论文标题
h $ _ {2} $ s在附近发光星系和ulirg mrk〜231中的顶点和诺玛的观察结果 - 密集气体性能与分子流出之间是否存在关系？
APEX and NOEMA observations of H$_{2}$S in nearby luminous galaxies and the ULIRG Mrk~231 -- Is there a relation between dense gas properties and molecular outflows?
论文作者
论文摘要
为了理解活性银河核（AGN）和恒星形成的进化和反馈，使用分子线作为物理条件和化学的探针很重要。我们使用H $ _ {2} $ S来研究发光和AGN活性对发光红外星系中分子星际介质化学的影响。使用Apex单盘望远镜，我们已经观察到$ 1_ {10} $ - $ 1_ {01} $ Ortho-H $ _ {2} $ S的过渡到168 GHz，向附近十二个发光的发光式高红外星系中心。我们还观察到与NOEMA干涉仪的超发光红外星系（ULIRG）MRK 〜231相同的线。我们已经检测到h $ _ {2} $ s to NGC〜253，NGC〜1068，NGC〜3256，NGC〜4418，NGC〜4826，NGC〜4945，Circinus，M〜83和MRK〜231。四个星系显示升高的H $ _ {2} $ s发射相对于HCN。我们建议高线比是由浓密气体中的h $ _ {2} $ s丰度引起的。但是，我们没有发现h $ _ {2} $ s/hcn线强度比与样品星系中分子流出的存在（或速度）之间的任何明确联系。因此，h $ _ {2} $ s的丰度似乎并未受到大规模外流的影响。我们讨论了建议的H $ _ {2} $ s丰度增强的可能机制，NGC〜4418，Circinus，NGC〜3256和NGC〜4826。这些包括辐射过程（例如X射线或宇宙射线）或较小的比例冲击。我们建议$ l _ {\ mathrm {h_ {2} s}}} $用作密集气体含量的示踪剂，类似于$ l _ {\ mathrm {hcn}} $，并且相关性是$ l _ {\ mathrm {\ mathrm {流出} $（h $ _2 $）意味着密集的气体储层与分子反馈的属性和演变之间的关系。这种潜在的联系需要进一步的研究，因为它对我们了解分子流出的性质与宿主星系的特性有重要的关键。
In order to understand the evolution and feedback of Active Galactic Nuclei (AGN) and star formation it is important to use molecular lines as probes of physical conditions and chemistry. We use H$_{2}$S to investigate the impact of starburst and AGN activity on the chemistry of the molecular interstellar medium in luminous infrared galaxies. Using the APEX single dish telescope, we have observed the $1_{10}$--$1_{01}$ transition of ortho-H$_{2}$S at 168 GHz towards the centres of twelve nearby luminous infrared galaxies. We have also observed the same line towards the ultra luminous infrared galaxy (ULIRG) Mrk~231 with the NOEMA interferometer. We have detected H$_{2}$S towards NGC~253, NGC~1068, NGC~3256, NGC~4418, NGC~4826, NGC~4945, Circinus, M~83 and Mrk~231. Four galaxies show elevated H$_{2}$S emission relative to HCN. We suggest that the high line ratios are caused by elevated H$_{2}$S abundances in the dense gas. However, we do not find any clear connection between the H$_{2}$S/HCN line intensity ratio, and the presence (or speed) of molecular outflows in the sample galaxies. Therefore H$_{2}$S abundances do not seem to be globally affected by the large-scale outflows. We discuss possible mechanisms behind the suggested H$_{2}$S abundance enhancements in NGC~4418, Circinus, NGC~3256 and NGC~4826. These include radiative processes (for example X-rays or cosmic-rays) or smaller scale shocks. We suggest that $L_{\mathrm{H_{2}S}}$ serves as a tracer of the dense gas content, similar to $L_{\mathrm{HCN}}$, and that the correlation between $L_{\mathrm{H_{2}S}}$ and $M_{\rm outflow}$(H$_2$) implies a relation between the dense gas reservoir and the properties and evolution of the molecular feedback. This potential link requires further study since it holds important keys to our understanding of how the properties of molecular outflows relate to that of their host galaxies.
