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Newly discovered Wolf–Rayet and weak emission‐line central stars of planetary nebulae

Identifieur interne : 006375 ( Main/Exploration ); précédent : 006374; suivant : 006376

Newly discovered Wolf–Rayet and weak emission‐line central stars of planetary nebulae

Auteurs : K. Depew [Australie] ; Q. A. Parker [Australie] ; B. Miszalski ; O. De Marco [Australie] ; D. J. Frew [Australie] ; A. Acker [France] ; A. V. Kovacevic [Australie] ; R. G. Sharp [Australie]

Source :

RBID : ISTEX:59ED1B043080A167DCFF204224F5386E084F65D4

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English descriptors

Abstract

We present the spectra of 32 previously unpublished confirmed and candidate Wolf–Rayet ([WR]) and weak emission‐line (WELS) central stars of planetary nebulae (CSPNe). 18 stars have been discovered in the Macquarie/AAO/Strasbourg Hα (MASH) PN survey sample, and we have also uncovered 14 confirmed and candidate [WR]s and WELS among the CSPNe of previously known PNe. Spectral classifications have been undertaken using both Acker & Neiner and Crowther, De Marco & Barlow schemes. 22 members in this sample are identified as probable [WR]s; the remaining 10 appear to be WELS. Observations undertaken as part of the MASH spectroscopic survey have now increased the number of known [WR]s by ∼30 per cent. This will permit a better analysis of [WR] subclass distribution, metallicity effects and evolutionary sequences in these uncommon objects.

Url:
DOI: 10.1111/j.1365-2966.2011.18337.x


Affiliations:


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Le document en format XML

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<div type="abstract" xml:lang="en">We present the spectra of 32 previously unpublished confirmed and candidate Wolf–Rayet ([WR]) and weak emission‐line (WELS) central stars of planetary nebulae (CSPNe). 18 stars have been discovered in the Macquarie/AAO/Strasbourg Hα (MASH) PN survey sample, and we have also uncovered 14 confirmed and candidate [WR]s and WELS among the CSPNe of previously known PNe. Spectral classifications have been undertaken using both Acker & Neiner and Crowther, De Marco & Barlow schemes. 22 members in this sample are identified as probable [WR]s; the remaining 10 appear to be WELS. Observations undertaken as part of the MASH spectroscopic survey have now increased the number of known [WR]s by ∼30 per cent. This will permit a better analysis of [WR] subclass distribution, metallicity effects and evolutionary sequences in these uncommon objects.</div>
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