Open Access

Fig. 14.


Comparison between the clumpiness and the mixed-model attenuation AV, tot toward the center (upper plot), and the equivalent width (EW) of Hα (lower panel) for 21 starbursts in the redshift range 0.5–0.9 analyzed in Calabrò et al. (2019). The corresponding IDs are added to each galaxy, while black crosses indicate X-ray detected sources. The Spearman correlation coefficient R and the corresponding p-value are highlighted in each panel. We derived no correlation for the first diagram and a mild correlation > 3σ for the second, thus only for the latter case is shown the best linear fit (blue line, with equation included the legend) and 1σ dispersion (blue shaded region). However, even in the first plot, the highest clumpiness values are found only for the less attenuated starbursts, while low clumpiness objects are systematically more obscured (AV, tot > 15). Given that AV, tot and EW(Hα) have been used as merger stage indicators in Calabrò et al. (2019), our findings provide an indication for a possible clumpiness evolution, decreasing from early-intermediate phases to late stage mergers. This is corroborated by the subset of X-ray AGNs (likely close to the blow-out phase) showing preferentially a lower clumpiness.

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.