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On ionisation effects and abundance ratios in damped Lyman-alpha systems
Astrophysics · Submitted 7 Sep 2000
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim If taken into account, the element abundance ratios in DLAs are quite consistent with those observed in Milky Way stars and in metal-poor H II regions in blue compact dwarf galaxies.
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The abstract, sentence by sentence
The similarity between observed velocity structures of Al III and singly ionised species in damped Lyman-alpha systems (DLAs) suggests the presence of ionised gas in the regions where most metal absorption lines are formed. To explore the possible implications of ionisation effects we construct a simplified two-region model for DLAs consisting of an ionisation bounded region with an internal radiation field and a neutral region with a lower metal content. Within this framework we find that ionisation effects are important. If taken into account, the element abundance ratios in DLAs are quite consistent with those observed in Milky Way stars and in metal-poor H II regions in blue compact dwarf galaxies. In particular we cannot exclude the same primary N origin in both DLAs and metal-poor galaxies. From our models no dust depletion of heavy elements needs to be invoked; little depletion is however not excluded.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The similarity between observed velocity structures of Al III and singly ionised species in damped Lyman-alpha systems (DLAs) suggests the presence of ionised gas in the regions where most metal absorption lines are formed. | background 0.85 | 0.17 | 0.08 | hedged possibility 1.00 |
| s1 | To explore the possible implications of ionisation effects we construct a simplified two-region model for DLAs consisting of an ionisation bounded region with an internal radiation field and a neutral region with a lower metal content. | method 0.91 | 0.93 | 0.05 | asserted 0.71 |
| s2 | Within this framework we find that ionisation effects are important. | result 0.99 | 0.95 | 0.28 | asserted 1.00 |
| s3 | If taken into account, the element abundance ratios in DLAs are quite consistent with those observed in Milky Way stars and in metal-poor H II regions in blue compact dwarf galaxies. | result 0.80 | 0.85 | 0.49 | hedged possibility 0.76 |
| s4 | In particular we cannot exclude the same primary N origin in both DLAs and metal-poor galaxies. | interpretation 0.78 | 0.77 | 0.14 | hedged possibility 0.99 |
| s5 | From our models no dust depletion of heavy elements needs to be invoked; little depletion is however not excluded. | result 0.89 | 0.89 | 0.09 | asserted 0.61 |
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The paper
Original abstract
The similarity between observed velocity structures of Al III and singly ionised species in damped Lyman-alpha systems (DLAs) suggests the presence of ionised gas in the regions where most metal absorption lines are formed. To explore the possible implications of ionisation effects we construct a simplified two-region model for DLAs consisting of an ionisation bounded region with an internal radiation field and a neutral region with a lower metal content. Within this framework we find that ionisation effects are important. If taken into account, the element abundance ratios in DLAs are quite consistent with those observed in Milky Way stars and in metal-poor H II regions in blue compact dwarf galaxies. In particular we cannot exclude the same primary N origin in both DLAs and metal-poor galaxies. From our models no dust depletion of heavy elements needs to be invoked; little depletion is however not excluded.
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Papers whose main result relates to this one's
States the same result 1 paper
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If these effects are taken into account, the element abundance ratios in DLAs are quite consistent with those observed in Milky Way stars and in H II regions of local low-metallicity blue compact dwarf galaxies.
On ionization effects and abundance ratios in damped Lyman alpha systems · 1.00
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