Diego Saez-Gomez

H(z = 0) = H 0 = 100 hkms −1 Mpc −1 ,h=0.71 ± 0.03 (5)
H (z) = κ2
2
Scalar-tensor representation of
ρ m
f(r) gravity
H 0 (1 + z)h(z) , → H (0) = κ2
ρ 0 m = 3 2H 0 2 Ω0 m . (6)
H (0) 0 (7)
Hu-Sawicki model
Ω m (z) , Cosmological Ω f(R) (z) evolution in viable modified(8)
gravity
Phase space
1.0
V + (φ) V − (φ) (9)
0.9
1.6
1.4
0.8
1.2
H 2 H 0
2
0.7
0.6
H 2 H 0
2
1.0
0.8
0.5
0.6
0.4
0.4
0.3
0.90 0.92 0.94 0.96 0.98 1.00
Φ
(a)
This branch of the potential makes the scalar field to tend to the boundary, where a
sudden singularity occurs.
2.0 2.2 2.4 2.6
Figure 9: Phase space H(φ) for the HS model (panel 9a), where different init
considered. The right panel corresponds to the NO model. For both models, the po
been assumed. As observed, all the curves in both models reach DSG, Class.Quant.Grav. the bounding 30 095008 (2013) of the sc
(b)
Φ