对500颗附近恒星的碎片盘进行无偏见的调查：JCMT遗产计划
An Unbiased Survey of 500 Nearby Stars for Debris Disks: A JCMT Legacy Program
摘要：
我们提出的科学动机和观测计划，即将到来的探测调查碎片磁盘使用詹姆斯克拉克麦克斯韦望远镜。SCUBA-2无偏邻近恒星巡天将观测附近500颗主序星和次巨星（A、F、G、K和M光谱类各100颗），观测范围达到850微米的河外混淆极限，以寻找次毫米波过量的证据，这是星周物质的一种迹象。M、K、G、F和A星的测量距离边界分别为8.6、16.5、22、25和45秒差距，所有目标都位于-40度至80度的赤纬之间。在这次调查中，没有恒星会因为其固有的性质而被拒绝：双星，行星同伴的存在，光谱类型或年龄。这将是自红外天文卫星以来对碎片盘进行的第一次无偏差的调查。我们预计将探测到约125个碎片盘，其中包括目前较短波长调查中无法探测到的约50个冷盘。将需要大量的补充数据来限制所发现的磁盘的温度和质量。可能需要高分辨率研究来解析许多磁盘。因此，这些系统将是未来观测研究的重点，使用各种观测站来表征其物理特性。对于未被探测到的系统，这项调查将对星周尘埃的数量设定限制（上限），通常为柯伊伯带质量的200倍，但对于样本中最近的恒星（约2 pc），低至柯伊伯带质量的10倍。
英文摘要：
We present the scientific motivation and observing plan for an upcoming detection survey for debris disks using the James Clerk Maxwell Telescope. The SCUBA-2 Unbiased Nearby Stars (SUNS) Survey will observe 500 nearby main sequence and sub-giant stars (100 of each of the A, F, G, K and M spectral classes) to the 850 micron extragalactic confusion limit to search for evidence of submillimeter excess, an indication of circumstellar material. The survey distance boundaries are 8.6, 16.5, 22, 25 and 45 pc for M, K, G, F and A stars, respectively, and all targets lie between the declinations of -40 deg to 80 deg. In this survey, no star will be rejected based on its inherent properties: binarity, presence of planetary companions, spectral type or age. This will be the first unbiased survey for debris disks since IRAS. We expect to detect ~125 debris disks, including ~50 cold disks not detectable in current shorter wavelength surveys. A substantial amount of complementary data will be required to constrain the temperatures and masses of discovered disks. High resolution studies will likely be required to resolve many of the disks. Therefore, these systems will be the focus of future observational studies using a variety of observatories to characterize their physical properties. For non-detected systems, this survey will set constraints (upper limits) on the amount of circumstellar dust, of typically 200 times the Kuiper Belt mass, but as low as 10 times the Kuiper Belt mass for the nearest stars in the sample (approximately 2 pc).
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