The impact of AGN on stellar kinematics and orbits in simulated massive galaxies

Frigo, Matteo; Naab, Thorsten; Hirschmann, Michaela; Choi, Ena; Somerville, Rachel S.; Krajnović, Davor; Davé, Romeel; Cappellari, Michele

doi:10.1093/mnras/stz2318

Cited by 27 publications

(46 citation statements)

References 109 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…These anti-correlations are typically found in remnants of gas-rich mergers (Bendo & Barnes 2000;Jesseit et al 2005;González-García et al 2006;Naab et al 2006aNaab et al , 2007Jesseit et al 2007;Hoffman et al 2009;Röttgers et al 2014) or in simulations of objects that did not have a strong feedback mechanism turned on (e.g. no AGN feedback Dubois et al 2016;Frigo et al 2019). We therefore conclude that it is likely that core-less slow rotators originate from dissipative processes and contain embedded discs or disc-like structures.…”

Section: Local Kinematic Parameterssupporting

confidence: 65%

“…from Frigo et al (2019), where for each spatial bin i, there is the local flux F i , the mean velocity V i , the velocity dispersion σ i , and the skewness parameter h 3,i of the LOSVD. This global parameter measures the slope of the distribution of points in the h 3 − V/σ plane, as shown by straight lines in Fig.…”

Section: Local Kinematic Parametersmentioning

confidence: 99%

“…It is tuned such that when h 3 and V/σ are fully (anti-)correlated, the correlation is given by h 3 = (1/ξ 3 )V/σ. Frigo et al (2019) showed examples of various h 3 and V/σ distributions with and without correlations, and corresponding ξ 3 parameters. Fast-rotating galaxies have ξ 3 < −4, while slow rotators are expected to have ξ 3 close to 0.…”

Section: Local Kinematic Parametersmentioning

confidence: 99%

“…In some of these mergers, a binary SMBH pair might form, but it could be of too low mass 7 to excavate an observable core (Rantala et al 2018), or the central starburst is able to refill the nuclei (Mihos & Hernquist 1994;Kormendy et al 2009, see also Section 5.4). Finally, radiative feedback from the active galactic nucleus, or a mechanical feedback from winds, can also facilitate the production of slow rotators by preventing the cooling and accretion of new gas (Serra et al 2014;Frigo et al 2019).…”

Section: Formation Of Slow Rotators With and Without Coresmentioning

confidence: 99%

See 3 more Smart Citations

Formation channels of slowly rotating early-type galaxies

Krajnović

Ural

Küntschner

et al. 2020

A&A

Self Cite

View full text Add to dashboard Cite

We study the evidence for a diversity of formation processes in early-type galaxies by presenting the first complete volume-limited sample of slow rotators with both integral-field kinematics from the ATLAS 3D Project and high spatial resolution photometry from the Hubble Space Telescope. Analysing the nuclear surface brightness profiles of 12 newly imaged slow rotators, we classify their light profiles as core-less, and place an upper limit to the core size of about 10 pc. Considering the full magnitude and volumelimited ATLAS 3D sample, we correlate the presence or lack of cores with stellar kinematics, including the proxy for the stellar angular momentum (λ Re ) and the velocity dispersion within one half-light radius (σ e ), stellar mass, stellar age, α-element abundance, and age and metallicity gradients. More than half of the slow rotators have core-less light profiles, and they are all less massive than 10 11 M . Core-less slow rotators show evidence for counter-rotating flattened structures, have steeper metallicity gradients, and a larger dispersion of gradient values (∆[Z/H] = −0.42 ± 0.18) than core slow rotators (∆[Z/H] = −0.23 ± 0.07). Our results suggest that core and core-less slow rotators have different assembly processes, where the former, as previously discussed, are the relics of massive dissipation-less merging in the presence of central supermassive black holes. Formation processes of core-less slow rotators are consistent with accretion of counter-rotating gas or gas-rich mergers of special orbital configurations, which lower the final net angular momentum of stars, but support star formation. We also highlight core fast rotators as galaxies that share properties of core slow rotators (i.e. cores, ages, σ e , and population gradients) and core-less slow rotators (i.e. kinematics, λ Re , mass, and larger spread in population gradients). Formation processes similar to those for core-less slow rotators can be invoked to explain the assembly of core fast rotators, with the distinction that these processes form or preserve cores.

show abstract

Section: Local Kinematic Parameterssupporting

confidence: 65%

Section: Local Kinematic Parametersmentioning

confidence: 99%

Section: Local Kinematic Parametersmentioning

confidence: 99%

Section: Formation Of Slow Rotators With and Without Coresmentioning

confidence: 99%

See 2 more Smart Citations

Formation channels of slowly rotating early-type galaxies

Krajnović

Ural

Küntschner

et al. 2020

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…in Cappellari et al (2006) for early-type galaxies and in Bianchini et al (2018) for globular clusters. The same methods can also essentially be used in analysing numerical simulations (Naab et al 2014;Lahén et al 2018;Rantala et al 2018;Frigo et al 2019). As we are modeling individual massive stars rather than massive stellar population particles, we discard seeing effects applied to larger scale simulations (Naab et al 2014), and instead directly fit the LOSVD to the Voronoi-tesselated particle data.…”

Section: Two-dimensional Kinematic Mapsmentioning

confidence: 99%

Structure and Rotation of Young Massive Star Clusters in a Simulated Dwarf Starburst

Lahén

Naab

Johansson

et al. 2020

ApJ

Self Cite

View full text Add to dashboard Cite

We analyze the three-dimensional shapes and kinematics of the young star cluster population forming in a high-resolution griffin project simulation of a metal-poor dwarf galaxy starburst. The star clusters, which follow a power-law mass distribution, form from the cold ISM phase with an IMF sampled with individual stars down to 4 solar masses at sub-parsec spatial resolution. Massive stars and their important feedback mechanisms are modelled in detail. The simulated clusters follow a surprisingly tight relation between the specific angular momentum and mass with indications of two sub-populations. Massive clusters (M cl 3 × 10 4 M ) have the highest specific angular momenta at low ellipticities ( ∼ 0.2) and show alignment between their shapes and rotation. Lower mass clusters have lower specific angular momenta with larger scatter, show a broader range of elongations, and are typically misaligned indicating that they are not shaped by rotation. The most massive clusters (M 10 5 M ) accrete gas and proto-clusters from a 100 pc scale local galactic environment on a t 10 Myr timescale, inheriting the ambient angular momentum properties. Their two-dimensional kinematic maps show ordered rotation at formation, up to v ∼ 8.5 kms −1 , consistent with observed young massive clusters and old globular clusters, which they might evolve into. The massive clusters have angular momentum parameters λ R 0.5 and show Gauss-Hermite coefficients h 3 that are anticorrelated with the velocity, indicating asymmetric line-of-sight velocity distributions as a signature of a dissipative formation process.

show abstract

Ionized gas kinematics of massive elliptical galaxies in CALIFA and in cosmological zoom-in simulations

Florian

Ziegler

Hirschmann

et al. 2020

A&A

Self Cite

View full text Add to dashboard Cite

Context. Powerful Active Galactic Nuclei (AGN) are supposed to play a key regulatory role on the evolution of their host galaxies by shaping the thermodynamic properties of their gas component. However, little is known as to the nature and the visibility timescale of the kinematical imprints of AGN-driven feedback. Gaining theoretical and observational insights into this subject is indispensable for a thorough understanding of the AGN-galaxy co-evolution and could yield empirical diagnostics for the identification of galaxies that have experienced a major AGN episode in the past. Aims. We present an investigation of kinematical imprints of AGN feedback on the Warm Ionized gas Medium (WIM) of massive early-type galaxies (ETGs). To this end, we take a two-fold approach that involves a comparative analysis of Hα velocity fields in 123 local ETGs from the CALIFA integral field spectroscopy survey with 20 simulated galaxies from high-resolution hydrodynamic cosmological SPHgal simulations. The latter were re-simulated for two modeling setups, one with and another without AGN feedback. Methods. In order to quantify the effects of AGN feedback on gas kinematics we measure three parameters that probe deviations from simple regular rotation using the kinemetry package. These indicators trace the possible presence of distinct kinematic components in Fourier space (k3,5/k1), variations in the radial profile of the kinematic major axis (σPA), and offsets between the stellar and gas velocity fields (∆φ). These quantities are monitored in the simulations from a redshift 3 to 0.2 to assess the connection between black hole accretion history, stellar mass growth and kinematical perturbation of the WIM. Results. Observed local massive galaxies show a broad range of irregularities, indicating disturbed warm gas motions, irrespective of being classified via diagnostic lines as AGN or not. Simulations of massive galaxies with AGN feedback generally exhibit higher irregularity parameters than without AGN feedback, more consistent with observations. Besides AGN feedback, other processes like major merger events or infalling gas clouds can lead to elevated irregularity parameters, but they are typically of shorter duration. More specifically, k3,5/k1 is most sensitive to AGN feedback, whereas ∆φ is most strongly affected by gas infall. Conclusions. We conclude that even if the general disturbance of the WIM velocity is not a unique indicator for AGN feedback, irregularity parameters, high enough to be consistent with observations, can only be reproduced in simulations with AGN feedback. Specifically, an elevated value for the deviation from simple ordered motion is a strong sign for previous events of AGN activity and feedback.

show abstract

The impact of AGN on stellar kinematics and orbits in simulated massive galaxies

Cited by 27 publications

References 109 publications

Formation channels of slowly rotating early-type galaxies

Formation channels of slowly rotating early-type galaxies

Structure and Rotation of Young Massive Star Clusters in a Simulated Dwarf Starburst

Ionized gas kinematics of massive elliptical galaxies in CALIFA and in cosmological zoom-in simulations

Contact Info

Product

Resources

About