Testing the Standard Model of Cosmology Using BAO data - KIAS

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Future SNAP data wz () = w+ w 0 1 z 1+ z erroneous Ω 0m = 0.22 true Ω 0m = 0.27 P-value = 26% erroneous Ω 0m = 0.32 Sahni, Shafieloo & Starobinsky, PRD 2008 Clarkson, Cortes & Bassett JCAP 2007 Shafieloo & Clarkson PRD 2010
Late Universe and Dark Energy Models • Lambda-CDM: The most favorite model • Brane Models • Quintessence and Quiessence Models • Phantoms, Ghosts, demons • Modified Gravity • etc... 2 H ( z) ⎡⎡ 3 dz = ⎢⎢Ω (1 + ) + Ω exp[ ∫ 0 3 1 ] 2 M z DE H ⎣⎣ 1+ z 0 ( ) ⎤⎤ + w( z) ⎥⎥ ⎦⎦
Page 1 and 2: Testing the Standard Model of Cosmo
Page 3 and 4: Standard Model of Cosmology Vanilla
Page 5 and 6: Beyond the Standard Model of Cosmol
Page 7 and 8: Parameter estimation within a cosmo
Page 9: Dark Energy Reconstruction • Any
Page 13 and 14: Y. Gong, JCAP (2005)
Page 15 and 16: wz () =−0.7 wz ( ) =−1.3 2 2 3
Page 17 and 18: To find cosmological quantities and
Page 19 and 20: Method of Smoothing A. Shafieloo, U
Page 21 and 22: h(z) Uncorrelated estimation of the
Page 23 and 24: Model Independent Reconstruction of
Page 25 and 26: Deriving h(z) from BAO Observable E
Page 27 and 28: Deriving h(z) from BAO
Page 29 and 30: Deriving h(z) from BAO Om diagnosti
Page 31 and 32: Alcock-Paczynski Measurement • An
Page 33 and 34: Combining the information from supe
Page 35 and 36: (Present)t Standard Model of Cosmol
Page 37 and 38: Conclusion • BAO links the early

Testing the Standard Model of Cosmology Using BAO data - KIAS

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