indicating that its stars are not chemically homogeneous.

   $m_{\rm F160W}$ bin   $N$   $f_{\rm MS-A}$    $\sigma_{\rm MS-A}$   $f_{\rm MS-B}$    $\sigma_{\rm MS-B}$   $f_{\rm MS-C}$    $\sigma_{\rm MS-C}$
  --------------------- ----- ----------------- --------------------- ----------------- --------------------- ----------------- ---------------------
       21.25-21.75       248   0.276$\pm$0.028          0.060          0.486$\pm$0.032          0.155          0.238$\pm$0.027          0.065
       20.75-21.25       280   0.255$\pm$0.026          0.052          0.464$\pm$0.030          0.140          0.281$\pm$0.027          0.061
       20.25-20.75       296   0.243$\pm$0.026          0.051          0.467$\pm$0.029          0.132          0.290$\pm$0.027          0.060
       19.75-20.25       341   0.265$\pm$0.024          0.042          0.476$\pm$0.028          0.142          0.259$\pm$0.024          0.063
       19.25-19.75       256   0.274$\pm$0.029          0.056          0.452$\pm$0.031          0.156          0.274$\pm$0.029          0.076

\
\[tab:data\]

The radial distribution of multiple populations
-----------------------------------------------

In past years, the multiple populations of NGC6752 have been investigated at different radial distances from the cluster center. Milone et al.(2013, 2017) identified the three main populations of NGC6752 within six arcmin from the cluster center and found that populations A, B and C comprise about 25%, 45% and 30% of the total number of cluster stars. Nardiello et al.(2015) extended the investigation at larger radial distances and concluded that the MS-A hosts 26$\pm$4% of the total number of MS stars in the region between $\sim$5.9 and 17.9 arcmin from the cluster center. Both papers by Milone et al.(2013) and Nardiello et al.(2015) conclude that there is no evidence for any radial gradient of the different stellar populations. 