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dc.contributor.authorCarilli, CL
dc.contributor.authorThyagarajan, N
dc.contributor.authorKent, J
dc.contributor.authorNikolic, B
dc.contributor.authorGale-Sides, K
dc.contributor.authorKern, NS
dc.contributor.authorBernardi, G
dc.contributor.authorMesinger, A
dc.contributor.authorMatika, S
dc.contributor.authorAbdurashidova, Z
dc.contributor.authorAguirre, JE
dc.contributor.authorAlexander, P
dc.contributor.authorAli, ZS
dc.contributor.authorBalfour, Y
dc.contributor.authorBeardsley, AP
dc.contributor.authorBillings, TS
dc.contributor.authorBowman, JD
dc.contributor.authorBradley, RF
dc.contributor.authorBull, P
dc.contributor.authorBurba, J
dc.contributor.authorCheng, C
dc.contributor.authorDeBoer, DR
dc.contributor.authorDexter, M
dc.contributor.authorAcedo, EDL
dc.contributor.authorDillon, JS
dc.contributor.authorEwall-Wice, A
dc.contributor.authorFagnoni, N
dc.contributor.authorFritz, R
dc.contributor.authorFurlanetto, SR
dc.contributor.authorGale-Sides, K
dc.contributor.authorGlendenning, B
dc.contributor.authorGorthi, D
dc.contributor.authorGreig, B
dc.contributor.authorGrobbelaar, J
dc.contributor.authorHalday, Z
dc.contributor.authorHazelton, BJ
dc.contributor.authorHewitt, JN
dc.contributor.authorHickish, J
dc.contributor.authorJacobs, DC
dc.contributor.authorJosaitis, A
dc.contributor.authorJulius, A
dc.contributor.authorKerrigan, J
dc.contributor.authorKim, H
dc.contributor.authorKittiwisit, P
dc.contributor.authorKohn, SA
dc.contributor.authorKolopanis, M
dc.contributor.authorLanman, A
dc.contributor.authorLa Plante, P
dc.contributor.authorLekalake, T
dc.contributor.authorLiu, A
dc.contributor.authorMacMahon, D
dc.contributor.authorMalan, L
dc.contributor.authorMalgas, C
dc.contributor.authorMaree, M
dc.contributor.authorMartinot, ZE
dc.contributor.authorMatsetela, E
dc.contributor.authorMolewa, M
dc.contributor.authorMorales, MF
dc.contributor.authorMosiane, T
dc.contributor.authorNeben, AR
dc.contributor.authorParra, JM
dc.contributor.authorParsons, AR
dc.contributor.authorPatra, N
dc.contributor.authorPieterse, S
dc.contributor.authorPober, JC
dc.contributor.authorRazavi-Ghods, N
dc.contributor.authorRobnett, J
dc.contributor.authorRosie, K
dc.contributor.authorSims, P
dc.contributor.authorSyce, A
dc.contributor.authorWilliams, PKG
dc.contributor.authorZheng, H
dc.date.accessioned2020-05-21T13:18:39Z
dc.date.available2020-05-21T13:18:39Z
dc.date.issued2020-04
dc.identifier.citationCarilli, C. L. et al. "Imaging And Modeling Data From The Hydrogen Epoch Of Reionization Array". The Astrophysical Journal Supplement Series, vol 247, no. 2, 2020, p. 67. American Astronomical Society, doi:10.3847/1538-4365/ab77b1. Accessed 21 May 2020.en_US
dc.identifier.issn0067-0049
dc.identifier.otherARTN 67
dc.identifier.otherARTN 67
dc.identifier.urihttps://qmro.qmul.ac.uk/xmlui/handle/123456789/64274
dc.description.abstractWe analyze data from the Hydrogen Epoch of Reionization Array (HERA). This is the third in a series of papers on the closure phase delay spectrum technique designed to detect the H i 21 cm emission from cosmic reionization. We present the details of the data and models employed in the power spectral analysis and discuss limitations to the process. We compare images and visibility spectra made with HERA data to parallel quantities generated from sky models based on the Galactic and Extra-Galactic All-Sky MWA (GLEAM) survey, incorporating the HERA telescope model. We find reasonable agreement between images made from HERA data with those generated from the models, down to the confusion level. For the visibility spectra, there is broad agreement between model and data across the full band of ~80 MHz. However, models with only GLEAM sources do not reproduce a roughly sinusoidal spectral structure at the tens of percent level seen in the observed visibility spectra on scales of ~10 MHz on 29 m baselines. We find that this structure is likely due to diffuse Galactic emission, predominantly the Galactic plane, filling the far sidelobes of the antenna primary beam. We show that our current knowledge of the frequency dependence of the diffuse sky radio emission, and the primary beam at large zenith angles, is inadequate to provide an accurate reproduction of the diffuse structure in the models. We discuss some implications arising due to this missing structure in the models, in terms of calibration, and in the search for the H i 21 cm signal, as well as possible mitigation techniques.en_US
dc.publisherIOP Publishingen_US
dc.relation.ispartofASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
dc.subjectCosmologyen_US
dc.subjectCosmological evolutionen_US
dc.subjectRadio interferometryen_US
dc.subjectReionizationen_US
dc.titleImaging and Modeling Data from the Hydrogen Epoch of Reionization Arrayen_US
dc.typeArticleen_US
dc.rights.holder© 2020. The American Astronomical Society.
dc.identifier.doi10.3847/1538-4365/ab77b1
pubs.author-urlhttp://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000525520500001&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=612ae0d773dcbdba3046f6df545e9f6aen_US
pubs.issue2en_US
pubs.notesNot knownen_US
pubs.publication-statusPublisheden_US
pubs.volume247en_US
rioxxterms.funderDefault funderen_US
rioxxterms.identifier.projectDefault projecten_US
rioxxterms.funder.project483cf8e1-88a1-4b8b-aecb-8402672d45f8en_US


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