RECORD
Search for an intrinsic metallicity spread in old globular clusters of the Large Magellanic Cloud
Astrophysics of Galaxies · Submitted 5 Sep 2018
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim These findings suggest, along with those from ages and light-element abundances, that the LMC GCs studied here are alike to the majority of Galactic GCs.
The compiled record
The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
Open the compiled record
The abstract, sentence by sentence
We report for the first time on the magnitude of the intrinsic [Fe/H] spread among ten old globular clusters (GCs) of the Large Magellanic Cloud (LMC). Such spreads are merely observed in approximately five per cent of the Milky Way GCs and recently gained more attention in theoretical models of GC evolution. We derived metallicities with a typical precision of 0.05 dex < sigma[Fe/H] < 0.20 dex for an average of 14 red giant branch stars per GC from Str\"omgren photometry. The respective, metallicity-sensitive indices have been calibrated to precise and accurate high-dispersion spectroscopy. For all clusters we found null [Fe/H] spreads with a typical uncertainty of 0.04 dex, with the possible exception of NGC1786 that shows an intrinsic dispersion of 0.07+-0.04 dex. The mean, observed standard deviation of the derived metallicities for nearly 40 per cent of our GC sample amounted to smaller than 0.05 dex. At present, we cannot exclude that the remaining GCs also have intrinsic Fe-abundance variations in excess of 0.05 dex, but in order to significantly detect those, the measurement errors on individual [Fe/H]-values would need to be lowered to the 0.03--0.07 dex level. These findings suggest, along with those from ages and light-element abundances, that the LMC GCs studied here are alike to the majority of Galactic GCs.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We report for the first time on the magnitude of the intrinsic [Fe/H] spread among ten old globular clusters (GCs) of the Large Magellanic Cloud (LMC). | contribution 0.99 | 0.94 | 0.10 | asserted 0.99 |
| s1 | Such spreads are merely observed in approximately five per cent of the Milky Way GCs and recently gained more attention in theoretical models of GC evolution. | background 1.00 | 0.04 | 0.03 | asserted 0.99 |
| s2 | We derived metallicities with a typical precision of 0.05 dex < sigma[Fe/H] < 0.20 dex for an average of 14 red giant branch stars per GC from Str\"omgren photometry. | method 0.99 | 0.97 | 0.03 | asserted 1.00 |
| s3 | The respective, metallicity-sensitive indices have been calibrated to precise and accurate high-dispersion spectroscopy. | method 1.00 | 0.53 | 0.02 | asserted 1.00 |
| s4 | For all clusters we found null [Fe/H] spreads with a typical uncertainty of 0.04 dex, with the possible exception of NGC1786 that shows an intrinsic dispersion of 0.07+-0.04 dex. | result 1.00 | 0.97 | 0.77 | asserted 0.94 |
| s5 | The mean, observed standard deviation of the derived metallicities for nearly 40 per cent of our GC sample amounted to smaller than 0.05 dex. | result 1.00 | 0.97 | 0.09 | asserted 1.00 |
| s6 | At present, we cannot exclude that the remaining GCs also have intrinsic Fe-abundance variations in excess of 0.05 dex, but in order to significantly detect those, the measurement errors on individual [Fe/H]-values would need to be lowered to the 0.03--0.07 dex level. | limitation 0.93 | 0.59 | 0.06 | hedged possibility 1.00 |
| s7 | These findings suggest, along with those from ages and light-element abundances, that the LMC GCs studied here are alike to the majority of Galactic GCs. | interpretation 1.00 | 0.39 | 0.74 | hedged possibility 1.00 |
What was examined, and what was not
- arXiv listing abstract v1
- full text
- figures and tables
- references and citing sentences
- relations to other papers
- P abstract
- S sections
- T body sentences
- C citations
- R cross-paper relations
The paper
Original abstract
We report for the first time on the magnitude of the intrinsic [Fe/H] spread among ten old globular clusters (GCs) of the Large Magellanic Cloud (LMC). Such spreads are merely observed in approximately five per cent of the Milky Way GCs and recently gained more attention in theoretical models of GC evolution. We derived metallicities with a typical precision of 0.05 dex < sigma[Fe/H] < 0.20 dex for an average of 14 red giant branch stars per GC from Str\"omgren photometry. The respective, metallicity-sensitive indices have been calibrated to precise and accurate high-dispersion spectroscopy. For all clusters we found null [Fe/H] spreads with a typical uncertainty of 0.04 dex, with the possible exception of NGC1786 that shows an intrinsic dispersion of 0.07+-0.04 dex. The mean, observed standard deviation of the derived metallicities for nearly 40 per cent of our GC sample amounted to smaller than 0.05 dex. At present, we cannot exclude that the remaining GCs also have intrinsic Fe-abundance variations in excess of 0.05 dex, but in order to significantly detect those, the measurement errors on individual [Fe/H]-values would need to be lowered to the 0.03--0.07 dex level. These findings suggest, along with those from ages and light-element abundances, that the LMC GCs studied here are alike to the majority of Galactic GCs.
Human review
How the literature uses it
2 arXiv papers cite this in 2 sentences
Papers citing it · 1 sentence without a confident label
Uses its method or tool 1 paper
-
In order to quantify the intrinsic abundance spread for each element, we follow the probabilistic approach of [ref] .
Chemodynamical evidence of the HR 1614 moving group as a bar resonance · Intrinsic abundance spreads · 1.00
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.