Cosmological MHD simulations of massive clusters of galaxies adopted in this work. Here, we include only cosmological models, i.e. simulations that start from cosmologically motivated initial conditions on large spatial scales, which are run to z ∼ 0. These simulations differ in which they adopt not only different codes (smooth-particle hydrodynamics, adaptive-mesh refinement, meshless or moving mesh) but also different underlying galaxy formation models. All simulations include feedback from super-massive black holes, but with varying choices and implementations. IllustrisTNG includes MHD. Magneticum includes thermal conduction.
| Simulation project . | Hydrangea . | Horizon-AGN . | Magneticum . | IllustrisTNG . |
|---|---|---|---|---|
| Run(s) | Hydrangea Zooms | AGN | Box4, Box2b | TNG100 |
| Code | GADGET-3 | RAMSES | GADGET-3 | AREPO |
| Lowest available redshift | z = 0 | z = 0 | z = 0.2 | z = 0 |
| Box size (com Mpc) | 3200a | 142 | 68, 909 | 111 |
| Star-particle mass resolution (106 M⊙) | 1.8 | 2.0 | 2.6, 50 | 1.4 |
| # clusters with |$M_\mathrm{200c}\ge 10^{14}\, {\rm M}_{\odot }$| | 24 | 14 | 3, 4268 | 14 |
| # clusters analyzed in this paperb | 27 | 14 | 1, 13 | 11 |
| ΛCDM cosmology | Planck2014 | WMAP7 | WMAP7 | Planck2015 |
| Planck Collaboration (2014) | Komatsu et al. (2011) | Komatsu et al. (2011) | Planck Collaboration (2016) | |
| Star formation | density threshold | density-threshold | density-threshold | density-threshold |
| Stellar feedback: method | direct ISM heating | direct (momentum and energy) | direct energy, temporary | temporary hydro decoupling |
| decoupled momentum | ||||
| Stellar feedback: timing | stochastic, ΔT = 107.5K | continuous (winds + SNII + SNIa)† | (continuous thermal, probabilistic | continuous probabilistic, ∝ SFR |
| winds) ∝ SNII, | ||||
| continuous thermal ∝ SNIa | ||||
| Stellar feedback: feedback | thermal | kinetic + thermal | kinetic + thermal | kinetic + thermal (warm) |
| Stellar feedback: orientation | random | isotropic | isotropic | isotropic |
| SMBH: seed mass (106 M⊙) | 0.1 | 0.12, 0.45 | 1.2 | |
| SMBH: accretion | Eddington/Bondi–Hoyle–Lyttleton | Eddington/Bondi–Hoyle–Lyttleton | Bondi–Hoyle | |
| SMBH feedback: mode(s) | thermal | thermal (high), kinetic (low) | dual: radio/quasar mode* | dual:high-state/low-state |
| SMBH feedback: timing | stochastic, ΔT = 109K | continuous | contineous | continuous/pulsated |
| SMBH feedback: energy | thermal | thermal/kinetic | thermal | thermal/kinetic |
| SMBH feedback: orientation | random | isotropic (high)/bipolar (low) | isotropic | isotropic |
| Simulation/Method References | Schaye et al. (2015) | Dubois et al. (2014) | Hirschmann et al. (2014) | ♣ |
| Bahé et al. (2017) | Teklu et al. (2015) |
| Simulation project . | Hydrangea . | Horizon-AGN . | Magneticum . | IllustrisTNG . |
|---|---|---|---|---|
| Run(s) | Hydrangea Zooms | AGN | Box4, Box2b | TNG100 |
| Code | GADGET-3 | RAMSES | GADGET-3 | AREPO |
| Lowest available redshift | z = 0 | z = 0 | z = 0.2 | z = 0 |
| Box size (com Mpc) | 3200a | 142 | 68, 909 | 111 |
| Star-particle mass resolution (106 M⊙) | 1.8 | 2.0 | 2.6, 50 | 1.4 |
| # clusters with |$M_\mathrm{200c}\ge 10^{14}\, {\rm M}_{\odot }$| | 24 | 14 | 3, 4268 | 14 |
| # clusters analyzed in this paperb | 27 | 14 | 1, 13 | 11 |
| ΛCDM cosmology | Planck2014 | WMAP7 | WMAP7 | Planck2015 |
| Planck Collaboration (2014) | Komatsu et al. (2011) | Komatsu et al. (2011) | Planck Collaboration (2016) | |
| Star formation | density threshold | density-threshold | density-threshold | density-threshold |
| Stellar feedback: method | direct ISM heating | direct (momentum and energy) | direct energy, temporary | temporary hydro decoupling |
| decoupled momentum | ||||
| Stellar feedback: timing | stochastic, ΔT = 107.5K | continuous (winds + SNII + SNIa)† | (continuous thermal, probabilistic | continuous probabilistic, ∝ SFR |
| winds) ∝ SNII, | ||||
| continuous thermal ∝ SNIa | ||||
| Stellar feedback: feedback | thermal | kinetic + thermal | kinetic + thermal | kinetic + thermal (warm) |
| Stellar feedback: orientation | random | isotropic | isotropic | isotropic |
| SMBH: seed mass (106 M⊙) | 0.1 | 0.12, 0.45 | 1.2 | |
| SMBH: accretion | Eddington/Bondi–Hoyle–Lyttleton | Eddington/Bondi–Hoyle–Lyttleton | Bondi–Hoyle | |
| SMBH feedback: mode(s) | thermal | thermal (high), kinetic (low) | dual: radio/quasar mode* | dual:high-state/low-state |
| SMBH feedback: timing | stochastic, ΔT = 109K | continuous | contineous | continuous/pulsated |
| SMBH feedback: energy | thermal | thermal/kinetic | thermal | thermal/kinetic |
| SMBH feedback: orientation | random | isotropic (high)/bipolar (low) | isotropic | isotropic |
| Simulation/Method References | Schaye et al. (2015) | Dubois et al. (2014) | Hirschmann et al. (2014) | ♣ |
| Bahé et al. (2017) | Teklu et al. (2015) |
a Here, the box size denotes the size of the parent box: Hydrangea comprises a number of so-called zoom-in simulations, with haloes identified and resimulated out of a large parent box.
b For this paper, we focus on clusters in a narrow mass range, namely: |$\log _{10}\, (M_\mathrm{200c}\, /{\rm M}_{\odot }{}) = [14.0, 14.5]$|. Additionally, in the case of the Magneticum run Box2b, we apply additional selection criteria based on relaxedness (see text for details).
† SNII: (Girardi et al. 2000), winds: (Leitherer, Robert & Drissen 1992), SNIa: (Matteucci & Greggio 1986)
* Fabjan et al. (2010)
♣ Marinacci et al. (2018); Naiman et al. (2018); Nelson et al. (2018); Springel et al. (2018); Pillepich et al. (2018b); Nelson et al. (2019)
Cosmological MHD simulations of massive clusters of galaxies adopted in this work. Here, we include only cosmological models, i.e. simulations that start from cosmologically motivated initial conditions on large spatial scales, which are run to z ∼ 0. These simulations differ in which they adopt not only different codes (smooth-particle hydrodynamics, adaptive-mesh refinement, meshless or moving mesh) but also different underlying galaxy formation models. All simulations include feedback from super-massive black holes, but with varying choices and implementations. IllustrisTNG includes MHD. Magneticum includes thermal conduction.
| Simulation project . | Hydrangea . | Horizon-AGN . | Magneticum . | IllustrisTNG . |
|---|---|---|---|---|
| Run(s) | Hydrangea Zooms | AGN | Box4, Box2b | TNG100 |
| Code | GADGET-3 | RAMSES | GADGET-3 | AREPO |
| Lowest available redshift | z = 0 | z = 0 | z = 0.2 | z = 0 |
| Box size (com Mpc) | 3200a | 142 | 68, 909 | 111 |
| Star-particle mass resolution (106 M⊙) | 1.8 | 2.0 | 2.6, 50 | 1.4 |
| # clusters with |$M_\mathrm{200c}\ge 10^{14}\, {\rm M}_{\odot }$| | 24 | 14 | 3, 4268 | 14 |
| # clusters analyzed in this paperb | 27 | 14 | 1, 13 | 11 |
| ΛCDM cosmology | Planck2014 | WMAP7 | WMAP7 | Planck2015 |
| Planck Collaboration (2014) | Komatsu et al. (2011) | Komatsu et al. (2011) | Planck Collaboration (2016) | |
| Star formation | density threshold | density-threshold | density-threshold | density-threshold |
| Stellar feedback: method | direct ISM heating | direct (momentum and energy) | direct energy, temporary | temporary hydro decoupling |
| decoupled momentum | ||||
| Stellar feedback: timing | stochastic, ΔT = 107.5K | continuous (winds + SNII + SNIa)† | (continuous thermal, probabilistic | continuous probabilistic, ∝ SFR |
| winds) ∝ SNII, | ||||
| continuous thermal ∝ SNIa | ||||
| Stellar feedback: feedback | thermal | kinetic + thermal | kinetic + thermal | kinetic + thermal (warm) |
| Stellar feedback: orientation | random | isotropic | isotropic | isotropic |
| SMBH: seed mass (106 M⊙) | 0.1 | 0.12, 0.45 | 1.2 | |
| SMBH: accretion | Eddington/Bondi–Hoyle–Lyttleton | Eddington/Bondi–Hoyle–Lyttleton | Bondi–Hoyle | |
| SMBH feedback: mode(s) | thermal | thermal (high), kinetic (low) | dual: radio/quasar mode* | dual:high-state/low-state |
| SMBH feedback: timing | stochastic, ΔT = 109K | continuous | contineous | continuous/pulsated |
| SMBH feedback: energy | thermal | thermal/kinetic | thermal | thermal/kinetic |
| SMBH feedback: orientation | random | isotropic (high)/bipolar (low) | isotropic | isotropic |
| Simulation/Method References | Schaye et al. (2015) | Dubois et al. (2014) | Hirschmann et al. (2014) | ♣ |
| Bahé et al. (2017) | Teklu et al. (2015) |
| Simulation project . | Hydrangea . | Horizon-AGN . | Magneticum . | IllustrisTNG . |
|---|---|---|---|---|
| Run(s) | Hydrangea Zooms | AGN | Box4, Box2b | TNG100 |
| Code | GADGET-3 | RAMSES | GADGET-3 | AREPO |
| Lowest available redshift | z = 0 | z = 0 | z = 0.2 | z = 0 |
| Box size (com Mpc) | 3200a | 142 | 68, 909 | 111 |
| Star-particle mass resolution (106 M⊙) | 1.8 | 2.0 | 2.6, 50 | 1.4 |
| # clusters with |$M_\mathrm{200c}\ge 10^{14}\, {\rm M}_{\odot }$| | 24 | 14 | 3, 4268 | 14 |
| # clusters analyzed in this paperb | 27 | 14 | 1, 13 | 11 |
| ΛCDM cosmology | Planck2014 | WMAP7 | WMAP7 | Planck2015 |
| Planck Collaboration (2014) | Komatsu et al. (2011) | Komatsu et al. (2011) | Planck Collaboration (2016) | |
| Star formation | density threshold | density-threshold | density-threshold | density-threshold |
| Stellar feedback: method | direct ISM heating | direct (momentum and energy) | direct energy, temporary | temporary hydro decoupling |
| decoupled momentum | ||||
| Stellar feedback: timing | stochastic, ΔT = 107.5K | continuous (winds + SNII + SNIa)† | (continuous thermal, probabilistic | continuous probabilistic, ∝ SFR |
| winds) ∝ SNII, | ||||
| continuous thermal ∝ SNIa | ||||
| Stellar feedback: feedback | thermal | kinetic + thermal | kinetic + thermal | kinetic + thermal (warm) |
| Stellar feedback: orientation | random | isotropic | isotropic | isotropic |
| SMBH: seed mass (106 M⊙) | 0.1 | 0.12, 0.45 | 1.2 | |
| SMBH: accretion | Eddington/Bondi–Hoyle–Lyttleton | Eddington/Bondi–Hoyle–Lyttleton | Bondi–Hoyle | |
| SMBH feedback: mode(s) | thermal | thermal (high), kinetic (low) | dual: radio/quasar mode* | dual:high-state/low-state |
| SMBH feedback: timing | stochastic, ΔT = 109K | continuous | contineous | continuous/pulsated |
| SMBH feedback: energy | thermal | thermal/kinetic | thermal | thermal/kinetic |
| SMBH feedback: orientation | random | isotropic (high)/bipolar (low) | isotropic | isotropic |
| Simulation/Method References | Schaye et al. (2015) | Dubois et al. (2014) | Hirschmann et al. (2014) | ♣ |
| Bahé et al. (2017) | Teklu et al. (2015) |
a Here, the box size denotes the size of the parent box: Hydrangea comprises a number of so-called zoom-in simulations, with haloes identified and resimulated out of a large parent box.
b For this paper, we focus on clusters in a narrow mass range, namely: |$\log _{10}\, (M_\mathrm{200c}\, /{\rm M}_{\odot }{}) = [14.0, 14.5]$|. Additionally, in the case of the Magneticum run Box2b, we apply additional selection criteria based on relaxedness (see text for details).
† SNII: (Girardi et al. 2000), winds: (Leitherer, Robert & Drissen 1992), SNIa: (Matteucci & Greggio 1986)
* Fabjan et al. (2010)
♣ Marinacci et al. (2018); Naiman et al. (2018); Nelson et al. (2018); Springel et al. (2018); Pillepich et al. (2018b); Nelson et al. (2019)
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