Extragalactic planetary nebulae: Tracers of the chemical evolution of nearby galaxies

Magrini, L.; Stanghellini, Letizia; Gonçalves, Denise R.

doi:10.1017/s1743921312011040

Cited by 8 publications

(6 citation statements)

References 36 publications

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“…Some interesting recent reviews on chemical abundances of PNe were made by Kwitter & Henry (2012); Magrini et al (2012); Delgado-Inglada (2016); García-Rojas (2016).…”

Section: Element Production By Pn Progenitorsmentioning

confidence: 99%

Nebular Spectroscopy: A Guide on H ii Regions and Planetary Nebulae

Peimbert

Delgado-Inglada

2017

PASP

139

125

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We present a tutorial on the determination of the physical conditions and chemical abundances in gaseous nebulae. We also include a brief review of recent results on the study of gaseous nebulae, their relevance for the study of stellar evolution, galactic chemical evolution, and the evolution of the universe. One of the most important problems in abundance determinations is the existence of a discrepancy between the abundances determined with collisionally excited lines and those determined by recombination lines, this is called the ADF (abundance discrepancy factor) problem; we review results related to this problem. Finally, we discuss possible reasons for the large t 2 values observed in gaseous nebulae.

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“…Some interesting recent reviews on chemical abundances of PNe were made by Kwitter & Henry (2012); Magrini et al (2012); Delgado-Inglada (2016); García-Rojas (2016).…”

Section: Element Production By Pn Progenitorsmentioning

confidence: 99%

Nebular Spectroscopy: A Guide on H ii Regions and Planetary Nebulae

Peimbert

Delgado-Inglada

2017

PASP

139

125

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“…Planetary nebulae (PNe) represent the final stage in the evolution of low-to intermediate-mass stars and they are important tools for the study of stellar evolution and gas dynamics (Kwok 2007), as well as tracers of the chemical abundance in nearby galaxies (Magrini et al 2012;Gonçalves 2019). PN studies rely on the knowledge of their physical properties such as the formation rate, Galactic distribution, total and ionized nebular masses, sizes, ages, luminosities and evolutionary states of their central stars (CSs), among others (Gurzadyan 1997;Osterbrock & Ferland 2006;Kwok 2007).…”

Section: Introductionmentioning

confidence: 99%

Distance mapping applied to four well-known planetary nebulae and a nova shell

Gómez-Gordillo

Akras

Gonçalves

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Accurate distance estimates of astrophysical objects such as planetary nebulae (PNe), and nova and supernova remnants, among others, allow us to constrain their physical characteristics, such as size, mass, luminosity, and age. An innovative technique based on the expansion parallax method, the so-called distance mapping technique (DMT), provides distance maps of expanding nebulae as well as an estimation of their distances. The DMT combines the tangential velocity vectors obtained from 3D morpho-kinematic models and the observed proper motion vectors to estimate the distance. We applied the DMT to four PNe (NGC 6702, NGC 6543, NGC 6302, and BD+30 3639) and one nova remnant (GK Persei) and derived new distances in good agreement with previous studies. New simple morpho-kinematic shape models were generated for NGC 6543, NGC 6302, and NGC 6702, whereas for BD+30 3639 and GK Persei published models were used. We demonstrate that the DMT is a useful tool to obtain distance values of PNe, in addition to revealing kinematically peculiar regions within the nebulae. Distances are also derived from the trigonometric Gaia parallaxes. The effect of the non-negligible parallax offset in the second Gaia data release is also discussed.

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“…Together, these two strong emission-line emitters give important constraints to the chemical evolution models, since in both the metallicity (gas-phase or nebular, O/H abundances) are derived in similar ways. For a review on the results for the chemistry of these two populations in nearby galaxies see, for instance, Magrini, Stanghellini & Gonçalves (2012).…”

Section: Pne and Their Chemical Abundances (O/h)mentioning

confidence: 99%

What do planetary nebulae and H II regions reveal about the chemical evolution of nearby dwarf galaxies?

Gonçalves

2018

Proc. IAU

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The Local Group contains a great number of dwarf irregulars and spheroidals, for which the spectroscopy of individual stars can be obtained. Thus, the chemical evolution of these galaxies can be traced, with the only need of finding populations spanning a large age range and such that we can accurately derive the composition. Planetary nebulae (PNe) are old-and intermediate-age star remnants and their chemical abundances can be obtained up to 3-4 Mpc. H ii regions, which are brighter and much easily detected, represent galaxies young content. PNe and H ii regions share similar spectroscopic features and are analysed in the same way. Both are among the best tracers of the chemical evolution allowing to draw the chemical time line of nearby galaxies. The focus in this review are the PN and H ii region populations as constraints to the chemical evolution models and the mass-metallicity relation of the local Universe.

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Extragalactic planetary nebulae: Tracers of the chemical evolution of nearby galaxies

Cited by 8 publications

References 36 publications

Nebular Spectroscopy: A Guide on H ii Regions and Planetary Nebulae

Nebular Spectroscopy: A Guide on H ii Regions and Planetary Nebulae

Distance mapping applied to four well-known planetary nebulae and a nova shell

What do planetary nebulae and H II regions reveal about the chemical evolution of nearby dwarf galaxies?

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