First results from the TNG50 simulation: galactic outflows driven by supernovae and black hole feedback

Nelson, Dylan; Pillepich, Annalisa; Springel, Volker; Pakmor, Rüdiger; Weinberger, Rainer; Genel, Shy; Torrey, Paul; Vogelsberger, Mark; Marinacci, Federico; Hernquist, Lars

doi:10.1093/mnras/stz2306

Cited by 794 publications

(710 citation statements)

References 185 publications

(213 reference statements)

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“…Figure 3 shows outflow velocities, v out,90,r=10 kpc , defined as the 90th percentile of the flux-weighted velocity distribution at a radius of 10 kpc, at z = 0.2, 1, 2, and 6 in stellar mass ranges similar to observational data points at the redshifts. This theoretical prediction by Nelson et al (2019) agrees well with our observational measurements, although the trend at z ∼ 0 is different. Muratov et al (2015) calculate the flux-weighted velocity of the outflowing gas at one quarter of the halo virial radius with the Feedback in Realistic Environments (FIRE) simulations, which computes the thermal and momentum input to the ISM considering the stellar and SN feedback.…”

Section: Comparisons With Theoretical Modelssupporting

confidence: 90%

“…Recent numerical and zoom-in simulations can be used to predict outflow velocities. These simulations compute energy input to the ISM surrounding SNe and investigate the statistics of galaxy and outflow properties (e.g., Muratov et al 2015;Christensen et al 2016;Mitchell et al 2018;Nelson et al 2019). Here we compare our results with simulation work that studies the redshift evolution of the outflow velocities.…”

Section: Comparisons With Theoretical Modelsmentioning

confidence: 99%

“…As described in Section 3 our observational technique traces low-ionized elements in warm gas ( 10 4 K). On the other hand, Muratov et al (2015) and Nelson et al (2019) compute the v max -v cir (M * ) relation from outflowing gas with all temperatures. It is noteworthy that a non-negligible fraction of outflowing gas in numerical simulations would be in a hot, diffuse phase which are not observable with optical absorption lines (e.g., Mitchell et al 2018;Nelson et al 2019).…”

Section: Comparisons With Theoretical Modelsmentioning

confidence: 99%

“…On the other hand, Muratov et al (2015) and Nelson et al (2019) compute the v max -v cir (M * ) relation from outflowing gas with all temperatures. It is noteworthy that a non-negligible fraction of outflowing gas in numerical simulations would be in a hot, diffuse phase which are not observable with optical absorption lines (e.g., Mitchell et al 2018;Nelson et al 2019). Moreover, in some numerical simulations, outflows in a hot phase tend to exhibit faster velocities than those in cold phases (e.g., Gallerani et al 2018;Mitchell et al 2018).…”

Section: Comparisons With Theoretical Modelsmentioning

confidence: 99%

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Fast Outflows Identified in Early Star-forming Galaxies at z = 5–6

Sugahara

Ouchi

Harikane

et al. 2019

ApJ

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We present velocities of galactic outflows in seven star-forming galaxies at z = 5-6 with stellar masses of M * ∼ 10 10.1 M . Although it is challenging to observationally determine the outflow velocities, we overcome this by using ALMA [C II]158 µm emission lines for systemic velocities and deep Keck spectra with metal absorption lines for velocity profiles available to date. We construct a composite Keck spectrum of the galaxies at z = 5-6 with the [C II]-systemic velocities, and fit outflow-line profiles to the Si II λ1260, C II λ1335, and Si IV λλ1394, 1403 absorption lines in the composite spectrum. We measure the maximum (90%) and central outflow velocities to be v max = 700 +180 −110 km s −1 and v out = 400 +100 −150 km s −1 on average, respectively, showing no significant differences between the outflow velocities derived with the low to high-ionization absorption lines. For M * ∼ 10 10.1 M , we find that the v max value of our z = 5-6 galaxies is 3 times higher than those of z ∼ 0 galaxies and comparable to z ∼ 2 galaxies. Estimating the halo circular velocity v cir from the stellar masses and the abundance matching results, we investigate a v max -v cir relation. Interestingly, v max for galaxies with M * = 10 10.0-10.8 M shows a clear positive correlation with v cir and/or the galaxy star formation rate over z = 0-6 with a small scatter of ±0.1 dex, which is in good agreement with theoretical predictions. This positive correlation suggests that the outflow velocity is physically related to the halo circular velocity, and that the redshift evolution of v max at fixed M * is explained by the increase in v cir toward high redshift.

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Section: Comparisons With Theoretical Modelssupporting

confidence: 90%

Section: Comparisons With Theoretical Modelsmentioning

confidence: 99%

Section: Comparisons With Theoretical Modelsmentioning

confidence: 99%

Section: Comparisons With Theoretical Modelsmentioning

confidence: 99%

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Fast Outflows Identified in Early Star-forming Galaxies at z = 5–6

Sugahara

Ouchi

Harikane

et al. 2019

ApJ

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“…However, fully investigating the merger-induced SFR budget requires a much higher mass resolution. Such a study will be possible with the forthcoming IllustrisTNG50 simulation (Nelson et al 2019b;Pillepich et al 2019).…”

Section: Q(ssf R)mentioning

confidence: 99%

Interacting galaxies in the IllustrisTNG simulations – II: star formation in the post-merger stage

Hani

Gosain

Ellison

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Galaxy mergers are a major evolutionary transformation whose effects are borne out by a plethora of observations and numerical simulations. However, most previous simulations have used idealised, isolated, binary mergers and there has not been significant progress on studying statistical samples of galaxy mergers in large cosmological simulations. We present a sample of 27,691 post-merger (PM) galaxies (0 ≤ z ≤ 1) identified from IllustrisTNG: a cosmological, large box, magneto-hydrodynamical simulation suite. The PM sample spans a wide range of merger and galaxy properties (M , µ, f gas ). We demonstrate that star forming (SF) PMs exhibit enhanced star formation rates (SFRs) on average by a factor of ∼ 2, while the passive PMs show no statistical enhancement. We find that the SFR enhancements: (1) show no dependence on redshift, (2) anti-correlate with the PM's stellar mass, and (3) correlate with the gas fraction of the PM's progenitors. However, SF PMs show stronger enhancements which may indicate other processes being at play (e.g., gas phase, feedback efficiency). Although the SFR enhancement correlates mildly with the merger mass ratio, the more abundant minor mergers (0.1 ≤ µ < 0.3) still contribute ∼ 50% of the total SFR enhancement. By tracing the PM sample forward in time, we find that galaxy mergers can drive significant SFR enhancements which decay over ∼ 0.5 Gyr independent of the merger mass ratio, although the decay timescale is dependent on the simulation resolution. The strongest merger-driven starburst galaxies evolve to be passive/quenched on faster timescales than their controls.

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Massive Black-Hole Mergers

Barausse

Lapi

2021

Handbook of Gravitational Wave Astronomy

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First results from the TNG50 simulation: galactic outflows driven by supernovae and black hole feedback

Cited by 794 publications

References 185 publications

Fast Outflows Identified in Early Star-forming Galaxies at z = 5–6

Fast Outflows Identified in Early Star-forming Galaxies at z = 5–6

Interacting galaxies in the IllustrisTNG simulations – II: star formation in the post-merger stage

Massive Black-Hole Mergers

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