Metal Abundances of KISS Galaxies. IV. Galaxian Luminosity‐Metallicity Relations in the Optical and Near‐Infrared

Salzer, John J.; Lee, Janice; Melbourne, Jason; Hinz, J. L.; Alonso‐Herrero, A.; Jangren, Anna

doi:10.1086/429386

Cited by 95 publications

(178 citation statements)

References 52 publications

Supporting

Mentioning

159

Contrasting

Order By: Relevance

“…Our sample does not show any trend with absolute magnitude of either C(Hβ) or EW(Hβ), contrary to what was obtained by Salzer et al (2005) for the KISS sample. The extinction in our sample galaxies is low.…”

Section: Luminosity-metallicity Relationcontrasting

confidence: 99%

“…The slopes of our L − Z relation of 0.134 (0.174) are very close to the slope of 0.153 by Skillman et al (1989) and to the slope of 0.147 by Richer & McCall (1995). Our sample is well populated in the low-luminosity range, while less than 10 galaxies from the KISS sample (Salzer et al 2005) which were used for the study of the L − Z relation are fainter than M B = −15, and none of them has an oxygen abundance less than 7.6. Our sample, excluding the SDSS subsample, has a lower dispersion around the dotted line compared to all our data and shows a shift to lower metallicities or/and higher luminosities.…”

Section: Luminosity-metallicity Relationmentioning

confidence: 99%

See 1 more Smart Citation

An investigation of the luminosity-metallicity relation for a large sample of low-metallicity emission-line galaxies

Гусева

Papaderos

Meyer

et al. 2009

A&A

103

View full text Add to dashboard Cite

Context. We present 8.2 m VLT spectroscopic observations of 28 H ii regions in 16 emission-line galaxies and 3.6 m ESO telescope spectroscopic observations of 38 H ii regions in 28 emission-line galaxies. These emission-line galaxies were selected mainly from the data release 6 (DR6) of the Sloan digital sky survey (SDSS) as metal-deficient galaxy candidates. Aims. We collect photometric and high-quality spectroscopic data for a large uniform sample of star forming galaxies including new observations. Our aim is to study the luminosity-metallicity (L − Z) relation for nearby galaxies, especially at its low-metallicity end and compare it with that for higher-redshift galaxies.Methods. Physical conditions and element abundances in the new sample are derived with the T e -method, excluding six H ii regions from the VLT observations and nearly two third of the H ii regions from the 3.6 m observations. Element abundances for the latter galaxies were derived with the semiempirical strong-line method.Results. From our new observations we find that the oxygen abundance in 61 out of the 66 H ii regions of our sample ranges from 12 + log O/H = 7.05 to 8.22. Our sample includes 27 new galaxies with 12 + log O/H < 7.6 which qualify as extremely metal-poor star-forming galaxies (XBCDs). Among them are 10 H ii regions with 12 + log O/H < 7.3. The new sample is combined with a further 93 low-metallicity galaxies with accurate oxygen abundance determinations from our previous studies, yielding in total a high-quality spectroscopic data set of 154 H ii regions. 9000 more galaxies with oxygen abundances, based mainly on the T e -method, are compiled from the SDSS. Photometric data for all galaxies of our combined sample are taken from the SDSS database while distances are from the NED. Our data set spans a range of 8 mag with respect to its absolute magnitude in SDSS g (-12 > ∼ M g > ∼ −20) and nearly 2 dex in its oxygen abundance (7.0 < ∼ 12 + log O/H < ∼ 8.8), allowing us to probe the L − Z relation in the nearby universe down to the lowest currently studied metallicity level. The L − Z relation established on the basis of the present sample is consistent with previous ones obtained for emission-line galaxies.

show abstract

Section: Luminosity-metallicity Relationcontrasting

confidence: 99%

Section: Luminosity-metallicity Relationmentioning

confidence: 99%

An investigation of the luminosity-metallicity relation for a large sample of low-metallicity emission-line galaxies

Гусева

Papaderos

Meyer

et al. 2009

A&A

103

View full text Add to dashboard Cite

show abstract

“…As proposed by Hidalgo-Gámez & Olofsson (1998) and reviewed by Salzer et al (2005), perhaps NIR magnitudes are more suitable than the optical B-magnitude to built metallicityluminosity diagrams. Indeed, NIR magnitudes are less affected by extinction and more directly related to the stellar mass of the galaxy than the optical luminosities.…”

Section: Metallicity-luminosity Relationsmentioning

confidence: 92%

“…Despite the huge observational effort, the origin of the luminosity-metallicity is still not well understood. The two basic ideas are (i) it represents an evolutionary sequencemore luminous galaxies have processed a larger fraction of their raw materials (McGaugh & deBlok 1997;Bell & deJong 2000;Boselli et al 2001) -or (ii) it is related to a mass-retention sequence -more massive galaxies retain a larger fraction of their processed material (Garnett 2002;Tremonti et al 2004;Salzer et al 2005). Furthermore, other factors may play a key role in the variation of the metal content of a galaxy, remarking the quick metal enrichment that strong star-formation events in dwarf galaxies, such as BCDGs, may experience.…”

Section: Metallicity-luminosity Relationsmentioning

confidence: 99%

“…These analyses have shown a clear correlation between mass and metallicity. In practice, luminosity has been used as substitute of mass because of the difficulty of deriving reliable galaxy masses, yielding to the socalled metallicity-luminosity relation (i.e., Rubin et al 1984;Richer & McCall 1995;Salzer et al 2005), although in recent years mass-metallicity relations are also explored (i.e., Tremonti et al 2004;Kewley & Elisson 2008), and are studied even at high redshifts (i.e., Kobulnicky et al 1999;Pettini et al 2001;Kobulnicky & Kewley 2004;Erb et al 2006;Liang et al 2006). The evolution of such relationships are now predicted by semianalytic models of galaxy formation within the Λ-cold dark matter framework that include chemical hydrodynamic simulations (De Lucia et al 2004;Tissera et al 2005;De Rossi et al 2006;Davé & Oppenheimer 2007).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

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

Five supernova survey galaxies in the southern hemisphere. I. Optical and near-infrared database

et al. 2009

View full text Add to dashboard Cite

The determination of the supernova (SN) rate is based not only on the number of detected events, but also on the properties of the parent galaxy population. This is the first paper of a series aimed at obtaining new, refined, SN rates from a set of five SN surveys, by making use of a joint analysis of near-infrared (NIR) data. We describe the properties of the 3838 galaxies that were monitored for SNe events, including newly determined morphologies and their DENIS and POSS-II/UKST I, 2MASS and DENIS J and K s and 2MASS H magnitudes. We have compared 2MASS, DENIS and POSS-II/UKST IJK magnitudes in order to findpossible systematic photometric shifts in the measurements. The DENIS and POSS-II/UKST I band magnitudes show large discrepancies (mean absolute difference of 0.4 mag), mostly due to different spectral responses of the two instruments, with an important contribution (0.33 mag rms) from the large uncertainties in the photometric calibration of the POSS-II and UKST photographic plates. In the other wavebands, the limiting near infrared magnitude, morphology, and inclination of the galaxies are the most influential factors which affect the determination of photometry of the galaxies. Nevertheless, no significant systematic differences have been found between of any pair of NIR magnitude measurements, except for a few percent of galaxies showing large discrepancies. This allows us to combine DENIS and 2MASS data for the J and K s filters.

show abstract

Metal Abundances of KISS Galaxies. IV. Galaxian Luminosity‐Metallicity Relations in the Optical and Near‐Infrared

Cited by 95 publications

References 52 publications

An investigation of the luminosity-metallicity relation for a large sample of low-metallicity emission-line galaxies

An investigation of the luminosity-metallicity relation for a large sample of low-metallicity emission-line galaxies

Massive star formation in Wolf-Rayet galaxies

Five supernova survey galaxies in the southern hemisphere. I. Optical and near-infrared database

Contact Info

Product

Resources

About