类星体Q 0151+048的暗物质晕中的Lyα团和Zabs { \approx } zem阻尼Lyα吸收体
A Lyα blob and zabs {\approx} zem damped Lyα absorber in the dark matter halo of the binary quasar Q 0151+048
摘要：
Q 0151 +048是一个物理上的类星体对，z = 1.929，在天空中的距离为3.3角秒。在Q 0151 + 048 A（qA）的光谱中，在较高的红移处观察到DLA。我们以前已经探测到这两个类星体的宿主星系，以及一个Lya斑点。我们进行了低分辨率光谱与扩展发射对齐的狭缝。我们还使用中等分辨率的VLT/X-shooter摄谱仪和与两个类星体对准的狭缝观察了该系统。我们分别从Hβ和Hα发射线测量了系统红移zem（A）=1.92924{ \pm }0.00036和zem（B）=1.92863{ \pm }0.00042。我们估计这两个类星体的黑洞质量分别为10^9.33 M{ \odot }和10^8.38 M{ \odot }。由此，我们推断出两个类星体所在的暗物质晕的质量：qA和qB的质量分别为10^13.74 M{ \odot }和10^13.13 M{ \odot }。我们观察到一个速度梯度沿长轴的Lya斑点一致的旋转曲线的大盘星系，但它也可能是由气体流入或流出。我们检测到残留连续的DLA槽，我们解释为发射从宿主星系的qA。推导出的DLA的H 0柱密度为log NH 0 = 20.34 { \pm } 0.02。金属柱密度导致0.01 Z{ \odot }的总金属度。我们检测CII*，这使我们能够制作DLA云的物理模型。从类星体的系统红移，我们得出结论，Lya斑点是与qA，而不是与DLA。DLA必须位于Lya斑点和qA的前面，距离大于30 kpc。这两个类星体以正常的爱丁顿比吸积。这个双类星体的DM晕将增长到我们的本地超星系团的质量在z=0。我们指出，这些对象因此形成了一个理想的实验室，以研究我们的本地超星系团的z=2前体的物理相互作用。
英文摘要：
Q0151+048 is a physical QSO pair at z ~ 1.929 with a separation of 3.3 arcsec on the sky. In the spectrum of Q0151+048A (qA), a DLA is observed at a higher redshift. We have previously detected the host galaxies of both QSOs, as well as a Lya blob. We performed low-resolution spectroscopy with the slit aligned with the extended emission. We also observed the system using the medium-resolution VLT/X-shooter spectrograph and the slit aligned with the two QSOs. We measure systemic redshifts of zem(A)=1.92924{\pm}0.00036 and zem(B)=1.92863{\pm}0.00042 from the Hβ and Hα emission lines, respectively. We estimate the masses of the black holes of the two QSOs to be 10^9.33 M{\odot} and 10^8.38 M{\odot} for qA and qB, respectively. From this we infered the mass of the dark matter halos hosting the two QSOs: 10^13.74 M{\odot} and 10^13.13 M{\odot} for qA and qB, respectively. We observe a velocity gradient along the major axis of the Lya blob consistent with the rotation curve of a large disk galaxy, but it may also be caused by gas inflow or outflow. We detect residual continuum in the DLA trough which we interpret as emission from the host galaxy of qA. The derived H0 column density of the DLA is log NH0 = 20.34 {\pm} 0.02. Metal column densities results in an overall metallicity of 0.01 Z{\odot}. We detect CII* which allows us to make a physical model of the DLA cloud. From the systemic redshifts of the QSOs, we conclude that the Lya blob is associated with qA rather than with the DLA. The DLA must be located in front of both the Lya blob and qA at a distance larger than 30 kpc. The two QSOs accrete at normal eddington ratios. The DM halo of this double quasar will grow to the mass of our local super-cluster at z=0. We point out that those objects therefore form an ideal laboratory to study the physical interactions in a z=2 pre-cursor of our local super-cluster.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
