Constraints on the early Universe star formation efficiency from galaxy clustering and halo modeling of Hα and [O III] emitters

Open Access

Fig. 6.

Relationship of M_UV − M_h (or UVHMR) for the redshift bins of our three line emitter samples. The solid lines and bold envelopes mark the M_UV range that we probe with the 2PCF, while the transparent envelopes mark the range probed by the UVLF. We compare with the model by Mason et al. (2015, 2023) that includes dust attenuation in dashed lines and the observational measurements from Harikane et al. (2022) in dots.

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