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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/20.500.12386/26880
DC FieldValueLanguage
dc.contributor.authorWu, Jianfengen_US
dc.contributor.authorGHISELLINI, Gabrieleen_US
dc.contributor.authorHodges-Kluck, Edmunden_US
dc.contributor.authorGallo, Elenaen_US
dc.contributor.authorCiardi, Benedettaen_US
dc.contributor.authorHAARDT, FRANCESCOen_US
dc.contributor.authorSbarrato, Tulliaen_US
dc.contributor.authorTAVECCHIO, Fabrizioen_US
dc.date.accessioned2020-08-27T12:46:47Z-
dc.date.available2020-08-27T12:46:47Z-
dc.date.issued2017en_US
dc.identifier.issn0035-8711en_US
dc.identifier.urihttp://hdl.handle.net/20.500.12386/26880-
dc.description.abstractIn an effort to understand the cause of the apparent depletion in the number density of radio-loud active galactic nuclei (AGNs) at z > 3, this work investigates the viability of the so-called cosmic microwave background (CMB) quenching mechanism of intrinsically jetted, high-z AGNs, whereby inverse Compton scattering of CMB photons off electrons within the extended lobes results in a substantial dimming of the lobe synchrotron emission at GHz frequencies, while simultaneously boosting their diffuse X-ray signal. We focus on five z > 3.5 radio galaxies that have sufficiently deep Chandra exposure (>50 ks) to warrant a meaningful investigation of any extended X-ray emission. For those objects with evidence for statistically significant extended X-ray lobes (4C 41.17 and 4C 03.24), we combine the Chandra measurements with literature data at lower frequencies to assemble the systems' spectral energy distributions (SEDs), and utilize state-of-the-art SED modelling - including emission from the disc, torus, jet, hotspots and lobes - to infer their physical parameters. For both radio galaxies, the magnetic energy density in the hotspots is found to exceed the energy density in CMB photons, whereas the opposite is true for the lobes. This implies that any extended synchrotron emission likely originates from the hotspots themselves, rather than the lobes. Conversely, inverse Compton scattering of CMB photons dominates the extended X-ray emission from the lobes, which are effectively 'radio-quenched'. As a result, CMB quenching is effective in these systems in spite of the fact that the observed X-ray to radio luminosity ratio does not bear the signature (1 + z)<SUP>4</SUP> dependence of the CMB energy density.en_US
dc.language.isoengen_US
dc.titleCMB-induced radio quenching of high-redshift jetted AGNs with highly magnetic hotspotsen_US
dc.typeArticle-
dc.identifier.doi10.1093/mnras/stx416en_US
dc.identifier.scopus2-s2.0-85017234588en_US
dc.identifier.isi000398419200008en_US
dc.identifier.urlhttps://academic.oup.com/mnras/article/468/1/109/3038247en_US
dc.relation.mediumSTAMPAen_US
dc.relation.volume468en_US
dc.relation.issue1en_US
dc.relation.firstpage109en_US
dc.type.refereeREF_1en_US
dc.description.numberofauthors8en_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.adsbibcode2017MNRAS.468..109Wen_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.fulltextWith Fulltext-
item.grantfulltextopen-
item.cerifentitytypePublications-
item.languageiso639-1en-
item.openairetypeArticle-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
crisitem.journal.journalissn0035-8711-
crisitem.journal.anceE112946-
crisitem.author.deptO.A. Brera-
crisitem.author.deptO.A. Brera-
crisitem.author.deptO.A. Brera-
crisitem.author.orcid0000-0002-0037-1974-
crisitem.author.orcid0000-0002-3069-9399-
crisitem.author.orcid0000-0003-0256-0995-
Appears in Collections:1.01 Articoli in rivista
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