Radiative Driving of the AGN Outflows in the Narrow-line Seyfert 1 Galaxy NGC 4051*
               
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Meena, Beena; Crenshaw, D. Michael; Schmitt, H. R.; Revalski, Mitchell; Fischer, Travis C.; Polack, Garrett E.; Kraemer, S. B.; Dashtamirova, Dzhuliya

doi:10.3847/1538-4357/ac0246

Cited by 14 publications

(17 citation statements)

References 137 publications

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“…We consider several outflow radial velocity profiles, motivated by previous works in the literature (e.g. Förster Schreiber et al 2014;Venturi et al 2018;Meena et al 2021), and different outflow inclinations with respect to the line of sight. More details on the simulations can be found in the appendix A.…”

Section: Caveats: Methods To Measure Outflow Parametersmentioning

confidence: 99%

Physics of ULIRGs with MUSE and ALMA: The PUMA project

Lamperti

Pereira-Santaella

Perna

et al. 2022

A&A

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We study molecular outflows in a sample of 25 nearby (z < 0.17, d < 750 Mpc) ultra-luminous infrared galaxy (ULIRG) systems (38 individual nuclei) as part of the Physics of ULIRGs with MUSE and ALMA (PUMA) survey, using ∼ 400 pc (0.1-1.0" beam FWHM) resolution ALMA CO(2-1) observations. We used a spectro-astrometry analysis to identify high-velocity (> 300 km s −1 ) molecular gas disconnected from the galaxy rotation, which we attribute to outflows. In 77% of the 26 nuclei with log L IR /L > 11.8, we identified molecular outflows with an average v out = 490 km s −1 , outflow masses 1 − 35 × 10 7 M , mass outflow rates Ṁout = 6 − 300 M yr −1 , mass-loading factors η = Ṁout /S FR = 0.1−1, and an average outflow mass escape fraction of 45±6%. The majority of these outflows (18/20) are spatially resolved with radii of 0.2 − 0.9 kpc and have short dynamical times (t dyn = R out /v out ) in the range 0.5 − 2.8 Myr. The outflow detection rate is higher in nuclei dominated by starbursts (SBs, 14/15 = 93%) than in active galactic nuclei (AGN, 6/11 = 55%). Outflows perpendicular to the kinematic major axis are mainly found in interacting SBs. We also find that our sample does not follow the Ṁout versus AGN luminosity relation reported in previous works. In our analysis, we include a sample of nearby main-sequence galaxies (SFR = 0.3 − 17 M yr −1 ) with detected molecular outflows from the PHANGS-ALMA survey to increase the L IR dynamic range. Using these two samples, we find a correlation between the outflow velocity and the star-formation rate (SFR), as traced by L IR (v out ∝ S FR 0.25±0.01 ), which is consistent with what was found for the atomic ionised and neutral phases. Using this correlation, and the relation between M out /R out and v out , we conclude that these outflows are likely momentum-driven. Finally, we compare the CO outflow velocities with the ones derived from the OH 119µm doublet. In 76% of the targets, the outflow is detected in both CO and OH, while in three targets (18%) the outflow is only detected in CO, and in one target the outflow is detected in OH but not in CO. The difference between the OH and CO outflow velocities could be due to the far-IR background source required by the OH absorption which makes these observations more dependent on the specific outflow geometry.

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Section: Caveats: Methods To Measure Outflow Parametersmentioning

confidence: 99%

Physics of ULIRGs with MUSE and ALMA: The PUMA project

Lamperti

Pereira-Santaella

Perna

et al. 2022

A&A

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“…The outflows in AGNs can be pushed by the line-driven force (e.g., Dannen et al 2019;Dyda & Proga 2018;Mas-Ribas & Mauland 2019), and accretion disk winds driven by the line force have the increasing velocity with roughly decreasing acceleration from the black hole to the far (Nomura et al 2020). Observations show the various outflows at accretion disk scales, the BLR scales, the NLR scales and the kpc scales, driven by F r from AGNs (Kang & Woo 2018;Meena et al 2021;Singha et al 2021). Thus, F r is prevalent, and might contribute to the force budget for inflow, e.g., F r decelerates inflow (Ferland et al 2009).…”

Section: Discussionmentioning

confidence: 99%

Measuring the Virial Factor in SDSS DR5 Quasars with Redshifted H$β$ and Fe ii Broad Emission Lines

Liu,

Feng,

et al. 2022

Preprint

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Under the hypothesis of gravitational redshift induced by the central supermassive black hole, and based on line widths and shifts of redward shifted Hβ and Fe ii broad emission lines for a sample of 1973 z < 0.8 SDSS DR5 quasars, we measured the virial factor in determining supermassive black hole masses, usually estimated by the reverberation mapping (RM) method or the relevant secondary methods. The virial factor had been believed to be from the geometric effect of broad-line region. The measured virial factor of Fe ii is larger than that of Hβ for 98% of these quasars. The virial factor is very different from object to object and for different emission lines. For most of these quasars, the virial factor of Hβ is larger than these averages that were usually used in determining the masses of black holes. There are three positive correlations among the measured virial factor of Hβ, dimensionless accretion rate and Fe ii/Hβ line ratio. A positive three-dimensional correlation is found among these three quantities, and this correlation indicates that the virial factor is likely dominated by the dimensionless accretion rate and metallicity. A negative correlation is found between the redward shift of Hβ and the scaled size of broad-line region radius in units of the gravitational radius of black hole. This negative correlation will be expected naturally if the redward shift of Hβ is mainly from the gravity of black hole. Radiation pressure from accretion disk may be a significant contributor to the virial factor.Subject headings: Active galactic nuclei (16) -Black hole physics (159) -Emission line galaxies (459) -Quasars (1319) -Supermassive black holes (1663)

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“…Following Zhang et al (2015) and Fu et al (2017), we model the emission lines using XSTAR. Some previous work adopted other approaches for modeling the emission line, such as multiple Gaussians (e.g., He et al 2017;Meena et al 2021), piecewise function, or spline fit (e.g., Veilleux et al 2022). To generate those photoionization components in XSTAR, we fit the strong emission lines with Gaussian models to measure the FWHM of each line and derive the Doppler broadening parameter or turbulent velocity.…”

Section: Spectral Analysis and Modelingmentioning

confidence: 99%

“…The velocity of the outflow is usually several hundred to several thousand kilometers per second (McKernan et al 2007); hence, it can propagate to a location of about 10 kpc (assuming a ∼10 million year lifetime of the AGN) away from the central black hole. In order to investigate the feedback efficiency of the AGN, it is necessary to quantify the physical properties of the outflows (Meena et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Fast Outflowing Warm Absorbers in Narrow-line Seyfert 1 Galaxy PG 1001+054 Revealed by HST/COS Spectra

Wang

et al. 2023

ApJ

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Narrow-line Seyfert 1 (NLS1) galaxies are an important type of active galactic nucleus (AGN), generally expected to be accreting at a high Eddington rate. The properties of their outflows and importance of AGN feedback remain intriguing. We report on the discovery of fast outflowing warm absorbers (WAs) in the NLS1 PG 1001+054 with velocities in the range of ∼7000–9000 km s−1. They are identified with blueshifted Lyα, N v, and Si iv lines in the high-resolution ultraviolet (UV) spectra taken with the Cosmic Origins Spectrograph on board the Hubble Space Telescope. We perform photoionization modeling using XSTAR with three WAs. The derived physical properties are typical of WAs in terms of ionization and column density, whereas the outflow velocities are significantly higher. The estimated location of these WAs ranges from 1 to 73 parsecs away from the AGN. Together with previous detection of high ionization absorbers in the X-ray for PG 1001+054, we suggest that fast outflowing UV absorbers are probably part of a multiphase outflow. Such a structure is likely produced by the outflow launched from the AGN at an accretion disk scale, which shocks the ambient interstellar medium (ISM), producing stratified absorbers. Assuming contribution from the three WAs at tens of parsecs, the estimated ratio between the kinetic power of the outflow and AGN Eddington luminosity could reach 1.7%, raising the possibility of sufficient influence on the host galaxy when compared to some theoretical models for efficient AGN feedback.

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Radiative Driving of the AGN Outflows in the Narrow-line Seyfert 1 Galaxy NGC 4051* †

Cited by 14 publications

References 137 publications

Physics of ULIRGs with MUSE and ALMA: The PUMA project

Physics of ULIRGs with MUSE and ALMA: The PUMA project

Measuring the Virial Factor in SDSS DR5 Quasars with Redshifted H$β$ and Fe ii Broad Emission Lines

Fast Outflowing Warm Absorbers in Narrow-line Seyfert 1 Galaxy PG 1001+054 Revealed by HST/COS Spectra

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