The connection between mass, environment, and slow rotation in simulated galaxies

Lagos, Claudia del P.; Schaye, Joop; Bahé, Yannick M.; Sande, Jesse van de; Kay, Scott T.; Barnes, David J.; Davis, Timothy A.; Vecchia, Claudio Dalla

doi:10.1093/mnras/sty489

Cited by 96 publications

(153 citation statements)

References 87 publications

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“…z > 1.0), (cosmological) numerical simulations will allow us to explore the evolution of angular momentum with time (e.g. Lagos et al 2018;Schulze et al 2018;Pillepich et al 2019 For an oblate galaxy, viewed at inclination i, we obtain…”

Section: Discussionmentioning

confidence: 99%

The CALIFA view on stellar angular momentum across the Hubble sequence

Falcón-Barroso

Ven

Lyubenova

et al. 2019

A&A

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We present the apparent stellar angular momentum over the optical extent of 300 galaxies across the Hubble sequence, using integral-field spectroscopic (IFS) data from the CALIFA survey. Adopting the same λ R parameter previously used to distinguish between slow and fast rotating early-type (elliptical and lenticular) galaxies, we show that spiral galaxies as expected are almost all fast rotators. Given the extent of our data, we provide relations for λ R measured in different apertures (e.g. fractions of the effective radius: 0.5 R e , R e , 2 R e ), including conversions to long-slit 1D apertures. Our sample displays a wide range of λ Re values, consistent with previous IFS studies. The fastest rotators are dominated by relatively massive and highly star-forming Sb galaxies, which preferentially reside in the main star-forming sequence. These galaxies reach λ Re values of ∼0.85, are the largest galaxies at a given mass, and display some of the strongest stellar population gradients. Compared to the population of S0 galaxies, our findings suggest that fading may not be the dominant mechanism transforming spirals into lenticulars. Interestingly, we find that λ Re decreases for late-type Sc and Sd spiral galaxies, with values than in occasions puts them in the slow-rotator regime. While for some of them this can be explained by their irregular morphologies and/or face-on configurations, others are edge-on systems with no signs of significant dust obscuration. The latter are typically at the low-mass end, but this does not explain their location in the classical (V/σ, ε) and (λ Re , ε) diagrams. Our initial investigations, based on dynamical models, suggest that these are dynamically hot disks, probably influenced by the observed important fraction of dark matter within R e .

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Section: Discussionmentioning

confidence: 99%

The CALIFA view on stellar angular momentum across the Hubble sequence

Falcón-Barroso

Ven

Lyubenova

et al. 2019

A&A

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“…These results are consistent with the notion that rotationally supported galaxies should have had quiescent accretion histories, and consequently lower f M * ,IHSC . Lagos et al (2018b) found that the highest V/σ galaxies can only be obtained in the absence of mergers. On the other hand, a dispersion-supported galaxy is expected to have experienced multiple mergers and interactions, which in turn should deposit higher amounts of mass into the IHSC, increasing its f M * ,IHSC .…”

Section: Kinematic Morphologymentioning

confidence: 99%

From stellar haloes to intracluster light: the physics of the Intra-Halo Stellar Component in cosmological hydrodynamical simulations

Cañas

Lagos

Elahi

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We study the Intra-Halo Stellar Component (IHSC) of Milky Way-mass systems up to galaxy clusters in the Horizon-AGN cosmological hydrodynamical simulation. We identify the IHSC using an improved phase-space galaxy finder algorithm which provides an adaptive, physically motivated and shape-independent definition of this stellar component, that can be applied to halos of arbitrary masses. We explore the IHSC mass fraction -total halo's stellar mass, f M * ,IHSC − M * , relation and the physical drivers of its scatter. We find that on average the f M * ,IHSC increases with total stellar mass, with the scatter decreasing strongly with mass from 2 dex at M * ,tot 10 11 M to 0.3 dex at group masses. At high masses, M * ,tot > 10 11.5 M , f M * ,IHSC increases with the number of substructures, and with the mass ratio between the central galaxy and largest satellite, at fixed M * ,tot . From mid-size groups and systems below M * ,tot < 10 12 M , we find that the central galaxy's stellar rotation-to-dispersion velocity ratio, V/σ, displays the strongest (anti)-correlation with f M * ,IHSC at fixed M * ,tot of all the galaxy and halo properties explored, transitioning from f M * ,IHSC < 0.1% for high V/σ, to f M * ,IHSC ≈ 5% for low V/σ galaxies. By studying the f M * ,IHSC temporal evolution, we find that, in the former, mergers not always take place, but if they did, they happened early (z > 1), while the high f M * ,IHSC population displays a much more active merger history. In the case of massive groups and galaxy clusters, M * ,tot 10 12 M , a fraction f M * ,IHSC ≈ 10 − 20% is reached at z ≈ 1 and then they evolve across lines of constant f M * ,IHSC modulo some small perturbations. Because of the limited simulation's volume, the latter is only tentative and requires a larger sample of simulated galaxy clusters to confirm.

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“…Simulations find that mergers impart a cumulative effect, and galaxies that have experienced successive multiple mergers are more likely to have lower spins (Lagos et al 2018). Furthermore, slow-rotating remnants from multiple mergers of disc galaxies are more likely to show kinematics twists, while remnants from binary mergers most often do not (Moody et al 2014).…”

Section: Discussionmentioning

confidence: 99%

The MASSIVE Survey XIV—Stellar Velocity Profiles and Kinematic Misalignments from 200 pc to 20 kpc in Massive Early-type Galaxies

Ene

Pei

Walsh

et al. 2020

ApJ

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We use high spatial resolution stellar velocity maps from the Gemini GMOS integral-field spectrograph (IFS) and wide-field velocity maps from the McDonald Mitchell IFS to study the stellar velocity profiles and kinematic misalignments from ∼ 200 pc to ∼ 20 kpc in 20 early-type galaxies with stellar mass M * > 10 11.7 M in the MASSIVE survey. While 80% of the galaxies have low spins (λ < 0.1) and low rotational velocities (< 50 km s −1 ) in both the central region and the main body, we find a diverse range of velocity features and misalignment angles. For the 18 galaxies with measurable central kinematic axes, 10 have well aligned kinematic axis and photometric major axis, and the other 8 galaxies have misalignment angles that are distributed quite evenly from 15 • to the maximal value of 90 • . There is a strong correlation between central kinematic misalignment and galaxy spin, where all 4 galaxies with significant spins have well aligned kinematic and photometric axes, but only 43% of the low-spin galaxies are well aligned. The central and main-body kinematic axes within a galaxy are not always aligned. When the two kinematic axes are aligned (∼ 60% of the cases), they are either also aligned with the photometric major axis or orthogonal to it. We find 13 galaxies to also exhibit noticeable local kinematic twists, and one galaxy to have a counter-rotating core. A diverse assembly history consisting of multiple gas-poor mergers of a variety of progenitor mass ratios and orbits is likely to be needed to account for the predominance of low spins and the wide range of central and main-body velocity features reported here for local massive ETGs.

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The connection between mass, environment, and slow rotation in simulated galaxies

Cited by 96 publications

References 87 publications

The CALIFA view on stellar angular momentum across the Hubble sequence

The CALIFA view on stellar angular momentum across the Hubble sequence

From stellar haloes to intracluster light: the physics of the Intra-Halo Stellar Component in cosmological hydrodynamical simulations

The MASSIVE Survey XIV—Stellar Velocity Profiles and Kinematic Misalignments from 200 pc to 20 kpc in Massive Early-type Galaxies

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