UVES Observations of QSO 0000−2620: Oxygen and Zinc Abundances in the Damped Lyα Galaxy at<i>z</i><sub>abs</sub> = 3.3901

Molaro, P.; Bonifacio, P.; Centurión, M.; D’Odorico, S.; Vladilo, G.; Santin, P.; Marcantonio, P. Di

doi:10.1086/309439

Cited by 97 publications

(105 citation statements)

References 36 publications

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“…It is interesting to compare our estimates of the metal abundances in I Zw 18 with those of two well-studied high redshift DLAs: the z = 3.390 DLA towards Q0000-2620 where [Fe/H] −2 and [α-chain/iron-peak] 0.20 were measured by Molaro et al (2000Molaro et al ( , 2001, and the z = 3.386 DLA towards Q0201+1120 with [Fe/H] −1.4 and [α-chain/iron-peak] 0.16 deduced by Ellison et al (2001). Both high-z DLAs do not show a pronounced enhancement of the α-elements as compared with I Zw 18.…”

Section: Discussionmentioning

confidence: 99%

“…The low [α-chain/iron-peak] ratios in metal-poor DLAs have been interpreted as evidence for low or episodic star formation in these galaxies, -there should be sufficient time since the last burst of star formation to accumulate iron in the ISM to a near-solar value relative to α-elements (e.g. Pettini et al 2000;Centurión et al 2000;Molaro et al 2000).…”

Section: Discussionmentioning

confidence: 99%

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Argon, silicon and iron abundances in the damped Ly-αsystem I Zw 18

Levshakov¹,

Kegel²,

Agafonova³

2001

A&A

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Abstract. We show how the ratio of the abundances of Ar, Si and Fe as derived from FUSE absorption spectra of I Zw 18 are affected by large-scale stochastic velocity fields (mesoturbulence). 21-cm observations with high spatial resolution show the presence of velocity fields with large correlation lengths. FUSE observations were performed with a large entrance aperture which fully covered the galaxy. This means that the observed profiles are averaged over the full body of I Zw 18. Taking this into account, we show that the observations are consistent with the abundance ratios [α-chain/Fe] being similar to those derived from Galactic metal-poor stars. Using a mesoturbulent approach, we found that the observed profiles can be reproduced well with IntroductionThe blue compact galaxy (BCG) I Zw 18 (Mrk 116) has been an intensively studied object for the last three decades since the first spectroscopic observations by Zwicky (1966). I Zw 18 shows a powerful and recent burst of star formation which makes this galaxy an attractive target for studies of the history of star formation. The neutral gas in I Zw 18 has been observed in the 21-cm line (see van Zee et al. 1998 and references cited therein) as well as in several UV lines (Kunth et al. 1994;Pettini & Lipman 1995;Vidal-Madjar et al. 2000). High velocity and high spatial resolution radio observations have shown that the overall kinematics of the H i gas associated with I Zw 18 is very complex and that the neutral gas velocity dispersion σ equals 13-14 km s −1 , or b ≡ √ 2σ = 18-20 km s −1 (van Zee et al. 1998). The H i column density in front of the bright star clusters in I Zw 18 deduced from the Ly-α absorption profile by Kunth et al., N H i = (3.5 ± 0.5) × 10 21 cm −2 , is comparable to the peak H i surface density found by van Zee et al., N H i 3.0 × 10 21 cm −2 . This high value is such that the neutral gas in I Zw 18 can be considered as a local damped Ly-α system (DLA), similar to high-redshift DLAs observed in the light of many background quasars.The first HST measurement of the (O/H) abundance in the H i region has indicated a possible discrepancy between the metal content in the neutral gas and in the H ii regions (Kunth et al. 1994). This, however, was not confirmed in later studies by Pettini & Lipman (1995) and by van Zee et al. (1998) who have shown that both the neutral and ionized gas in I Zw 18 may have the same oxygen abundance.Article published by EDP Sciences and available at http://www.aanda.org or http://dx

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Argon, silicon and iron abundances in the damped Ly-αsystem I Zw 18

Levshakov¹,

Kegel²,

Agafonova³

2001

A&A

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“…Other cases of DLAs with small dust content are reported in Molaro et al (2000), in Pettini et al (2000), and in Prochaska & Wolfe (1999). -199.…”

Section: <1455mentioning

confidence: 95%

Metal abundances and ionization conditions in a possibly dust-free damped Lyα system at $\mathsf{\vec{z}=2.3}$

López

Reimers

D’Odorico³

et al. 2002

A&A

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Abstract.We have obtained a high resolution, high S/N UVES spectrum of the bright QSO HE 2243−6031 to analyze the damped Lyα system (DLA) observed at z = 2.33. We measure column densities for H i, 86. All of these ratios support an environment that is in an early evolutionary stage, where the onset of star formation has begun only shortly before the DLA was observed. We also perform a cloud-by-cloud analysis -without precedent at high redshift -and find a tight correlation of all low-ionization species with respect to Fe ii extending over 2.5 orders of magnitude in N(Fe ii). We interpret this trend as being due to homogeneous physical conditions (very mild ionization effects, common dust-destruction histories, same chemical composition) and propose that this line-of-sight encounters absorbing clouds that share a common environment. In addition, photoionization models show that these single clouds are shielded from the external ionizing radiation, so the fraction of ionized gas is small and, except for argon, does not influence the measured metal abundances. The observed Al iii/low-ion ratios suggest the mildly ionized gas occurs in shells surrounding neutral cores of Al ii.

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“…In DLA systems supersolar [Zn/Fe] ratios have often been observed, but they have been explained by assuming that dust depletion is larger for Fe than for Zn (e.g., Lu et al 1996 ;Pettini et al 1999 ;Prochaska & Wolfe 1999 ;Molaro et al 2000 ;Hou, Boissier, & Prantzos 2001). However, recent observations (Primas et al 2000 ;Blake et al 2001) suggest that the assumption [Zn/Fe] \ 0 may not always be correct.…”

Section: Introductionmentioning

confidence: 99%

Nucleosynthesis of Zinc and Iron Peak Elements in Population III Type II Supernovae: Comparison with Abundances of Very Metal Poor Halo Stars

Umeda

Nomoto

2002

ApJ

540

636

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We calculate nucleosynthesis in core collapse explosions of massive Population III stars and compare the results with abundances of metal-poor halo stars to constrain the parameters of Population III supernovae. We focus on iron peak elements, and, in particular, we try to reproduce the large [Zn/Fe] ] D 0.5. The observed trends of the abundance ratios among the M _ ) iron peak elements are better explained with this high-energy ("" hypernova ÏÏ) model than with the simple "" deep ÏÏ mass cut e †ect because the overabundance of Ni can be avoided in the hypernova models. We also present the yields of pair instability supernova explosions of M^130È300 stars and discuss M _ that the abundance features of very metal-poor stars cannot be explained by pair instability supernovae.

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UVES Observations of QSO 0000−2620: Oxygen and Zinc Abundances in the Damped Lyα Galaxy atz_abs = 3.3901

Cited by 97 publications

References 36 publications

Argon, silicon and iron abundances in the damped Ly-αsystem I Zw 18

Argon, silicon and iron abundances in the damped Ly-αsystem I Zw 18

Metal abundances and ionization conditions in a possibly dust-free damped Lyα system at $\mathsf{\vec{z}=2.3}$

Nucleosynthesis of Zinc and Iron Peak Elements in Population III Type II Supernovae: Comparison with Abundances of Very Metal Poor Halo Stars

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UVES Observations of QSO 0000−2620: Oxygen and Zinc Abundances in the Damped Lyα Galaxy atzabs = 3.3901

Cited by 97 publications

References 36 publications

Argon, silicon and iron abundances in the damped Ly-αsystem I Zw 18

Argon, silicon and iron abundances in the damped Ly-αsystem I Zw 18

Metal abundances and ionization conditions in a possibly dust-free damped Lyα system at $\mathsf{\vec{z}=2.3}$

Nucleosynthesis of Zinc and Iron Peak Elements in Population III Type II Supernovae: Comparison with Abundances of Very Metal Poor Halo Stars

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UVES Observations of QSO 0000−2620: Oxygen and Zinc Abundances in the Damped Lyα Galaxy atz_abs = 3.3901