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Refining the UKST Hα Survey's PN Database Using MSX

Published online by Cambridge University Press:  26 May 2016

Martin Cohen  and
Quentin A. Parker
Martin Cohen
Affiliation:
Radio Astronomy Laboratory, 601 Campbell Hall, University of California, Berkeley, CA 94720, USA
Quentin A. Parker
Affiliation:
Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, Edinburgh EH9 3HJ, Scotland, UK Dept. Physics, University of Macquarie, NSW 21090, Australia

Abstract

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We are combining images in the mid-infrared (from MSX, the US Midcourse Space Experiment) with those from the high resolution UKST/AAO Hα survey of the Galactic Plane to investigate the relationship between the mid-infrared (MIR) and optical emission line properties of candidate Planetary Nebulae (PN) discovered by the Hα survey. Preliminary results indicate that only 10–20% of likely bona fide PN have a counterpart detected in the MIR. By sharp contrast one can readily recognize pre-main- sequence objects and HII regions emitting Hα and largely embedded in dust by the simultaneous presence of 8.3 and 21.3-μm emission suggestive of dust spanning a variety of temperatures. The sharpest criteria for recognizing true PN appear to be optical morphology and spectra (particularly the presence of [OIII]), and, where detected, MIR characteristics.

Type
Part II: Planetary Nebulae Surveys and their Distribution in Galaxies
Information
Symposium - International Astronomical Union , Volume 209: Planetary Nebulae: Their Evolution and Role in the Universe , 2003 , pp. 33 - 40
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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