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2006MNRAS.369..875Z - Mon. Not. R. Astron. Soc., 369, 875-890 (2006/June-3)
The planetary nebula population of the Sagittarius dwarf spheroidal galaxy.
ZIJLSTRA A.A., GESICKI K., WALSH J.R., PEQUIGNOT D., VAN HOOF P.A.M. and MINNITI D.
Abstract (from CDS):
Hubble Space Telescope images of three of the PNe reveal well-developed bipolar morphologies, and provide clear detections of the central stars. All three stars with deep spectra show WR lines, suggesting that the progenitor mass and metallicity determines whether a PN central star develops a WR spectrum. One Sgr PN belongs to the class of IR-[WC] stars. Expansion velocities are determined for three nebulae. Comparison with hydrodynamical models indicates an initial density profile of ρ ∝ r–3. This is evidence for increasing mass-loss rates on the asymptotic giant branch. Peak mass-loss rates are indicated of ∼10–4M☉/yr.
The IR-[WC] PN, He2-436, provides the sole direct detection of dust in a dwarf spheroidal galaxy, to date.
Abstract Copyright: 2006 The Authors. Journal compilation © 2006 RAS
Journal keyword(s): stars: abundances - stars: mass-loss - planetary nebulae: general - galaxies: individual: Sagittarius dwarf spheroidal
Simbad objects: 27
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