Using Planetary Nebulae to Probe the Structure of the Galactic Thin Disk

Details Using Planetary Nebulae to Probe the Structure of the Galactic Thin Disk Using Planetary Nebulae to Probe the Structure of the Galactic Thin Disk

Oct 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005rmxaa..41..407p&link_type=abstract

Revista Mexicana de Astronomía y Astrofísica Vol. 41, pp. 407-414 (2005) (http://www.astroscu.unam.mx/~rmaa/)

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Ism: Jets And Outflows, Planetary Nebulae: General

Scientific paper

Most planetary nebulae appear to arise from progenitors with mass MPG ≈ 1 M&sun;. One would therefore expect them to be closely associated with stars located within the galactic thin disk. This has been confirmed through a series of recent estimates of scale height, which imply values z0(PNe) of order ˜ 220 pc. We shall show, in the following, that it is also possible to evaluate the variation of z0(PNe) with galactocentric distance R. Although such an analysis is subject to several uncertainties, including those associated with the distances to these outflows, it is nevertheless possible to demonstrate that z0(PNe) increases with increasing R. This spatial ``flaring'' is consistent with what is known of various other disk components.

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