The Chemistry of Planetary Nebulae in the Outer Regions of M31

Corradi, R. L. M.; Kwitter, K. B.; Balick, Bruce; Henry, R. B. C.; Hensley, Kerry

doi:10.1088/0004-637x/807/2/181

Cited by 28 publications

(56 citation statements)

References 42 publications

(65 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The published H II region abundances (e.g., Zurita and Bresolin 2012;Sanders et al 2012) do not extend beyond 25 kpc, and thus whether a similar behaviour is encountered for the younger stellar populations cannot be verified. A flat gradient, with an approximately Solar O/H value, extending out to ∼100 kpc, has been reported for planetary nebulae by Balick et al (2013) and Corradi et al (2015). These authors attribute this finding to a star formation burst following interactions and merger processes, perhaps related to an encounter with M33, that occurred approximately 3 Gyrs ago.…”

Section: Other Systemsmentioning

confidence: 54%

Metallicities in the Outer Regions of Spiral Galaxies

Bresolin

2017

Astrophysics and Space Science Library

View full text Add to dashboard Cite

The analysis of the chemical composition of galaxies provides fundamental insights into their evolution. This holds true also in the case of the outer regions of spiral galaxies. This Chapter presents the observational data, accumulated in the past few years mostly from the analysis of H II region spectra, concerning the metallicity of the outer disks of spirals that are characterized by extended H I envelopes and low star formation rates. I present evidence from the literature that the metal radial distribution flattens at large galactocentric distances, with levels of enrichment that exceed those expected given the large gas mass fractions and the weak star formation activity. The interpretation of these results leads to speculations regarding mechanisms of metal mixing in galactic disks and the possibility that metal-enriched gas infall plays a role in determining the chemical evolution of the outskirts of spirals.

show abstract

Section: Other Systemsmentioning

confidence: 54%

Metallicities in the Outer Regions of Spiral Galaxies

Bresolin

2017

Astrophysics and Space Science Library

View full text Add to dashboard Cite

show abstract

“…3, we present 12 Tables A.3 In their Fig. 4, Corradi et al (2015b) found for M 31 PNe that there seems to be a tendency toward decreasing metallicity with decreasing [O ] luminosity. They also seem to find a similar tendency when plotting M 33 data from Magrini et al (2009).…”

Section: O Abundancesmentioning

confidence: 90%

The planetary nebulae and H II regions in NGC 6822 revisited. Clues to AGB nucleosynthesis

García‐Rojas

Peña

Flores-Durán

et al. 2016

A&A

View full text Add to dashboard Cite

Aims. The chemical behaviour of an ample sample of planetary nebulae (PNe) in NGC 6822 is analysed.Methods. Spectrophotometric data of 11 PNe and two H  regions were obtained with the OSIRIS spectrograph attached to the Gran Telescopio Canarias. Data for other 13 PNe and three H  regions were retrieved from the literature. Physical conditions and chemical abundances of O, N, Ne, Ar, and S were derived in a consistent way for 19 PNe and 4 H  regions.Results. Abundances in the PNe sample are widely distributed showing 12 + log (O/H) from 7.4 to 8.2 and 12 + log (Ar/H) from 4.97 to 5.80. Two groups of PNe can be differentiated: one old with low metallicity (12 + log (O/H) < 8.0 and 12 + log (Ar/H) < 5.7) and another younger one with metallicities similar to the values for H  regions. The old objects are distributed in a larger volume than the young ones. An important fraction of PNe (over 30%) was found to be highly N-rich (Peimbert Type I PNe). Such PNe occur at any metallicity. In addition, about 60% of the sample presents high ionization (He ++ /He ≥ 0.1), possessing a central star with effective temperature higher than 100 000 K. Possible biases in the sample are discussed. From comparison with stellar evolution models by Karakas (2010) and Fishlock et al. (2014) of the observed N/O abundance ratios, our PNe should have had initial masses that are lower than 4 M , although if the comparison is made with Ne vs. O abundances, the initial masses should have been lower than 2 M . It appears that these models of stars of 2−3 M are producing too much 22 Ne in the stellar surface at the end of the AGB. On the other hand, the comparison with another set of stellar evolution models with a different treatment of convection and on the assumptions about the overshoot of the convective core during the core H-burning phase, provided there is reasonable agreement between the observed and predicted N/O and Ne/H ratios if initial masses of more massive stars are about 4 M .

show abstract

“…This is potentially not inconsistent with the interaction hypothesis; Davidge et al (2012) show that the AGB population of M31 is lop-sided, even though some of these stars have ages of a few billion years, and it may be the other disk stellar populations are not well mixed. Independent from HST surveys, analysis of the M31 Planetary Nebulae populution by Balick et al (2013) and Corradi et al (2015) suggest that there was a global period of star formation approximately 2 Gyrs ago, that they attribute to an M31 -M33 interaction.…”

Section: A Census Of M31 Stellar Halo Substructurementioning

confidence: 99%

The Large-scale Structure of the Halo of the Andromeda Galaxy. II. Hierarchical Structure in the Pan-Andromeda Archaeological Survey

McConnachie¹,

Ibata

Martín

et al. 2018

ApJ

151

133

View full text Add to dashboard Cite

The Pan-Andromeda Archaeological Survey is a survey of > 400 square degrees centered on the Andromeda (M31) and Triangulum (M33) galaxies that has provided the most extensive panorama of a L ⋆ galaxy group to large projected galactocentric radii. Here, we collate and summarise the current status of our knowledge of the substructures in the stellar halo of M31, and discuss connections between these features. We estimate that the 13 most distinctive substructures were produced by at least 5 different accretion events, all in the last 3 or 4 Gyrs. We suggest that a few of the substructures furthest from M31 may be shells from a single accretion event. We calculate the luminosities of some prominent substructures for which previous estimates were not available, and we estimate the stellar mass budget of the outer halo of M31. We revisit the problem of quantifying the properties of a highly structured dataset; specifically, we use the OPTICS clustering algorithm to quantify the hierarchical structure of M31's stellar halo, and identify three new faint structures. M31's halo, in projection, appears to be dominated by two "mega-structures", that can be considered as the two most significant branches of a merger tree produced by breaking M31's stellar halo into smaller and smaller structures

show abstract

The Chemistry of Planetary Nebulae in the Outer Regions of M31

Cited by 28 publications

References 42 publications

Metallicities in the Outer Regions of Spiral Galaxies

Metallicities in the Outer Regions of Spiral Galaxies

The planetary nebulae and H II regions in NGC 6822 revisited. Clues to AGB nucleosynthesis

The Large-scale Structure of the Halo of the Andromeda Galaxy. II. Hierarchical Structure in the Pan-Andromeda Archaeological Survey

Contact Info

Product

Resources

About