β Pictoris b 希尔球凌星观测计划。论文 II：通过 δ Scuti 脉动的时间延迟分析搜寻 β Pictoris 系外行星的信号
The $β$ Pictoris b Hill sphere transit campaign. Paper II: Searching for the signatures of the $β$ Pictoris exoplanets through time delay analysis of the $δ$ Scuti pulsations
AI总结：
本文通过多年测光数据与 maelstrom 分析 β Pictoris 的 δ Scuti 脉动时间延迟，试图间接探测其行星 b 和 c，但未探测到预期信号，并发现脉动模式本身年际漂移从根本上限制了该方法。
摘要：
β Pictoris 系统是已知距离最近、直接探测到气态巨行星的恒星系统，具有侧向的 circumstellar 盘，并存在下落升华天体和凌星系外彗星的证据。内行星 β Pictoris c 也已通过径向速度（RV）测量被间接探测到。该恒星是已知的 δ Scuti 脉动变星，这些脉动的长期稳定性为通过光行时变化引起的脉动时间延迟来间接探测气态巨行星提供了可能。我们搜寻与已知行星 β Pictoris b 和 c 一致的 δ Scuti 脉动相位偏移，并对 β Pictoris 的恒星脉动进行了多年时间尺度的分析。我们使用 BRITE-Constellation、bRing、ASTEP 和 TESS 收集的测光数据，得出最强和最显著的 δ Scuti 脉动列表。我们利用开源 python 软件包 maelstrom 进行分析，研究 β Pictoris 脉动模式的稳定性，以确定观测脉动的长期趋势。我们没有探测到 β Pictoris b 或 β Pictoris c 的预期信号。β Pictoris c 的预期时间延迟为 6 秒，β Pictoris b 为 24 秒。通过模拟，我们确定所有合并数据集中的测光噪声无法达到探测预期计时漂移所需的灵敏度。使用 maelstrom 对 β Pictoris 脉动模式的分析表明，这些模式本身在一年时间尺度上发生漂移，从根本上限制了我们通过脉动计时探测 β Pictoris 周围系外行星的能力。
英文摘要：
The $β$ 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 seconds for $β$ Pictoris c and 24 seconds 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.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
