Simulation characteristics for the z = 0 halo samples. Table adapted from Anbajagane et al. (2020) with modifications. Note that for MGTM alone we do not have a z = 0 data set and thus characterize the z = 0.06 output instead. From left to right, we show: (i) simulation acronym as used in this work, (ii) comoving box size, (iii) cosmic matter density parameter at the present epoch, (iv) Hubble constant, (v) force softening scale, (vi) initial mass of stellar particles, (vii) mass of DM particles, (viii) number of haloes with |$M_{\rm 200c}\gt 10^{13.5} \, {\rm M}_\odot$|, (ix) number of satellite galaxies within r < R200c of host haloes with |$M_{\rm 200c}\gt 10^{13.5} \, {\rm M}_\odot$| and above the minimum stellar mass threshold used for each simulation, and (x) empirical sources used for tuning sub-grid parameters of each simulation, which consist of the Galaxy Stellar Mass Function (GSMF), supermassive black hole scaling (SMBH), metallicity scaling (metals), and cluster hot gas mass fraction <R500c (CL fgas). All simulations assume a flat ΛCDM cosmology, with |$\Omega _\Lambda = 1- \Omega _m$|. See text for references. MDPL2 is an N-body, DMO simulation, and does not have stellar particles, and The300 consists of zoom-in (re)simulations of the 324 most massive haloes drawn from MDPL2.
| Simulation . | L [Mpc] . | Ωm . | |$H_0\, [\frac{\rm km\,s^{ -1}}{\, {\rm Mpc}}]$| . | |$\epsilon _{\rm \, DM}^{z=0} \, \rm [kpc]$| . | |$m_\star \, [\, {\rm M}_\odot ]$| . | |$m_{\rm DM} \, [\, {\rm M}_\odot ]$| . | Nhaloes . | |$N_{\rm sat, tot}$| . | Calibration . |
|---|---|---|---|---|---|---|---|---|---|
| TNG300 | 303 | 0.3089 | 67.74 | 1.48 | 1.1 × 107 | 5.9 × 107 | 1146 | 40436 | See Pillepich et al. (2018a) |
| MGTM | 500 | 0.2726 | 70.40 | 5.33 | 5.0 × 107 | 9.8 × 108 | 4207 | 90255 | SMBH, Metals, CL fgas |
| BM | 596 | 0.3175 | 67.11 | 5.96 | 1.2 × 109 | 6.6 × 109 | 9430 | 132334 | GSMF, CL fgas |
| MDPL2 | 1475 | 0.3071 | 67.77 | 7.4 | – | 2.2 × 109 | 157051 | 2339642 | See Behroozi et al. (2019) |
| The300 | – | 0.3071 | 67.77 | 9.6 | 3.5 × 108 | 1.9 × 109 | 3180 | 156662 | See Cui et al. (2018) |
| Simulation . | L [Mpc] . | Ωm . | |$H_0\, [\frac{\rm km\,s^{ -1}}{\, {\rm Mpc}}]$| . | |$\epsilon _{\rm \, DM}^{z=0} \, \rm [kpc]$| . | |$m_\star \, [\, {\rm M}_\odot ]$| . | |$m_{\rm DM} \, [\, {\rm M}_\odot ]$| . | Nhaloes . | |$N_{\rm sat, tot}$| . | Calibration . |
|---|---|---|---|---|---|---|---|---|---|
| TNG300 | 303 | 0.3089 | 67.74 | 1.48 | 1.1 × 107 | 5.9 × 107 | 1146 | 40436 | See Pillepich et al. (2018a) |
| MGTM | 500 | 0.2726 | 70.40 | 5.33 | 5.0 × 107 | 9.8 × 108 | 4207 | 90255 | SMBH, Metals, CL fgas |
| BM | 596 | 0.3175 | 67.11 | 5.96 | 1.2 × 109 | 6.6 × 109 | 9430 | 132334 | GSMF, CL fgas |
| MDPL2 | 1475 | 0.3071 | 67.77 | 7.4 | – | 2.2 × 109 | 157051 | 2339642 | See Behroozi et al. (2019) |
| The300 | – | 0.3071 | 67.77 | 9.6 | 3.5 × 108 | 1.9 × 109 | 3180 | 156662 | See Cui et al. (2018) |
Simulation characteristics for the z = 0 halo samples. Table adapted from Anbajagane et al. (2020) with modifications. Note that for MGTM alone we do not have a z = 0 data set and thus characterize the z = 0.06 output instead. From left to right, we show: (i) simulation acronym as used in this work, (ii) comoving box size, (iii) cosmic matter density parameter at the present epoch, (iv) Hubble constant, (v) force softening scale, (vi) initial mass of stellar particles, (vii) mass of DM particles, (viii) number of haloes with |$M_{\rm 200c}\gt 10^{13.5} \, {\rm M}_\odot$|, (ix) number of satellite galaxies within r < R200c of host haloes with |$M_{\rm 200c}\gt 10^{13.5} \, {\rm M}_\odot$| and above the minimum stellar mass threshold used for each simulation, and (x) empirical sources used for tuning sub-grid parameters of each simulation, which consist of the Galaxy Stellar Mass Function (GSMF), supermassive black hole scaling (SMBH), metallicity scaling (metals), and cluster hot gas mass fraction <R500c (CL fgas). All simulations assume a flat ΛCDM cosmology, with |$\Omega _\Lambda = 1- \Omega _m$|. See text for references. MDPL2 is an N-body, DMO simulation, and does not have stellar particles, and The300 consists of zoom-in (re)simulations of the 324 most massive haloes drawn from MDPL2.
| Simulation . | L [Mpc] . | Ωm . | |$H_0\, [\frac{\rm km\,s^{ -1}}{\, {\rm Mpc}}]$| . | |$\epsilon _{\rm \, DM}^{z=0} \, \rm [kpc]$| . | |$m_\star \, [\, {\rm M}_\odot ]$| . | |$m_{\rm DM} \, [\, {\rm M}_\odot ]$| . | Nhaloes . | |$N_{\rm sat, tot}$| . | Calibration . |
|---|---|---|---|---|---|---|---|---|---|
| TNG300 | 303 | 0.3089 | 67.74 | 1.48 | 1.1 × 107 | 5.9 × 107 | 1146 | 40436 | See Pillepich et al. (2018a) |
| MGTM | 500 | 0.2726 | 70.40 | 5.33 | 5.0 × 107 | 9.8 × 108 | 4207 | 90255 | SMBH, Metals, CL fgas |
| BM | 596 | 0.3175 | 67.11 | 5.96 | 1.2 × 109 | 6.6 × 109 | 9430 | 132334 | GSMF, CL fgas |
| MDPL2 | 1475 | 0.3071 | 67.77 | 7.4 | – | 2.2 × 109 | 157051 | 2339642 | See Behroozi et al. (2019) |
| The300 | – | 0.3071 | 67.77 | 9.6 | 3.5 × 108 | 1.9 × 109 | 3180 | 156662 | See Cui et al. (2018) |
| Simulation . | L [Mpc] . | Ωm . | |$H_0\, [\frac{\rm km\,s^{ -1}}{\, {\rm Mpc}}]$| . | |$\epsilon _{\rm \, DM}^{z=0} \, \rm [kpc]$| . | |$m_\star \, [\, {\rm M}_\odot ]$| . | |$m_{\rm DM} \, [\, {\rm M}_\odot ]$| . | Nhaloes . | |$N_{\rm sat, tot}$| . | Calibration . |
|---|---|---|---|---|---|---|---|---|---|
| TNG300 | 303 | 0.3089 | 67.74 | 1.48 | 1.1 × 107 | 5.9 × 107 | 1146 | 40436 | See Pillepich et al. (2018a) |
| MGTM | 500 | 0.2726 | 70.40 | 5.33 | 5.0 × 107 | 9.8 × 108 | 4207 | 90255 | SMBH, Metals, CL fgas |
| BM | 596 | 0.3175 | 67.11 | 5.96 | 1.2 × 109 | 6.6 × 109 | 9430 | 132334 | GSMF, CL fgas |
| MDPL2 | 1475 | 0.3071 | 67.77 | 7.4 | – | 2.2 × 109 | 157051 | 2339642 | See Behroozi et al. (2019) |
| The300 | – | 0.3071 | 67.77 | 9.6 | 3.5 × 108 | 1.9 × 109 | 3180 | 156662 | See Cui et al. (2018) |
This PDF is available to Subscribers Only
View Article Abstract & Purchase OptionsFor full access to this pdf, sign in to an existing account, or purchase an annual subscription.
