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arXiv 0911.0666astro-ph.CO
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用Keck干涉仪探测1型活动星系核的内部

Exploring the inner region of Type 1 AGNs with the Keck interferometer

Makoto Kishimoto, Sebastian F. Hoenig, Robert Antonucci, Takayuki Kotani, Richard Barvainis, Konrad R. W. Tristram, Gerd Weigelt

摘要:

用长基线干涉仪近红外探测河外天体的工作非常有限。在这里,我们报告成功的观测与凯克干涉仪在K波段(2.2微米)的四个类型1活动星系核,即NGC 4151,Mrk 231,NGC 4051,和类星体IRAS 13349 +2438在z=0.108。对于后三个物体,这是第一次红外线长基线干涉测量。我们检测到所有四个对象的高V^2(V^2 ~ 0.8-0.9),包括NGC 4151,我们确认了Swain等人测量的高V^2水平。(2003年)的报告。我们在NGC 4151中检测到V^2随基线长度的增加而略微减小,尽管在非常有限的范围内,其中减小和绝对V^2与半径为0.45+/-0.04 mas(0.039+/-0.003 pc)的环形模型拟合良好。引人注目的是,这与被认为是探测尘埃升华半径的光学-红外反射的独立半径测量相匹配。我们还表明,其他对象的有效半径,从相同的环模型,是大致等于或略大于混响半径作为活动星系核光度的函数。这表明我们确实部分地解决了尘埃升华区域。有效环半径与混响半径的比值也可能给我们一个近似的探测器,用于探测每个物体内部吸积物质的径向结构。这一点应通过进一步的观察加以详细审查。

英文摘要:

The exploration of extragalactic objects with long-baseline interferometers in the near-infrared has been very limited. Here we report successful observations with the Keck interferometer at K-band (2.2 um) for four Type 1 AGNs, namely NGC4151, Mrk231, NGC4051, and the QSO IRAS13349+2438 at z=0.108. For the latter three objects, these are the first long-baseline interferometric measurements in the infrared. We detect high visibilities (V^2 ~ 0.8-0.9) for all the four objects, including NGC4151 for which we confirm the high V^2 level measured by Swain et al.(2003). We marginally detect a decrease of V^2 with increasing baseline lengths for NGC4151, although over a very limited range, where the decrease and absolute V^2 are well fitted with a ring model of radius 0.45+/-0.04 mas (0.039+/-0.003 pc). Strikingly, this matches independent radius measurements from optical--infrared reverberations that are thought to be probing the dust sublimation radius. We also show that the effective radius of the other objects, obtained from the same ring model, is either roughly equal to or slightly larger than the reverberation radius as a function of AGN luminosity. This suggests that we are indeed partially resolving the dust sublimation region. The ratio of the effective ring radius to the reverberation radius might also give us an approximate probe for the radial structure of the inner accreting material in each object. This should be scrutinized with further observations.

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