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

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dc.contributor.authorWalter, Fabian
dc.contributor.authorDecarli, Roberto
dc.contributor.authorAravena, M.
dc.contributor.authorCarilli, C L
dc.contributor.authorBouwens, Rychard John
dc.contributor.authorda Cunha, Elisabete
dc.contributor.authorDaddi, E.
dc.contributor.authorIvison, Robert J
dc.contributor.authorRiechers, Dominik
dc.contributor.authorSmail, Ian
dc.date.accessioned2018-11-29T22:52:45Z
dc.date.available2018-11-29T22:52:45Z
dc.date.issued2016
dc.date.updated2018-11-29T07:48:23Z
dc.description.abstractWe 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 ~1' region covered within the UDF was chosen to overlap with the deepest available imaging from the Hubble Space Telescope. 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}_{\mathrm{CO}}^{\prime }\,\sim $ 2 × 109 K km s−1 pc2), and continuum noise levels of 3.8 μJy beam−1 and 12.7 μJy beam−1, respectively. The molecular surveys cover the different rotational transitions of the CO molecule, leading to essentially full redshift coverage. The [C ii] emission line is also covered at redshifts $6.0\lt z\lt 8.0$. 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 3 mm (1 mm) band, and our statistical analysis shows that <4 of these (in each band) are likely spurious. Less than one-third 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
dc.format.mimetypeapplication/pdfen_AU
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/1885/152266
dc.publisherIOP Publishing
dc.sourceThe Astrophysical Journal
dc.titleAlma Spectroscopic Survey in the Hubble Ultra Deep Field: Survey Description
dc.typeJournal article
dcterms.accessRightsOpen Accessen_AU
local.bibliographicCitation.issue1
local.bibliographicCitation.lastpage15
local.bibliographicCitation.startpage1
local.contributor.affiliationWalter, Fabian, Max Planck Institute for Astronomy
local.contributor.affiliationDecarli, Roberto, Max-Planck Institut fur Astronomie
local.contributor.affiliationAravena, M., Núcleo de Astronomía, Facultad de Ingeniería, Universidad Diego Portales
local.contributor.affiliationCarilli, C L, National Radio Astronomy Observatory
local.contributor.affiliationBouwens, Rychard John, Leiden University
local.contributor.affiliationda Cunha, Elisabete, College of Science, ANU
local.contributor.affiliationDaddi, E., DSM-CNRS-Universite Paris Diderot
local.contributor.affiliationIvison, Robert J, Royal Observatory Edinburgh
local.contributor.affiliationRiechers, Dominik, Cornell University
local.contributor.affiliationSmail, Ian, Durham University
local.contributor.authoremailu6091514@anu.edu.au
local.contributor.authoruidda Cunha, Elisabete, u6091514
local.description.notesImported from ARIES
local.identifier.absfor020110 - Stellar Astronomy and Planetary Systems
local.identifier.absfor020104 - Galactic Astronomy
local.identifier.ariespublicationu5957081xPUB11
local.identifier.citationvolume833
local.identifier.doi10.3847/1538-4357/833/1/67
local.identifier.scopusID2-s2.0-85006386452
local.identifier.thomsonID000399326800001
local.identifier.uidSubmittedByu5957081
local.type.statusPublished Version

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