Spatially resolve chemodynamics of Green Pea galaxies
Green Pea (GP) galaxies are the best local analogues of young high-redshift galaxies and ideal laboratories to study galaxy formation, reionization and feedback under extreme physical conditions. Complex emission line profiles for 6 GPs were observed using high-resolution spectroscopy at the WHT sho...
Guardado en:
| Autores principales: | , , , , , , , , , , |
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| Formato: | Objeto de conferencia |
| Lenguaje: | Español |
| Publicado: |
2019
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| Materias: | |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/167504 |
| Aporte de: |
| Sumario: | Green Pea (GP) galaxies are the best local analogues of young high-redshift galaxies and ideal laboratories to study galaxy formation, reionization and feedback under extreme physical conditions. Complex emission line profiles for 6 GPs were observed using high-resolution spectroscopy at the WHT showing a very broad line underlying more than one narrower component. The broad components indicate large expansion velocities (full width zero intensity ~1000km/s) probably showing the imprint of energetic outflows from supernovae. Using GMOS-IFU Gemini observations of a GP, we deconvolve the Hα, HeI5676Å, [OI]6300Å, [NII]6548, 6584Å, and [SII]6717, 6731Å emission-line profiles, as well as the temperature sensitive auroral emission line [OII]7325Å. This allow us to study the origin of the different emission line components and estimate the electron densities and the presence of shocks. This work present a new methodology for analyzing IFU observations of emission line spectra, considering the presence of multiple components, and preliminary physical conditions results. |
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