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Determinación de la abundancia primordial de helio mediante el análisis espectral de galaxias HII.
Vital Fernández
Elena Terlevich
Ángeles Díaz Beltrán
Acceso Abierto
Atribución-NoComercial-SinDerivadas
Cosmology
Primordial
Abundances
The primordial helium abundance Ⲩ🇵 is calculated using sulfur as metallicity tracer in the classical methodology (with Ⲩ🇵 as an extrapolation of Ⲩ to zero metals). The calculated value, Ⲩ🇵,🇸 = 0.244±0.006, is in good agreement with the estimate from the Planck experiment, as well as, determinations in the literature using oxygen as the metallicity tracer. These results were derived from long-slit observations of low metallicity HII galaxies with the two arm spectrograph ISIS in the William Herschel telescope. The chemical analysis includes the subtraction of the nebular continuum and the stellar continuum. The latter was computed from simple stellar population synthesis grids. The S⁺² content is measured from the near infrared [SI I I] λλ9069Å, 9532Å lines, while an ICF (S³⁺) is proposed based on the Ar³⁺/Ar²⁺ fraction. Additionally, a multivariable linear regression using simultaneously oxygen, nitrogen and sulfur abundances was applied for the first time to determine the primordial helium abundance resulting in Ⲩ🇵₋🇴͵🇳͵🇸 = 0.245± 0.007. Finally a Bayesian spectral synthesizer was developed to fit the nebular, stellar en emission line components. The results obtained with this new technique are in agreement with those derived from the classical methodology and the direct method.
Instituto Nacional de Astrofísica, Óptica y Electrónica
2018-09
Tesis de doctorado
Inglés
Estudiantes
Investigadores
Público en general
Gutiérrez Fernández, V., (2018), Determinación de la abundancia primordial de helio mediante el análisis espectral de galaxias HII, Tesis de Doctorado, Instituto Nacional de Astrofísica, Óptica y Electrónica
ASTRONOMÍA Y ASTROFÍSICA
Versión aceptada
acceptedVersion - Versión aceptada
Aparece en las colecciones: Doctorado en Astrofísica

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