SUZAKU VIEW OF THE SWIFT/BAT ACTIVE GALACTIC NUCLEI. III. APPLICATION OF NUMERICAL TORUS MODELS TO TWO NEARLY COMPTON THICK ACTIVE GALACTIC NUCLEI (NGC 612 AND NGC 3081)
SUZAKU VIEW OF THE SWIFT/BAT ACTIVE GALACTIC NUCLEI. III. APPLICATION OF NUMERICAL TORUS MODELS TO TWO NEARLY COMPTON THICK ACTIVE GALACTIC NUCLEI (NGC 612 AND NGC 3081)
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DOI：
10.1088/0004-637x/729/1/31
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发表时间：
2010-12
期刊：
影响因子：
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通讯作者：
S. Eguchi;Y. Ueda;H. Awaki;J. Aird;Y. Terashima;R. Mushotzky
中科院分区：
文献类型：
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作者：
S. Eguchi;Y. Ueda;H. Awaki;J. Aird;Y. Terashima;R. Mushotzky
研究了由Suzaku后续观测获得的两个SWIFT/BAT活动星系核(AGN)的宽带光谱：NGC612和NGC3081。通过与标准模型的拟合，我们发现这两个光源都具有相似的光谱特征，在NH≃10 2 4 cm−2处有强吸收，散射光的分数为FSCAT=0.5%~0.8%，反射分量的立体角为Ω/2π=0.4~1.1。为了研究环面的几何形状，我们使用了池田等人的蒙特卡罗模拟的数值光谱模型。到铃鹿的光谱。我们发现这个有四个几何参数的环面模型很好地解释了我们的数据。拟合结果表明，NGC612的环面半开口角为≃60°-70°，在有少量散射气体的情况下是从接近侧面的角度观察到的，而NGC3081的开口角很小，为≃15°，更像是Ueda等人发现的深埋在地下的“新型”活动星系核。我们展示了将这种数值模拟直接应用于高质量的宽带光谱以揭示活动星系核的内部结构的潜在力量。
The broadband spectra of two Swift/BAT active galactic nuclei (AGNs) obtained from Suzaku follow-up observations are studied: NGC 612 and NGC 3081. Fitting with standard models, we find that both sources show similar spectra characterized by heavy absorption with NH ≃ 1024 cm−2, and the fraction of scattered light is fscat = 0.5%–0.8%, and the solid angle of the reflection component is Ω/2π = 0.4–1.1. To investigate the geometry of the torus, we apply numerical spectral models utilizing Monte Carlo simulations by Ikeda et al. to the Suzaku spectra. We find that our data are well explained by this torus model, which has four geometrical parameters. The fit results suggest that NGC 612 has a torus half-opening angle of ≃60°–70° and is observed from a nearly edge-on angle with a small amount of scattering gas, while NGC 3081 has a very small opening angle of ≃15° and is observed on a face-on geometry, more like the deeply buried “new type” AGNs found by Ueda et al. We demonstrate the potential power of direct application of such numerical simulations to high-quality broadband spectra to unveil the inner structure of AGNs.