<i>Hubble Space Telescope</i>Observations of Planetary Nebulae in the Magellanic Clouds. V. Mass Dependence of Dredge‐up and the Chemical History of the Large Magellanic Cloud

Dopita, Michael A.; Vassiliadis, E.; Wood, P. R.; Meatheringham, S. J.; Harrington, J. P.; Bohlin, R. C.; Ford, H. C.; Stecher, T. P.; Maran, S. P.

doi:10.1086/303444

Cited by 101 publications

(94 citation statements)

References 54 publications

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“…These changes lead to an Similarly to what we did with our H  region models, we derived the abundances from our planetary nebula models using the classical T e -based method. Here, we assumed There is some concern that, in planetary nebulae, oxygen might not trace the abundance of the interstellar medium exactly, principally due to nuclear and mixing processes in the progenitor star (Dopita et al 1997). If this were true, planetary nebulae would not be convenient objects for studying the metallicity gradients in galaxies.…”

Section: The Use Of Planetary Nebulae As Substitutes For H II Regionsmentioning

confidence: 99%

Biases in abundance derivations for metal-rich nebulae

Stasińska¹

2005

A&A

173

211

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Abstract. Using ab-initio photoionization models of giant H  regions, we test methods for abundance determinations based on a direct measurement of the electron temperature, now possible even for moderate to high-metallicity objects. We find that, for metallicities larger than solar, the computed abundances deviate systematically from the real ones, generally by larger amounts for more metal-rich H  regions. We discuss the reasons for this, and present diagrams allowing the reader to better understand the various factors coming into play. We briefly discuss less classical methods to derive abundances in metal-rich H  regions.In particular, we comment on the interest of the oxygen and carbon recombination lines. We also show that, contrary to the case of giant H  regions, the physical conditions in bright extragalactic planetary nebulae are such that their chemical composition can be accurately derived even at high metallicities. Thus, extragalactic planetary nebulae are promising potential probes of the metallicity of the interstellar medium in the internal parts of spiral galaxies as well as in metal-rich elliptical galaxies.

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Section: The Use Of Planetary Nebulae As Substitutes For H II Regionsmentioning

confidence: 99%

Biases in abundance derivations for metal-rich nebulae

Stasińska¹

2005

A&A

173

211

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“…The sudden rise in the SFR could explain the corresponding sudden rise in the metallicity possibly connected to a former close encounter with the Milky Way that took place ∼1.5 Gyr ago. The metallicity and SFR connected to this event have been observed both from the metallicity in the clusters (Olszewski et al 1996;Geisler et al 1997) and from α-particle elements in planetary nebulae (Dopita 1997). A&A 554, A16 (2013) Notes.…”

Section: Introductionmentioning

confidence: 97%

Age – metallicity relation in the Magellanic Clouds clusters

Livanou

Dapergolas

Kontizas

et al. 2013

A&A

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Aims.We study small open star clusters, using Strömgren photometry to investigate a possible dependence between age and metallicity in the Magellanic Clouds (MCs). Our goals are to trace evidence of an age metallicity relation (AMR) and correlate it with the mutual interactions of the two MCs and to correlate the AMR with the spatial distribution of the clusters. In the Large Magellanic Cloud (LMC), the majority of the selected clusters are young (up to 1 Gyr), and we search for an AMR at this epoch, which has not been much studied. Methods. We report results for 15 LMC and 8 Small Magellanic Cloud (SMC) clusters, scattered all over the area of these galaxies, to cover a wide spatial distribution and metallicity range. The selected LMC clusters were observed with the 1.54 m Danish Telescope in Chile, using the Danish Faint Object Spectrograph and Camera (DFOSC) with a single 2k × 2k CCD. The SMC clusters were observed with the ESO 3.6 m Telescope, also in Chile, using the ESO Faint Object Spectrograph and Camera (EFOSC). The obtained frames were analysed with the conventional DAOPHOT and IRAF software. We used Strömgren filters in order to achieve reliable metallicities from photometry. Isochrone fitting was used to determine the ages and metallicities. Results. The AMR for the LMC displays a metallicity gradient, with higher metallicities for the younger ages. The AMR for LMC-SMC star clusters shows a possible jump in metallicity and a considerable increase at about 6 × 10 8 yr. It is possible that this is connected to the latest LMC-SMC interaction. The AMR for the LMC also displays a metallicity gradient with distance from the centre. The metallicities in SMC are lower, as expected for a metal-poor host galaxy.

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“…One can accurately observe helium and neon abundances in PNe, unlike in a typical stellar photosphere (Kaler 1978;Henry 1989;Dopita et al 1997;Stanghellini et al 2000). This is because a strong ultraviolet flux from the central star of the PN has ionised the surrounding gas.…”

Section: Introductionmentioning

confidence: 99%

“…The forbidden emission lines form in PNe (and diffuse nebulae) because of the low densities, where collisional de-excitation is so slow that a photon is emitted after a time of the order of seconds (Pagel 1997). The C, N and O abundances can also be accurately measured, as well as a host of rare elements including S, Cl and Ar (Dopita et al 1997) and also elements affected by s-processing, such as Ge (Sterling, Dinerstein, & Bowers 2002) and Zn (Dinerstein & Geballe 2001).…”

Section: Introductionmentioning

confidence: 99%

AGB Stars and the Observed Abundance of Neon in Planetary Nebulae

Karakas

Lattanzio

2003

Publ. – Astron. Soc. Aust

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Asymptotic giant branch stars are expected to produce 22 Ne through the combined H and He burning that operates during their thermally pulsing evolution. However, observationally there is a fairly tight correlation between the O and Ne abundances as measured in planetary nebulae in various populations. In this paper we use recent detailed stellar evolutionary calculations for compositions appropriate to the Galaxy and the Large Magellanic Cloud, in an attempt to determine if the models are consistent with the observed abundances. We show that there is only a narrow range in stellar mass, about 2 to 4 M ⊙ (lower for lower [Fe/H]) where 22 Ne is produced in sufficient quantities to affect the total observed elemental neon abundance, which is mostly 20 Ne. The models appear to be consistent with the observations, but a more thorough analysis is required.

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Hubble Space TelescopeObservations of Planetary Nebulae in the Magellanic Clouds. V. Mass Dependence of Dredge‐up and the Chemical History of the Large Magellanic Cloud

Cited by 101 publications

References 54 publications

Biases in abundance derivations for metal-rich nebulae

Biases in abundance derivations for metal-rich nebulae

Age – metallicity relation in the Magellanic Clouds clusters

AGB Stars and the Observed Abundance of Neon in Planetary Nebulae

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