@Article{Moura-SantosCarPenNovWue:2016:BaEsCM,
               author = "Moura-Santos, E. and Carvalho, Fabio Cabral and Penna-Lima, M. and 
                         Novaes, Camila Paiva and Wuensche, Carlos Alexandre",
          affiliation = "{Universidade de S{\~a}o Paulo (USP)} and {Universidade do Estado 
                         do Rio Grande do Norte (UERN)} and {Universit{\'e} Paris Diderot} 
                         and {Instituto Nacional de Pesquisas Espaciais (INPE)} and 
                         {Instituto Nacional de Pesquisas Espaciais (INPE)}",
                title = "A bayesian estimate of the CMB-large-scale structure 
                         cross-correlation",
              journal = "Astrophysical Journal",
                 year = "2016",
               volume = "826",
               number = "2",
                pages = "121",
                month = "Aug.",
             keywords = "cosmic background radiation, cosmology: observations, large-scale 
                         structure of universe, methods: data analysis, methods: 
                         statistical.",
             abstract = "Evidences for late-time acceleration of the universe are provided 
                         by multiple probes, such as Type Ia supernovae, the cosmic 
                         microwave background (CMB), and large-scale structure (LSS). In 
                         this work, we focus on the integrated Sachs-Wolfe (ISW) effect, 
                         i.e., secondary CMB fluctuations generated by evolving 
                         gravitational potentials due to the transition between, e.g., the 
                         matter and dark energy (DE) dominated phases. Therefore, assuming 
                         a flat universe, DE properties can be inferred from ISW 
                         detections. We present a Bayesian approach to compute the CMB-LSS 
                         cross-correlation signal. The method is based on the estimate of 
                         the likelihood for measuring a combined set consisting of a CMB 
                         temperature and galaxy contrast maps, provided that we have some 
                         information on the statistical properties of the fluctuations 
                         affecting these maps. The likelihood is estimated by a sampling 
                         algorithm, therefore avoiding the computationally demanding 
                         techniques of direct evaluation in either pixel or harmonic space. 
                         As local tracers of the matter distribution at large scales, we 
                         used the Two Micron All Sky Survey galaxy catalog and, for the CMB 
                         temperature fluctuations, the ninth-year data release of the 
                         Wilkinson Microwave Anisotropy Probe (WMAP9). The results show a 
                         dominance of cosmic variance over the weak recovered signal, due 
                         mainly to the shallowness of the catalog used, with systematics 
                         associated with the sampling algorithm playing a secondary role as 
                         sources of uncertainty. When combined with other complementary 
                         probes, the method presented in this paper is expected to be a 
                         useful tool to late-time acceleration studies in cosmology.",
                  doi = "10.3847/0004-637X/826/2/121",
                  url = "http://dx.doi.org/10.3847/0004-637X/826/2/121",
                 issn = "0004-637X and 1538-4357",
             language = "en",
        urlaccessdate = "27 abr. 2024"
}