O mistério do Local Cosmic Void
DOI:
https://doi.org/10.47456/Cad.Astro.v5nEspecial.44878Palavras-chave:
Cosmologia, modelo padrão, local voidResumo
O Modelo ΛCDM-plano (Λ é a constante cosmológica e CDM, cold dark matter) é o que melhor se ajusta aos dados observacionais atualmente. Ele se fundamenta no Princípio Cosmológico, que assume a homogeneidade e a isotropia estatísticas do universo em larga escala. Estudando as propriedades desta última no Universo Local (UL) por meio do catálogo ALFALFA (Arecibo Legacy Fast ALFA Survey) – um levantamento que cobre ∼ 7000 deg2 do céu e conta com 31502 fontes extragalácticas de HI, distribuídas no intervalo 0 < z < 0.06 e divididas entre os hemisférios Norte e Sul Galácticos – encontramos resultados que indicam a existência de uma região contendo poucas galáxias, e que foi descrita pela primeira vez por Tully & Fischer (1987), ficando conhecida como Local Cosmic Void. Nossas análises são independentes de modelo e usam a função de correlação angular de dois pontos (2PACF) como aferidor estatístico, além de simulações do tipo lognormal (que consideram os parâmetros cosmológicos) para a estimativa das incertezas dos resultados. Para entender as propriedades e a morfologia da estrutura encontrada, fizemos testes com voids simulados, além de investigações comparativas com as descrições de voids do UL disponíveis na literatura. Nossos resultados indicam que o LCV possui contraste de densidade numérica δ ≃ −0.3, correspondente a uma subdensidade de ∼ 150 Mpc de comprimento e ∼ 60 Mpc de largura, características que concordam com a literatura.
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