| Full text | |
| Author(s): |
Souza, S. O.
[1]
;
Kerber, L. O.
[1, 2]
;
Barbuy, B.
[1]
;
Perez-Villegas, A.
[1]
;
Oliveira, R. A. P.
[1]
;
Nardiello, D.
[3, 4, 5]
Total Authors: 6
|
| Affiliation: | [1] Univ Sao Paulo, IAG, Rua Matao 1226, BR-05508900 Sao Paulo - Brazil
[2] Univ Estadual Santa Cruz, Rodovia Jorge Amado Km 16, BR-45662000 Ilheus, BA - Brazil
[3] Aix Marseille Univ, CNRS, CNES, LAM, Marseille - France
[4] Univ Padua, Dipartimento Fis Astron Galileo Galilei, Vicolo Osservatorio 3, I-35122 Padua - Italy
[5] Ist Nazl Astrofis, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua - Italy
Total Affiliations: 5
|
| Document type: | Journal article |
| Source: | ASTROPHYSICAL JOURNAL; v. 890, n. 1 FEB 10 2020. |
| Web of Science Citations: | 1 |
| Abstract | |
The Bayesian isochrone fitting using the Markov chain Monte Carlo algorithm is applied, to derive the probability distribution of the parameters age, metallicity, reddening, and absolute distance modulus. We introduce the SIRIUS code by means of simulated color-magnitude diagrams (CMDs), including the analysis of multiple stellar populations (MPs). The population tagging is applied from the red giant branch to the bottom of the main sequence. Through sanity checks using synthetic Hubble Space Telescope CMDs of globular clusters we verify the code reliability in the context of simple and MPs. In such tests, the formal uncertainties in age or age difference, metallicity, reddening, and absolute distance modulus can reach 400 Myr, 0.03 dex, 0.01 mag, and 0.03 mag, respectively. We apply the method to analyze NGC 6752, using Dartmouth stellar evolutionary models. Assuming a single stellar population, we derive an age of 13.7 +/- 0.5 Gyr and a distance of d(circle dot) = 4.11 +/- 0.08 kpc, with the latter in agreement within 3 sigma with the inverse Gaia parallax. In the analysis of the MPs, three populations are clearly identified. From the Chromosome Map and UV/Optical two-color diagrams inspection, we found a fraction of stars of 25 +/- 5, 46 +/- 7, and 29 +/- 5%, for the first, second, and third generations, respectively. These fractions are in good agreement with the literature. An age difference of 500 +/- 410 Myr between the first and the third generation is found, with the uncertainty decreasing to 400 Myr when the helium enhancement is taken into account. (AU) | |
| FAPESP's process: | 17/15893-1 - Globular cluster orbits of bulge: the formation and evolution of the Milky Way |
| Grantee: | Maria de Los Angeles Perez Villegas |
| Support Opportunities: | Scholarships in Brazil - Post-Doctoral |
| FAPESP's process: | 18/22044-3 - Bulge globular clusters: relics of the early formation of the galaxy |
| Grantee: | Stefano Oliveira de Souza |
| Support Opportunities: | Scholarships in Brazil - Doctorate (Direct) |
| FAPESP's process: | 18/22181-0 - Age and metallicity gradients of stellar clusters in the Magellanic Bridge |
| Grantee: | Raphael Augusto Pereira de Oliveira |
| Support Opportunities: | Scholarships in Brazil - Doctorate |