Modelo da galáxia utilizando contagens de estrelas no infravermelho / Galaxy model by using infrared star counts

AUTOR(ES)
FONTE

IBICT - Instituto Brasileiro de Informação em Ciência e Tecnologia

DATA DE PUBLICAÇÃO

29/02/2008

RESUMO

The majority of first quantitative models for the structure of Galaxy used the star counts method to explore the most important galactic structure parameters as a whole. Some of the most important models owe to Bahcall \& Soneira (1980), the Besançon group (Robin \& Crezé (1986)), Wainscoat et al. (1992), Ortiz \& Lépine (1993), among others. The datum used suffered, however, photometric coverage completeness and spatial coverage completeness. Same the IRAS survey, realized in 1980 s scanning entire sky in wavelenghts between 12 and 100 $ {\mu}$m, suffer of weak sources completeness problems due to moderate sensitivity and low spatial resolution. The beginning of large area detectors in near infrared, in 1990 s, carried to realization of large scale surveys like 2MASS and DENIS. These surveys filled magnitude zones between 4 and 14 on J, H, K$ _{S}$ and I bands with complete spatial coverage and adequate photometric quality. The GLIMPSE survey realized by Spitzer telescope between 3.8 and 8 $ {\mu} $m explored galactic plane region with arcsecond order spatial resolution. These surveys were consolidated in public acess databases which can be asked by simple way, producing adequate format answers to compare with galactic structure models. Taking as point of beginning the Ortiz \& Lépine star counts model, elaborated on pre epoch of 2MASS, we realized comparations between previsions and modern measures that are summarized in this work. We described the systematics of samples grades production in the sky, the source counts histograms constructions in bands J, H and K$ _{S}$ , the model premisses, its functioning and bigger priorities in term of advance to the model. We summarized alike the route to be used for an exploration of outstanding parameters with an adequate sample algorithm for large data numbers and large parameter numbers.

ASSUNTO(S)

galáxia estrutura espiral contagens de estrelas infravermelho via láctea galaxy spiral structure infrared milky way

ACESSO AO ARTIGO

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