Behaviour of age and [(Si+Ca)/Fe] as a function of [Fe/H] (upper and lower panel, respectively) for the MW in situ GCs (grey diamonds), for G-E (green diamonds), and for NGC 121 (red square). For MW GCs, the ages are from VandenBerg et al. (2013). The chemical abundances are from the MW control sample of this study and from Marino et al. (2011, 2015, 2021), Carretta et al. (2013, 2014), Muñoz et al. (2013), Koch & McWilliam (2014), San Roman et al. (2015), Johnson et al. (2016), Rojas-Arriagada et al. (2016), Villanova et al. (2016), Massari et al. (2017), Mura-Guzmán et al. (2018), Masseron et al. (2019), and Koch-Hansen et al. (2021). Dynamical associations of the GCs are from Massari et al. (2019). In the lower panel, [(Si+Ca)/Fe] from the APOGEE results from the 17th Data Release of the Sloan Digital Sky Survey (Abdurro’uf et al. 2022) are shown for the sake of comparison, and consider MW giant stars within 2 kpc (grey points) and G-E stars (light green circles) selected according to Hasselquist et al. (2021).