article published yes Jorryt J Matthee author 7439a258-f3c0-11ec-9501-9df22fe067200000-0003-2871-127X David Sobral author Philip Best author Ian Smail author Fuyan Bian author Behnam Darvish author Huub Röttgering author Xiaohui Fan author We present a sample of ∼1000 emission-line galaxies at z = 0.4–4.7 from the ∼0.7deg2 High-z Emission-Line Survey in the Boötes field identified with a suite of six narrow-band filters at ≈0.4–2.1 μm. These galaxies have been selected on their Ly α (73), [O II] (285), H β/[O III] (387) or H α (362) emission line, and have been classified with optical to near-infrared colours. A subsample of 98 sources have reliable redshifts from multiple narrow-band (e.g. [O II]–H α) detections and/or spectroscopy. In this survey paper, we present the observations, selection and catalogues of emitters. We measure number densities of Ly α, [O II], H β/[O III] and H α and confirm strong luminosity evolution in star-forming galaxies from z ∼ 0.4 to ∼5, in agreement with previous results. To demonstrate the usefulness of dual-line emitters, we use the sample of dual [O II]–H α emitters to measure the observed [O II]/H α ratio at z = 1.47. The observed [O II]/H α ratio increases significantly from 0.40 ± 0.01 at z = 0.1 to 0.52 ± 0.05 at z = 1.47, which we attribute to either decreasing dust attenuation with redshift, or due to a bias in the (typically) fibre measurements in the local Universe that only measure the central kpc regions. At the bright end, we find that both the H α and Ly α number densities at z ≈ 2.2 deviate significantly from a Schechter form, following a power law. We show that this is driven entirely by an increasing X-ray/active galactic nucleus fraction with line luminosity, which reaches ≈100 per cent at line luminosities L ≳ 3 × 1044 erg s−1. Oxford University Press2017 eng Space and Planetary ScienceAstronomy and Astrophysics galaxiesactivegalaxiesevolutiongalaxieshigh-redshiftgalaxiesluminosity functionmass functiongalaxies: star formation 0035-8711 1365-2966 1702.0472110.1093/mnras/stx1569 4711629-649 yes J. J. Matthee <i>et al.</i>, “Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 1. Oxford University Press, pp. 629–649, 2017. Matthee JJ, Sobral D, Best P, et al. Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(1):629-649. doi:<a href="https://doi.org/10.1093/mnras/stx1569">10.1093/mnras/stx1569</a> Matthee, Jorryt J, David Sobral, Philip Best, Ian Smail, Fuyan Bian, Behnam Darvish, Huub Röttgering, and Xiaohui Fan. “Boötes-HiZELS: An Optical to near-Infrared Survey of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx1569">https://doi.org/10.1093/mnras/stx1569</a>. Matthee JJ, Sobral D, Best P, Smail I, Bian F, Darvish B, Röttgering H, Fan X. 2017. Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. Monthly Notices of the Royal Astronomical Society. 471(1), 629–649. Matthee, J. J., Sobral, D., Best, P., Smail, I., Bian, F., Darvish, B., … Fan, X. (2017). Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx1569">https://doi.org/10.1093/mnras/stx1569</a> J.J. Matthee, D. Sobral, P. Best, I. Smail, F. Bian, B. Darvish, H. Röttgering, X. Fan, Monthly Notices of the Royal Astronomical Society 471 (2017) 629–649. Matthee, Jorryt J., et al. “Boötes-HiZELS: An Optical to near-Infrared Survey of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 1, Oxford University Press, 2017, pp. 629–49, doi:<a href="https://doi.org/10.1093/mnras/stx1569">10.1093/mnras/stx1569</a>. 115612022-07-12T11:01:35Z2024-10-14T11:34:07Z