Comprehensive comparison between APOGEE and LAMOST
Comprehensive comparison between APOGEE and LAMOST
复制标题
DOI：
10.1051/0004-6361/201833387
复制
发表时间：
2018-07
影响因子：
6.5
通讯作者：
B. Anguiano;S. Majewski;C. Allende-Prieto;Szabolcs Mészáros;H. Jönsson;D. A. Garc'ia-Hern'andez;
中科院分区：
文献类型：
--
作者：
B. Anguiano;S. Majewski;C. Allende-Prieto;Szabolcs Mészáros;H. Jönsson;D. A. Garc'ia-Hern'andez;
上下文在大规模光谱测量的时代，自动化的恒星参数管道及其验证对于光谱的有效科学利用至关重要。目标。我们进行一个关键的和全面的比较的径向速度和主要的恒星大气参数之间的最新数据发布的阿帕奇点天文台星系演化实验（APOGEE）和大天区多目标光谱望远镜（LAMOST）的调查。方法. APOGEE是一个高分辨率（R = 22 500）光谱测量，具有高信噪比，是斯隆数字巡天（SDSS）的一部分。最新发布的SDSS DR 14数据包括263444颗恒星的APOGEE光谱，以及主要恒星参数和多达20种化学物质的个体丰度。LAMOST是一种低分辨率（R = 1800）的光学光谱测量，也在北方半球，其中4000光纤可以同时分配。LAMOST DR 3包含3177995颗恒星。结果在APOGEE DR 14- LAMOST DR 3星表中共有42420颗矮星和巨星。APOGEE和LAMOST返回式飞行器之间的比较显示出4.54 ± 0.03 km s-1的明显偏移，5.8 km s-1的色散，在这个意义上，APOGEE径向速度更高。我们观察到一个小的偏移约13 K的有效温度，与分散的155 K。还观察到约0.06 dex的[Fe/H]的小偏移以及0.13 dex的散射。我们注意到，两次测量之间的最大偏移发生在表面重力上。仅使用APOGEE DR 14中校准的红巨星的表面重力，其中有24 074颗恒星是共同的，发现0.14 dex的偏差与大量的散射（0.25 dex）。在APOGEE DR 14和LAMOST中有17482颗红巨星是共同的，它们通过称为Cannon的代码与APOGEE DR 12联系在一起。这两个数据集之间一般都很一致。然而，我们发现恒星参数的差异取决于有效温度。令人惊讶的是，我们发现Teff的内部APOGEE DR 14-DR 12差异与DR 14- LAMOST中与DR 12相关的差异之间没有相关性，因为LAMOST已经被校准到APOGEE DR 12。我们发现[Fe/H]差异之间没有相关性，这表明LAMOST/Cannon与APOGEE DR 12恒星参数尺度没有很好的耦合。本文报道了APOGEE DR 12和DR 14恒星参数之间的[Fe/H]依赖关系。我们发现一个弱的相关性之间的差异APOGEE DR 14-DR 12和LAMOST的DR 12表面重力的恒星热超过4800 K，在2.0和2.8 dex之间的log g范围。我们没有观察到[Fe/H]依赖于重力差异。
Context. In the era of massive spectroscopy surveys, automated stellar parameter pipelines and their validation are extremely important for an efficient scientific exploitation of the spectra. Aims. We undertake a critical and comprehensive comparison of the radial velocities and the main stellar atmosphere parameters for stars in common between the latest data releases from the Apache Point Observatory Galaxy Evolution Experiment (APOGEE) and the Large sky Area Multi-Object Spectroscopic Telescope (LAMOST) surveys. Methods. APOGEE is a high-resolution (R = 22 500) spectroscopic survey with high signal-to-noise ratio that is part of the Sloan Digital Sky Survey (SDSS). The latest data release, SDSS DR14, comprises APOGEE spectra for 263 444 stars, together with main stellar parameters and individual abundances for up to 20 chemical species. LAMOST is a low-resolution (R = 1800) optical spectroscopic survey also in the Northern Hemisphere, where 4000 fibers can be allocated simultaneously. LAMOST DR3 contains 3 177 995 stars. Results. A total of 42 420 dwarfs and giants stars are in common between the APOGEE DR14 – LAMOST DR3 stellar catalogs. A comparison between APOGEE and LAMOST RVs shows a clear offset of 4.54 ± 0.03 km s−1, with a dispersion of 5.8 km s−1, in the sense that APOGEE radial velocities are higher. We observe a small offset in the effective temperatures of about 13 K, with a scatter of 155 K. A small offset in [Fe/H] of about 0.06 dex together with a scatter of 0.13 dex is also observed. We note that the largest offset between the surveys occurs in the surface gravities. Using only surface gravities in calibrated red giants from APOGEE DR14, with which there are 24 074 stars in common, a deviation of 0.14 dex is found with substantial scatter (0.25 dex). There are 17 482 red giant stars in common between APOGEE DR14 and those in LAMOST tied to APOGEE DR12 via the code called the Cannon. There is generally good agreement between the two data-sets. However, we find that the differences in the stellar parameters depend on effective temperature. For metal-rich stars, a different trend for the [Fe/H] discrepancies is found. Surprisingly, we see no correlation between the internal APOGEE DR14 – DR12 differences in Teff and those in DR14 – LAMOST tied to DR12, where a correlation should be expected since LAMOST has been calibrated to APOGEE DR12. We find no correlation either between the [Fe/H] discrepancies, suggesting that LAMOST/Cannon is not well coupled to the APOGEE DR12 stellar parameter scale. An [Fe/H] dependence between the stellar parameters in APOGEE DR12 and those in DR14 is reported. We find a weak correlation in the differences between APOGEE DR14 – DR12 and LAMOST on DR12 surface gravity for stars hotter than 4800 K and in the log g range between 2.0 and 2.8 dex. We do not observe an [Fe/H] dependency in the gravity discrepancies.