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Physical properties of the eclipsing binary KIC 9851944: Appendix A: Ephemeris Determinationby@exoplanetology

Physical properties of the eclipsing binary KIC 9851944: Appendix A: Ephemeris Determination

by Exoplanetology Tech: Research on the Study of Planets
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May 25th, 2024
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Stars that are both pulsating and eclipsing offer an important opportunity to better understand many of the physical phenomena that occur in stars.
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Exoplanetology Tech: Research on the Study of Planets

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Academic Research Paper

Academic Research Paper

Part of HackerNoon's growing list of open-source research papers, promoting free access to academic material.

This paper is available on arxiv under CC 4.0 license.

Authors:

(1) Z. Jennings, Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK (E-mail: z.jennings@keele.ac.uk);

(2) J. Southworth, Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK;

(3) K. Pavlovski, Department of Physics, Faculty of Science, University of Zagreb, 10000 Zagreb, Croatia;

(4) T. Van Reeth, Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium.

APPENDIX A: EPHEMERIS DETERMINATION

This appendix presents the results from the preliminary JKTEBOP analaysis as well as times of primary minimum and fitted values calculated in section 3.


Table A1. Prelimimary light curve results from JKTEBOP fits to the Kepler and TESS light curves. We do not present the error bars associated to each parameter in Table A1 because 1; uncertainties from the covariance matrix of a light curve fit are notoriously underestimated and the results from these preliminary fits are not reliable (see below) so we did not attempt to derive better uncertainties, and 2; excluding the error bar from the result makes it clear that these are not our final values for the light curve parameters.

Table A1. Prelimimary light curve results from JKTEBOP fits to the Kepler and TESS light curves. We do not present the error bars associated to each parameter in Table A1 because 1; uncertainties from the covariance matrix of a light curve fit are notoriously underestimated and the results from these preliminary fits are not reliable (see below) so we did not attempt to derive better uncertainties, and 2; excluding the error bar from the result makes it clear that these are not our final values for the light curve parameters.


Table A2. Measured and fitted times of primary minimum derived in section 3.

Table A2. Measured and fitted times of primary minimum derived in section 3.

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