z=3.9类星体宿主星系中0.3”分辨率的分子气体成像：APM 08279+5255中的中心亚千秒差距尺度恒星形成储层
Imaging the Molecular Gas in a z=3.9 Quasar Host Galaxy at 0.3" Resolution: A Central, Sub-Kiloparsec Scale Star Formation Reservoir in APM 08279+5255
摘要：
我们利用甚大射电天阵以0.3”分辨率绘制了强透镜高红移类星体APM 08279+5255（z=3.911）的宿主星系中分子气体含量的图。CO（J=1-0）的排放量在我们的地图中清楚地解决。从这些图中得到的CO（J=1-0）线光度与以前的单碟测量结果吻合得很好。与以前的基于干涉仪的研究相比，我们发现，完整的分子气藏位于两个紧凑的峰，相隔<~0.4”。我们的观测结果表明，第一次，从冷分子气体的发射几乎是同空间的光学/近红外连续辐射的中央活动星系核在这个源。这种形态上的惊人相似性表明分子气体位于靠近活动星系核的致密区域。基于高分辨率CO图，我们提出了一个修正的模型，在这个系统中的引力透镜，这表明分子气体排放放大只有4倍（与以前建议的100倍）。这个模型表明，CO位于一个半径约为550 pc的环核盘中，可能以<25度的倾角看到，即，根据CO光度，我们推导出该星系的分子气体质量为M_gas= 1.3 × 10^11 M_sun。由CO的结构和线宽，我们导出了动力学质量M_dyn（sin i）^2= 4.0 × 10^10 M_sun.基于对M_BH= 2.3 × 10^10 M_sun中心黑洞质量的修正估计和分子线研究结果，我们发现APM 08279+5255的恒星核球质量与邻近星系的局部M_BH-sigma_bulge关系相差一个数量级以上，支持最近的建议，这种关系可能会随着宇宙时间的演变和/或朝着高质量端的变化。
英文摘要：
We have mapped the molecular gas content in the host galaxy of the strongly lensed high redshift quasar APM 08279+5255 (z=3.911) with the Very Large Array at 0.3" resolution. The CO(J=1-0) emission is clearly resolved in our maps. The CO(J=1-0) line luminosity derived from these maps is in good agreement with a previous single-dish measurement. In contrast to previous interferometer-based studies, we find that the full molecular gas reservoir is situated in two compact peaks separated by <~0.4". Our observations reveal, for the first time, that the emission from cold molecular gas is virtually cospatial with the optical/near-infrared continuum emission of the central AGN in this source. This striking similarity in morphology indicates that the molecular gas is situated in a compact region close to the AGN. Based on the high resolution CO maps, we present a revised model for the gravitational lensing in this system, which indicates that the molecular gas emission is magnified by only a factor of 4 (in contrast to previously suggested factors of 100). This model suggests that the CO is situated in a circumnuclear disk of ~550 pc radius that is possibly seen at an inclination of <~25 deg, i.e., relatively close to face-on. From the CO luminosity, we derive a molecular gas mass of M_gas=1.3x10^11 M_sun for this galaxy. From the CO structure and linewidth, we derive a dynamical mass of M_dyn(sin i)^2=4.0x10^10 M_sun. Based on a revised mass estimate for the central black hole of M_BH=2.3x10^10 M_sun and the results of our molecular line study, we find that the mass of the stellar bulge of APM 08279+5255 falls short of the local M_BH-sigma_bulge relationship of nearby galaxies by more than an order of magnitude, lending support to recent suggestions that this relation may evolve with cosmic time and/or change toward the high mass end.
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