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http://hdl.handle.net/20.500.12386/32254
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | LA PALOMBARA, NICOLA | en_US |
dc.contributor.author | SIDOLI, Lara | en_US |
dc.contributor.author | Esposito, P. | en_US |
dc.contributor.author | ISRAEL, Gian Luca | en_US |
dc.contributor.author | RODRIGUEZ CASTILLO, Guillermo Andres | en_US |
dc.date.accessioned | 2022-06-09T14:57:49Z | - |
dc.date.available | 2022-06-09T14:57:49Z | - |
dc.date.issued | 2021 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/32254 | - |
dc.description.abstract | We report on the follow-up XMM-Newton observation of the persistent X-ray pulsar CXOU J225355.1+624336, which was discovered with the CATS@BAR project on archival Chandra data. The source was detected at f<SUB>X</SUB>(0.5−10 keV) = 3.4 × 10<SUP>−12</SUP> erg cm<SUP>−2</SUP> s<SUP>−1</SUP>, a flux level that is fully consistent with previous observations performed with ROSAT, Swift, and Chandra. When compared with previous measurements, the measured pulse period P = 46.753(3) s implies a constant spin down at an average rate of Ṗ = 5.3 × 10<SUP>−10</SUP> s s<SUP>−1</SUP>. The pulse profile is energy dependent, showing three peaks at low energy and a less structured profile above about 3.5 keV. The pulsed fraction slightly increases with energy. We described the time-averaged EPIC spectrum with four different emission models: a partially covered power law, a cutoff power law, and a power law with an additional thermal component (either a black body or a collisionally ionised gas). In all cases we obtained equally good fits, so it was not possible to prefer or reject any emission model on a statistical basis. However, we disfavour the presence of thermal components since their modeled X-ray flux, resulting from a region larger than the neutron star surface, would largely dominate the X-ray emission from the pulsar. The phase-resolved spectral analysis showed that a simple flux variation cannot explain the source variability and proved that there is a spectral variability along the pulse phase. The results of the XMM-Newton observation confirmed that CXOU J225355.1+624336 is a Be X-ray binary (BeXB) with a low luminosity (L<SUB>X</SUB> ∼ 10<SUP>34−35</SUP> erg s<SUP>−1</SUP>), limited variability, and a constant spin down. Therefore, these results reinforce its source classification as a persistent BeXB. <P />Based on observations obtained with XMM-Newton, an ESA science mission, with instruments and contributions directly funded by ESA Member States and NASA. | en_US |
dc.language.iso | eng | en_US |
dc.title | A deep XMM-Newton observation of the X-Persei-like binary system CXOU J225355.1+624336 | en_US |
dc.identifier.doi | 10.1051/0004-6361/202140760 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/full_html/2021/05/aa40760-21/aa40760-21.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 649 | en_US |
dc.relation.firstpage | A118 | en_US |
dc.relation.numberofpages | 7 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 5 | en_US |
dc.description.international | no | en_US |
dc.contributor.country | ITA | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | ASTRONOMY & ASTROPHYSICS | en_US |
dc.identifier.adsbibcode | 2021A&A...649A.118L | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_10 High energy and particle astronomy – X-rays, cosmic rays, gamma rays, neutrinos | 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.languageiso639-1 | en | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | IASF Palermo | - |
crisitem.author.orcid | 0000-0001-7015-6359 | - |
crisitem.author.orcid | 0000-0001-9705-2883 | - |
crisitem.author.orcid | 0000-0001-5480-6438 | - |
crisitem.author.orcid | 0000-0003-3952-7291 | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
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