Simulations

This pages lists the various FLAMINGO simulations and their parameters. The first table describes the hydrodynamical simulations, the second table lists the dark matter only simulations, and the third table lists the various cosmologies.

Hydrodynamical simulations

The first table below contain the hydrodynamical simulations in the set. The first four lines list the simulations that use the fiducial galaxy formation model and assume the fiducial cosmology, but use different volumes and resolutions. The remaining lines list the model variations, which all use a 1 Gpc box and intermediate resolution. The link after each simulation name gives the paper where the simulation was introduced. The columns list the simulation identifier (where m8, m9 and m10 indicate log₁₀ of the mean baryonic particle mass and correspond to high, intermediate, and low resolution, respectively; absence of this part implies m9 resolution); the number of standard deviations by which the observed stellar masses are shifted before calibration, Δm_*; the number of standard deviations by which the observed cluster gas fractions are shifted before calibration, Δf_gas; the AGN feedback implementation (thermal or jets); the comoving box side length, L; the number of baryonic particles, N_b (which equals the number of CDM particles, N_CDM; the number of neutrino particles, N_ν; the initial mean baryonic particle mass, m_g; the mean CDM particle mass, m_CDM; the Plummer-equivalent comoving gravitational softening length, ε_com; the maximum proper gravitational softening length, ε_prop; and the assumed cosmology (which refers to the cosmology table).

Dark matter only simulations

The second table contains the gravity-only FLAMINGO simulations. Simulation L1_m9_ip_DMO is identical to L1_m9_DMO except that the phases in the initial conditions were inverted. Note that there are no hydrodynamical counterparts for L5p6_m10_DMO, PlanckNu0p12Var_DMO, L1_m9_ip_DMO, L11p2_m11_DMO, and FLAMINGO-10K.

Cosmologies

Finally, the table below lists the values of the cosmological parameters used in different simulations (Table 4 from Schaye et al. 2023, Table 1 from Elbers et al. 2024). The columns list the prefix used to indicate the cosmology in the simulation name (note that for brevity the prefix 'D3A' that indicates the fiducial cosmology is omitted from the simulation identifiers); the dimensionless Hubble constant, h; the total matter density parameter, Ω_m; the dark energy density parameter, Ω_Λ; the baryonic matter density parameter, Ω_b; the sum of the particle masses of the neutrino species, ∑ m_νc²; the amplitude of the primordial matter power spectrum, A_s; the power-law index of the primordial matter power spectrum, n_s; the amplitude of the initial power spectrum parametrized as the r.m.s. mass density fluctuation in spheres of radius 8 h^-1 Mpc extrapolated to z=0 using linear theory, σ₈; the amplitude of the initial power spectrum parametrized as S₈ ≡ σ₈(Ω_m/0.3)^1/2; the neutrino matter density parameter, Ω_ν ≅ ∑ m_νc²/(93.14 h² eV); the dark matter decay rate, Γ. Note that the values of the Hubble and density parameters are given at z=0.

References

[1] The FLAMINGO project: cosmological hydrodynamical simulations for large-scale structure and galaxy cluster surveys (Schaye et al. 2023)

[2] The FLAMINGO project: the coupling between baryonic feedback and cosmology in light of the S8 tension (Elbers et al. 2024)

[3] A unified model for the clustering of quasars and galaxies at z≈6 (Pizzati et al. 2024)

[4] FLAMINGO: combining kinetic SZ effect and galaxy-galaxy lensing measurements to gauge the impact of feedback on large-scale structure (McCarthy et al. 2024)

[5] L1_m9_ip_DMO has not been presented in any of the FLAMINGO papers. It is identical to L1_m9_DMO except that the phases in the initial conditions were inverted.