Negative and Positive Outflow-Feedback in Nearby (U)LIRGs

Cazzoli, S.

doi:10.3389/fspas.2017.00062

Cited by 2 publications

(1 citation statement)

References 26 publications

(34 reference statements)

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“…However, this is a complex process to understand. (i) Merger-induced star-burst and AGN activity consume gas, (ii) they also blow out the gas through negative feedback, and (iii) AGN contributes to star-formation (positive feedback) during the merger in some galaxies like ultra-luminous infrared galaxies (ULIRGs) (e.g., [70]). So, galaxy mergers and AGN may work together [71,72].…”

Section: Galaxy Merger and Feedbackmentioning

confidence: 99%

AGN Feedback Signatures in UV Emission

Rubinur

2024

Galaxies

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Supermassive black holes (SMBH) are believed to influence galaxy evolution through AGN (active galactic nuclei) feedback. Galaxy mergers are key processes of galaxy formation that lead to AGN activity and star formation. The relative contribution of AGN feedback and mergers to star formation is not yet well understood. In radio-loud objects, AGN outflows are dominated by large jets. However, in radio-quiet objects, outflows are more complex and involve jet, wind, and radiation. In this review, we discuss the signatures of AGN feedback through the alignment of radio and UV emissions. Current research on AGN feedback is discussed, along with a few examples of studies such as the galaxy merger system MRK 212, the radio-quiet AGN NGC 2639, and the radio-loud system Centaurus A. Multi-frequency observations of MRK 212 indicate the presence of dual AGN, as well as feedback-induced star-forming UV clumps. The fourth episode of AGN activity was detected in radio observations of the Seyfert galaxy NGC 2639, which also showed a central cavity of 6 kpc radius in CO and UV maps. This indicates that multi-epoch jets of radio-quiet AGN can blow out cold molecular gas, which can further reduce star formation in the center of the galaxies. Recent UV observations of Cen A have revealed two sets of stellar population in the northern star-forming region, which may have two different origins. Recent studies have shown that there is evidence that both positive and negative feedback can be present in galaxies at different scales and times. High-resolution, multi-band observations of large samples of different types of AGN and their host galaxies are important for understanding the two types of AGN feedback and their effect on the host galaxies. Future instruments like INSIST and UVEX will be able to help achieve some of these goals.

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Section: Galaxy Merger and Feedbackmentioning

confidence: 99%

AGN Feedback Signatures in UV Emission

Rubinur

2024

Galaxies

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Role of AGN and star formation feedback in the evolution of galaxy outflows

Clavijo-Bohórquez,

de Gouveia Dal Pino,

Melioli

2024

Monthly Notices of the Royal Astronomical Society

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We conducted 3D-MHD simulations to investigate the feedback processes in the central 1-kpc scale of galaxies hosting both active star formation (SF) and an AGN wind. Our simulations naturally generated a turbulent and clumpy interstellar medium driven by SF evolution. We found that the AGN wind duty cycle plays a crucial role in shaping the evolution of the outflows. A single duty cycle (which can repeat several times over the galaxy lifetime) consists of an active, a remnant and an inactive phase, lasting up to 1.5 Myr in our simulations. The duration of the cycle increases with larger star formation rate (SFR) and smaller AGN wind power (tested for luminosities 1042 − 1044 erg s−1 and SFR=1 – 1000 M⊙ yr−1). The feedback on SF, whether positive or negative, depends on various factors, including the AGN outflow opening angle, power, and phase of activity, as well as the initial SFR. The passage of the AGN wind enhances SF in a ring around it, resembling the structures observed in ULIRGs and LINERS, and is stronger for larger AGN power or SFR. Also, a higher SFR enhances the mixing of interstellar matter with the AGN wind, resulting in a greater number of colder, denser structures with volume filling factors ∼ 0.02 to 0.12 and velocities comparable to those observed in Seyferts and LINERs, but smaller than those observed in ULIRGs. The efficiency of the AGN wind in transporting mass to kiloparsec distances diminishes with increasing SFR. The mass loss rates range from 50 to 250 M⊙ yr−1 within the initial 2 Myr of evolution, which aligns with observed rates in nearby Seyferts and ULIRGs.

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Negative and Positive Outflow-Feedback in Nearby (U)LIRGs

Cited by 2 publications

References 26 publications

AGN Feedback Signatures in UV Emission

AGN Feedback Signatures in UV Emission

Role of AGN and star formation feedback in the evolution of galaxy outflows

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