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Lue / Physics Reports 423 (2006) 1 – 48 41 Late-time ISW would then seem to be a promising candidate for modified-gravity theories of the sort that anticipate cosmic acceleration, as we see that the potentials are altered by substantial corrections. Indeed, for a particular set of modified-gravity theories, this assertion is indeed the case [86]. However, for DGP gravity, there is an unfortunate catch. Recall in Section 7, we argued that when considering linear potentials satisfied Eqs. 2), our results generalized beyond just spherical perturbations.

3 in DGP gravity and in CDM. The right panel shows the ratio of the solutions once they are both expressed as a function of their linear density contrasts. Figure from Ref. [56]. the correction disappears (since DGP becomes Einstein at high-densities), so most of the difference between the two evolutions happens in the linear regime, which is encoded in the linear growth factor. 3. Observational consequences What are the implications of these results for testing DGP gravity using large-scale structure?

The vertical lines show the best-fit and 1 error bars from fitting DGP gravity to the supernova data from Ref. [31]. 8–2 . In order to compare this prediction of 8 to observations one must be careful since most determinations of 8 have built in the assumption of Einstein gravity or CDM models. 2 for higher-order moments, should provide a test of galaxy biasing independent of gravity being DGP or Einstein. 1. We can convert this value to 8 for dark matter at z = 0 as follows. 2. 9L∗ . 15(L/L∗ ), which is in very good agreement with SDSS (see Fig.

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