Angular diameters and fluxes of Magellanic Cloud planetary nebulae. II - High-speed direct imaging

Wood, P. R.; Meatheringham, S. J.; Dopita, Michael A.; Morgan, D. H.

doi:10.1086/165533

Cited by 40 publications

(23 citation statements)

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“…This was done, in the same way as in Méndez & Soffner (1997), in order to compensate for an obvious selection effect: the observed distributions in our Galaxy and in the LMC are not likely to include PNs with very low L central stars, all of which have high surface temperatures. Figure 5 shows, then, our corrected theoretical distribution, compared with two observed distributions: one for 118 PNs in the LMC (data taken from Wood et al 1987;Meatheringham et al 1988;Jacoby et al 1990;Meatheringham & Dopita 1991a, 1991bVassiliadis et al 1992) and another one for 983 PNs in our Galaxy, taken from the Strasbourg-ESO Catalogue of Galactic PNs (Acker et al 1992). These are the same two distributions used in Figure 3 of Méndez & Soffner (1997).…”

Section: Resultsmentioning

confidence: 99%

Toward Better Simulations of Planetary Nebulae Luminosity Functions

Méndez

Teodorescu

Schönberner

et al. 2008

ApJ

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We describe a procedure for the numerical simulation of the planetary nebulae luminosity function ( PNLF), improving on previous work. Earlier PNLF simulations were based on an imitation of the observed distribution of the intensities of [O iii] k5007 relative to H , generated predominantly using random numbers. We are now able to replace this by a distribution derived from the predictions of hydrodynamical PN models (Schönberner et al. 2007), which are made to evolve as the central star moves across the HR diagram, using proper initial and boundary conditions. In this way we move one step closer to a physically consistent procedure for the generation of a PNLF. As an example of these new simulations, we have been able to reproduce the observed PNLF in the Small Magellanic Cloud.

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Section: Resultsmentioning

confidence: 99%

Toward Better Simulations of Planetary Nebulae Luminosity Functions

Méndez

Teodorescu

Schönberner

et al. 2008

ApJ

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“…The line fluxes are listed in Meatheringham et al (1998); ; Shaw et al (2006); Stanghellini et al (2002Stanghellini et al ( , 2005; Villaver et al (2003Villaver et al ( , 2004; Wood et al (1987). b Flux in units of erg s À1 cm À2 .…”

Section: Line Emissionmentioning

confidence: 99%

Neon and Sulfur Abundances of Planetary Nebulae in the Magellanic Clouds

Bernard─Salas

Pottasch²,

Gutenkunst

et al. 2008

ApJ

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The chemical abundances of neon and sulfur for 25 planetary nebulae (PNe) in the Magellanic Clouds are presented. These abundances have been derived using mainly infrared data from the Spitzer Space Telescope. The implications for the chemical evolution of these elements are discussed. A comparison with similarly obtained abundances of Galactic PNe and HII regions and Magellanic Clouds HII regions is also given. The average neon abundances are 6.0x10(-5) and 2.7x10(-5) for the PNe in the Large and Small Magellanic Clouds respectively. These are ~1/3 and 1/6 of the average abundances of Galactic planetary nebulae to which we compare. The average sulfur abundances for the LMC and SMC are respectively 2.7x10(-6) and 1.0x10(-6). The Ne/S ratio (23.5) is on average higher than the ratio found in Galactic PNe (16) but the range of values in both data sets is similar for most of the objects. The neon abundances found in PNe and HII regions agree with each other. It is possible that a few (3-4) of the PNe in the sample have experienced some neon enrichment, but for two of these objects the high Ne/S ratio can be explained by their very low sulfur abundances. The neon and sulfur abundances derived in this paper are also compared to previously published abundances using optical data and photo-ionization models.Comment: 13 pages, 4 tables, 5 figures. Accepted for publication in Ap

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“…However, it is likely that the uncertainties are similar to those for the other planetary nebulae. In this figure we also plot the relationship between these abundances found by Izotov et al (2006) in emission-line galaxies, where the relation is set by the nucleosynthetic yields of Type II Aller et al 1987;Barlow 1987;Monk et al 1988;Wood et al 1987;Dopita et al 1988;Meatheringham et al 1988;Henry et al 1989;Meatheringham & Dopita 1991a, 1991bDopita & Meatheringham 1991;Vassiliadis et al 1992;Jacoby & Kaler 1993;Leisy & Dennefeld 1996;see Richer 1993, Richer & McCall 1995, and Stasińska et al 1998 for more details; (6) Peimbert et al 2005; (7) Lee et al 2006;(8) this study ( planetary nebulae only). -We present the correlation of neon and oxygen abundances in bright planetary nebulae in the sample of dwarf irregular galaxies for which these data exist.…”

Section: Chemical Similarity Between Planetary Nebulae and H II Regionsmentioning

confidence: 99%

The Progenitors of Planetary Nebulae in Dwarf Irregular Galaxies

Richer

McCall

2007

ApJ

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We present chemical abundances for planetary nebulae and H II regions in the Local Group dwarf irregular galaxy NGC 6822 based upon spectroscopy obtained at the Canada-France-Hawaii Telescope using the Multi-Object Spectrograph. From these and similar data compiled from the literature for planetary nebulae in the Magellanic Clouds, Sextans A, Sextans B, and Leo A, we consider the origin and evolution of the stellar progenitors of bright planetary nebulae in dwarf irregular galaxies. On average, the oxygen abundance observed in the bright planetary nebulae in these galaxies coincides with that measured in the interstellar medium, indicating that, in general, the bright planetary nebulae in dwarf irregulars descend primarily, though not exclusively, from stars formed in the relatively recent past. We also find that the ratio of neon to oxygen abundances in these bright planetary nebulae is identical to that measured in the interstellar medium, indicating that neither abundance is significantly altered as a result of the evolution of their stellar progenitors. We do find two planetary nebulae, that in Sextans A and S33 in NGC 6822, where oxygen appears to have been dredged up, but these are the exception rather than the rule. In fact, we find that even nitrogen is not always dredged up, so it appears that the dredge-up of oxygen is uncommon for the abundance range of the sample.Comment: accepted for publication in Ap

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Angular diameters and fluxes of Magellanic Cloud planetary nebulae. II - High-speed direct imaging

Cited by 40 publications

References 0 publications

Toward Better Simulations of Planetary Nebulae Luminosity Functions

Toward Better Simulations of Planetary Nebulae Luminosity Functions

Neon and Sulfur Abundances of Planetary Nebulae in the Magellanic Clouds

The Progenitors of Planetary Nebulae in Dwarf Irregular Galaxies

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