论文标题
探测Au〜显微镜碎片磁盘的最内向区域
Probing the innermost region of the AU~Microscopii debris disk
论文作者
论文摘要
Au Mic是一位年轻且附近的M-warf恒星，上面有一个杂物片，最近在8D轨道上发现了一个星球。还发现了磁盘内的大规模结构，并以高速度向外移动。我们旨在研究以最高空间分辨率的最高空间分辨率来研究该系统，以探测最内向的区域并寻找其他低质量伴侣或设定的检测限制。用两种不同的技术观察到恒星，探测互补的空间尺度。我们获得了新的SAM观察结果，并将其与NACO，Pionier和Gravity的数据相结合。我们没有从恒星中检测到0.02-7au内的其他伴侣。我们确定了在0.02-0.5au内的H〜9.8mag同伴的上限，ks〜11.2毫克在0.4-2.4au内，在0.7-7au内的L'〜10.7毫米内。我们使用理论等时线，分别转化为〜17MJUP，〜12MJUP和〜9JUP的质量上限。先驱观察结果使我们能够确定AU MIC的角直径为0.825 +/- 0.050Mas，它转换为r = 0.862 +/- 0.052rsun。我们没有检测到新发现的行星，但我们衍生了Au Mic最内向区域的上限质量。我们没有任何超出3sigma的显着性的检测，最显着的信号为2.9 sigma，球体为1.6σ。我们应用了PYMESS2代码来估计伴侣的检测概率，通过结合径向速度，球体成像和我们的干涉检测图。我们表明，可以在0.02au或1MJUP内检测到99％的同伴下降到约0.5MJUP。由于其近距离轨道和非常高的对比度（k中〜10E-10E），在<0.11AU处绕<0.11AU的低质量行星无法直接检测到。它也将低于下一个ELT IR成像仪器的角度分辨率和对比度极限。
AU Mic is a young and nearby M-dwarf star harbouring a circumstellar debris disk and one recently discovered planet on an 8d orbit. Large-scale structures within the disk were also discovered and are moving outward at high velocity. We aim at studying this system with the highest spatial resolution in order to probe the innermost regions and to search for additional low-mass companion or set detection limits. The star was observed with two different techniques probing complementary spatial scales. We obtained new SAM observations with SPHERE, which we combined with data from NACO, PIONIER and GRAVITY. We did not detect additional companions within 0.02-7au from the star. We determined magnitude upper limits for companions of H~9.8mag within 0.02-0.5au, Ks~11.2mag within 0.4-2.4au and L'~10.7mag within 0.7-7au. Using theoretical isochrones, we converted into mass upper limits of ~17Mjup, ~12Mjup and ~9jup, respectively. The PIONIER observations allowed us to determine the angular diameter of AU Mic, 0.825+/-0.050mas, which converts to R = 0.862+/-0.052Rsun. We did not detect the newly discovered planets, but we derived upper limit masses for the innermost region of AU Mic. We do not have any detection with a significance beyond 3sigma, the most significant signal with PIONIER being 2.9sigma and with SPHERE being 1.6σ. We applied the pyMESS2 code to estimate the detection probability of companions by combining radial velocities, SPHERE imaging and our interferometric detection maps. We show that 99% of the companions down to ~0.5Mjup can be detected within 0.02au or 1Mjup down to 0.2au. The low-mass planets orbiting at <0.11au will not be directly detectable with the current AO and interferometric instruments due to its close orbit and very high contrast (~10e-10 in K). It will be also below the angular resolution and contrast limit of the next ELT IR imaging instruments.
