The nature of Hβ+[O III] and [O II] emitters to z ∼ 5 with HiZELS: stellar mass functions and the evolution of EWs

December 2016 • 2016MNRAS.463.2363K

Authors • Khostovan, A. A. • Sobral, D. • Mobasher, B. • Smail, I. • Darvish, B. • Nayyeri, H. • Hemmati, S. • Stott, J. P.

Abstract • We investigate the properties of ∼7000 narrow-band selected galaxies with strong Hβ+[O III] and [O II] nebular emission lines from the High-z Emission-Line Survey between z ∼ 0.8 and 5.0. Our sample covers a wide range in stellar mass (M_stellar ∼ 10^7.5-12.0 M_⊙), rest-frame equivalent widths (EW_rest∼10-10⁵ Å), and line luminosities (L_line ∼ 10^40.5-43.2 erg s^-1). We measure the Hβ+[O III]-selected stellar mass functions out to z ∼ 3.5 and find that both M_⋆ and φ_⋆ increases with cosmic time. The [O II]-selected stellar mass functions show a constant M_⋆ ≈ 10^11.6 M_⊙ and a strong, increasing evolution with cosmic time in φ_⋆ in line with Hα studies. We also investigate the evolution of the EW_rest as a function of redshift with a fixed mass range (10^9.5-10.0 M_⊙) and find an increasing trend best represented by (1 + z)^{3.81 ± 0.14} and (1 + z)^{2.72 ± 0.19} up to z ∼ 2 and ∼3 for Hβ+[O III] and [O II] emitters, respectively. This is the first time that the EW_rest evolution has been directly measured for Hβ+[O III] and [O II] emitters up to these redshifts. There is evidence for a slower evolution for z > 2 in the Hβ+[O III] EW_rest and a decreasing trend for z > 3 in the [O II] EW_rest evolution, which would imply low [O II] EW at the highest redshifts and higher [O III]/[O II] line ratios. This suggests that the ionization parameter at higher redshift may be significantly higher than the local Universe. Our results set the stage for future near-IR space-based spectroscopic surveys to test our extrapolated predictions and also produce z > 5 measurements to constrain the high-z end of the EW_rest and [O III]/[O II] evolution.

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Shoubaneh Hemmati

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