The study of the 'chromosome maps' of Galactic globular clusters has shown that the stars identified as 'first generation' often define an extended sequence in the mF275W. mF814W colour, whose straightforward interpretation, by comparison with synthetic spectra, is that they are inhomogeneous in helium content. The cluster M3 (NGC 5272) is one of the most prominent example of this phenomenon, since its first generation is distributed on an extended colour range, formally corresponding to a large helium enhancement (~0.1). It is necessary to ask whether the bulk of photometric observations available for this cluster supports or falsifies this interpretation. For this purpose, we examine the horizontal branch morphology, the period and magnitude distributions of the RR Lyrae variables, and the main sequence colour distribution. Simulating the first generation stars with such internal variation of helium content we cannot meet all the observational constraints at the same time, concluding that the origin of the first generation colour spread is still without a straightforward explanation.

Is helium the key parameter in the extended colour spread of the first generation stars in M3?

Tailo M.;D'Antona F.;Milone A. P.;Marino A. F.;Lagioia E.;Cordoni G.
2019

Abstract

The study of the 'chromosome maps' of Galactic globular clusters has shown that the stars identified as 'first generation' often define an extended sequence in the mF275W. mF814W colour, whose straightforward interpretation, by comparison with synthetic spectra, is that they are inhomogeneous in helium content. The cluster M3 (NGC 5272) is one of the most prominent example of this phenomenon, since its first generation is distributed on an extended colour range, formally corresponding to a large helium enhancement (~0.1). It is necessary to ask whether the bulk of photometric observations available for this cluster supports or falsifies this interpretation. For this purpose, we examine the horizontal branch morphology, the period and magnitude distributions of the RR Lyrae variables, and the main sequence colour distribution. Simulating the first generation stars with such internal variation of helium content we cannot meet all the observational constraints at the same time, concluding that the origin of the first generation colour spread is still without a straightforward explanation.
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11577/3325249
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