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Conference Paper: Refining the UKST Hα survey's PN database using MSX

TitleRefining the UKST Hα survey's PN database using MSX
Authors
Issue Date1-Jan-2003
PublisherAstronomical Society of the Pacific
AbstractWe are combining images in the mid-infrared (from MSX, the US Midcourse Space Experiment) with those from the high resolution UKST/AAO Halpha 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 Ha 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 Ha and largely embedded in dust by the simultaneous presence of 8.3 and 21.3 mum 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.
Persistent Identifierhttp://hdl.handle.net/10722/342821
ISBN
ISSN
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorCohen, M-
dc.contributor.authorParker, QA-
dc.date.accessioned2024-05-02T03:06:06Z-
dc.date.available2024-05-02T03:06:06Z-
dc.date.issued2003-01-01-
dc.identifier.isbn1-58381-148-6-
dc.identifier.issn0074-1809-
dc.identifier.urihttp://hdl.handle.net/10722/342821-
dc.description.abstractWe are combining images in the mid-infrared (from MSX, the US Midcourse Space Experiment) with those from the high resolution UKST/AAO Halpha 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 Ha 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 Ha and largely embedded in dust by the simultaneous presence of 8.3 and 21.3 mum 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.-
dc.languageeng-
dc.publisherAstronomical Society of the Pacific-
dc.relation.ispartofProceedings of the 195th Symposium of the International Astronomical Union --- Highly Energetic Physical Processes and Mechanisms for Emission from Astrophysical Plasmas-
dc.titleRefining the UKST Hα survey's PN database using MSX-
dc.typeConference_Paper-
dc.identifier.issue209-
dc.identifier.spage33-
dc.identifier.epage40-
dc.identifier.isiWOS:000187344400004-
dc.publisher.placeSAN FRANCISCO-
dc.identifier.issnl0074-1809-

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