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Revista mexicana de astronomía y astrofísica
Print version ISSN 0185-1101
Rev. mex. astron. astrofis vol.41 n.2 Ciudad de México Oct. 2005
A new determination of the rotation curve from galactic disk planetary nebulae
W. J. Maciel and L. G. Lago
Departamento de Astronomia, IAG/USP, Rua do Matao 1226, Cidade Universitaria, CEP 05508-900, Sao Paulo SP, Brazil (maciel@astro.iag.usp.br, leonardo@astro.iag.usp.br).
Received, 2005 February 18
Accepted 2005 April 1
RESUMEN
La curva galáctica de rotación se determina en base a una gran muestra de nebulosas planetarias con velocidades radiales conocidas. Se adoptan cuatro escalas de distancia y se establece la curva para distancias galactocéntricas entre 4 a 14 kpc, aproximadamente, adoptando R0 = 8.5 kpc para la distancia galactocéntrica de SLR. Las conclusiones principales son: (i) no existe indicación de que haya una disminución de la curva de rotación medida más allá del círculo solar; (ii) no hay diferencias importantes entre las escalas estadísticas de distancia consideradas, ya sean "cortas" o "largas", si bien las nebulosas individuales pueden tener muy diferentes distancias de acuerdo a las diferentes escalas, y (iii) las curvas derivadas son similares a la curva de rotación obtenida de las regiones H II, tomando en cuenta el hecho que las nebulosas planetarias son generalmente objetos más viejos y tienen componentes de velocidad perpendiculares al plano galáctico mayores.
ABSTRACT
The galactic rotation curve is determined on the basis of a large sample of planetary nebulae with known radial velocities. Four distance scales are adopted and the curve is established for galactocentric distances of 4 to 14 kpc, approximately, adopting R0 = 8.5 kpc for the galactocentric distance of the LSR. The main conclusions are: (i) there is no indication of a measurable decrease of the rotation curve beyond the solar circle; (ii) there are no important differences among the statistical distance scales considered, irrespective of the "short" or "long" nature of the scale, even though individual nebulae can have very different distances according to the different scales, and (iii) the derived curves are similar to the rotation curve derived from H II regions, taking into account the fact that PN are generally older objects and have larger velocity components perpendicular to the galactic plane.
Key Words: Galaxy: Kinematics and dynamics Planetary nebulae.
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