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A radio view at high-frequencies";s:9:"metadata6";s:93:"Chiaraluce, E; Panessa, F; Bruni, G; Baldi, RD; Behar, E; Vagnetti, F; Tombesi, F; McHardy, I";s:9:"metadata7";N;s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:1;a:14:{s:9:"citazione";s:185:"Middei, R., Tombesi, F., Vagnetti, F., Serafinelli, R., Bianchi, S., Miniutti, G., et al. (2020). A broadband X-ray view of the NLSy1 1E 0754.6+392.8. ASTRONOMY & ASTROPHYSICS, 635, 18.";s:4:"data";s:10:"2020-01-12";s:2:"id";s:20:"PUBBLICAZIONE_365934";s:6:"handle";s:11:"2108/226857";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:51:"A broadband X-ray view of the NLSy1 1E 0754.6+392.8";s:9:"metadata6";s:136:"Middei, R; Tombesi, F; Vagnetti, F; Serafinelli, R; Bianchi, S; Miniutti, G; Marinucci, A; Matzeu, Ga; Petrucci, P-; Ursini, F; Zaino, A";s:9:"metadata7";N;s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:2;a:14:{s:9:"citazione";s:231:"Poulain, M., Paolillo, M., De Cicco, D., Brandt, W.n., Bauer, F.e., Falocco, S., et al. (2020). Extending the variability selection of active galactic nuclei in the W-CDF-S and SERVS/SWIRE region. ASTRONOMY & ASTROPHYSICS, 634, 50.";s:4:"data";s:10:"2020-01-08";s:2:"id";s:20:"PUBBLICAZIONE_365587";s:6:"handle";s:11:"2108/226532";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:99:"Extending the variability selection of active galactic nuclei in the W-CDF-S and SERVS/SWIRE region";s:9:"metadata6";s:211:"Poulain, M; Paolillo, M; De Cicco, D; Brandt, Wn; Bauer, Fe; Falocco, S; Vagnetti, F; Grado, A; Ragosta, F; Botticella, Mt; Cappellaro, E; Pignata, G; Vaccari, M; Schipani, P; Covone, G; Longo, G; Napolitano, Nr";s:9:"metadata7";N;s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:3;a:14:{s:9:"citazione";s:175:"Laurenti, M., Vagnetti, F., & Middei, R. (2020). Optical variability of Active Galactic Nuclei from Catalina Surveys data. JOURNAL OF PHYSICS. CONFERENCE SERIES, 1548, 012015.";s:4:"data";s:4:"2020";s:2:"id";s:20:"PUBBLICAZIONE_392047";s:6:"handle";s:11:"2108/249267";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:14:"Settore FIS/05";s:9:"metadata4";N;s:9:"metadata5";s:72:"Optical variability of Active Galactic Nuclei from Catalina Surveys data";s:9:"metadata6";s:35:"Laurenti, M; Vagnetti, F; Middei, R";s:9:"metadata7";s:31:"10.1088/1742-6596/1548/1/012015";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:4;a:14:{s:9:"citazione";s:213:"Serafinelli, R., Tombesi, F., Vagnetti, F., Piconcelli, E., Gaspari, M., & Saturni, F.g. (2019). Multiphase quasar-driven outflows in PG 1114+445. I. Entrained ultra-fast outflows. ASTRONOMY & ASTROPHYSICS, 627.";s:4:"data";s:10:"2019-07-10";s:2:"id";s:20:"PUBBLICAZIONE_351089";s:6:"handle";s:11:"2108/214652";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";s:37:"astro-ph.GA; astro-ph.GA; astro-ph.HE";s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:84:"Multiphase quasar-driven outflows in PG 1114+445. I. Entrained ultra-fast outflows";s:9:"metadata6";s:79:"Serafinelli, R; Tombesi, F; Vagnetti, F; Piconcelli, E; Gaspari, M; Saturni, Fg";s:9:"metadata7";N;s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:5;a:14:{s:9:"citazione";s:216:"De Cicco, D., Paolillo, M., Falocco, S., Poulain, M., Brandt, W.n., Bauer, F.e., et al. (2019). Optically variable active galactic nuclei in the 3 yr VST survey of the COSMOS field. ASTRONOMY & ASTROPHYSICS, 627, 33.";s:4:"data";s:7:"2019-07";s:2:"id";s:20:"PUBBLICAZIONE_350665";s:6:"handle";s:11:"2108/214288";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:84:"Optically variable active galactic nuclei in the 3 yr VST survey of the COSMOS field";s:9:"metadata6";s:235:"De Cicco, D; Paolillo, M; Falocco, S; Poulain, M; Brandt, Wn; Bauer, Fe; Vagnetti, F; Longo, G; Grado, A; Ragosta, F; Botticella, Mt; Pignata, G; Vaccari, M; Radovich, M; Salvato, M; Covone, G; Napolitano, Nr; Marchetti, L; Schipani, P";s:9:"metadata7";N;s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:6;a:14:{s:9:"citazione";s:239:"Chiaraluce, E., Bruni, G., Panessa, F., Giroletti, M., Orienti, M., Rampadarath, H., et al. (2019). From radio-quiet to radio-silent: low luminosity Seyfert radio cores. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 485(3), 3185-3202.";s:4:"data";s:7:"2019-05";s:2:"id";s:20:"PUBBLICAZIONE_345423";s:6:"handle";s:11:"2108/210293";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";s:24:"astro-ph.GA; astro-ph.GA";s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:68:"From radio-quiet to radio-silent: low luminosity Seyfert radio cores";s:9:"metadata6";s:102:"Chiaraluce, E; Bruni, G; Panessa, F; Giroletti, M; Orienti, M; Rampadarath, H; Vagnetti, F; Tombesi, F";s:9:"metadata7";s:20:"10.1093/mnras/stz595";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:7;a:14:{s:9:"citazione";s:197:"Ronchini, S., Tombesi, F., Vagnetti, F., Panessa, F., & Bruni, G. (2019). X-ray analysis of the accreting supermassive black hole in the radio galaxy PKS 2251+11. ASTRONOMY & ASTROPHYSICS, 625, 26.";s:4:"data";s:10:"2019-03-15";s:2:"id";s:20:"PUBBLICAZIONE_346233";s:6:"handle";s:11:"2108/210996";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1901:"We investigate the dichotomy between jetted and non-jetted Active Galactic Nuclei (AGNs), focusing on the fundamental differences of these two classes in the accretion physics onto the central supermassive black hole (SMBH). Our aim is to study and constrain the structure, kinematics and physical state of the nuclear environment in the Broad Line Radio Galaxy (BLRG) PKS 2251+11. The high X-ray luminosity and the relative proximity make such AGN an ideal candidate for a detailed analysis of the accretion regions in radio galaxies. We performed a spectral and timing analysis of a $\sim$64 ks observation of PKS 2251+11 in the X-ray band with XMM-Newton. We modeled the spectrum considering an absorbed power law superimposed to a reflection component. We performed a time-resolved spectral analysis to search for variability of the X-ray flux and of the individual spectral components. We found that the power law has a photon index $\Gamma=1.8\pm 0.1$, absorbed by an ionized partial covering medium with a column density $N_H=(10.1\pm 0.8) \times 10^23$ cm$^-2$, a ionization parameter $\log\xi=1.3\pm 0.1$ erg s$^-1$ cm and a covering factor $f\simeq90\%$. Considering a density of the absorber typical of the Broad Line Region (BLR), its distance from the central SMBH is of the order of $r\sim 0.1$ pc. An Fe K$\alpha$ emission line is found at 6.4 keV, whose intensity shows variability on time scales of hours. We derived that the reflecting material is located at a distance $r\gtrsim600r_s$, where $r_s$ is the Schwarzschild radius. Concerning the X-ray properties, we found that PKS 2251+11 does not differ significantly from the non-jetted AGNs, confirming the validity of the unified model in describing the inner regions around the central SMBH, but the lack of information regarding the state of the very innermost disk and SMBH spin still leave unconstrained the origin of the jet.";s:9:"metadata5";s:87:"X-ray analysis of the accreting supermassive black hole in the radio galaxy PKS 2251+11";s:9:"metadata6";s:58:"Ronchini, S; Tombesi, F; Vagnetti, F; Panessa, F; Bruni, G";s:9:"metadata7";s:27:"10.1051/0004-6361/201935176";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:8;a:14:{s:9:"citazione";s:217:"Luminari, A., Piconcelli, E., Tombesi, F., Zappacosta, L., Fiore, F., Piro, L., et al. (2018). Constraining the geometry of the nuclear wind in PDS 456 using a novel emission model. ASTRONOMY & ASTROPHYSICS, 619, 149.";s:4:"data";s:10:"2018-11-19";s:2:"id";s:20:"PUBBLICAZIONE_339193";s:6:"handle";s:11:"2108/205053";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:85:"Constraining the geometry of the nuclear wind in PDS 456 using a novel emission model";s:9:"metadata6";s:85:"Luminari, A; Piconcelli, E; Tombesi, F; Zappacosta, L; Fiore, F; Piro, L; Vagnetti, F";s:9:"metadata7";s:27:"10.1051/0004-6361/201833623";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:9;a:14:{s:9:"citazione";s:168:"Elia, C., Vagnetti, F., Tombesi, F., & Maurizio, P. (2018). The X-ray/UV ratio in Active Galactic Nuclei: dispersion and variability. 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ASTRONOMY & ASTROPHYSICS, 618.";s:4:"data";s:10:"2018-10-25";s:2:"id";s:20:"PUBBLICAZIONE_336641";s:6:"handle";s:11:"2108/203009";s:9:"metadata1";s:19:"Articolo su rivista";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";N;s:9:"metadata5";s:50:"The NuSTAR view of the Seyfert Galaxy HE 0436-4717";s:9:"metadata6";s:83:"Middei, R; Vagnetti, F; Tombesi, F; Bianchi, S; Marinucci, A; Ursini, F; Tortosa, A";s:9:"metadata7";s:27:"10.1051/0004-6361/201833598";s:9:"metadata8";N;s:9:"metadata9";N;s:10:"metadata10";N;}i:11;a:14:{s:9:"citazione";s:176:"Cherenkov Telescope Array Consortium, T., :, ., Acharya, B.s., Agudo, I., Al Samarai, I., Alfaro, R., et al. (2017). Science with the Cherenkov Telescope Array [Working paper].";s:4:"data";s:10:"2017-09-23";s:2:"id";s:20:"PUBBLICAZIONE_325351";s:6:"handle";s:11:"2108/193310";s:9:"metadata1";s:5:"Altro";s:9:"metadata2";N;s:9:"metadata3";s:41:"Settore FIS/05 - Astronomia e Astrofisica";s:9:"metadata4";s:1874:"The Cherenkov Telescope Array, CTA, will be the major global observatory for very high energy gamma-ray astronomy over the next decade and beyond. The scientific potential of CTA is extremely broad: from understanding the role of relativistic cosmic particles to the search for dark matter. CTA is an explorer of the extreme universe, probing environments from the immediate neighbourhood of black holes to cosmic voids on the largest scales. Covering a huge range in photon energy from 20 GeV to 300 TeV, CTA will improve on all aspects of performance with respect to current instruments. The observatory will operate arrays on sites in both hemispheres to provide full sky coverage and will hence maximize the potential for the rarest phenomena such as very nearby supernovae, gamma-ray bursts or gravitational wave transients. With 99 telescopes on the southern site and 19 telescopes on the northern site, flexible operation will be possible, with sub-arrays available for specific tasks. CTA will have important synergies with many of the new generation of major astronomical and astroparticle observatories. Multi-wavelength and multi-messenger approaches combining CTA data with those from other instruments will lead to a deeper understanding of the broad-band non-thermal properties of target sources. The CTA Observatory will be operated as an open, proposal-driven observatory, with all data available on a public archive after a pre-defined proprietary period. Scientists from institutions worldwide have combined together to form the CTA Consortium. This Consortium has prepared a proposal for a Core Programme of highly motivated observations. The programme, encompassing approximately 40% of the available observing time over the first ten years of CTA operation, is made up of individual Key Science Projects (KSPs), which are presented in this document.";s:9:"metadata5";s:42:"Science with the Cherenkov Telescope Array";s:9:"metadata6";s:7356:"Cherenkov Telescope Array Consortium, T; :, ; Acharya, Bs; Agudo, I; Al Samarai, I; Alfaro, R; Alfaro, J; Alispach, C; Alves Batista, R; Amans, J-; Amato, E; Ambrosi, G; Antolini, E; Antonelli, La; Aramo, C; Araya, M; Armstrong, T; Arqueros, F; Arrabito, L; Asano, K; Ashley, M; Backes, M; Balazs, C; Balbo, M; Ballester, O; Ballet, J; Bamba, A; Barkov, M; Barres de Almeida, U; Barrio, Ja; Bastieri, D; Becherini, Y; Belfiore, A; Benbow, W; Berge, D; Bernardini, E; Bernardini, Mg; Bernardos, M; Bernlöhr, K; Bertucci, B; Biasuzzi, B; Bigongiari, C; Biland, A; Bissaldi, E; Biteau, J; Blanch, O; Blazek, J; Boisson, C; Bolmont, J; Bonanno, G; Bonardi, A; Bonavolontà, C; Bonnoli, G; Bosnjak, Z; Böttcher, M; Braiding, C; Bregeon, J; Brill, A; Brown, Am; Brun, P; Brunetti, G; Buanes, T; Buckley, J; Bugaev, V; Bühler, R; Bulgarelli, A; Bulik, T; Burton, M; Burtovoi, A; Busetto, G; Canestrari, R; Capalbi, M; Capitanio, F; Caproni, A; Caraveo, P; Cárdenas, V; Carlile, C; Carosi, R; Carquín, E; Carr, J; Casanova, S; Cascone, E; Catalani, F; Catalano, O; Cauz, D; Cerruti, M; Chadwick, P; Chaty, S; Chaves, Rcg; Chen, A; Chen, X; Chernyakova, M; Chikawa, M; Christov, A; Chudoba, J; Cieślar, M; Coco, V; Colafrancesco, S; Colin, P; Conforti, V; Connaughton, V; Conrad, J; Contreras, Jl; Cortina, J; Costa, A; Costantini, H; Cotter, G; Covino, S; Crocker, R; Cuadra, J; Cuevas, O; Cumani, P; D'Aì, A; D'Ammando, F; D'Avanzo, P; D'Urso, D; Daniel, M; Davids, I; Dawson, B; Dazzi, F; De Angelis, A; de Cássia dos Anjos, R; De Cesare, G; De Franco, A; de Gouveia Dal Pino, Em; de la Calle, I; de los Reyes Lopez, R; De Lotto, B; De Luca, A; De Lucia, M; de Naurois, M; de Oña Wilhelmi, E; De Palma, F; De Persio, F; de Souza, V; Deil, C; Del Santo, M; Delgado, C; della Volpe, D; Di Girolamo, T; Di Pierro, F; Di Venere, L; Díaz, C; Dib, C; Diebold, S; Djannati-Ataï, A; Domínguez, A; Dominis Prester, D; Dorner, D; Doro, M; Drass, H; Dravins, D; Dubus, G; Dwarkadas, Vv; Ebr, J; Eckner, C; Egberts, K; Einecke, S; Ekoume, Trn; Elsässer, D; Ernenwein, J-; Espinoza, C; Evoli, C; Fairbairn, M; Falceta-Goncalves, D; Falcone, A; Farnier, C; Fasola, G; Fedorova, E; Fegan, S; Fernandez-Alonso, M; Fernández-Barral, A; Ferrand, G; Fesquet, M; Filipovic, M; Fioretti, V; Fontaine, G; Fornasa, M; Fortson, L; Freixas Coromina, L; Fruck, C; Fujita, Y; Fukazawa, Y; Funk, S; Füßling, M; Gabici, S; Gadola, A; Gallant, Y; Garcia, B; Garcia López, R; Garczarczyk, M; Gaskins, J; Gasparetto, T; Gaug, M; Gerard, L; Giavitto, G; Giglietto, N; Giommi, P; Giordano, F; Giro, E; Giroletti, M; Giuliani, A; Glicenstein, J-; Gnatyk, R; Godinovic, N; Goldoni, P; Gómez-Vargas, G; González, Mm; González, Jm; Götz, D; Graham, J; Grandi, P; Granot, J; Green, Aj; Greenshaw, T; Griffiths, S; Gunji, S; Hadasch, D; Hara, S; Hardcastle, Mj; Hassan, T; Hayashi, K; Hayashida, M; Heller, M; Helo, Jc; Hermann, G; Hinton, J; Hnatyk, B; Hofmann, W; Holder, J; Horan, D; Hörandel, J; Horns, D; Horvath, P; Hovatta, T; Hrabovsky, M; Hrupec, D; Humensky, Tb; Hütten, M; Iarlori, M; Inada, T; Inome, Y; Inoue, S; Inoue, T; Inoue, Y; Iocco, F; Ioka, K; Iori, M; Ishio, K; Iwamura, Y; Jamrozy, M; Janecek, P; Jankowsky, D; Jean, P; Jung-Richardt, I; Jurysek, J; Kaaret, P; Karkar, S; Katagiri, H; Katz, U; Kawanaka, N; Kazanas, D; Khélifi, B; Kieda, Db; Kimeswenger, S; Kimura, S; Kisaka, S; Knapp, J; Knödlseder, J; Koch, B; Kohri, K; Komin, N; Kosack, K; Kraus, M; Krause, M; Krauß, F; Kubo, H; Kukec Mezek, G; Kuroda, H; Kushida, J; La Palombara, N; Lamanna, G; Lang, Rg; Lapington, J; Le Blanc, O; Leach, S; Lees, J-; Lefaucheur, J; Leigui de Oliveira, Ma; Lenain, J-; Lico, R; Limon, M; Lindfors, E; Lohse, T; Lombardi, S; Longo, F; López, M; 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