R. E. Garlos Reyes,1,2 F. A. R. Navarro,1 J. Meléndez,3 J. Steiner,3 and F. Elizalde4
1 Universidad Nacional Mayor de San Marcos, UNMSM, Facultad de Ciencias Físicas, Calle Germán Amézaga N° 375, Lima 1, Perú (raedcare@hotmail.com).
2 Universidad Nacional del Callao, UNAC, Callao, Perú.
3 Universidade de São Paulo, IAG/USP, São Paulo, Brazil.
4 Instituto Nacional de Pesquisas Espaciais, Divisão de Astrofísica - DAS/INPE, São Paulo, Brazil.
]]> Received December 23 2014.
RESUMEN
Usamos datos en la región ultravioleta, visible e infrarroja de 11 regiones HII en las Nubes de Magallanes, a fin de determinar sus parámetros físicos y abundancias químicas. Así, hacemos un modelo de fotoionización de seis regiones HII en la Gran Nube de Magallanes (GNM) y cinco regiones HII en la Pequeña Nube de Magallanes (PNM), lo cual nos permite calcular las abundancias de He, G, N, O, Ne, S y Ar. Los valores calculados se comparan con los encontrados en la literatura para regiones HII, nebulosas planetarias y estrellas. Obtuvimos los valores de las abundancias ajustando modelos del código CLOUDY para las intensidades de línea observadas. Además, las observaciones en el Observatorio Pico dos Dias de [S II] λ6717/λ6731 para regiones HII en la PNM nos permiten determinar la densidad electrónica. Los datos IUE de las líneas [C III] λ1909 se usan para determinar la abundancia de C de seis y cinco regiones HII en la GNM y en la PNM, respectivamente.
ABSTRACT
We used ultraviolet, optical and infrared data of eleven HII regions in the Magellanic Clouds in order to determine their physical parameters and chemical abundances. The photoionization modeling of six HII regions in the LMC and five HII regions in the SMC, allowed us to derive the abundances of He, C, N, O, Ne, S and Ar, which were compared with those obtained in the literature for HII regions, PN, and stars. The abundances were obtained by adjusting models of the CLOUDY code to the observed line intensities. The observations obtained at the Observatório Pico dos Dias of [S II] λ6717/λ6731 line ratios for HII regions in the SMC allowed the determination of the electron density with a high precision. Furthermore, the IUE data on [C III] λ1909 lines were used to determine the abundance of carbon of six and five HII regions in the LMC and SMC, respectively.
Key Words: HII regions — Magellanic Clouds — methods: data analysis.
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ACKNOWLEDGMENT
Rafael E. Carlos Reyes thanks the Brazilian entity CNPq (The National Council for Scientific and Technological Development) for its support through contract 381314/97-9. Likewise, F. Elizalde thanks INPE, where he was working during the development of the present research; he would like to clarify that he is not currently affiliated to INPE.
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