Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/28227
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Igoshev, Andrei P. | en_US |
dc.contributor.author | Tsygankov, Sergey S. | en_US |
dc.contributor.author | RIGOSELLI, MICHELA | en_US |
dc.contributor.author | MEREGHETTI, Sandro | en_US |
dc.contributor.author | Popov, Sergei B. | en_US |
dc.contributor.author | Elfritz, Justin G. | en_US |
dc.contributor.author | Mushtukov, Alexander A. | en_US |
dc.date.accessioned | 2020-11-09T14:58:34Z | - |
dc.date.available | 2020-11-09T14:58:34Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/28227 | - |
dc.description.abstract | We report on the first X-ray observation of the 0.28 s isolated radio pulsar PSR J1154-6250 obtained with the XMM-Newton observatory in 2018 February. A point-like source is firmly detected at a position consistent with that of PSR J1154-6250. The two closest stars are outside the 3σ confidence limits of the source position and thus unlikely to be responsible for the observed X-ray emission. The energy spectrum of the source can be fitted equally well either with an absorbed power law with a steep photon index Γ ≈ 3.3 or with an absorbed blackbody with temperature kT = 0.21 ± 0.04 keV and emitting radius R <SUB>BB</SUB> ≈ 80 m (assuming a distance of 1.36 kpc). The X-ray luminosity of 4.4 × 10<SUP>30</SUP> erg s<SUP>-1</SUP> derived with the power-law fit corresponds to an efficiency of {η }<SUB>X</SUB>={L}<SUB>X</SUB><SUP>unabs</SUP>}/\dot{E}=4.5× {10}<SUP>-3</SUP>, similar to those of other old pulsars. The X-ray properties of PSR J1154-6250 are consistent with an old age and suggest that the spatial coincidence of this pulsar with the OB association Cru OB1 is due to a chance alignment. | en_US |
dc.language.iso | eng | en_US |
dc.title | Discovery of X-Rays from the Old and Faint Pulsar J1154-6250 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/aadd93 | en_US |
dc.identifier.scopus | 2-s2.0-85054797933 | en_US |
dc.identifier.isi | 000445888000002 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/aadd93 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 865 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 116 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | FIN | en_US |
dc.contributor.country | ISR | en_US |
dc.contributor.country | NLD | en_US |
dc.contributor.country | RUS | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2018ApJ...865..116I | 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.cerifentitytype | Publications | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.orcid | 0000-0001-6641-5450 | - |
crisitem.author.orcid | 0000-0003-3259-7801 | - |
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