SINFONI adaptive optics integral field spectroscopy of the Circinus Galaxy
SINFONI adaptive optics integral field spectroscopy of the Circinus Galaxy
复制标题
圆规座星系的 SINFONI 自适应光学积分场光谱
DOI：
10.1051/0004-6361:20054387
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发表时间：
2006
影响因子：
6.5
通讯作者：
A. Sternberg
中科院分区：
文献类型：
--
作者：
F. Sanchez;R. Davies;F. Eisenhauer;L. Tacconi;R. Genzel;A. Sternberg
目标。我们在几个秒差距的尺度上研究了环星系核心的恒星形成活动和气体和恒星动力学。方法。利用VLT上的自适应光学近红外积分场光谱仪SINFONI，我们在几个秒差距的尺度上以70 km s−1 FWHM的光谱分辨率获得了环座星系的观测结果。利用从SINFONI数据立方中提取的线形图和速度图分析了核的物理性质。星暴模型使用Brγ通量、恒星连续体（通过CO吸收带向2.3 μ m追踪）和射电连续体进行约束。结果。H2 - 0S(1) 2.12µma和Brγ 2.17µm谱线的形态与恒星连续体的相似性以及它们的运动学表明它们在恒星形成过程中有共同的起源。在AGN的8%范围内，我们发现在最近的100 Myr中，最近发生了一次星暴，目前占银河系放热光度的1.4%。恒星和气体存在的空间尺度的相似性表明，这种恒星形成发生在环体内；通过环面的气柱密度与恒星的最大可能光学深度的比较表明，环面是一种块状介质。日冕线呈现不对称轮廓，空间紧凑的窄成分和空间扩展的蓝色翼。这些特征与一些被引力束缚在AGN上的云所产生的辐射，以及一些从被束缚的云所侵蚀的云所流出的辐射是一致的。
Aims. We investigate the star formation activity and the gas and stellar dynamics on scales of a few parsecs in the nucleus of the Circinus Galaxy. Methods. Using the adaptive optics near infrared integral field spectrometer SINFONI on the VLT, we have obtained observations of the Circinus galaxy on scales of a few parsecs and at a spectral resolution of 70 km s −1 FWHM. The physical properties of the nucleus are analyzed by means of line and velocity maps extracted from the SINFONI datacube. Starburst models are constrained using the Brγ flux, stellar continuum (as traced via the CO absorption bandheads longward of 2.3 µm), and radio continuum. Results. The similarity of the morphologies of the H2 1−0S (1) 2.12 µ ma nd Brγ 2.17 µm lines to the stellar continuum and also their kinematics, suggest a common origin in star formation. Within 8 pc of the AGN we find there has been a recent starburst in the last 100 Myr, which currently accounts for 1.4% of the galaxy’s bolometric luminosity. The similarity of the spatial scales over which the stars and gas exist indicates that this star formation is occuring within the torus; and comparison of the gas column density through the torus to the maximum possible optical depth to the stars implies the torus is a clumpy medium. The coronal lines show asymmetric profiles with a spatially compact narrow component and a spatially extended blue wing. These characteristics are consistent with some of the emission arising in clouds gravitationally bound to the AGN, and some outflowing in cloudlets which have been eroded away from the bound clouds.