对IBL和LBL天体的快速观测
Swift observations of IBL and LBL objects
摘要：
BL Lac是一类神秘的活动星系核（AGN），其特征是典型的同步辐射和逆康普顿辐射的非热连续性。根据这些分量的最大值的频率位置，它们被细分为三个子类LBL、IBL和HBL。我们提出了一组的观测结果的8 BL Lac对象的LBL和IBL型的XRT和UVOT探测器船上的斯威夫特卫星在2005年1月和2006年11月之间进行。我们主要感兴趣的是测量光谱参数，特别是UV和X射线波段之间的陡度，这对确定这些源的分类很有用。我们将这些源的行为与以前的XMM-牛顿，BeppoSAX观测以及X射线和光学波段的历史数据进行了比较。我们也有兴趣在我们的样本的基础上进行分类的观察和比较，他们在文献中提出的分类来源。我们进行了X射线光谱分析所观察到的BL Lac对象使用一个简单的幂律，并在少数情况下的对数抛物线模型。我们还结合了紫外辐射与低能X射线数据，我们使用观测数据来分类源在我们的样本和推导出的光谱能量分布参数。我们发现，对于IBLs的X射线低状态显示的高能量分量的功能，通常被解释为由于逆康普顿发射。在我们的样本中的源表现出一系列的时间UV和X射线行为，一些对象具有清晰和整洁的相关UV和X射线的变化（例如ON 231）和其他对象显示没有明确的（例如AO 0235+164）UV和X射线的相关性。最后，我们还注意到，我们的估计光谱曲率的范围内的HBLs测量。
英文摘要：
BL Lacs are an enigmatic class of active galactic nuclei (AGNs), characterized by the non-thermal continuum typically attributed to synchrotron and inverse Compton emission. Depending on the frequency location of the maxima of these components, they are subdivided into three subclasses LBLs, IBLs, and HBLs. We present the results of a set of observations of eight BL Lac objects of LBL and IBL type performed by the XRT and UVOT detectors onboard the Swift satellite between January 2005 and November 2006. We are mainly interested in measuring the spectral parameters, and particularly the steepness between the UV and the X-ray band, useful for determining the classification of these sources. We compare the behavior of these sources with previous XMM-Newton, BeppoSAX obser- vations and with historical data in the X-ray and in the optical band. We are also interested in classifying the sources in our sample on the basis of the observations and comparing them with their classification presented in literature. We performed X-ray spectral analysis of observed BL Lac objects using a simple powerlaw and in a few cases the log-parabolic model. We also combined the UV emission with the low energy X-ray data to We used observational data to classify sources in our sample and derived parameters of their spectral energy distribution. We found that for the IBLs X-rays low states show features of the high energy component, usually interpreted as due to inverse Compton emission. Sources in our sample exhibit a range of temporal UV and X-ray behaviors, some objects having clear and neat correlated UV and X-ray variations (e.g. ON231) and other objects showing no clear (e.g. AO 0235+164) UV and X-ray correlation. Finally, we also note that our estimates of spectral curvature are in the range of that measured for the HBLs.
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