Zieba, SebastianZwintz, KonstanzeKenworthy, MatthewHey, DanielMurphy, Simon J.Kuschnig, RainerAbe, LyuAgabi, AbdelkrimMekarnia, DjamelGuillot, TristanSchmider, François XavierStee, PhilippeDe Pra, YuriButtu, MarcoCrouzet, NicolasMellon, SamuelBailey, JebStuik, RemkoDorval, PatrickTalens, Geert JanCrawford, StevenMamajek, EricLaginja, IvaIreland, MichaelLomberg, BlaineKuhn, RudiSnellen, IgnasKalas, PaulWang, Jason J.Stevenson, Kevin B.De Mooij, ErnstLagrange, Anne MarieLacour, SylvestreNowak, MathiasStrøm, Paul A.Hui, ZhangWang, Lifan2025-05-232025-05-230004-6361http://www.scopus.com/inward/record.url?scp=85200146350&partnerID=8YFLogxKhttps://hdl.handle.net/1885/733752712The β Pictoris system is the closest known stellar system with directly detected gas giant planets, an edge-on circumstellar disc, and evidence of falling sublimating bodies and transiting exocomets. The inner planet, β Pictoris c, has also been indirectly detected with radial velocity (RV) measurements. The star is a known δ Scuti pulsator, and the long-term stability of these pulsations opens up the possibility of indirectly detecting the gas giant planets through time delays of the pulsations due to a varying light travel time. We search for phase shifts in the δ Scuti pulsations consistent with the known planets β Pictoris b and c and carry out an analysis of the stellar pulsations of β Pictoris over a multi-year timescale. We used photometric data collected by the BRITE-Constellation, bRing, ASTEP, and TESS to derive a list of the strongest and most significant δ Scuti pulsations. We carried out an analysis with the open-source python package maelstrom to study the stability of the pulsation modes of β Pictoris in order to determine the long-term trends in the observed pulsations. We did not detect the expected signal for β Pictoris b or β Pictoris c. The expected time delay is 6 s for β Pictoris c and 24 s for β Pictoris b. With simulations, we determined that the photometric noise in all the combined data sets cannot reach the sensitivity needed to detect the expected timing drifts. An analysis of the pulsational modes of β Pictoris using maelstrom showed that the modes themselves drift on the timescale of a year, fundamentally limiting our ability to detect exoplanets around β Pictoris via pulsation timing.This work includes dala collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by the NASA Explorer Program. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://wvfw.cosmos.esa.int/gaia). processed by the Gaia Data Processing and Analysis Consortium (DPAC. https://www. cosmos.esa. int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions partici- pating in the Gaia Multilateral Agreement. We made use of the software package Period\u03B84 (Lenz & Breger 2005), the Python programming language (Rossum 1995), and the open-source Python packages numpy (van der Walt et al. 2011), matplotlib (Hunter 2007), astropy (Astropy Collaboration 2013), lightkurve (Lightkurve Collaboration 2018), timedelay8, maelstrom9 and SMURFS (M\u00FCllner 2020), This research has made use of the SIMBAD database, operated at CDS, Strasbourg. France. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). This research has made use of data collected by the BRITE-Constellation satellite mission, designed, built, launched, operated and supported by the Austrian Research Promotion Agency (FFG), the University of Vienna, the Technical University of Graz, the University of Innsbruck, the Canadian Space Agency (CSA), the Uni-versity of Toronto Institute for Aerospace Studies (UTIAS), the Foundation for Polish Science & Technology (FNiTP MNiSW), and National Science Centre (NCN). The bRing observatory at Siding Springs. Australia was supported by a University of Rochester University Research Award. The field activities at Dome C for ASTEP benefit from the support of the French and Italian polar agencies 1PEV and PNRA in the framework of the Concordia station programme. The PicSat team thanks funding from the European Research Council (ERC) under the Horizon 2020 research and innovation programme (Grant agreement No. 639248. LITHIUM). SJM was supported by the Australian Research Council (ARC) through Future Fellowship FT210100485. This work includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by the NASA Explorer Program. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the G\u03B1i\u03B1 Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the G\u03B1i\u03B1 Multilateral Agreement. We made use of the software package Period04 (Lenz & Breger 2005), the Python programming language (Rossum 1995), and the open-source Python packages numpy (van der Walt et al. 2011), matplotlib (Hunter 2007), astropy (Astropy Collaboration 2013), lightkurve (Lightkurve Collaboration 2018), timedelay 8, maelstrom 9 and SMURFS (M\u00FCllner 2020). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). This research has made use of data collected by the BRITE-Constellation satellite mission, designed, built, launched, operated and supported by the Austrian Research Promotion Agency (FFG), the University of Vienna, the Technical University of Graz, the University of Innsbruck, the Canadian Space Agency (CSA), the University of Toronto Institute for Aerospace Studies (UTIAS), the Foundation for Polish Science & Technology (FNiTP MNiSW), and National Science Centre (NCN). The bRing observatory at Siding Springs, Australia was supported by a University of Rochester University Research Award. The field activities at Dome C for ASTEP benefit from the support of the French and Italian polar agencies IPEV and PNRA in the framework of the Concordia station programme. The PicSat team thanks funding from the European Research Council (ERC) under the Horizon 2020 research and innovation programme (Grant agreement No. 639248, LITHIUM). SJM was supported by the Australian Research Council (ARC) through Future Fellowship FT210100485.enPublisher Copyright: © The Authors 2024.AsteroseismologyMethods: observationalPlanets and satellites: generalStars: individual: β pictorisStars: variables: δ ScutiTechniques: photometric2024-07-0110.1051/0004-6361/20234775485200146350