Oscillation mode frequencies of 61 main-sequence and subgiant stars observed by Kepler
Oscillation mode frequencies of 61 main-sequence and subgiant stars observed by Kepler
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DOI：
10.1051/0004-6361/201218948
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发表时间：
2012-04
影响因子：
6.5
通讯作者：
T. Appourchaux;W. Chaplin;R. García;M. Gruberbauer;G. Verner;H. M. Antia;O. Benomar;T. Campante;G. Davies;S. Deheuvels;R. Handberg;S. Hekker;R. Howe;C. R'egulo;D. Salabert;T. Bedding;T. White;J. Ballot;S. Mathur;V. S. Aguirre;Y. Elsworth;S. Basu;R. Gilliland;J. Christensen-Dalsgaard;H. Kjeldsen;K. Uddin;Martin C. Stumpe;T. Barclay
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文献类型：
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作者：
T. Appourchaux;W. Chaplin;R. García;M. Gruberbauer;G. Verner;H. M. Antia;O. Benomar;T. Campante;G. Davies;S. Deheuvels;R. Handberg;S. Hekker;R. Howe;C. R'egulo;D. Salabert;T. Bedding;T. White;J. Ballot;S. Mathur;V. S. Aguirre;Y. Elsworth;S. Basu;R. Gilliland;J. Christensen-Dalsgaard;H. Kjeldsen;K. Uddin;Martin C. Stumpe;T. Barclay
上下文。开普勒和CoRoT在几颗太阳型恒星上观测到了类似太阳的振荡，从而为利用星震学目标探测恒星提供了一种方法。我们提供了各种恒星振荡的模态频率，以便与恒星建模得到的模态频率进行比较。方法。我们对每颗恒星使用了9个月的时间序列数据。观测到的61颗恒星被分为三组：单星、类f星和混合星。简单星群包括那些模态度识别明显的恒星。类f星群包括星度难以确定的恒星。混合模群包括模态不遵循低频渐近关系的演化恒星。根据这一分类，61颗主序星和次巨星的功率谱使用最大似然估计器和贝叶斯估计器进行了分析，提供了单个模态特征，如频率、线宽和模态高度。我们开发并描述了一种方法，用于从由不同方法和单个科学家导出的多组中提取单一组模态频率。我们报告了如何使用似然比检验和后验概率来评估拟合参数的质量。结果。我们给出了61颗恒星的模态频率（带有它们的1 σ误差条），以及它们相关的梯形图。
Context. Solar-like oscillations have been observed by Kepler and CoRoT in several solar-type stars, thereby providing a way to probe the stars using asteroseismology Aims. We provide the mode frequencies of the oscillations of various stars required to perform a comparison with those obtained from stellar modelling. Methods. We used a time series of nine months of data for each star. The 61 stars observed were categorised in three groups: simple, F-like, and mixed-mode. The simple group includes stars for which the identification of the mode degree is obvious. The F-like group includes stars for which the identification of the degree is ambiguous. The mixed-mode group includes evolved stars for which the modes do not follow the asymptotic relation of low-degree frequencies. Following this categorisation, the power spectra of the 61 main-sequence and subgiant stars were analysed using both maximum likelihood estimators and Bayesian estimators, providing individual mode characteristics such as frequencies, linewidths, and mode heights. We developed and describe a methodology for extracting a single set of mode frequencies from multiple sets derived by different methods and individual scientists. We report on how one can assess the quality of the fitted parameters using the likelihood ratio test and the posterior probabilities. Results. We provide the mode frequencies of 61 stars (with their 1-σ error bars), as well as their associated echelle diagrams.