Spectrophotometric properties of galaxies at intermediate redshifts
(<i>z</i> ~ 0.2–1.0)

Lamareille, F.; Contini, T.; Brinchmann, Jarle; Borgne, Jean-François Le; Charlot, S.; Richard, Johan

doi:10.1051/0004-6361:20053602

Cited by 40 publications

(58 citation statements)

References 53 publications

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“…On the contrary, Carollo & Lilly (2001), from emission-line ratios of 15 galaxies in a range of 0.5 < z < 1, found that their metallicities appear to be remarkably similar to those of local galaxies selected with the same criteria. A similar result, consistent with no significant evolution, was found for the luminosity-metallicity relation by Lamareille et al (2006), comparing 131 intermediate redshift star-forming galaxies (0.2 < z < 1, split in 0.2 redshift bins). However, a recent study of Lamareille et al (2009), focussed on the evolution of the M − Z relation up to z ∼ 0.9, suggesting that the M − Z relation is flatter at higher redshifts.…”

Section: Introductionsupporting

confidence: 87%

“…Since then, as luminosities are easier to estimate than masses, many studies have focussed on the L − Z relation (e.g., Skillman et al 1989;Brodie & Huchra 1991;Zaritsky et al 1994;Garnett et al 1997;Lamareille et al 2004Lamareille et al , 2006Maier et al 2004), which correlates the absolute magnitude of galaxies with metallicity, being the more metal rich, the more luminous. The M − Z and L − Z relations have been studied at both, low and high redshift (e.g.…”

Section: Effect Of the Mass And Luminosity-metallicity Relationsmentioning

confidence: 99%

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Study of star-forming galaxies in SDSS up to redshift 0.4

Lara-López

Bongiovanni

Cepa

et al. 2010

A&A

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Context. The chemical composition of the gas in galaxies versus cosmic time provides a very important tool for understanding galaxy evolution. Although there are many studies at high redshift, they are rather scarce at lower redshifts. However, low redshift studies can provide important clues about the evolution of galaxies, furnishing the required link between local and high redshift universe. In this work we focus on the metallicity of the gas of star-forming galaxies at low redshift, looking for signs of chemical evolution. Aims. To analyze the metallicity contents star-forming galaxies of similar luminosities and masses at different redshifts. With this purpose, we present a study of the metallicity of relatively massive (log(M star /M ⊙ ) 10.5) star forming galaxies from SDSS-DR5 (Sloan Digital Sky Survey-Data Release 5), using different redshift intervals from 0.04 to 0.4. Methods. We used data processed with the STARLIGHT spectral synthesis code, correcting the fluxes for dust extinction, estimating metallicities using the R 23 method, and segregating the samples with respect to the value of the [N ii] λ6583/[O ii] λ3727 line ratio in order to break the R 23 degeneracy selecting the upper branch. We analyze the luminosity and mass-metallicity relations, and the effect of the Sloan fiber diameter looking for possible biases. Results. By dividing our redshift samples in intervals of similar magnitude and comparing them, significant signs of metallicity evolution are found. Metallicity correlates inversely with redshift: from redshift 0 to 0.4 a decrement of ∼0.1 dex in 12+log(O/H) is found.

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Section: Introductionsupporting

confidence: 87%

Section: Effect Of the Mass And Luminosity-metallicity Relationsmentioning

confidence: 99%

Study of star-forming galaxies in SDSS up to redshift 0.4

Lara-López

Bongiovanni

Cepa

et al. 2010

A&A

View full text Add to dashboard Cite

show abstract

“…However, the adopted calibration of R 23 is not based on galaxies with direct metallicities but on grids of photoionization models, which may produce a systematic bias. To overcome these differences, we follow Pérez- Montero et al (2013) and convert the metallicities derived from R 23 to those derived from N2 using the linear relations described in Lamareille et al (2006b), which are based on models of Charlot & Longhetti (2001). This way, the adopted estimators find metallicities that are broadly consistent, within the uncertainties, with each other.…”

Section: Metallicity From Strong-line Methodsmentioning

confidence: 99%

Extreme emission-line galaxies out toz~ 1 in zCOSMOS

Amorín

Pérez-Montero

Contini

et al. 2015

A&A

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102

113

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Context. The study of large and representative samples of low-metallicity star-forming galaxies at different cosmic epochs is of great interest to the detailed understanding of the assembly history and evolution of low-mass galaxies. Aims. We present a thorough characterization of a large sample of 183 extreme emission-line galaxies (EELGs) at redshift 0.11 ≤ z ≤ 0.93 selected from the 20k zCOSMOS bright survey because of their unusually large emission line equivalent widths. Methods. We use multiwavelength COSMOS photometry, HST-ACS I-band imaging, and optical zCOSMOS spectroscopy to derive the main global properties of star-forming EELGs, such as sizes, stellar masses, star formation rates (SFR), and reliable oxygen abundances using both "direct" and "strong-line" methods. Results. The EELGs are extremely compact (r 50 ∼ 1.3 kpc), low-mass (M * ∼ 10 7 −10 10 M ) galaxies forming stars at unusually high specific star formation rates (sSFR ≡ SFR/M up to 10 −7 yr −1 ) compared to main sequence star-forming galaxies of the same stellar mass and redshift. At rest-frame UV wavelengths, the EELGs are luminous and show high surface brightness and include strong Lyα emitters, as revealed by GALEX spectroscopy. We show that zCOSMOS EELGs are high-ionization, low-metallicity systems, with median 12+ log(O/H) = 8.16 ± 0.21 (0.2 Z ) including a handful of extremely metal-deficient (<0.1 Z ) EELGs. While ∼80% of the EELGs show non-axisymmetric morphologies, including clumpy and cometary or tadpole galaxies, we find that ∼29% of them show additional low-surface-brightness features, which strongly suggests recent or ongoing interactions. As star-forming dwarfs in the local Universe, EELGs are most often found in relative isolation. While only very few EELGs belong to compact groups, almost one third of them are found in spectroscopically confirmed loose pairs or triplets. Conclusions. The zCOSMOS EELGs are galaxies caught in a transient and probably early period of their evolution, where they are efficiently building up a significant fraction of their present-day stellar mass in an ongoing, galaxy-wide starburst. Therefore, the EELGs constitute an ideal benchmark for comparison studies between low-and high-redshift low-mass star-forming galaxies.

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“…Since then, as luminosities are easier to estimate than masses, many studies have focused on the L − Z relation (e.g., Skillman et al 1989;Brodie & Huchra 1991;Zaritsky et al 1994;Garnett et al 1997;Lamareille et al 2004Lamareille et al , 2006Maier et al 2004), which correlates the absolute magnitude of galaxies with metallicity, the more metal rich being more luminous. The M − Z and L − Z relations have been studied at both low and high redshift (e.g.…”

Section: Effect Of the Mass And Luminosity-metallicity Relationsmentioning

confidence: 99%

Study of star-forming galaxies in SDSS up to redshift 0.4

Lara-López¹,

Cepa

Bongiovanni³

et al. 2009

A&A

View full text Add to dashboard Cite

Context. The chemical composition of the gas in galaxies over cosmic time provides a very important tool for understanding galaxy evolution. Although there are many studies at high redshift, they are rather scarce at lower redshifts. However, low redshift studies can provide important clues about the evolution of galaxies, furnishing the required link between the local and high redshift universe. In this work, we focus on the metallicity of the gas of star-forming galaxies at low redshift, looking for signs of chemical evolution.Aims. We aim to analyze the metallicity contents star-forming galaxies of similar luminosities and masses at different redshifts. With this purpose, we present a study of the metallicity of relatively massive (log(M star /M ) 10.5) star forming galaxies from SDSS-DR5 (Sloan Digital Sky Survey-data release 5), using different redshift intervals from 0.04 to 0.4. Methods. We used data processed with the STARLIGHT spectral synthesis code, correcting the fluxes for dust extinction, estimating metallicities using the R 23 method, and segregating the samples with respect to the value of the [N ii] λ6583/[O ii] λ3727 line ratio in order to break the R 23 degeneracy selecting the upper branch. We analyze the luminosity and mass-metallicity relations, and the effect of the Sloan fiber diameter looking for possible biases. Results. By dividing our redshift samples in intervals of similar magnitude and comparing them, significant signs of metallicity evolution are found. Metallicity correlates inversely with redshift: from redshift 0 to 0.4 a decrement of ∼0.1 dex in 12 + log(O/H) is found.

show abstract

Spectrophotometric properties of galaxies at intermediate redshifts (z ~ 0.2–1.0)

Cited by 40 publications

References 53 publications

Study of star-forming galaxies in SDSS up to redshift 0.4

Study of star-forming galaxies in SDSS up to redshift 0.4

Extreme emission-line galaxies out toz~ 1 in zCOSMOS

Study of star-forming galaxies in SDSS up to redshift 0.4

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