The Nuclear Region of NGC 1365: Star Formation, Negative Feedback, and Outflow Structure

Gao, Yongheng; Egusa, Fumi; Liu, Guilin; Kohno, Kotaro; Bao, Min; Morokuma-Matsui, Kana; Kong, Xu; Chen, Xiaoyang

doi:10.3847/1538-4357/abf738

Cited by 23 publications

(29 citation statements)

References 93 publications

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“…As discussed in Section 2.3 and 4.5, there are traces of AGN-driven outflows that can contribute to the enhanced velocity dispersions discussed above, quenching the star formation in the innermost regions of NGC 3169. Similar negative feedback mechanisms are discussed in recent works of Venturi et al (2021) and Gao et al (2021). On the other hand, we also identified a fraction of AGN-ionisation in the star-forming ring, associated with diffuse emissions surrounding the H𝛼 peaks (see Section 3.3).…”

Section: Agn Feedbacksupporting

confidence: 86%

WISDOM project -- XI. Star Formation Efficiency in the Bulge of the AGN-host Galaxy NGC 3169 with SITELLE and ALMA

Lu,

Boyce,

Haggard

et al. 2022

Preprint

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The star formation efficiency (SFE) has been shown to vary across different environments, particularly within galactic starbursts and deep within the bulges of galaxies. Various quenching mechanisms may be responsible, ranging from galactic dynamics to feedback from active galactic nuclei (AGN). Here, we use spatially-resolved observations of warm ionised gas emission lines (H𝛽, [O ] 𝜆𝜆4959,5007, [N ] 𝜆𝜆6548,6583, H𝛼 and [S ] 𝜆𝜆6716,6731) from the imaging Fourier transform spectrograph SITELLE at the Canada-France-Hawaii Telescope (CFHT) and cold molecular gas ( 12 CO(2-1)) from the Atacama Large Millimeter/submillimeter Array (ALMA) to study the SFE in the bulge of the AGN-host galaxy NGC 3169. After distinguishing star-forming regions from AGN-ionised regions using emission-line ratio diagnostics, we measure spatially-resolved molecular gas depletion times (𝜏 dep ≡1/SFE) with a spatial resolution of ≈ 100 pc within a galactocentric radius of 1.8 kpc. We identify a star-forming ring located at radii 1.25 ± 0.6 kpc with an average 𝜏 dep of 0.3 Gyr. At radii < 0.9 kpc, however, the molecular gas surface densities and depletion times increase with decreasing radius, the latter reaching approximately 2.3 Gyr at a radius ≈ 500 pc. Based on analyses of the gas kinematics and comparisons with simulations, we identify AGN feedback, bulge morphology and dynamics as the possible causes of the radial profile of SFE observed in the central region of NGC 3169.

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Section: Agn Feedbacksupporting

confidence: 86%

WISDOM project -- XI. Star Formation Efficiency in the Bulge of the AGN-host Galaxy NGC 3169 with SITELLE and ALMA

Lu,

Boyce,

Haggard

et al. 2022

Preprint

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“…Warm ionized gas outflows ( -T K 10 4 ) traced by [O III] and [N II]+Hα are prevalent in AGNs and star-forming galaxies. Integral field spectroscopy (IFS) provides more detailed information such as spatial resolved kinematics, ionization structure, and morphology of ionized outflows, which enables better understanding of physical processes in outflows (e.g., Harrison et al 2014;Wylezalek et al 2017;Venturi et al 2018;López-Cobá et al 2020;Gao et al 2021;Dall'Agnol de Oliveira et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Spatially Resolved Ionized Outflows Extending to ∼ 2 kpc in Seyfert 1 Galaxy NGC 7469 Revealed by the Very Large Telescope/MUSE

Wang

2022

ApJ

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The Seyfert 1 galaxy NGC 7469 possesses a prominent nuclear starburst ring and a luminous active galactic nucleus (AGN). Evidence of an outflow in the innermost nuclear region has been found in previous works. We detect the ionized gas outflow on a larger scale in the galaxy using the archival Very Large Telescope/MUSE and Chandra observations. The optical emission lines are modeled using two Gaussian components, and a nonparametric approach is applied to measure the kinematics of [O iii] and Hα emitting gas. Line ratio diagnostics and spatially resolved maps are derived to examine the origin of the outflow. The kiloparsec-scale kinematics of [O iii] are dominated by a blueshifted component whereas the velocity map of Hα shows a rotational disk with a complex nonrotational substructure. The starburst wind around the circumnuclear ring is confirmed, and we find evidence of an AGN-driven outflow extending to a radial distance of ∼ 2 kpc from the nucleus, with a morphology consistent with a nearly face-on ionization cone. The previously reported circumnuclear outflow resembles part of the bright base. We derive mass and energy outflow rates for both the starburst wind and the AGN-driven outflow. The estimated kinetic coupling efficiency of the kiloparsec-scale AGN outflow is E ̇ out / L bol ∼ 0.1 % , lower than the threshold predicted by the “two-stage” theoretical model for effective feedback. Our results reinforce the importance of spatially resolved study to disentangle feedback where AGNs and starbursts coexist, which may be common during the cosmic noon of black hole and galaxy growth.

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“…Kara et al (2015) estimated soft lag due to the presence of an eclipsing cloud along the line of sight using NuSTAR observations. The star formation and gas accretion to the central object were studied using near-infrared (NIR) data by Fazeli et al (2019) and Gao et al (2021) to check for more recent star formation activities and outflow structure of the source.…”

Section: Introductionmentioning

confidence: 99%

Variable mass accretion and failed wind explain changing-look phenomena in NGC 1365

Mondal

Adhikari

Hryniewicz

et al. 2022

A&A

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Changing-look active galactic nuclei (CLAGNs) show a complex nature in their X-ray spectral shape and line-of-sight column-density variation. The physical mechanisms responsible for these variations are unclear. Here, we study the spectral properties of a CLAGN, NGC 1365 using combined XMM-Newton and NuSTAR observations to understand the CL behavior. The model-fitted mass-accretion rate varied between 0.003 ± 0.001 and 0.009 ± 0.002 ṀEdd and the dynamic corona changed from 28 ± 3 to 10 ± 1 rg. We found that the variable absorption column density correlates with the mass accretion rate and the geometry of the corona. The derived wind velocity was sufficiently low compared to the escape velocity to drive the wind away from the disc for the epochs during which column densities were high. This suggests that the high and variable absorption can be due to failed winds from the disc. Our estimated ratio of mass outflow to inflow rate from the inner region of the disc lies between 0.019 ± 0.006 and 0.12 ± 0.04. From spectral fitting of the combined data, we found the mass of the central black hole to be constant 4.38 ± 0.34−4.51 ± 0.29 × 106 M⊙, consistent with earlier findings. The confidence contours of NH with other model parameters show that the model-fitted parameters are robust and non-degenerate. Our study construed that the changing accretion rate, which is a fundamental physical quantity and the geometry of the corona are driving the CL phenomena in NGC 1365. The physical picture considered in this work connects both variable continuum and variable absorbing medium scenarios.

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The Nuclear Region of NGC 1365: Star Formation, Negative Feedback, and Outflow Structure

Cited by 23 publications

References 93 publications

WISDOM project -- XI. Star Formation Efficiency in the Bulge of the AGN-host Galaxy NGC 3169 with SITELLE and ALMA

WISDOM project -- XI. Star Formation Efficiency in the Bulge of the AGN-host Galaxy NGC 3169 with SITELLE and ALMA

Spatially Resolved Ionized Outflows Extending to ∼ 2 kpc in Seyfert 1 Galaxy NGC 7469 Revealed by the Very Large Telescope/MUSE

Variable mass accretion and failed wind explain changing-look phenomena in NGC 1365

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