古尔德带星际云的斯皮策巡天。IV。使用IRAC和MIPS观察到的狼疮V和VI
The Spitzer Survey of Interstellar Clouds in the Gould Belt. IV. Lupus V and VI Observed with IRAC and MIPS
摘要：
我们提出了古尔德带（GB）斯皮策IRAC和MIPS观测狼疮V和VI云，并结合近红外（2 MASS）数据进行讨论。我们的观测结果补充了斯皮策“核心到磁盘”（c2 d）遗产调查框架内获得的其他狼疮云。我们发现43年轻恒星对象（YSO）的候选人在狼疮V和45在狼疮VI，包括2过渡盘，使用标准的c2 d/GB选择方法。在之前的光学、近红外和X射线巡天中，这些来源都没有被归类为前主序星。这些YSO候选者中的绝大多数似乎被薄盘包围（III类;狼疮V中约79%，狼疮VI中约87%）。这些III类丰度与其他狼疮云和c2 d/GB调查的恒星形成区域观察到的丰度显着不同，其中光学厚盘（II类）的物体占主导地位的年轻人口。我们调查了各种可以解释这种差异的情况。特别是，我们表明，光盘光蒸发由于附近的OB星是不负责的III类对象的高比例。测量到的狼疮V和VI的气体表面密度低于恒星形成阈值（AV { \eqsim }8.6等），而其他狼疮云的情况并非如此。因此，在狼疮V和VI的YSO相对于其他狼疮云的年龄大了几个百万年，这是这些云中III类天体比例高的最可能解释，而更高的特征恒星质量可能是一个贡献因素。更好地约束年龄和二进制分数
英文摘要：
We present Gould's Belt (GB) Spitzer IRAC and MIPS observations of the Lupus V and VI clouds and discuss them in combination with near-infrared (2MASS) data. Our observations complement those obtained for other Lupus clouds within the frame of the Spitzer "Core to Disk" (c2d) Legacy Survey. We found 43 Young Stellar Object (YSO) candidates in Lupus V and 45 in Lupus VI, including 2 transition disks, using the standard c2d/GB selection method. None of these sources was classified as a pre-main sequence star from previous optical, near-IR and X-ray surveys. A large majority of these YSO candidates appear to be surrounded by thin disks (Class III; ~79% in Lupus V and ~87% in Lupus VI). These Class III abundances differ significantly from those observed for the other Lupus clouds and c2d/GB surveyed star-forming regions, where objects with optically thick disks (Class II) dominate the young population. We investigate various scenarios that can explain this discrepancy. In particular, we show that disk photo-evaporation due to nearby OB stars is not responsible for the high fraction of Class III objects. The gas surface densities measured for Lupus V and VI lies below the star-formation threshold (AV {\eqsim}8.6 mag), while this is not the case for other Lupus clouds. Thus, few Myrs older age for the YSOs in Lupus V and VI with respect to other Lupus clouds is the most likely explanation of the high fraction of Class III objects in these clouds, while a higher characteristic stellar mass might be a contributing factor. Better constraints on the age and binary fraction of
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