Testing the Standard Model of Cosmology Using BAO data - KIAS

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Om diagnostic Om() z h 2 () z −1 = + z 3 − (1 ) 1 V. Sahni, A. Shafieloo, A. Starobinsky, PRD 2008 arXive:0807.3548 Also look at: C. Zunckel & C. Clarkson, PRL 2008 arXive:0807.4304 Om(z) is constant only for FLAT LCDM model w w w =−1 → Om( z) =Ω Ω 0m 0m om LCDM Phantom Quintessence We Only Need h(z)
To find cosmological quantities and parameters there are two general approaches: 1. Parametric methods Easy to confront with cosmological observations to put constrains on the parameters, but the results are highly biased by the assumed models and parametric forms. 2. Non Parametric methods . Difficult to apply on the raw data, but the results will less biased and more reliable and independent of theoretical models or parametric forms.
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 and 10: Dark Energy Reconstruction • Any
Page 11 and 12: Late Universe and Dark Energy Model
Page 13 and 14: Y. Gong, JCAP (2005)
Page 15: wz () =−0.7 wz ( ) =−1.3 2 2 3
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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