2019
DOI: 10.1093/mnrasl/slz135
View full text |Buy / Rent full text
|
Sign up to set email alerts
|

Abstract: The discovery of star-to-star abundance variations (a.k.a. multiple populations -MPs) within globular clusters (GCs), which are generally not found in the field or in lower mass open clusters, has led to a search for the unique property of GCs that allow them to host this phenomenon. Recent studies have shown that MPs are not limited to the ancient GCs but are also found in massive clusters with ages down to (at least) 2 Gyr. This finding is important for understanding the physics of the MP phenomenon, as thes… Show more

Help me understand this report
View preprint versions

Search citation statements

Order By: Relevance

Paper Sections

Select...
3
1
1

Citation Types

1
21
0

Year Published

2020
2020
2020
2020

Publication Types

Select...
2

Relationship

2
0

Authors

Journals

citations
Cited by 20 publications
(63 citation statements)
references
References 41 publications
(63 reference statements)
1
21
0
Order By: Relevance
“…The use of a different filter does not affect our results (see e.g. Saracino et al 2019Saracino et al , 2020a. We then used the ChM to separate the two populations present in NGC 416 and Lindsay 1.…”
Section: Chromosome Mapmentioning
confidence: 59%
See 3 more Smart Citations
“…The use of a different filter does not affect our results (see e.g. Saracino et al 2019Saracino et al , 2020a. We then used the ChM to separate the two populations present in NGC 416 and Lindsay 1.…”
Section: Chromosome Mapmentioning
confidence: 59%
“…Finally, the local DR δE(B −V) for each individual star is obtained by moving back into the classical m F555W − m F814W vs. m F555W CMD through the same extinction vectors. As stated in Saracino et al (2019), for Lindsay 1 the DR is very low, with a mean δE(B − V) ∼0.003 mag. NGC 416 is affected more strongly by DR (see Niederhofer et al 2017b).…”
Section: Differential Reddeningmentioning
confidence: 72%
See 2 more Smart Citations
“…The upshot is that the observed RGB widths in M19 are determined by a combination of the initial N spreads plus the effect of the dredge up. This is true for any colour or pseudocolour sensitive to the surface N abundance in RGB stars, like C F275W,F336W,F438W ≡ (F275W − F336W) − (F336W − F438W) (see, e.g., Milone et al 2017;Saracino et al 2019 ), devised to detect MPs in GCs and younger MC massive clusters by means of the so-called 'chromosome maps'.…”
Section: Introductionmentioning
confidence: 99%