ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: Survey Description

Fabian Walter, Roberto Decarli, Manuel Aravena, Chris Carilli, Rychard Bouwens, Elisabete da Cunha, Emanuele Daddi, R. J. Ivison, Dominik Riechers, Ian Smail, Mark Swinbank, Axel Weiss, Timo Anguita, Roberto Assef, Roland Bacon, Franz Bauer, Eric F. Bell, Frank Bertoldi, Scott Chapman, Luis Colina, Paulo C. Cortes, Pierre Cox, Mark Dickinson, David Elbaz, Jorge Gónzalez-López, Edo Ibar, Hanae Inami, Leopoldo Infante, Jacqueline Hodge, Alex Karim, Olivier Le Fevre, Benjamin Magnelli, Roberto Neri, Pascal Oesch, Kazuaki Ota, Gergö Popping, Hans-Walter Rix, Mark Sargent, Kartik Sheth, Arjen van der Wel, Paul van der Werf, Jeff Wagg

Published 2016-07-22Version 1

We present the rationale for and the observational description of ASPECS: The ALMA SPECtroscopic Survey in the Hubble Ultra-Deep Field (UDF), the cosmological deep field that has the deepest multi-wavelength data available. Our overarching goal is to obtain an unbiased census of molecular gas and dust continuum emission in high-redshift (z$>$0.5) galaxies. The $\sim$1$'$ region covered within the UDF was chosen to overlap with the deepest available imaging from HST. Our ALMA observations consist of full frequency scans in band 3 (84-115 GHz) and band 6 (212-272 GHz) at approximately uniform line sensitivity ($L'_{\rm CO}\sim$2$\times$10$^{9}$ K km/s pc$^2$), and continuum noise levels of 3.8 $\mu$Jy beam$^{-1}$ and 12.7 $\mu$Jy beam$^{-1}$, respectively. The molecular surveys cover the different rotational transitions of the CO molecule, leading to essentially full redshift coverage. The [CII] emission line is also covered at redshifts $6.0<z<8.0$. We present a customized algorithm to identify line candidates in the molecular line scans, and quantify our ability to recover artificial sources from our data. Based on whether multiple CO lines are detected, and whether optical spectroscopic redshifts as well as optical counterparts exist, we constrain the most likely line identification. We report 10 (11) CO line candidates in the 3mm (1mm) band, and our statistical analysis shows that $<$4 of these (in each band) are likely spurious. Less than 1/3 of the total CO flux in the low-J CO line candidates are from sources that are not associated with an optical/NIR counterpart. We also present continuum maps of both the band 3 and band 6 observations. The data presented here form the basis of a number of dedicated studies that are presented in subsequent papers.