蛇夫座ρ星系团候选新成员的重要星群
A Significant Population of Candidate New Members of the Rho Ophiuchi Cluster
摘要：
我们提出了一个通用的方法，用于识别任何恒星形成区域的主序前人口，无偏相对于磁盘的存在或不存在，相反，主要通过他们的中红外发射斯皮策调查选择的样品。我们已经将这种技术应用于一个新的，深，宽场，近红外成像调查的Rho蛇夫座云核心，以寻找候选的低质量成员。结合已发表的Spitzer IRAC测光，以及模型光谱（COND，DUSTY，NextGen和黑体）与观测光谱能量分布的最小二乘拟合，我们在J=20.0，H=20.0和KS =18.50的90%完整性范围内确定了948个候选云成员。这个人口代表了一个因素的增加约3的年轻恒星天体的数量在蛇夫座ρ云。大部分候选星团成员（81% +/- 3%）表现出与盘的存在一致的红外过量发射，从而加强了它们是真正的云成员的可能性。光谱跟踪将确认单个物体的性质，更好地约束它们的参数，并允许导出初始质量函数。
英文摘要：
We present a general method for identifying the pre-main-sequence population of any star-forming region, unbiased with respect to the presence or absence of disks, in contrast to samples selected primarily via their mid-infrared emission from Spitzer surveys. We have applied this technique to a new, deep, wide-field, near-infrared imaging survey of the Rho Ophiuchi cloud core to search for candidate low mass members. In conjunction with published Spitzer IRAC photometry, and least squares fits of model spectra (COND, DUSTY, NextGen, and blackbody) to the observed spectral energy distributions, we have identified 948 candidate cloud members within our 90% completeness limits of J=20.0, H=20.0, and K_S=18.50. This population represents a factor of ~3 increase in the number of known young stellar objects in the Rho Ophiuchi cloud. A large fraction of the candidate cluster members (81% +/- 3%) exhibit infrared excess emission consistent with the presence of disks, thus strengthening the possibility of their being bona fide cloud members. Spectroscopic follow-up will confirm the nature of individual objects, better constrain their parameters, and allow an initial mass function to be derived.
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