Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/29846
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | RODRIGUEZ CASTILLO, Guillermo Andres | en_US |
dc.contributor.author | ISRAEL, Gian Luca | en_US |
dc.contributor.author | Belfiore, A. | en_US |
dc.contributor.author | BERNARDINI, Federico | en_US |
dc.contributor.author | Esposito, P. | en_US |
dc.contributor.author | Pintore, Fabio | en_US |
dc.contributor.author | DE LUCA, Andrea | en_US |
dc.contributor.author | PAPITTO, ALESSANDRO | en_US |
dc.contributor.author | STELLA, Luigi | en_US |
dc.contributor.author | Tiengo, A. | en_US |
dc.contributor.author | ZAMPIERI, Luca | en_US |
dc.contributor.author | BACHETTI, Matteo | en_US |
dc.contributor.author | Brightman, M. | en_US |
dc.contributor.author | CASELLA, Piergiorgio | en_US |
dc.contributor.author | D’Agostino, D. | en_US |
dc.contributor.author | Dall’Osso, S. | en_US |
dc.contributor.author | Earnshaw, H. P. | en_US |
dc.contributor.author | Fürst, F. | en_US |
dc.contributor.author | Haberl, F. | en_US |
dc.contributor.author | Harrison, F. A. | en_US |
dc.contributor.author | Mapelli, M. | en_US |
dc.contributor.author | MARELLI, MARTINO | en_US |
dc.contributor.author | Middleton, M. | en_US |
dc.contributor.author | Pinto, C. | en_US |
dc.contributor.author | Roberts, T. P. | en_US |
dc.contributor.author | SALVATERRA, Ruben | en_US |
dc.contributor.author | Turolla, R. | en_US |
dc.contributor.author | Walton, D. J. | en_US |
dc.contributor.author | WOLTER, Anna Luisa Maria | en_US |
dc.date.accessioned | 2021-01-19T12:39:21Z | - |
dc.date.available | 2021-01-19T12:39:21Z | - |
dc.date.issued | 2020 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/29846 | - |
dc.description.abstract | We discovered 2.8 s pulsations in the X-ray emission of the ultraluminous X-ray source (ULX) M51 ULX-7 within the UNSEeN project, which was designed to hunt for new pulsating ULXs (PULXs) with XMM-Newton. The pulse shape is sinusoidal, and large variations of its amplitude were observed even within single exposures (pulsed fraction from less than 5% to 20%). Source M51 ULX-7 is variable, generally observed at an X-ray luminosity between 1039 and 1040 erg s-1, located in the outskirts of the spiral galaxy M51a at a distance of 8.6 Mpc. According to our analysis, the X-ray pulsar orbits in a 2 day binary with a projected semimajor axis aXsinI≃ 28 lt-s. For a neutron star (NS) of 1.4 M☉, this implies a lower limit on the companion mass of 8 M☉, placing the system hosting M51 ULX-7 in the high-mass X-ray binary class. The barycentric pulse period decreased by ≃0.4 ms in the 31 days spanned by our 2018 May-June observations, corresponding to a spin-up rate P˙≃−1.5×10−10s s−1 . In an archival 2005 XMM-Newton exposure, we measured a spin period of ∼3.3 s, indicating a secular spin-up of P˙sec≃−10−9s s−1 , a value in the range of other known PULXs. Our findings suggest that the system consists of a massive donor, possibly an OB giant or supergiant, and a moderately magnetic (dipole field component in the range 1012 G ≲Bdip≲1013 G) accreting NS with weakly beamed emission ( 1/12≲b≲1/4 ). | en_US |
dc.language.iso | eng | en_US |
dc.title | Discovery of a 2.8 s Pulsar in a 2 Day Orbit High-mass X-Ray Binary Powering the Ultraluminous X-Ray Source ULX-7 in M51 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/ab8a44 | en_US |
dc.identifier.scopus | 2-s2.0-85087429960 | en_US |
dc.identifier.isi | 000537822600001 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/ab8a44 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 895 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 60 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 29 | en_US |
dc.description.international | sì | 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 | 2020ApJ...895...60R | 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 | IASF Palermo | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | IASF Palermo | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Cagliari | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.orcid | 0000-0003-3952-7291 | - |
crisitem.author.orcid | 0000-0001-5480-6438 | - |
crisitem.author.orcid | 0000-0001-5326-2010 | - |
crisitem.author.orcid | 0000-0002-3869-2925 | - |
crisitem.author.orcid | 0000-0001-6739-687X | - |
crisitem.author.orcid | 0000-0001-6289-7413 | - |
crisitem.author.orcid | 0000-0002-0018-1687 | - |
crisitem.author.orcid | 0000-0002-6516-1329 | - |
crisitem.author.orcid | 0000-0002-4576-9337 | - |
crisitem.author.orcid | 0000-0002-0752-3301 | - |
crisitem.author.orcid | 0000-0002-8017-0338 | - |
crisitem.author.orcid | 0000-0002-9393-8078 | - |
crisitem.author.orcid | 0000-0001-5840-9835 | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
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