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首页> 外文期刊>The Astrophysical journal >PROBING THE DUST OBSCURATION IN SEYFERT GALAXIES USING INFRARED SPECTROSCOPY
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PROBING THE DUST OBSCURATION IN SEYFERT GALAXIES USING INFRARED SPECTROSCOPY

机译：红外光谱法研究塞弗特星系中的尘埃残留

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We present near-infrared spectroscopy of four Seyfert 1 galaxies, one Seyfert 1.9 galaxy, and one Seyfert 2 galaxy, obtained using the Gemini infrared camera at the Lick Observatory 3 m Shane telescope. With the unique design of the Gemini camera, full J- and K-band spectra were taken simultaneously through the same slit. This produced a more accurate comparison of hydrogen recombination line fluxes than previous infrared studies. We have also used template galaxies to remove stellar features from the infrared spectra and produced more accurate measurements of the weak Brγ feature. We concentrate on the velocity-resolved ratio of Paβ/Brγ and its implication for dust within the central active galactic nucleus (AGN). For our Seyfert 1s, the line ratios of Paβ/Brγ are not only comparable in both broad- and narrow-line regions but also consistent with case B recombination, confirming that the ratio Paβ/Brγ is less affected by collisional effects than optical lines and is a good indicator of dust extinction up to A_v ～ 10 in AGN. Using the same diagnostic the Seyfert 1.9 galaxy, NGC 2992, has an extinction of A_v = 4.03 ± 0.20 to the broad-line region while the narrow-line region is unobscured. Assuming that Seyfert 1.9 galaxy has the same broad-line region that Seyfert 1 galaxies have, we conclude that the obscuring dust is located between the broad-line regions and the narrow-line regions, consistent with the AGN unification model. The Seyfert 2 galaxy, NGC 5929, consistent with dust being present on larger scales, shows significant obscuration to the narrow-line region. These data are part of a larger program to measure many spectral properties of Seyfert galaxies.
机译：我们介绍了使用塞米特天文台3 m Shane望远镜的双子座红外摄像机获得的四个塞弗特1星系，一个塞弗特1.9星系和一个塞弗特2星系的近红外光谱。采用双子座相机的独特设计，可以通过同一条缝隙同时拍摄全J和K波段光谱。与以前的红外研究相比，这产生了氢重组线通量的更准确的比较。我们还使用模板星系从红外光谱中删除了恒星特征，并对弱Brγ特征进行了更准确的测量。我们专注于Paβ/Brγ的速度分辨比及其对中央活动银河核（AGN）中尘埃的影响。对于我们的Seyfert 1s，Paβ/Brγ的线比不仅在宽线和窄线区域都可比，而且与情况B的重组一致，这证实了Paβ/Brγ的比线受光学效应和碰撞的影响较小。是AGN中高达A_v〜10的粉尘消灭的良好指标。使用相同的诊断程序，塞弗特1.9星系NGC 2992对宽线区域的消光度为A_v = 4.03±0.20，而对窄线区域的消光度则未被遮挡。假设塞弗特1.9星系与塞弗特1星系具有相同的宽线区域，我们得出的结论是，模糊尘埃位于宽线区域和窄线区域之间，与AGN统一模型一致。 Seyfert 2星系，NGC 5929，与大范围存在的尘埃一致，显示出对窄线区域的明显遮盖。这些数据是一个较大的程序的一部分，该程序可以测量塞弗特星系的许多光谱特性。

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