First results from the IllustrisTNG simulations: a tale of two elements – chemical evolution of magnesium and europium

Naiman, Jill; Pillepich, Annalisa; Springel, Volker; Ramírez-Ruiz, E.; Torrey, Paul; Vogelsberger, Mark; Pakmor, Rüdiger; Nelson, Dylan; Marinacci, Federico; Hernquist, Lars; Weinberger, Rainer; Genel, Shy

doi:10.1093/mnras/sty618

Cited by 1,224 publications

(870 citation statements)

References 151 publications

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“…Weinberger et al (2018) and Pillepich et al (2018a) provide a complete description of the physical models. Additional details about these simulations are given by Pillepich et al (2018b), Springel et al (2018), Nelson et al (2018), Naiman et al (2018), and Marinacci et al (2018).…”

Section: The Illustristng Simulationsmentioning

confidence: 99%

Interacting galaxies in the IllustrisTNG simulations - I: Triggered star formation in a cosmological context

Patton

Wilson

Metrow

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We use the IllustrisTNG cosmological hydrodynamical simulations to investigate how the specific star formation rates (sSFRs) of massive galaxies (M * > 10 10 M ) depend on the distance to their closest companions. We estimate sSFR enhancements by comparing with control samples that are matched in redshift, stellar mass, local density and isolation, and we restrict our analysis to pairs with stellar mass ratios of 0.1 to 10. At small separations (∼ 15 kpc), the mean sSFR is enhanced by a factor of 2.0 ± 0.1 in the flagship (110.7 Mpc) 3 simulation (TNG100-1). Statistically significant enhancements extend out to 3D separations of 280 kpc in the (302.6 Mpc) 3 simulation (TNG300-1). We find similar trends in the EAGLE and Illustris simulations, although their sSFR enhancements are lower than those in TNG100-1 by about a factor of two. Enhancements in IllustrisTNG galaxies are seen throughout the redshift range explored (0 z < 1), with the strength of the enhancements decreasing with increasing redshift for galaxies with close companions. In order to more closely compare with observational results, we separately consider 2D projected distances between galaxies in IllustrisTNG. We detect significant sSFR enhancements out to projected separations of 260 kpc in TNG300-1, with projection effects diluting the size of the enhancements by about 20 per cent below 50 kpc. We find similar sSFR enhancements in TNG100-1 and Sloan Digital Sky Survey galaxies, with enhancements extending out to projected separations of about 150 kpc for star-forming galaxies at z < 0.2. Finally, by summing over all separations, we estimate that the presence of closest companions boosts the average sSFR of massive galaxies in TNG100-1 by 14.5 per cent.

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Section: The Illustristng Simulationsmentioning

confidence: 99%

Interacting galaxies in the IllustrisTNG simulations - I: Triggered star formation in a cosmological context

Patton

Wilson

Metrow

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The sample and measured quantities are derived from the TNG300 solution of the IllustrisTNG project 1 . Our sample consists of a subset of data that is provided publicly by the IllustrisTNG team (Nelson et al 2018;Pillepich et al 2018a;Springel et al 2018;Marinacci et al 2018;Naiman et al 2018).…”

Section: The Samplementioning

confidence: 99%

Aging haloes: implications of the magnitude gap on conditional statistics of stellar and gas properties of massive haloes

Farahi

Trac

2020

Monthly Notices of the Royal Astronomical Society

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Cold dark matter model predicts that the large-scale structure grows hierarchically. Small dark matter halos form first. Then, they grow gradually via continuous merger and accretion. These halos host the majority of baryonic matter in the Universe in the form of hot gas and cold stellar phase. Determining how baryons are partitioned into these phases requires detailed modeling of galaxy formation and their assembly history. It is speculated that formation time of the same mass halos might be correlated with their baryonic content. To evaluate this hypothesis, we employ halos of mass above 10 14 M realized by TNG300 solution of the IllustrisTNG project. Formation time is not directly observable. Hence, we rely on the magnitude gap between the brightest and the fourth brightest halo galaxy member, which is shown that traces formation time of the host halo. We compute the conditional statistics of the stellar and gas content of halos conditioned on their total mass and magnitude gap. We find a strong correlation between magnitude gap and gas mass, BCG stellar mass, and satellite galaxies stellar mass, but not the total stellar mass of halo. Conditioning on the magnitude gap can reduce the scatter about halo property-halo mass relation and has a significant impact on the conditional covariance. Reduction in the scatter can be as significant as 30%, which implies more accurate halo mass prediction. Incorporating the magnitude gap has a potential to improve cosmological constraints using halo abundance and allows us to gain insight into the baryon evolution within these systems.

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“…). However, a more realistic treatment of mixing has resulted in differing conclusions on whether NSMs can explain the [Eu/Fe] scatter at low metallicities in the halo (Naiman et al 2018;Haynes & Kobayashi 2019).…”

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confidence: 99%

The Stars in M15 Were Born with the r-process*

Kirby

Duggan

Ramírez-Ruiz

et al. 2020

ApJL

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High-resolution spectroscopy of stars on the red giant branch (RGB) of the globular cluster M15 has revealed a large (∼ 1 dex) dispersion in the abundances of r-process elements, like Ba and Eu. Neutron star mergers (NSMs) have been proposed as a major source of the r-process. However, most NSM models predict a delay time longer than the timescale for cluster formation. One possibility is that a NSM polluted the surfaces of stars in M15 long after the cluster finished forming. In this case, the abundances of the polluting elements would decrease in the first dredge-up as stars turn on to the RGB. We present Keck/DEIMOS abundances of Ba in 66 stars along the entire RGB and the top of the main sequence. The Ba abundances have no trend with stellar luminosity (evolutionary phase). Therefore, the stars were born with the Ba they have today, and Ba did not originate in a source with a delay time longer than the timescale for cluster formation. In particular, if the source of Ba was a neutron star merger, it would have had a very short delay time. Alternatively, if Ba enrichment took place before the formation of the cluster, an inhomogeneity of a factor of 30 in Ba abundance needs to be able to persist over the length scale of the gas cloud that formed M15, which is unlikely.

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First results from the IllustrisTNG simulations: a tale of two elements – chemical evolution of magnesium and europium

Cited by 1,224 publications

References 151 publications

Interacting galaxies in the IllustrisTNG simulations - I: Triggered star formation in a cosmological context

Interacting galaxies in the IllustrisTNG simulations - I: Triggered star formation in a cosmological context

Aging haloes: implications of the magnitude gap on conditional statistics of stellar and gas properties of massive haloes

The Stars in M15 Were Born with the r-process*

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