Hostname: page-component-78c5997874-dh8gc Total loading time: 0 Render date: 2024-11-10T16:03:32.987Z Has data issue: false hasContentIssue false
  • English
  • Français

What the JWST can tell us about the Origin of Multiple Stellar Populations in Globular Clusters

Published online by Cambridge University Press:  13 February 2024

Anna F. Marino Open the ORCID record for Anna F. Marino [Opens in a new window]
Anna F. Marino*
Affiliation:
Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, Padova, IT-35122 Istituto Nazionale di Astrofisica - Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi, 5, Firenze, IT-50125.
*
email: anna.marino@inaf.it
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

I present the first results of multiple stellar populations in globular clusters from James Webb Space Telescope (JWST) data. We obtained combined NIRSpec and NIRCam data of the GC 47 Tucanae to investigate the properties of the different stellar populations in the low-mass regime, down to ∼0.5 M⊙. Our analysis of both the photometric data and the spectra suggests that the multiple stellar populations among M dwarfs share similar properties of those extensively studied on bright red giant branch stars. The comparison between stellar populations’ properties at different stellar mass, e.g. at the red giants and M dwarfs’ phases, can potentially provide strong constraints to the formation scenarios of the still eluding phenomenon of the multiple populations in star clusters.

Keywords

globular clusters: generalstars: population IIstars: abundancestechniques: photometrytechniques: spectroscopy
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S377: Early Disk-Galaxy Formation from JWST to the Milky Way , December 2022 , pp. 65 - 74
Check for updates
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Baraffe, I., Homeier, D., Allard, F., et al. 2015, A&A, 577, A42. doi: 10.1051/0004-6361/201425481 Google Scholar
Bastian, N., Lamers, H. J. G. L. M., de Mink, S. E., et al. 2013, MNRAS, 436, 2398. doi: 10.1093/mnras/stt1745 CrossRefGoogle Scholar
Carretta, E., Bragaglia, A., Gratton, R. G., et al. 2009, A&A, 505, 117. doi: 10.1051/0004-6361/200912096 Google Scholar
D’Antona, F. & Mazzitelli, I. 1994, ApJ, 90, 467. doi: 10.1086/191867 Google Scholar
Decressin, T., Meynet, G., Charbonnel, C., et al. 2007, A&A, 464, 1029. doi: 10.1051/0004-6361:20066013 Google Scholar
de Mink, S. E., Pols, O. R., Langer, N., et al. 2009, A&A, 507, L1. doi: 10.1051/0004-6361/200913205 Google Scholar
Denissenkov, P. A. & Hartwick, F. D. A. 2014, MNRAS, 437, L21. doi: 10.1093/mnrasl/slt133 CrossRefGoogle Scholar
Dondoglio, E., Milone, A. P., Renzini, A., et al. 2022, ApJ, 927, 207. doi: 10.3847/1538-4357/ac5046 CrossRefGoogle Scholar
Dotter, A., Chaboyer, B., Jevremović, D., et al. 2008, ApJS, 178, 89. doi: 10.1086/589654 CrossRefGoogle Scholar
Dotter, A., Ferguson, J. W., Conroy, C., et al. 2015, MNRAS, 446, 1641. doi: 10.1093/mnras/stu2170 CrossRefGoogle Scholar
Gieles, M., Charbonnel, C., Krause, M. G. H., et al. 2018, MNRAS, 478, 2461. doi: 10.1093/mnras/sty1059 CrossRefGoogle Scholar
Legnardi, M. V., Milone, A. P., Armillotta, L., et al. 2022, mnras, 513, 735. doi: 10.1093/mnras/stac734 CrossRefGoogle Scholar
Marino, A. F., Milone, A. P., Renzini, A., et al. 2019a, MNRAS, 487, 3815. doi: 10.1093/mnras/stz1415 CrossRefGoogle Scholar
Marino, A. F., Milone, A. P., Sills, A., et al. 2019b, ApJ, 887, 91. doi: 10.3847/1538-4357/ab53d9 CrossRefGoogle Scholar
Marino, A. F., et al. 2023a, in preparationGoogle Scholar
Marino, A. F., et al. 2023b, in preparationGoogle Scholar
Milone, A. P., Marino, A. F., Cassisi, S., et al. 2012, ApJL, 754, L34. doi: 10.1088/2041-8205/754/2/L34 CrossRefGoogle Scholar
Milone, A. P., Marino, A. F., Bedin, L. R., et al. 2014, MNRAS, 439, 1588. doi: 10.1093/mnras/stu030 CrossRefGoogle Scholar
Milone, A. P., Marino, A. F., Piotto, G., et al. 2015, ApJ, 808, 51. doi: 10.1088/0004-637X/808/1/51 CrossRefGoogle Scholar
Milone, A. P., Piotto, G., Renzini, A., et al. 2017, MNRAS, 464, 3636 CrossRefGoogle Scholar
Milone, A. P., Marino, A. F., Bedin, L. R., et al. 2019, MNRAS, 484, 4046. doi: 10.1093/mnras/stz277 CrossRefGoogle Scholar
Milone, A. P., Marino, A. F., Dotter, A., et al. 2023, arXiv:2301.10889. doi: 10.48550/arXiv.2301.10889 CrossRefGoogle Scholar
Milone, A. P. & Marino, A. F. 2022, Universe, 8, 359. doi: 10.3390/universe8070359 CrossRefGoogle Scholar
Renzini, A., D’Antona, F., Cassisi, S., et al. 2015, MNRAS, 454, 4197. doi: 10.1093/mnras/stv2268 CrossRefGoogle Scholar
Renzini, A., Marino, A. F., & Milone, A. P. 2022, MNRAS, 513, 2111. doi: 10.1093/mnras/stac973 CrossRefGoogle Scholar
Ventura, P. & D’Antona, F. 2009, A&A, 499, 835. doi: 10.1051/0004-6361/200811139 Google Scholar