Abundances of recently discovered planetary nebulae towards the galactic bulge

Escudero, Alfonso; Costa, R. D. D.

doi:10.1051/0004-6361:20011490

Cited by 42 publications

(71 citation statements)

References 27 publications

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“…They also had to contain enough objects to allow us to assess their quality and internal integrity in a way that is similar to our own data presented here. These requirements were met by the following papers: de Freitas Pacheco et al (1992), Kingsburgh & Barlow (1994), Cuisinier et al (1996Cuisinier et al ( , 2000, Ratag et al (1997), Escudero & Costa (2001), Kwitter & Henry (2001), Peña et al (2001), Milingo et al (2002), Escudero et al (2004), Exter et al (2004), Górny et al (2004Górny et al ( , 2009, Girard et al (2007), Wang & Liu (2007), Cavichia et al (2010), Henry et al (2010), and Górny (2014). In short, we found useful optical spectroscopic literature data for 76, 30, and nine Galactic PNe in the lists by Stanghellini et al (2012), Perea-Calderón et al (2009), andGutenkunst et al (2008), respectively.…”

Section: Nebular Abundances From Literature Datamentioning

confidence: 99%

Chemical abundances in Galactic planetary nebulae withSpitzerspectra

García-Hernández

Górny

2014

A&A

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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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Section: Nebular Abundances From Literature Datamentioning

confidence: 99%

Chemical abundances in Galactic planetary nebulae withSpitzerspectra

García-Hernández

Górny

2014

A&A

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“…The data set for 164 PNe from Górny et al (2004) come from the merging of data for 44 PNe observed by Górny in 2000 with those for PNe observed by Cuisinier et al (2000), Escudero & Costa (2001), and Escudero et al (2004). In this way, we obtain the largest sample of PNe with high-quality data observed in the direction of the Galactic bulge (for a detailed description, see Górny et al 2009), with 245 objects (for the 39 objects belonging to more than one sample, the best data were chosen).…”

Section: Bulge and Inner-diskmentioning

confidence: 99%

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

Chiappini¹,

Górny²,

Stasińska³

et al. 2008

A&A

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Context. Our understanding of the chemical evolution (CE) of the Galactic bulge requires the determination of abundances in large samples of giant stars and planetary nebulae (PNe). Studies based on high resolution spectroscopy of giant stars in several fields of the Galactic bulge obtained with very large telescopes have allowed important progress. Aims. We discuss PNe abundances in the Galactic bulge and compare these results with those presented in the literature for giant stars.Methods. We present the largest, high-quality data-set available for PNe in the direction of the Galactic bulge (inner-disk/bulge). For comparison purposes, we also consider a sample of PNe in the Large Magellanic Cloud (LMC). We derive the element abundances in a consistent way for all the PNe studied. By comparing the abundances for the bulge, inner-disk, and LMC, we identify elements that have not been modified during the evolution of the PN progenitor and can be used to trace the bulge chemical enrichment history. We then compare the PN abundances with abundances of bulge field giant. Results. At the metallicity of the bulge, we find that the abundances of O and Ne are close to the values for the interstellar medium at the time of the PN progenitor formation, and hence these elements can be used as tracers of the bulge CE, in the same way as S and Ar, which are not expected to be affected by nucleosynthetic processes during the evolution of the PN progenitors. The PN oxygen abundance distribution is shifted to lower values by 0.3 dex with respect to the distribution given by giants. A similar shift appears to occur for Ne and S. We discuss possible reasons for this PNe-giant discrepancy and conclude that this is probably due to systematic errors in the abundance derivations in either giants or PNe (or both). We issue an important warning concerning the use of absolute abundances in CE studies.

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“…This number is low compared with the estimated numbers of ∼ 2000 GBPNe by Gesicki et al (2014) and ∼ 3500 GBPNe by Peyaud et al (2006). The currently number of GBPNe with accurate chemical abundances is ∼ 300, considering the works done by Escudero & Costa (2001); Escudero et al (2004); Cavichia et al (2010), hereafter IAG-USP sample, and also the works of Górny et al (2009), Wang & Liu (2007), Cuisinier et al (2000), Exter et al (2004), as compiled by Chiappini et al (2009). The fact that PNe are originated from stars of different masses and, consequently, evolutionary pathways, hamper the construction of representatives samples for unbiased chemical composition studies.…”

Section: Introductionmentioning

confidence: 77%

The population of planetary nebulae near the Galactic Centre: chemical abundances

Mollá¹,

Cavichia

Costa

et al. 2016

Proc. IAU

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Planetary nebulae (PNe) constitute an important tool to study the chemical evolution of the Milky Way and other galaxies, probing the nucleosynthesis processes, abundance gradients and the chemical enrichment of the interstellar medium. In particular, Galactic bulge PNe (GBPNe) have been extensively used in the literature to study the chemical properties of this Galactic structure. However, the presently available GBPNe chemical composition studies are strongly biased, since they were focused on brighter objects, predominantly located in Galactic regions of low interstellar reddening. In this work, we report physical parameters and abundances derived for a sample of 17 high extinction PNe located in the inner 2• of the Galactic bulge, based on low dispersion spectroscopy secured at the SOAR telescope using the Goodman spectrograph. The new data allow us to extend our database including faint objects, providing chemical compositions for PNe located in this region of the bulge and an estimation for the masses of their progenitors to explore the chemical enrichment history of the central region of the Galactic bulge. The results show that there is an enhancement in the N/O abundance ratio in the Galactic centre PNe compared with PNe located in the outer regions of the Galactic bulge. This may indicate recent episodes of star formation occurring near the Galactic centre.

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Abundances of recently discovered planetary nebulae towards the galactic bulge

Cited by 42 publications

References 27 publications

Chemical abundances in Galactic planetary nebulae withSpitzerspectra

Chemical abundances in Galactic planetary nebulae withSpitzerspectra

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

The population of planetary nebulae near the Galactic Centre: chemical abundances

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