论文标题
早期宇宙中的蚀刻玻璃：在z = 4.7处的QSO-SMG对中的发光HF和水发射
Etching glass in the early Universe: Luminous HF and water emission in a QSO-SMG pair at z=4.7
论文作者
论文摘要
（删节）我们提出了氟化氢，HF J = 1-0，H20（220-211）的ALMA观察结果，以及Z = 4.7 System BR1202-0725的1.2 THz REST-FRAME连续发射。 BR1202-0725是一个由QSO，次毫米星系（SMG）和两个Ly-Alpha发射器组成的星系组。我们检测到QSO发射的HF，并可能在SMG中吸收，而在QSO和SMG的发射中都检测到水。 QSO是尚未发现的最具发光的HF发射极，其比率与红外发射线相同，与局部AGN和猎户座棒的样本相同。这种一致性涵盖了大约10个红外光度的魔力顺序，l_ir。基于猎户座棒中HF发射研究的结论和建模，QSO中的HF发射是通过与电子和H2的碰撞在分子等离子体中被AGN和强烈恒星形成所辐射的分子等离子体中的激发，或者通过与H2碰撞的碰撞，与H2碰撞，与电子的贡献，对电子的贡献，在一个相对高度的温度（〜120 k），〜120 k），〜120^n eforns中。尽管HF应该是分子流出的出色示踪剂，但我们找不到QSO或SMG中HF流出的有力证据。从SMG中HF中的推定吸收特征，我们估计流出速率的上限DM/DT_OUTFLOW <〜45 m_sun/yr。 SMG的流出率与恒星形成率的比率<5％。 SMG中H2O系的宽度FWHM〜1020 km/s可能表明，要么大尺度上的气体（> 4 kpc）在相互作用和与集体的其他成员相互作用或质量交流的情况下，要么与强烈恒星形成的能量的耗散或两者相互交流，因此更加受到干扰和湍流。任何一个来源中缺乏明显的分子流出可能意味着在其ISM中消散了强烈的恒星形成和AGN活性的大部分能量。
(abridged) We present ALMA observations of hydrogen fluoride, HF J=1-0, H20 (220-211), and the 1.2 THz rest-frame continuum emission from the z=4.7 system BR1202-0725. BR1202-0725 is a galaxy group consisting of a QSO, a sub-millimeter galaxy (SMG), and two Ly-alpha emitters. We detected HF in emission in the QSO and possibly in absorption in the SMG, while water is detected in emission in both the QSO and SMG. The QSO is the most luminous HF emitter yet found and has the same ratio of HF emission line to infrared luminosity as a sample of local AGN and the Orion Bar. This consistency covers about 10 orders-of-magnitude in infrared luminosity, L_IR. Based on the conclusions of a study of HF emission in the Orion Bar and modeling, the HF emission in the QSO is either excited by collisions with electrons and H2 in molecular plasmas irradiated by the AGN and intense star formation or predominately by collisions with H2, with a modest contribution from electrons, in a relatively high temperature (~120 K), dense (~10^5 cm^-3) medium. Although HF should be an excellent tracer of molecular outflows, we do not find strong evidence for outflows in HF in either the QSO or the SMG. From a putative absorption feature in HF in the SMG, we estimate an upper limit on the outflow rate, dM/dt_outflow <~45 M_sun/yr. The ratio of the outflow rate to the star formation rate is <5% for the SMG. The broadness of the H2O line in the SMG, FWHM~1020 km/s, may suggest that either the gas on large scales (>4 kpc) is significantly more disturbed and turbulent due either to interactions and mass exchange with the other members of the group or to the dissipation of the energy of the intense star formation or both. The lack of significant molecular outflows in either source may imply that much of the energy from the intense star formation and AGN activity in this pair is being dissipated in their ISM.
