Diego Saez-Gomez
Diego Saez-Gomez Diego Saez-Gomez
n at redshift z = 1000 where δ is assumed to behave as in a matter k-dependence. In Fig. 1 we have plotted the evolution of the density he strong k-dependence of equation (40) renders the evolution of these ity contrast evolution provided by the Concordance ΛCDM model and 100. F(R,T) gravity Evolution of the matter perturbations in the quasi-static limit f B (R 0 ,T 0 )=R 0 + α T 1/2 0 − 2β α < 0 nd in (19), which also satisfies the usual continuity equation in the s supplemented with a cosmological constant −2β. The first FLRW 10 1 Ω 0 ma −1 − c 1 Ω 0 ma 1/2 + c 2 a 2 , (49) order to provide the correct dimensions 10 0 to the free constants parameters (witha(z = 0) = 1), one gets the constraint, Log[δ k ] Ω 0 m + c 2 → c 2 =1− Ω 0 m(1 − c 1 ) . (50) 10 -1 k=50 H 0 k=100 H 0 k=200 H 0 k=500 H 0 k=1000 H 0 ΛCDM 10 2 0 0.5 1 1.5 2 2.5 3 imensionless parameters {c 1 ,c 2 }, where one remains arbitrary. As for in the equation (37) leads to an evolution of the matter perturbations only a very restricted limit for 10 -2 the free parameter c 1 can avoid such 10 -3 Log[1+z] igure 2: δ k evolution for f B (R, T )modelaccordingtothequasi-staticevolutiongivenby(37)andΛCDM given by (39). Here we ave assumed a value c 1 = −10 −3 .Aspreviously,thedependenceonk leads to a strong growth of the matter perturbations for large values of k, whereasthebehaviorissimilartotheΛCDM model for the modes k
en at redshift z = 1000 where δ is assumed to behave as in a matter F(R,T) gravity ok-dependence. In Fig. 1 we have plotted the evolution of the density the strong k-dependence of equation (40) renders the evolution of these sity contrast evolution provided by the Concordance ΛCDM model and ≈ 100. Evolution of the matter perturbations in the quasi-static limit f B (R 0 ,T 0 )=R 0 + α T 1/2 0 − 2β 1 α > 0 und in (19), which also satisfies 0.9 the usual continuity equation in the is supplemented with a cosmological constant −2β. The first FLRW 0.8 = Ω 0 ma −1 − c 1 Ω 0 ma 1/2 + c 2 a 2 0.7 , (49) 0.6 order to provide the correct dimensions to the free constants parameters (witha(z = 0) = 1), one gets0.5 the constraint, δ k 1Ω 0 m + c 2 → c 2 =1− Ω 0 0.4 m(1 − c 1 ) . (50) 0.3 dimensionless parameters {c 1 ,c 2 }, where one remains arbitrary. As for k in the equation (37) leads to0.2 an evolution of the matter perturbations , only a very restricted limit for the free parameter c 1 can avoid such 0.1 k=50 H 0 k=100 H 0 k=200 H 0 k=500 H 0 k=1000 H 0 ΛCDM 1 0 -0.1 0 0.5 1 1.5 2 2.5 3 Log[1+z] igure 3: δ k evolution for f B (R, T )modelaccordingtothequasi-staticevolutiongivenby(37)andΛCDM given by (39). Here we have assumed a positive value for the free parameter c 1 =10 −3 ,whichleadstoanoscillatingbehaviorofthematterperturbations, which turns out stronger as k is larger, and whose oscillations are observed for large small redshifts. The model mimics the ΛCDM F. Alvarenga, A. Cruz-Dombriz, S. Houndjo, M. Rodrigues, DSG, to appear in PRD, ArXiv:1302.1866 model only those modes small enough k
- Page 1 and 2: Cosmological constraints on modifie
- Page 3 and 4: Brief Article The Author April 6, 2
- Page 5 and 6: FLRW cosmologies 12 3 No Big Bang (
- Page 7 and 8: FLRW cosmologies Future singulariti
- Page 9 and 10: Viable f(r) gravity Viability condi
- Page 11 and 12: 3 Cosmological evolution in viable
- Page 13 and 14: Cosmological evolution in viable f(
- Page 15 and 16: Cosmological evolution in viable f(
- Page 17 and 18: 8 − 3H 2 − 2Ḣ = 1 κ 2 p m +
- Page 19 and 20: (z = 0) = H 0 = 100 hkms −1 Mpc
- Page 21 and 22: (z = 0) = H 0 = 100 hkms −1 Mpc
- Page 23 and 24: effective repulsive force 12h R ∼
- Page 25 and 26: Testing F(R) gravity with Sne Ia da
- Page 27 and 28: Testing F(R) gravity with Sne Ia da
- Page 29 and 30: ere right lethand us remind side (r
- Page 31: e previous section, we study two pa
en at redshift z = 1000 where δ is assumed to behave as in a matter<br />
F(R,T) gravity<br />
ok-dependence. In Fig. 1 we have plotted the evolution of the density<br />
the strong k-dependence of equation (40) renders the evolution of these<br />
sity contrast evolution provided by the Concordance ΛCDM model and<br />
≈ 100.<br />
Evolution of the matter perturbations in the quasi-static limit<br />
f B (R 0 ,T 0 )=R 0 + α T 1/2<br />
0 − 2β<br />
1<br />
α > 0<br />
und in (19), which also satisfies 0.9 the usual continuity equation in the<br />
is supplemented with a cosmological constant −2β. The first FLRW<br />
0.8<br />
= Ω 0 ma −1 − c 1 Ω 0 ma 1/2 + c 2 a 2 0.7<br />
, (49)<br />
0.6<br />
order to provide the correct dimensions to the free constants parameters<br />
(witha(z = 0) = 1), one gets0.5<br />
the constraint,<br />
δ k<br />
1Ω 0 m + c 2 → c 2 =1− Ω 0 0.4<br />
m(1 − c 1 ) . (50)<br />
0.3<br />
dimensionless parameters {c 1 ,c 2 }, where one remains arbitrary. As for<br />
k in the equation (37) leads to0.2<br />
an evolution of the matter perturbations<br />
, only a very restricted limit for the free parameter c 1 can avoid such<br />
0.1<br />
k=50 H 0<br />
k=100 H 0<br />
k=200 H 0<br />
k=500 H 0<br />
k=1000 H 0<br />
ΛCDM<br />
1<br />
0<br />
-0.1<br />
0 0.5 1 1.5 2 2.5 3<br />
Log[1+z]<br />
igure 3: δ k evolution for f B (R, T )modelaccordingtothequasi-staticevolutiongivenby(37)andΛCDM given by (39). Here we<br />
have assumed a positive value for the free parameter c 1 =10 −3 ,whichleadstoanoscillatingbehaviorofthematterperturbations,<br />
which turns out stronger as k is larger, and whose oscillations are observed for large small redshifts. The model mimics the ΛCDM<br />
F. Alvarenga, A. Cruz-Dombriz, S. Houndjo, M. Rodrigues, DSG, to appear in PRD, ArXiv:1302.1866<br />
model only those modes small enough k
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