论文标题
由核棒驱动的大量分子流入式的ESO 320-G030中的原始折叠物
A proto-pseudobulge in ESO 320-G030 fed by a massive molecular inflow driven by a nuclear bar
论文作者
论文摘要
据信具有核条的星系有效地向内驱动气体，产生核星爆，可能是活跃的银河核（AGN）。我们基于对Herschel和Alma光谱观测的分析，确认了孤立的，双键，发光的红外星系320-G030的情况。 ESO 320-G030的Herschel/PAC和尖峰观测显示，在18条H2O中的吸收/发射，我们将其与Alma H2O 423-330 448 GHz系（Eupper〜400 K）和连续图像结合使用，并研究核区域。辐射转移模型表明，需要3个核成分以说明H2O和连续数据。带有r〜130-150 pc的信封，t_dust〜50 k和n_h2〜2x10^{23} cm^{ - 2}，围绕着带有r〜40 pc和tau_100um 〜1.5-3（n_h2〜2x10^{24} cm^{24} cm^{ - 2}的核盘，以及一个非常极端的（n_h2〜2x10^{2x10^{2x10^{2 x），以及一个非常极端的（〜12 PCACT）（〜 （tau_100um> 5，n_h2> 〜5x10^{24} cm^{ - 2}）核心组件。三个核成分占星系L_IR的70％（SFR〜16-18 MSUN YR^{ - 1}）。核是由与核棒有关的ALMA中CO 2-1观察到的分子流入式的。随着半径降低（r = 450-225 PC），质量流入率最高为〜20 msun yr^{ - 1}，这与核SFR相似，表明Starburst由流入量持续。在较低的r处，远红外OH地面双线会最好探测流入，估计流入率为〜30 msun yr^{ - 1}。核气补充的短时间尺寸约为20 MYR，表明了世俗的进化，并表明我们目睹了由强大的核棒驱动的大量流入剂中的中间阶段（<100 MYR）的原始质量。我们还将H2O模型应用于H2^{18} o，哦，$^{18}的Herschel Far-Infrared光谱观察结果
Galaxies with nuclear bars are believed to efficiently drive gas inward, generating a nuclear starburst and possibly an active galactic nucleus (AGN). We confirm this scenario for the isolated, double-barred, luminous infrared galaxy ESO 320-G030 based on an analysis of Herschel and ALMA spectroscopic observations. Herschel/PACS and SPIRE observations of ESO 320-G030 show absorption/emission in 18 lines of H2O, which we combine with the ALMA H2O 423-330 448 GHz line (Eupper~400 K) and continuum images to study the nuclear region. Radiative transfer models indicate that 3 nuclear components are required to account for the H2O and continuum data. An envelope, with R~130-150 pc, T_dust~50 K, and N_H2~2x10^{23} cm^{-2}, surrounds a nuclear disk with R~40 pc and tau_100um~1.5-3 (N_H2~2x10^{24} cm^{-2}) and an extremely compact (R~12 pc), warm (~100 K), and buried (tau_100um>5, N_H2>~5x10^{24} cm^{-2}) core component. The three nuclear components account for 70% of the galaxy L_IR (SFR~16-18 Msun yr^{-1}). The nucleus is fed by a molecular inflow observed in CO 2-1 with ALMA, which is associated with the nuclear bar. With decreasing radius (r=450-225 pc), the mass inflow rate increases up to ~20 Msun yr^{-1}, which is similar to the nuclear SFR, indicating that the starburst is sustained by the inflow. At lower r, the inflow is best probed by the far-infrared OH ground-state doublets, with an estimated inflow rate of ~30 Msun yr^{-1}. The short timescale of ~20 Myr for nuclear gas replenishment indicates quick secular evolution, and indicates that we are witnessing an intermediate stage (<100 Myr) proto-pseudobulge fed by a massive inflow that is driven by a strong nuclear bar. We also apply the H2O model to the Herschel far-infrared spectroscopic observations of H2^{18}O, OH, $^{18}OH, OH+, H2O^+, H3O^+, NH, NH2, NH3, CH, CH^+, ^{13}CH^+, HF, SH, and C3, and estimate their abundances.
