Reconciling the Metallicity Distributions of Gamma‐Ray Burst, Damped Lyα, and Lyman Break Galaxies at<i>z</i>≈ 3

Fynbo, J. P. U.; Prochaska, J. Xavier; Sommer–Larsen, Jesper; Dessauges‐Zavadsky, M.; Møller, P.

doi:10.1086/589555

Cited by 167 publications

(246 citation statements)

References 91 publications

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“…On the other hand, emission selected galaxies will naturally be drawn mostly from the bright end. Fynbo et al (2008) show that QSO-DLAs as well as GRB host galaxies, which are referred to as GRB-DLAs when observed in absorption, are consistent with being drawn from the same population as Lyman-break galaxies (LBGs), which are UV-selected star-forming galaxies.…”

Section: Galaxy Counterparts Of Metal-rich Dlas 2739mentioning

confidence: 60%

“…This study reports on an ongoing observational survey with the Xshooter spectrograph on the European Southern Observatory (ESO) Very Large Telescope (VLT) with the aim to identify and study DLA counterparts by their emission lines, and also to test observationally the hypothesis in Fynbo et al (2008) that DLAs and LBGs are drawn from the same parent population. Earlier successes within this campaign are presented in Fynbo et al (2010Fynbo et al ( , 2011Fynbo et al ( , 2013, and are summarized in Section 5 together with detections of DLAassociated emission from other campaigns.…”

Section: Galaxy Counterparts Of Metal-rich Dlas 2739mentioning

confidence: 99%

“…The choice for this triangulation strategy is based on the model described in Fynbo et al (2008), and is aimed at optimizing the probability to detect the emission of the galaxy that is producing the DLA. According to this model, a DLA with a metallicity of >0.1 solar at z ∼ 2.2 has an ∼90 per cent probability to be detected in at least one of the slits in our configuration (see Fynbo et al 2008Fynbo et al , 2010 for details and an application to a similar case). Furthermore, the QSOs are exposed for a total of three hours, resulting in high-signal-to-noise spectra with clear absorption lines at intermediate resolution (see Fig.…”

Section: S T R At E G Y a N D O B S E Rvat I O N Smentioning

confidence: 99%

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Galaxy counterparts of metal-rich damped Lyα absorbers: the case of J205922.4−052842★

Hartoog

Fynbo

Kaper

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Disclaimer/Complaints regulationsIf you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: http://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. ABSTRACTWe present observations of three new sources in the European Southern Observatory VLT/Xshooter survey dedicated to the detection of the emitting counterparts of damped Lyα (DLA) systems towards bright quasars (QSOs). The aim is to bridge the observational gap between absorption (i.e. DLAs) and emission-selected galaxies at z ∼ 2.2-2.5, in order to get a more complete picture of (proto)galaxies around this epoch. The hypothesis is that because DLA galaxies fulfil metallicity-velocity width and luminosity-metallicity relations, highmetallicity DLAs are more likely to be detected in emission. The region around each QSO is covered with slits (1. We conclude that focusing on metal-rich DLAs is a good way to find counterparts, but the non-detections at high metallicity (e.g. that of the DLA in J105744.5+062914) show that there is not a one-to-one relationship, and cautions us to not naively apply the properties of the DLA counterparts to all metal-rich DLAs.

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Section: Galaxy Counterparts Of Metal-rich Dlas 2739mentioning

confidence: 60%

Section: Galaxy Counterparts Of Metal-rich Dlas 2739mentioning

confidence: 99%

Section: S T R At E G Y a N D O B S E Rvat I O N Smentioning

confidence: 99%

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Galaxy counterparts of metal-rich damped Lyα absorbers: the case of J205922.4−052842★

Hartoog

Fynbo

Kaper

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…The correlations between metallicity and other fundamental galaxy properties such as stellar mass, luminosity, and star formation rate are crucial to understanding galaxy populations at both low and high redshifts (e.g., Tremonti et al 2004;Savaglio et al 2005;Maiolino et al 2008;Mannucci et al 2010), including DLA galaxies (e.g., Ledoux et al 2006;Fynbo et al 2008;Pontzen et al 2008;Prochaska, Hennawi, & Herbert-Fort 2008;Krogager et al 2012;Møller et al 2013). Møller et al (2013) analyze the redshift evolution of the mass-metallicity relation in a sample of 110 DLAs and report a formula (Equation 6) for estimating stellar mass given metallicity and redshift.…”

Section: Mass-metallicity Relationmentioning

confidence: 99%

Quasar 2175 Å dust absorbers – II. Correlation analysis and relationship with other absorption line systems

Prochaska

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the cold neutral content (H i and C i gas) of 13 quasar 2175Å dust absorbers (2DAs) at z = 1.6 -2.5 to investigate the correlation between the presence of the UV extinction bump with other physical characteristics. These 2DAs were initially selected from the Sloan Digital Sky Surveys I -III and followed up with the Keck-II telescope and the Multiple Mirror Telescope as detailed in our Paper I. We perform a correlation analysis between metallicity, redshift, depletion level, velocity width, and explore relationships between 2DAs and other absorption line systems. The 2DAs on average have higher metallicity, higher depletion levels, and larger velocity widths than Damped Lyman-α absorbers (DLAs) or subDLAs. The correlation between [Zn/H] and [Fe/Zn] or [Zn/H] and log∆V 90 can be used as alternative stellar mass estimators based on the well-established mass-metallicity relation. The estimated stellar masses of the 2DAs in this sample are in the range of ∼ 10 9 to ∼2 × 10 11 M ⊙ with a median value of ∼2 × 10 10 M ⊙ . The relationship with other quasar absorption line systems can be described as (1) 2DAs are a subset of Mg ii and Fe ii absorbers, (2) 2DAs are preferentially metal-strong DLAs/subDLAs, (3) More importantly, all of the 2DAs show C i detections with logN(C i) > 14.0 cm −2 , (4) 2DAs can be used as molecular gas tracers. Their host galaxies are likely to be chemically enriched, evolved, massive (more massive than typical DLA/subDLA galaxies), and presumably star-forming galaxies.

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“…We note that the metallicity of the GRB host galaxies are also studied via absorption lines in the GRB afterglow spectra (e.g., Fynbo et al 2008;Savaglio et al 2009;Cucchiara et al 2014), and high metallicities are found in some cases (e.g., Savaglio et al 2012). However, the absorption line study would give the metallicity averaged over the line-of-sight in the host galaxy, and its relation with the metallicity in the immediate environment of a GRB is not understood well.…”

Section: Implications For Grb/cc Sn Site Studiesmentioning

confidence: 95%

Metallicity measurements of gamma-ray burst and supernova explosion sites: lessons from H ii regions in M31

Niino

Nagamine

Zhang

2015

Monthly Notices of the Royal Astronomical Society

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We examine how the small-scale (< kpc) variation of metallicity within a galaxy, which is found in nearby galaxies, affect the observational estimates of metallicity in the explosion sites of transient events such as core-collapse supernovae (CC SNe) and gamma-ray bursts (GRBs). Assuming the same luminosity, metallicity, and spatial distributions of H ii regions (hereafter HIIRs) as observed in M31, we compute the apparent metallicities that we would obtain when the spectrum of a target region is blended with those of surrounding HIIRs within the length scale of typical spatial resolution. When the spatial resolution of spectroscopy is ∼ < 0.5 kpc, which is typical for the existing studies of CC SN sites, we find that the apparent metallicities reflect the metallicities of target regions, but with significant systematic uncertainties in some cases. When the spatial resolution is ∼ > 1.0 kpc, regardless of the target regions (which has a wide range of metallicity that spans ∼ 0.6 dex for the M31 HIIRs), we always obtain the apparent metallicities similar to the average metallicity of the M31 HIIRs. Given that the apparent metallicities measured with ∼ > kpc scale resolution do not necessarily reflect the immediate environment of the stellar explosions, the current observational estimates of high metallicities for some of the long GRB host galaxies do not rule out the hypothesis that the long GRBs are exclusively born in a low-metallicity environment.

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Reconciling the Metallicity Distributions of Gamma‐Ray Burst, Damped Lyα, and Lyman Break Galaxies atz≈ 3

Cited by 167 publications

References 91 publications

Galaxy counterparts of metal-rich damped Lyα absorbers: the case of J205922.4−052842★

Galaxy counterparts of metal-rich damped Lyα absorbers: the case of J205922.4−052842★

Quasar 2175 Å dust absorbers – II. Correlation analysis and relationship with other absorption line systems

Metallicity measurements of gamma-ray burst and supernova explosion sites: lessons from H ii regions in M31

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