The history of star-forming galaxies in the Sloan Digital Sky Survey

Asari, N. Vale; Fernandes, R. Cid; Stasińska, G.; Torres‐Papaqui, J. P.; Mateus, A.; Sodré, L.; Schoenell, W.; Gomes, J. M.

doi:10.1111/j.1365-2966.2007.12255.x

Cited by 276 publications

(342 citation statements)

References 72 publications

(129 reference statements)

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“…We attempted to reproduce the spectral absorption lines and continua of the sample galaxy spectra to study their stellar populations by using the software STARLIGHT 5 (Cid Fernandes et al 2005, 2007Mateus et al 2006;Asari et al 2007;Chen et al 2009). This is a program that fits an observed spectrum O λ with a model M λ that combines up to N * SSPs with different ages and metallicities from different stellar population synthesis models.…”

Section: Spectral Synthesis Methodsmentioning

confidence: 99%

“…Cid Fernandes and his colleagues have studied the spectral synthesis on the SDSS galaxies by using the BC03 model and their STARLIGHT code. They also measured the properties of the galaxies, such as the dust extinction, stellar mass, SFH (Cid Fernandes et al 2004, 2007Mateus et al 2006;Asari et al 2007Asari et al , 2009Stasińska et al 2008). Koleva et al (2008) compared different models, and found that the Pégase-HR (Le Borgne et al 2004) and Vazdekis/Miles models were in precise agreement, while the BC03 model exhibited biases, which might be due to the poor metallicity coverage of STELIB library causing unreliable results at non-solar metallicities.…”

Section: Introductionmentioning

confidence: 99%

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Comparing six evolutionary population synthesis models by performing spectral synthesis for galaxies

Chen

Liang

Hammer

et al. 2010

A&A

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Aims. We compare six popularly used evolutionary population synthesis (EPS) models by fitting the full optical spectra of six representative types of galaxies (star-forming and composite galaxies, Seyfert 2s, LINERs, E+A, and early-type galaxies) taken from the Sloan Digital Sky Survey (SDSS). We explore the dependence of stellar population synthesis results on the main ingredients of the EPS models and study whether there is an age sequence among these types of galaxies. Methods. We use the simple stellar populations (SSPs) of each EPS model and the software STARLIGHT to perform our fits. Firstly, we explore the dependence of stellar population synthesis on EPS models by fixing the age, metallicity, and initial mass function (IMF) to construct a standard SSP group. We then use the standard SSP group of each EPS model (BC03, CB07, Ma05, GALEV, GRASIL, and Vazdekis/Miles) to fit the spectra of star-forming and E+A galaxies. Secondly, we fix the IMF and alter the age and metallicity to construct eight additional SSP groups. We then use these SSP groups to fit the spectra of star-forming and E+A galaxies to verify the effects of age and metallicity on stellar populations. Finally, we study the effect of stellar evolution tracks and stellar spectral libraries on our results, and present a possible age sequence among these types of galaxies. Results. Using different EPS models, the numerical values of contributing light fractions obviously change, even though the dominant populations are unaltered. The stellar population synthesis does depend on the selection of age and metallicity, but does not depend significantly on the stellar evolution track. The importance of young populations decreases from star-forming, composite, Seyfert 2, LINER, to early-type galaxies, and the properties of E+A galaxies are between composite galaxies and Seyfert 2s in most cases. Conclusions. Different EPS models infer different stellar population parameters, so that it is not reasonable to directly compare stellar populations estimated from different EPS models. To obtain reliable results, we should use the same EPS model to derive the parameter values that we compare.

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Section: Spectral Synthesis Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Comparing six evolutionary population synthesis models by performing spectral synthesis for galaxies

Chen

Liang

Hammer

et al. 2010

A&A

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“…We used the SDSS-DR5 spectra from the STARLIGHT database 1 , which were processed through the STARLIGHT spectral synthesis code, developed by Cid Fernandes and colleagues (Cid Fernandes et al 2005Mateus et al 2006;Asari et al 2007). From them, we obtained the emission lines fluxes measurements of our samples from the contiuum subtracted spectra.…”

Section: Sample Selectionmentioning

confidence: 99%

“…To this aim, our sample is divided in redshift intervals of 0.1 from z ∼ 0 to 0.4. The purpose for selecting small ranges in luminosity is to alleviate the problem of the magnitude completeness, since the Sloan sample is only complete in the magnitude range 14.5 < m r < 17.7 (e.g., Asari et al 2007), and then becomes incomplete at redshift above z > 0.1 (e.g., Kewley et al 2006). However, this procedure limits the study to the more luminous galaxies, since they are the ones detected at any redshift interval.…”

Section: Sample Selectionmentioning

confidence: 99%

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

Lara-López¹,

Cepa

Bongiovanni³

et al. 2009

A&A

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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.

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“…The AGB phase of intermediate mass stars (1 M⊙ 8) and massive stars ( 8M⊙) which end their lives as Type II supernovae (SNe) are considered the dominant source of stellar dust production in star-forming galaxies while dust in the ISM may also form in situ from accretion of enriched gas processed by stars (Dwek 1998). Dust forms from metals and a strong correlation between gas-phase oxygen abundance and dust content is observed in local (Heckman et al 1998;Boissier et al 2004;Asari et al 2007;Garn & Best 2010;Xiao et al 2012;Zahid et al 2012b) and high redshifts galaxies Domínguez et al 2013).…”

Section: Introductionmentioning

confidence: 99%

The slow flow model of dust efflux in local star-forming galaxies

Zahid

Torrey

Kudritzki

et al. 2013

Monthly Notices of the Royal Astronomical Society

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We develop a dust efflux model of radiation pressure acting on dust grains which successfully reproduces the relation between stellar mass, dust opacity and star formation rate observed in local star-forming galaxies. The dust content of local star-forming galaxies is set by the competition between the physical processes of dust production and dust loss in our model. The dust loss rate is proportional to the dust opacity and star formation rate. Observations of the relation between stellar mass and star formation rate at several epochs imply that the majority of local star-forming galaxies are best characterized as having continuous star formation histories. Dust loss is a consequence of sustained interaction of dust with the radiation field generated by continuous star formation. Dust efflux driven by radiation pressure rather than dust destruction offers a more consistent physical interpretation of the dust loss mechanism. By comparing our model results with the observed relation between stellar mass, dust extinction and star formation rate in local star-forming galaxies we are able to constrain the timescale and magnitude of dust loss. The timescale of dust loss is long and therefore dust is effluxed in a "Slow Flow". Dust loss is modest in low mass galaxies but massive galaxies may lose up to 70 ∼ 80% of their dust over their lifetime. Our Slow Flow model shows that mass loss driven by dust opacity and star formation may be an important physical process for understanding normal star-forming galaxy evolution.

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The history of star-forming galaxies in the Sloan Digital Sky Survey

Cited by 276 publications

References 72 publications

Comparing six evolutionary population synthesis models by performing spectral synthesis for galaxies

Comparing six evolutionary population synthesis models by performing spectral synthesis for galaxies

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

The slow flow model of dust efflux in local star-forming galaxies

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