Table 2.
Best-fitting effective halo model parameters for different combinations of power spectra from the BAHAMAS simulations.
Model | Parameter | Equation | Fitted parameter | 107.6 K | 107.8 K | 108.0 K |
---|---|---|---|---|---|---|
(1) Stars | A* = A*, 0 + A*, 1z | (27) | A*, 0 | 0.0348 | 0.0330 | 0.0309 |
A*, 1 | −0.0093 | −0.0088 | −0.0082 | |||
M* = M*, 0exp(M*, 1z) | (27) | log10(M*, 0/ h−1 M⊙) | 12.4620 | 12.4479 | 12.3923 | |
M*, 1 | −0.3664 | −0.3521 | −0.3073 | |||
η | (29) | η | −0.3428 | −0.3556 | −0.3505 | |
(2) Matter | ϵ1 = ϵ1, 0 + ϵ1, 1z | (34) | ϵ1, 0 | 0.2841 | 0.2038 | 0.0526 |
ϵ1, 1 | −0.0046 | −0.0047 | 0.0365 | |||
Γ | (35) | Γ | 1.2363 | 1.3376 | 1.6237 | |
M0 | (25) | log10(M0/h−1 M⊙) | 13.0020 | 13.3658 | 14.0226 | |
(3) Matter, electron pressure | ϵ1 = ϵ1, 0 + ϵ1, 1z | (34) | ϵ1, 0 | −0.1002 | −0.1065 | −0.1253 |
ϵ1, 1 | −0.0456 | −0.1073 | −0.0111 | |||
Γ | (35) | Γ | 1.1647 | 1.1770 | 1.1966 | |
M0 | (25) | log10(M0/h−1 M⊙) | 13.1949 | 13.5937 | 14.2480 | |
α | (39) | α | 0.7642 | 0.8471 | 1.0314 | |
Tw = Tw, 0exp(Tw, 1z) | Below (40) | log10(Tw, 0/K) | 6.6762 | 6.6545 | 6.6615 | |
Tw, 1 | −0.5566 | −0.3652 | −0.0617 | |||
(4) Matter, CDM, gas, stars | A* = A*, 0 + A*, 1z | (27) | A*, 0 | 0.0346 | 0.0342 | 0.0321 |
A*, 1 | −0.0092 | −0.0105 | −0.0094 | |||
M* = M*, 0exp(M*, 1z) | (27) | log10(M*, 0/h−1 M⊙) | 12.5506 | 12.3715 | 12.3032 | |
M*, 1 | −0.4615 | 0.0149 | −0.0817 | |||
η | (29) | η | −0.4970 | −0.4052 | −0.3443 | |
ϵ1 = ϵ1, 0 + ϵ1, 1z | (34) | ϵ1, 0 | 0.4021 | 0.1236 | −0.1158 | |
ϵ1, 1 | 0.0435 | −0.0187 | 0.1408 | |||
Γ = Γ0 + zΓ1 | (35) | Γ0 | 1.2763 | 1.2956 | 1.2861 | |
Γ1 | −0.0554 | −0.0937 | −0.1382 | |||
M0 | (25) | log10(M0/h−1 M⊙) | 13.0978 | 13.4854 | 14.1254 |
Notes. In each case, the halo model is fitted to the three different AGN heating temperatures separately (107.6, 107.8 and 108.0 K). We interpolate between parameters as a function of TAGN to get a model for intermediate temperatures and that we think is robust to modest extrapolation.
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