The triggering of local AGN and their role in regulating star formation

Kaviraj, Sugata; Shabala, Stanislav S.; Deller, Adam T.; Middelberg, E.

doi:10.1093/mnras/stv1329

Cited by 37 publications

(40 citation statements)

References 109 publications

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“…Our results appear consistent with recent work that has suggested a strong connection between merging and the onset of AGN activity at low redshift (e.g. Koss et al 2010;Ellison et al 2011;Scott & Kaviraj 2014;Kaviraj et al 2015), although the role of mergers in triggering AGN may become negligible at high redshift (e.g. Chiaberge & Marconi 2011;Kocevski et al 2012;Schawinski et al 2012).…”

supporting

confidence: 92%

“…Observational work indicates that radio AGN, at least in the local Universe, are more common in early-type galaxies (ETGs). For example, Kaviraj et al (2015) have shown that the detection rate in very long baseline interferometry (VLBI) observations for ETGs is around an order of magnitude higher than in their late-type counterparts, when galaxy stellar mass is controlled for -this is qualitatively similar to the findings of other studies in the literature (e.g. Ledlow et al 2001;Sadler et al 2014).…”

Section: Introductionsupporting

confidence: 82%

“…It is worth noting that the requirements for LTGs to host radio AGN are akin to those in their early-type counterparts that inhabit similar (low-density) environments i.e. massive galaxies that have red colours and are likely to be involved in a merger (Kaviraj et al 2015). Nevertheless, the detection rate in early types is almost an order of magnitude higher (Kaviraj et al 2015).…”

mentioning

confidence: 99%

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Radio AGN in spiral galaxies

Kaviraj

Shabala

Deller

et al. 2015

Mon. Not. R. Astron. Soc.

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Radio AGN in the nearby Universe are more likely to be found in galaxies with early-type morphology, the detection rate in spiral or late-type galaxies (LTGs) being around an order of magnitude lower. We combine the mJy Imaging VLBA Exploration at 20 cm survey with the Sloan Digital Sky Survey, to study the relatively rare population of AGN in LTGs that have nuclear radio luminosities similar to that in their early-type counterparts. The LTG AGN population is preferentially hosted by galaxies that have high stellar masses (M * > 10 10.8 M ), red colours and low star formation rates, with little dependence on the detailed morphology or local environment of the host LTG. The merger fraction in the LTG AGN is ∼4 times higher than that in the general LTG population, indicating that merging is an important trigger for radio AGN in these systems. The red colours of our systems extend recent work which indicates that merger-triggered AGN in the nearby Universe appear after the peak of the associated starburst, implying that they do not strongly regulate star formation. Finally, we find that in systems where parsec-scale jets are clearly observed in our very long baseline interferometry images, the jets are perpendicular to the major axis of the galaxy, indicating strong alignment between the accretion disc and the host galaxy stellar disc.

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supporting

confidence: 92%

Section: Introductionsupporting

confidence: 82%

mentioning

confidence: 99%

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Radio AGN in spiral galaxies

Kaviraj

Shabala

Deller

et al. 2015

Mon. Not. R. Astron. Soc.

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“…We also note that AGN activity has been found to peak during different stages along the merger quenching sequence (Schawinski et al 2010;Koss et al 2010;Ellison et al 2011;Carpineti et al 2012;Kaviraj et al 2015;Carpineti et al 2015). As we discussed above the definition of the post merger and blue early type stage depends on the specifics of the sample and the method used to select, for instance, post merger galaxies.…”

Section: Red Early Type Stagementioning

confidence: 83%

Galaxy Zoo: Major Galaxy Mergers Are Not a Significant Quenching Pathway*

Weigel

Schawinski

Čaplar

et al. 2017

ApJ

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We use stellar mass functions to study the properties and the significance of quenching through major galaxy mergers. In addition to SDSS DR7 and Galaxy Zoo 1 data, we use samples of visually selected major galaxy mergers and post merger galaxies. We determine the stellar mass functions of the stages that we would expect major merger quenched galaxies to pass through on their way from the blue cloud to the red sequence: 1: major merger, 2: post merger, 3: blue early type, 4: green early type and 5: red early type. Based on the similar mass function shapes we conclude that major mergers are likely to form an evolutionary sequence from star formation to quiescence via quenching. Relative to all blue galaxies, the major merger fraction increases as a function of stellar mass. Major merger quenching is inconsistent with the mass and environment quenching model. At z ∼ 0 major merger quenched galaxies are unlikely to constitute the majority of galaxies that transition the green valley. Furthermore, between z ∼ 0 − 0.5 major merger quenched galaxies account for 1 − 5% of all quenched galaxies at a given stellar mass. Major galaxy mergers are therefore not a significant quenching pathway, neither at z ∼ 0 nor within the last 5 Gyr. The majority of red galaxies must have been quenched through an alternative quenching mechanism which causes a slow blue to red evolution.

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“…power and the SFR. In addition irregular fuel supply (Tadhunter et al 2011;Kaviraj et al 2015) and variability in the AGN "on" phase (Hickox et al 2014) will further weaken the correlation.…”

Section: Radio Power and Sfr Relationmentioning

confidence: 99%

Constraints on Feedback in the Local Universe: The Relation Between Star Formation and Agn Activity in Early-Type Galaxies

Vaddi

O’Dea

Baum

et al. 2016

ApJ

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We address the relation between star formation and active galactic nucleus (AGN) activity in a sample of 231 nearby (0.0002 < z < 0.0358) early-type galaxies by carrying out a multi-wavelength study using archival observations in the UV, IR, and radio. Our results indicate that early-type galaxies in the current epoch are rarely powerful AGNs, with P 10 WHz 22 1 < -for a majority of the galaxies. Only massive galaxies are capable of hosting powerful radio sources while less massive galaxies are hosts to lower radio power sources. Evidence of ongoing star formation is seen in approximately 7% of the sample. The star formation rate (SFR) of these galaxies is less than 0.1 M e yr −1 . They also tend to be radio faint (P 10 WHzThere is a nearly equal fraction of star-forming galaxies in radio faint (P 10 WHz 22 1 < -) and radio bright galaxies (P 10 WHz 22 1  -) suggesting that both star formation and radio mode feedback are constrained to be very low in our sample. We notice that our galaxy sample and the Brightest Cluster Galaxies follow similar trends in radio power versus SFR. This may be produced if both radio power and SFR are related to stellar mass.

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The triggering of local AGN and their role in regulating star formation

Cited by 37 publications

References 109 publications

Radio AGN in spiral galaxies

Radio AGN in spiral galaxies

Galaxy Zoo: Major Galaxy Mergers Are Not a Significant Quenching Pathway*

Constraints on Feedback in the Local Universe: The Relation Between Star Formation and Agn Activity in Early-Type Galaxies

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