Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/30221
Campo DC | Valore | Lingua |
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dc.contributor.author | Goyal, A. | en_US |
dc.contributor.author | Stawarz, Ł. | en_US |
dc.contributor.author | Zola, S. | en_US |
dc.contributor.author | Marchenko, V. | en_US |
dc.contributor.author | Soida, M. | en_US |
dc.contributor.author | Nilsson, K. | en_US |
dc.contributor.author | Ciprini, S. | en_US |
dc.contributor.author | Baran, A. | en_US |
dc.contributor.author | Ostrowski, M. | en_US |
dc.contributor.author | Wiita, P. J. | en_US |
dc.contributor.author | Gopal-Krishna | en_US |
dc.contributor.author | Siemiginowska, A. | en_US |
dc.contributor.author | Sobolewska, M. | en_US |
dc.contributor.author | Jorstad, S. | en_US |
dc.contributor.author | Marscher, A. | en_US |
dc.contributor.author | Aller, M. F. | en_US |
dc.contributor.author | Aller, H. D. | en_US |
dc.contributor.author | Hovatta, T. | en_US |
dc.contributor.author | Caton, D. B. | en_US |
dc.contributor.author | Reichart, D. | en_US |
dc.contributor.author | Matsumoto, K. | en_US |
dc.contributor.author | Sadakane, K. | en_US |
dc.contributor.author | Gazeas, K. | en_US |
dc.contributor.author | Kidger, M. | en_US |
dc.contributor.author | Piirola, V. | en_US |
dc.contributor.author | Jermak, H. | en_US |
dc.contributor.author | Alicavus, F. | en_US |
dc.contributor.author | Baliyan, K. S. | en_US |
dc.contributor.author | Baransky, A. | en_US |
dc.contributor.author | Berdyugin, A. | en_US |
dc.contributor.author | Blay, P. | en_US |
dc.contributor.author | Boumis, P. | en_US |
dc.contributor.author | Boyd, D. | en_US |
dc.contributor.author | Bufan, Y. | en_US |
dc.contributor.author | Campas Torrent, M. | en_US |
dc.contributor.author | Campos, F. | en_US |
dc.contributor.author | Carrillo Gómez, J. | en_US |
dc.contributor.author | Dalessio, J. | en_US |
dc.contributor.author | Debski, B. | en_US |
dc.contributor.author | Dimitrov, D. | en_US |
dc.contributor.author | Drozdz, M. | en_US |
dc.contributor.author | Er, H. | en_US |
dc.contributor.author | Erdem, A. | en_US |
dc.contributor.author | Escartin Pérez, A. | en_US |
dc.contributor.author | Fallah Ramazani, V. | en_US |
dc.contributor.author | Filippenko, A. V. | en_US |
dc.contributor.author | Gafton, E. | en_US |
dc.contributor.author | Garcia, F. | en_US |
dc.contributor.author | Godunova, V. | en_US |
dc.contributor.author | Gómez Pinilla, F. | en_US |
dc.contributor.author | Gopinathan, M. | en_US |
dc.contributor.author | Haislip, J. B. | en_US |
dc.contributor.author | Haque, S. | en_US |
dc.contributor.author | Harmanen, J. | en_US |
dc.contributor.author | Hudec, R. | en_US |
dc.contributor.author | Hurst, G. | en_US |
dc.contributor.author | Ivarsen, K. M. | en_US |
dc.contributor.author | Joshi, A. | en_US |
dc.contributor.author | Kagitani, M. | en_US |
dc.contributor.author | Karaman, N. | en_US |
dc.contributor.author | Karjalainen, R. | en_US |
dc.contributor.author | Kaur, N. | en_US |
dc.contributor.author | Kozieł-Wierzbowska, D. | en_US |
dc.contributor.author | Kuligowska, E. | en_US |
dc.contributor.author | Kundera, T. | en_US |
dc.contributor.author | Kurowski, S. | en_US |
dc.contributor.author | Kvammen, A. | en_US |
dc.contributor.author | LaCluyze, A. P. | en_US |
dc.contributor.author | Lee, B. C. | en_US |
dc.contributor.author | Liakos, A. | en_US |
dc.contributor.author | Lozano de Haro, J. | en_US |
dc.contributor.author | Moore, J. P. | en_US |
dc.contributor.author | Mugrauer, M. | en_US |
dc.contributor.author | Naves Nogues, R. | en_US |
dc.contributor.author | Neely, A. W. | en_US |
dc.contributor.author | Ogloza, W. | en_US |
dc.contributor.author | Okano, S. | en_US |
dc.contributor.author | Pajdosz, U. | en_US |
dc.contributor.author | Pandey, J. C. | en_US |
dc.contributor.author | PERRI, Matteo | en_US |
dc.contributor.author | Poyner, G. | en_US |
dc.contributor.author | Provencal, J. | en_US |
dc.contributor.author | Pursimo, T. | en_US |
dc.contributor.author | Raj, A. | en_US |
dc.contributor.author | Rajkumar, B. | en_US |
dc.contributor.author | Reinthal, R. | en_US |
dc.contributor.author | Reynolds, T. | en_US |
dc.contributor.author | Saario, J. | en_US |
dc.contributor.author | Sadegi, S. | en_US |
dc.contributor.author | Sakanoi, T. | en_US |
dc.contributor.author | Salto González, J. L. | en_US |
dc.contributor.author | Sameer | en_US |
dc.contributor.author | Simon, A. O. | en_US |
dc.contributor.author | Siwak, M. | en_US |
dc.contributor.author | Schweyer, T. | en_US |
dc.contributor.author | Soldán Alfaro, F. C. | en_US |
dc.contributor.author | Sonbas, E. | en_US |
dc.contributor.author | Strobl, J. | en_US |
dc.contributor.author | Takalo, L. O. | en_US |
dc.contributor.author | Tremosa Espasa, L. | en_US |
dc.contributor.author | Valdes, J. R. | en_US |
dc.contributor.author | Vasylenko, V. V. | en_US |
dc.contributor.author | VERRECCHIA, Francesco | en_US |
dc.contributor.author | Webb, J. R. | en_US |
dc.contributor.author | Yoneda, M. | en_US |
dc.contributor.author | Zejmo, M. | en_US |
dc.contributor.author | Zheng, W. | en_US |
dc.contributor.author | Zielinski, P. | en_US |
dc.contributor.author | Janik, J. | en_US |
dc.contributor.author | Chavushyan, V. | en_US |
dc.contributor.author | Mohammed, I. | en_US |
dc.contributor.author | Cheung, C. C. | en_US |
dc.contributor.author | GIROLETTI, MARCELLO | en_US |
dc.date.accessioned | 2021-02-08T10:26:36Z | - |
dc.date.available | 2021-02-08T10:26:36Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/30221 | - |
dc.description.abstract | We present the results of our power spectral density analysis for the BL Lac object OJ 287, utilizing the Fermi-LAT survey at high-energy γ-rays, Swift-XRT in X-rays, several ground-based telescopes and the Kepler satellite in the optical, and radio telescopes at GHz frequencies. The light curves are modeled in terms of continuous-time autoregressive moving average (CARMA) processes. Owing to the inclusion of the Kepler data, we were able to construct for the first time the optical variability power spectrum of a blazar without any gaps across ∼6 dex in temporal frequencies. Our analysis reveals that the radio power spectra are of a colored-noise type on timescales ranging from tens of years down to months, with no evidence for breaks or other spectral features. The overall optical power spectrum is also consistent with a colored noise on the variability timescales ranging from 117 years down to hours, with no hints of any quasi-periodic oscillations. The X-ray power spectrum resembles the radio and optical power spectra on the analogous timescales ranging from tens of years down to months. Finally, the γ-ray power spectrum is noticeably different from the radio, optical, and X-ray power spectra of the source: we have detected a characteristic relaxation timescale in the Fermi-LAT data, corresponding to ∼150 days, such that on timescales longer than this, the power spectrum is consistent with uncorrelated (white) noise, while on shorter variability timescales there is correlated (colored) noise. | en_US |
dc.language.iso | eng | en_US |
dc.title | Stochastic Modeling of Multiwavelength Variability of the Classical BL Lac Object OJ 287 on Timescales Ranging from Decades to Hours | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/aad2de | en_US |
dc.identifier.scopus | 2-s2.0-85052370335 | en_US |
dc.identifier.isi | 000442628400011 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/aad2de | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 863 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 175 | en_US |
dc.type.referee | REF_1 | 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 | 2018ApJ...863..175G | 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.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 | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | IRA Bologna | - |
crisitem.author.orcid | 0000-0003-3613-4409 | - |
crisitem.author.orcid | 0000-0003-3455-5082 | - |
crisitem.author.orcid | 0000-0002-8657-8852 | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
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Goyal_2018_ApJ_863_175.pdf | Pdf editoriale | 4.92 MB | Adobe PDF | Visualizza/apri |
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