船帆座分子脊云D中毫米尘埃核的近红外和远红外对应物
Near- and Far-Infrared Counterparts of Millimeter Dust Cores in the Vela Molecular Ridge Cloud D
摘要：
本文的目的是通过新的红外观测（2.12微米的H_2窄带和10.4微米的N宽带）以及对现有红外星表的研究来识别船帆座分子脊云D尘埃毫米核的年轻原恒星对应物。根据空间符合、红外颜色和光谱能量分布，建立了毫米波连续辐射与星表（IRAS，MSX，2 MASS）、文献中的JHK数据和新观测的红外源的联系。在29个已解析的毫米核中，只有7个（以及26个未解析核中的16个）没有显示出恒星形成活动的标志。其它的则与远红外源、H_2喷流或近红外天体的高本征色余有关。与相关源有关的谱指数的分布在I类对象的典型值处达到峰值，而三个对象被信号通知为候选0类源。我们注意到，由位于mm核内部的源驱动的H_2喷流的高探测率（30%）。它们似乎不是由场中最明亮的天体驱动的，而是由年轻星团中较不明亮的天体驱动的，证明了低质量和中等质量恒星形成的共存。所提供的结果可靠地描述了VMR-D的年轻人群。然而，统计评估的活动与不活动的调查核心，即使在良好的协议与其他恒星形成区域的结果，似乎反映了有限的敏感性，而不是任何固有的毫米凝聚的设施。
英文摘要：
The aim of this paper is to identify the young protostellar counterparts associated to dust millimeter cores of the Vela Molecular Ridge Cloud D through new IR observations (H_2 narrow-band at 2.12 micron and N broad band at 10.4 micron) along with an investigation performed on the existing IR catalogues. The association of mm continuum emission with infrared sources from catalogues (IRAS, MSX, 2MASS), JHK data from the literature and new observations, has been established according to spatial coincidence, infrared colours and spectral energy distributions. Only 7 out of 29 resolved mm cores (and 16 out of the 26 unresolved ones) do not exhibit signposts of star formation activity. The other ones are clearly associated with: far-IR sources, H_2 jets or near-IR objects showing a high intrinsic colour excess. The distribution of the spectral indices pertaining to the associated sources is peaked at values typical of Class I objects, while three objects are signalled as candidates Class 0 sources. We remark the high detection rate (30%) of H_2 jets driven by sources located inside the mm-cores. They appear not driven by the most luminous objects in the field, but rather by less luminous objects in young clusters, testifying the co-existence of both low- and intermediate-mass star formation. The presented results reliably describe the young population of VMR-D. However, the statistical evaluation of activity vs inactivity of the investigated cores, even in good agreement with results found for other star forming regions, seems to reflect the limiting sensitivity of the available facilities rather than any property intrinsic to the mm-condensations.
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