Differential attenuation in star-forming galaxies at 0.3 ≲ z ≲ 1.5 in the SHARDS/CANDELS

We use a sample of 706 galaxies, selected as [O II]lambda 3727 ([O II]) emitters in the Survey for High-z Absorption Red and Dead Sources SHARDS) on the CANDELS/GOODS-N field, to study the differential attenuation of the nebular emission with respect to the stellar continuum. The sample includes only galaxies with a counterpart in the infrared and log(10) (M-*/M-circle dot) > 9, over the redshift interval 0.3 less than or similar to z less than or similar to 1.5. Our methodology consists in the comparison of the star formation rates inferred from [O II] and Haemission lines with a robust quantification of the total star-forming activity (SFR TOT) that is independently estimated based on both infrared and ultraviolet (UV) luminosities. We obtain f = E(B - V)(stellar)/E(B - V)(nebular) = 0.69(0.69)(0.71) and 0.55(0.53)(0.56) for [O II] and H alpha, respectively. Our resulting f-factors display a significant positive correlation with the UV attenuation and shallower or not-significant trends with the stellar mass, the SFR TOT, the distance to the main sequence, and the redshift. Finally, our results favour an average nebular attenuation curve similar in shape to the typical dust curve of local starbursts.

Automated summary

The research uses a sample of 706 galaxies to study the differential attenuation of the nebular emission, finding a significant positive correlation with UV attenuation and weaker associations with other factors.