solarFLAG野兔和猎犬：根据太阳-恒星日震学资料估算p-模式频率
solarFLAG hare and hounds: estimation of p-mode frequencies from Sun-as-star helioseismology data
摘要：
我们报告的结果，最新的solarFLAG野兔和猎犬练习，这是关注的测试方法，从太阳作为一个明星的观测收集的数据中提取的低度太阳p模式的频率。我们已经使用了新的solarFLAG模拟器，其中包括相关模式的激励和背景噪声的相关性的影响，使人工时间序列数据，模仿多普勒速度观测太阳作为一个明星。这种相关性导致了频率功率谱中模峰的不对称性。该小组的10名成员（猎犬）将他们的“峰值装袋”代码应用于3456天的数据集，并将估计的模式频率返回给兔子（WJC）进行比较。结果的分析表明，在约1.8兆赫以上的模式的估计频率的系统偏差。偏差是负的，这意味着估计的频率系统地低估了输入频率。我们确定了两个源，是占主导地位的贡献的频率偏置。这两种来源都涉及未能准确地模拟所拟合的频率功率谱的部分（窗口）中观测到的功率谱密度的细微方面。偏差的一个来源是未能考虑到来自所有那些频率位于拟合窗口之外的模式的功率谱密度。另一个来源是由于没有考虑到弱l=4和5模的功率谱密度，这在太阳作为恒星的分析中经常被忽略。太阳作为一颗星的峰值装袋码需要考虑到这两个来源，否则频率可能会有偏差。
英文摘要：
We report on the results of the latest solarFLAG hare-and-hounds exercise, which was concerned with testing methods for extraction of frequencies of low-degree solar p modes from data collected by Sun-as-a-star observations. We have used the new solarFLAG simulator, which includes the effects of correlated mode excitation and correlations with background noise, to make artificial timeseries data that mimic Doppler velocity observations of the Sun as a star. The correlations give rise to asymmetry of mode peaks in the frequency power spectrum. Ten members of the group (the hounds) applied their ``peak bagging'' codes to a 3456-day dataset, and the estimated mode frequencies were returned to the hare (who was WJC) for comparison. Analysis of the results reveals a systematic bias in the estimated frequencies of modes above approximately 1.8 mHz. The bias is negative, meaning the estimated frequencies systematically underestimate the input frequencies. We identify two sources that are the dominant contributions to the frequency bias. Both sources involve failure to model accurately subtle aspects of the observed power spectral density in the part (window) of the frequency power spectrum that is being fitted. One source of bias arises from a failure to account for the power spectral density coming from all those modes whose frequencies lie outside the fitting windows. The other source arises from a failure to account for the power spectral density of the weak l=4 and 5 modes, which are often ignored in Sun-as-a-star analysis. The Sun-as-a-star peak-bagging codes need to allow for both sources, otherwise the frequencies are likely to be biased.
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