-line stars (50 thousand). More precise and detailed astrophysical parameters based on epoch BP, RP, and RVS are planned for the next Gaia data release.
