The Angular Momentum of the Circumgalactic Medium in the TNG100 Simulation

DeFelippis, Daniel; Genel, Shy; Bryan, Greg L.; Nelson, Dylan; Pillepich, Annalisa; Hernquist, Lars

doi:10.3847/1538-4357/ab8a4a

Cited by 45 publications

(45 citation statements)

References 87 publications

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“…Tangential velocities were also explored using the Illustris-TNG simulations by DeFelippis et al (2020), where they also found higher cool than hot v tan that greatly increase inside 0.5R 200 for z = 0 10 11.75−12.25 M haloes. They divide their sample into quartiles based on specific stellar angular momentum, j * , and examine all L * centrals in Illustris-TNG, while excising gas bound to satellites.…”

Section: Velocitymentioning

confidence: 99%

“…Their lowest j * quartile shows angles of ≈60 • , more similar to our results. The existence of extended CGM structures, including the CGM associated with satellites that is excised by DeFelippis et al (2020), likely biases high our angles between stars and the CGM. We therefore analyse the angular momentum alignment in our haloes after filtering out the CGM around satellites with the goal of assessing the impact of these extended CGM structures.…”

Section: Angular Momentummentioning

confidence: 99%

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The changing circumgalactic medium over the last 10 Gyr – I. Physical and dynamical properties

Huscher¹,

Oppenheimer

Lonardi³

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the physical and dynamical states of two sets of EAGLE zoom simulations of galaxy haloes, one at high redshift (z = 2 − 3) and the other at low redshift (z = 0), with masses of ≈1012 M⊙. Our focus is how the circumgalactic medium (CGM) of these L* star-forming galaxies change over the last 10 Gyr. We find that the high-z CGM is almost equally divided between the “cool” (T < 105 K) and “hot” (T ≥ 105 K) phases, while at low-z the hot CGM phase contains 5 × more mass than the cool phase. The high-z hot CGM contains 60% more metals than the cool CGM, while the low-z cool CGM contains 35% more metals than the hot CGM. The metals are evenly distributed radially between the hot and cool phases throughout the high-z CGM. At high z, the CGM volume is dominated by hot outflows, but also contains cool gas mainly inflowing and cool metals mainly outflowing. At low z, the cool metals dominate the interior and the hot metals are more prevalent at larger radii. The low-z cool CGM has tangential motions consistent with rotational support out to 0.2R200, often exhibiting r ≈ 40 kpc disc-like structures. The low-z hot CGM has several times greater angular momentum than the cool CGM, and a more flattened radial density profile than the high-z hot CGM. This study verifies that, just as galaxies demonstrate significant transformations over cosmic time, the gaseous haloes surrounding them also undergo considerable changes of their own both in physical characteristics of density, temperature, and metallicity, and dynamic properties of velocity and angular momentum.

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Section: Velocitymentioning

confidence: 99%

Section: Angular Momentummentioning

confidence: 99%

The changing circumgalactic medium over the last 10 Gyr – I. Physical and dynamical properties

Huscher¹,

Oppenheimer

Lonardi³

et al. 2020

Monthly Notices of the Royal Astronomical Society

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show abstract

“…While gas accretes on to galaxies from the cosmic web filaments, outflowing gas preferentially leaves the galaxy following the path of least resistance, along its minor axis. Where they compete, galactic winds prevent infall of material from regions above and below the disc place (Brook et al 2011;Mitchell et al 2020b;DeFelippis et al 2020). As a result, inflowing gas is almost co-planar with the major axis of the galaxy (Stewart et al 2011;Shen et al 2012;.…”

mentioning

confidence: 99%

Predictions for the angular dependence of gas mass flow rate and metallicity in the circumgalactic medium

Péroux

Nelson

Voort

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We use cosmological hydrodynamical simulations to examine the physical properties of the gas in the circumgalactic media (CGM) of star-forming galaxies as a function of angular orientation. We utilise TNG50 of the IllustrisTNG project, as well as the EAGLE simulation to show that observable properties of CGM gas correlate with azimuthal angle, defined as the galiocentric angle with respect to the central galaxy. Both simulations are in remarkable agreement in predicting a strong modulation of flow rate direction with azimuthal angle: inflow is more substantial along the galaxy major axis, while outflow is strongest along the minor axis. The absolute rates are noticeably larger for higher ($\log {(M_\star / \rm {M}_\odot )} \sim 10.5$) stellar mass galaxies, up to an order of magnitude compared to $\dot{M} \lesssim 1$ M⊙ yr−1 sr−1 for $\log {(M_\star / \rm {M}_\odot )}\sim 9.5$ objects. Notwithstanding the different numerical and physical models, both TNG50 and EAGLE predict that the average metallicity of the CGM is higher along the minor versus major axes of galaxies. The angular signal is robust across a wide range of galaxy stellar mass $8.5 < \log {(M_\star / \rm {M}_\odot )} < 10.5$ at z < 1. This azimuthal dependence is particularly clear at larger impact parameters b ≥ 100 kpc. Our results present a global picture whereby, despite the numerous mixing processes, there is a clear angular dependence of the CGM metallicity. We make forecasts for future large survey programs that will be able to compare against these expectations. Indeed, characterising the kinematics, spatial distribution and metal content of CGM gas is key to a full understanding of the exchange of mass, metals, and energy between galaxies and their surrounding environments.

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“…As disks evolve from z = 2 to the present, they must grow from a vast reservoir of corotating cold accreting material in the circumgalactic medium (CGM) as argued in Renzini (2020). This is also strongly supported by hydro-dynamical simulations which predict roughly coplanar gaseous structures (Stewart et al 2013(Stewart et al , 2017Danovich et al 2015;Ho et al 2019;Kretschmer et al 2020;DeFelippis et al 2021) embedded in a rotating CGM (DeFelippis et al 2020). These coplanar structures were initially found by Barcons et al (1995) and Steidel et al (2002) in a handful of background quasar sight-lines, but they are now routinely observed on scales of 20-80 kpc (as in Bouché et al 2013Bouché et al , 2016Ho et al 2017;Lopez et al 2018;Martin et al 2019;Zabl et al 2019).…”

Section: Introductionmentioning

confidence: 82%

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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The Angular Momentum of the Circumgalactic Medium in the TNG100 Simulation

Cited by 45 publications

References 87 publications

The changing circumgalactic medium over the last 10 Gyr – I. Physical and dynamical properties

The changing circumgalactic medium over the last 10 Gyr – I. Physical and dynamical properties

Predictions for the angular dependence of gas mass flow rate and metallicity in the circumgalactic medium

The MUSEHubbleUltra Deep Field Survey

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