Gaia Data Release 3 Analysis of the Gaia BP/RP spectra using the General Stellar Parameterizer from Photometry
Gaia Data Release 3 Analysis of the Gaia BP/RP spectra using the General Stellar Parameterizer from Photometry
复制标题
盖亚数据版本 3 使用光度学的通用恒星参数化器分析盖亚 BP/RP 光谱
DOI：
10.1051/0004-6361/202243462
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发表时间：
2023
影响因子：
6.5
通讯作者：
Andrae R
中科院分区：
文献类型：
--
作者：
Andrae R
背景来源的天体物理特征是第三次GaiaData发布(DR3)中的主要新数据产品之一。特别是，从低分辨率BP/RP光谱估计的4.71亿个源的恒星参数。目的我们介绍了来自光度学的通用恒星参数化器(GSP-PHOT)，它是天体物理参数推断系统(APIS)的一部分。GSP-PHOT旨在根据天体测量、光度学和低分辨率BP/RP光谱，为数亿颗单一的不变星制作一个均匀的参数目录。这些参数是每颗恒星的有效温度、表面重力、金属丰度、绝对MG星等、半径、距离和消光。方法GSP-PHOT使用贝叶斯正演方法来同时拟合BP/RP光谱、视差和明显的G星等。GSP-PHOT的一个主要设计特点是利用BP/RP光谱的视通量水平，结合等时模型推导出对半径和距离的严格观测约束。我们通过利用相同来源的重复GAIA观测数据仔细地验证了不确定度估计。结果数据发布包括具有g<； 19的4.71亿个来源的GSP-PHOT结果。与文献值的典型差异是T为110K，LOG为0.2-0.25，但这些差异强烈依赖于数据质量。特别是，对于视差测量良好的恒星(ϖ/σϖ>； 20)，GSP-PHOT的结果要好得多，大部分在2kpc以内。与文献值相比，金属丰度估算显示出很大的偏差，并且仅在定性水平上有用。然而，我们提供了我们的金属丰度估计的经验校准，在很大程度上消除了这些偏差。消光系数A0和ABP与参考值0.07-0.09毫克显示出典型的差异。95%的源也提供了MCMC参数样本。结论GSP-PHOT提供了一个均匀的恒星参数、距离和消光星表，可用于各种目的，如样本选择(OB星、红巨星、太阳类似物等)。在小行星地震学或地面干涉测量的背景下，目标通常是明亮的，具有良好的视差测量，GSP-PHOT结果对于组合分析或目标选择特别有用。
ContextThe astrophysical characterisation of sources is among the major new data products in the thirdGaiaData Release (DR3). In particular, there are stellar parameters for 471 million sources estimated from low-resolution BP/RP spectra.AimsWe present the General Stellar Parameterizer from Photometry (GSP-Phot), which is part of the astrophysical parameters inference system (Apsis). GSP-Phot is designed to produce a homogeneous catalogue of parameters for hundreds of millions of single non-variable stars based on their astrometry, photometry, and low-resolution BP/RP spectra. These parameters are effective temperature, surface gravity, metallicity, absoluteMGmagnitude, radius, distance, and extinction for each star.MethodsGSP-Phot uses a Bayesian forward-modelling approach to simultaneously fit the BP/RP spectrum, parallax, and apparentGmagnitude. A major design feature of GSP-Phot is the use of the apparent flux levels of BP/RP spectra to derive, in combination with isochrone models, tight observational constraints on radii and distances. We carefully validate the uncertainty estimates by exploiting repeatGaiaobservations of the same source.ResultsThe data release includes GSP-Phot results for 471 million sources withG< 19. Typical differences to literature values are 110 K forTeffand 0.2–0.25 for logg, but these depend strongly on data quality. In particular, GSP-Phot results are significantly better for stars with good parallax measurements (ϖ/σϖ> 20), mostly within 2 kpc. Metallicity estimates exhibit substantial biases compared to literature values and are only useful at a qualitative level. However, we provide an empirical calibration of our metallicity estimates that largely removes these biases. ExtinctionsA0andABPshow typical differences from reference values of 0.07–0.09 mag. MCMC samples of the parameters are also available for 95% of the sources.ConclusionsGSP-Phot provides a homogeneous catalogue of stellar parameters, distances, and extinctions that can be used for various purposes, such as sample selections (OB stars, red giants, solar analogues etc.). In the context of asteroseismology or ground-based interferometry, where targets are usually bright and have good parallax measurements, GSP-Phot results should be particularly useful for combined analysis or target selection.