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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/32317
DC FieldValueLanguage
dc.contributor.authorGarsden, H.en_US
dc.contributor.authorGreenhill, L.en_US
dc.contributor.authorBERNARDI, GIANNIen_US
dc.contributor.authorFialkov, A.en_US
dc.contributor.authorPrice, D. C.en_US
dc.contributor.authorMitchell, D.en_US
dc.contributor.authorDowell, J.en_US
dc.contributor.authorSPINELLI, MARTAen_US
dc.contributor.authorSchinzel, F. K.en_US
dc.date.accessioned2022-06-14T15:28:29Z-
dc.date.available2022-06-14T15:28:29Z-
dc.date.issued2021en_US
dc.identifier.issn0035-8711en_US
dc.identifier.urihttp://hdl.handle.net/20.500.12386/32317-
dc.description.abstractThe Large-aperture Experiment to detect the Dark Age (LEDA) was designed to measure the 21-cm signal from neutral hydrogen at Cosmic Dawn, z ≍ 15-30. Using observations made with the ≍ 200 m diameter core of the Owens Valley Radio Observatory Long Wavelength Array (OVRO-LWA), we present a 2D cylindrical spatial power spectrum for data at 43.1-53.5 MHz (z<SUB>median</SUB> ≍ 28) incoherently integrated for 4 h, and an analysis of the array sensitivity. Power from foregrounds is localized to a 'wedge' within k<SUB>⊥</SUB>, $k_\parallel$ space. After calibration of visibilities using five bright compact sources including Vir A, we measure Δ<SUP>2</SUP>(k) ≍ 2 × 10<SUP>12</SUP> mK<SUP>2</SUP> outside the foreground wedge, where an uncontaminated cosmological signal would lie, in principle. The measured Δ<SUP>2</SUP>(k) is an upper limit that reflects a combination of thermal instrumental and sky noise, and unmodelled systematics that scatter power from the wedge, as will be discussed. By differencing calibrated visibilities for close pairs of frequency channels, we suppress foreground sky structure and systematics, extract thermal noise, and use a mix of coherent and incoherent integration to simulate a noise-dominated power spectrum for a 3000 h observation and z = 16-37. For suitable calibration quality, the resulting noise level, Δ<SUP>2</SUP>(k) ≍ 100 mK<SUP>2</SUP> (k = 0.3 Mpc<SUP>-1</SUP>), would be sufficient to detect peaks in the 21-cm spatial power spectrum due to early Ly-α and X-ray sources, as predicted for a range of theoretical model parameters.en_US
dc.language.isoengen_US
dc.titleA 21-cm power spectrum at 48 MHz, using the Owens Valley Long Wavelength Arrayen_US
dc.typeArticle-
dc.identifier.doi10.1093/mnras/stab1671en_US
dc.identifier.scopus2-s2.0-85118159414en_US
dc.identifier.urlhttps://academic.oup.com/mnras/article/506/4/5802/6296658en_US
dc.identifier.urlhttp://arxiv.org/abs/2102.09596v3en_US
dc.relation.mediumSTAMPAen_US
dc.relation.volume506en_US
dc.relation.issue4en_US
dc.relation.firstpage5802en_US
dc.relation.lastpage5817en_US
dc.type.refereeREF_1en_US
dc.description.internationalsìen_US
dc.contributor.countryITAen_US
dc.contributor.countryUSAen_US
dc.relation.scientificsectorFIS/05 - ASTRONOMIA E ASTROFISICAen_US
dc.relation.journalMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETYen_US
dc.type.miur262 Articolo in rivista-
dc.identifier.adsbibcode2021MNRAS.506.5802Gen_US
dc.relation.ercsectorERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentationen_US
dc.description.apcnoen_US
dc.description.oa1 – prodotto con file in versione Open Access (allegare il file al passo  5-Carica)en_US
item.grantfulltextopen-
item.languageiso639-1en-
item.fulltextWith Fulltext-
item.openairetypeArticle-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.cerifentitytypePublications-
crisitem.journal.journalissn0035-8711-
crisitem.journal.anceE112946-
crisitem.author.deptIRA Bologna-
crisitem.author.orcid0000-0002-0916-7443-
crisitem.author.orcid0000-0003-0148-3254-
Appears in Collections:1.01 Articoli in rivista
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