The connection between X-ray binaries and star clusters in NGC 4490 and NGC 4395

In this study, the possible relationship between X-ray Binary (XRB) systems and star clusters in the galaxies NGC 4490 and NGC 4395 was investigated using archival data from X-ray (Chandra) and optical (HST) observatories. Star clusters with high stellar densities are considered to be ideal regions for the formation of XRBs. Some XRBs exhibit spatial correlations with star clusters, while others do not, suggesting that these sources may have been dynamically ejected from their parent clusters after formation.From the Chandra data, While 84 XRBs were detected in NGC 4490, this was 19 in NGC 4395. By applying astrometric corrections, optical counterparts were identified for 11 out of 33 XRBs in NGC 4490 and for one out of five XRBs in NGC 4395. These sources were classified as high-mass XRBs (HMXBs) and intermediate-mass XRBs (IMXBs), respectively. The sources that could not be identified optically were classified as low-mass XRBs (LMXBs). Also, using HST data, 728 and 233 compact star clusters were identified in NGC 4490 and NGC 4395, respectively. The age and mass values of these clusters were obtained by applying the most appropriate SSP models to the constructed color-color diagrams. It was determined that in NGC 4490 and NGC 4395, predominantly HMXBs are associated with young (<108 Myr) star clusters, while LMXBs are associated with older (>108 Myr) star clusters. Our findings support the relationship between different types of XRBs and cluster ages found in other galaxies in the literature. Keywords: Galaxies, Compact Star Clusters, X-ray Binaries