对大质量年轻恒星天体CRL 2136的中红外干涉测量：在尘埃边缘内
Mid-infrared interferometry towards the massive young stellar object CRL 2136: inside the dust rim
摘要：
我们应用中红外光谱干涉测量的大质量的年轻恒星对象CRL 2136。这些观测是用甚大望远镜干涉仪和射电望远镜仪器在42米的基线上进行的，探测角标度为50毫弧秒。我们平行于24.5微米和N波段的衍射极限图像（分辨率分别为0.6”和0.3”），以及光谱能量分布，对观察到的粒子进行建模。弧秒尺度的空间信息揭示了尘埃包层的高分辨辐射。通过同时建模的空间和光谱数据，我们发现，大部分的尘埃排放发生在几个尘埃升华半径（约170 AU）。这再现了高的中红外通量，同时也再现了在波长向8.5微米的长波数据中观察到的低的紫外线。然而，短的波长的能见度数据显示了一个急剧的上升，指示紧凑的排放。我们讨论了这种排放的各种潜在来源。我们排除了一个尘埃盘负责观察到的光谱印记上的vibrium。一个冷的超巨星和一个吸积盘被认为是可行的起源紧凑的中红外辐射。我们建议，CRL 2136是嵌入在尘埃信封，截断在几倍的尘埃升华半径。在赤道地区有一个尘埃环。我们发现，光谱干涉的N波段信号可以再现的气体盘或膨胀的中央恒星。如果圆盘延伸到恒星表面，它的吸积速率为3.0 × 10^（-3）Msun/yr。
英文摘要：
We apply mid-infrared spectro-interferometry to the massive young stellar object CRL2136. The observations were performed with the Very Large Telescope Interferometer and the MIDI instrument at a 42m baseline probing angular scales of 50 milli-arcseconds. We model the observed visibilities in parallel with diffraction-limited images at both 24.5micron and in the N-band (with resolutions of 0.6" and 0.3", respectively), as well as the spectral energy distribution. The arcsec-scale spatial information reveals the well-resolved emission from the dusty envelope. By simultaneously modelling the spatial and spectral data, we find that the bulk of the dust emission occurs at several dust sublimation radii (approximately 170 AU). This reproduces the high mid-infrared fluxes and at the same time the low visibilities observed in the MIDI data for wavelengths longward of 8.5micron. However, shortward of this wavelength the visibility data show a sharp up-turn indicative of compact emission. We discuss various potential sources of this emission. We exclude a dust disk being responsible for the observed spectral imprint on the visibilities. A cool supergiant star and an accretion disk are considered and both shown to be viable origins of the compact mid-infrared emission. We propose that CRL2136 is embedded in a dusty envelope, which truncates at several times the dust sublimation radius. A dust torus is manifest in the equatorial region. We find that the spectro-interferometric N-band signal can be reproduced by either a gaseous disk or a bloated central star. If the disk extends to the stellar surface, it accretes at a rate of 3.0 10^(-3) Msun/yr.
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