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Linking the structural properties of galaxies and their star formation histories with STAGES

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Figure

Figure 1. Subsample definitions used in this work. This plot shows the(but many ‘disturbed’ objects are not visually classified as mergers, althoughsome of them may be minor and/or advanced mergers
Fig. 2for disturbed galaxies not classified as mergers (blue circles), re-laxed galaxies (small black squares), and visual mergers (red infinity presents the Specific SFR (SSFR; star formation rate per unitstellar mass) as a function of the photometric stellar mass (M∗/M⊙)symbols) in both the cluster and the field for all morphological types.
Figure 3. Specificcircles (pluses (and the red histogram the visual mergers. The SSFR histogram excludes objects with only SFR upper or lower limits
Figure 4. �(W462 − W518) versus stellar mass density � (upper plot in each panel) and stellar mass density histograms (lower plot in each panel) for the fourdifferent morphological types E, S0, Sp, Irr at the cluster redshift
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