A search for transiting planets in the β Pictoris system
Open accessAbstract
Context. Transiting exoplanets provide an opportunity for the characterization of their atmospheres, and finding the brightest star in the sky with a transiting planet enables high signal-to-noise ratio observations. The Kepler satellite has detected over 365 multiple transiting exoplanet systems, a large fraction of which have nearly coplanar orbits. If one planet is seen to transit the star, then it is likely that other planets in the system will transit the star too. The bright (V = 3.86) star β Pictoris is a nearby young star with a debris disk and gas giant exoplanet, β Pictoris b, in a multi-decade orbit around it. Both the planet’s orbit and disk are almost edge-on to our line of sight. Aims. We carry out a search for any transiting planets in the β Pictoris system with orbits of less than 30 days that are coplanar with the planet β Pictoris b. Methods. We search for a planetary transit using data from the BRITE-Constellation nanosatellite BRITE-Heweliusz, analyzing the photometry using the Box-Fitting Least Squares Algorithm (BLS). The sensitivity of the method is verified by injection of artificial planetary transit signals using the Bad-Ass Transit Model cAlculatioN (BATMAN) code. Results. No planet was found in the BRITE-Constellation data set. We rule out planets larger than 0.6 RJ for periods of less than 5 days, larger than 0.75 RJ for periods of less than 10 days, and larger than 1.05 RJ for periods of less than 20 days.
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The sensitivity plots show similar trends as the ones in the search for planets orbiting Pictoris in Lous et al. (2018).
“The sensitivity plots (Figures 8 and 9) show similar trends as the ones in the search for planets orbiting Pictoris in Lous et al. (2018).”
From A search for transiting companions in the J1407 (V1400 Cen) system (2021) · cites this paper as Lous et al. 2018
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Self-citationThe β Pictoris b Hill sphere transit campaign
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Self-citationSpectroscopic transit search: a self-calibrating method for detecting planets around bright stars
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Self-citationA search for transiting companions in the J1407 (V1400 Cen) system
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A search for transiting companions in the J1407 (V1400 Cen) system
Barmentloo, S., Dik, C., Kenworthy, M. A., Mamajek, E. E., Hambsch, F.-J., Reichart, D. E., Rodriguez, J. E., & van Dam, D. M. (2021) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/202140768/pdf · Cited by 1 · see citing works
Self-citation
- Authors
- Mol Lous, M., Weenk, E., Kenworthy, M. A., Zwintz, K., & Kuschnig, R.
- Affiliations
- Leiden University (NL)
- Universität Innsbruck (AT)
- Graz University of Technology (AT)
- Venue
- Astronomy & Astrophysics
- Publisher
- EDP Sciences
- Published
- 2018-07
- Volume
- 615
- Pages
- A145
- ISSN
- 0004-6361 (ISSN-L)
- 1432-0746
- OpenAlex
- W2796496098
- Cited by
- 10
- References
- 37
- Citations by year
- 2026: 1 · 2023: 1 · 2021: 4 · 2020: 1 · 2019: 3
- FWCI
- 1.05
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- Astronomy and Astrophysics (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- Leiden Repository (Leiden University) (submittedVersion)
- Data Archiving and Networked Services (DANS) (submittedVersion, other-oa)
- arXiv (Cornell University)
- Funders
- Fundacja na rzecz Nauki Polskiej
- Austrian Science Fund (V431-NBL)
- Universität Wien
- University of Toronto
- Ministerstwo Edukacji i Nauki
- Österreichische Forschungsförderungsgesellschaft
- Karl-Franzens-Universität Graz
- Canadian Space Agency
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Instrumentation › Astronomy and Astrophysical Research
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › History and Developments in Astronomy
- Keywords
- Beta Pictoris, transiting exoplanets, Beta Pictoris b, debris disks, young stars, coplanar orbits, BRITE-Constellation, Box Least Squares, transit search
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