| Title: |
KMHK 1762: Another star cluster in the Large Magellanic Cloud age gap |
| Authors: |
M. Gatto; V. Ripepi; M. Bellazzini; M. Tosi; C. Tortora; M. Cignoni; M. Dall???Ora; M. -R. L. Cioni; F. Cusano; G. Longo; M. Marconi; I. Musella; P. Schipani; M. Spavone |
| Contributors: |
Gatto, M.; Ripepi, V.; Bellazzini, M.; Tosi, M.; Tortora, C.; Cignoni, M.; Dall???ora, M.; Cioni, M. -R. L.; Cusano, F.; Longo, G.; Marconi, M.; Musella, I.; Schipani, P.; Spavone, M. |
| Publication Year: |
2022 |
| Collection: |
IRIS Università degli Studi di Napoli Federico II |
| Subject Terms: |
Magellanic Cloud; galaxies: star clusters; general; galaxies: star clusters: individual; KMHK 1762; Hertzsprung-Russell and C-M diagrams stars; kinematics and dynamics; Astrophysics; Astrophysics of Galaxies; Solar and Stellar Astrophysics |
| Description: |
Context. The star cluster (SC) age distribution of the Large Magellanic Cloud (LMC) exhibits a gap from ∼4 to 10 Gyr ago, with an almost total absence of SCs. Within this age gap, only two confirmed SCs have been identified hitherto. Nonetheless, the star field counterpart does not show the same characteristics, making the LMC a peculiar galaxy where the star formation history and cluster formation history appear to differ significantly. Aims: We re-analysed the colour-magnitude diagram (CMD) of the KMHK 1762 SC by using the deep optical photometry provided by the `Yes, Magellanic Clouds Again' survey, so as to robustly assess its age. Methods: First, we partially removed foreground and/or field stars by means of parallaxes and proper motions obtained from the Gaia Early Data Release 3. Then, we applied the Automated Stellar Cluster Analysis package to the cleaned photometric catalogue to identify the isochrone that best matches the CMD of KMHK 1762. Results: The estimated age of KMHK 1762 is log(t)=9.74 ± 0.15 dex (∼5.5 Gyr), which is more than 2 Gyr older than the previous estimation which was obtained with shallower photometry. This value makes KMHK 1762 the third confirmed age-gap SC of the LMC. Conclusions: The physical existence of a quiescent period of the LMC SC formation is questioned. We suggest it can be the re |
| Document Type: |
article in journal/newspaper |
| Language: |
English |
| Relation: |
info:eu-repo/semantics/altIdentifier/wos/WOS:000841821100005; volume:664; firstpage:12; lastpage:17; numberofpages:6; journal:ASTRONOMY & ASTROPHYSICS; https://hdl.handle.net/11588/909070 |
| DOI: |
10.1051/0004-6361/202243993 |
| Availability: |
https://hdl.handle.net/11588/909070; https://doi.org/10.1051/0004-6361/202243993 |
| Rights: |
info:eu-repo/semantics/openAccess ; license:Copyright dell'editore ; license uri:publisher |
| Accession Number: |
edsbas.1DCEE615 |
| Database: |
BASE |