用Keck干涉仪探测活动星系核最内层的尘埃结构
The innermost dusty structure in active galactic nuclei as probed by the Keck interferometer
摘要：
我们正在用Keck干涉仪在近红外波段探测活动星系核的内部区域。添加到以前研究的四个目标，我们报告测量的K波段（2.2微米）vibrium的四个目标，即AKN 120，IC 4329 A，Mrk 6，和无线电响亮的类星体3C 273在z=0.158。所观察到的vibration是相当高的所有目标，我们解释为部分分辨率的尘埃升华区域的指示。由观测到的活动星系核的光度标度近似地导出了活动星系核的有效环半径，其中L是活动星系核的光度。将这些半径与来自独立的光学红外混响测量的半径进行比较，这些数据支持我们先前的主张，即干涉环半径大致等于或略大于混响半径。我们解释这两个半径的比值为一个给定的L作为一个近似的探针的径向分布的内部吸积物质。我们表明，这种内部的径向结构可能是密切相关的中央引擎的无线电响度的初步证据。最后，我们重新观察了最亮的Seyfert 1星系NGC 4151。与我们一年前获得的先前测量结果相比，它在较短的预测基线上的可见度略高，进一步支持了内部结构的部分分辨率。我们没有发现任何显着的变化，隐含的排放量的大小时，K-波段通量的增亮因子为1.5，在一年的时间间隔。
英文摘要：
We are now exploring the inner region of Type 1 active galactic nuclei (AGNs) with the Keck interferometer in the near-infrared. Adding to the four targets previously studied, we report measurements of the K-band (2.2 um) visibilities for four more targets, namely AKN120, IC4329A, Mrk6, and the radio-loud QSO 3C273 at z=0.158. The observed visibilities are quite high for all the targets, which we interpret as an indication of the partial resolution of the dust sublimation region. The effective ring radii derived from the observed visibilities scale approximately with L^1/2, where L is the AGN luminosity. Comparing the radii with those from independent optical-infrared reverberation measurements, these data support our previous claim that the interferometric ring radius is either roughly equal to or slightly larger than the reverberation radius. We interpret the ratio of these two radii for a given L as an approximate probe of the radial distribution of the inner accreting material. We show tentative evidence that this inner radial structure might be closely related to the radio-loudness of the central engine. Finally, we re-observed the brightest Seyfert 1 galaxy NGC4151. Its marginally higher visibility at a shorter projected baseline, compared to our previous measurements obtained one year before, further supports the partial resolution of the inner structure. We did not detect any significant change in the implied emission size when the K-band flux was brightened by a factor of 1.5 over a time interval of one year.
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