On the Metallicity of Star‐forming Dwarf Galaxies

Legrand, François; Tenorio-Tagle, G.; Silich, S. A.; Kunth, D.; Cerviño, M.

doi:10.1086/322960

Cited by 33 publications

(44 citation statements)

References 28 publications

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“…All data used for this study are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/572/A90 large fraction of the Hubble time, perhaps coupled with an initial phase of vigorous star formation, is a seemingly viable way of explaining the cessation of star-formation activity in galaxies and is invoked by several studies as the primary method of building up stellar mass in galaxies (e.g., Legrand et al 2001;Noeske et al 2007a,b;James et al 2008;Rodighiero et al 2011;Gladders et al 2013;Oesch et al 2013). This scenario is not, however, the only method of transforming the gas-rich galaxies observed in the high-redshift universe (e.g., Daddi et al 2010a) into those whose baryonic component is dominated by their stellar matter.…”

Section: Introductionmentioning

confidence: 99%

Hidden starbursts and active galactic nuclei at 0 < z < 4 from theHerschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback

Lemaux

Floc’h

Fèvre

et al. 2014

A&A

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We investigate of the properties of ∼2000 Herschel/SPIRE far-infrared-selected galaxies from 0 < z < 4 in the CFHTLS-D1 field. Using a combination of extensive spectroscopy from the VVDS and ORELSE surveys, deep multiwavelength imaging from CFHT, VLA, Spitzer, XMM-Newton, and Herschel, and well-calibrated spectral energy distribution fitting, Herschel-bright galaxies are compared to optically-selected galaxies at a variety of redshifts. Herschel-selected galaxies are observed to span a range of stellar masses, colors, and absolute magnitudes equivalent to galaxies undetected in SPIRE. Though many Herschel galaxies appear to be in transition, such galaxies are largely consistent with normal star-forming galaxies when rest-frame colors are utilized. The nature of the star-forming "main sequence" is studied and we warn against adopting this framework unless the main sequence is determined precisely. Herschel galaxies at different total infrared luminosities (L TIR ) are compared. Bluer optical colors, larger nebular extinctions, and larger contributions from younger stellar populations are observed for galaxies with larger L TIR , suggesting that low-L TIR galaxies are undergoing rejuvenated starbursts while galaxies with higher L TIR are forming a larger percentage of their stellar mass. A variety of methods are used to select powerful active galactic nuclei (AGN). Galaxies hosting all types of AGN are observed to be undergoing starbursts more commonly and vigorously than a matched sample of galaxies without powerful AGN and, additionally, the fraction of galaxies with an AGN increases with increasing star formation rate at all redshifts. At all redshifts (0 < z < 4) the most prodigious star-forming galaxies are found to contain the highest fraction of powerful AGN. For redshift bins that allow a comparison (z > 0.5), the highest L TIR galaxies in a given redshift bin are unobserved by SPIRE at subsequently lower redshifts, a trend linked to downsizing. In conjunction with other results, this evidence is used to argue for prevalent AGN-driven quenching in starburst galaxies across cosmic time.

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Section: Introductionmentioning

confidence: 99%

Hidden starbursts and active galactic nuclei at 0 < z < 4 from theHerschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback

Lemaux

Floc’h

Fèvre

et al. 2014

A&A

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“…Many authors (De Young & Heckman 1994;D'Ercole & Brighenti 1999;MacLow & Ferrara 1999) believe that the metals are easily channelled along the funnel created by the galactic wind, so they are ejected outside the galaxy more easily than the pristine gas. Other authors (Silich & Tenorio-Tagle 1998;Legrand et al 2001) have suggested that the metal-rich gas is barely lost from the galaxies, since it is trapped by extended halos surrounding the galaxies, although the existence of such halos is still unproved. Rieschick & Hensler (2000) have suggested that ∼25% of the metals can mix rapidly, remaining trapped in the galaxy, whereas the other 75% of metals undergoes a cycle lasting ∼1 Gyr, in which an outflow is created.…”

Section: Introductionmentioning

confidence: 99%

Continuous star formation in IZw18

Recchi

Matteuccí²,

D’Ercole

et al. 2004

A&A

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Abstract. We study the dynamical and chemical evolution of a galaxy similar to IZw18 under the assumption of a continuous star formation during bursts. We adopt a 2-D hydrocode coupled with detailed chemical yields originating from SNeII, SNeIa and from single intermediate-mass stars. Different nucleosynthetic yields and different IMF slopes are tested. In most of the explored cases, a galactic wind develops, mostly carrying out of the galaxy the metal-enriched gas produced by the burst itself. The chemical species with the largest escape probabilities are Fe and N. Consequently, we predict that the [α/Fe] and [α/N] ratios outside the galaxy are lower than inside. In order to reproduce the chemical composition of IZw18, the best choice seems to be the adoption of the yields of Meynet & Maeder (2002) which take into account stellar rotation, although these authors do not follow the whole evolution of all the stars. Models with a flat IMF (x = 0.5) seem to be able to better reproduce the chemical properties of IZw18, but they inject in the gas a much larger amount of energy and the resulting galactic wind is very strong, at variance with observations. We also predict the evolution of the abundances in the H  medium and compare them with recent FUSE observations.

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“…Kunth & Sargent (1986) point out the self-enrichment of the H II region used for measuring. However, the time-scale for the SN ejecta to cool down and mix is of the order of several hundred Myr (e.g., Legrand et al, 2001) and, thus, longer than the age of the H II regions. This fact eliminates the possibility of self-contamination.…”

Section: Existence Of a Minimum Metallicity For The Star-forming Gasmentioning

confidence: 99%

Gas Accretion and Star Formation Rates

Alméida

2017

Gas Accretion Onto Galaxies

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Cosmological numerical simulations of galaxy evolution show that accretion of metal-poor gas from the cosmic web drives the star formation in galaxy disks. Unfortunately, the observational support for this theoretical prediction is still indirect, and modeling and analysis are required to identify hints as actual signs of star-formation feeding from metal-poor gas accretion. Thus, a meticulous interpretation of the observations is crucial, and this observational review begins with a simple theoretical description of the physical process and the key ingredients it involves, including the properties of the accreted gas and of the star-formation that it induces. A number of observations pointing out the connection between metalpoor gas accretion and star-formation are analyzed, specifically, the short gas consumption time-scale compared to the age of the stellar populations, the fundamental metallicity relationship, the relationship between disk morphology and gas metallicity, the existence of metallicity drops in starbursts of star-forming galaxies, the socalled G dwarf problem, the existence of a minimum metallicity for the star-forming gas in the local universe, the origin of the α-enhanced gas forming stars in the local universe, the metallicity of the quiescent BCDs, and the direct measurements of gas accretion onto galaxies. A final section discusses intrinsic difficulties to obtain direct observational evidence, and points out alternative observational pathways to further consolidate the current ideas.

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On the Metallicity of Star‐forming Dwarf Galaxies

Cited by 33 publications

References 28 publications

Hidden starbursts and active galactic nuclei at 0 < z < 4 from theHerschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback

Hidden starbursts and active galactic nuclei at 0 < z < 4 from theHerschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback

Continuous star formation in IZw18

Gas Accretion and Star Formation Rates

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