论文标题
$ herschel $/pacs OH Seyfert，Liner和Starburst星系的光谱
$Herschel$/PACS OH Spectroscopy of Seyfert, LINER, and Starburst Galaxies
论文作者
论文摘要
我们研究了65美元$ $ m，71 $μ$ m，79 $ $ m，84 $ $ m，119美元$ $ m，163 $μ$ m oh oh oh oh oh oh doubles of 178 local（0 <$ z $ <0.35）星系。使用$ Herschel $/PACS光谱仪观察到它们，包括Seyfert星系，衬里和形成星系的星系。我们仅在吸收（OH71）中观察到这些双线，主要是吸收（OH65，OH84），主要是在发射中（OH79），仅在发射（OH163）中，甚至大约是两者的混合物（OH119）。在19个星系中，我们在OH Doublets中找到了P-Cygni或反向P-Cygni线轮廓。我们使用几个星系可观测物来探测光谱分类，中央AGN/Starburst组件的亮度和辐射场强度。我们发现OH79，OH119和OH163更有可能显示出明亮，无镜的AGN的强劲发射。对于较不发光的，遮盖的AGN和非活性星系，我们发现吸收强的群体（OH119），发射较弱（OH163）以及弱发射和弱吸收（OH79）的混合物。对于OH65，OH71和OH84，我们发现与上面列出的观察物没有显着相关性。我们确实发现OH79和OH119之间的关系与9.7 $ $ M硅酸盐的特征和Balmer减少尘埃灭绝示踪剂，其中更多的灰尘会导致发射较弱 /吸收较强。讨论了观察到的OH双峰的发射起源，无论是从碰撞激发还是来自红外光子的辐射泵送。
We investigated the 65$μ$m, 71$μ$m, 79$μ$m, 84$μ$m, 119$μ$m, and 163$μ$m OH doublets of 178 local (0 < $z$ < 0.35) galaxies. They were observed using the $Herschel$/PACS spectrometer, including Seyfert galaxies, LINERs, and star-forming galaxies. We observe these doublets exclusively in absorption (OH71), primarily in absorption (OH65, OH84), mostly in emission (OH79), only in emission (OH163) and an approximately even mix of the both (OH119). In 19 galaxies we find P-Cygni or reverse P-Cygni line profiles in the OH doublets. We use several galaxy observables to probe spectral classification, brightness of a central AGN/starburst component, and radiation field strength. We find that OH79, OH119, and OH163 are more likely to display strong emission for bright, unobscured AGN. For less luminous, obscured AGN and non-active galaxies, we find populations of strong absorption (OH119), weaker emission (OH163), and a mix of weak emission and weak absorption (OH79). For OH65, OH71 and OH84, we do not find significant correlations with the observables listed above. We do find relationships between OH79 and OH119 with both the 9.7$μ$m silicate feature and Balmer decrement dust extinction tracers in which more dust leads to weaker emission / stronger absorption. The origin of emission for the observed OH doublets, whether from collisional excitation, or from radiative pumping by infrared photons, is discussed.
