双子座深行星巡天-- GDPS
The Gemini Deep Planet Survey -- GDPS
摘要：
我们提出了双子座深行星调查的结果，近红外自适应光学搜索附近的年轻恒星周围的巨行星和褐矮星。观测是在双子座北望远镜的牛郎星自适应光学系统和角微分成像被用来抑制中央恒星的斑点噪声。观测到的85颗恒星的探测极限，以及在它们周围探测到的所有微弱点源的列表。通常情况下，观察结果对超过0.5”的角间距敏感，其中在1.6微米处的幅度差的5-sigma对比度灵敏度为0.5”处9.5，1”处12.9，2”处15.0和5”处16.5。对于调查的典型目标，距离太阳22 pc的1亿年老K 0恒星，观测足够灵敏，可以检测到质量超过2 Mjup的行星，预计距离在40-200 AU范围内。对54颗候选恒星中的48颗恒星的第二纪元观测证实，所有候选恒星都是不相关的背景恒星。详细的统计分析的调查结果，产生上限的分数的恒星与巨行星或低质量的棕矮星的同伴，提出。假设行星的质量分布为dN/dm m^{-1.2}，半长轴分布为dN/da a^{-1}，则在10-25 AU范围内，至少有一颗质量为0.5-13兆焦耳的行星的恒星比例的95%可信上限为0.28，25-50 AU为0.13，50-250 AU为0.093。不考虑质量和半长轴分布的任何假设，拥有至少一颗半长轴在25-250 AU范围内的棕矮星伴星的恒星比例的95%可信区间为0.019（-0.015/+0.083）。HD 14802、HD 166181和HD 213845这三颗恒星首次被解析成双星。
英文摘要：
We present the results of the Gemini Deep Planet Survey, a near-infrared adaptive optics search for giant planets and brown dwarfs around nearby young stars. The observations were obtained with the Altair adaptive optics system at the Gemini North telescope and angular differential imaging was used to suppress the speckle noise of the central star. Detection limits for the 85 stars observed are presented, along with a list of all faint point sources detected around them. Typically, the observations are sensitive to angular separations beyond 0.5" with 5-sigma contrast sensitivities in magnitude difference at 1.6 micron of 9.5 at 0.5", 12.9 at 1", 15.0 at 2", and 16.5 at 5". For the typical target of the survey, a 100 Myr old K0 star located 22 pc from the Sun, the observations are sensitive enough to detect planets more massive than 2 Mjup with a projected separation in the range 40-200 AU. Second epoch observations of 48 stars with candidates (out of 54) have confirmed that all candidates are unrelated background stars. A detailed statistical analysis of the survey results, yielding upper limits on the fractions of stars with giant planet or low mass brown dwarf companions, is presented. Assuming a planet mass distribution dN/dm m^{-1.2} and a semi-major axis distribution dN/da a^{-1}, the 95% credible upper limits on the fraction of stars with at least one planet of mass 0.5-13 Mjup are 0.28 for the range 10-25 AU, 0.13 for 25-50 AU, and 0.093 for 50-250 AU. The 95% credible interval for the fraction of stars with at least one brown dwarf companion having a semi-major axis in the range 25-250 AU is 0.019 (-0.015/+0.083), irrespective of any assumption on the mass and semi-major axis distributions. The stars HD 14802, HD 166181, and HD 213845 have been resolved into binaries for the first time.
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