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La distancia geométrica y el movimiento propio de la Galaxia Triángulo (M33)
Andreas Brunthaler1, Mark J Reid, Heino Falcke
1Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany. brunthaler@jive.nl
Science (New York, N.Y.)
|March 5, 2005
Resumen
Los astrónomos utilizaron el Very Long Baseline Array para medir la distancia y el movimiento de la Galaxia Triángulo (M33). Esto proporciona nuevos conocimientos sobre la dinámica del Grupo Local y las estimaciones de masa de las galaxias.
Área de la Ciencia:
- La astronomía y la astrofísica.
- Cosmología Cosmología.
- Dinámica Galáctica es la dinámica galáctica.
Sus antecedentes:
- La Galaxia del Triángulo (M33) es un componente clave del Grupo Local.
- Las mediciones precisas de distancia y movimiento son cruciales para comprender las interacciones galácticas y la masa.
Objetivo del estudio:
- Para medir con precisión la distancia a la Galaxia del Triángulo (M33) utilizando observaciones de máser.
- Para determinar el movimiento propio de M33 en relación con la Vía Láctea.
- Para refinar los modelos dinámicos del Grupo Local y estimar las masas de las galaxias.
Principales métodos:
- Utilizó el Very Long Baseline Array (VLBA) para observar máseres de H2O en M33.3.
- Rotación angular medida y movimiento propio de las fuentes de maser.
- Distancia calculada comparando la velocidad de rotación con la inclinación y la velocidad.
Principales resultados:
- Se determinó una distancia a M33 de 730 ± 168 kiloparsecs.
- Se midió la velocidad de M33 en relación con la Vía Láctea a 190 ± 59 km/s.
- Los resultados son consistentes con las recientes mediciones de distancia de las Cefeidas.
Conclusiones:
- La técnica de observación de maser empleada proporciona un método confiable para la determinación de la distancia extragaláctica.
- Estas mediciones ayudarán a desarrollar modelos dinámicos para el Grupo Local.
- Permite una mejor estimación de la masa y los halos de materia oscura para M31, M33 y la Vía Láctea.
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