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History of the mass ejection in K4-37: from the AGB to the evolved planetary nebula phase

AutorMiranda, Luis F. ; Guillen, P. F.; Olguin, L; Vazquez, R
Palabras claveCircumstellar matter
ISM: jets and outflows
Planetary nebulae: individual: K4-37
Fecha de publicación13-dic-2016
EditorOxford University Press
CitaciónMonthly Notices of the Royal Astronomical Society 466(2): 2151-2160 (2017)
ResumenWe present narrow-band, broad-band and Wide-field Infrared Survey Explorer (WISE) archive images, and high-and intermediate-resolution long-slit spectra of K4-37, a planetary nebula that has never been analysed in detail. Although K4-37 appears bipolar, the morphokinematical analysis discloses the existence of three distinct axes and additional particular directions in the object, indicating that K4-37 is a multi-axis planetary nebula that has probably been shaped by several bipolar outflows at different directions. A 4-6 M-circle dot main-sequence progenitor is estimated from the derived high nebular He and N abundances, and very high N/O abundance ratio (similar to 2.32). The general properties are compatible with K4-37 being a highly evolved planetary nebula located at similar to 14 kpc. The WISE image at 22 mu m reveals K4-37 to be surrounded by a large (similar to 13 x 8 pc(2)) elliptical detached shell probably related to material ejected from the asymptotic giant branch (AGB) progenitor. The observed elliptical morphology suggests deformation of an originally spherical AGB shell by the interstellar medium magnetic field or by the influence of a companion. We compare K4-37 and NGC 6309 and found remarkable similarities in their physical structure but noticeably different chemical abundances that indicate very different progenitor mass. This strongly suggests that, irrespective of the initial mass, their (presumably binary) central stars have shared a very similar mass ejection history. © 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.
Versión del editorhttp://dx.doi.org/10.1093/mnras/stw3245
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