Table 1.
Selected cluster properties for investigation of possible correlations.
| Symbol | Explanation |
|---|---|
| SFR | Instantaneous total star formation rate of the halo. |
| SFRc | Instantaneous total star formation rate of the central galaxy. |
| Z | Mass-weighted mean metallicity of all gas in the halo. |
| Zc | Mass-weighted mean metallicity of all gas in the central galaxy. |
| Nsat | The number of satellites in the halo with stellar masses above 109 M⊙. |
| M∗,halo | Stellar mass of the halo. |
| M∗,central | Stellar mass of the central galaxy, including all gravitationally bound stars. |
| MSMBH, tot | Total mass of all SMBHs in the halo. |
| MSMBH | Mass of the most massive SMBH in the halo (typically in the central galaxy). |
| ṀSMBH,tot | Total instantaneous mass accretion rate of all SMBHs in the halo. |
| μmode | A measure for the SMBH feedback mode of the most massive SMBH: the Eddington ratio normalized by the switchover threshold χ of the SMBH, i.e. μmode = (Ṁ/ṀEdd)/χ. a |
| Ecum, tot | Total cumulative energy injected by the most massive SMBH of the cluster over its lifetime. |
| Ecum, kin | Cumulative energy injected by the most massive SMBH while in the kinetic feedback mode. |
| Ecum, th | Cumulative energy injected by the most massive SMBH while in the thermal (quasar) feedback mode. |
| Ekin/Etot | Cumulative energy injected in kinetic mode by the most massive SMBH of the cluster, normalized by the total cumulative energy ejected irrespective of feedback mode. |
| Mkin/Mtot | Cumulative mass accretion of the most massive SMBH of the cluster while in kinetic mode over its total accreted mass. |
| Mcum, tot | Total cumulative mass accreted by the most massive SMBH of the cluster over its lifetime. |
| Mcum, kin | Cumulative mass accreted by the most massive SMBH while in the kinetic feedback mode. |
| Mcum, th | Cumulative mass accreted by the most massive SMBH while in the thermal (quasar) feedback mode |
| NSMBH, prog | Number of progenitors of the most massive SMBH of the cluster, i.e. number of SMBH mergers. |
| δr | Relaxedness, defined as the distance between the center of mass and the position of the most bound particle, normalized by R200c. b |
| Mcentral/Mtot | Relaxedness, defined as the ratio between the mass of the central subhalo and the total. b |
| zform | Formation redshift of the cluster, i.e. when the halo obtained half of its mass M200c. b |
| CCT | Central cooling time. c |
Notes. Selected cluster properties that we investigate for possible correlations with the cool gas mass fractions in clusters.
Gas in the halo refers to within the FoF group, while gas in the central galaxy must also be gravitationally bound.
See Weinberger et al. (2017); see Ayromlou et al. (2024); see Lehle et al. (2024).
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