Abundances in the Galactic bulge: results from planetary nebulae and giant stars

Chiappini, Cristina; Górny, S. K.; Stasińska, G.; Barbuy, B.

doi:10.1051/0004-6361:200810849

Cited by 45 publications

(89 citation statements)

References 70 publications

(147 reference statements)

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“…SMP L39, SMP L52, and RP 659 were assigned the default value of 0.1 per Gathier (1987) since measured values for those PNe were not available. Calculations for the remaining PNe used helium abundances from Chiappini et al (2009). No values for the fraction of doubly ionised helium were available so we adopted the default value of 1/3 as used by Gathier (1987).…”

Section: Radio-continuum Properties Of the Detected Pnementioning

confidence: 99%

Radio Planetary Nebulae in the Large Magellanic Cloud

Leverenz

Filipović

Vukotić

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present 21 new radio-continuum detections at catalogued planetary nebula (PN) positions in the Large Magellanic Cloud (LMC) using all presently available data from the Australia Telescope Online Archive at 3, 6, 13 and 20 cm. Additionally, 11 previously detected LMC radio PNe are re-examined with 7 detections confirmed and reported here. An additional three PNe from our previous surveys are also studied. The last of the 11 previous detections is now classified as a compact H ii region which makes for a total sample of 31 radio PNe in the LMC. The radio-surface brightness to diameter (Σ-D) relation is parametrised as Σ ∝ D −β . With the available 6 cm Σ-D data we construct Σ-D samples from 28 LMC PNe and 9 Small Magellanic Cloud (SMC) radio detected PNe. The results of our sampled PNe in the Magellanic Clouds (MCs) are comparable to previous measurements of the Galactic PNe. We obtain β = 2.9 ± 0.4 for the MC PNe compared to β = 3.1 ± 0.4 for the Galaxy. For a better insight into sample completeness and evolutionary features we reconstruct the Σ-D data probability density function (PDF). The PDF analysis implies that PNe are not likely to follow linear evolutionary paths. To estimate the significance of sensitivity selection effects we perform a Monte Carlo sensitivity simulation on the Σ-D data. The results suggest that selection effects are significant for values larger than β ∼ 2.6 and that a measured slope of β = 2.9 should correspond to a sensitivity-free value of ∼ 3.4.

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Section: Radio-continuum Properties Of the Detected Pnementioning

confidence: 99%

Radio Planetary Nebulae in the Large Magellanic Cloud

Leverenz

Filipović

Vukotić

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…The chemical composition and the observed line intensities were adopted from the literature. For most of the PNe, the chemical abundances were recently published by Chiappini et al (2009) and Górny et al (2009), while some data were used from Stasińska et al (1998). These abundances were used in the photo-ionization model.…”

Section: Photoionization Modelling Of the Nebulaementioning

confidence: 99%

Accelerated post-AGB evolution, initial-final mass relations, and the star-formation history of the Galactic bulge

Gęsicki

Zijlstra

Hajduk

et al. 2014

A&A

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Aims. We study the star-formation history of the Galactic bulge, as derived from the age distribution of the central stars of planetary nebulae that belong to this stellar population. Methods. The high resolution imaging and spectroscopic observations of 31 compact planetary nebulae are used to derive their central star masses. We use the Blöcker post asymptotic giant branch (post-AGB) evolutionary models, which are accelerated by a factor of three in this case to better fit the white dwarf mass distribution and asteroseismological masses. Initial-final mass relations (IFMR) are derived using white dwarfs in clusters. These are applied to determine original stellar masses and ages. The age distribution is corrected for observational bias as a function of stellar mass. We predict that there are about 2000 planetary nebulae in the bulge. Results. The planetary nebula population points at a young bulge population with an extended star-formation history. The Blöcker tracks with the cluster IFMR result in ages, which are unexpectedly young. We find that the Blöcker post-AGB tracks need to be accelerated by a factor of three to fit the local white dwarf masses. This acceleration extends the age distribution. We adjust the IFMR as a free parameter to map the central star ages on the full age range of bulge stellar populations. This fit requires a steeper IFMR than the cluster relation. We find a star-formation rate in the Galactic bulge, which is approximately constant between 3 and 10 Gyr ago. The result indicates that planetary nebulae are mainly associated with the younger and more metal-rich bulge populations. Conclusions. The constant rate of star-formation between 3 and 10 Gyr agrees with suggestions that the metal-rich component of the bulge is formed during an extended process, such as a bar interaction.

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“…The second and third rows give the upper and lower limits of these parameters, respectively. If there was only one source of data, these errors were calculated with Monte Carlo simulations (see Chiappini et al 2009, for more details). Also, if there was more than one entry for a given object, these values are again averages of individually determined errors.…”

Section: Nebular Abundances From Literature Datamentioning

confidence: 99%

“…Chiappini et al 2009). The few (3-4) DC bulge PNe with reliable Ar abundances, however, display high Ar abundances (nearly solar), and the apparent N overproduction (and higher N/O ratios) could be due to stronger HBB in higher mass stars.…”

Section: Pne Nebular Abundances Vs Major Spitzer Dust Typesmentioning

confidence: 99%

Chemical abundances in Galactic planetary nebulae withSpitzerspectra

García-Hernández

Górny

2014

A&A

Self Cite

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We present new low-resolution (R ∼ 800) optical spectra of 22 Galactic planetary nebulae (PNe) with Spitzer spectra. These data are combined with recent optical spectroscopic data available in the literature to construct representative samples of compact (and presumably young) Galactic disc and bulge PNe with Spitzer spectra. Attending to the nature of the dust features -C-rich, O-rich, and both C-and O-rich dust features (or double chemistry) -seen in their Spitzer spectra, the Galactic disc and bulge PNe are classified according to four major dust types (oxygen chemistry or OC, carbon chemistry or CC, double chemistry or DC, featureless or F) and subtypes (amorphous and crystalline, and aliphatic and aromatic), and their Galactic distributions are presented. Nebular gas abundances of He, N, O, Ne, S, Cl, and Ar, as well as plasma parameters (e.g. N e , T e ) are homogeneously derived by using the classical empirical method. We study the median chemical abundances and nebular properties in Galactic disc and bulge PNe depending on their Spitzer dust types and subtypes. The differences and similarities between PNe in the Galactic disc and bulge are reported. In particular, the median abundances for the major Spitzer dust types CC and OC are representative of the dominant dust subtype (which are different in both Galactic environments), while these values in DC PNe are representative of the two DC subtypes. A comparison of the derived median abundance patterns with AGB nucleosynthesis predictions mainly show that i) DC PNe, both with amorphous and crystalline silicates, display high-metallicity (solar/supra-solar) and the highest He abundances and N/O abundance ratios, suggesting relatively massive (∼3-5 M ) hot bottom burning AGB stars as progenitors; ii) PNe with O-rich and C-rich unevolved dust (amorphous and aliphatic) seem to evolve from subsolar metallicity (z ∼ 0.008) and lower mass (<3 M ) AGB stars; iii) a few O-rich PNe and a significant fraction of C-rich PNe with more evolved dust (crystalline and aromatic, respectively) display chemical abundances similar to DC PNe, suggesting that they are related objects. A comparison of the derived nebular properties with predictions from models combining the theoretical central star evolution with a simple nebular model is also presented. Finally, a possible link between the Spitzer dust properties, chemical abundances, and evolutionary status is discussed.

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Abundances in the Galactic bulge: results from planetary nebulae and giant stars

Cited by 45 publications

References 70 publications

Radio Planetary Nebulae in the Large Magellanic Cloud

Radio Planetary Nebulae in the Large Magellanic Cloud

Accelerated post-AGB evolution, initial-final mass relations, and the star-formation history of the Galactic bulge

Chemical abundances in Galactic planetary nebulae withSpitzerspectra

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