Galactic kinematics of planetary nebulae with [WC] central star1
Miriam Peña,2 Jackeline S. Rechy–García,2 and Jorge García–Rojas3,4
2 Instituto de Astronomía, Universidad Nacional Autónoma de México. Apdo. Postal 70–264, México D.F., 04510, México. (miriam@astro.unam.mx, jrechy@astro.unam.mx).
3 Instituto de Astrofísica de Canarias, Vía Láctea s/n, E–38200, La Laguna, Tenerife, Spain.
4 Departamento de Astrofísica, Universidad de la Laguna, E–38205, La Laguna, Tenerife, Spain. (jogarcia@iac.es).
]]> Received 2012 October 18.
RESUMEN
Usando espectros de alta resolución, analizamos la distribución y cinemática galáctica de nebulosas planetarias con estrella central [WR] y 'wels' ([WR]PN y WLPN). Se calcularon las velocidades circulares y peculiares (Vpec) de los objetos, y obtuvimos que: (a) Las [WR]PNe pertenecen al disco galáctico y están más concentradas que las WLPNe y PN normales, lo que corresponde a objetos más jóvenes, (b) Clasificamos la muestra en Tipos de Peimbert y encontramos que las PNe de Tipo I tienen Vpec < 50 km s–1, como corresponde a objetos jóvenes; la mayoría de las [WR]PN son del Tipo II con Vpec < 60 km s–1, aunque un porcentaje de la muestra es del Tipo III con Vpec más alta, lo que indica que el fenómeno Wolf–Rayet en estrellas centrales puede ocurrir con cualquier masa estelar y en objetos viejos. Ninguna WLPN de la muestra es Tipo I. Así, [WR]PNe y WLPNe no están relacionados.
ABSTRACT
High resolution spectra are used to analyze the galactic kinematics and distribution of a sample of planetary nebulae with [WR] and 'wel' central star ([WR]PN and WLPN). The circular and peculiar velocities, (Vpec), of the objects were derived. The results are: (a) [WR]PNe are distributed mainly in the galactic disk and they are more concentrated in a thinner disk than WLPNe and normal PNe, which corresponds to a younger population, (b) The sample was separated in Peimbert's types, and it is found that Type I PNe have Vpec < 50 km s–1, indicating young objects. Most of the [WR]PNe are of Type II showing Vpec < 60 km s–1, although a small percentage is of Type III with larger Vpec. This shows that the Wolf–Rayet phenomenon in central stars can occur at any stellar mass and in old objects. None of our WLPNe is of Type I. Thus, [WR]PNe and WLPNe are unrelated objects.
Key Words: planetary nebulae: general — stars: kinematics and dynamics — stars: Wolf–Rayet.
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ACKNOWLEDGMENTS
J.S.R.–G. acknowledges scholarship from Conacyt–Mexico. J.G.–R. received financial support from the Spanish Ministerio de Educación y Ciencia (MEC), under project AYA2007–63030. This work received financial support from DGAPA–Universidad Nacional Autónoma de México (PAPIIT project IN105511).
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]]> 1 Based on observations collected at the Observatorio Astronómico Nacional, SPM, B. C, Mexico. Based on data obtained at Las Campanas Observatory, Carnegie Institution, Chile. ]]>