%0 Generic %1 Blanchard2005 %A Blanchard, Alain %A Douspis, Marian %A Rowan-Robinson, Michael %A Sarkar, Subir %D 2005 %K Large-Scale Model Void %T Large-scale galaxy correlations as a test for dark energy %U http://arxiv.org/abs/astro-ph/0512085 %X We have shown earlier that, contrary to popular belief, Einstein--de Sitter (E--deS) models can still fit the WMAP data on the cosmic microwave background provided one adopts a low Hubble constant and relaxes the usual assumption that the primordial density perturbation is scale-free. The recent SDSS measurement of the large-scale correlation function of luminous red galaxies at $z 0.35$ has however provided a new constraint by detecting a `baryon acoustic peak'. Our best-fit E--deS models do possess a baryonic feature at a similar physical scale as the best-fit $Łambda$CDM concordance model, but do not fit the new observations as well as the latter. In particular the shape of the correlation function in the range $10-100 h^-1$ Mpc cannot be reproduced properly without violating the CMB angular power spectrum in the multipole range $l 100-1000$. Thus, the combination of the CMB fluctuations and the shape of the correlation function up to $100 h^-1$Mpc, if confirmed, does seem to require dark energy for a homogeneous cosmological model based on (adiabatic) inflationary perturbations.

@misc{Blanchard2005, abstract = { We have shown earlier that, contrary to popular belief, Einstein--de Sitter (E--deS) models can still fit the {\sl WMAP} data on the cosmic microwave background provided one adopts a low Hubble constant and relaxes the usual assumption that the primordial density perturbation is scale-free. The recent {\sl SDSS} measurement of the large-scale correlation function of luminous red galaxies at $z \sim 0.35$ has however provided a new constraint by detecting a `baryon acoustic peak'. Our best-fit E--deS models do possess a baryonic feature at a similar physical scale as the best-fit $\Lambda$CDM concordance model, but do not fit the new observations as well as the latter. In particular the shape of the correlation function in the range $\sim 10-100 h^{-1}$ Mpc cannot be reproduced properly without violating the CMB angular power spectrum in the multipole range $l \sim 100-1000$. Thus, the combination of the CMB fluctuations and the shape of the correlation function up to $\sim 100 h^{-1}$Mpc, if confirmed, does seem to require dark energy for a homogeneous cosmological model based on (adiabatic) inflationary perturbations. }, added-at = {2011-05-27T17:39:33.000+0200}, author = {Blanchard, Alain and Douspis, Marian and Rowan-Robinson, Michael and Sarkar, Subir}, biburl = {https://www.bibsonomy.org/bibtex/2e247019854638f5c85a0a8d59425c09b/ad4}, description = {Large-scale galaxy correlations as a test for dark energy}, interhash = {5bb4deda093099d4c3a28f563baf912d}, intrahash = {e247019854638f5c85a0a8d59425c09b}, keywords = {Large-Scale Model Void}, note = {cite arxiv:astro-ph/0512085 Comment: 4 pages, 2 figures, revised version, accepted to A&A}, timestamp = {2011-05-27T17:39:33.000+0200}, title = {Large-scale galaxy correlations as a test for dark energy}, url = {http://arxiv.org/abs/astro-ph/0512085}, year = 2005 }