New perspective on the multiple population phenomenon in Galactic globular clusters from a wide-field photometric survey

• DOI: 10.48550/arxiv.2502.02585
• Publication Date: 2025-02-26
• Authors: S. Jang; A. P. Milone; A. F. Marino; M. Tailo; E. Dondoglio; M. V. Legnardi; G. Cordoni; T. Ziliotto; E. P. Lagioia; M. Carlos; A. Mohandasan; E. Bortolan; Y.-W. Lee
• Keywords: Photometry; QB460-466; Population II stars; Astronomi, astrofysik och kosmologi; Astrophysics of Galaxies (astro-ph.GA); Astronomy, Astrophysics and Cosmology; FOS: Physical sciences; Astrophysics; Astrophysics - Astrophysics of Galaxies; Globular star clusters

Abstract Wide-field photometry of Galactic globular clusters (GCs) has been investigated to overcome limitations from the small field of view of the Hubble Space Telescope in the study of multiple populations. In particular, “chromosome maps” (ChMs) built with ground-based photometry were constructed to identify the first- and second-generation (1G and 2G) stars over the wide field of view. The ChMs allow us to derive the fraction of distinct populations in an analyzed field of view. We present here the radial distribution of the 2G fraction in 29 GCs. The distributions show that all the GCs have either a flat distribution or more centrally concentrated 2G stars. Notably, we find that the fraction of 1G stars outside the half-light radius is clearly bifurcated across all mass range. It implies that a group of GCs with lower 1G fractions (hereafter Group II) have efficiently lost their 1G stars in the outermost cluster regions. In fact, in connection with the trends of the radial distribution, most GCs of Group II have spatially mixed populations, while only less massive GCs in Group I (a group with higher 1G fraction) show that feature. Lastly, we investigate links between these two groups and host cluster parameters. We find that most GCs of Group II are distributed along a broader range of galactocentric distances with smaller perigalactic distances < 3.5 kpc. Besides, by using the Gaia data, it is observed that Group II GCs have higher energy on the integrals of motion diagrams than Group I GCs.