The MEGARA/GTC Optical Perspective on the X-ray Ultra-Fast Outflow (UFO) in IRAS17020+4544

“The MEGARA/GTC Optical Perspective on the X-ray Ultra-Fast Outflow (UFO) in IRAS17020+4544" “IV IPARCOS congress”, 10th Dec 2025 Enrica Bellocchi (Universidad Complutense de Madrid) In collaboration with A. Longinotti (UNAM), Q. Salomé (Univ. of Turku), A. Gil de Paz (UCM), J. P. Torres-Papaqui (UGTO), D. Mayya (INAOE), Y. Krongold (UNAM), A. Castillo Morales (UCM), A. Robleto (UNAN), C. Catalán-Torrecilla (UCM), O. Vega (INAOE), D. Rosa González (INAOE) ESA/ATG medialab/NASA/CXC y Nahks Tr’Ehn CO(1-0) molecular blueshifted wind SDSS image IRAS17020 PID2022-138621NB-I00 and PID2021-123417OB-I00, funded by MCIN/AEI/10.13039/501100011033/FEDER, EU Why AGN outflow are so important? •Outflows may provide the connection between BH and host galaxies required to reconcile theory & observations →they carry out mass and energy out to larger scales The activity of the BH influences the life of the galaxy ! (Silk & Rees 1998; King 2003) •If this material eventually leaves the AGN, then outflows might carry significant mass out of the AGN and, as a consequence, give a substantial contribution to the chemical enrichment ofthe IGM •MBH-𝛔★(Kormendy & Ho 2013): nuclear and galaxy scale relation (King et al. 2003) supported by theoretical models and hydrodinamical simulations of galaxy formation and evolution (e.g., Di Matteo et al. 2005, Hopkins & Elvis 2010) →tight coupling between the growth ofthe central BH & the bulge ofits host Galaxy →Feedback by AGN as key ingredient for regulating star formation and clearing up the gas in galaxies (Zubovas & King 2012) Cicone et al. 2018 MBH (M⨀) 𝝈★(km s-1) Kormendy & Ho 2013 Outflows can be: Multi-phase → highly ionized, warm ionized, neutral atomic and molecular Ultra Fast Outflow (UFO): These outflows are characterized by mildly relativistic speeds (v ~ 0.1-0.3 c), high ionization states, and prominent blueshifted X-ray absorption lines (Fe K band) Cicone et al. 2018; Harrison et al. 2017, 2018 Kew questions: 1) What are the mechanisms responsible for launching UFOs? 2) Are the different gas phases connected? 3) How does the nuclear X-ray wind transfer its energy from nuclear to galaxy-scale? Tombesi et al. 2010a, b, 2015; Chartas et al. 2014; Nardini et al. 2015, Matzeu et al. 2017, 2019; Parker et al. 2017; Reeves et al. 2020; Laurenti et al. 2021 … Zubovas & King 2012 (Faucher-Giguere+2012, King & Pounds 2015) The nuclear, ultra fast X-ray wind (vout ≥ 104km/s) interacts with the galaxy ISM in shock processes oIn the momentum-driven case, the narrow shocks rapidly cool to become effectively isothermal, leading to very low kinetic energy. oIn the energy-driven outflow, the shocked regions are much wider and do not cool →Their adiabatic expansion transfers most ofthe kinetic energy ofthe wind to the large scale outflow Transfer of wind energy to large scales →Outflow momentum rate Multi-wavelength campaign can help: →to understand the effect ofa powerful nuclear X-ray wind during its encounter through the ISM →to follow the evolution ofthe shocked outflow initiated by this wind in its propagation at larger scale →Momentum boost in the “energy conserving" regime → “The cooling of the shocked wind, rather than the shocked ambient medium, that determines whether the outflow is energyor momentum conserving (King+2011)”. Our targets are Narrow Line Seyfert 1 (NLSy1) Galaxies hosting an UFO ❑NLSy1s are one of the key AGN subclasses in investigating the origin of the MBH-𝝈★ relation because of their high accretion rate and significantly low MBH →these two characteristics may imply that NLS1s are young phases of AGNs (Mathur et al. 2001; Véron-Cetty et al. 2001; Boroson 2002, Woo+2015) ❑What do we know about NLSy1 with UFO? Not much... (e.g., Marasco et al.2020, Tozzi et al.2021…) •Sy1 Galaxies with exceptionallynarrow Balmer lines (Osterbrock & Pogge 1985) •FWHM Hβ<2000 km/s, [OIII]5007/Hβ <3, strong FeII lines •Strong X-ray variability & Steep X-ray power law continua •Smaller MBH (~106 -108 M⨀) •High Accretion Rates Ṁ = LBol/LEDD related to high radiative efficiency drives disk winds (e.g. Komossa et al. 2018, Boroson et al. 2011, Panessa et al. 2011, Berton & Jrvel 2021) 1s 2s Blazars The case of the NLSy1 IRAS17020+4544 →Multi-wavelength campaign in the last years (X-ray, sub-mm, radio bands…) XMM-Newton X-ray spectrum: a stratified, multi-component wind 5 UFO distinct components wide range of ionization, NHoutflowing and velocity range v~0.1-0.3 c → UFO launched at the accretion disk scale ❑Fast + Slow winds with complex velocity pattern in IRAS17 (Longinotti et al. 2015, see also Sanfrutos et al. 2018) Large Millimeter Telescope (LMT): fast molecular outflow Massive molecular blueshifted outflow (Δv = -660 km/s) wInd force / radiation force The molecular outflow follows the "energyconserving” regime (Longinotti et al. 2018) - Host galaxy is a (barred) Sp -z ~0.0612 (1.181 kpc/arsec) - Small MBH ~6 ×106 M⨀ - High Ṁ= LBol/LEDD~0.7 The case of the NLSy1 IRAS17020+4544 NOEMA (NOrthern Extended Millimeter Array) PdB Interferometry Salomé et al. 2021 Salomé et al. 2021 found that the molecular gas is distributed into a central disc-like structure of ~109M⨀→Discovery of a companion toward the North located up to8 kpc (possibily interacting with IRAS17, at the early phase of merger) with a molecular gas mass MH2∼108M⨀ R-band image taken by the ALFOSC/NOT with CO contours (white) Longinotti et al. 2023 Chandra X-ray RCO = 2.8 ±0.3 kpc radio emission VLBI e-MERLIN @ 1.5 GHz Blue and red contours trace the approaching and recedingmolecular outflowing gas Giroletti et al. 2017 CO(1-0) systemic emission CO(1-0) outflowemission NOEMA results confirm the “energy-conserving” regime for the spatially resolved molecular outflow (Longinotti et al. 2023) →Multi-wavelength campaign in the last years (X-ray, sub-mm, radio bands…) Within the framework of the “MATRIOSKA” Project [Multiphase nAture of ulTra-fast outflows in naRrow lIne seyfert 1: the Optical Survey and Kinematic Analysis] →we present the analysis of IRAS 17020+4544 using MEGARA/GTC In this work we used MEGARA/GTC IFU to characterize the ionized gas phase in the optical band as traced by the H𝛂and [OIII] emission lines Gil de Paz, A. et al. 2018 Carrasco et al. 2018 Castillo-Morales, A. et al. 2020 ✓We use MEGARA/GTC data at low- (LR, R=6000) and medium-resolution (MR; R=12,000), with FWHM~1") to characterize the ionized outflow, which covers the region encompassed by the resolved, powerful molecular outflow ✓Multi-Gaussian line fit allowed us to derive its kinematics and energetics (velocity, mass, kinetic power, and momentum), we evaluate the outflow’s energy budget and compare it with that of the molecular and X-ray phases and check if the ionized gas phase also follows an “energy-conserving” regime, as previously found for the molecular phase (Longinotti et al. 2023) Bellocchi et al. submitted to A&A PI: Longinotti A. spatial resolution 0.62” (hexagonal spaxel) MEGARA = Multi-Espectrógrafo en GTC de Alta Resolución para Astronomía Multi Gaussian (3c) line fit using MEGARA/GTC data →[OI], H𝛂+[NII], [SII] →H𝛃-[OIII] →H𝛃-[OIII] Nuclear region (LR-R) Nuclear region (MR-G)