（亚）毫米线和连续深场的经验预测
Empirical predictions for (sub-)millimeter line and continuum deep fields
摘要：
现代（亚）毫米/射电干涉仪将使我们能够测量来自亮度低于银河系的星系的尘埃和分子气体发射，达到高红移，并具有前所未有的空间分辨率和灵敏度。这将提供新的限制恒星形成的属性和气体储层在整个宇宙时代的星系通过专门的深场运动针对CO/[CII]线和尘埃连续排放。在本文中，我们提出了经验预测这样的（亚）毫米线和连续深场。我们的基础上最深的光学/近红外ACS和NICMOS数据的哈勃超深场这些预测。使用物理动机的光谱能量分布模型，我们拟合观测到的13,099个星系的光学/近红外发射的红移z=5，并获得其恒星质量，恒星形成率，尘埃衰减和尘埃光度的中值似然估计。我们推导出统计约束的尘埃发射在红外和（亚）毫米，这是一致的观察到的光学/近红外发射的能量平衡。这使我们能够估计，对于每个星系，在几个ALMA，PdBI/NOEMA和JVLA波段的（亚）毫米连续通量密度。利用观测到的CO/[CII]线光度与红外光度之间的经验关系，我们从估算的样本中每个星系的红外光度推断了CO（1-0）和[CII]线的通量。然后，我们预测的通量较高的CO过渡线CO（2-1）CO（7-6）包围两个极端的气体激发的情况。我们用我们的预测来讨论可能的深场战略与ALMA。在这项研究中提出的预测将作为一个直接的基准，为未来的深场运动在（亚）毫米政权。
英文摘要：
[abridged] Modern (sub-)millimeter/radio interferometers will enable us to measure the dust and molecular gas emission from galaxies that have luminosities lower than the Milky Way, out to high redshifts and with unprecedented spatial resolution and sensitivity. This will provide new constraints on the star formation properties and gas reservoir in galaxies throughout cosmic times through dedicated deep field campaigns targeting the CO/[CII] lines and dust continuum emission. In this paper, we present empirical predictions for such (sub-)millimeter line and continuum deep fields. We base these predictions on the deepest available optical/near-infrared ACS and NICMOS data on the Hubble Ultra Deep Field. Using a physically-motivated spectral energy distribution model, we fit the observed optical/near-infrared emission of 13,099 galaxies with redshifts up to z=5, and obtain median likelihood estimates of their stellar mass, star formation rate, dust attenuation and dust luminosity. We derive statistical constraints on the dust emission in the infrared and (sub-)millimeter which are consistent with the observed optical/near-infrared emission in terms of energy balance. This allows us to estimate, for each galaxy, the (sub-)millimeter continuum flux densities in several ALMA, PdBI/NOEMA and JVLA bands. Using empirical relations between the observed CO/[CII] line luminosities and the infrared luminosity, we infer the flux of the CO(1-0) and [CII] lines from the estimated infrared luminosity of each galaxy in our sample. We then predict the fluxes of higher CO transition lines CO(2-1) to CO(7-6) bracketing two extreme gas excitation scenarios. We use our predictions to discuss possible deep field strategies with ALMA. The predictions presented in this study will serve as a direct benchmark for future deep field campaigns in the (sub-)millimeter regime.
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