Stellar Kinematics and Environment at z ∼ 0.8 in the LEGA-C Survey: Massive Slow Rotators Are Built First in Overdense Environments

Cole, Justin W.; Bezanson, Rachel; Wel, Arjen van der; Bell, Eric F.; D’Eugenio, Francesco; Franx, Marijn; Gallazzi, Anna; Houdt, Josha van; Muzzin, Adam; Pacifici, Camilla; Sande, Jesse van de; Sobral, David; Straatman, Caroline; Wu, Po-Feng

doi:10.3847/2041-8213/ab7241

Cited by 21 publications

(16 citation statements)

References 67 publications

(73 reference statements)

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“…1.5 − 2 Gyrs; the quick transformation of λ r 50 in individual galaxies is happening mostly throughout lookback times ≈ 2−6 Gyr. This agrees with the low fraction of SRs found in observations at z ≈ 0.6, which increases rapidly to z = 0 (Cole et al 2020).…”

Section: Kinematic Transformation and Quenching Of Slow Rotatorssupporting

confidence: 91%

The diverse nature and formation paths of slow rotator galaxies in the eagle simulations

Lagos

Emsellem

Sande

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We use a sample of z = 0 galaxies visually classified as slow rotators (SRs) in the eagle hydrodynamical simulations to explore the effect of galaxy mergers on their formation, characterise their intrinsic galaxy properties, and study the connection between quenching and kinematic transformation. SRs that have had major or minor mergers (mass ratios ≥0.3 and 0.1 − 0.3, respectively) tend to have a higher triaxiality parameter and ex-situ stellar fractions than those that had exclusively very minor mergers or formed in the absence of mergers (“no-merger” SRs). No-merger SRs are more compact, have lower black hole-to-stellar mass ratios and quenched later than other SRs, leaving imprints on their z = 0 chemical composition. For the vast majority of SRs we find that quenching, driven by active galactic nuclei feedback, precedes kinematic transformation, except for satellite SRs, in which these processes happen in tandem. However, in ≈50 per cent of these satellites, satellite-satellite mergers are responsible for their SR fate, while environment (i.e. tidal field and interactions with the central) can account for the transformation in the rest. By splitting SRs into kinematic sub-classes, we find that flat SRs prefer major mergers; round SRs prefer minor or very minor mergers; prolate SRs prefer gas-poor mergers. Flat and prolate SRs are more common among satellites hosted by massive haloes ($>10^{13.6}\, \rm M_{\odot }$) and centrals of high masses ($M_{\star } > 10^{10.5}\, \rm M_{\odot }$). Although eagle galaxies display kinematic properties that broadly agree with observations, there are areas of disagreement, such as inverted stellar age and velocity dispersion profiles. We discuss these and how upcoming simulations can solve them.

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Section: Kinematic Transformation and Quenching Of Slow Rotatorssupporting

confidence: 91%

The diverse nature and formation paths of slow rotator galaxies in the eagle simulations

Lagos

Emsellem

Sande

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…Some works have shown that galaxies exhibit a lower net angular momentum for a higher local density (e.g. Cappellari et al 2011a;Cortese et al 2019;Graham et al 2019;Cole et al 2020), while others find that there is no additional dependence on the environment once the correlation between the angular momentum and stellar mass is accounted for (Brough et al 2017). Finally, the stellar population parameters also suffer from conflicting correlations.…”

Section: Introductionmentioning

confidence: 99%

The Fornax3D project: Assembly histories of lenticular galaxies from a combined dynamical and population orbital analysis

Poci,

McDermid,

Lyubenova

et al. 2021

Preprint

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In order to assess the impact of the environment on the formation and evolution of galaxies, accurate assembly histories of such galaxies are needed. However, these measurements are observationally difficult owing to the diversity of formation paths that lead to the same present-day state of a galaxy. In this work, we apply a powerful new technique in order to observationally derive accurate assembly histories through a self-consistent combined stellar dynamical and population galaxy model. We present this approach for three edge-on lenticular galaxies from the Fornax3D project -FCC 153, FCC 170, and FCC 177 -in order to infer their mass assembly histories individually and in the context of the Fornax cluster. The method was tested on mock data from simulations to quantify its reliability. We find that the galaxies studied here have all been able to form dynamically-cold (intrinsic vertical velocity dispersion σ z 50 km s −1 ) stellar disks after cluster infall. Moreover, the pre-existing (old) high angular momentum components have retained their angular momentum (orbital circularity λ z > 0.8) through to the present day. Comparing the derived assembly histories with a comparable galaxy in a low-density environment -NGC 3115 -we find evidence for cluster-driven suppression of stellar accretion and merging. We measured the intrinsic stellar age-velocity-dispersion relation and find that the shape of the relation is consistent with galaxies in the literature across redshift. There is tentative evidence for enhancement in the luminosity-weighted intrinsic vertical velocity dispersion due to the cluster environment. But importantly, there is an indication that metallicity may be a key driver of this relation. We finally speculate that the cluster environment is responsible for the S0 morphology of these galaxies via the gradual external perturbations, or 'harassment', generated within the cluster.

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“…(2), one needs the stellar mass profile Σ (r) and the stellar rotation curve v (r). However, determining stellar kinematics beyond z = 0 is challenging in SFGs (but see Guérou et al 2017, for a first attempt) or even in passive galaxies with strong continuum (e.g., van de Sande et al 2013;Bezanson et al 2018;Cole et al 2020). As a result, most studies of the j − M relation use the star-forming gas v Hα kinematics as a proxy for v (e.g., Burkert et al 2016;Harrison et al 2017;Swinbank et al 2017).…”

Section: Definitionsmentioning

confidence: 99%

The MUSEHubbleUltra Deep Field Survey

Bouché

Genel

Pellissier

et al. 2021

A&A

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We investigate the specific angular momentum (sAM) j(< r) profiles of intermediate redshift (0.4 < z < 1.4) star-forming galaxies (SFGs) in the relatively unexplored regime of low masses (down to M⋆ ∼ 108 M⊙) and small sizes (down to Re ∼ 1.5 kpc), and we characterize the sAM scaling relation (i.e., Fall relation) and its redshift evolution. We have developed a 3D methodology to constrain sAM profiles of the star-forming gas using a forward modeling approach with GAlPAK3D that incorporates the effects of beam smearing, yielding the intrinsic morpho-kinematic properties even with limited spatial resolution data. Using mock observations from the TNG50 simulation, we find that our 3D methodology robustly recovers the star formation rate (SFR)-weighted j̃⋆(<r) profiles down to a low effective signal-to-noise ratio of ⪆3. We applied our methodology blindly to a sample of 494 [O II]-selected SFGs in the MUSE Ultra Deep Field (UDF) 9 arcmin2 mosaic data, covering the unexplored 8 < log M⋆/M⊙ < 9 mass range. We find that the (SFR-weighted) sAM relation follows j̃⋆ ∝ M⋆α with an index α varying from α = 0.3 to α = 0.5, from log M⋆/M⊙ = 8 to log M⋆/M⊙ = 10.5. The UDF sample supports a redshift evolution j̃⋆ ∝(1+z)a, with a = −0.27−0.56+0.42 which is consistent with the (1 + z)−0.5 expectation from a universe in expansion. The scatter of the sAM sequence is a strong function of the dynamical state with logj|M⋆ ∝ 0.65−0.08+0.06 × log(Vmax/σ), where σ is the velocity dispersion at 2Re. In TNG50, SFGs also form a j̃⋆−M⋆−(V/σ) plane, but it correlates more with galaxy size than with morphological parameters. Our results suggest that SFGs might experience a dynamical transformation, and lose their sAM, before their morphological transformation to becoming passive via either merging or secular evolution.

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Stellar Kinematics and Environment at z ∼ 0.8 in the LEGA-C Survey: Massive Slow Rotators Are Built First in Overdense Environments

Cited by 21 publications

References 67 publications

The diverse nature and formation paths of slow rotator galaxies in the eagle simulations

The diverse nature and formation paths of slow rotator galaxies in the eagle simulations

The Fornax3D project: Assembly histories of lenticular galaxies from a combined dynamical and population orbital analysis

The MUSEHubbleUltra Deep Field Survey

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