Sulfur, Chlorine, and Argon in Planetary Nebulae. IIA. Observations of a Southern Sample

Milingo, J. B.; Kwitter, K. B.; Henry, R. B. C.; Cohen, Roger E.

doi:10.1086/324291

Cited by 24 publications

(18 citation statements)

References 5 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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“…We've acquired spectra for 38 Galactic disk PNe with coverage that extends from 3600Å to 9600Å. Using the same instrumentation and setup as our previous Type II PNe program (Milingo et al 2002a Table 1 lists the objects, total exposure times in the blue and red grating configurations, and the run during which the spectra were acquired.…”

Section: Observations and Reductionsmentioning

confidence: 99%

Alpha Element Abundances in a Large Sample of Galactic Planetary Nebulae

Milingo

Kwitter

Henry

et al. 2010

ApJ

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In this paper we present emission line strengths, abundances, and element ratios (X/O for Ne, S, Cl, and Ar) for a sample of 38 Galactic disk planetary nebulae (PNe) consisting primarily of Peimbert classification Type I. Spectrophotometry for these PNe incorporates an extended optical/near-IR range of λλ3600-9600Å including the [S III] lines at 9069Å and 9532Å, setting this relatively large sample apart from typical spectral coverage. We've utilized ELSA (Emission Line Spectrum Analyzer), a 5-level atom abundance routine, to determine T e , N e , ICFs, and total element abundances, thereby continuing our work toward a uniformly processed set of data. With a compilation

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“…They observed IC 2448 with the 1.5 m telescope and Cassegrain spectrograph at the Cerro Tololo Inter-American Observatory in the spring of 1997 using a 5 00 ; 320 00 slit. The slit width is about half of the diameter of IC 2448, and so Milingo et al (2002a) missed some of the nebular flux. We assume that the optical lines measured in the small aperture are representative of the entire nebula of IC 2448, because IC 2448 has evenly distributed optical [N ii] and [O iii] line emission (Palen et al 2002).…”

Section: Optical and Uv Datamentioning

confidence: 99%

“…We assume that the optical lines measured in the small aperture are representative of the entire nebula of IC 2448, because IC 2448 has evenly distributed optical [N ii] and [O iii] line emission (Palen et al 2002). The extinction-corrected fluxes for the lines we use are listed in Table 2 as given by Milingo et al (2002a). These authors report uncertainties in their line fluxes of P10% for their strong lines (with strengths !H ) and have flagged uncertainties of k25% and k50% for the weaker lines.…”

Section: Optical and Uv Datamentioning

confidence: 99%

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TheSpitzerIRS Infrared Spectrum and Abundances of the Planetary Nebula IC 2448

Guiles¹,

Bernard─Salas²,

Pottasch³

et al. 2007

ApJ

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We present the mid-infrared spectrum of the planetary nebula IC 2448. In order to determine the chemical composition of the nebula, we use the infrared line fluxes from the Spitzer spectrum along with optical line fluxes from the literature and ultraviolet line fluxes from archival IUE spectra. We determine an extinction of C H ¼ 0:27 from hydrogen recombination lines and the radio to H ratio. Forbidden line ratios give an electron density of 1860 cm À3 and an average electron temperature of 12,700 K. The use of infrared lines allows us to determine more accurate abundances than previously possible because abundances derived from infrared lines do not vary greatly with the adopted electron temperature and extinction, and additional ionization stages are observed. Elements left mostly unchanged by stellar evolution (Ar, Ne, S, and O) all have subsolar values in IC 2448, indicating that the progenitor star formed out of moderately metal deficient material. Evidence from the Spitzer spectrum of IC 2448 supports previous claims that IC 2448 is an old nebula formed from a low-mass progenitor star. Subject headingg s: infrared: general -ISM: abundances -ISM: lines and bandsplanetary nebulae: individual (IC 2448) -stars: AGB and post-AGB

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Sulfur, Chlorine, and Argon in Planetary Nebulae. IIA. Observations of a Southern Sample

Cited by 24 publications

References 5 publications

Chemical abundances in Galactic planetary nebulae withSpitzerspectra

Chemical abundances in Galactic planetary nebulae withSpitzerspectra

Alpha Element Abundances in a Large Sample of Galactic Planetary Nebulae

TheSpitzerIRS Infrared Spectrum and Abundances of the Planetary Nebula IC 2448

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