Abstract :
[en] Given their tendency to mix in with real pulsations, the reflection of super-Nyquist frequencies (SNFs) pose a threat to asteroseismic properties. Although SNFs have been studied in several pulsating stars, a systematic survey remains to be explored. Here, we propose a method for identifying SNFs from Kepler and TESS photometry by characterizing their periodic frequency modulations using a sliding Fourier transform. After analyzing long-cadence photometry in the Kepler legacy, we identified 304 SNFs in 56 stars from 45 607 frequencies in ∼600 γ Doradus stars, corresponding to a fraction of approximately 0.67% and 9.2%, respectively. Most SNFs were detected in the frequency range of pressure mode over 120 μHz and the fraction of SNF detection increases as frequency up to ∼7%. We found only two potential SNFs mixed with gravity modes in two γ Doradus stars. These findings indicate that SNFs have a negligible impact on global seismic properties, such as those derived from period spacing in γ Doradus stars. However, we stress that SNFs must be carefully and systematically examined by this method in other pulsating stars, particularly δ Scuti and hot B subdwarf stars, to establish a solid foundation for the precise asteroseismolgy of various types of pulsators.
Funding text :
The authors acknowledge the support from the National Natural Science Foundation of China (NSFC) through grant Nos. 12273002, 12090040 and 12090042. This work is supported by the International Centre of Supernovae at Yunnan Key Laboratory (Nos. 202302AN360001 and 202302AN36000102) and the science research grants from the China Manned Space Project. S.C. has financial support from the Centre National d'Etudes Spatiales (CNES, France). T.W. acknowledges the support from the National Key Research and Development Program of China (grant No. 2021YFA1600402), the B-type Strategic Priority Program of the Chinese Academy of Sciences (grant No. XDB41000000), and the Yunnan Ten Thousand Talents Plan Young & Elite Talents Project. All of the Kepler and TESS data used in this paper can be found in MAST. The authors appreciate all who have contributed to making these missions possible. Funding for the Kepler and TESS mission is provided by NASA's Science Mission Directorate.The authors acknowledge the support from the National Natural Science Foundation of China (NSFC) through grant Nos. 12273002, 12090040 and 12090042. This work is supported by the International Centre of Supernovae at Yunnan Key Laboratory (Nos. 202302AN360001 and 202302AN36000102) and the science research grants from the China Manned Space Project. S.C. has financial support from the Centre National d\u2019Etudes Spatiales (CNES, France). T.W. acknowledges the support from the National Key Research and Development Program of China (grant No. 2021YFA1600402), the B-type Strategic Priority Program of the Chinese Academy of Sciences (grant No. XDB41000000), and the Yunnan Ten Thousand Talents Plan Young & Elite Talents Project. All of the Kepler and TESS data used in this paper can be found in MAST. The authors appreciate all who have contributed to making these missions possible. Funding for the Kepler and TESS mission is provided by NASA\u2019s Science Mission Directorate.
Scopus citations®
without self-citations
0
