Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/33028
DC Field | Value | Language |
---|---|---|
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 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
aa12953-09.pdf | Pdf editoriale | 635.92 kB | Adobe PDF | View/Open |
0909.1701.pdf | arXiv | 1.41 MB | Adobe PDF | View/Open |
Page view(s)
35
checked on Jul 27, 2024
Download(s)
20
checked on Jul 27, 2024
Google ScholarTM
Check
Altmetric
Altmetric
Items in DSpace are published in Open Access, unless otherwise indicated.