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

Vaddi, Sravani; O’Dea, C. P.; Baum, Stefi A.; Whitmore, Samantha; Ahmed, Rabeea; Pierce, K.; Leary, Sara

doi:10.3847/0004-637x/818/2/182

Cited by 30 publications

(30 citation statements)

References 119 publications

(135 reference statements)

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“…This is in agreement with several works finding that AGN host galaxies have similar star formation properties as their non-AGN counterparts (e.g. Harrison et al 2012;Husemann et al 2014;Xu et al 2015;Balmaverde et al 2016;Vaddi et al 2016;Zhang et al 2016;Suh et al 2017;Rosario et al 2018;Shangguan et al 2018), while others report a significant decrease in the SFR (e.g. Farrah et al 2012;Mullaney et al 2015;Shimizu et al 2015;Wylezalek & Zakamska 2016) for different kind of AGN samples.…”

Section: Implications For Agn Feedbacksupporting

confidence: 93%

The Close AGN Reference Survey (CARS)

Husemann

Scharwächter

Davis

et al. 2019

A&A

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Context. Galaxy-wide outflows driven by star formation and/or an active galactic nucleus (AGN) are thought to play a crucial rule in the evolution of galaxies and the metal enrichment of the inter-galactic medium. Direct measurements of these processes are still scarce and new observations are needed to reveal the nature of outflows in the majority of the galaxy population. Aims. We combine extensive, spatially-resolved, multi-wavelength observations, taken as part of the Close AGN Reference Survey (CARS), for the edge-on disc galaxy HE 1353−1917 in order to characterise the impact of the AGN on its host galaxy via outflows and radiation. Methods. Multi-color broad-band photometry was combined with spatially-resolved optical, near-infrared (NIR) and sub-mm and radio observations taken with the Multi-Unit Spectroscopy Explorer (MUSE), the Near-infrared Integral Field Spectrometer (NIFS), the Atacama Large Millimeter Array (ALMA), and the Karl G. Jansky Very Large Array (VLA) to map the physical properties and kinematics of the multi-phase interstellar medium. Results. We detect a biconical extended narrow-line region ionised by the luminous AGN orientated nearly parallel to the galaxy disc, extending out to at least 25 kpc. The extra-planar gas originates from galactic fountains initiated by star formation processes in the disc, rather than an AGN outflow, as shown by the kinematics and the metallicity of the gas. Nevertheless, a fast, multi-phase, AGN-driven outflow with speeds up to 1000 km s−1 is detected close to the nucleus at 1 kpc distance. A radio jet, in connection with the AGN radiation field, is likely responsible for driving the outflow as confirmed by the energetics and the spatial alignment of the jet and multi-phase outflow. Evidence for negative AGN feedback suppressing the star formation rate (SFR) is mild and restricted to the central kpc. But while any SFR suppression must have happened recently, the outflow has the potential to greatly impact the future evolution of the galaxy disc due to its geometrical orientation. Conclusions.. Our observations reveal that low-power radio jets can play a major role in driving fast, multi-phase, galaxy-scale outflows even in radio-quiet AGN. Since the outflow energetics for HE 1353−1917 are consistent with literature, scaling relation of AGN-driven outflows the contribution of radio jets as the driving mechanisms still needs to be systematically explored.

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Section: Implications For Agn Feedbacksupporting

confidence: 93%

The Close AGN Reference Survey (CARS)

Husemann

Scharwächter

Davis

et al. 2019

A&A

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“…Blue color in bulge-dominated galaxies is directly related to star formation (Silverman et al 2008). NGC 2329, however, has a low star formation rate (SFR = 4.11×10 −2 M yr −1 ) which is consistent with other FR I radio galaxies (Vaddi et al 2016).…”

Section: Discussionsupporting

confidence: 74%

“…The galaxy had exceptional blue 𝑉 − 𝐼 color as compared to the other giant ellipticals in their sample. Verdoes 1999), (4) Vaddi et al (2016). Kleĳn et al (1999Kleĳn et al ( , 2002 detected a small ∼0.3 arcsec (114 pc) optical jet-like extension emerging from the core at position angle (PA) 322 • .…”

Section: Ngc 2329mentioning

confidence: 99%

The peculiar WAT NGC 2329 with Seyfert/FR I-like radio lobes

Das,

Kharb,

Morganti

et al. 2021

Preprint

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We report the complex radio properties of the radio galaxy NGC 2329 that resides in the centre of the galaxy cluster Abell 569. For this study, we have used archival data from the Very Large Array (VLA) at various resolutions and frequencies, as well as the Very Long Baseline Array (VLBA). While the wide-angle tailed (WAT) Fanaroff-Riley type I (FR I) radio morphology of the source has been discussed widely in the literature, the nature of the inner lobes has not been as widely discussed. In particular, we note that the inner lobes resemble the bubble-like radio structures observed in Seyfert galaxies. Polarization-sensitive data from the VLA clearly show magnetic field structures consistent with FR Is for the outer lobes and Seyferts for the inner lobes in NGC 2329. FR Is are classified as radio-loud (RL) active galactic nuclei (AGN) and Seyferts as radio-quiet (RQ) AGN, making this source unique. The VLBA shows a onesided radio jet suggesting a relativistic pc-scale outflow, leading into the inner lobes. Electron lifetime estimates suggest that the outer FR I-like lobes are nearly twice as old (∼45 Myr) as the inner Seyfert-like lobes (∼25 Myr). Gas inflow in this merging cluster seems to have rejuvenated the AGN about ∼25 Myr ago, and may have caused a change in the accretion disc state. The complex composite radio morphology of NGC 2329 suggests that the RL/RQ dichotomy is a function of time in the lifecycle of an AGN.

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“…Integrating within a radius of 25 kpc, we obtain aṀ cool of 1.4 M yr −1 in spite of an observed star formation rate of 0.1 M yr −1 (Vaddi et al 2016). We observe a total of 3.4 × 10 7 M cool gas in the rims and filaments, corresponding to an uplift rate oḟ M uplift = 2.5 M yr −1 (Table 3).…”

Section: Uplift Of Cluster Gas By Radio Lobesmentioning

confidence: 99%

Buoyant AGN Bubbles in the Quasi-isothermal Potential of NGC 1399

Nulsen

Kraft

et al. 2017

ApJ

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The Fornax Cluster is a low-mass cool-core galaxy cluster. We present a deep Chandra study of NGC 1399, the central dominant elliptical galaxy of Fornax. The cluster center harbors two symmetric X-ray cavities coincident with a pair of radio lobes fed by two collimated jets along a north-south axis. A temperature map reveals that the AGN outburst has created a channel filled with cooler gas out to a radius of 10 kpc. The cavities are surrounded by cool bright rims and filaments that may have been lifted from smaller radii by the buoyant bubbles. X-ray imaging suggests a potential ghost bubble of 5 kpc diameter to the northwest. We find that the amount of gas lifted by AGN bubbles is comparable to that which would otherwise cool, demonstrating that AGN driven outflow is effective in offsetting cooling in low-mass clusters. The cluster cooling time scale is > 30 times longer than the dynamical time scale, which is consistent with the lack of cold molecular gas at the cluster center. The X-ray hydrostatic mass is consistent within 10% with the total mass derived from the optical data. The observed entropy profile rises linearly, following a steeper slope than that observed at the centers of massive clusters; gas shed by stars in NGC 1399 may be incorporated in the hot phase. However, it is far-fetched for supernova-driven outflow to produce and maintain the thermal distribution in NGC 1399 and it is in tension with the metal content in the hot gas.

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

Cited by 30 publications

References 119 publications

The Close AGN Reference Survey (CARS)

The Close AGN Reference Survey (CARS)

The peculiar WAT NGC 2329 with Seyfert/FR I-like radio lobes

Buoyant AGN Bubbles in the Quasi-isothermal Potential of NGC 1399

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