Examinando por Autor "Padovani, P."

Mostrando 1 - 3 de 3

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.