M. G. Richer,2 J. A. López,2 E. Díaz–Méndez,3 H. Riesgo,2 S.–H. Báez,4 Ma.–T. García–Díaz,2 J. Meaburn,5 D. M. Clark,2 R. M. Calderón Olvera,6 G. López Soto,6 and O. Toledano Rebolo7
2 Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 877, 22830, Ensenada, B. C., México (tere@astrosmo.unam.mx, jal@astrosmo.unam.mx, richer@astrosmo.unam.mx, hriesgo@astrosmo.unam.mx).
3 Dept. of Physics and Astronomy, Texas Christian University, Fort Worth, Texas, US. 76109 (e.d.mendez@tcu.edu).
4 Facultad de Física e Inteligencia Artificial, Universidad Veracruzana, Circuito G. Aguirre Beltrán s/n, Zona Universitaria, Xalapa, Veracruz, México (solharet@hotmail.com).
5 Jodrell Bank Observatory, Dept. of Physics & Astronomy, University of Manchester, Macclesfield, Cheshire SK11 9DL, UK (jm@ast.man.ac.uk).
6 Universidad Nacional Autóma de México, Ciudad Universitaria, 04510 México, D.F., México (roxanama@msn.com, blackholemx@yahoo.com.mx).
7 Instituto de Ciencias Físicas, Universidad Nacional Autónoma de México, Av.Universidad s/n, 62210, Cuernavaca, Morelos, México (oswaldotoledano@hotmail.com).
]]>Received 2009 October 14
Accepted 2010 April 17
RESUMEN
Presentamos datos cinemáticos para 211 nebulosas planetarias brillantes en once galaxias del Grupo Local: M31 (137 NPs), M32 (13), M33 (33), Fornax (1), Sagittarius (3), NGC 147 (2), NGC 185 (5), NGC 205 (9), NGC 6822 (6), Leo A (1), y Sextans A (1). Adquirimos los datos en el Observatorio Astronómico Nacional en la Sierra de San Pedro Mártir con el telescopio de 2.1 m y el espectrómetro Manchester Echelle en la línea de [O III]λ5007 con una resolución de 11 kms–1. Observamos algunos objetos en Hα. La cinemática de nebulosas planetarias brillantes no depende fuertemente de la metalicidad o la edad de la población estelar progenitora en sus galaxias huéspedes, aunque existen pequeñas diferencias sistemáticas. La cinemática y la luminosidad en Hβ de las cáscaras nebulares requieren la aceleración de las cascaras durante la evolución temprana de las estrellas centrales. Así, la cinemática representa otro argumento a favor de estrellas progenitoras similares para las nebulosas planetarias brillantes en todas galaxias.
ABSTRACT
We present kinematic data for 211 bright planetary nebulae in eleven Local Group galaxies: M31 (137 PNe), M32 (13), M33 (33), Fornax (1), Sagittarius (3), NGC 147 (2), NGC 185 (5), NGC 205 (9), NGC 6822 (5), Leo A (1), and Sextans A (1). The data were acquired at the Observatorio Astronómico Nacional in the Sierra de San Pedro Mártir using the 2.1 m telescope and the Manchester Echelle Spectrometer in the light of [O III]λ5007 at a resolution of 11 kms–1. A few objects were observed in Hα. The internal kinematics of bright planetary nebulae do not depend strongly upon the metallicity or age of their progenitor stellar populations, though small systematic differences exist. The nebular kinematics and Hβ luminosity require that the nebular shells be accelerated during the early evolution of their central stars. Thus, kinematics provides an additional argument favoring similar stellar progenitors for bright planetary nebulae in all galaxies.
Key Words: ISM: kinematics and dynamics — Local Group — planetary nebulae: general — stars: evolution.
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ACKNOWLEDGMENTS
We thank the telescope operators during our runs, Gabriel García, Gustavo Melgoza, Salvador Monrroy, and Felipe Montalvo, for their help. We thank M. Arnaboldi for kindly providing the line widths for the planetary nebulae in the Virgo Cluster that are shown in Figure 8. We thank the referee for helpful comments and suggestions. We gratefully acknowledge financial support throughout this project from Conacyt grants 37214, 43121, 49447, and 82066 and from DGAPA–Universidad Nacional Autónoma de México grants 108406-2, 108506–2, 112103, and 116908–3. We acknowledge the use of NASA's SkyView facility (http://skyview.gsfc.nasa.gov) located at NASA Goddard Space Flight Center in generating Figure 9.
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