Physical Properties of KIC 9851944: Conclusion, Data Availability, Acknowledgments, and References

Table of Links

• Abstract and Intro
• Observation
• Orbital Ephemeris
• Radial Velocity Analysis
• Spectral Analysis
• Analysis of the Light Curve
• Physical Properties
• Asteroseismic Analysis
• Discussion
• Conclusion, Data Availability, Acknowledgments, and References
• Appendix A: Ephemeris Determination
• Appendix B: Iteratively Prewhitened Frequencies
• Appendix C: Detected Tidally Perturbed Pulsations

10 CONCLUSIONS

We investigated the systemic errors associated to using the cross correlation technique to extract RVs, which arise due to blending between the spectral lines of the components in a binary system. We find that the effect is small when using TODCOR but correcting for the issue is still necessary because the resulting shifts are clearly systematic in nature and have a non-negligible impact on the results. We used three independent spectroscopic methods to determine the light ratio for the system. The results are in agreement with each other and consistent with the value obtained from modelling the light curve which supports the reliability of our light curve solution. We compared our results to those reported by Guo et al. (2016) and find that we have improved the precision of the measured masses significantly, but the precision in the radius estimates are comparable. Both these outcomes are expected since we use much higher-resolution spectra but the same photometry (Kepler).

By analysing the residuals of the light curve model, we confirm the detection of tidally perturbed p-mode pulsations, possibly in both components of KIC 9851944. A short period spacing pattern was detected among the g modes and was assigned to the primary component, where perturbations to one of the g-modes was detected. Thus, the primary component is a δ Scuti/γ Doradus hybrid. If pulsation mode identification can be performed (as in, e.g., Bedding et al. 2020) on the p modes, KIC 9851944 will become a well-equipped laboratory for stellar physics.

DATA AVAILABILITY

This paper includes data collected by the Kepler and TESS missions which is publicly available at the Mikilski Archive for Space Telescopes (MAST) at the Space Telescope Science institute (STScl) (https://mast.stsci.edu).

ACKNOWLEDGEMENTS

We gratefully acknowledge Barry Smalley for his insightful comments regarding the properties of lines with synthetics, and sharing his thoughts on the possibility that the components of KIC 9851944 are Am stars.

We are grateful to Kelsey Clubb for assisting in obtaining and reducing the spectroscopic observations from the Shane telescope. TVR gratefully acknowledges funding from the KU Leuven Research Council (grant C16/18/005: PARADISE). We gratefully acknowledge financial support from the Science and Technology Facilities Council. This research has made use of the SIMBAD and CDS databases operated by the Centre de Données astronomiques de Strasbourg, France. This paper also made use of data from the Kepler and TESS missions obtained from the MAST data archive at the Space Telescope Science Institue (STScI). Funding for the Kepler and TESS missions is provided by the NASA Science Mission Directorate and NASA Explorer Program, respectively. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555.

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