Fig. 7


Rest-frame C III] λλ1907, 1909 EW from MUSE spectroscopy vs. (top) rest-frame [O III] λλ4959,5007 EW and (bottom) the ratio of [O III] to [O II] flux, all from WFC3/G141 grism spectroscopy. Lower limits in the bottom panel are based on the grism flux limit (3σ ~ 3.9 × 10-18 erg s-1 cm-2; Brammer et al. 2013) when [O II] is not detected spectroscopically. A (linear) relation is expected between the EWs of C III] and [O III] since the intense ionizing radiation fields necessary for exciting C III] are also expected to generate the collisional excitations needed for [O III] emission; here we find a linear relation between the rest-frame EWs of [O III] = 47.9 × C III ] + 349. The [O III] to [O II] ratio traces two different ionization levels of the oxygen gas and therefore serves as a measure of the intensity of the radiation field within the galaxy. The dashed line in the bottom panel shows the median ratio of 0.794 from Paalvast et al. (in prep.) for MUSE star-forming galaxies at 0.28 <z< 0.85. The C III] emitters predominantly have higher [O III] to [O II] ratios than the lower-z sample.

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