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Potential-‐driven slow-‐roll inflation Planck 2013 results. XXIII. Isotropy and Statistics of <strong>the</strong> CMB : arXiv:1303.5083
S.T., J. Ohashi, S. Kuroyanagi, A De Felice, arXiv: 1305.3044 Potential−driven slow−roll inflation 10 0 Inclusion of high L data prefers Planck+WP+BAO+high L <strong>the</strong> smaller spectral index. Planck+WP+BAO 4 power law inflation 10 −1 2 1 r 0.05 natural 2/3 10 −2 large−field small−field R 2 inflation 10 −3 very small field hybrid2 hybrid1 0.94 0.95 0.96 0.97 0.98 0.99 1 1.01 n s
Page 1 and 2: S. Tsujikawa, J. Ohashi, S.Kuro
Page 3 and 4: Old inflation (Sato, Kazanas, G
Page 5 and 6: Standard slow-‐roll inflation
Page 7 and 8: S = ⇤ d 4 x ⇥ g ⇥ R 16 G + X
Page 9: Discrimination between inflaton
Page 13 and 14: Horndeski’s paper in 1973
Page 15 and 16: Power spectrum of curvature per
Page 17 and 18: We can apply our general resul
Page 19 and 20: Planck constraints on Brans-Dicke g
Page 21 and 22: Higgs inflation There are severa
Page 23 and 24: Running kinetic couplings 0.3 0.25
Page 25 and 26: f NL B R f NL ・・・nonlinear e
Page 27 and 28: Observational constraints on power-
Page 29: Potentials favored from observat

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