tokens: The real-time duration of the video is 9 s. (An animation of this figure is available.) The first column of Figure 2 presents the evolution of the photospheric continuum I c . We can observe that this expanding structure begins to form a central dark spot (Δ t = 252 s), which eventually grows in size while the EG splits into two smaller granules (Δ t = 504 s). Then, the southernmost descendant granule located at undergoes the same evolution (Δ t = 756 s), until it splits into four granules (Δ t = 1008 s). The second column of Figure 2 shows the integrated signal of V measured . The emerging flux region first appears at Δ t = 0 s, being located at [5′′, 4′′]. Magnetic field patches with apparent opposite polarity appear close to each other. These magnetic patches expand and occupy the EG area (Δ t = 252 s), showing a pattern of alternate polarities (salt-and-pepper or sea-serpent configuration). Some of these flux kernels intensify: notably, this occurs in the region where the first dark spot is forming (Δ t = 504 s). Later, this structure becomes an intergranular lane (Δ t = 756 s). Doppler velocity maps, displayed in Figure 2 (third column), highlight the plasma motions in the region. They indicate that the structure is generally characterized by conspicuous blueshifts, corresponding to upflows up to 1–1.5 km s −1 . In the central dark patch, downflows of ≃0.5 km s −1 are found (Δ t = 504 s and, partly, at Δ t = 1008 s), in agreement with previous observations. The same coherent behavior is also visible in the online movie. The maps of magnetic flux density (Figure 2 , fourth column) reveal that the distribution of the magnetic areas derived from V integrated is representative of the real magnetic flux patches. Indeed, a mixture of polarities is found where V integrated maps show an apparent salt-and-pepper configuration, suggesting once again that the quantity described in Equation ( 3 ) is a good qualitative proxy for the longitudinal component of the magnetic field, . The evolution of magnetic flux density qualitatively follows that of V integrated , as mentioned above. A polarimetric analysis of the dead-calm region (see Martínez González et al. 2012b ) in FoV QS , used as a control box for comparison, is presented in Figure 3 . This region of very quiet Sun entered the IMaX FoV after the first 200 s of the EG evolution. In Figure 3 (top panels) we present the maps of the integrated signal of V measured , at the same representative times shown for FoV EG in Figure 2 (second column). No new magnetic structures are seen to emerge during the analyzed time series. Figure 3 (bottom panel) shows a plot of the mean polarization signal averaged over FoV EG (black symbols) within the region of interest occupied by the EG inside FoV EG (red symbols), and over FoV QS (empty circles), along the sequence. The signal in FoV EG is on average 2.7 times stronger than in FoV QS . Moreover, the polarization signal in FoV QS remains almost constant during the
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