Schematic illustration of the scenario proposed in Sect. 4.1.2: the three LTGs in Fig. 5 may be regarded as morphological snapshots in a sequence of increasing bulge stellar mass , age , surface density Σ_⋆,B and ⟨δμ_9G ⟩. The progenitors of high-mass LTGs (e.g., NGC 0776, i.e., systems in the ⟨δμ_9G ⟩ interval iC; ≥−0.5 mag) form in more massive halos and experience the dominant phase of their bulge assembly earlier than 9 Gyr ago (vertical line). Conversely, the precursors of low-⟨δμ_9G⟩ (≤−1.5 mag; i.e., iA) LTGs, such as IC 0776, assemble at a calm pace within lower-mass halos and undergo an overall retarded structural and chemical evolution toward intermediate-⟨δμ_9G⟩ LTGs (iB), such as NGC 0001. Once the bulge has grown to (10;9), AGN-driven feedback initiates a gradual cessation of SF (depicted in red), while the bulge mass may continue increasing through inward stellar migration from the disk and multiple minor dry mergers.