Examinando por Autor "Vignali, C."

Mostrando 1 - 7 de 7

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.
Restringido
Mid-IR cosmological spectrophotometric surveys from space: Measuring AGN and star formation at the cosmic noon with a SPICA-like mission
(Cambridge University Press, 2021-04-23) Spignoglio, L.; Mordini, S.; Fernández Ontiveros, J. A.; Alonso Herrero, A.; Armus, L.; Bisigello, L.; Calura, F.; Carrera, F. J.; Cooray, A.; Dannerbauer, H.; Decarli, R.; Egami, E.; Elbaz, D.; Franceschini, A.; González Alfonso, E.; Graziani, L.; Gruppioni, C.; Hatziminaoglou, Evanthia; Kaneda, H.; Kohno, K.; Labiano, Á.; Magdis, Georgios E.; Malkan, M. A.; Matsuhara, H.; Nagao, T.; Naylor, D.; Pereira Santaella, M.; Pozzi, F.; Rodighiero, G.; Roelfsema, P.; Serjeant, S.; Vignali, C.; Wang, L.; Yamada, T.; Agenzia Spaziale Italiana (ASI); Agencia Estatal de Investigación (AEI); Comunidad de Madrid; Spignoglio, L. [0000-0001-8840-1551]; Fernández Ontiveros, J. A. [0000-0001-9490-899X]; Gruppioni, C. [0000-0002-5836-4056]; Graziani, L. [0000-0002-9231-1505]; Unidad de Excelencia Científica María de Maeztu Instituto de Astrofísica de Cantabria, MDM-2017-0765; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
We use the SPace Infrared telescope for Cosmology and Astrophysics (SPICA) project as a template to demonstrate how deep spectrophotometric surveys covering large cosmological volumes over extended fields (1– ) with a mid-IR imaging spectrometer (17– ) in conjunction with deep photometry with a far-IR camera, at wavelengths which are not affected by dust extinction can answer the most crucial questions in current galaxy evolution studies. A SPICA-like mission will be able for the first time to provide an unobscured three-dimensional (3D, i.e. x, y, and redshift z) view of galaxy evolution back to an age of the universe of less than 2 Gyrs, in the mid-IR rest frame. This survey strategy will produce a full census of the Star Formation Rate (SFR) in the universe, using polycyclic aromatic hydrocarbons (PAH) bands and fine-structure ionic lines, reaching the characteristic knee of the galaxy luminosity function, where the bulk of the population is distributed, at any redshift up to . Deep follow-up pointed spectroscopic observations with grating spectrometers onboard the satellite, across the full IR spectral range (17– ), would simultaneously measure Black Hole Accretion Rate (BHAR), from high-ionisation fine-structure lines, and SFR, from PAH and low- to mid-ionisation lines in thousands of galaxies from solar to low metallicities, down to the knee of their luminosity functions. The analysis of the resulting atlas of IR spectra will reveal the physical processes at play in evolving galaxies across cosmic time, especially its heavily dust-embedded phase during the activity peak at the cosmic noon ( –3), through IR emission lines and features that are insensitive to the dust obscuration.
Acceso Abierto
SUPER II. Spatially resolved ionised gas kinematics and scaling relations in z ∼ 2 AGN host galaxies
(EDP Sciences, 2020-10-13) Kakkad, D.; Mainieri, V.; Vietri, G.; Carniani, S.; Harrison, C. M.; Perna, M.; Scholtz, J.; Circosta, C.; Cresci, G.; Husemann, B.; Bischetti, M.; Feruglio, C.; Fiore, F.; Marconi, A.; Padovani, P.; Brusa, M.; Cicone, C.; Comastri, A.; Lanzuisi, G.; Mannucci, F.; Menci, N.; Netzer, H.; Piconcelli, E.; Puglisi, A.; Salvato, M.; Schramm, M.; Silverman, J.; Vignali, C.; Zamorani, G.; Zappacosta, L.; Comunidad de Madrid; Kakkad, D. [0000-0002-2603-2639]; Manieri, V. [0000-0002-1047-9583]; Vietri, G. [0000-0001-9155-8875]; Carniani, S. [0000-0002-6719-380X]; Perna, M. [0000-0002-0362-5941]; Creci, G. [0000-0002-5281-1417]; Husemann, B. [0000-0003-2901-6842]; Bischetti, M. [0000-0002-4314-021X]; Fiore, F. [0000-0002-4031-4157]; Marconi, A. [0000-0002-9889-4238]; Padovani, P. [0000-0002-4707-6841]; Cicone, C. [0000-0003-0522-6941]; Comastri, A. [0000-0003-3451-9970]; Mannucci, F. [0000-0002-4803-2381]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Aims. The SINFONI survey for Unveiling the Physics and Effect of Radiative feedback (SUPER) aims to trace and characterise ionised gas outflows and their impact on star formation in a statistical sample of X-ray selected active galactic nuclei (AGN) at z ∼ 2. We present the first SINFONI results for a sample of 21 Type 1 AGN spanning a wide range in bolometric luminosity (log Lbol = 45.4–47.9 erg s−1). The main aims of this paper are to determine the extension of the ionised gas, characterise the occurrence of AGN-driven outflows, and link the properties of such outflows with those of the AGN. Methods. We used adaptive optics-assisted SINFONI observations to trace ionised gas in the extended narrow line region using the [O III] λ5007 line. We classified a target as hosting an outflow if its non-parametric velocity of the [O III] line, w80, was larger than 600 km s−1. We studied the presence of extended emission using dedicated point-spread function (PSF) observations, after modelling the PSF from the Balmer lines originating from the broad line region. Results. We detect outflows in all the Type 1 AGN sample based on the w80 value from the integrated spectrum, which is in the range ∼650–2700 km s−1. There is a clear positive correlation between w80 and the AGN bolometric luminosity (> 99% correlation probability), and the black hole mass (98% correlation probability). A comparison of the PSF and the [O III] radial profile shows that the [O III] emission is spatially resolved for ∼35% of the Type 1 sample and the outflows show an extension up to ∼6 kpc. The relation between maximum velocity and the bolometric luminosity is consistent with model predictions for shocks from an AGN-driven outflow. The escape fraction of the outflowing gas increases with the AGN luminosity, although for most galaxies, this fraction is less than 10%.
Acceso Abierto
SUPER III. Broad Line Region properties of AGN at z
(EDP Sciences, 2020-12-18) Vietri, G.; Mainieri, V.; Kakkad, D.; Netzer, H.; Perna, M.; Circosta, C.; Harrison, C. M.; Zappacosta, L.; Husemann, B.; Padovani, P.; Bischetti, M.; Bongiorno, A.; Brusa, M.; Carniani, S.; Cicone, C.; Comastri, A.; Cresci, G.; Feruglio, C.; Fiore, F.; Lanzuisi, G.; Mannucci, F.; Marconi, A.; Piconcelli, E.; Puglisi, A.; Salvato, M.; Schramm, M.; Schulze, A.; Scholtz, J.; Vignali, C.; Zamorani, G.; Comunidad de Madrid; Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR); Deutsche Forschungsgemeinschaft (DFG); Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Aims. The SINFONI survey for Unveiling the Physics and Effect of Radiative feedback (SUPER) was designed to conduct a blind search for AGN-driven outflows on X-ray-selected AGNs at redshift z ∼ 2 with high (∼2 kpc) spatial resolution, and to correlate them with the properties of their host galaxy and central black hole. The main aims of this paper are: (a) to derive reliable estimates for the masses of the black holes and accretion rates for the Type-1 AGNs in this survey; and (b) to characterise the properties of the AGN-driven winds in the broad line region (BLR). Methods. We analysed rest-frame optical and UV spectra of 21 Type-1 AGNs. We used Hα, Hβ, and MgII line profiles to estimate the masses of the black holes. We used the blueshift of the CIV line profile to trace the presence of winds in the BLR. Results. We find that the Hα and Hβ line widths are strongly correlated, as is the line continuum luminosity at 5100 Å with Hα line luminosity, resulting in a well-defined correlation between black hole masses estimated from Hα and Hβ. Using these lines, we estimate that the black hole masses for our objects are in the range Log (MBH/M⊙) = 8.4–10.8 and are accreting at λEdd = 0.04–1.3. Furthermore, we confirm the well-known finding that the CIV line width does not correlate with the Balmer lines and the peak of the line profile is blueshifted with respect to the [OIII]-based systemic redshift. These findings support the idea that the CIV line is tracing outflowing gas in the BLR for which we estimated velocities up to ∼4700 km s−1. We confirm the strong dependence of the BLR wind velocity on the UV-to-X-ray continuum slope, the bolometric luminosity, and Eddington ratio. We infer BLR mass outflow rates in the range 0.005–3 M⊙ yr−1, revealing a correlation with the bolometric luminosity consistent with that observed for ionised winds in the narrow line region (NLR), and X-ray winds detected in local AGNs, and kinetic power ∼10−7 − 10−4 × LBol. The coupling efficiencies predicted by AGN-feedback models are much higher than the values reported for the BLR winds in the SUPER sample; although it should be noted that only a fraction of the energy injected by the AGN into the surrounding medium is expected to become kinetic power in the outflow. Finally, we find an anti-correlation between the equivalent width of the [OIII] line and the CIV velocity shift, and a positive correlation between this latter parameter and [OIII] outflow velocity. These findings, for the first time in an unbiased sample of AGNs at z ∼ 2, support a scenario where BLR winds are connected to galaxy-scale detected outflows, and are therefore capable of affecting the gas in the NLR located at kiloparsec scale distances.
Acceso Abierto
SUPER IV. CO(J = 3–2) properties of active galactic nucleus hosts at cosmic noon revealed by ALMA
(EDP Sciences, 2021-02-16) Circosta, C.; Mainieri, V.; Lamperti, I.; Padovani, P.; Bischetti, M.; Harrison, C. M.; Kakkad, D.; Zanella, A.; Vietri, G.; Lanzuisi, G.; Salvato, M.; Brusa, M.; Carniani, S.; Cicone, C.; Cresci, G.; Feruglio, C.; Husemann, B.; Mannucci, F.; Marconi, A.; Perna, M.; Piconcelli, E.; Puglisi, A.; Saintonge, A.; Schramm, M.; Vignali, C.; Zappacosta, L.; Science and Technology Facilities Council (STFC); Comunidad de Madrid; Mannucci, F. [0000-0002-4803-2381]
Feedback from active galactic nuclei (AGN) is thought to be key in shaping the life cycle of their host galaxies by regulating star-formation activity. Therefore, to understand the impact of AGN on star formation, it is essential to trace the molecular gas out of which stars form. In this paper we present the first systematic study of the CO properties of AGN hosts at z ≈ 2 for a sample of 27 X-ray selected AGN spanning two orders of magnitude in AGN bolometric luminosity (log Lbol / erg s−1 = 44.7 − 46.9) by using ALMA Band 3 observations of the CO(3-2) transition (∼1″ angular resolution). To search for evidence of AGN feedback on the CO properties of the host galaxies, we compared our AGN with a sample of inactive (i.e., non-AGN) galaxies from the PHIBSS survey with similar redshift, stellar masses, and star-formation rates (SFRs). We used the same CO transition as a consistent proxy for the gas mass for the two samples in order to avoid systematics involved when assuming conversion factors (e.g., excitation corrections and αCO). By adopting a Bayesian approach to take upper limits into account, we analyzed CO luminosities as a function of stellar masses and SFRs, as well as the ratio LCO(3–2)′/M∗ (a proxy for the gas fraction). The two samples show statistically consistent trends in the LCO(3–2)′−LFIR and LCO(3–2)′−M∗ planes. However, there are indications that AGN feature lower CO(3-2) luminosities (0.4–0.7 dex) than inactive galaxies at the 2–3σ level when we focus on the subset of parameters where the results are better constrained (i.e., LFIR ≈ 1012.2 L⊙ and M* > 1011 M⊙) and on the distribution of the mean log(LCO(3–2)′/M∗). Therefore, even by conservatively assuming the same excitation factor r31, we would find lower molecular gas masses in AGN, and assuming higher r31 would exacerbate this difference. We interpret our result as a hint of the potential effect of AGN activity (such as radiation and outflows), which may be able to heat, excite, dissociate, and/or deplete the gas reservoir of the host galaxies. Better SFR measurements and deeper CO observations for AGN as well as larger and more uniformly selected samples of both AGN and inactive galaxies are required to confirm whether there is a true difference between the two populations.
Restringido
The quest for dual and binary supermassive black holes: A multi-messenger view
(Elsevier BV, 2019-12-12) De Rosa, A.; Vignali, C.; Bogdanovic, T.; Capelo, P. R.; Charisi, M.; Dotti, M.; Husemann, B.; Lusso, E.; Mayer, L.; Paragi, Z.; Runnoe, J.; Sesana, A.; Steinborn, L.; Bianchi, S.; Colpi, M.; Del Valle, L.; Frey, S.; Gabányi, K. É.; Giustini, M.; Guainazzi, M.; Haiman, Z.; Herrera Ruiz, N.; Herrero Illana, R.; Iwasawa, K.; Komossa, S.; Lena, D.; Loiseau, N.; Pérez Torres, M.; Piconcelli, E.; Volonteri, M.; Agenzia Spaziale Italiana (ASI); Istituto Nazionale Astrofisica (INAF); National Aeronautics and Space Administration (NASA); Hungarian Scientific Research Fund (OTKA); Hungarian Academy of Sciences (MTA); Deutsche Forschungsgemeinschaft (DFG); European Union COFUND/Durham Junior Research Fellowship (EU); European Research Council (ERC); Swiss National Science Foundation (SNSF); Federal Ministry of Education & Research (BMBF); Ministerio de Economía y Competitividad (MINECO); Comunidad de Madrid; Agencia Estatal de Investigación (AEI); Lena, D. [0000-0003-4184-6152]; Loiseau, N. [0000-0001-5471-3776]; Haiman, Z. [0000-0003-3633-5403]; De Rosa, A. [0000-0001-5668-6863]; Husemann, B. [0000-0003-2901-6842]; Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709; Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Cosmos (ICCUB), MDM-2014-0369; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
The quest for binary and dual supermassive black holes (SMBHs) at the dawn of the multi-messenger era is compelling. Detecting dual active galactic nuclei (AGN) - active SMBHs at projected separations larger than several parsecs - and binary AGN - probing the scale where SMBHs are bound in a Keplerian binary - is an observational challenge. The study of AGN pairs (either dual or binary) also represents an overarching theoretical problem in cosmology and astrophysics. The AGN triggering calls for detailed knowledge of the hydrodynamical conditions of gas in the imminent surroundings of the SMBHs and, at the same time, their duality calls for detailed knowledge on how galaxies assemble through major and minor mergers and grow fed by matter along the filaments of the cosmic web. This review describes the techniques used across the electromagnetic spectrum to detect dual and binary AGN candidates and proposes new avenues for their search. The current observational status is compared with the state-of-the-art numerical simulations and models for formation of dual and binary AGN. Binary SMBHs are among the loudest sources of gravitational waves (GWs) in the Universe. The search for a background of GWs at nHz frequencies from inspiralling SMBHs at low redshifts, and the direct detection of signals from their coalescence by the Laser Interferometer Space Antenna in the next decade, make this a theme of major interest for multi-messenger astrophysics. This review discusses the future facilities and observational strategies that are likely to significantly advance this fascinating field.
Acceso Abierto
The WISSH quasars project VII. The impact of extreme radiative field in the accretion disc and X-ray corona interplay
(EDP Sciences, 2020-03-10) Zappacosta, L.; Piconcelli, E.; Giustini, M.; Vietri, G.; Duras, F.; Miniutti, G.; Bischetti, M.; Bongiorno, A.; Brusa, M.; Chiaberge, M.; Comastri, A.; Feruglio, C.; Luminari, A.; Marconi, A.; Ricci, C.; Vignali, C.; Fiore, F.; Comisión Nacional de Investigación Científica y Tecnológica (CONICYT); Agenzia Spaziale Italiana (ASI); Agencia Estatal de Investigación (AEI); Comunidad de Madrid; Zappacosta, L. [0000-0002-4205-6884]; Piconcelli, E. [0000-0001-9095-2782]; Guistini, M. [0000-0002-1329-658X]; Vietri, G. [0000-0001-9155-8875]; Miniutti, G. [0000-0003-0707-4531]; Bischetti, M. [0000-0002-4314-021X]; Bongiorno, A. [0000-0002-0101-6624]; Chiaberge, M. [0000-0003-1564-3802]; Comastri, A. [0000-0003-3451-9970]; Luminari, A. [0000-0002-1035-8618]; Marconi, A. [0000-0002-9889-4238]; Ricci, C. [0000-0001-5231-2645]; Vignali, C. [0000-0002-8853-9611]; Fiore, F. [0000-0002-4031-4157]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Hyper-luminous quasars (L-bol & x2004;greater than or similar to & x2004;10(47) erg s(-1)) are ideal laboratories to study the interaction and impact of the extreme radiative field and the most powerful winds in the active galactic nuclei (AGN) nuclear regions. They typically exhibit low coronal X-ray luminosity (L-X) compared to the ultraviolet (UV) and mid-infrared (MIR) radiative outputs (L-UV and L-UV); a non-negligible fraction of them report even similar to 1 dex weaker L-X compared to the prediction of the well established L-X-L-UV and L-X-L-UV relations followed by the bulk of the AGN population. In our WISE/SDSS-selected Hyper-luminous (WISSH) z & x2004;=& x2004;2 - 4 broad-line quasar sample, we report on the discovery of a dependence between the intrinsic 2-10 keV luminosity (L2 - 10) and the blueshifted velocity of the CIV emission line (v(CIV)) that is indicative of accretion disc winds. In particular, sources with the fastest winds (v(CIV) greater than or similar to 3000 km s(-1)) possess similar to 0.5-1 dex lower L2 - 10 than sources with negligible v(CIV). No similar dependence is found on L-UV, L-UV, L-bol, the photon index, or the absorption column density. We interpret these findings in the context of accretion disc wind models. Both magnetohydrodynamic and line-driven models can qualitatively explain the reported relations as a consequence of X-ray shielding from the inner wind regions. In case of line-driven winds, the launch of fast winds is favoured by a reduced X-ray emission, and we speculate that these winds may play a role in directly limiting the coronal hard X-ray production.