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dc.contributor.authorWalter, Fabian
dc.contributor.authorDecarli, R.
dc.contributor.authorAravena, Manuel
dc.contributor.authorCarilli, Chris L.
dc.contributor.authorBouwens, Rychard
dc.contributor.authorCunha, Elisabete da
dc.contributor.authorDaddi, Emanuele
dc.contributor.authorIvison, R. J.
dc.contributor.authorRiechers, Dominik A.
dc.contributor.authorSmail, Ian R.
dc.contributor.authorSwinbank, Mark
dc.contributor.authorWeiss, Axel
dc.contributor.authorAnguita, Timo
dc.contributor.authorAssef, Roberto
dc.contributor.authorBacon, Roland
dc.contributor.authorBauer, Franz E.
dc.contributor.authorBell, Eric F.
dc.contributor.authorBertoldi, Frank
dc.contributor.authorChapman, Scott
dc.contributor.authorColina, Luis
dc.contributor.authorCortes, Paulo C.
dc.contributor.authorCox, Pierre
dc.contributor.authorDickinson, Mark
dc.contributor.authorElbaz, David
dc.contributor.authorGónzalez-López, Jorge
dc.contributor.authorIbar, Edo
dc.contributor.authorInami, Hanae
dc.contributor.authorInfante, Leopoldo
dc.contributor.authorHodge, Jacqueline
dc.contributor.authorKarim, Alex
dc.contributor.authorFevre, Olivier Le
dc.contributor.authorMagnelli, Benjamin
dc.contributor.authorNeri, Roberto
dc.contributor.authorOesch, Pascal
dc.contributor.authorOta, Kazuaki
dc.contributor.authorPopping, Gergö
dc.contributor.authorRix, Hans-Walter
dc.contributor.authorSargent, Mark
dc.contributor.authorSheth, Kartik
dc.contributor.authorWel, Arjen van der
dc.contributor.authorWerf, Paul van der
dc.contributor.authorWagg, Jeff
dc.date.accessioned2017-06-06T00:17:57Z
dc.date.available2017-06-06T00:17:57Z
dc.date.issued2016-12-08
dc.identifier.citationALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: SURVEY DESCRIPTION 2016, 833 (1):67 The Astrophysical Journalen
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/833/1/67
dc.identifier.urihttp://hdl.handle.net/10150/623953
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 similar to 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'(CO) similar to 2 x 10(9) K km s(-1) pc(2)), and continuum noise levels of 3.8 mu Jy beam(-1) and 12.7 ae Jy 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 < 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 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.description.sponsorshipERC [COSMIC-DAWN, DUSTYGAL, COSMICISM]; FONDECYT [1140099, 1141218, 1151408]; National Science Foundation [1614213]; Conicyt [Basal-CATA PFB-06/2007, Anilo ACT1417]; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC120009]; STFC [ST/L00075X/1]; Collaborative Research Council 956 - Deutsche Forschungsgemeinschaft (DFG); Conict [Basal-CATA PFB-06/2007, Anilo ACT1417]; German ARCen
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/0004-637X/833/i=1/a=67?key=crossref.587db85883c2c04d3140c6eeb4f83976en
dc.rights© 2016. The American Astronomical Society. All rights reserved.en
dc.subjectgalaxies:evolutionen
dc.subjectgalaxies:ISMen
dc.subjectgalaxies:high-redshiften
dc.subjectgalaxies:formationen
dc.subjectsurveysen
dc.titleALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: SURVEY DESCRIPTIONen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalThe Astrophysical Journalen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-08-18T15:24:02Z
html.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 similar to 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'(CO) similar to 2 x 10(9) K km s(-1) pc(2)), and continuum noise levels of 3.8 mu Jy beam(-1) and 12.7 ae Jy 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 < 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 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.


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