A web portal for hydrodynamical, cosmological simulations

Ragagnin, Antonio; Dolag, K.; Biffi, V.; Bel, M. Cadolle; Hammer, N. J.; Krukau, Aliaksei; Petkova, Margarita; Steinborn, Daniel

doi:10.1016/j.ascom.2017.05.001

Cited by 56 publications

(48 citation statements)

References 29 publications

(42 reference statements)

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“…This indicates that the origin of the variation is due to macroscopic events, linked to the global evolution of the clusters. The same trend is found in the clusters extracted from the cosmological box (of size 640h −1 Mpc) of the Magneticum simulations 9 (Dolag et al 2016;Ragagnin et al 2017) at redshifts z = 0 and z ≈ 1, 1.5, 2. As a further confirmation that this finding does not depend on the SZ-like selection, we explore the slope evolution for the M − T sl relations derived from all objects that at each redshift are above M500 > 10 13 M .…”

Section: The Slopesupporting

confidence: 80%

Cosmological hydrodynamical simulations of galaxy clusters: X-ray scaling relations and their evolution

Truong

Rasia

Mazzotta

et al. 2017

Monthly Notices of the Royal Astronomical Society

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102

118

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We analyse cosmological hydrodynamical simulations of galaxy clusters to study the X-ray scaling relations between total masses and observable quantities such as X-ray luminosity, gas mass, X-ray temperature, and Y X . Three sets of simulations are performed with an improved version of the smoothed-particle-hydrodynamics GADGET-3 code. These consider the following: non-radiative gas, star formation and stellar feedback, and the addition of activegalactic-nucleus (AGN) feedback. We select clusters with M 500 > 10 14 M E(z) −1 , mimicking the typical selection of Sunyaev-Zeldovich samples. This permits to have a mass range large enough to enable robust fitting of the relations even at z ∼ 2. The results of the analysis show a general agreement with observations. The values of the slope of the mass -gas mass and mass − temperature relations at z = 2 are 10 per cent lower with respect to z = 0 due to the applied mass selection, in the former case, and to the effect of early merger in the latter. We investigate the impact of the slope variation on the study of the evolution of the normalization. We conclude that cosmological studies through scaling relations should be limited to the redshift range z = 0 − 1, where we find that the slope, the scatter, and the covariance matrix of the relations are stable. The scaling between mass and Y X is confirmed to be the most robust relation, being almost independent of the gas physics. At higher redshifts, the scaling relations are sensitive to the inclusion of AGNs which influences low-mass systems. The detailed study of these objects will be crucial to evaluate the AGN effect on the ICM.

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Section: The Slopesupporting

confidence: 80%

Cosmological hydrodynamical simulations of galaxy clusters: X-ray scaling relations and their evolution

Truong

Rasia

Mazzotta

et al. 2017

Monthly Notices of the Royal Astronomical Society

Self Cite

102

118

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“…• 500Mpc/hr: The second simulation considered in this work comprises a large volume of (500Mpc) 3 with a resolution of M dm = 6.9 · 10 8 M /h and Mgas = 1.4 · 10 8 M /h, enabling us to study the evolution of a large AGN population, including very massive and very luminous AGN (Hirschmann et al 2014). This simulation run is publicly available via our web interface (see Ragagnin et al 2017).…”

Section: The Theoretical Set-upmentioning

confidence: 99%

Cosmological simulations of black hole growth II: how (in)significant are merger events for fuelling nuclear activity?

Steinborn

Hirschmann

Dolag

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Which mechanism(s) are mainly driving nuclear activity in the centres of galaxies is a major unsettled question. In this study, we investigate the statistical relevance of galaxy mergers for fuelling gas onto the central few kpc of a galaxy, potentially resulting in an active galactic nucleus (AGN). To robustly address that, we employ large-scale cosmological hydrodynamic simulations from the Magneticum Pathfinder set, including models for BH accretion and AGN feedback. Our simulations predict that for luminous AGN (L AGN > 10 45 erg/s) at z = 2, more than 50 per cent of their host galaxies have experienced a merger in the last 0.5 Gyr. These high merger fractions, however, merely reflect the intrinsically high merger fractions of massive galaxies at z = 2, in which luminous AGN preferentially occur. Apart from that, our simulations suggest that merger events are not the statistically dominant fuelling mechanism for nuclear activity over a redshift range z = 0−2: irrespective of AGN luminosity, less than 20 per cent of AGN hosts have on average undergone a recent merger, in agreement with a number of observational studies. The central ISM conditions required for inducing AGN activity can be, but are not necessarily caused by a merger. Despite the statistically minor relevance of mergers, at a given AGN luminosity and stellar mass, the merger fractions of AGN hosts can be by up to three times higher than that of inactive galaxies. Such elevated merger fractions still point towards an intrinsic connection between AGN and mergers, consistent with our traditional expectation.

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“…More recently, significant infrastructure research and development has focused on providing remote computational resources, including the NOAO Data Lab (Fitzpatrick et al, 2014) and the SciServer project (Medvedev et al, 2016;Raddick et al, 2017). Web-based orchestration projects also include Ragagnin et al (2017), Tangos (Pontzen and Tremmel, 2018), and Jovial (Araya et al, 2018).…”

Section: Introductionmentioning

confidence: 99%

The IllustrisTNG simulations: public data release

et al. 2019

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We present the full public release of all data from the TNG100 and TNG300 simulations of the Illus-trisTNG project. IllustrisTNG is a suite of large volume, cosmological, gravo-magnetohydrodynamical simulations run with the moving-mesh code Arepo. TNG includes a comprehensive model for galaxy formation physics, and each TNG simulation selfconsistently solves for the coupled evolution of dark matter, cosmic gas, luminous stars, and supermassive blackholes from early time to the present day, z = 0. Each of the flagship runs -TNG50, TNG100, and TNG300 -are accompanied by halo/subhalo catalogs, merger trees, lower-resolution and darkmatter only counterparts, all available with 100 snapshots. We discuss scientific and numerical cautions and caveats relevant when using TNG.The data volume now directly accessible online is ∼750 TB, including 1200 full volume snapshots and ∼80,000 high time-resolution subbox snapshots. This will increase to ∼1.1 PB with the future release of TNG50. Data access and analysis examples are available in IDL, Python, and Matlab. We describe improvements and new functionality in the webbased API, including on-demand visualization and analysis of galaxies and halos, exploratory plotting of scaling relations and other relationships between galactic and halo properties, and a new Jupyter-Lab interface. This provides an online, browserbased, near-native data analysis platform enabling user computation with local access to TNG data, alleviating the need to download large datasets.

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A web portal for hydrodynamical, cosmological simulations

Cited by 56 publications

References 29 publications

Cosmological hydrodynamical simulations of galaxy clusters: X-ray scaling relations and their evolution

Cosmological hydrodynamical simulations of galaxy clusters: X-ray scaling relations and their evolution

Cosmological simulations of black hole growth II: how (in)significant are merger events for fuelling nuclear activity?

The IllustrisTNG simulations: public data release

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