Van Grootel, V, Pozuelos, FJ, Thuillier, A, Charpinet, S, Delrez, L, Beck, M, Fortier, A, Hoyer, S, Sousa, SG, Barlow, BN, Billot, N, Dévora-Pajares, M, Østensen, RH, Alibert, Y, Alonso, R, Anglada Escudé, G, Asquier, J, Barrado, D, Barros, SCC, Baumjohann, W, Beck, T, Bekkelien, A, Benz, W, Bonfils, X, Brandeker, A, Broeg, C, Bruno, G, Bárczy, T, Cabrera, J, Cameron, AC, Charnoz, S, Davies, MB, Deleuil, M, Demangeon, ODS, Demory, B-O, Ehrenreich, D, Erikson, A, Fossati, L, Fridlund, M, Futyan, D, Gandolfi, D, Gillon, M, Guedel, M, Heng, K, Isaak, KG, Kiss, L, Laskar, J, Lecavelier des Etangs, A, Lendl, M, Lovis, C, Magrin, D, Maxted, PFL, Mecina, M, Mustill, AJ, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piotto, G, Plesseria, J-Y, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Santos, NC, Scandariato, G, Ségransan, D, Silvotti, R, Simon, AE, Smith, AMS, Steller, M, Szabó, GM, Thomas, N, Udry, S, Viotto, V, Walton, NA, Westerdorff, K and Wilson, TG (2021) A search for transiting planets around hot subdwarfs. Astronomy & Astrophysics, 650 (A205). ISSN 0004-6361

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Context. Hot subdwarfs experienced strong mass loss on the red giant branch (RGB) and are now hot and small He-burning objects. These stars constitute excellent opportunities for addressing the question of the evolution of exoplanetary systems directly after the RGB phase of evolution.

Aims. In this project we aim to perform a transit survey in all available light curves of hot subdwarfs from space-based telescopes (Kepler, K2, TESS, and CHEOPS) with our custom-made pipeline SHERLOCK in order to determine the occurrence rate of planets around these stars as a function of orbital period and planetary radius. We also aim to determine whether planets that were previously engulfed in the envelope of their red giant host star can survive, even partially, as a planetary remnant.

Methods. For this first paper, we performed injection-and-recovery tests of synthetic transits for a selection of representative Kepler, K2, and TESS light curves to determine which transiting bodies in terms of object radius and orbital period we will be able to detect with our tools. We also provide estimates for CHEOPS data, which we analyzed with the pycheops package.

Results. Transiting objects with a radius less than or similar to 1.0 R-circle times can be detected in most of the Kepler, K2, and CHEOPS targets for the shortest orbital periods (1 d and shorter), reaching values as low as similar to 0.3 R-circle times in the best cases. Sub-Earth-sized bodies are only reached for the brightest TESS targets and for those that were observed in a significant number of sectors. We also give a series of representative results for larger planets at greater distances, which strongly depend on the target magnitude and on the length and quality of the data.

Conclusions. The TESS sample will provide the most important statistics for the global aim of measuring the planet occurrence rate around hot subdwarfs. The Kepler, K2, and CHEOPS data will allow us to search for planetary remnants, that is, very close and small (possibly disintegrating) objects.

Item Type: Article
Additional Information: The final version of this article and all relevant information related to it, including copyrights, can be found online at;
Uncontrolled Keywords: planet-star interactions; planetary systems; stars: horizontal-branch; subdwarfs; techniques: photometric
Subjects: Q Science > Q Science (General)
Q Science > QB Astronomy
Q Science > QB Astronomy > QB600 Planets. Planetology
Q Science > QB Astronomy > QB799 Stars
Q Science > QC Physics
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Depositing User: Symplectic
Date Deposited: 04 Aug 2021 10:42
Last Modified: 20 Aug 2021 15:31

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