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The Structure of NGC 6309: BRET or Bipolar Outflow?

Published online by Cambridge University Press:  26 May 2016

R. Vázquez ,
L. F. Miranda ,
L. Olguín ,
J. M. Torrelles  and
J. A. López
R. Vázquez
Affiliation:
1Instituto de Astronomía, UNAM, Ensenada, B. C., Mexico
L. F. Miranda
Affiliation:
2Instituto de Astrofísica de Andalucía, CSIC, Granada, Spain
L. Olguín
Affiliation:
3Instituto de Astronomía, UNAM, México, D. F., Mexico
J. M. Torrelles
Affiliation:
4Institut d'Estudis Espacials de Catalunya (IEEC/CSIC) and Instituto de Ciencias del Espacio, CSIC, Barcelona, Spain
J. A. López
Affiliation:
1Instituto de Astronomía, UNAM, Ensenada, B. C., Mexico

Abstract

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Multiwavelength and multitechnique observations towards NGC 6309 are presented. The data consist of λ3.6-cm continuum, ground- and space-based imaging, and high and low-dispersion longslit spectra. The structure of the central region seems to be a distorted, ring of 20″ in diameter. The lack of [N II] emission is conspicuous, as revealed by imaging and low dispersion spectra. Notably, the kinematics of the point-symmetric (PS) structures of NGC 6309 indicates the presence of lobes or cavities as those generally found in bipolar nebulae. The results lead to conclude that the origin of this peculiar morphology is not related to BRETs, but rather to that of a bipolar PN with PS structures in its lobes.

Type
Part VII: Nebular Morphology and Dynamics
Information
Symposium - International Astronomical Union , Volume 209: Planetary Nebulae: Their Evolution and Role in the Universe , 2003 , pp. 537 - 538
Copyright
Copyright © Astronomical Society of the Pacific 2003