Oxygen abundances and chemical evolution in low surface brightness galaxies

Naray, Rachel Kuzio de; McGaugh, Stacy S.; Blok, W. J. G. de

doi:10.1111/j.1365-2966.2004.08364.x

Cited by 70 publications

(64 citation statements)

References 41 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…As these galaxies have on average lower metallicities (de Naray et al 2004;Gerritsen & de Blok 1999) than their higher surface brightness counterparts, it is likely that the galaxies' SFR has not remained constant throughout the their lifetimes. Indeed, the simplest explanation for the current similar SFRs and higher gas massto-luminosity ratios for the studied galaxies than for their higher surface brightness counterparts is that the galaxies' past SFRs were significantly different than is currently seen.…”

Section: Resultsmentioning

confidence: 99%

“…Studies of large LSB galaxies have discovered a number of intriguing facts: large LSB galaxies, in contrast to dwarf LSB galaxies, can exhibit molecular gas ( Das et al 2006;O'Neil & Schinnerer 2004;O'Neil et al 2000bO'Neil et al , 2003; the gas mass-to-luminosity ratios of large LSB galaxies are typically higher than for similar high surface brightness counterparts by a factor of 2 or more ; and, like dwarf LSB galaxies, large LSB systems are typically dark-matter-dominated (Pickering et al 1997;McGaugh et al 2001). These properties, added to their typically low metallicities (de Naray et al 2004;Gerritsen & de Blok 1999), lead to the inference that even large LSB galaxies are underevolved compared to their high surface brightness (HSB) counterparts. Once their typically low gas surface densities (M H i 10 21 cm À2 ) (Pickering et al 1997) and low baryonic-to-dark matter ratios (Gurovich et al 2004;McGaugh et al 2000) are taken into account, the question becomes less why LSB galaxies are underevolved than how they can form stars at all (O'Neil et al 2000a and references therein).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Star Formation in Galaxies with Large Lower Surface Brightness Disks

2007

View full text Add to dashboard Cite

We present B, R, and H imaging data of 19 large disk galaxies whose properties are intermediate between classical low surface brightness galaxies and ordinary high surface brightness galaxies. We use data taken from the Lowell 1.8 m Perkins telescope to determine the galaxies' overall morphology, color, and star formation properties. Morphologically, the galaxies range from Sb through Irr and include galaxies with and without nuclear bars. The colors of the galaxies vary from B À R ¼ 0:3 to 1.9, and most show at least a slight bluing of the colors with increasing radius. The H images of these galaxies show an average star formation rate lower than is found for similar samples with higher surface brightness disks. In addition, the galaxies studied have both higher gas mass-to-luminosity ratios and more diffuse H emission than is found in higher surface brightness samples.

show abstract

Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Star Formation in Galaxies with Large Lower Surface Brightness Disks

2007

View full text Add to dashboard Cite

show abstract

“…Binggeli et al 1985;Schombert et al 1992;Bothun et al 1993;Bernstein et al 1995;Impey et al 1996;Sprayberry et al 1996;Ulmer et al 1996;O'Neil et al 1997;Kuzio de Naray et al 2004).…”

Section: Introductionunclassified

A search for faint low surface brightness galaxies in the relaxed cluster Abell 496

Ulmer

Adami

Durret

et al. 2011

A&A

View full text Add to dashboard Cite

Context. Cluster faint low surface brightness galaxies (fLSBs) are difficult to observe. Consequently, their origin, physical properties and number density are not well known. After a first search for fLSBs in the highly substructured Coma cluster, we present here a search for fLSBs in the nearly relaxed Abell 496 cluster. Aims. Abell 496 appears to be a much more relaxed cluster than Coma, but still embedded in a large scale filament of galaxies. Our aim is to compare the properties of fLSBs in these two very different clusters, to search for environmental effects. Methods. Based on deep CFHT/Megacam images in the u * , g , r and i bands, we selected galaxies with r > 21 and μ r > 24 mag arcsec −2 . We estimated photometric redshifts for all these galaxies and kept the 142 fLSBs with photo-z < 0.2. Results. In a g − i versus i color-magnitude diagram, we find that a large part of these fLSBs follow the red sequence (RS) of brighter galaxies. The fLSBs within ±1σ of the RS show a homogeneous spatial distribution, while those above the RS appear to be concentrated along the large scale filament of galaxies. Conclusions. These properties are interpreted as agreeing with the idea that RS fLSBs are formed in groups prior to cluster assembly. The formation of red fLSBs could be related to infalling galaxies.

show abstract

“…Empirical calibrations are inspired partly by photo-ionization models and partly by observational trends of line strengths with galactocentric distance in gas-rich spirals, which are believed to be due to a radial abundance gradient with abundances decreasing outwards. In extragalactic objects, the usefulness of the empirical methods goes beyond the derivation of abundance gradients in spirals (Pilyugin et al 2004), as these methods find application in chemical abundance studies of a variety of objects, including low-surface brightness galaxies (de Naray et al 2004) and star-forming galaxies at intermediate and high redshift, where the advent of 8-10 m class telescopes has made it possible to extend observations (e.g., Teplitz et al 2000;Pettini et al 2001;Kobulnicky et al 2003;Lilly et al 2003;Steidel et al 2004;Kobulnicky & Kewley 2004;Erb et al 2006).…”

Section: Appendix A: Empirical Calibrations Of the Oxygen Abundancementioning

confidence: 99%

Massive star formation in Wolf-Rayet galaxies

López-Sánchez

Esteban

2010

A&A

125

121

View full text Add to dashboard Cite

Aims. We have performed a comprehensive multiwavelength analysis of a sample of 20 starburst galaxies that show a substantial population of very young massive stars, most of them classified as Wolf-Rayet (WR) galaxies. In this paper, the forth of the series, we present the global analysis of the derived photometric and chemical properties. Methods. We compare optical/NIR colours and the physical properties (reddening coefficient, equivalent widths of the emission and underlying absorption lines, ionization degree, electron density, and electron temperature) and chemical properties (oxygen abundances and N/O, S/O, Ne/O, Ar/O, and Fe/O ratios) with previous observations and galaxy evolution models. We compile 41 independent star-forming regions -with oxygen abundances between 12 + log(O/H) = 7.58 and 8.75 -, of which 31 have a direct estimate of the electron temperature of the ionized gas.Results. According to their absolute B-magnitude, many of them are not dwarf galaxies, but they should be during their quiescent phase. We found that both c(Hβ) and W abs increase with increasing metallicity. The differences in the N/O ratio is explained assuming differences in the star formation histories. We detected a high N/O ratio in objects showing strong WR features (HCG 31 AC, UM 420, IRAS 0828+2816, III Zw 107, ESO 566-8 and NGC 5253). The ejecta of the WR stars may be the origin of the N enrichment in these galaxies. We compared the abundances provided by the direct method with those obtained through empirical calibrations, finding that (i) the Pilyugin method is the best suited empirical calibration for these star-forming galaxies; (ii) the relations provided by Pettini & Pagel (2004, MNRAS, 348, 59) give acceptable results for objects with 12 + log(O/H) > 8.0; and (iii) the results provided by empirical calibrations based on photoionization models are systematically 0.2-0.3 dex higher than the values derived from the direct method. The O and N abundances and the N/O ratios are clearly related to the optical/NIR luminosity; the dispersion of the data is a consequence of the differences in the star-formation histories. The L-Z relations tend to be tighter when using NIR luminosities, which facilitates distinguishing tidal dwarf galaxies candidates and pre-existing dwarf objects. Galaxies with redder colours tend to have higher oxygen and nitrogen abundances. Conclusions. Our detailed analysis is fundamental to understand the nature of galaxies that show strong starbursts, as well as to know their star formation history and the relationships with the environment. This study is complementary -but usually more powerful-to the less detailed analysis of large galaxy samples that are very common nowadays.

show abstract

Oxygen abundances and chemical evolution in low surface brightness galaxies

Cited by 70 publications

References 41 publications

Star Formation in Galaxies with Large Lower Surface Brightness Disks

Star Formation in Galaxies with Large Lower Surface Brightness Disks

A search for faint low surface brightness galaxies in the relaxed cluster Abell 496

Massive star formation in Wolf-Rayet galaxies

Contact Info

Product

Resources

About