J. Bohigas
Instituto de Astronomía, Universidad Nacional Autónoma de México, Km 103 Carretera Tijuana–Ensenada, 22860 Ensenada, Baja California, México (jbb@astrosen.unam.mx).
Received 2012 May 18.
Accepted 2012 July 30.
RESUMEN
]]> Espectroscopía óptica de toda la nebulosa planetaria M 1–9, revela pronunciadas variaciones de densidad, una distribución de temperatura en la que Te(N+) es mayor que Te(O+2) y abundancias que indican que es una planetaria del halo, identificación validada por su alta velocidad radial y su distancia al plano galáctico. La masa ionizada es de 0.1 a 0.4 Mʘ. Un modelo de fotoionización con densidad uniforme (Cloudy, versión 10.00) reproduce la mayor parte del espectro, aunque la intensidad de [O III] 4363 Å es mucho mayor que la observada. En este modelo, las abundancias nebulares son más bajas que las obtenidas con técnicas usuales y la temperatura y luminosidad estelar son 84900° K y 1025 Lʘ, lo que significa que la progenitora probablemente fue una estrella de ≈1 Mʘ en secuencia principal.
ABSTRACT
Optical spectroscopy of the entire planetary nebula M 1–9, reveals pronounced density variations, a temperature distribution where Te(N+) is larger than Te(0+2) and abundances indicating that it is a halo planetary nebulae, an association supported by it is very large radial velocity and distance to the galactic plane. The ionized mass is between 0.1 and 0.4 Mʘ. A uniform density photoionization model (Cloudy, version 10.00) reproduced most of the spectrum, but the intensity of [O III] 4363 Å is much larger than observed. In this model, nebular abundances are smaller than those derived using standard techniques and the stellar temperature and luminosity are 84900° K and 1025 Lʘ, which implies that the progenitor probably was a ≈1 Mʘ zero–age main sequence star.
Key Words: ISM: abundances — ISM: individual objects (M 1–9) — planetary nebulae: general.
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1 Based on observations collected at the Observatorio Astronómico Nacional in San Pedro Mártir, B. C, México.
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