Carbon in Field F and G Disk Dwarfs

Tomkin, J.; Woolf, Vincent M.; Lambert, David L.; Lemke, Michael

doi:10.1086/117446

Cited by 48 publications

(42 citation statements)

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“…Abundance studies of carbon (e.g. Tomkin et al 1995) Measures of C and O in DLASs are generally complicated by the fact that often the only available lines are C  λ 1334 and O  λ 1302 which most of the times are heavily saturated. In the DLAS described in Sect.…”

Section: Comments On the Measures Of [O/fe] And [C/fe]mentioning

confidence: 99%

High matter density peaks from UVES observations of QSO pairs: Correlation properties and chemical abundances

D’Odorico

Petitjean

Cristiani

2002

A&A

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Abstract. We study the transverse clustering properties of high matter density peaks as traced by high column density absorption systems (either Lyman limit systems characterized by N(H ) ≥ 2 × 10 17 cm −2 or C  systems with W r > 0.5 Å) at redshifts between 2 and 3 with UVES spectra of two QSO pairs (UM680/UM681 at 56 arcsec angular separation and Q2344+1228/Q2343+1232 at 5 arcmin angular separation) and a QSO triplet (Q2139-4433/Q2139-4434/Q2138-4427 at 1, 7 and 8 arcmin angular separation). We find 3 damped Lyman-α systems (N(H ) ≥ 2 × 10 20 cm −2 ): 2 coinciding with strong metal systems in the nearby line of sight and 1 matching the emission redshift of the paired QSO; plus 7 Lyman limit systems: 4 forming two matching couples and 3 without a corresponding metal system within ∼3000 km s −1 in the coupled line of sight. In summary, we detect five out of ten matching systems within 1000 km s −1 , indicating a highly significant overdensity of strong absorption systems over separation lengths from ∼1 to 8 h −1 Mpc. The observed coincidences could arise in gas due to starburst-driven superwinds associated with a quasar or a galaxy, or gas belonging to large scale structures like filaments or sheets. We also determine chemical abundance ratios for three damped Lyman-α systems. In particular, for the damped system at z ∼ 2.53788 in the spectrum of Q2344+1228, new estimates of the ratios O/Fe, C/Fe are obtained: −0.02 < [C/Fe] < 0.06, −0.06 < [O/Fe] < 0.2. They indicate that O and C are not over-solar in this system.

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Section: Comments On the Measures Of [O/fe] And [C/fe]mentioning

confidence: 99%

High matter density peaks from UVES observations of QSO pairs: Correlation properties and chemical abundances

D’Odorico

Petitjean

Cristiani

2002

A&A

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“…Their results showed that the C abundances are +0.2 higher than those derived from the CH lines. Andersson & Edvardsson (1994) Tomkin et al (1995) (using C i 7100Å) and Gustafsson et al (1999) Carretta et al (2000) analyzed a sample of 19 stars, and reanalyzed the stars of Tomkin et al (1992) and Edvardsson et al (1993). Their results showed that [C/Fe] is roughly solar in the whole metallicity range of [Fe/H] > −2.5.…”

Section: [C/fe] Vs [Fe/h]mentioning

confidence: 99%

Sources of carbon and the evolution of the abundance of CNO elements

Liang

Zhao

Shi

2001

A&A

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Abstract.Using the standard infall model of Galactic chemical evolution, we explore the origin of carbon and calculate the abundance evolution of CNO elements for 8 different models of stellar nucleosynthesis yields. The results show that, in the early stage of the Galaxy, massive stars are the main producer of carbon, and that as our Galaxy evolves to the late stage, the longer lived intermediate-and low-mass stars play an increasingly important role, while at the same time, metal-rich Wolf-Rayet stars eject a significant amount of carbon into the ISM by radiative-driven stellar winds. However, from the present published nucleosynthesis yields we cannot distinguish whether the main source of carbon in the late Galactic stage is just the massive stars

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“…The abundance results combined with accurate velocity data enabled a detailed study of the chemical evolution of kinematically distinct populations. Extensions of this study were made by Tomkin et al (1995) and Woolf et al (1995) who measured carbon and europium abundances, respectively, for about half of the stars in the Edvardsson et al (1993a) sample.…”

Section: Introductionmentioning

confidence: 83%