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Fig. 5.


A comparison of the derived star formation rate (SFR) from the Hαλ6563, Hβλ4861 and [O II] λ3727 luminosities for the HUDF (top panels, circles) and the HDFS (bottom panels, triangles). Left panels: logarithm of the SFR from Hαλ6563 vs. the difference between the log Hβλ4861 and log Hαλ6563 SFRs. Right panels: same for Hβλ4861 vs. [O II] λ3727. In each panel σ indicates the standard deviation (in dex) around the one-to-one relation. Colour indicates the signal-to-noise ratio (S/N) in the faintest line; Hγλ4340. Only galaxies that allowed for more than one SFR indicator are included in the plot. Overall the SFRs from Hβλ4861 and [O II] λ3727 agree reasonably well, considering we have not taken into account the metallicity dependence in SFR([O II] λ3727). The scatter in Hαλ6563 vs. Hβλ4861 SFR is largely driven by Hγλ4340 S/N.

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