BeppoSAX observations of Seyfert 1s in the Piccinotti sample I. poorly studied sources
BeppoSAX observations of Seyfert 1s in the Piccinotti sample I. poorly studied sources
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Piccinotti 样本中 Seyfert 1 的 BeppoSAX 观察结果 I. 研究不足的来源
DOI：
10.1051/0004-6361:20031466
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发表时间：
2003
期刊：
影响因子：
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通讯作者：
G. Malaguti
中科院分区：
文献类型：
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作者：
A. Quadrelli;A. Malizia;L. Bassani;G. Malaguti
在这项工作中，我们提出了两篇论文的第一个专门研究的X射线光谱特征的塞弗特1星系的Piccinotti样本。特别是，我们在这里分析BeppoSAX宽带（0.1-100千电子伏）数据的4个对象，尽管他们的X射线亮度，一直以来很少研究，由于他们的后期识别活动星系核;这些是H 0111 -149（MKN 1152）、H 0235 -525（ESO 198-G24）、H 0557 -385（IRAS F05563-3820）和H1846-786（IRAS F18389-7834）。我们假设所有的源都有一个基线模型，其中包括一个指数截止的幂律加上一个反射分量和一个铁Kα线;我们还搜索了本征吸收和/或软过剩分量的存在。我们的分析表明，在两个对象（H 0557 -385和H 0111 -149）的复杂吸收的存在下，最好由两个均匀的吸收体，一个冷，一个暖的组合来描述。仅在一个源H 0557 -385中测量到软过量分量。主连续谱最好用正则幂律（Γ= 1.7−2）来描述，截止能量在40-130 keV之间。冷反射分量可能存在于所有光源中，其值范围从小于0.6到大于2。在4个物体中的3个中，我们发现了具有典型的Seyfert 1 s（100-200 eV）的等效宽度的冷铁线。
In this work we present the first of two papers devoted to the study of the X-ray spectral characteristics of Seyfert 1 galaxies in the Piccinotti sample. In particular we analyse here the BeppoSAX broad band (0.1-100 keV) data of 4 objects which, despite their X-ray brightness, have been historically poorly studied due to their late identification with an AGN; these are H0111-149 (MKN 1152), H0235-525 (ESO 198-G24), H0557-385 (IRAS F05563-3820) and H1846-786 (IRAS F18389-7834). We have assumed for all the sources a baseline model which includes a power law with an exponential cut-off plus a reflection component and an iron Kα line; we have also searched for the presence of intrinsic absorption and/or a soft excess component. Our analysis indicates the presence of complex absorption in two objects (H0557-385 and H0111-149) best described by a combination of two uniform absorbers, one cold and one warm. Only in one source, H0557-385, a soft excess component has been measured. The primary continuum is best described by a canonical power law ( Γ= 1.7−2) with a high energy cut-off in the range 40-130 keV. A cold reflection component is likely present in all sources with values ranging from less than 0.6 to higher than 2. In 3 out of 4 objects we find a cold iron line having equivalent width typical of Seyfert 1s (100-200 eV).