Examinando por Autor "Tombesi, F."

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Acceso Abierto
A broadband X-ray view of the NLSy1 1E 0754.6+3928
(EDP Sciences, 2020-02-28) Middei, R.; Tombesi, F.; Vagnetti, F.; Serafinelli, R.; Bianchi, S.; Miniutti, G.; Marinucci, A.; Matzeu, G. A.; Petrucci, P. O.; Ursini, F.; Zaino, A.; Agenzia Spaziale Italiana (ASI); Istituto Nazionale Astrofisica (INAF); European Space Agency (ESA); 0000-0001-9815-9092; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Context. The soft X-ray band of many active galactic nuclei (AGNs) is affected by obscuration due to partially ionised matter crossing our line of sight. In this context, two past XMM-Newton observations that were six months apart and a simultaneous NuSTAR-Swift exposure of the Narrow Line Seyfert 1 galaxy 1E 0754.6+3928, which was approximately eight years later, revealed an intense and variable warm absorber (WA) and hints of additional absorbers in the Fe K alpha band.Aims. We aim to provide the first X-ray characterisation of this AGN by discussing its broadband (0.3-79 keV) spectrum and temporal properties.Methods. We conduct a temporal and spectroscopic analysis on two similar to 10 ks (net exposure) XMM-Newton snapshots performed in April and October 2006. We also study the high energy behaviour of 1E 0754.6+3928 and model its broadband spectrum by using simultaneous Swift-NuSTAR data. Both phenomenological and physically motivated models are tested.Results. We find the presence of flux variability of similar to 150% and 30% for 0.3-2 and 2-10 keV bands, respectively, and spectral changes at months timescales of Delta Gamma similar to 0.4. A reflection component that is consistent with being constant over years and arising from relatively cold material that is far from the central super massive black hole is detected. The main spectral feature shaping the 1E 0754.6+3928 spectrum is a WA. Such a component is persistent over the years and the variability of its ionisation and column density is observed down on months in the ranges 3x10(22)cm(-2)less than or similar to N-H less than or similar to 7.2x10(22)cm(-2) and 1.5 less than or similar to log (xi/erg s(-1) cm) less than or similar to 2.1. Despite the short exposures, we find possible evidence of two additional high-ionisation and high-velocity outflow components in absorption.Conclusions. Our analysis suggests the existence of a complex system of absorbers in 1E 0754.6+3928. Longer exposures are required in order to characterise, on more solid grounds, the absorbers in this AGN.
Restringido
Accretion in strong field gravity with eXTP
(Springer Link, 2018-12-07) De Rosa, A.; Uttley, P.; Gou, L.; Liu, Y.; Bambi, C.; Barret, Didier; Belloni, T.; Berti, E.; Bianchi, S.; Caiazzo, I.; Casella, P.; Cui, W. K.; D´Ammando, F.; Dauser, T.; Del Santo, M.; De Marco, B.; Di Salvo, T.; Done, C.; Dovciak, M.; Fabian, A. C.; Falanga, M.; Gambino, A. F.; Gendre, B.; Grinberg, V.; Heger, A.; Homan, J.; Iaria, R.; Jiang, J.; Jin, C. C.; Koerding, E.; Linares, M.; Liu, Z.; Maccarone, Thomas J.; Malzac, J.; Manousakis, A.; Marin, F.; Marinucci, A.; Mehdipour, M.; Méndez, M.; Migliari, S.; Miller, C.; Miniutti, G.; Nardini, E.; O´Brien, P. T.; Osborne, Julian P.; Petrucci, P. O.; Possenti, A.; Riggio, A.; Rodríguez, J.; Sanna, A.; Shao, L. J.; Sobolewska, M.; Sramkova, E.; Stevens, A. L.; Stiele, H.; Stratta, G.; Stuchlik, Z.; Svoboda, J.; Tamburini, F.; Tauris, T. M.; Tombesi, F.; Torok, G.; Urbanec, M.; Vicent, F.; Wu, Q. W.; Yuan, F.; Zand, J. J. M.; Zdziarski, A. A.; Zhou, X.; Feroci, M.; Ferrari, V.; Gualtieri, L.; Heyl, J.; Ingram, A.; Karas, V.; Lu, F. J.; Luo, B.; Matt, G.; Motta, S. E.; Neilsen, J.; Pani, P.; Santangelo, A.; Shu, X. W.; Wang, J. F.; Wang, J. M.; Xue, Y. Q.; Xu, Y. P.; Yuan, W. M.; Yuan, Y. F.; Zhang, S. N.; Zhang, S.; Agudo, I.; Amati, L.; Andersson, N. A.; Baglio, C.; Bakala, P.; Baykal, A.; Bhattacharyya, S.; Bombaci, I.; Bucciantini, N.; Capitanio, F.; Ciolfi, R.; Istituto Nazionale di Astrofisica (INAF); Chinese Academy of Sciences (CAS); National Science Centre, Poland (NCN)
In this paper we describe the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to accretion flows in the strong field gravity regime around both stellar-mass and supermassive black-holes. eXTP has the unique capability of using advanced “spectral-timing-polarimetry” techniques to analyze the rapid variations with three orthogonal diagnostics of the flow and its geometry, yielding unprecedented insight into the inner accreting regions, the effects of strong field gravity on the material within them and the powerful outflows which are driven by the accretion process. X-spinmeasurements
Acceso Abierto
Galaxy-scale ionised winds driven by ultra-fast outflows in two nearby quasars
(EDP Sciences, 2020-11-24) Marasco, A.; Cresci, G.; Nardini, E.; Mannucci, F.; Marconi, A.; Tozzi, P.; Amiri, A.; Venturi, G.; Piconcelli, E.; Lanzuisi, G.; Tombesi, F.; Mingozzi, M.; Perna, M.; Carniani, S.; Brusa, M.; Di Serego Alighieri, S.; Istituto Nazionale Astrofisica (INAF); Agenzia Spaziale Italiana (ASI); Marasco, A. [0000-0002-5655-6054]; Cresci, G. [0000-0002-5281-1417]; Nardini, E. [0000-0001-9226-8992]; Manucci, F. [0000-0002-4803-2381]; Marconi, A. [0000-0002-9889-4238]; Tozzi, G. [0000-0003-4226-7777]; Amiri, A. [0000-0002-8553-1964]; Venturi, G. [0000-0001-8349-3055]; Piconcelli, E. [0000-0001-9095-2782]; Lanzuisi, G. [0000-0001-9094-0984]; Tombesi, F. [0000-0002-6562-8654]; Mingozzi, M. [0000-0003-2589-762X]; Perna, M. [0000-0002-0362-5941]; Carniani, S. [0000-0002-6719-380X]; Brusa, M. [0000-0002-5059-6848]; Di Serego Alighieri, S. [0000-0001-8769-2692]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
We used MUSE adaptive optics data in narrow field mode to study the properties of the ionised gas in MR 2251-178 and PG 1126-041, two nearby (z similar or equal to 0.06) bright quasars (QSOs) hosting sub-pc scale ultra-fast outflows (UFOs) detected in the X-ray band. We decomposed the optical emission from diffuse gas into a low- and a high-velocity components. The former is characterised by a clean, regular velocity field and a low (similar to 80 km s(-1)) velocity dispersion. It traces regularly rotating gas in PG 1126-041, while in MR 2251-178 it is possibly associated with tidal debris from a recent merger or flyby. The other component is found to be extended up to a few kpc from the nuclei, and shows a high (similar to 800 km s(-1)) velocity dispersion and a blue-shifted mean velocity, as is expected from outflows driven by active galactic nuclei (AGN). We estimate mass outflow rates up to a few M-circle dot yr(-1) and kinetic efficiencies L-KIN/L-BOL between 1-4x10(-4), in line with those of galaxies hosting AGN of similar luminosities. The momentum rates of these ionised outflows are comparable to those measured for the UFOs at sub-pc scales, which is consistent with a momentum-driven wind propagation. Pure energy-driven winds are excluded unless about 100x additional momentum is locked in massive molecular winds. In comparing the outflow properties of our sources with those of a small sample of well-studied QSOs hosting UFOs from the literature, we find that winds seem to systematically lie either in a momentum-driven or an energy-driven regime, indicating that these two theoretical models bracket the physics of AGN-driven winds very well.
Restringido
Observatory science with eXTP
(Springer Link, 2018-08-30) Zand, J. J. M.; Bozzo, E.; Qu, J.; Li, X. D.; Amati, L.; Chen, Y.; Donnarumma, I.; Doroshenko, V.; Drake, S. A.; Hernanz, M.; Jenke, P. A.; Baykal, A.; Cumming, A.; Miller, M. C.; Gendre, B.; McHardy, I.; Peretz, U.; Schatz, H.; Brown, E. F.; Neubert, T.; Gill, R.; Mikusincova, R.; Prescod Weinstein, C.; Shearer, A.; Campana, R.; Pacciani, L.; Götz, D.; Rodríguez, J.; Stappers, B. W.; Chambers, F.; Paul, B.; Gouiffès, C.; Rózanska, A.; Strohmayer, T. E.; Chenevez, J.; De Martino, D.; Malzac, J.; Suleimanov, V. F.; Ciolfi, R.; Tauris, T. M.; Méndez, M.; Svoboda, J.; D´aì, A.; Atteia, J. L.; Motch, C.; Thielemann, F. K.; D´Ammando, F.; Mahmoodifar, S.; Tombesi, F.; Degenaar, N.; Zingale, M.; Torres, D. F.; D´Elia, V.; Zhang, S.; Torresi, E.; Doyle, G.; Zhang, S. N.; Fan, X.; Zdziarski, A. A.; Malyshev, D.; Zane, S.; Maccarone, Thomas J.; Zampieri, L.; Zhang, X.; Yuan, F.; Stratta, G.; Yu, W.; Younes, G.; Yan, Z.; Xu, Y.; Xiong, S. L.; Sala, G.; Agudo, I.; Ballantyne, D. R.; Bianchi, S.; Brandt, S.; Cackett, E. M.; Grandi, P.; Granot, J.; Güdel, M.; Heger, A.; Heinke, C. O.; Homan, J.; Iaria, R.; Iwasawa, K.; Izzo, L.; Ji, L.; Del Santo, M.; De Pasquale, M.; Dai, Z. G.; Constantin, E.; Chernyakova, M.; Chen, L.; Casella, P.; Burderi, L.; Braga, J.; Belloni, T.; Andersson, N. A.; Osborne, Julian P.; Wilms, J.; Nardini, E.; De Rosa, A.; Behar, E.; Turriziani, S.; Altamirano, D.; Cavecchi, Y.; Di Salvo, T.; Papadakis, L. E.; Blay, P.; Vacchi, A.; Chen, Y. P.; Falanga, M.; Pérez Torres, M. A.; Bucciantini, N.; Vercellone, S.; Jin, C. C.; Ferdman, R. D.; Reig, P.; Campana, S.; Rowlinson, A.; Feroci, M.; Rodríguez Gil, P.; Lu., F.; Zhou, P.; Fraschetti, F.; Sakamoto, T.; Mehdipour, M.; Baglio, C.; Galloway, D. K.; Salvaterra, R.; Bhattacharyya, S.; Gambino, A. F.; Santagelo, A.; Longo, F.; Gandhi, P.; Schanne, S.; Liang, E. W.; Ge, M.; Shao, L.; Kunneriath, D.; Shore, S. N.; Kuiper, L.; Rossi, E. M.; Kreykenbohm, I.; Wu, X.; Komossa, S.; Linares, M.; Keek, L.; Li, G.; Kawai, N.; Kargaltsev, O.; Kalemci, E.; Kaastra, J. S.; José, J.; Jonker, P. G.; Manousakis, A.; Mignani, R. P.; Nättilä, J.; Orlandini, M.; Paolillo, M.; Vink, J. S.; Wang, J. J.; Wang, J. F.; Watts, A. L.; Weng, S.; Weinberg, N. N.; Wheatley, P. J.; Wijnands, R.; Woods, T. E.; Woosley, S. E.; Savolainen, T.; Sanna, A.; Salmi, T.; Romano, P.; Riggio, A.; Perinati, E.; Pellizzoni, A.; Paltani, Stéphane; O´Brien, P. T.; Miniutti, G.; Men, Y.; Bilous, A.; Lutovinov, A. A.; National Natural Science Foundation of China (NSFC); European Research Council (ERC); National Aeronautics and Space Administration (NASA); Agencia Estatal de Investigación (AEI); Royal Society; Strategic Priority Research Program of the Chinese Academy of Sciences; European Research Council (ERC); National Science Centre, Poland (NCN); Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Cosmos (ICCUB), MDM-2014-0369
In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s.