LSD: Lyman-break galaxies Stellar populations and Dynamics - I. Mass, metallicity and gas at<i>z</i>∼ 3.1

Mannucci, F.; Cresci, G.; Maiolino, R.; Marconi, A.; Pastorini, Guia; Pozzetti, L.; Gnerucci, Alessio; Risaliti, G.; Schneider, Raffaella; Lehnert, M. D.; Salvati, M.

doi:10.1111/j.1365-2966.2009.15185.x

Cited by 381 publications

(535 citation statements)

References 116 publications

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“…Fig. 15 shows the result for GRB hosts with z > 4 compared to two other samples for field galaxies of z ∼ 2.3 (Erb et al, 2006) and z ∼ 3.1 (Mannucci et al, 2009). GRB 050904 at z = 6.29 with our corrected metallicity and GRB 060223A clearly lie below the galaxies at z ∼ 3.1 while the other four hosts, including GRB 100219A, are consistent with the relation at lower redshifts.…”

Section: The Mass-metallicity Relation At High Redshiftssupporting

confidence: 67%

“…It has become clear that the M-Z relation at increasing redshift changes towards lower metallicities for a given stellar mass (Kewley & Ellison, 2008;Savaglio et al, 2005;Erb et al, 2006;Mannucci et al, 2009). This effect is largely due to the enrichment with metals over time but the metal enrichment of galaxies is also a complex function of star-formation efficiency and feedback with the intergalactic medium.…”

Section: The Mass-metallicity Relation At High Redshiftsmentioning

confidence: 99%

“…Luminosity-metallicity relation of z > 4 GRBs compared to field galaxy samples at slightly lower redshifts. Galaxy data are from Erb et al (2006) for z ∼ 2.3 and from Mannucci et al (2009) for z ∼ 3.1. Salvaterra et al (2011) studied the redshift evolution of the mass-metallicity relation from redshift 5 to 10 using galaxy evolution simulations with the GADGET code (Springel, 2005).…”

Section: The Mass-metallicity Relation At High Redshiftsmentioning

confidence: 99%

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GRB 100219A with X-shooter – abundances in a galaxy at z =4.7

Thöne¹,

Fynbo²,

Goldoni³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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Context. Abundances of galaxies at redshifts z > 4 are difficult to obtain from damped Ly α (DLA) systems in the sightlines of quasars (QSOs) due to the Ly α forest blanketing and the low number of high-redshift quasars detected. Gamma-ray bursts (GRBs) with their higher luminosity are well suited to study galaxies out to the formation of the first stars at z > 10. Its large wavelength coverage makes the X-shooter spectrograph an excellent tool to study the interstellar medium (ISM) of high redshift galaxies, in particular if the redshift is not known beforehand. Aims. We want to determine the properties of a GRB host at z = 4.66723 from absorption lines. This is one of the highest redshifts where a detailed analysis with medium-resolution data is possible. Furthermore, we determine the dust extinction using the spectral energy distribution from X-rays to near infrared. Finally, we put the results in context to other GRBs at z > 4 and properties of (high redshift) QSO absorbers. Methods. The velocity components of the resonant and fine-structure absorption lines are fitted with Voigt-profiles and the metallicity determined from S, Si, Fe and O. Si II* together with the energy released in the UV restframe as determined from GROND photometric data gives us the distance of the absorbing material from the GRB. The extinction is determined from the spectral slope using X-ray spectral information and the flux calibrated X-shooter spectrum, cross calibrated with photometric data from GROND. We also collect information on all GRB hosts with z > 4. Results. We measure a relatively high metallicity of [M/H] = −1.0 ± 0.1 from S, the distance of the material showing fine-structure lines is 0.3 to 1.0 kpc. The extinction is moderate with A V = 0.24 ± 0.06 mag. Low-and high ionization as well as fine-structure lines show a complicated kinematic structure probably pointing to a merger in progress. We detect one intervening system at z = 2.18. Conclusions. GRB-DLAs have a shallower evolution of metallicity with redshift than QSO absorbers and no evolution in their HI column density or ionization fraction. GRB hosts at high redshift seem to continue the trend of the metallicity-luminosity relation towards lower metallicities but the sample is still too small to draw a definite conclusion. While the detection of GRBs at z > 4 with current satellites is still difficult, they are very important for our understanding of the early epochs of star-and galaxy-formation in the Universe.

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Section: The Mass-metallicity Relation At High Redshiftssupporting

confidence: 67%

Section: The Mass-metallicity Relation At High Redshiftsmentioning

confidence: 99%

Section: The Mass-metallicity Relation At High Redshiftsmentioning

confidence: 99%

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GRB 100219A with X-shooter – abundances in a galaxy at z =4.7

Thöne¹,

Fynbo²,

Goldoni³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…Schaye et al 2003;Fumagalli et al 2016b). Indeed, a ≈ 10%-solar metallicity resembles the metal content of the interstellar medium of ≈ 10 8.5 − 10 9 M galaxies according to the z ≈ 3 mass-metallicity relation (Mannucci et al 2009). In addition to tidal interactions, galactic outflows are also a plausible mechanism to enrich Figure 7.…”

Section: Contribution From In Situ Star Formationmentioning

confidence: 99%

Witnessing galaxy assembly in an extended z≈3 structure

Fumagalli

Mackenzie

Trayford

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present new observations acquired with the Multi Unit Spectroscopic Explorer instrument on the Very Large Telescope in a quasar field that hosts a high columndensity damped Lyα absorber (DLA) at z ≈ 3.25. We detect Lyα emission from a nebula at the redshift of the DLA with line luminosity (27 ± 1) × 10 41 erg s −1 , which extends over 37±1 kpc above a surface brightness limit of 6×10 −19 erg s −1 cm −2 arcsec −2 at a projected distance of 30.5±0.5 kpc from the quasar sightline. Two clumps lie inside this nebula, both with Lyα rest-frame equivalent width > 50 Å and with relative lineof-sight velocities aligned with two main absorption components seen in the DLA spectrum. In addition, we identify a compact galaxy at a projected distance of 19.1 ± 0.5 kpc from the quasar sightline. The galaxy spectrum is noisy but consistent with that of a star-forming galaxy at the DLA redshift. We argue that the Lyα nebula is ionized by radiation from star formation inside the two clumps, or by radiation from the compact galaxy. In either case, these data imply the presence of a structure with size 50 kpc inside which galaxies are assembling, a picture consistent with galaxy formation in groups and filaments as predicted by cosmological simulations such as the eagle simulations.

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“…The heavy element content of star-forming galaxies is characterized by a strong relation between the stellar mass and average gas-phase oxygen abundance (Lequeux et al 1979;Tremonti et al 2004). This so-called mass-metallicity relation (MZR) extends to low stellar mass galaxies (∼ 10 7 M⊙ Lee et al 2006;Zahid et al 2012a;Berg et al 2012) and is observed at intermediate (Savaglio et al 2005;Cowie & Barger 2008;Zahid et al 2011;Moustakas et al 2011;Zahid et al 2013a) and high redshifts (Erb et al 2006;Mannucci et al 2009;Laskar et al 2011). The metallicity at all stellar masses increases with time and the high mass end of the relation flattens at late times as galaxies enrich to an empirical upper limit in the gas-phase abundance (Zahid et al 2013a).…”

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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LSD: Lyman-break galaxies Stellar populations and Dynamics - I. Mass, metallicity and gas atz∼ 3.1

Cited by 381 publications

References 116 publications

GRB 100219A with X-shooter – abundances in a galaxy at z =4.7

GRB 100219A with X-shooter – abundances in a galaxy at z =4.7

Witnessing galaxy assembly in an extended z≈3 structure

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

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