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Linking the small-scale relativistic winds and the large-scale molecular outflows in the z = 1.51 lensed quasar HS 0810+2554
Monthly Notices of the Royal Astronomical Society ( IF 4.7 ) Pub Date : 2020-04-03 , DOI: 10.1093/mnras/staa1534
G Chartas 1 , E Davidson 1 , M Brusa 2, 3 , C Vignali 2, 3 , M Cappi 3 , M Dadina 3 , G Cresci 4 , R Paladino 5 , G Lanzuisi 3 , A Comastri 3
Affiliation  

We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the quadruply lensed z=1.51 quasar HS 0810+2554 which provide useful insight on the kinematics and morphology of the CO molecular gas and the ~2 mm continuum emission in the quasar host galaxy. Lens modeling of the mm-continuum and the spectrally integrated CO(3-2) images indicates that the source of the mm-continuum has an eccentricity of e~0.9 with a size of ~1.6 kpc and the source of line emission has an eccentricity of e~0.7 with a size of ~1 kpc. The spatially integrated emission of the CO(2-1) and CO(3-2) lines shows a triple peak structure with the outer peaks separated by Dv_21 = 220 +\- 19 km s^-1 and Dv_32 = 245 +/- 28 km s^-1, respectively, suggesting the presence of rotating molecular CO line emitting gas. Lensing inversion of the high spatial resolution images confirms the presence of rotation of the line emitting gas. Assuming a conversion factor of alpha_CO = 0.8 M_solar (K km s^-1 pc^2)^-1 we find the molecular gas mass of HS 0810+2554 to be M _ Mol = [(5.2 +/- 1.5)/mu_32] x10^10 M_solar, where mu_32 is the magnification of the CO(3-2) emission. We report the possible detection, at the 3.0 - 4.7 sigma confidence level, of shifted CO(3-2) emission lines of high-velocity clumps of CO emission with velocities up to 1702 km s^-1. We find that the momentum boost of the large scale molecular wind is below the value predicted for an energy-conserving outflow given the momentum flux observed in the small scale ultrafast outflow.

中文翻译:

将 z = 1.51 透镜类星体 HS 0810+2554 中的小尺度相对论风和大尺度分子外流联系起来

我们展示了四重透镜 z=1.51 类星体 HS 0810+2554 的阿塔卡马大型毫米/亚毫米阵列 (ALMA) 观测结果,它提供了对 CO 分子气体的运动学和形态以及类星体宿主星系中~2 mm 连续发射的有用见解. 毫米连续谱和光谱积分 CO(3-2) 图像的透镜建模表明,毫米连续谱源的偏心率为 e~0.9,尺寸为~1.6 kpc,线发射源具有偏心率e~0.7,大小为~1 kpc。CO(2-1) 和 CO(3-2) 线的空间积分发射显示出三峰结构,外峰由 Dv_21 = 220 +/- 19 km s^-1 和 Dv_32 = 245 +/- 隔开分别为 28 km s^-1,表明存在旋转分子 CO 线排放气体。高空间分辨率图像的透镜反演证实了线发射气体旋转的存在。假设转换因子 alpha_CO = 0.8 M_solar (K km s^-1 pc^2)^-1 我们发现 HS 0810+2554 的分子气体质量为 M _ Mol = [(5.2 +/- 1.5)/mu_32 ] x10^10 M_solar,其中 mu_32 是 CO(3-2) 发射的放大倍数。我们报告了在 3.0 - 4.7 sigma 置信度水平下可能检测到高速 CO 排放团块的移动 CO(3-2) 排放线,其速度高达 1702 km s^-1。我们发现,鉴于在小尺度超快流出中观察到的动量通量,大规模分子风的动量提升低于能量守恒流出的预测值。8 M_solar (K km s^-1 pc^2)^-1 我们发现 HS 0810+2554 的分子气体质量为 M _ Mol = [(5.2 +/- 1.5)/mu_32] x10^10 M_solar,其中mu_32 是 CO(3-2) 发射的放大倍数。我们报告了在 3.0 - 4.7 sigma 置信度水平下可能检测到高速 CO 排放团块的移动 CO(3-2) 排放线,其速度高达 1702 km s^-1。我们发现,鉴于在小尺度超快流出中观察到的动量通量,大规模分子风的动量提升低于能量守恒流出的预测值。8 M_solar (K km s^-1 pc^2)^-1 我们发现 HS 0810+2554 的分子气体质量为 M _ Mol = [(5.2 +/- 1.5)/mu_32] x10^10 M_solar,其中mu_32 是 CO(3-2) 发射的放大倍数。我们报告了在 3.0 - 4.7 sigma 置信度水平下可能检测到高速 CO 排放团块的移动 CO(3-2) 排放线,其速度高达 1702 km s^-1。我们发现,鉴于在小尺度超快流出中观察到的动量通量,大规模分子风的动量提升低于能量守恒流出的预测值。速度高达 1702 km s^-1 的高速 CO 排放块的移动 CO(3-2) 排放线。我们发现,鉴于在小尺度超快流出中观察到的动量通量,大规模分子风的动量提升低于能量守恒流出的预测值。速度高达 1702 km s^-1 的高速 CO 排放块的移动 CO(3-2) 排放线。我们发现,鉴于在小尺度超快流出中观察到的动量通量,大规模分子风的动量提升低于能量守恒流出的预测值。
更新日期:2020-04-03
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