Cluster Ages to Reconstruct the Milky Way Assembly (CARMA). III. NGC 288 as the first Splashed globular cluster

Ceccarelli, E, Massari, D, Aguado-Agelet, F, Mucciarelli, A, Cassisi, S, Monelli, M, Pancino, E, Salaris, M ORCID: 0000-0002-2744-1928 and Saracino, S Cluster Ages to Reconstruct the Milky Way Assembly (CARMA). III. NGC 288 as the first Splashed globular cluster. Astronomy & Astrophysics. ISSN 0004-6361 (Accepted)

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Abstract

The system of globular clusters (GCs) in the Milky Way (MW) comprises a mixture of both in situ and accreted clusters. Tracing the origin of GCs provides invaluable insights into the formation history of the MW. However, reconciling diverse strands of evidence is often challenging. A notable example is NGC 288, where despite significant efforts in the literature, the available chronochemodynamical data have yet to provide a definitive conclusion regarding its origin. On the one hand, all post-Gaia dynamical studies indicate an accreted origin for NGC 288, pointing towards its formation taking place in the Gaia-Sausage-Enceladus (GSE)dwarf galaxy. On the other hand, NGC 288 has been found to be 2.5 Gyr older than other GSE GCs at the same metallicity, suggesting a different (and possibly in situ) origin. In this work, we address the unresolved question on the origin of NGC 288 by analysing its chrono-chemical properties in an unprecedentedly homogeneous framework. First, we compared the location of NGC 288 in the age-metallicity plane with that of other two GCs at similar metallicity, namely, NGC 6218 and NGC 6362, whose chemodynamical properties unambiguously identify them as in situ. The age estimates obtained within the homogeneous framework of the CARMA collaboration show that the three clusters are coeval, reinforcing the contrast with the dynamical interpretation. Then, we derived the chemical composition of NGC 288 using UVES-FLAMES at VLT high-resolution spectroscopic archival data and compared the abundances with a sample of in situ and accreted clusters at similar metallicity. We found a consistency with the chemistry of in situ systems, especially in Si, Ti, Zn, and abundance ratios relative to Eu. To reconcile these results with its orbital properties, we propose a scenario where NGC 288 formed in the proto-disc of the MW and was then dynamically heated by the interaction with the GSE merger. This is a fate that resembles that of proto-disc stars undergoing the so-called Splash event. Therefore, NGC 288 demonstrates the importance of a homogeneous chronochemodynamical information in the interpretation of the origin of MW GCs.

Item Type:	Article
Uncontrolled Keywords:	5109 Space Sciences; 51 Physical Sciences
Subjects:	Q Science > QB Astronomy Q Science > QC Physics
Divisions:	Astrophysics Research Institute
Publisher:	EDP Sciences
Date of acceptance:	31 July 2025
Date of first compliant Open Access:	7 November 2025
Date Deposited:	07 Nov 2025 10:09
Last Modified:	07 Nov 2025 10:15
URI:	https://researchonline.ljmu.ac.uk/id/eprint/27517

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