$β$风景如画的希尔球transit运动。文件一：尘埃和光环的光度限度
The $β$ Pictoris b Hill sphere transit campaign. Paper I: Photometric limits to dust and rings
摘要：
在1981年，美如画β的光度监测显示，在几天内有高达4%的异常波动，与前景物质通过恒星盘一致。随后发现的气体巨行星β Picasso b和预测的希尔球凌日在0.1天文单位的投影距离内的行星提供了一个机会，以寻找凌日的环行星际盘在这个$21\pm 4$ Myr古老的行星系。对β Picasso进行连续的宽带光度监测需要多个地面观测站提供冗余，并为快速光谱跟踪提供触发。这些观测站包括位于萨瑟兰和赛丁斯普林斯的专门的Beta Picture监测观测站bRing，位于康科迪亚的ASTEP400望远镜，以及来自BRITE和哈勃空间望远镜的观测。我们搜索组合光变曲线的证据造成的短期瞬态事件的环和长期的光度变化，由于弥漫的环行物质。我们没有发现与1981年11月的事件相匹配的光度事件，也没有系统的光度变暗的恒星作为希尔球半径的函数。我们的结论是，1981年的事件不是由环绕行星盘在毕宿二周围的过境引起的。毕赤星长期变化的上限是希尔球内尘埃的$1.8\times 10^{22}$ g。环行星际物质要么凝聚成一个非凌日盘，要么凝聚成一个有小行星度卫星的盘，或者低于我们的探测阈值。这是第一次专门的国际运动已经绘制了10 au的气体巨型太阳系外行星的希尔球过境。
英文摘要：
Photometric monitoring of Beta Pictoris in 1981 showed anomalous fluctuations of up to 4% over several days, consistent with foreground material transiting the stellar disk. The subsequent discovery of the gas giant planet Beta Pictoris b and the predicted transit of its Hill sphere to within 0.1 au projected distance of the planet provided an opportunity to search for the transit of a circumplanetary disk in this $21\pm 4$ Myr-old planetary system. Continuous broadband photometric monitoring of Beta Pictoris requires ground-based observatories at multiple longitudes to provide redundancy and to provide triggers for rapid spectroscopic followup. These observatories include the dedicated Beta Pictoris monitoring observatory bRing at Sutherland and Siding Springs, the ASTEP400 telescope at Concordia, and observations from the space observatories BRITE and Hubble Space Telescope. We search the combined light curves for evidence of short period transient events caused by rings and for longer term photometric variability due to diffuse circumplanetary material. We find no photometric event that matches with the event seen in November 1981, and there is no systematic photometric dimming of the star as a function of the Hill sphere radius. We conclude that the 1981 event was not caused by the transit of a circumplanetary disk around Beta Pictoris b. The upper limit on the long term variability of Beta Pictoris places an upper limit of $1.8\times 10^{22}$ g of dust within the Hill sphere. Circumplanetary material is either condensed into a non-transiting disk, is condensed into a disk with moons that has a small obliquity, or is below our detection threshold. This is the first time that a dedicated international campaign has mapped the Hill sphere transit of a gas giant extrasolar planet at 10 au.
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