Examinando por Autor "Tozzi, P."

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Acceso Abierto
Connecting X-ray nuclear winds with galaxy-scale ionised outflows in two z ∼ 1.5 lensed quasars
(EDP Sciences, 2021-04-20) Tozzi, P.; Cresci, G.; Marasco, A.; Nardini, E.; Marconi, A.; Mannucci, F.; Chartas, G.; Rizzo, F.; Amiri, A.; Brusa, M.; Comastri, A.; Dadina, M.; Lanzuisi, G.; Mainieri, V.; Mingozzi, M.; Perna, M.; Venturi, G.; Vignali, C.; Italian Ministry for University and Research (MUR); Agencia Estatal de Investigación (AEI); Comunidad de Madrid; Tozzi, G. [0000-0003-4226-7777]; Cresci, G. [0000-0002-5281-1417]; Marasco, A. [0000-0002-5655-6054]; Nardini, E. [0000-0001-9226-8992]; Marconi, A. [0000-0002-9889-4238]; Mannucci, F. [0000-0002-4803-2381]; Rizzo, F. [0000-0001-9705-2461]; Amiri, A. [0000-0002-8553-1964]; Dadina, M. [0000-0002-7858-7564]; Lanzuisi, G. [0000-0001-9094-0984]; Mainieri, V. [0000-0002-1047-9583]; Mingozzi, M. [0000-0003-2589-762X]; Perna, M. [0000-0002-0362-5941]; Venturi, G. [0000-0001-8349-3055]
Aims. Outflows driven by active galactic nuclei (AGN) are expected to have a significant impact on host galaxy evolution, but the matter of how they are accelerated and propagated on galaxy-wide scales is still under debate. This work addresses these questions by studying the link between X-ray, nuclear ultra-fast outflows (UFOs), and extended ionised outflows, for the first time, in two quasars close to the peak of AGN activity (z ∼ 2), where AGN feedback is expected to be more effective. Methods. Our selected targets, HS 0810+2554 and SDSS J1353+1138, are two multiple-lensed quasars at z ∼ 1.5 with UFO detection that have been observed with the near-IR integral field spectrometer SINFONI at the VLT. We performed a kinematical analysis of the [O III]λ5007 optical emission line to trace the presence of ionised outflows. Results. We detected spatially resolved ionised outflows in both galaxies, extended more than 8 kpc and moving up to v > 2000 km s−1. We derived mass outflow rates of ∼12 M⊙ yr−1 and ∼2 M⊙ yr−1 for HS 0810+2554 and SDSS J1353+1138. Conclusions. Compared with the co-hosted UFO energetics, the ionised outflow energetics in HS 0810+2554 is broadly consistent with a momentum-driven regime of wind propagation, whereas in SDSS J1353+1138, it differs by about two orders of magnitude from theoretical predictions, requiring either a massive molecular outflow or a high variability of the AGN activity to account for such a discrepancy. By additionally considering our results together with those from the small sample of well-studied objects (all local but one) having both UFO and extended (ionised, atomic, or molecular) outflow detections, we found that in 10 out of 12 galaxies, the large-scale outflow energetics is consistent with the theoretical predictions of either a momentum- or an energy-driven scenario of wind propagation. This suggests that such models explain the acceleration mechanism of AGN-driven winds on large scales relatively well.
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.
Acceso Abierto
The GAPS Programme at TNG XXI. A GIARPS case study of known young planetary candidates: confirmation of HD 285507 b and refutation of AD Leonis b
(EDP Sciences, 2020-05-29) Carleo, I.; Malavolta, L.; Lanza, A. F.; Damasso, M.; Desidera, S.; Borsa, F.; Mallonn, M.; Pinamonti, M.; Gratton, R.; Alei, E.; Benatti, S.; Mancini, L.; Maldonado, J.; Biazzo, K.; Esposito, M.; Frustagli, G.; González Álvarez, E.; Micela, G.; Scandariato, G.; Sozzatti, A.; Affer, L.; Bignamini, A.; Bonomo, A. S.; Claudi, R.; Cosentino, R.; Covino, E.; Fiorenzano, A. F. M.; Giacobbe, P.; Harutyunyan, A.; Leto, G.; Maggio, A.; Molinari, E.; Nascimbeni, V.; Pagano, I.; Pedani, M.; Piotto, G.; Poretti, E.; Rainer, M.; Redfield, S.; Baffa, C.; Baruffolo, A.; Buschschacher, N.; Billoti, V.; Cecconi, M.; Falcini, G.; Fantinel, D.; Fini, L.; Galli, A.; Ghedina, A.; Ghinassi, F.; Giani, E.; Guerra, J.; Hernández Díaz, M.; Hernández, N.; Luzzolino, M.; Lodi, M.; Oliva, E.; Origlia, L.; Pérez Ventura, H.; Puglisi, A.; Riverol, C.; Riverol, L.; San Juan, J.; Sanna, N.; Scuderi, S.; Seemann, U.; Sozzi, M.; Tozzi, P.; González Hernández, Carmen; Jimeno González, María; Agenzia Spaziale Italiana (ASI); European Commission (EC); Claudi, R. [0000-0001-7707-5105]; Leto, G. [0000-0002-0040-5011]; Piotto, G. [0000-0002-9937-6387]; Bonomo, A. S. [0000-0002-6177-198X]; Sozzetti, A. [0000-0002-7504-365X]; Biazzo, K. [0000-0002-1892-2180]; Ghedina, A. [0000-0003-4702-5152]; Damasso, M. [0000-0001-9984-4278]; Cosentino, R. [0000-0003-1784-1431]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Context. The existence of hot Jupiters is still not well understood. Two main channels are thought to be responsible for their current location: a smooth planet migration through the protoplanetary disk or the circularization of an initial highly eccentric orbit by tidal dissipation leading to a strong decrease in the semimajor axis. Different formation scenarios result in different observable effects, such as orbital parameters (obliquity and eccentricity) or frequency of planets at different stellar ages. Aims. In the context of the GAPS Young Objects project, we are carrying out a radial velocity survey with the aim of searching and characterizing young hot-Jupiter planets. Our purpose is to put constraints on evolutionary models and establish statistical properties, such as the frequency of these planets from a homogeneous sample. Methods. Since young stars are in general magnetically very active, we performed multi-band (visible and near-infrared) spectroscopy with simultaneous GIANO-B + HARPS-N (GIARPS) observing mode at TNG. This helps in dealing with stellar activity and distinguishing the nature of radial velocity variations: stellar activity will introduce a wavelength-dependent radial velocity amplitude, whereas a Keplerian signal is achromatic. As a pilot study, we present here the cases of two known hot Jupiters orbiting young stars: HD 285507 b and AD Leo b. Results. Our analysis of simultaneous high-precision GIARPS spectroscopic data confirms the Keplerian nature of the variation in the HD 285507 radial velocities and refines the orbital parameters of the hot Jupiter, obtaining an eccentricity consistent with a circular orbit. Instead, our analysis does not confirm the signal previously attributed to a planet orbiting AD Leo. This demonstrates the power of the multi-band spectroscopic technique when observing active stars.