METALLICITY EVOLUTION OF DAMPED Lyα SYSTEMS OUT TO<i>z</i>∼ 5

Rafelski, Marc; Wolfe, Arthur M.; Prochaska, J. Xavier; Neeleman, Marcel; Mendez, Alexander

doi:10.1088/0004-637x/755/2/89

Cited by 366 publications

(624 citation statements)

References 174 publications

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“…The black contours mark the position of the quasar (labelled "Q") and the continuum-detected galaxy assumed at the DLA redshift (labelled "G"). riched above the median value of log Z/Z ≈ −1.5 for the DLA population at z ≈ 2 − 3 (Rafelski et al 2012). Moreover, the line profiles exhibit a complex kinematic structure with two main velocity components stretching over > 200 km s −1 , placing this DLA in the upper end of the metallicity and kinematics distribution of the DLA population at these redshifts (Ledoux et al 2006;Neeleman et al 2013).…”

Section: Data Acquisition and Reductionmentioning

confidence: 87%

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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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Section: Data Acquisition and Reductionmentioning

confidence: 87%

“…No ionization corrections are included, as they are known to be negligible for DLAs. Similarly, no corrections for dust depletion have been applied, although we note they may be non-negligible given the metallicity of this system (up to ≈ 0.5 dex, but generally 0.2 dex for Si; Rafelski et al 2012;De Cia et al 2016).…”

Section: Data Acquisition and Reductionmentioning

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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“…From 0 < z < 5, the relationship has a slope of −0.2 dex per unit z, a large scatter (±1 dex at a given z), and a lower limit that extends at least to Z /3000 (Rafelski et al 2012(Rafelski et al , 2014Cooke et al 2011b). There are also reports of null detection at high redshift: Z < 10 −4.2 Z at z = 3.4 (Fumagalli et al 2011a, LLS), and Z < 10 −4 Z at z = 7.1 (Simcoe et al 2012, LLS/DLA).…”

Section: The Role Of Mergersmentioning

confidence: 98%

Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

178

130

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Numerical simulations predict that metal-poor gas accretion from the cosmic web fuels the formation of disk galaxies. This paper discusses how cosmic gas accretion controls star formation, and summarizes the physical properties expected for the cosmic gas accreted by galaxies. The paper also collects observational evidence for gas accretion sustaining star formation. It reviews evidence inferred from neutral and ionized hydrogen, as well as from stars. A number of properties characterizing large samples of star-forming galaxies can be explained by metal-poor gas accretion, in particular, the relationship among stellar mass, metallicity, and star-formation rate (the so-called fundamental metallicity relationship). They are put forward and analyzed. Theory predicts gas accretion to be particularly important at high redshift, so indications based on distant objects are reviewed, including the global star-formation history of the universe, and the gas around galaxies as inferred from absorption features in the spectra of background sources.

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“…From this, we could derive that the cloud is located between 230 and 580 pc from the quasar. The metallicity of the cloud, Z = 0.16 Z⊙, is typical of the metallicity of standard intervening DLAs (Rafelski et al 2012).…”

Section: Nature Of the Dlamentioning

confidence: 99%

A coronagraphic absorbing cloud reveals the narrow-line region and extended Lyman α emission of QSO J0823+0529

Fathivavsari

Petitjean

Noterdaeme

et al. 2015

Mon. Not. R. Astron. Soc.

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We report long-slit spectroscopic observations of the quasar SDSS J082303.22+052907.6 (z CIV ∼3.1875), whose Broad Line Region (BLR) is partly eclipsed by a strong damped Lyman-α (DLA; logN (HI)=21.7) cloud. This allows us to study the Narrow Line Region (NLR) of the quasar and the Lyman-α emission from the host galaxy. Using cloudy models that explain the presence of strong NV and PV absorption together with the detection of SiII * and OI * * absorption in the DLA, we show that the density and the distance of the cloud to the quasar are in the ranges 180 < n H < 710 cm −3 and 580 > r 0 >230 pc, respectively. Sizes of the neutral(∼2-9pc) and highly ionized phases (∼3-80pc) are consistent with the partial coverage of the CIV broad line region by the CIV absorption from the DLA (covering factor of ∼0.85). We show that the residuals are consistent with emission from the NLR with CIV/Lyman-α ratios varying from 0 to 0.29 through the profile. Remarkably, we detect extended Lyman-α emission up to 25kpc to the North and West directions and 15kpc to the South and East. We interpret the emission as the superposition of strong emission in the plane of the galaxy up to 10kpc with emission in a wind of projected velocity ∼500km s −1 which is seen up to 25kpc. The low metallicity of the DLA (0.27 solar) argues for at least part of this gas being in-falling towards the AGN and possibly being located where accretion from cold streams ends up.

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METALLICITY EVOLUTION OF DAMPED Lyα SYSTEMS OUT TOz∼ 5

Cited by 366 publications

References 174 publications

Witnessing galaxy assembly in an extended z≈3 structure

Witnessing galaxy assembly in an extended z≈3 structure

Star formation sustained by gas accretion

A coronagraphic absorbing cloud reveals the narrow-line region and extended Lyman α emission of QSO J0823+0529

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