TESS first look at evolved compact pulsators Known ZZ Ceti stars of the southern ecliptic hemisphere as seen by TESS
TESS first look at evolved compact pulsators Known ZZ Ceti stars of the southern ecliptic hemisphere as seen by TESS
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TESS 首次观察演化后的紧凑型脉动星 TESS 所见的南黄道半球已知的 ZZ 鲸鱼座恒星
DOI：
10.1051/0004-6361/202037470
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发表时间：
2020
影响因子：
6.5
通讯作者：
Zong W.
中科院分区：
文献类型：
--
作者：
Bognar Zs;Kawaler S. D.;Bell K. J.;Schr;t C.;Baran A. S.;Bradley P. A.;Hermes J. J.;Charpinet S.;H;ler G.;Mullally S. E.;Murphy S. J.;Raddi R.;Sodor A.;Tremblay P-E;Uzundag M.;Zong W.
语境。我们展示了在对南黄道半球进行巡天观测期间，TESS 太空望远镜以 120 秒节奏模式观测到的 18 颗先前已知的 ZZ 鲸鱼座恒星的发现。目标。我们重点关注天基观测的频率分析，将结果与之前的地面测量结果进行比较。 TESS 观测检测到的频率可以作为未来星震分析的输入。方法。我们对数据集进行了标准的预白化，以得出不同目标的可能脉动频率。在某些情况下，我们将洛伦兹拟合到由于 TESS 观测期间发生的短期幅度或相位变化而出现的频率组。结果。我们通过TESS以120秒的节奏观测到了7颗ZZ鲸鱼座星中的40多个脉动频率，精度优于0.1μHz。我们发现HE 0532-5605可能是一个新爆发的ZZ Ceti。由于其固有的模糊性和/或大 TESS 像素上的拥挤，十个目标在其傅立叶变换中没有显示任何显着的脉动频率。在某些情况下，我们还在 TESS 观测期间检测到了可能的幅度或相位变化。这些目标的这种行为之前并未通过地面观测发现。
Context. We present our findings on 18 previously known ZZ Ceti stars observed by the TESS space telescope in 120 s cadence mode during the survey observation of the southern ecliptic hemisphere. Aims. We focus on the frequency analysis of the space-based observations, comparing the results with findings of previous ground-based measurements. The frequencies detected by the TESS observations can serve as inputs for future asteroseismic analyses. Methods. We performed standard pre-whitening of the data sets to derive the possible pulsation frequencies of the different targets. In some cases, we fit Lorentzians to the frequency groups that emerged as the result of short-term amplitude or phase variations that occurred during the TESS observations. Results. We detected more than 40 pulsation frequencies in seven ZZ Ceti stars observed in the 120 s cadence by TESS, with precision better than 0.1 mu Hz. We found that HE 0532-5605 may be a new outbursting ZZ Ceti. Ten targets do not show any significant pulsation frequencies in their Fourier transforms, due to a combination of their intrinsic faintness and/or crowding on the large TESS pixels. We also detected possible amplitude or phase variations during the TESS observations in some cases. Such behaviour in these targets was not previously identified from ground-based observations.