Tsujikawa, Phys. Rev. D 77, 023507 (2008)

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m à:mMMDistanceestimator::ApparentmagnitudeAbsolutemagnitude< SNLS data >Pure mattercosmologyΩ m =1.00Ω Λ =0.00zNo. 6Flat ΛcosmologyΩ m =0.26Ω Λ =0.741H 2 0ä Ω=aà m2(1 + z) 3 + Ω ΛôΩ m ñ 2 ú(t 0 )3H20ΛΩ Λ ñ 3H20: Density parameter for matter: Density parameter for ΛFrom [Astier et al. [The SNLSCollaboration], Astron. Astrophys.447, 31 (2006)]1+z = aa 0, za 0 =1: Red shift‘‘0’’ denotes quantitiesat the present time . t 0
7-year WMAP data on the current value of >K =0・ For the flat universe, constant w :Cf.Ω Λ =(68% CL)(68% CL)(95% CL)(FromwKΩ K ñ (a0 H 0 ) 2No. 7From [E. Komatsu et al. [WMAPCollaboration], Astrophys. J. Suppl.192, 18 (2011) [arXiv:1001.4538[astro-ph.CO]]].Hubble constant ( H 0 ) measurementBaryon acoustic oscillation (BAO): Special pattern in the large-scalecorrelation function of SloanDigital Sky Survey (SDSS)luminous red galaxies: Time delay distance: Density parameterfor the curvatureK =0 : Flat universe.)
Page 1: Equation of state for dark energyin
Page 4 and 5: (1) General relativistic approach
Page 9 and 10: Canonical scalar field >⎧S þ =
Page 11 and 12: ・In the flat FLRW background, gra
Page 13 and 14: Models of f(R) gravity (examples) >
Page 15 and 16: Data fitting of w(z) >zw(z)=w 0 + w
Page 17 and 18: w DEw DE = à 1< Cosmological evolu
Page 19 and 20: II. Future crossing of the phantom
Page 21 and 22: Future evolutions of 1+w DE as func
Page 23 and 24: III. Equation of state for dark ene
Page 25 and 26: Combined f(T) theory >No. 25u(> 0):
Page 27 and 28: A. Non-local gravity< Action >g =de
Page 29 and 30: ・In the flat FLRW space-time, we
Page 31 and 32: ・The finite-time future singulari
Page 33 and 34: ・We estimate the present valueof
Page 35 and 36: Future evolutions of H as functions
Page 37 and 38: ・・In the future ( ), the crossi
Page 39 and 40: Conditions for the viability of f(R
Page 41 and 42: We solve Equations (1) and (2) by i
Page 43 and 44: Equation of state for (the componen
Page 45 and 46: No. 32We consider only non-relativi
Page 47 and 48: Gravitational field equations in th
Page 49: ・By using and ,No. 39・We take a
Page 52 and 53: Future crossing of the phantom divi
Page 54 and 55: B. Relations between the model para
Page 56 and 57:
IV. Effective equation of state for
Page 58 and 59:
(2) Extension of gravitational theo
Page 60 and 61:
Conditions for the viability of f(R
Page 62 and 63:
(5) Existence of a matter-dominated
Page 64 and 65:
Conclusions of Sec. II >・We have
Page 66 and 67:
Conclusions of Sec. IV >No. 64・
Page 68 and 69:
・We assume the flat FLRW space-ti
Page 70 and 71:
No. 45p =0.001p =0.01p = à 0.1p =0
Page 72 and 73:
(b). Logarithmic f(T) theory >No. 4
Page 74 and 75:
The best-fit values >No. 42The mini
Page 76 and 77:
(4) Solar system constraintsf(R) gr
Page 78 and 79:
(4) Stability of the late-time de S
Page 80 and 81:
Data fitting of w(z) (3) >No. B-7Fr
Page 82 and 83:
Bekenstein-Hawking entropy on the a
Page 84 and 85:
Hu-Sawicki modelStarobinsky’s mod
Page 86 and 87:
(a). Exponential f(T) theory >No. 1
Page 88 and 89:
(c). Combined f(T) theory >No. 16
Page 90 and 91:
p : Constantú Mand P M : Energy de
Page 92 and 93:
IV. Effective equation of state for
Page 94 and 95:
・It is known that the finite-time
Page 96 and 97:
Other models >No. A-10・Appleby-Ba
Page 98 and 99:
w effNo. A-13< Cosmological evoluti
Page 100 and 101:
Cosmological evolutions of , and in
Page 102 and 103:
Initial conditions >Models of (i),
Page 104 and 105:
No. A-21・・ By examining the cos
Page 106 and 107:
No. A-23
Page 108 and 109:
Second law of thermodynamics >[KB a
Page 110 and 111:
Residuals for the best fit to a fla
Page 112 and 113:
5-year WMAP data on >・ For the fl
Page 114 and 115:
Appendix B
Page 116 and 117:
Recent work >No. B-3[Martinelli, Me
Page 118:
(5) Existence of a matter-dominated
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Tsujikawa, Phys. Rev. D 77, 023507 (2008)

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