The AGN fuelling/feedback cycle in nearby radio galaxies – II. Kinematics of the molecular gas

Ruffa, Ilaria; Davis, Timothy A.; Prandoni, I.; Laing, R. A.; Paladino, R.; Parma, P.; Ruiter, H. de; Casasola, V.; Bureau, Martin; Warren, Joshua

doi:10.1093/mnras/stz2368

Cited by 31 publications

(34 citation statements)

References 123 publications

(172 reference statements)

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“…Additionally, another complication with the lower X-ray luminosity systems is that one cannot assume that any undetected X-ray cavities are well traced by the radio lobes, since such systems often host high-power radio sources whose lobes extend far beyond the dense atmospheres (e.g. NGC 4261, IC4296, IC1459, NGC 1600, NGC 5090, UGC11294, ARP308; Diehl & Statler 2008;Sun 2009;Cavagnolo et al 2010;Duţan & Caramete 2015;Kolokythas et al 2018;Ruffa et al 2019;Grossová et al 2019). Table 3 shows that H α filaments are mostly found in groups and ellipticals where the radio emission is filling the X-ray cavities (the exceptions are NGC 499, NGC 410, and NGC 4104, see Table 3).…”

Section: Group and Ellipticals Subsamplementioning

confidence: 99%

LOFAR observations of X-ray cavity systems

Bîrzan

Rafferty

Brüggen

et al. 2020

Monthly Notices of the Royal Astronomical Society

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ABSTRACT We present LOFAR observations at 120–168 MHz of 42 systems with possible X-ray cavities in their hot atmosphere, of which 17 are groups or ellipticals, 19 are nearby clusters (z < 0.3), and six are higher redshift clusters (z > 0.3). The X-ray cavities, formed by the radio lobes of the central active galactic nucleus (AGN), are evidence of radio-mode AGN feedback. In the groups and ellipticals sample, half of the systems have X-ray cavities for which no associated lobe emission was detected. Conversely, we report the discovery of large radio lobes in NGC 6338, extending far beyond the emission reported previously in the literature. In the case of the nearby clusters, our observations show that there is little low-frequency radio emission that extends beyond the cavities (e.g. MS 0735.6+7421, A2052). For the first time, we report secure cavity-radio associations in 2A 0335+096, ZwCl 2701, and ZwCl 8276 that strengthens their interpretation as AGN-created cavities. However, in some known cavity systems (e.g. A1795 and ZwCl 3146) we report the lack of detectable low-frequency radio emission associated with the cavities. Our sample of higher redshifts systems is small, and unfortunately the present LOFAR observations are not able to resolve the lobes in many of them. Nevertheless, our sample represents one of the best available for investigating the connection between radio and jet power in radio-mode AGN feedback.

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Section: Group and Ellipticals Subsamplementioning

confidence: 99%

LOFAR observations of X-ray cavity systems

Bîrzan

Rafferty

Brüggen

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Furthermore, it has been shown that gas inflows could be a result of gravity torques from non-axisymmetric potentials in the central regions of galaxies, such as streaming motions along a bar (see e.g. Ruffa et al 2019).…”

Section: Kinematical Perturbationsmentioning

confidence: 99%

Molecular gas kinematics in the nuclear region of nearby Seyfert galaxies with ALMA

Belete

Andreani

Fernández-Ontiveros

et al. 2021

A&A

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Context. The study of the distribution, morphology, and kinematics of cold molecular gas in the nuclear and circumnuclear regions of active galactic nuclei (AGNs) helps to characterise and hence to quantify the impact of the AGNs on the host galaxy over its lifetime. Aims. We present the analysis of the molecular gas in the nuclear regions of three Seyfert galaxies, NGC 4968, NGC 4845, and MCG-06-30-15, using Atacama Large sub-Millimetre Array (ALMA) observations of the CO(2−1) emission line. The aim is to determine the kinematics of the gas in the central (∼1 kpc) region and thereby to probe nuclear fueling and feedback of AGNs. Methods. We used two different softwares, namely the 3D-Based Analysis of Rotating Object via Line Observations and DiskFit, to model the kinematics of the gas in the molecular disc, and thereby to determine the gas rotation and any kinematical perturbations. Results. Circular motions dominate the kinematics of the molecular gas in the central discs, mainly in NGC 4845 and MCG-06-30-15; however there is clear evidence of non-circular motions in the central (∼1 kpc) region of NGC 4845 and NGC 4968. The strongest non-circular motion is detected in the inner disc of NGC 4968, mainly along the minor kinematic axis, with a velocity ∼115 km s−1. Of all DiskFit models, the bisymmetric model is found to give the best fit for NGC 4968 and NGC 4845, indicating that the observed non-circular motions in the inner disc of these galaxies could result from the nuclear barred structure, where the gas streams in elliptical orbits aligned along the bar. If the dynamics of NGC 4968 is modelled as a corotation pattern just outside of the bar, the bar pattern speed becomes Ωb = 52 km s−1 kpc−1; the corotation is set at 3.5 kpc; and the inner Lindblad resonance (ILR) ring is R = 300 pc, corresponding to the CO emission ring. In the NGC 4968 galaxy, the torques exerted on the gas by the bar are positive in the centre, within the gas nuclear ring, and negative outside. This shows that the gas is transiently trapped in the ILR. The comparison of the CO intensity maps with the map of the cold dust emission shows an absence of CO in the centre of NGC 4968; also the dust distribution and CO emission in and around the centre of NGC 4845 have similar extensions. The 1.2 mm ALMA continuum is peaked and compact in NGC 4968 and MCG-06-30-15, but their CO(2−1) emissions have extended distributions. Allowing the CO-to-H2 conversion factor αCO between 0.8 and 3.2, which is typical of nearby galaxies of the same type, the molecular mass M(H2) is estimated to be ∼3 − 12 × 107 M⊙ (NGC 4968), ∼9 − 36 × 107 M⊙ (NGC 4845), and ∼1 − 4 × 107 M⊙ (MCG-06-30-15). Conclusions. We conclude that the observed non-circular motions in the molecular disc of NGC 4968 and likely those seen in NGC 4845 are due to the presence of the bar in the nuclear region. We discuss the possibility that the observed pattern in the kinematics might be a consequence of the presence of AGNs, and this might be the case for NGC 4845. At the current spectral and spatial resolution and sensitivity, we cannot claim any strong evidence in these sources of the long sought feedback or feeding effect resulting from the presence of AGNs.

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“…Other groups have also used the same method to constrain SMBH masses (e.g. Onishi et al 2015;Barth et al 2016a,b;Boizelle et al 2019;Nagai et al 2019;Ruffa et al 2019;Nguyen et al 2020). In addition to measuring SMBH masses, the same data can be used to investigate the physical state of the molecular gas and study giant molecular clouds (Utomo et al 2015;Liu et al in preparation).…”

Section: Introductionmentioning

confidence: 99%

WISDOM project – VI. Exploring the relation between supermassive black hole mass and galaxy rotation with molecular gas

Smith

Bureau

Davis

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Empirical correlations between the masses of supermassive black holes (SMBHs) and properties of their host galaxies are well-established. Among these is the correlation with the flat rotation velocity of each galaxy measured either at a large radius in its rotation curve or via a spatially-integrated emission line width. We propose here the use of the de-projected integrated CO emission line width as an alternative tracer of this rotation velocity, that has already been shown useful for the Tully-Fisher (luminosity-rotation velocity) relation. We investigate the correlation between CO line widths and SMBH masses for two samples of galaxies with dynamical SMBH mass measurements, with respectively spatially-resolved and unresolved CO observations. The tightest correlation is found using the resolved sample of 25 galaxies as log (MBH/M⊙) = (7.5 ± 0.1) + (8.5 ± 0.9)[log (W50/sin i km s−1) − 2.7], where MBH is the central SMBH mass, W50 the full-width at half-maximum of a double-horned emission line profile, and i the inclination of the CO disc. This relation has a total scatter of 0.6 dex, comparable to those of other SMBH mass correlations, and dominated by the intrinsic scatter of 0.5 dex. A tight correlation is also found between the de-projected CO line widths and the stellar velocity dispersions averaged within one effective radius. We apply our correlation to the COLD GASS sample to estimate the local SMBH mass function.

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The AGN fuelling/feedback cycle in nearby radio galaxies – II. Kinematics of the molecular gas

Cited by 31 publications

References 123 publications

LOFAR observations of X-ray cavity systems

LOFAR observations of X-ray cavity systems

Molecular gas kinematics in the nuclear region of nearby Seyfert galaxies with ALMA

WISDOM project – VI. Exploring the relation between supermassive black hole mass and galaxy rotation with molecular gas

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