Echelle spectroscopy of the nuclei of the highly collimated bipolar planetary nebulae M 2–9 and M 1–91¹

 

S. Torres–Peimbert,² A. Arrieta,³ and M. Bautista⁴

 

² Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 70–264, México, D. F. 04510, México (silvia@astroscu.unam.mx).

³ Universidad Iberoamericana, Depto. de Física y Matemáticas, Prol. Paseo de la Reforma 880, Lomas de Santa Fe, México D. F. 01219, México (anabel.arrieta@uia.mx).

⁴ Department of Physics, Western Michigan University, Kalamazoo, MI 49008, USA.

 

Received 2010 January 21
Accepted 2010 May 20

 

RESUMEN

Presentamos espectroscopia echelle del núcleo sin resolver de las nebulosas bipolares M 2–9 and M 1–91. Los espectros están dominados por líneas de emisión emitidas en un amplio intervalo de condiciones físicas. De las observaciones identificamos las líneas de emisión, las condiciones físicas y los movimientos relativos de las diferentes especies ionizadas en la región circunestelar de ambos objetos. Proponemos que las líneas prohibidas observadas se originan en la parte interior del toro extendido que rodea a cada objeto.

 

ABSTRACT

We present echelle spectroscopy of the unresolved nuclei of the bipolar plane–tary nebulae M 2–9 and M 1–91. The spectrum is dominated by emission lines emitted under a wide range of physical conditions. From the observations we identify the emission lines, derive physical conditions and relative motions of the different ionized species in the circumstellar region of both objects. We propose that the observed forbidden lines arise in the inner part of the extended torus that surrounds each object.

Key Words: planetary nebulae: individual (M 2–9, M 1–91).

 

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ACKNOWLEDGMENTS

ST–P and AA have received support from DGAPA–IN112708, Conacyt–60967 and Conacyt–46904 grants. We are grateful for the comments from the referee and many fruitful discussions with L. N. Georgiev.

Note added in proof: R. Corradi (private communication) kindly informed us that the distance of 650 pc assigned to M 2–9 (Schwarz et al. 1997) is not correct, and that it should be 1.3 kpc. This value, if confirmed, would modify our size and time estimates by a factor of 2.

 

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NOTE

¹ Based on observations obtained at the Observatorio Astronómico Nacional at San Pedro Mártir, Baja California, México.