The origin of primary nitrogen in galaxies

Meynet, Georges; Maeder, A.

doi:10.1051/0004-6361:20011554

Cited by 135 publications

(121 citation statements)

References 26 publications

(48 reference statements)

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“…In low-metallicity blue compact galaxies, they argue that the oxygen and nitrogen come from the same massive stars, and there is no delay between the time of the oxygen and ( primary) nitrogen enrichment. Stellar rotation can enable massive stars to synthesize primary N, but Meynet & Maeder (2002a conclude that stellar rotation will actually cause intermediate-mass stars to be the main source of primary nitrogen, in which case there should be a lag between the oxygen enrichment and the nitrogen injection. If rotation is not important, then primary N synthesis can occur when C and O from an Heburning core diffuse into a hydrogen-burning shell, the so-called hot bottom burning; this should also occur mainly in intermediatemass stars (Marigo 2001).…”

Section: Chemical Evolutionmentioning

confidence: 99%

A Near‐Solar Metallicity, Nitrogen‐deficient Lyman Limit Absorber Associated with Two S0 Galaxies

Jenkins

Bowen

Tripp³

et al. 2005

ApJ

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The UV spectrum of the bright quasar PHL 1811 at z em ¼ 0:192 reveals a foreground gas system at z ¼ 0:080923 with log N (H i) ¼ 17:98 AE 0:05. We have determined the abundances of various atomic species in this system from a spectrum covering the wavelength range 1160-1730 8 recorded at 7 km s À1 resolution by the E140M grating of the Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope (HST ), supplemented by coverage at shorter wavelengths by the Far Ultraviolet Spectroscopic Explorer (FUSE ). The abundances of C ii, Si ii, S ii, and Fe ii compared to that of O i indicate that a considerable fraction of the gas is in locations where the hydrogen is ionized. An oxygen abundance ½O/ H ¼ À0:19 AE 0:08 in the H i-bearing gas indicates that the chemical enrichment of the gas is unusually high for an extragalactic QSO absorption system. However, this same material has an unusually low abundance of nitrogen, ½N/ O < À0:59, indicating that there may not have been enough time during this enrichment for secondary nitrogen to arise from low-and intermediate-mass stars. From the convergence of high Lyman series lines we can determine the velocity width of H i, and after correcting for turbulent broadening shown by the O i absorption feature, we derive a temperature T ¼ 7070 þ3860 À4680 K. We determine a lower bound for the electron density n(e) > 10 À3 cm À3 by modeling the ionization by the intergalactic radiation field and an upper bound n(e) < 0:07 cm À3 from the absence of much C ii in an excited fine-structure level. The thermal pressure in the range 4 cm À3 K < p / k < 140 cm À3 K could be confined by a warm-hot intergalactic medium (WHIM) structure with /¯$ 20 that might accompany a wall of galaxies at the same redshift, seen in data from the Sloan Digital Sky Survey. An r-band image of the field surrounding PHL 1811 recorded by the ACS instrument on HST shows that two galaxies at the same redshift as the gas are S0 galaxies, separated by only 34 and 87 h À1 70 kpc from the line of sight. One or both of these galaxies may be the source of the material in the Lyman limit system, which may have been expelled from them in a fast wind, by tidal stripping, or by ram pressure stripping. Subtraction of the ACS point-spread function from the image of the QSO reveals the presence of a face-on spiral galaxy under the glare of the quasar; while it is possible that this galaxy may be responsible for the Lyman limit absorption, the exact alignment of the QSO with the center of the galaxy suggests that the spiral is the quasar host.

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Section: Chemical Evolutionmentioning

confidence: 99%

A Near‐Solar Metallicity, Nitrogen‐deficient Lyman Limit Absorber Associated with Two S0 Galaxies

Jenkins

Bowen

Tripp³

et al. 2005

ApJ

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“…While elements from O up to the Fe-group are produced by supernovae, the main sources of carbon and nitrogen are still being debated. Both elements are believed to originate from a wide range of sources including winds of short-lived massive metal rich stars, longerlived low-and intermediate-mass stars, and also an early generation of massive stars (e.g., Gustafsson et al 1999;Chiappini et al 2003;Meynet and Maeder 2002).…”

Section: Sources Of Metalsmentioning

confidence: 99%

Observations of Metals in the Intra-Cluster Medium

et al. 2008

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Because of their deep gravitational potential wells, clusters of galaxies retain all the metals produced by the stellar populations of the member galaxies. Most of these metals reside in the hot plasma which dominates the baryon content of clusters. This makes them excellent laboratories for the study of the nucleosynthesis and chemical enrichment history of the Universe. Here we review the history, current possibilities and limitations of the abundance studies, and the present observational status of X-ray measurements of the chemical composition of the intra-cluster medium. We summarise the latest progress in using the abundance patterns in clusters to put constraints on theoretical models of supernovae and we show how cluster abundances provide new insights into the star-formation history of the Universe.

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“…At this point we must mention that rotation may be a source of mixing and CN processing (see Meynet & Maeder 2002), and that other non-standard mixing mechanisms have been investigated along the RGB, which may have altered the 12 C/ 13 C ratio and the C/N ratio in CS 22949-037 itself (Charbonnel 1995).…”

Section: Comparison Of the Abundance Pattern Of Cs 22949-037 With Varmentioning

confidence: 99%

First Stars II. Elemental abundances in the extremely metal-poor star CS 22949–037

Depagne¹,

Hill²,

Spite³

et al. 2002

A&A

170

179

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Abstract. CS 22949-037 is one of the most metal-poor giants known ([Fe/H] ≈ −4.0), and it exhibits large overabundances of carbon and nitrogen (Norris et al.). Using VLT-UVES spectra of unprecedented quality, regarding resolution and S /N ratio, covering a wide wavelength range (from λ = 350 to 900 nm), we have determined abundances for 21 elements in this star over a wide range of atomic mass. The major new discovery is an exceptionally large oxygen enhancement, [O/Fe] , we discuss the pairinstability supernovae. Such very massive objects indeed produce large amounts of oxygen, and have been found to be possible sources of primary nitrogen. However, the predicted odd/even effect is too large, and the predicted Zn abundance much too low. Other scenarios are also discussed. In particular, the yields of a recent model (Z35Z) from Heger and Woosley are shown to be in fair agreement with the observations. The only discrepant prediction is the very low abundance of nitrogen, possibly curable by taking into account other effects such as rotationally induced mixing. Alternatively, the absence of lithium in our star, and the values of the isotopic ratios 12 C/ 13 C and 13 C/ 14 N close to the equilibrium value of the CN cycle, suggest that the CNO abundances now observed might have been altered by nuclear processing in the star itself. A 30-40 M supernova, with fallback, seems the most likely progenitor for CS 22949-037. Article published by EDP Sciences and available at

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The origin of primary nitrogen in galaxies

Cited by 135 publications

References 26 publications

A Near‐Solar Metallicity, Nitrogen‐deficient Lyman Limit Absorber Associated with Two S0 Galaxies

A Near‐Solar Metallicity, Nitrogen‐deficient Lyman Limit Absorber Associated with Two S0 Galaxies

Observations of Metals in the Intra-Cluster Medium

First Stars II. Elemental abundances in the extremely metal-poor star CS 22949–037

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