Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/25221
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Akiyama, Kazunori | en_US |
dc.contributor.author | Stawarz, Łukasz | en_US |
dc.contributor.author | Tanaka, Yasuyuki T. | en_US |
dc.contributor.author | Nagai, Hiroshi | en_US |
dc.contributor.author | GIROLETTI, MARCELLO | en_US |
dc.contributor.author | Honma, Mareki | en_US |
dc.date.accessioned | 2020-05-27T10:42:16Z | - |
dc.date.available | 2020-05-27T10:42:16Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 2041-8205 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/25221 | - |
dc.description.abstract | We report on the 1.6 GHz (18 cm) very long baseline interferometry (VLBI) observations of the unresolved, steady TeV source HESS J1943+213 located in the Galactic plane, performed with the European VLBI Network (EVN) in 2014. Our new observations with a nearly full EVN array provide the deepest image of HESS J1943+213 at the highest resolution ever achieved, enabling us to resolve the long-standing issues of the source identification. The milliarcsecond-scale structure of HESS J1943+213 has a clear asymmetric morphology consisting of a compact core and a diffuse jet-like tail. This is broadly consistent with the previous e-EVN observations of the source performed in 2011 and re-analyzed in this work. The core component is characterized by the brightness temperature of ≳ 1.8× {10}<SUP>9</SUP> K, which is typical for low-luminosity blazars in general. Overall, the radio properties of HESS J1943+213 are consistent with the source classification as an “extreme high-frequency-peaked BL Lac object.” Remarkably, we note that because HESS J1943+213 does not reveal any optical or infrared signatures of the active galactic nucleus activity, it would never be recognized and identified as a BL Lac object if not for its location close to the Galactic plane where the High Energy Stereoscopic System surveyed for and the follow-up dedicated X-ray and radio studies triggered by the source detection in the TeV range. Our results suggest, therefore, a presence of an unrecognized, possibly very numerous population of particularly extreme HBLs and simultaneously demonstrate that the low-frequency VLBI observations with high angular resolution are indispensable for a proper identification of such objects. | en_US |
dc.language.iso | eng | en_US |
dc.title | EVN Observations of HESS J1943+213: Evidence for an Extreme TeV BL Lac Object | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/2041-8205/823/2/L26 | en_US |
dc.identifier.scopus | 2-s2.0-84975068896 | en_US |
dc.identifier.isi | 000377031700005 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/2041-8205/823/2/L26 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 823 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | L26 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | en_US |
dc.contributor.country | JPN | en_US |
dc.contributor.country | POL | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL LETTERS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2016ApJ...823L..26A | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | IRA Bologna | - |
crisitem.author.orcid | 0000-0002-8657-8852 | - |
crisitem.journal.journalissn | 2041-8205 | - |
crisitem.journal.ance | E196528 | - |
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Akiyama_2016_ApJL_823_L26.pdf | Pdf editoriale | 1.54 MB | Adobe PDF | Visualizza/apri |
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