LEMONY – a library of empirical medium-resolution spectra by observations with the NAOC Xinglong 2.16-m and YNAO Gaomeigu 2.4-m telescopes
LEMONY – a library of empirical medium-resolution spectra by observations with the NAOC Xinglong 2.16-m and YNAO Gaomeigu 2.4-m telescopes
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LEMONY — 使用 NAOC 兴隆 2.16 米和 YNAO 高美谷 2.4 米望远镜观测的经验中分辨率光谱库
DOI：
10.1093/mnras/sty2069
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发表时间：
2018-08
影响因子：
4.8
通讯作者：
Y L Shao
中科院分区：
文献类型：
--
作者：
C Wang;X W Liu;Y Huang;M S Xiang;J J Ren;H B Yuan;B Q Chen;Z J Tian;J M Bai;N C Sun;F Zuo;H W Zhang;Y W Zhang;Z Fan;A L Luo;J R Shi;J Li;Y L Shao
在本研究中，我们扩大了MILES模板星在参数空间中分布的覆盖范围并提高了分布的均匀性，并将模板光谱的波长覆盖范围扩展到了Can三重态之外的远红光。为了实现这一目标，我们使用两台长缝光谱仪开展了一项重大观测活动：安装在中国国家天文台（NAOC）2.16米望远镜上的OMR和安装在云南天文台（YNAO）2.4米望远镜上的云南微弱天体光谱仪和相机（YFOSC）。原始样本基于MILES库，辅以从PASTEL数据库中选取的918颗星。总共收集并缩减了 822 个 OMR 和 1324 个 YFOSC 光谱，分别覆盖波长范围 lambda lambda 3800-5180 和 lambda lambda 5150-9000。光谱的平均分辨率半高宽约为 3.3 埃，并且经过波长和通量校准，精度分别约为 20 km s(-1) 和 5%。通过与理论光谱的互相关，进一步将波长校准中的系统误差校正到接近 4 km s(-1) 的精度。几乎所有光谱的平均信噪比均优于每像素 100。结合 MILES 光谱，目前光谱覆盖 lambda 3800-5180、lambda 3800-7500、lambda 5150-9000 和 lambda 3800-9000 的恒星分别为 1731、1542、1324 和 1273 颗。在本文中，我们描述了我们的模板星选择、观测和数据缩减，并展示了迄今为止收集的缩减光谱。
In this study, we expand the coverage and improve the homogeneity of the distribution of MILES template stars in the parameter space, as well as extend the wavelength coverage of the template spectra to the far red beyond the Can triplet. To achieve this, we have carried out a major observational campaign using two long-slit spectrographs: the OMR mounted on the National Astronomy Observatory of China (NAOC) 2.16-m telescope and the Yunnan Faint Object Spectrograph and Camera (YFOSC) mounted on the Yunnan Astronomical Observatory (YNAO) 2.4-m telescope. The original sample is based on the MILES library, supplemented by 918 stars selected from the PASTEL data base. In total, 822 OMR and 1324 YFOSC spectra have been collected and reduced, covering the wavelength ranges lambda lambda 3800-5180 and lambda lambda 5150-9000, respectively. The spectra have a mean resolution full width at halfmaximum of similar to 3.3 angstrom and are wavelength- and flux-calibrated to an accuracy of similar to 20 km s(-1) and similar to 5 per cent, respectively. The spectra are further corrected for systematic errors in the wavelength calibration to an accuracy of similar to 4 km s(-1) by cross-correlating with the theoretical spectra. Almost all the spectra have an average signal-to-noise ratio better than 100 per pixel. Combined with the MILES spectra, there are now 1731, 1542, 1324 and 1273 stars with spectra covering lambda lambda 3800-5180, lambda lambda 3800-7500, lambda lambda 5150-9000 and lambda lambda 3800-9000, respectively. In this paper, we describe our template star selection, the observation and data reduction, and we present the reduced spectra collected hitherto.
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影响因子：
4.8
作者：
Huang Y;Liu X W;Yuan H B;Xiang M S;Chen B Q;Zhang H W
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发表时间：
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影响因子：
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作者：
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影响因子：
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10.1111/j.1365-2966.2006.10699.x
发表时间：
2006-07
影响因子：
4.8
作者：
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通讯作者：
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