Multiple Stellar Populations in Metal-poor Globular Clusters with JWST: A NIRCam View of M92

Recent work on metal-intermediate globular clusters (GCs) with [Fe/H] = -1.5 and -0.75 has illustrated the theoretical behavior of multiple populations in photometric diagrams obtained with the JWST. These results are confirmed by observations of multiple populations among the M dwarfs of 47 Tucanae. Here we explore multiple populations in metal-poor GCs with [Fe/H] = -2.3. We take advantage of synthetic spectra and isochrones that account for the chemical composition of multiple populations to identify photometric diagrams that separate the distinct stellar populations of GCs. We derive high-precision photometry and proper motion for main-sequence (MS) stars in the metal-poor GC M92 from JWST and Hubble Space Telescope images. We identify a first-generation (1G) and two main groups of second-generation (2G(A) and 2G(B)) stars and investigate their kinematics and chemical composition. We find isotropic motions with no differences among the distinct populations. The comparison between the observed colors of the M92 stars and the colors derived by synthetic spectra reveals that the helium abundances of 2G(A) and 2G(B) stars are higher than those of the 1G by & UDelta;Y & SIM; 0.01 and 0.04, respectively. The m (F090W) versus m (F090W) - m (F277W) color-magnitude diagram shows that below the knee MS stars exhibit a wide color broadening due to multiple populations. We constrain the amount of oxygen variation needed to reproduce the observed MS width, which is consistent with results on red giant branch stars. We conclude that multiple populations with masses of & SIM;0.1-0.8 M (& ODOT;) share similar chemical compositions.

Automated summary

Recent studies have shown the theoretical behavior of multiple populations in metal-intermediate globular clusters using the JWST. These findings are supported by observations of multiple populations in M dwarfs. In this study, the authors explore multiple populations in metal-poor GCs and identify distinct stellar populations using synthetic spectra and isochrones. The researchers find that the helium abundances of second-generation stars are higher than those of the first generation, and that the color-magnitude diagram shows a wide color broadening due to multiple populations.