Kinematic and chemical study of planetary nebulae and H II regions in NGC 3109

Flores-Durán, S. N.; Peña, M.; Ruíz, M. T.

doi:10.1051/0004-6361/201629040

Cited by 7 publications

(8 citation statements)

References 54 publications

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“…Gradients based on oxygen abundances have been also calculated from PN data although for the case of highly ionized objects a correction due to the presence of O +3 is required. However, it has been shown that O in PNe may be enriched (or depleted) due to stellar nucleosynthesis, particularly in low-metallicity environments (Peña, Stasińska, & Richer 2007;Flores-Durán, Peña, & Ruiz 2017) and also in Galactic PNe with carbon-rich dust (Delgado-Inglada et al 2015). Therefore metallicity gradients derived from O abundances in PNe could be perturbed by stellar nucleosynthesis and thus this element could be not adequate to analyze the chemical gradients and the evolution of galaxies.…”

Section: Introductionmentioning

confidence: 99%

“…Therefore metallicity gradients derived from O abundances in PNe could be perturbed by stellar nucleosynthesis and thus this element could be not adequate to analyze the chemical gradients and the evolution of galaxies. Apparently Ne abundances are also modified by stellar nucleosynthesis in lowmetallicity environments (Karakas 2010;Milingo et al 2010;Flores-Durán, Peña, & Ruiz 2017). On the other hand, Ar and S abundances in PNe are not expected to be modified in such processes during the PN progenitor lifetime, although their abundance determinations have large uncertainties due to large uncertainties in the ionization correction factors when only one ion (Ar ++ or S + ) is observed (Delgado-Inglada, Morisset, & Stasińska 2014).…”

Section: Introductionmentioning

confidence: 99%

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Metallicity Gradients in M31, M 33, NGC 300 and the Milky Way Using Abundances of Different Elements

Peña

Flores-Durán

2019

RMxAA

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RESUMENEstudiamos los gradientes de metalicidad de O, Ne y Ar, derivados de nebulosas planetarias (PNe), en comparación con los de regiones H ii en las galaxias M 31, M 33, NGC 300 y la Vía Láctea. Radios galactocéntricos y abundancias fueron recopilados de la literatura, seleccionando con cuidado una muestra homogénea de objetos en cada galaxia. Los gradientes de las PNe son más planos que los de las regiones H ii en todos los casos. El caso más extremo es el de M 31, donde las abundancias de las PNe no están relacionadas con la distancia galactocéntrica y los gradientes son consistentes con cero. Calculamos gradientes para PNe del Tipo I y no-Tipo I de Peimbert, encontrando que los gradientes del Tipo I son más empinados y más similares a los de las regiones H ii, lo que indicaría que los gradientes de metalicidad se empinan con el tiempo. Alternativamente los gradientes planos de las viejas PNe indican que la migración radial juega un importante papel en las galaxias.ABSTRACT Metallicity gradients derived from planetary nebulae (PNe) using O, Ne, and Ar abundances are studied and compared to those from H ii regions in the galaxies M 31, M 33, NGC 300 and the Milky Way. Galactocentric radii and chemical abundances were collected from the literature, carefully selecting a homogeneous sample for each galaxy. Metallicity gradients shown by PNe are flatter than those of H ii regions in all cases. The extreme case is M 31 where PN abundances are not related to galactocentric distances and the gradients are consistent with zero.To analyze the evolution of gradients with time we build gradients for Peimbert Type I and non-Type I PNe finding that Type I PNe show steeper gradients than non-Type I PNe and more similar to the ones of H ii regions indicating that the chemical gradients might steepen with time. Alternatively, the flat gradients for old PNe show that radial migration could have an important role in the evolution of galaxies.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Metallicity Gradients in M31, M 33, NGC 300 and the Milky Way Using Abundances of Different Elements

Peña

Flores-Durán

2019

RMxAA

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“…Lines of [O ii] λλ3726+29 are summed in the tables even if observations allow one to separate the lines. The only PNe where this doublet is resolved are: one object in NGC 3109 observed by Peña et al (2007b) and the sample studied by Flores-Durán et al (2017), the PNe in the LMC and SMC reported by Tsamis et al (2003), and the SMC sample observed by Shaw et al (2010).…”

Section: Line Fluxesmentioning

confidence: 90%

A study of extragalactic planetary nebulae populations based on spectroscopy. I. Data compilation and first findings

Delgado-Inglada,

García-Rojas,

Stasińska

et al. 2020

Preprint

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We compile published spectroscopic data and [O iii] magnitudes of almost 500 extragalactic planetary nebulae (PNe) in 13 galaxies of various masses and morphological types. This is the first paper of a series that aims to analyze the PN populations and their progenitors in these galaxies. Although the samples are not complete or homogeneous we obtain some first findings through the comparison of a few intensity line ratios and nebular parameters. We find that the ionized masses and the luminosities in Hβ, L Hβ , of around 30 objects previously identified as PNe indicate that they are most likely compact H ii regions. We find an anticorrelation between the electron densities and the ionized masses in M 31, M 33, and NGC 300 which suggests that most of the PNe observed in these galaxies are probably ionization bounded. This trend is absent in LMC and SMC suggesting that many of their PNe are density bounded. The He ii λ4686/Hβ values found in many PNe in LMC and some in M 33 and SMC are higher than in the other galaxies. Photoionization models predict that these high values can only be reached in density bounded PNe. We also find that the brightest PNe in the sample are not necessarily the youngest since there is no correlation between electron densities and the Hβ luminosities. The strong correlation found between L Hβ -L [O iii] implies that the so far not understood cut off of the planetary luminosity function (PNLF) based on [O iii] magnitudes can be investigated using L Hβ , a parameter much easier to study.

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“…Chemical abundance determinations in these systems are mainly limited to H II regions (e.g., Izotov & Thuan 1999;Kniazev et al 2005;Magrini et al 2005;van Zee & Haynes 2006;Guseva et al 2011;Haurberg et al 2013;Berg et al 2012) and to a few supergiant stars (Venn et al 2001(Venn et al , 2003Kaufer et al 2004;Leaman et al 2009Leaman et al , 2013, which probe a look-back time of at most ∼10 Myr. Chemical abundance studies of planetary nebulae (e.g., Magrini et al 2005;Peña et al 2007;García-Rojas et al 2016;Flores-Durán et al 2017;Annibali et al 2017) and unresolved star clusters (e.g., Strader et al 2003;Puzia & Sharina 2008;Sharina et al 2010;Hwang et al 2014) provide a valuable tool to explore more ancient epochs and have been attempted in a few dwarf irregulars. The H II region and young supergiant tracers indicate typically low [α/Fe] ratios, as expected in galaxies that have formed stars at a low rate over a long period of time and where galactic winds may have possibly contributed to the expulsion of the α-elements.…”

Section: [α/Fe] Ratiosmentioning

confidence: 99%

LBT/MODS spectroscopy of globular clusters in the irregular galaxy NGC 4449

Annibali¹,

Morandi

Watkins

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present intermediate-resolution (R∼1000) spectra in the ∼3 500-10 000Å range of 14 globular clusters in the magellanic irregular galaxy NGC 4449 acquired with the Multi Object Double Spectrograph on the Large Binocular Telescope. We derived Lick indices in the optical and the CaII-triplet index in the near-infrared in order to infer the clusters' stellar population properties. The inferred cluster ages are typically older than ∼9 Gyr, although ages are derived with large uncertainties. The clusters exhibit intermediate metallicities, in the range −1.2 [Fe/H] −0.7, and typically sub-solar [α/F e] ratios, with a peak at ∼ −0.4. These properties suggest that i) during the first few Gyrs NGC 4449 formed stars slowly and inefficiently, with galactic winds having possibly contributed to the expulsion of the α-elements, and ii) globular clusters in NGC 4449 formed relatively "late", from a medium already enriched in the products of type Ia supernovae. The majority of clusters appear also under-abundant in CN compared to Milky Way halo globular clusters, perhaps because of the lack of a conspicuous N-enriched, second-generation of stars like that observed in Galactic globular clusters. Using the cluster velocities, we infer the dynamical mass of NGC 4449 inside 2.88 kpc to be M(<2.88 kpc)=3.15 +3.16 −0.75 × 10 9 M ⊙ . We also report the serendipitous discovery of a planetary nebula within one of the targeted clusters, a rather rare event.

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Kinematic and chemical study of planetary nebulae and H II regions in NGC 3109

Cited by 7 publications

References 54 publications

Metallicity Gradients in M31, M 33, NGC 300 and the Milky Way Using Abundances of Different Elements

Metallicity Gradients in M31, M 33, NGC 300 and the Milky Way Using Abundances of Different Elements

A study of extragalactic planetary nebulae populations based on spectroscopy. I. Data compilation and first findings

LBT/MODS spectroscopy of globular clusters in the irregular galaxy NGC 4449

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