论文标题
Alma 200 PC的Z〜7类星体成像揭示了一个紧凑的，磁盘状的宿主星系
ALMA 200 pc imaging of a z~7 quasar reveals a compact, disk-like host galaxy
论文作者
论文摘要
我们提出了158 UM [CII]线和Z的潜在灰尘连续体的0“ .035分辨率（〜200 PC）成像，Z = 6.9 Quasar J234833.34-305410.0。18 H Alma观察值表明，非常紧凑的发射（直径〜1 kpc）与简单的face-face-face-face-face-face-faction-faction-factiation-foct-faction-factiation-foction-face-face-sot-coltation-coltation-coltation-coltation-coltation-coltation-sot-sot-sot。 〜160 km/s的分散量仅为4x10^9 m_sun，大约要高于中央超级黑洞的一个。在整个磁盘中，几乎没有恒星和/或暗物质的质量贡献。 M_SUN / YR / KPC^2仍然可以用某些假设的恒星形成的Eddington限制来解释，但也可能暗示中央超级质量黑洞有助于中央110 PC中的灰尘加热。
We present 0".035 resolution (~200 pc) imaging of the 158 um [CII] line and the underlying dust continuum of the z=6.9 quasar J234833.34-305410.0. The 18 h ALMA observations reveal extremely compact emission (diameter ~1 kpc) that is consistent with a simple, almost face-on, rotation-supported disk with a significant velocity dispersion of ~160 km/s. The gas mass in just the central 200 pc is ~4x10^9 M_sun, about a factor two higher than that of the central supermassive black hole. Consequently we do not resolve the black hole's sphere of influence, and find no kinematic signature of the central supermassive black hole. Kinematic modeling of the [CII] line shows that the dynamical mass at large radii is consistent with the gas mass, leaving little room for a significant mass contribution by stars and/or dark matter. The Toomre-Q parameter is less than unity throughout the disk, and thus is conducive to star formation, consistent with the high infrared luminosity of the system. The dust in the central region is optically thick, at a temperature >132 K. Using standard scaling relations of dust heating by star formation, this implies an unprecedented high star formation rate density of >10^4 M_sun / yr / kpc^2. Such a high number can still be explained with the Eddington limit for star formation under certain assumptions, but could also imply that the central supermassive black hole contributes to the heating of the dust in the central 110 pc.
