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| Auteurs principaux: | , , , , , , , , , , |
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| Format: | Preprint |
| Publié: |
2024
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| Accès en ligne: | https://arxiv.org/abs/2403.03262 |
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| _version_ | 1866911789987397632 |
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| author | Scalco, M. Gerasimov, R. Bedin, L. R. Vesperini, E. Nardiello, D. Salaris, M. Burgasser, A. Anderson, J. Libralato, M. Bellini, A. Rosati, P. |
| author_facet | Scalco, M. Gerasimov, R. Bedin, L. R. Vesperini, E. Nardiello, D. Salaris, M. Burgasser, A. Anderson, J. Libralato, M. Bellini, A. Rosati, P. |
| contents | We exploit the astro-photometric dataset of the multi-epoch infrared parallel field of a $\textit{Hubble Space Telescope}$ Large Programme aimed at studying the faintest stars of the globular cluster NGC$\,$6752 to determine the luminosity and mass functions of the multiple stellar populations of this cluster. Thanks to the measurement of proper motions and deeper completeness, the results presented in this paper represent a significant improvement over those of previous studies. We successfully derived membership probabilities reaching stars as faint as $m_{\rm F160W} \sim 25$, allowing us to reliably distinguish the three main stellar populations detected within this cluster. We employed a new set of model isochrones that have been individually fit to the colour-magnitude diagram of each population. We present a comprehensive analysis of the luminosity and mass functions for three stellar populations within NGC$\,$6752. Notably, our findings reveal differences in the present-day luminosity and mass functions of first-generation and second-generation stars; these differences are consistent with the manifestation of the effects of dynamical processes acting on populations with different initial spatial distributions. Finally, we publicly release the catalogues with positions, photometry, proper motions, and memberships probabilities, as well as the stacked-image atlases and all newly calculated stellar models. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2403_03262 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The $\textit{HST}$ Large Programme on NGC$\,$6752 -- V. Differences in Luminosity and Mass Functions among Multiple Stellar Populations Scalco, M. Gerasimov, R. Bedin, L. R. Vesperini, E. Nardiello, D. Salaris, M. Burgasser, A. Anderson, J. Libralato, M. Bellini, A. Rosati, P. Solar and Stellar Astrophysics Astrophysics of Galaxies We exploit the astro-photometric dataset of the multi-epoch infrared parallel field of a $\textit{Hubble Space Telescope}$ Large Programme aimed at studying the faintest stars of the globular cluster NGC$\,$6752 to determine the luminosity and mass functions of the multiple stellar populations of this cluster. Thanks to the measurement of proper motions and deeper completeness, the results presented in this paper represent a significant improvement over those of previous studies. We successfully derived membership probabilities reaching stars as faint as $m_{\rm F160W} \sim 25$, allowing us to reliably distinguish the three main stellar populations detected within this cluster. We employed a new set of model isochrones that have been individually fit to the colour-magnitude diagram of each population. We present a comprehensive analysis of the luminosity and mass functions for three stellar populations within NGC$\,$6752. Notably, our findings reveal differences in the present-day luminosity and mass functions of first-generation and second-generation stars; these differences are consistent with the manifestation of the effects of dynamical processes acting on populations with different initial spatial distributions. Finally, we publicly release the catalogues with positions, photometry, proper motions, and memberships probabilities, as well as the stacked-image atlases and all newly calculated stellar models. |
| title | The $\textit{HST}$ Large Programme on NGC$\,$6752 -- V. Differences in Luminosity and Mass Functions among Multiple Stellar Populations |
| topic | Solar and Stellar Astrophysics Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2403.03262 |