EMPIRICAL PREDICTIONS FOR (SUB-)MILLIMETER LINE AND CONTINUUM DEEP FIELDS
EMPIRICAL PREDICTIONS FOR (SUB-)MILLIMETER LINE AND CONTINUUM DEEP FIELDS
复制标题
（亚）毫米线和连续体深场的经验预测
作者：
E. D. Cunha;F. Walter;R. Decarli;F. Bertoldi;C. Carilli;E. Daddi;D. Elbaz;R. Ivison;R. Maiolino;D. Riechers;H. Rix;M. Sargent;I. Smail;A. Weiss
现代（亚）毫米/射电干涉仪，如阿尔马，JVLA，和PdBI的继任者NOEMA将使我们能够测量尘埃和分子气体排放的星系，亮度低于银河系，高红移和前所未有的空间分辨率和灵敏度。这将提供新的限制星星的形成性能和气体储层在整个宇宙时代的星系通过专门的深场运动的目标CO/[C二]线和尘埃连续排放（亚）毫米制度。在本文中，我们提出了经验预测这样的线和连续深场。我们的基础上，这些预测最深的光学/近红外高级相机的调查和NICMOS数据的哈勃超深场（在约12弧分2的面积）。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，星星形成率，尘埃衰减和尘埃光度的中位似然估计。我们结合联合收割机的衰减恒星光谱的红外辐射模型库跨越了广泛的尘埃温度，得出在红外和（亚）毫米的尘埃辐射的统计约束与观测到的光学/近红外辐射的能量平衡。这使我们能够估计，为每个星系，（亚）毫米连续通量密度在几个阿尔马，PdBI/NOEMA，和JVLA带。作为一致性检查，我们验证了850 μm的计数和河外背景光使用我们的预测是与以前的观测一致。利用观测到的CO/[C ii]线光度与恒星形成星系的红外光度之间的经验关系，我们从我们样本中每个星系的估计红外光度推断出CO（1-0）和[C ii]线的光度。然后，我们根据两种极端气体激发情景：静止（银河系）和星暴（M82），预测CO较高跃迁线CO（2-1）到CO（7-6）的亮度。我们使用我们的预测讨论可能的深场战略与阿尔马。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。
Modern (sub-)millimeter/radio interferometers such as ALMA, JVLA, and the PdBI successor NOEMA 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/[C ii] lines and dust continuum emission in the (sub-)millimeter regime. In this paper, we present empirical predictions for such line and continuum deep fields. We base these predictions on the deepest available optical/near-infrared Advanced Camera for Surveys and NICMOS data on the Hubble Ultra Deep Field (over an area of about 12 arcmin2). 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 combine the attenuated stellar spectra with a library of infrared emission models spanning a wide range of dust temperatures to 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. As a consistency check, we verify that the 850 μm number counts and extragalactic background light derived using our predictions are consistent with previous observations. Using empirical relations between the observed CO/[C ii] line luminosities and the infrared luminosity of star-forming galaxies, we infer the luminosity of the CO(1–0) and [C ii] lines from the estimated infrared luminosity of each galaxy in our sample. We then predict the luminosities of higher CO transition lines CO(2–1) to CO(7–6) based on two extreme gas excitation scenarios: quiescent (Milky Way) and starburst (M82). 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.
DOI：
10.1088/2041-8205/714/2/l190
发表时间：
2010-03
期刊：
The Astrophysical Journal Letters
影响因子：
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作者：
M. Sargent;E. Schinnerer;E. Murphy;C. Carilli;G. Helou;H. Aussel;É. Le Floc'h;D. Frayer;O. Ilbert;P. Oesch;M. Salvato;V. Smolčić;J. Kartaltepe;D. Sanders
通讯作者：
M. Sargent;E. Schinnerer;E. Murphy;C. Carilli;G. Helou;H. Aussel;É. Le Floc'h;D. Frayer;O. Ilbert;P. Oesch;M. Salvato;V. Smolčić;J. Kartaltepe;D. Sanders