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Fehrenbach, Lenka; Oldenziel, Ruth; Heymann, Matthias; Rieger, Bernhard; Höhler, Sabine; Zeller, Thomas; Gugerli, David; Kohlrausch, Martin; Weber, Heike; Heßler, Martina; Trischler, Helmuth; Laak, Dirk van

doi:10.30965/9783657703081

Cited by 1 publication

(1 citation statement)

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“…In this context, it should be noticed that in clusters with very high radial velocities the H-α line is redshifted to the edge or even outside the passband of the F656N filter. For this reason, we can not exlude that the small fraction of Be stars with excess in the F656N band in NGC 1805 is due to its radial velocity of ∼ +390 km s −1 (Fehrenbach 1974). The oldest cluster analyzed in this section, NGC 1856, seems to host a smaller fraction of emitting stars than the other GCs.…”

Section: Stars With H-α Emissionmentioning

confidence: 81%

Multiple stellar populations in Magellanic Cloud clusters – VI. A survey of multiple sequences and Be stars in young clusters

Milone

Marino

Criscienzo

et al. 2018

Monthly Notices of the Royal Astronomical Society

110

184

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The split main sequences (MSs) and extended MS turnoffs (eMSTOs) detected in a few young clusters have demonstrated that these stellar systems host multiple populations differing in a number of properties such as rotation and, possibly, age.We analyze Hubble Space Telescope photometry for thirteen clusters with ages between ∼40 and ∼1000 Myrs and of different masses. Our goal is to investigate for the first time the occurrence of multiple populations in a large sample of young clusters.We find that all the clusters exhibit the eMSTO phenomenon and that MS stars more massive than ∼1.6 M ⊙ define a blue and red MS, with the latter hosting the majority of MS stars. The comparison between the observations and isochrones suggests that the blue MSs are made of slow-rotating stars, while the red MSs host stars with rotational velocities close to the breakup value.About half of the bright MS stars in the youngest clusters are H-alpha emitters. These Be stars populate the red MS and the reddest part of the eMSTO thus supporting the idea that the red MS is made of fast rotators.We conclude that the split MS and the eMSTO are a common feature of young clusters in both Magellanic Clouds. The phenomena of a split MS and an eMSTO occur for stars that are more massive than a specific threshold which is independent of the host-cluster mass.As a by-product, we report the serendipitous discovery of a young SMC cluster, GAL-FOR1.

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Section: Stars With H-α Emissionmentioning

confidence: 81%