A detection threshold in the amplitude spectra calculated from Kepler data obtained during K2 mission
A detection threshold in the amplitude spectra calculated from Kepler data obtained during K2 mission
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DOI：
10.1093/mnrasl/slu194
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发表时间：
2014-12
影响因子：
4.8
通讯作者：
A. Baran;C. Koen;B. Pokrzywka
中科院分区：
文献类型：
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作者：
A. Baran;C. Koen;B. Pokrzywka
我们提出了我们的模拟数据的分析，以推导出一个检测阈值，可用于预白化过程中的振幅谱。在脉动星的地面数据的情况下，这个阈值通常被认为是振幅谱中平均噪声水平的四倍。在分析天基数据时，这一阈值值得怀疑。我们的努力的目的是在连续90天的开普勒K2相位观测的情况下修改这个阈值。我们的结果清楚地表明，一个95%的置信水平，常见的地面观测，可以达到平均噪声水平的5.4倍，是覆盖依赖。此外，如果节奏的数量改变，则该阈值在4.8和5.7之间变化。这一结论应确保进一步的预白化，并有助于避免过度解释开普勒航天器在K2阶段观测到的脉动星的光谱。我们将我们的结果与文献中广泛使用的标准方法进行比较。
We present our analysis of simulated data in order to derive a detection threshold which can be used in the pre-whitening process of amplitude spectra. In case of ground-based data of pulsating stars, this threshold is conventionally taken to be four times the mean noise level in an amplitude spectrum. This threshold is questionable when space-based data are analyzed. Our effort is aimed at revising this threshold in the case of continuous 90-day Kepler K2 phase observations. Our result clearly shows that a 95% confidence level, common for ground observations, can be reached at 5.4 times the mean noise level and is coverage dependent. In addition, this threshold varies between 4.8 and 5.7, if the number of cadences is changed. This conclusion should secure further pre-whitening and helps to avoid over-interpretation of spectra of pulsating stars observed with the Kepler spacecraft during K2 phase. We compare our results with the standard approach widely used in the literature.