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- W3105873518 abstract "Recent versions of the observed cosmic star-formation history (SFH) have resolved an inconsistency with the stellar mass density history. We show that the revised SFH also scales up the delay-time distribution (DTD) of Type Ia supernovae (SNe Ia), as determined from the observed volumetric SN Ia rate history, aligning it with other field-galaxy SN Ia DTD measurements. The revised-SFH-based DTD has a $t^{-1.1 pm 0.1}$ form and a Hubble-time-integrated production efficiency of $N/M_star=1.3pm0.1$ SNe Ia per $1000~{rm M_odot}$ of formed stellar mass. Using these revised histories and updated empirical iron yields of the various SN types, we re-derive the cosmic iron accumulation history. Core-collapse SNe and SNe Ia have contributed about equally to the total mass of iron in the Universe today. We find the track of the average cosmic gas element in the [$alpha$/Fe] vs. [Fe/H] abundance-ratio plane. The track is broadly similar to the observed main locus of Galactic stars in this plane, indicating a Milky Way (MW) SFH similar in form to the cosmic one. We easily find a simple MW SFH that makes the track closely match this stellar locus. Galaxy clusters appear to have a higher-normalization DTD. This cluster DTD, combined with a short-burst MW SFH peaked at $z=3$, produces a track that matches remarkably well the observed high-$alpha$ locus of MW stars, suggesting the halo/thick-disk population has had a galaxy-cluster-like formation mode. Thus, a simple two-component SFH, combined with empirical DTDs and SN iron yields, suffices to closely reproduce the MW's stellar abundance patterns." @default.
- W3105873518 created "2020-11-23" @default.
- W3105873518 creator A5037085989 @default.
- W3105873518 creator A5080522773 @default.
- W3105873518 date "2017-10-09" @default.
- W3105873518 modified "2023-10-17" @default.
- W3105873518 title "Star Formation, Supernovae, Iron, and<i>α</i>: Consistent Cosmic and Galactic Histories" @default.
- W3105873518 cites W1921554691 @default.
- W3105873518 cites W1934387688 @default.
- W3105873518 cites W1970058472 @default.
- W3105873518 cites W1976129429 @default.
- W3105873518 cites W1980935497 @default.
- W3105873518 cites W2003685212 @default.
- W3105873518 cites W2005549045 @default.
- W3105873518 cites W2031905411 @default.
- W3105873518 cites W2038347333 @default.
- W3105873518 cites W2060449082 @default.
- W3105873518 cites W2061347162 @default.
- W3105873518 cites W2064743375 @default.
- W3105873518 cites W2071751087 @default.
- W3105873518 cites W2073488875 @default.
- W3105873518 cites W2074037441 @default.
- W3105873518 cites W2081661745 @default.
- W3105873518 cites W2089609573 @default.
- W3105873518 cites W2091286481 @default.
- W3105873518 cites W2092131964 @default.
- W3105873518 cites W2092430749 @default.
- W3105873518 cites W2097111096 @default.
- W3105873518 cites W2098830799 @default.
- W3105873518 cites W2103126597 @default.
- W3105873518 cites W2107337450 @default.
- W3105873518 cites W2114095787 @default.
- W3105873518 cites W2118514220 @default.
- W3105873518 cites W2121404382 @default.
- W3105873518 cites W2124199755 @default.
- W3105873518 cites W2126297006 @default.
- W3105873518 cites W2127569230 @default.
- W3105873518 cites W2128806658 @default.
- W3105873518 cites W2129760210 @default.
- W3105873518 cites W2137194113 @default.
- W3105873518 cites W2147875900 @default.
- W3105873518 cites W2156856858 @default.
- W3105873518 cites W2157917411 @default.
- W3105873518 cites W2157990947 @default.
- W3105873518 cites W2161362013 @default.
- W3105873518 cites W2169344843 @default.
- W3105873518 cites W2171695188 @default.
- W3105873518 cites W2253893063 @default.
- W3105873518 cites W2344683712 @default.
- W3105873518 cites W2519754188 @default.
- W3105873518 cites W2544944039 @default.
- W3105873518 cites W2899497983 @default.
- W3105873518 cites W2952751471 @default.
- W3105873518 cites W2997687071 @default.
- W3105873518 cites W3098301582 @default.
- W3105873518 cites W3098603824 @default.
- W3105873518 cites W3098722645 @default.
- W3105873518 cites W3099073446 @default.
- W3105873518 cites W3099716837 @default.
- W3105873518 cites W3099823618 @default.
- W3105873518 cites W3100149672 @default.
- W3105873518 cites W3100158924 @default.
- W3105873518 cites W3100697534 @default.
- W3105873518 cites W3100877462 @default.
- W3105873518 cites W3101511519 @default.
- W3105873518 cites W3101523623 @default.
- W3105873518 cites W3101823643 @default.
- W3105873518 cites W3102457250 @default.
- W3105873518 cites W3102524225 @default.
- W3105873518 cites W3102726682 @default.
- W3105873518 cites W3102918392 @default.
- W3105873518 cites W3103948737 @default.
- W3105873518 cites W3104008351 @default.
- W3105873518 cites W3104728800 @default.
- W3105873518 cites W3104999290 @default.
- W3105873518 cites W3106294757 @default.
- W3105873518 cites W3106351357 @default.
- W3105873518 cites W3121747574 @default.
- W3105873518 cites W3122090959 @default.
- W3105873518 cites W3122457873 @default.
- W3105873518 cites W3124280327 @default.
- W3105873518 cites W3124280501 @default.
- W3105873518 cites W3125844369 @default.
- W3105873518 cites W4289981565 @default.
- W3105873518 cites W4293241594 @default.
- W3105873518 doi "https://doi.org/10.3847/1538-4357/aa8b6e" @default.
- W3105873518 hasPublicationYear "2017" @default.
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