The Atacama Large Millimeter/submillimeter Array Spectroscopic Survey in the Hubble Ultra Deep Field: CO Emission Lines and 3 mm Continuum Sources
The Atacama Large Millimeter/submillimeter Array Spectroscopic Survey in the Hubble Ultra Deep Field: CO Emission Lines and 3 mm Continuum Sources
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DOI：
10.3847/1538-4357/ab3105
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发表时间：
2019-09
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影响因子：
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通讯作者：
J. González-López;R. Decarli;R. Pavesi;F. Walter;M. Aravena;C. Carilli;L. Boogaard;G. Popping;A. Weiss;R. Assef;F. Bauer;F. Bertoldi;R. Bouwens;T. Contini;P. Cortés;P. Cox;E. da Cunha;E. Daddi;T. Díaz-Santos;H. Inami;J. Hodge;R. Ivison;O. Le Fèvre;B. Magnelli;P. Oesch;D. Riechers;H. Rix;I. Smail;A. M. Swinbank;R. Somerville;B. Uzgil;P. P. van der Werf-P.
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文献类型：
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作者：
J. González-López;R. Decarli;R. Pavesi;F. Walter;M. Aravena;C. Carilli;L. Boogaard;G. Popping;A. Weiss;R. Assef;F. Bauer;F. Bertoldi;R. Bouwens;T. Contini;P. Cortés;P. Cox;E. da Cunha;E. Daddi;T. Díaz-Santos;H. Inami;J. Hodge;R. Ivison;O. Le Fèvre;B. Magnelli;P. Oesch;D. Riechers;H. Rix;I. Smail;A. M. Swinbank;R. Somerville;B. Uzgil;P. P. van der Werf-P.
哈勃超深场(HUDF)中的阿塔卡马大毫米/亚毫米阵列(ALMA)光谱测量是一个ALMA大型项目，它获得了3毫米波段的频率扫描，以探测遥远星系中分子气体的发射线。在这里，我们介绍了我们在HUDF中寻找发射线和连续源的策略。我们比较了文献中使用的几种线搜索算法，并在评估重要性时关键地考虑了候选发射线的线宽。在我们的搜索中，我们发现了16条高保真的发射线。将这些源与多波长数据进行比较，我们发现所有源都有光学/红外对应物。我们的搜索还恢复了重要性较低的候选者，这些候选者可以用来统计地推导出例如CO光度函数。我们应用相同的检测算法来获得6个3 mm连续谱源的样本。所有这些在1.2 mm连续介质中也可以用光学/近红外对应物探测到。我们使用连续谱源计算了亚毫米扬斯基区域的3毫米数计数，发现它们比同步加速器为主的源高出一个数量级。然而，在沙尘发射率指数β=1.5，沙尘温度35K，平均红移z=2.5的情况下，一旦外推到3 mm，得到的尘埃个数与较短波长(0.85-1.3 mm)的计数一致。这些结果代表了迄今为止对3 mm数字计数的模糊结束的最好限制。
The Atacama Large Millimeter/submillimeter Array (ALMA) SPECtroscopic Survey in the Hubble Ultra Deep Field (HUDF) is an ALMA large program that obtained a frequency scan in the 3 mm band to detect emission lines from the molecular gas in distant galaxies. Here we present our search strategy for emission lines and continuum sources in the HUDF. We compare several line search algorithms used in the literature, and critically account for the line widths of the emission line candidates when assessing significance. We identify 16 emission lines at high fidelity in our search. Comparing these sources to multiwavelength data we find that all sources have optical/infrared counterparts. Our search also recovers candidates of lower significance that can be used statistically to derive, e.g., the CO luminosity function. We apply the same detection algorithm to obtain a sample of six 3 mm continuum sources. All of these are also detected in the 1.2 mm continuum with optical/near-infrared counterparts. We use the continuum sources to compute 3 mm number counts in the sub-millijansky regime, and find them to be higher by an order of magnitude than expected for synchrotron-dominated sources. However, the number counts are consistent with those derived at shorter wavelengths (0.85–1.3 mm) once extrapolating to 3 mm with a dust emissivity index of β = 1.5, dust temperature of 35 K, and an average redshift of z = 2.5. These results represent the best constraints to date on the faint end of the 3 mm number counts.