---
res:
  bibo_abstract:
  - Rest-frame ultraviolet (UV) emission lines probe electron densities, gas-phase
    abundances, metallicities, and ionization parameters of the emitting star-forming
    galaxies and their environments. The strongest main UV emission line, Lyα, has
    been instrumental in advancing the general knowledge of galaxy formation in the
    early universe. However, observing Lyα emission becomes increasingly challenging
    at z ≳ 6 when the neutral hydrogen fraction of the circumgalactic and intergalactic
    media increases. Secondary weaker UV emission lines provide important alternative
    methods for studying galaxy properties at high redshift. We present a large sample
    of rest-frame UV emission line sources at intermediate redshift for calibrating
    and exploring the connection between secondary UV lines and the emitting galaxies’
    physical properties and their Lyα emission. The sample of 2052 emission line sources
    with 1.5 < z < 6.4 was collected from integral field data from the MUSE-Wide and
    MUSE-Deep surveys taken as part of Guaranteed Time Observations. The objects were
    selected through untargeted source detection (i.e., no preselection of sources
    as in dedicated spectroscopic campaigns) in the three-dimensional MUSE data cubes.
    We searched optimally extracted one-dimensional spectra of the full sample for
    UV emission features via emission line template matching, resulting in a sample
    of more than 100 rest-frame UV emission line detections. We show that the detection
    efficiency of (non-Lyα) UV emission lines increases with survey depth, and that
    the emission line strength of He IIλ1640 Å, [O III] λ1661 + O III] λ1666, and
    [Si III] λ1883 + Si III] λ1892 correlate with the strength of [C III] λ1907 +
    C III] λ1909. The rest-frame equivalent width (EW0) of [C III] λ1907 + C III]
    λ1909 is found to be roughly 0.22 ± 0.18 of EW0(Lyα). We measured the velocity
    offsets of resonant emission lines with respect to systemic tracers. For C IVλ1548
    + C IVλ1551 we find that ΔvC IV ≲ 250 km s−1, whereas ΔvLyα falls in the range
    of 250−500 km s−1 which is in agreement with previous results from the literature.
    The electron density ne measured from [Si III] λ1883 + Si III] λ1892 and [C III]
    λ1907 + C III] λ1909 line flux ratios is generally < 105 cm−3 and the gas-phase
    abundance is below solar at 12 + log10(O/H)≈8. Lastly, we used “PhotoIonization
    Model Probability Density Functions” to infer physical parameters of the full
    sample and individual systems based on photoionization model parameter grids and
    observational constraints from our UV emission line searches. This reveals that
    the UV line emitters generally have ionization parameter log10(U) ≈ −2.5 and metal
    mass fractions that scatter around Z ≈ 10−2, that is Z ≈ 0.66 Z⊙. Value-added
    catalogs of the full sample of MUSE objects studied in this work and a collection
    of UV line emitters from the literature are provided with this paper.@eng
  bibo_authorlist:
  - foaf_Person:
      foaf_givenName: K. B.
      foaf_name: Schmidt, K. B.
      foaf_surname: Schmidt
  - foaf_Person:
      foaf_givenName: J.
      foaf_name: Kerutt, J.
      foaf_surname: Kerutt
  - foaf_Person:
      foaf_givenName: L.
      foaf_name: Wisotzki, L.
      foaf_surname: Wisotzki
  - foaf_Person:
      foaf_givenName: T.
      foaf_name: Urrutia, T.
      foaf_surname: Urrutia
  - foaf_Person:
      foaf_givenName: A.
      foaf_name: Feltre, A.
      foaf_surname: Feltre
  - foaf_Person:
      foaf_givenName: M. V.
      foaf_name: Maseda, M. V.
      foaf_surname: Maseda
  - foaf_Person:
      foaf_givenName: T.
      foaf_name: Nanayakkara, T.
      foaf_surname: Nanayakkara
  - foaf_Person:
      foaf_givenName: R.
      foaf_name: Bacon, R.
      foaf_surname: Bacon
  - foaf_Person:
      foaf_givenName: L. A.
      foaf_name: Boogaard, L. A.
      foaf_surname: Boogaard
  - foaf_Person:
      foaf_givenName: S.
      foaf_name: Conseil, S.
      foaf_surname: Conseil
  - foaf_Person:
      foaf_givenName: T.
      foaf_name: Contini, T.
      foaf_surname: Contini
  - foaf_Person:
      foaf_givenName: E. C.
      foaf_name: Herenz, E. C.
      foaf_surname: Herenz
  - foaf_Person:
      foaf_givenName: W.
      foaf_name: Kollatschny, W.
      foaf_surname: Kollatschny
  - foaf_Person:
      foaf_givenName: M.
      foaf_name: Krumpe, M.
      foaf_surname: Krumpe
  - foaf_Person:
      foaf_givenName: F.
      foaf_name: Leclercq, F.
      foaf_surname: Leclercq
  - foaf_Person:
      foaf_givenName: G.
      foaf_name: Mahler, G.
      foaf_surname: Mahler
  - foaf_Person:
      foaf_givenName: Jorryt J
      foaf_name: Matthee, Jorryt J
      foaf_surname: Matthee
      foaf_workInfoHomepage: http://www.librecat.org/personId=7439a258-f3c0-11ec-9501-9df22fe06720
    orcid: 0000-0003-2871-127X
  - foaf_Person:
      foaf_givenName: V.
      foaf_name: Mauerhofer, V.
      foaf_surname: Mauerhofer
  - foaf_Person:
      foaf_givenName: J.
      foaf_name: Richard, J.
      foaf_surname: Richard
  - foaf_Person:
      foaf_givenName: J.
      foaf_name: Schaye, J.
      foaf_surname: Schaye
  bibo_doi: 10.1051/0004-6361/202140876
  bibo_volume: 654
  dct_date: 2021^xs_gYear
  dct_isPartOf:
  - http://id.crossref.org/issn/0004-6361
  - http://id.crossref.org/issn/1432-0746
  dct_language: eng
  dct_publisher: EDP Sciences@
  dct_subject:
  - Space and Planetary Science
  - Astronomy and Astrophysics
  - 'ultraviolet: galaxies / galaxies: high-redshift / galaxies: ISM / ISM: lines
    and bands / methods: observational / techniques: imaging spectroscopy'
  dct_title: Recovery and analysis of rest-frame UV emission lines in 2052 galaxies
    observed with MUSE at 1.5 < z < 6.4@
...