Outflows in the inner kiloparsec of NGC 1566 as revealed by molecular (ALMA) and ionized gas (Gemini-GMOS/IFU) kinematics

Slater, R.; Nagar, Neil M.; Schnorr-Müller, A.; Storchi‐Bergmann, Thaisa; Finlez, C.; Lena, Davide; Mundell, C. G.; Riffel, Rogemar A.; Peterson, Bradley M.; Robinson, Andrew; Orellana, G.

doi:10.1051/0004-6361/201730634

Cited by 28 publications

(18 citation statements)

References 105 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Given the uncertainties, we only conclude that the mass of central SMBH is of the order of several 10 7 M , which is a typical mass for SMBHs in nearby galaxies (e.g. Greene & Ho 2005;Busch et al 2017;Humire et al 2018;Slater et al 2019;Fazeli et al 2019).…”

Section: Smbh Massmentioning

confidence: 77%

Near-infrared observations of the gas structure and kinematics in the circumnuclear region of NGC 1672

Fazeli

Eckart

Busch

et al. 2020

A&A

View full text Add to dashboard Cite

We present our near-infrared, integral-field spectroscopy observations of the central 550 × 550 pc2 (10″ × 10″) of the local galaxy NGC 1672. Our aim is to investigate the morphology and kinematics of gas and stars to probe evidence for feeding and feedback phenomena. For this purpose the near-infrared wavelength regime and integral-field unit technique provide a vast amount of useful information. The narrow emission line ratios suggest that the galaxy hosts a low-luminosity active galactic nucleus. From the MBH − σ* relation, we find a black hole mass of a few 107 M⊙. The total reservoir of hot molecular and ionised gas is estimated, using flux of H2 and Brγ emission lines, to be 258 M⊙ and 2.3 × 106 M⊙ respectively. The most striking feature in the emission line flux maps is the star-forming ring at a radius of ∼3″. The stellar and gaseous kinematics both show a rotation pattern in a disc that is blue-shifted in the north-west and red-shifted in the south-east. However, unlike the stellar kinematics, gas kinematics show various complexities, such as higher amplitudes in the central region (within the star-forming ring). The molecular gas velocity-field map shows deviations from pure disc motion in the form of an S-shaped zero-velocity line. In particular the position angle of the zero-velocity line changes in the central arcsecond, resembling the decoupled nuclear disc or molecular torus found in CO(3–2). There is an offset of 0.″5 between the nuclear continuum barycentre and kinematic centre of molecular gas towards the north-west. The velocity field of Brγ emitting gas on the other hand, is highly red-shifted in the centre and offset from the continuum emission peak by about 1″. Investigating the spectra of this region we detect a doubled-horn Brγ emission line in the nucleus and north-west. This region is also luminous in radio 3 cm emission connecting the nucleus to the star-forming ring.

show abstract

Section: Smbh Massmentioning

confidence: 77%

Near-infrared observations of the gas structure and kinematics in the circumnuclear region of NGC 1672

Fazeli

Eckart

Busch

et al. 2020

A&A

View full text Add to dashboard Cite

show abstract

“…All four of our targets show clear spiral features (see Figure 1), with Harry and Theodore showing a strong bar feature, Neville a weak bar feature (Nair & Abraham 2010) and Padma a barlens feature (an oval-like strucutre along the bar major axis, see Athanassoula et al 2015). Simulations suggest both bars and spiral arms can drive inflows at rates an order of magnitude larger than needed to power the combined outflow and SMBH accretion rates for all four targets (0.1−few 𝑀 yr −1 ; Regan & Teuben 2004;Davies et al 2009;Lin et al 2013;Fanali et al 2015;Slater et al 2019). This order of magnitude difference is promising, since our simplifying assumption here is that the inflow must be at least enough to power both the SMBH accretion and the outflow, this means that the inflow would be sufficient to also fuel central star formation or contribute to the central gas reservoir (Tacconi & Young 1986;Böker et al 2003;Bigiel et al 2008;Leroy et al 2013;Moreno et al 2021).…”

Section: Discussionmentioning

confidence: 94%

Kiloparsec-scale AGN outflows and feedback in merger-free galaxies

Smethurst

Simmons

Coil

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Recent observations and simulations have challenged the long-held paradigm that mergers are the dominant mechanism driving the growth of both galaxies and supermassive black holes (SMBH), in favour of non-merger (secular) processes. In this pilot study of merger-free SMBH and galaxy growth, we use Keck Cosmic Web Imager spectral observations to examine four low-redshift (0.043 < z < 0.073) disk-dominated ‘bulgeless’ galaxies hosting luminous AGN, assumed to be merger-free. We detect blueshifted broadened [O iii] emission from outflows in all four sources, which the $\rm{[O\, \small {III}]}$/$\rm {H}\beta$ ratios reveal are ionised by the AGN. We calculate outflow rates in the range $0.12-0.7~\rm {M}_{\odot }~\rm {yr}^{-1}$, with velocities of $675-1710~\rm {km}~\rm {s}^{-1}$, large radial extents of $0.6-2.4~\rm {kpc}$, and SMBH accretion rates of $0.02-0.07~\rm {M}_{\odot }~\rm {yr}^{-1}$. We find that the outflow rates, kinematics, and energy injection rates are typical of the wider population of low-redshift AGN, and have velocities exceeding the galaxy escape velocity by a factor of ∼30, suggesting that these outflows will have a substantial impact through AGN feedback. Therefore, if both merger-driven and non-merger-driven SMBH growth lead to co-evolution, this suggests that co-evolution is regulated by feedback in both scenarios. Simulations find that bars and spiral arms can drive inflows to galactic centres at rates an order of magnitude larger than the combined SMBH accretion and outflow rates of our four targets. This work therefore provides further evidence that non-merger processes are sufficient to fuel SMBH growth and AGN outflows in disk galaxies.

show abstract

“…They find a conspicuous nuclear trailing spiral and weak non-circular motions at the periphery of the nuclear spiral arms. Recently, by analysing the nuclear kinematics of the same galaxy NGC 1566 via ALMA observations of the CO(2−1) emission, Slater et al (2019) show the presence of significant non-circular motions in the innermost (200 pc) and along spiral arms in the central kpc. They find a molecular outflow in the disc with velocities of ∼180 km s −1 in the nucleus.…”

Section: Introductionmentioning

confidence: 99%

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

Belete

Andreani

Fernández-Ontiveros

et al. 2021

A&A

Self Cite

View full text Add to dashboard Cite

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.

show abstract

Outflows in the inner kiloparsec of NGC 1566 as revealed by molecular (ALMA) and ionized gas (Gemini-GMOS/IFU) kinematics

Cited by 28 publications

References 105 publications

Near-infrared observations of the gas structure and kinematics in the circumnuclear region of NGC 1672

Near-infrared observations of the gas structure and kinematics in the circumnuclear region of NGC 1672

Kiloparsec-scale AGN outflows and feedback in merger-free galaxies

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

Contact Info

Product

Resources

About