VIBES:使用SPHERE进行视觉双系外行星调查

J. Hagelberg, N. Engler, C. Fontanive, S. Daemgen, S. Quanz, J. Kuhn, M. Reggiani, M. Meyer, R. Jayawardhana, V. B. I. F. T. Physics, Astrophysics, E. Zurich, Switzerland., G. Observatory, U. Geneva, Center for Space, Habitability, U. Bern, Bern, Institute of Astrophysics, K. Leuven, Celestijnlaan 200D, Leuven, Belgium, U. Michigan, A. Department, Usa, D. Astronomy, C. University, Ithaca, Ny, NasaGsfc
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引用次数: 6

摘要

最近的调查表明,双星系统中的行星比以前认为的要多,这与双星系统中盘动力学和行星形成的理论工作一致。为了测量双星系统中宽轨道巨型系外行星的丰度和物理特征,我们设计了“视觉双星系外行星调查与球体”(VIBES)来搜索视觉双星中的行星。它使用VLT的SPHERE仪器在23个视觉双星系统和4个视觉三星系统中搜索行星,这些行星的年龄小于145 Myr,距离小于150 pc。我们使用SPHERE上的IRDIS双频成像仪获取了样品目标的高对比度图像。对于每一个双星,用日冕仪同时观测两个组成部分,只遮挡主星。对于三星,为了数据简化,紧构件被当作单星处理。这使我们能够有效地搜索大约50颗双星和4颗三元双星的伴星。我们得出了在视双星中主星周围的恒星伴星的频率上限< 13.7%,在视双星中次级恒星周围的恒星伴星的比例上限< 26.5%,在视双星的任何一个组成部分周围的巨行星和褐矮星的发生率上限< 9.0%。我们将我们的观察结果与文献测量相结合,首次从天文计量学上证实,20个双星系统和两个三重系统,这些之前已知的系统,确实是物理结合的。最后,我们发现了双星HD~121336的第三个组成部分。我们得到的上限与双星通过核心吸积和引力不稳定过程形成的行星是相容的。这些限制也与单星和环双星行星搜索调查中发现的限制一致。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
VIBES: Visual Binary Exoplanet survey with SPHERE
Recent surveys indicate that planets in binary systems are more abundant than previously thought, which is in agreement with theoretical work on disc dynamics and planet formation in binaries. In order to measure the abundance and physical characteristics of wide-orbit giant exoplanets in binary systems, we have designed the 'VIsual Binary Exoplanet survey with Sphere' (VIBES) to search for planets in visual binaries. It uses the SPHERE instrument at VLT to search for planets in 23 visual binary and four visual triple systems with ages of <145 Myr and distances of <150 pc. We used the IRDIS dual-band imager on SPHERE to acquire high-contrast images of the sample targets. For each binary, the two components were observed at the same time with a coronagraph masking only the primary star. For the triple star, the tight components were treated as a single star for data reduction. This enabled us to effectively search for companions around 50 individual stars in binaries and four binaries in triples. We derived upper limits of $<$13.7\% for the frequency of sub-stellar companions around primaries in visual binaries, $<$26.5\% for the fraction of sub-stellar companions around secondaries in visual binaries, and an occurrence rate of $<$9.0\% for giant planets and brown dwarfs around either component of visual binaries. We have combined our observations with literature measurements to astrometrically confirm, for the first time, that 20 binaries and two triple systems, which were previously known, are indeed physically bound. Finally, we discovered a third component of the binary HD~121336. The upper limits we derived are compatible with planet formation through the core accretion and the gravitational instability processes in binaries. These limits are also in line with limits found for single star and circumbinary planet search surveys.
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