---
_id: '11498'
abstract:
- lang: eng
  text: 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.
acknowledgement: 'We would like to thank Charlotte Mason for useful discussions and
  for providing the data for the curves shown in Fig. 13 and Dawn Erb for providing
  the observational data for the comparison sample studied by Steidel et al. (2014),
  also shown in Fig. 13. This work has been supported by the BMBF grant 05A14BAC and
  we acknowledge support by the Competitive Fund of the Leibniz Association through
  grant SAW-2015-AIP-2. AF acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001.
  JS acknowledges the support from Vici grant 639.043.409 from the Dutch Research
  Council (NWO). GM received funding from the European Union’s Horizon 2020 research
  and innovation programme under the Marie Sklodowska-Curie grant agreement No MARACAS
  – DLV-896778. This paper is based on observations collected at the European Organisation
  for Astronomical Research in the Southern Hemisphere under ESO programmes 094.A-0289(B),
  095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 094.A-0205, 095.A-0240, 096.A-0090,
  097.A-0160, and 098.A-0017. This paper also makes use of observations made with
  the NASA/ESA Hubble Space Telescope obtained at STScI. This research made use of
  the following programs and open-source packages for Python and we are thankful to
  their developers: DS9 (Joye & Mandel 2003), Astropy (Astropy Collaboration 2013,
  2018), APLpy (Robitaille & Bressert 2012), iPython (Pérez & Granger 2007), numpy
  (van der Walt et al. 2011), matplotlib (Hunter 2007), and SciPy (Jones et al. 2001).'
article_number: A80
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: K. B.
  full_name: Schmidt, K. B.
  last_name: Schmidt
- first_name: J.
  full_name: Kerutt, J.
  last_name: Kerutt
- first_name: L.
  full_name: Wisotzki, L.
  last_name: Wisotzki
- first_name: T.
  full_name: Urrutia, T.
  last_name: Urrutia
- first_name: A.
  full_name: Feltre, A.
  last_name: Feltre
- first_name: M. V.
  full_name: Maseda, M. V.
  last_name: Maseda
- first_name: T.
  full_name: Nanayakkara, T.
  last_name: Nanayakkara
- first_name: R.
  full_name: Bacon, R.
  last_name: Bacon
- first_name: L. A.
  full_name: Boogaard, L. A.
  last_name: Boogaard
- first_name: S.
  full_name: Conseil, S.
  last_name: Conseil
- first_name: T.
  full_name: Contini, T.
  last_name: Contini
- first_name: E. C.
  full_name: Herenz, E. C.
  last_name: Herenz
- first_name: W.
  full_name: Kollatschny, W.
  last_name: Kollatschny
- first_name: M.
  full_name: Krumpe, M.
  last_name: Krumpe
- first_name: F.
  full_name: Leclercq, F.
  last_name: Leclercq
- first_name: G.
  full_name: Mahler, G.
  last_name: Mahler
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: V.
  full_name: Mauerhofer, V.
  last_name: Mauerhofer
- first_name: J.
  full_name: Richard, J.
  last_name: Richard
- first_name: J.
  full_name: Schaye, J.
  last_name: Schaye
citation:
  ama: Schmidt KB, Kerutt J, Wisotzki L, et al. Recovery and analysis of rest-frame
    UV emission lines in 2052 galaxies observed with MUSE at 1.5 &#60; z &#60; 6.4.
    <i>Astronomy &#38; Astrophysics</i>. 2021;654. doi:<a href="https://doi.org/10.1051/0004-6361/202140876">10.1051/0004-6361/202140876</a>
  apa: Schmidt, K. B., Kerutt, J., Wisotzki, L., Urrutia, T., Feltre, A., Maseda,
    M. V., … Schaye, J. (2021). Recovery and analysis of rest-frame UV emission lines
    in 2052 galaxies observed with MUSE at 1.5 &#60; z &#60; 6.4. <i>Astronomy &#38;
    Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/202140876">https://doi.org/10.1051/0004-6361/202140876</a>
  chicago: Schmidt, K. B., J. Kerutt, L. Wisotzki, T. Urrutia, A. Feltre, M. V. Maseda,
    T. Nanayakkara, et al. “Recovery and Analysis of Rest-Frame UV Emission Lines
    in 2052 Galaxies Observed with MUSE at 1.5 &#60; z &#60; 6.4.” <i>Astronomy &#38;
    Astrophysics</i>. EDP Sciences, 2021. <a href="https://doi.org/10.1051/0004-6361/202140876">https://doi.org/10.1051/0004-6361/202140876</a>.
  ieee: K. B. Schmidt <i>et al.</i>, “Recovery and analysis of rest-frame UV emission
    lines in 2052 galaxies observed with MUSE at 1.5 &#60; z &#60; 6.4,” <i>Astronomy
    &#38; Astrophysics</i>, vol. 654. EDP Sciences, 2021.
  ista: Schmidt KB, Kerutt J, Wisotzki L, Urrutia T, Feltre A, Maseda MV, Nanayakkara
    T, Bacon R, Boogaard LA, Conseil S, Contini T, Herenz EC, Kollatschny W, Krumpe
    M, Leclercq F, Mahler G, Matthee JJ, Mauerhofer V, Richard J, Schaye J. 2021.
    Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed
    with MUSE at 1.5 &#60; z &#60; 6.4. Astronomy &#38; Astrophysics. 654, A80.
  mla: Schmidt, K. B., et al. “Recovery and Analysis of Rest-Frame UV Emission Lines
    in 2052 Galaxies Observed with MUSE at 1.5 &#60; z &#60; 6.4.” <i>Astronomy &#38;
    Astrophysics</i>, vol. 654, A80, EDP Sciences, 2021, doi:<a href="https://doi.org/10.1051/0004-6361/202140876">10.1051/0004-6361/202140876</a>.
  short: K.B. Schmidt, J. Kerutt, L. Wisotzki, T. Urrutia, A. Feltre, M.V. Maseda,
    T. Nanayakkara, R. Bacon, L.A. Boogaard, S. Conseil, T. Contini, E.C. Herenz,
    W. Kollatschny, M. Krumpe, F. Leclercq, G. Mahler, J.J. Matthee, V. Mauerhofer,
    J. Richard, J. Schaye, Astronomy &#38; Astrophysics 654 (2021).
date_created: 2022-07-06T08:49:03Z
date_published: 2021-10-15T00:00:00Z
date_updated: 2022-07-19T09:34:36Z
day: '15'
doi: 10.1051/0004-6361/202140876
extern: '1'
external_id:
  arxiv:
  - '2108.01713'
intvolume: '       654'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'ultraviolet: galaxies / galaxies: high-redshift / galaxies: ISM / ISM: lines and
  bands / methods: observational / techniques: imaging spectroscopy'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/2108.01713
month: '10'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed
  with MUSE at 1.5 < z < 6.4
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 654
year: '2021'
...
---
_id: '11526'
abstract:
- lang: eng
  text: We present the results from a MUSE survey of twelve z ≃ 3.15 quasars, which
    were selected to be much fainter (20 < iSDSS < 23) than in previous studies of
    giant Ly α nebulae around the brightest quasars (16.6 < iAB < 18.7). We detect
    H I Ly α nebulae around 100 per cent of our target quasars, with emission extending
    to scales of at least 60 physical kpc, and up to 190 pkpc. We explore correlations
    between properties of the nebulae and their host quasars, with the goal of connecting
    variations in the properties of the illuminating QSO to the response in nebular
    emission. We show that the surface brightness profiles of the nebulae are similar
    to those of nebulae around bright quasars, but with a lower normalization. Our
    targeted quasars are on average 3.7 mag (≃30 times) fainter in UV continuum than
    our bright reference sample, and yet the nebulae around them are only 4.3 times
    fainter in mean Ly α surface brightness, measured between 20 and 50 pkpc. We find
    significant correlations between the surface brightness of the nebula and the
    luminosity of the quasar in both UV continuum and Ly α. The latter can be interpreted
    as evidence for a substantial contribution from unresolved inner parts of the
    nebulae to the narrow components seen in the Ly α lines of some of our faint quasars,
    possibly from the inner circumgalactic medium or from the host galaxy’s interstellar
    medium.
acknowledgement: The authors thank Daichi Kashino, for providing access to unpublished
  zCOSMOS Deep data, and Jakob S. den Brok for sharing code used in den Brok et al.
  (2020). GP and SC acknowledge the support of the Swiss National Science Foundation
  [grant PP00P2163824]. SM is supported by the Experienced Researchers Fellowship,
  Alexander von Humboldt-Stiftung, Germany. This work is based on observations collected
  at the European Organisation for Astronomical Research in the Southern Hemisphere
  under the MUSE GTO programme. The major analysis and production of figures in this
  work was conducted in Python, using standard libraries which include NumPy (Harris
  et al. 2020), SciPy (Virtanen et al. 2020), Matplotlib (Hunter 2007) and the interactive
  command shell IPython (Pérez & Granger 2007). This research also made use of Astropy,
  a community-developed core Python package for Astronomy (Astropy Collaboration et
  al. 2013), and Photutils, an Astropy package for detection and photometry of astronomica
  sources (Bradley et al. 2019). The python interface dustmaps (Green 2018) was used
  to query galactic extinction maps. topcat, a graphical tool for manipulating tabular
  data, was also utilized in this analysis (Taylor 2005). This research has made use
  of the "Aladin sky atlas" developed at CDS, Strasbourg Observatory, France (Bonnarel
  et al. 2000).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Ruari
  full_name: Mackenzie, Ruari
  last_name: Mackenzie
- first_name: Gabriele
  full_name: Pezzulli, Gabriele
  last_name: Pezzulli
- first_name: Sebastiano
  full_name: Cantalupo, Sebastiano
  last_name: Cantalupo
- first_name: Raffaella A
  full_name: Marino, Raffaella A
  last_name: Marino
- first_name: Simon
  full_name: Lilly, Simon
  last_name: Lilly
- first_name: Sowgat
  full_name: Muzahid, Sowgat
  last_name: Muzahid
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: Joop
  full_name: Schaye, Joop
  last_name: Schaye
- first_name: Lutz
  full_name: Wisotzki, Lutz
  last_name: Wisotzki
citation:
  ama: Mackenzie R, Pezzulli G, Cantalupo S, et al. Revealing the impact of quasar
    luminosity on giant Lyα nebulae. <i>Monthly Notices of the Royal Astronomical
    Society</i>. 2021;502(1):494-509. doi:<a href="https://doi.org/10.1093/mnras/staa3277">10.1093/mnras/staa3277</a>
  apa: Mackenzie, R., Pezzulli, G., Cantalupo, S., Marino, R. A., Lilly, S., Muzahid,
    S., … Wisotzki, L. (2021). Revealing the impact of quasar luminosity on giant
    Lyα nebulae. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford
    University Press. <a href="https://doi.org/10.1093/mnras/staa3277">https://doi.org/10.1093/mnras/staa3277</a>
  chicago: Mackenzie, Ruari, Gabriele Pezzulli, Sebastiano Cantalupo, Raffaella A
    Marino, Simon Lilly, Sowgat Muzahid, Jorryt J Matthee, Joop Schaye, and Lutz Wisotzki.
    “Revealing the Impact of Quasar Luminosity on Giant Lyα Nebulae.” <i>Monthly Notices
    of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href="https://doi.org/10.1093/mnras/staa3277">https://doi.org/10.1093/mnras/staa3277</a>.
  ieee: R. Mackenzie <i>et al.</i>, “Revealing the impact of quasar luminosity on
    giant Lyα nebulae,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 502, no. 1. Oxford University Press, pp. 494–509, 2021.
  ista: Mackenzie R, Pezzulli G, Cantalupo S, Marino RA, Lilly S, Muzahid S, Matthee
    JJ, Schaye J, Wisotzki L. 2021. Revealing the impact of quasar luminosity on giant
    Lyα nebulae. Monthly Notices of the Royal Astronomical Society. 502(1), 494–509.
  mla: Mackenzie, Ruari, et al. “Revealing the Impact of Quasar Luminosity on Giant
    Lyα Nebulae.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 502,
    no. 1, Oxford University Press, 2021, pp. 494–509, doi:<a href="https://doi.org/10.1093/mnras/staa3277">10.1093/mnras/staa3277</a>.
  short: R. Mackenzie, G. Pezzulli, S. Cantalupo, R.A. Marino, S. Lilly, S. Muzahid,
    J.J. Matthee, J. Schaye, L. Wisotzki, Monthly Notices of the Royal Astronomical
    Society 502 (2021) 494–509.
date_created: 2022-07-07T10:11:15Z
date_published: 2021-03-01T00:00:00Z
date_updated: 2022-08-18T10:56:28Z
day: '01'
doi: 10.1093/mnras/staa3277
extern: '1'
external_id:
  arxiv:
  - '2010.12589'
intvolume: '       502'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'techniques: imaging spectroscopy'
- intergalactic medium
- 'quasars: emission lines'
- 'quasars: general'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/2010.12589
month: '03'
oa: 1
oa_version: Preprint
page: 494-509
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Revealing the impact of quasar luminosity on giant Lyα nebulae
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 502
year: '2021'
...