Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/33028
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | RAITERI, Claudia Maria | en_US |
dc.contributor.author | VILLATA, Massimo | en_US |
dc.contributor.author | CAPETTI, Alessandro | en_US |
dc.contributor.author | Aller, M.F. | en_US |
dc.contributor.author | Bach, U. | en_US |
dc.contributor.author | Calcidese, P. | en_US |
dc.contributor.author | Gurwell, M.A. | en_US |
dc.contributor.author | Larionov, V.M. | en_US |
dc.contributor.author | Ohlert, J. | en_US |
dc.contributor.author | Nilsson, K. | en_US |
dc.contributor.author | Strigachev, A. | en_US |
dc.contributor.author | Agudo, I. | en_US |
dc.contributor.author | Aller, H.D. | en_US |
dc.contributor.author | Bachev, R. | en_US |
dc.contributor.author | Benítez, E. | en_US |
dc.contributor.author | Berdyugin, A. | en_US |
dc.contributor.author | Böttcher, M. | en_US |
dc.contributor.author | BUEMI, CARLA SIMONA | en_US |
dc.contributor.author | Buttiglione, S. | en_US |
dc.contributor.author | Carosati, D. | en_US |
dc.contributor.author | Charlot, P. | en_US |
dc.contributor.author | Chen, W.P. | en_US |
dc.contributor.author | Dultzin, D. | en_US |
dc.contributor.author | Forné, E. | en_US |
dc.contributor.author | Fuhrmann, L. | en_US |
dc.contributor.author | Gómez, J.L. | en_US |
dc.contributor.author | Gupta, A.C. | en_US |
dc.contributor.author | Heidt, J. | en_US |
dc.contributor.author | Hiriart, D. | en_US |
dc.contributor.author | Hsiao, W.-S. | en_US |
dc.contributor.author | Jelínek, M. | en_US |
dc.contributor.author | Jorstad, S.G. | en_US |
dc.contributor.author | Kimeridze, G.N. | en_US |
dc.contributor.author | Konstantinova, T.S. | en_US |
dc.contributor.author | Kopatskaya, E.N. | en_US |
dc.contributor.author | Kostov, A. | en_US |
dc.contributor.author | Kurtanidze, O.M. | en_US |
dc.contributor.author | Lähteenmäki, A. | en_US |
dc.contributor.author | LANTERI, Luciano | en_US |
dc.contributor.author | Larionova, L.V. | en_US |
dc.contributor.author | LETO, PAOLO | en_US |
dc.contributor.author | Latev, G. | en_US |
dc.contributor.author | Le Campion, J.-F. | en_US |
dc.contributor.author | Lee, C.-U. | en_US |
dc.contributor.author | Ligustri, R. | en_US |
dc.contributor.author | Lindfors, E. | en_US |
dc.contributor.author | Marscher, A.P. | en_US |
dc.contributor.author | Mihov, B. | en_US |
dc.contributor.author | Nikolashvili, M.G. | en_US |
dc.contributor.author | Nikolov, Y. | en_US |
dc.contributor.author | Ovcharov, E. | en_US |
dc.contributor.author | Principe, D. | en_US |
dc.contributor.author | Pursimo, T. | en_US |
dc.contributor.author | Ragozzine, B. | en_US |
dc.contributor.author | Robb, R.M. | en_US |
dc.contributor.author | Ros, J.A. | en_US |
dc.contributor.author | Sadun, A.C. | en_US |
dc.contributor.author | Sagar, R. | en_US |
dc.contributor.author | Semkov, E. | en_US |
dc.contributor.author | Sigua, L.A. | en_US |
dc.contributor.author | SMART, Richard Laurence | en_US |
dc.contributor.author | Sorcia, M. | en_US |
dc.contributor.author | Takalo, L.O. | en_US |
dc.contributor.author | Tornikoski, M. | en_US |
dc.contributor.author | TRIGILIO, CORRADO | en_US |
dc.contributor.author | Uckert, K. | en_US |
dc.contributor.author | UMANA, Grazia Maria Gloria | en_US |
dc.contributor.author | Valcheva, A. | en_US |
dc.contributor.author | Volvach, A. | en_US |
dc.date.accessioned | 2023-01-24T11:41:03Z | - |
dc.date.available | 2023-01-24T11:41:03Z | - |
dc.date.issued | 2009 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/33028 | - |
dc.description.abstract | In 2007-2008 we carried out a new multiwavelength campaign of the Whole Earth Blazar Telescope (WEBT) on BL Lacertae, involving three pointings by the XMM-Newton satellite, to study its emission properties. The source was monitored in the optical-to-radio bands by 37 telescopes. The brightness level was relatively low. Some episodes of very fast variability were detected in the optical bands. The X-ray spectra are well fitted by a power law with photon index of about 2 and photoelectric absorption exceeding the Galactic value. However, when taking into account the presence of a molecular cloud on the line of sight, the data are best fitted by a double power law, implying a concave X-ray spectrum. The spectral energy distributions (SEDs) built with simultaneous radio-to-X-ray data at the epochs of the XMM-Newton observations suggest that the peak of the synchrotron emission lies in the near-IR band, and show a prominent UV excess, besides a slight soft-X-ray excess. A comparison with the SEDs corresponding to previous observations with X-ray satellites shows that the X-ray spectrum is extremely variable. We ascribe the UV excess to thermal emission from the accretion disc, and the other broad-band spectral features to the presence of two synchrotron components, with their related SSC emission. We fit the thermal emission with a black body law and the non-thermal components by means of a helical jet model. The fit indicates a disc temperature greater than 20000 K and a luminosity greater than 6 x 10^44 erg/s. | en_US |
dc.language.iso | eng | en_US |
dc.title | WEBT multiwavelength monitoring and XMM-Newton observations of BL Lacertae in 2007-2008 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/200912953 | en_US |
dc.identifier.scopus | 2-s2.0-70450207356 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/full_html/2009/44/aa12953-09/aa12953-09.html | en_US |
dc.identifier.url | http://www.scopus.com/inward/record.url?eid=2-s2.0-70450207356&partnerID=MN8TOARS | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 507 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 769 | en_US |
dc.relation.lastpage | 779 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 69 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | ASTRONOMY & ASTROPHYSICS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2009A&A...507..769R | 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 | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.orcid | 0000-0003-1784-2784 | - |
crisitem.author.orcid | 0000-0003-1743-6946 | - |
crisitem.author.orcid | 0000-0003-3684-4275 | - |
crisitem.author.orcid | 0000-0002-7288-4613 | - |
crisitem.author.orcid | 0000-0001-9738-5493 | - |
crisitem.author.orcid | 0000-0003-4864-2806 | - |
crisitem.author.orcid | 0000-0002-4424-4766 | - |
crisitem.author.orcid | 0000-0002-1216-7831 | - |
crisitem.author.orcid | 0000-0002-6972-8388 | - |
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aa12953-09.pdf | Pdf editoriale | 635.92 kB | Adobe PDF | Visualizza/apri |
0909.1701.pdf | arXiv | 1.41 MB | Adobe PDF | Visualizza/apri |
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