论文标题
使用XMM和Nustar将IGR J18007-4146分类为中级极性
Classifying IGR J18007-4146 as an intermediate polar using XMM and NuSTAR
论文作者
论文摘要
持续的硬X射线调查最近揭示了许多新的和身份不明的银河系来源。其中很大一部分已被证明是称为灾难变量（CVS）的白色矮人的类型。通常需要进行后续观察来对这些来源进行分类和分类，并且还可能确定潜在的独特或有趣的情况。一种情况是IGR J18007-4146，它可能是基于Chandra观察结果和光学/IR目录的约束的CV。利用同时进行XMM-Newton和Nustar观测值以及可用的光学/IR数据，我们确认IGR J18007-4146的性质是中间极性型CV。对XMM数据的定时分析揭示了我们在424.4 +/- 0.7 s处的周期性信号，我们将其解释为白矮人的自旋周期。为0.3-78 keV频谱进行建模，我们使用了热的bremsstrahlung连续体，但需要固有的吸收以及柔软的成分和6和7 keV之间的强Fe线。我们使用具有KT = 73 +8/-6 eV的单个单位黑体对软件进行建模。从X射线频谱中，我们能够测量白矮人的质量为1.06 +0.19/-0.10 msun，这意味着IGR J18007-4146比磁性CV的平均值更大。
Many new and unidentified Galactic sources have recently been revealed by ongoing hard X-ray surveys. A significant fraction of these have been shown to be the type of accreting white dwarfs known as cataclysmic variables (CVs). Follow-up observations are often required to categorize and classify these sources, and may also identify potentially unique or interesting cases. One such case is IGR J18007-4146, which is likely a CV based on follow-up Chandra observations and constraints from optical/IR catalogs. Utilizing simultaneous XMM-Newton and NuSTAR observations, as well as the available optical/IR data, we confirm the nature of IGR J18007-4146 as an intermediate polar type CV. Timing analysis of the XMM data reveals a periodic signal at 424.4 +/- 0.7 s that we interpret as the spin period of the white dwarf. Modeling the 0.3-78 keV spectrum, we use a thermal bremsstrahlung continuum but require intrinsic absorption as well as a soft component and strong Fe lines between 6 and 7 keV. We model the soft component using a single-temperature blackbody with kT = 73 +8/-6 eV. From the X-ray spectrum, we are able to measure the mass of the white dwarf to be 1.06 +0.19/-0.10 Msun, which means IGR J18007-4146 is more massive than the average for magnetic CVs.
