---
_id: '11586'
abstract:
- lang: eng
  text: Distant luminous Lyman-α emitters are excellent targets for detailed observations
    of galaxies in the epoch of reionisation. Spatially resolved observations of these
    galaxies allow us to simultaneously probe the emission from young stars, partially
    ionised gas in the interstellar medium and to constrain the properties of the
    surrounding hydrogen in the circumgalactic medium. We review recent results from
    (spectroscopic) follow-up studies of the rest-frame UV, Lyman-α and [CII] emission
    in luminous galaxies observed ∼500 Myr after the Big Bang with ALMA, HST/WFC3
    and VLT/X-SHOOTER. These galaxies likely reside in early ionised bubbles and are
    complex systems, consisting of multiple well separated and resolved components
    where traces of metals are already present.
article_processing_charge: No
arxiv: 1
author:
- 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: David
  full_name: Sobral, David
  last_name: Sobral
citation:
  ama: 'Matthee JJ, Sobral D. Unveiling the most luminous Lyman-α emitters in the
    epoch of reionisation. In: <i>Proceedings of the International Astronomical Union</i>.
    Vol 15. Cambridge University Press; 2020:21-25. doi:<a href="https://doi.org/10.1017/s1743921319009451">10.1017/s1743921319009451</a>'
  apa: Matthee, J. J., &#38; Sobral, D. (2020). Unveiling the most luminous Lyman-α
    emitters in the epoch of reionisation. In <i>Proceedings of the International
    Astronomical Union</i> (Vol. 15, pp. 21–25). Cambridge University Press. <a href="https://doi.org/10.1017/s1743921319009451">https://doi.org/10.1017/s1743921319009451</a>
  chicago: Matthee, Jorryt J, and David Sobral. “Unveiling the Most Luminous Lyman-α
    Emitters in the Epoch of Reionisation.” In <i>Proceedings of the International
    Astronomical Union</i>, 15:21–25. Cambridge University Press, 2020. <a href="https://doi.org/10.1017/s1743921319009451">https://doi.org/10.1017/s1743921319009451</a>.
  ieee: J. J. Matthee and D. Sobral, “Unveiling the most luminous Lyman-α emitters
    in the epoch of reionisation,” in <i>Proceedings of the International Astronomical
    Union</i>, 2020, vol. 15, no. S352, pp. 21–25.
  ista: Matthee JJ, Sobral D. 2020. Unveiling the most luminous Lyman-α emitters in
    the epoch of reionisation. Proceedings of the International Astronomical Union.
    vol. 15, 21–25.
  mla: Matthee, Jorryt J., and David Sobral. “Unveiling the Most Luminous Lyman-α
    Emitters in the Epoch of Reionisation.” <i>Proceedings of the International Astronomical
    Union</i>, vol. 15, no. S352, Cambridge University Press, 2020, pp. 21–25, doi:<a
    href="https://doi.org/10.1017/s1743921319009451">10.1017/s1743921319009451</a>.
  short: J.J. Matthee, D. Sobral, in:, Proceedings of the International Astronomical
    Union, Cambridge University Press, 2020, pp. 21–25.
date_created: 2022-07-14T14:08:41Z
date_published: 2020-06-04T00:00:00Z
date_updated: 2022-08-19T08:41:12Z
day: '04'
doi: 10.1017/s1743921319009451
extern: '1'
external_id:
  arxiv:
  - '1911.04774'
intvolume: '        15'
issue: S352
keyword:
- Astronomy and Astrophysics
- Space and Planetary Science
- 'galaxies: formation'
- 'galaxies: evolution'
- 'galaxies: high-redshift'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1911.04774
month: '06'
oa: 1
oa_version: Preprint
page: 21-25
publication: Proceedings of the International Astronomical Union
publication_identifier:
  eissn:
  - 1743-9221
  issn:
  - 1743-9213
publication_status: published
publisher: Cambridge University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Unveiling the most luminous Lyman-α emitters in the epoch of reionisation
type: conference
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 15
year: '2020'
...
---
_id: '11499'
abstract:
- lang: eng
  text: Deep optical spectroscopic surveys of galaxies provide a unique opportunity
    to investigate rest-frame ultra-violet (UV) emission line properties of galaxies
    at z ∼ 2 − 4.5. Here we combine VLT/MUSE Guaranteed Time Observations of the Hubble
    Deep Field South, Ultra Deep Field, COSMOS, and several quasar fields with other
    publicly available data from VLT/VIMOS and VLT/FORS2 to construct a catalogue
    of He II λ1640 emitters at z ≳ 2. The deepest areas of our MUSE pointings reach
    a 3σ line flux limit of 3.1 × 10−19 erg s−1 cm−2. After discarding broad-line
    active galactic nuclei, we find 13 He II λ1640 detections from MUSE with a median
    MUV = −20.1 and 21 tentative He II λ1640 detections from other public surveys.
    Excluding Lyα, all except two galaxies in our sample show at least one other rest-UV
    emission line, with C III] λ1907, λ1909 being the most prominent. We use multi-wavelength
    data available in the Hubble legacy fields to derive basic galaxy properties of
    our sample through spectral energy distribution fitting techniques. Taking advantage
    of the high-quality spectra obtained by MUSE (∼10 − 30 h of exposure time per
    pointing), we use photo-ionisation models to study the rest-UV emission line diagnostics
    of the He II λ1640 emitters. Line ratios of our sample can be reproduced by moderately
    sub-solar photo-ionisation models, however, we find that including effects of
    binary stars lead to degeneracies in most free parameters. Even after considering
    extra ionising photons produced by extreme sub-solar metallicity binary stellar
    models, photo-ionisation models are unable to reproduce rest-frame He II λ1640
    equivalent widths (∼0.2 − 10 Å), thus additional mechanisms are necessary in models
    to match the observed He II λ1640 properties.
acknowledgement: 'The authors wish to thank the referee for constructive comments
  that improved the paper substantially. We thank the BPASS team for making the stellar
  population models available. We thank Elizabeth Stanway, Claus Leitherer, Daniel
  Schaerer, Jorick Vink, and Nell Byler for insightful discussions. We thank the Lorentz
  Centre and the scientific organizers of the Characterizing galaxies with spectroscopy
  with a view for JWST workshop held at the Lorentz Centre in 2017 October, which
  promoted useful discussions in the wider community. TN, JB, and RB acknowledges
  the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) top grant TOP1.16.057.
  AF acknowledges support from the ERC via an Advanced Grant under grant agreement
  no. 339659-MUSICOS. JB acknowledges support by Fundação para a Ciência e a Tecnologia
  (FCT) through national funds (UID/FIS/04434/2013) and Investigador FCT contract
  IF/01654/2014/CP1215/CT0003, and by FEDER through COMPETE2020 (POCI-01-0145-FEDER-007672).
  JR acknowledges support from the ERC Starting grant 336736 (CALENDS). This research
  made use of astropy (http://www.astropy.org) a community-developed core Python package
  for Astronomy (Astropy Collaboration 2013, 2018) and pandas (McKinney 2010). Figures
  were generated using matplotlib (Hunter 2007) and seaborn (https://seaborn.pydata.org).
  Facilities: VLT (MUSE).'
article_number: A89
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Themiya
  full_name: Nanayakkara, Themiya
  last_name: Nanayakkara
- first_name: Jarle
  full_name: Brinchmann, Jarle
  last_name: Brinchmann
- first_name: Leindert
  full_name: Boogaard, Leindert
  last_name: Boogaard
- first_name: Rychard
  full_name: Bouwens, Rychard
  last_name: Bouwens
- first_name: Sebastiano
  full_name: Cantalupo, Sebastiano
  last_name: Cantalupo
- first_name: Anna
  full_name: Feltre, Anna
  last_name: Feltre
- first_name: Wolfram
  full_name: Kollatschny, Wolfram
  last_name: Kollatschny
- first_name: Raffaella Anna
  full_name: Marino, Raffaella Anna
  last_name: Marino
- first_name: Michael
  full_name: Maseda, Michael
  last_name: Maseda
- 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: Mieke
  full_name: Paalvast, Mieke
  last_name: Paalvast
- first_name: Johan
  full_name: Richard, Johan
  last_name: Richard
- first_name: Anne
  full_name: Verhamme, Anne
  last_name: Verhamme
citation:
  ama: Nanayakkara T, Brinchmann J, Boogaard L, et al. Exploring He II λ1640 emission
    line properties at z ∼2−4. <i>Astronomy &#38; Astrophysics</i>. 2019;648. doi:<a
    href="https://doi.org/10.1051/0004-6361/201834565">10.1051/0004-6361/201834565</a>
  apa: Nanayakkara, T., Brinchmann, J., Boogaard, L., Bouwens, R., Cantalupo, S.,
    Feltre, A., … Verhamme, A. (2019). Exploring He II λ1640 emission line properties
    at z ∼2−4. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/201834565">https://doi.org/10.1051/0004-6361/201834565</a>
  chicago: Nanayakkara, Themiya, Jarle Brinchmann, Leindert Boogaard, Rychard Bouwens,
    Sebastiano Cantalupo, Anna Feltre, Wolfram Kollatschny, et al. “Exploring He II Λ1640
    Emission Line Properties at z ∼2−4.” <i>Astronomy &#38; Astrophysics</i>. EDP
    Sciences, 2019. <a href="https://doi.org/10.1051/0004-6361/201834565">https://doi.org/10.1051/0004-6361/201834565</a>.
  ieee: T. Nanayakkara <i>et al.</i>, “Exploring He II λ1640 emission line properties
    at z ∼2−4,” <i>Astronomy &#38; Astrophysics</i>, vol. 648. EDP Sciences, 2019.
  ista: Nanayakkara T, Brinchmann J, Boogaard L, Bouwens R, Cantalupo S, Feltre A,
    Kollatschny W, Marino RA, Maseda M, Matthee JJ, Paalvast M, Richard J, Verhamme
    A. 2019. Exploring He II λ1640 emission line properties at z ∼2−4. Astronomy &#38;
    Astrophysics. 648, A89.
  mla: Nanayakkara, Themiya, et al. “Exploring He II Λ1640 Emission Line Properties
    at z ∼2−4.” <i>Astronomy &#38; Astrophysics</i>, vol. 648, A89, EDP Sciences,
    2019, doi:<a href="https://doi.org/10.1051/0004-6361/201834565">10.1051/0004-6361/201834565</a>.
  short: T. Nanayakkara, J. Brinchmann, L. Boogaard, R. Bouwens, S. Cantalupo, A.
    Feltre, W. Kollatschny, R.A. Marino, M. Maseda, J.J. Matthee, M. Paalvast, J.
    Richard, A. Verhamme, Astronomy &#38; Astrophysics 648 (2019).
date_created: 2022-07-06T09:07:06Z
date_published: 2019-04-16T00:00:00Z
date_updated: 2022-07-19T09:36:08Z
day: '16'
doi: 10.1051/0004-6361/201834565
extern: '1'
external_id:
  arxiv:
  - '1902.05960'
intvolume: '       648'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: ISM / galaxies: star formation / galaxies: evolution / galaxies: high-redshift'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1902.05960
month: '04'
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'
related_material:
  link:
  - relation: erratum
    url: https://doi.org/10.1051/0004-6361/201834565e
scopus_import: '1'
status: public
title: Exploring He II λ1640 emission line properties at z ∼2−4
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 648
year: '2019'
...
---
_id: '11505'
abstract:
- lang: eng
  text: "Contact. This paper presents the results obtained with the Multi-Unit Spectroscopic
    Explorer (MUSE) at the ESO Very Large Telescope on the faint end of the Lyman-alpha
    luminosity function (LF) based on deep observations of four lensing clusters.
    The goal of our project is to set strong constraints on the relative contribution
    of the Lyman-alpha emitter (LAE) population to cosmic reionization.\r\n\r\nAims.
    The precise aim of the present study is to further constrain the abundance of
    LAEs by taking advantage of the magnification provided by lensing clusters to
    build a blindly selected sample of galaxies which is less biased than current
    blank field samples in redshift and luminosity. By construction, this sample of
    LAEs is complementary to those built from deep blank fields, whether observed
    by MUSE or by other facilities, and makes it possible to determine the shape of
    the LF at fainter levels, as well as its evolution with redshift.\r\n\r\nMethods.
    We selected a sample of 156 LAEs with redshifts between 2.9 ≤ z ≤ 6.7 and magnification-corrected
    luminosities in the range 39 ≲ log LLyα [erg s−1] ≲43. To properly take into account
    the individual differences in detection conditions between the LAEs when computing
    the LF, including lensing configurations, and spatial and spectral morphologies,
    the non-parametric 1/Vmax method was adopted. The price to pay to benefit from
    magnification is a reduction of the effective volume of the survey, together with
    a more complex analysis procedure to properly determine the effective volume Vmax
    for each galaxy. In this paper we present a complete procedure for the determination
    of the LF based on IFU detections in lensing clusters. This procedure, including
    some new methods for masking, effective volume integration and (individual) completeness
    determinations, has been fully automated when possible, and it can be easily generalized
    to the analysis of IFU observations in blank fields.\r\n\r\nResults. As a result
    of this analysis, the Lyman-alpha LF has been obtained in four different redshift
    bins: 2.9 <  z <  6, 7, 2.9 <  z <  4.0, 4.0 <  z <  5.0, and 5.0 <  z <  6.7
    with constraints down to log LLyα = 40.5. From our data only, no significant evolution
    of LF mean slope can be found. When performing a Schechter analysis also including
    data from the literature to complete the present sample towards the brightest
    luminosities, a steep faint end slope was measured varying from α = −1.69−0.08+0.08
    to α = −1.87−0.12+0.12 between the lowest and the highest redshift bins.\r\n\r\nConclusions.
    The contribution of the LAE population to the star formation rate density at z ∼ 6
    is ≲50% depending on the luminosity limit considered, which is of the same order
    as the Lyman-break galaxy (LBG) contribution. The evolution of the LAE contribution
    with redshift depends on the assumed escape fraction of Lyman-alpha photons, and
    appears to slightly increase with increasing redshift when this fraction is conservatively
    set to one. Depending on the intersection between the LAE/LBG populations, the
    contribution of the observed galaxies to the ionizing flux may suffice to keep
    the universe ionized at z ∼ 6."
acknowledgement: We thank the anonymous referee for their critical review and useful
  suggestions. This work has been carried out thanks to the support of the OCEVU Labex
  (ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02) funded by the “Investissements
  d’Avenir” French government programme managed by the ANR. Partially funded by the
  ERC starting grant CALENDS (JR, VP, BC, JM), the Agence Nationale de la recherche
  bearing the reference ANR-13-BS05-0010-02 (FOGHAR), and the “Programme National
  de Cosmologie and Galaxies” (PNCG) of CNRS/INSU, France. GdV, RP, JR, GM, JM, BC,
  and VP also acknowledge support by the Programa de Cooperacion Cientifica – ECOS
  SUD Program C16U02. NL acknowledges funding from the European Research Council (ERC)
  under the European Union’s Horizon 2020 research and innovation programme (grant
  agreement No 669253), ABD acknowledges support from the ERC advanced grant “Cosmic
  Gas”. LW acknowledges support by the Competitive Fund of the Leibniz Association
  through grant SAW-2015-AIP-2, and TG acknowledges support from the European Research
  Council under grant agreement ERC-stg-757258 (TRIPLE).. Based on observations made
  with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 060.A-9345,
  094.A-0115, 095.A-0181, 096.A-0710, 097.A0269, 100.A-0249, and 294.A-5032. Also
  based on observations obtained with the NASA/ESA Hubble Space Telescope, retrieved
  from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science
  Institute (STScI). STScI is operated by the Association of Universities for Research
  in Astronomy, Inc. under NASA contract NAS 5-26555. This research made use of Astropy,
  a community-developed core Python package for Astronomy (Astropy Collaboration 2013).
  All plots in this paper were created using Matplotlib (Hunter 2007).
article_number: A3
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: G.
  full_name: de La Vieuville, G.
  last_name: de La Vieuville
- first_name: D.
  full_name: Bina, D.
  last_name: Bina
- first_name: R.
  full_name: Pello, R.
  last_name: Pello
- first_name: G.
  full_name: Mahler, G.
  last_name: Mahler
- first_name: J.
  full_name: Richard, J.
  last_name: Richard
- first_name: A. B.
  full_name: Drake, A. B.
  last_name: Drake
- first_name: E. C.
  full_name: Herenz, E. C.
  last_name: Herenz
- first_name: F. E.
  full_name: Bauer, F. E.
  last_name: Bauer
- first_name: B.
  full_name: Clément, B.
  last_name: Clément
- first_name: D.
  full_name: Lagattuta, D.
  last_name: Lagattuta
- first_name: N.
  full_name: Laporte, N.
  last_name: Laporte
- first_name: J.
  full_name: Martinez, J.
  last_name: Martinez
- first_name: V.
  full_name: Patrício, V.
  last_name: Patrício
- first_name: L.
  full_name: Wisotzki, L.
  last_name: Wisotzki
- first_name: J.
  full_name: Zabl, J.
  last_name: Zabl
- first_name: R. J.
  full_name: Bouwens, R. J.
  last_name: Bouwens
- first_name: T.
  full_name: Contini, T.
  last_name: Contini
- first_name: T.
  full_name: Garel, T.
  last_name: Garel
- first_name: B.
  full_name: Guiderdoni, B.
  last_name: Guiderdoni
- first_name: R. A.
  full_name: Marino, R. A.
  last_name: Marino
- first_name: M. V.
  full_name: Maseda, M. V.
  last_name: Maseda
- 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: J.
  full_name: Schaye, J.
  last_name: Schaye
- first_name: G.
  full_name: Soucail, G.
  last_name: Soucail
citation:
  ama: de La Vieuville G, Bina D, Pello R, et al. Faint end of the z ∼ 3–7 luminosity
    function of Lyman-alpha emitters behind lensing clusters observed with MUSE. <i>Astronomy
    &#38; Astrophysics</i>. 2019;628. doi:<a href="https://doi.org/10.1051/0004-6361/201834471">10.1051/0004-6361/201834471</a>
  apa: de La Vieuville, G., Bina, D., Pello, R., Mahler, G., Richard, J., Drake, A.
    B., … Soucail, G. (2019). Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha
    emitters behind lensing clusters observed with MUSE. <i>Astronomy &#38; Astrophysics</i>.
    EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/201834471">https://doi.org/10.1051/0004-6361/201834471</a>
  chicago: La Vieuville, G. de, D. Bina, R. Pello, G. Mahler, J. Richard, A. B. Drake,
    E. C. Herenz, et al. “Faint End of the z ∼ 3–7 Luminosity Function of Lyman-Alpha
    Emitters behind Lensing Clusters Observed with MUSE.” <i>Astronomy &#38; Astrophysics</i>.
    EDP Sciences, 2019. <a href="https://doi.org/10.1051/0004-6361/201834471">https://doi.org/10.1051/0004-6361/201834471</a>.
  ieee: G. de La Vieuville <i>et al.</i>, “Faint end of the z ∼ 3–7 luminosity function
    of Lyman-alpha emitters behind lensing clusters observed with MUSE,” <i>Astronomy
    &#38; Astrophysics</i>, vol. 628. EDP Sciences, 2019.
  ista: de La Vieuville G, Bina D, Pello R, Mahler G, Richard J, Drake AB, Herenz
    EC, Bauer FE, Clément B, Lagattuta D, Laporte N, Martinez J, Patrício V, Wisotzki
    L, Zabl J, Bouwens RJ, Contini T, Garel T, Guiderdoni B, Marino RA, Maseda MV,
    Matthee JJ, Schaye J, Soucail G. 2019. Faint end of the z ∼ 3–7 luminosity function
    of Lyman-alpha emitters behind lensing clusters observed with MUSE. Astronomy
    &#38; Astrophysics. 628, A3.
  mla: de La Vieuville, G., et al. “Faint End of the z ∼ 3–7 Luminosity Function of
    Lyman-Alpha Emitters behind Lensing Clusters Observed with MUSE.” <i>Astronomy
    &#38; Astrophysics</i>, vol. 628, A3, EDP Sciences, 2019, doi:<a href="https://doi.org/10.1051/0004-6361/201834471">10.1051/0004-6361/201834471</a>.
  short: G. de La Vieuville, D. Bina, R. Pello, G. Mahler, J. Richard, A.B. Drake,
    E.C. Herenz, F.E. Bauer, B. Clément, D. Lagattuta, N. Laporte, J. Martinez, V.
    Patrício, L. Wisotzki, J. Zabl, R.J. Bouwens, T. Contini, T. Garel, B. Guiderdoni,
    R.A. Marino, M.V. Maseda, J.J. Matthee, J. Schaye, G. Soucail, Astronomy &#38;
    Astrophysics 628 (2019).
date_created: 2022-07-06T10:09:36Z
date_published: 2019-07-25T00:00:00Z
date_updated: 2022-07-19T09:36:31Z
day: '25'
doi: 10.1051/0004-6361/201834471
extern: '1'
external_id:
  arxiv:
  - '1905.13696'
intvolume: '       628'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'gravitational lensing: strong / galaxies: high-redshift / dark ages'
- reionization
- 'first stars / galaxies: clusters: general / galaxies: luminosity function'
- mass function
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1905.13696
month: '07'
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: Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind
  lensing clusters observed with MUSE
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 628
year: '2019'
...
---
_id: '11507'
abstract:
- lang: eng
  text: 'Lyman-α (Lyα) is intrinsically the brightest line emitted from active galaxies.
    While it originates from many physical processes, for star-forming galaxies the
    intrinsic Lyα luminosity is a direct tracer of the Lyman-continuum (LyC) radiation
    produced by the most massive O- and early-type B-stars (M⋆ ≳ 10 M⊙) with lifetimes
    of a few Myrs. As such, Lyα luminosity should be an excellent instantaneous star
    formation rate (SFR) indicator. However, its resonant nature and susceptibility
    to dust as a rest-frame UV photon makes Lyα very hard to interpret due to the
    uncertain Lyα escape fraction, fesc, Lyα. Here we explore results from the CAlibrating
    LYMan-α with Hα (CALYMHA) survey at z = 2.2, follow-up of Lyα emitters (LAEs)
    at z = 2.2 − 2.6 and a z ∼ 0−0.3 compilation of LAEs to directly measure fesc, Lyα
    with Hα. We derive a simple empirical relation that robustly retrieves fesc, Lyα
    as a function of Lyα rest-frame EW (EW0): fesc,Lyα = 0.0048 EW0[Å] ± 0.05 and
    we show that it constrains a well-defined anti-correlation between ionisation
    efficiency (ξion) and dust extinction in LAEs. Observed Lyα luminosities and EW0
    are easy measurable quantities at high redshift, thus making our relation a practical
    tool to estimate intrinsic Lyα and LyC luminosities under well controlled and
    simple assumptions. Our results allow observed Lyα luminosities to be used to
    compute SFRs for LAEs at z ∼ 0−2.6 within ±0.2 dex of the Hα dust corrected SFRs.
    We apply our empirical SFR(Lyα,EW0) calibration to several sources at z ≥ 2.6
    to find that star-forming LAEs have SFRs typically ranging from 0.1 to 20 M⊙ yr−1
    and that our calibration might be even applicable for the most luminous LAEs within
    the epoch of re-ionisation. Our results imply high ionisation efficiencies (log10[ξion/Hz erg−1]
    = 25.4−25.6) and low dust content in LAEs across cosmic time, and will be easily
    tested with future observations with JWST which can obtain Hα and Hβ measurements
    for high-redshift LAEs.'
acknowledgement: We thank the anonymous referees for multiple comments and suggestions
  which have improved the manuscript. JM acknowledges the support of a Huygens PhD
  fellowship from Leiden University. We have benefited greatly from the publicly available
  programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt et al. 2011;
  Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration
  2013) packages, and the TOPCAT analysis program (Taylor 2013). The results and samples
  of LAEs used for this paper are publicly available (see e.g. Sobral et al. 2017,
  2018a) and we also provide the toy model used as a PYTHON script.
article_number: A157
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
citation:
  ama: 'Sobral D, Matthee JJ. Predicting Lyα escape fractions with a simple observable:
    Lyα in emission as an empirically calibrated star formation rate indicator. <i>Astronomy
    &#38; Astrophysics</i>. 2019;623. doi:<a href="https://doi.org/10.1051/0004-6361/201833075">10.1051/0004-6361/201833075</a>'
  apa: 'Sobral, D., &#38; Matthee, J. J. (2019). Predicting Lyα escape fractions with
    a simple observable: Lyα in emission as an empirically calibrated star formation
    rate indicator. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/201833075">https://doi.org/10.1051/0004-6361/201833075</a>'
  chicago: 'Sobral, David, and Jorryt J Matthee. “Predicting Lyα Escape Fractions
    with a Simple Observable: Lyα in Emission as an Empirically Calibrated Star Formation
    Rate Indicator.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href="https://doi.org/10.1051/0004-6361/201833075">https://doi.org/10.1051/0004-6361/201833075</a>.'
  ieee: 'D. Sobral and J. J. Matthee, “Predicting Lyα escape fractions with a simple
    observable: Lyα in emission as an empirically calibrated star formation rate indicator,”
    <i>Astronomy &#38; Astrophysics</i>, vol. 623. EDP Sciences, 2019.'
  ista: 'Sobral D, Matthee JJ. 2019. Predicting Lyα escape fractions with a simple
    observable: Lyα in emission as an empirically calibrated star formation rate indicator.
    Astronomy &#38; Astrophysics. 623, A157.'
  mla: 'Sobral, David, and Jorryt J. Matthee. “Predicting Lyα Escape Fractions with
    a Simple Observable: Lyα in Emission as an Empirically Calibrated Star Formation
    Rate Indicator.” <i>Astronomy &#38; Astrophysics</i>, vol. 623, A157, EDP Sciences,
    2019, doi:<a href="https://doi.org/10.1051/0004-6361/201833075">10.1051/0004-6361/201833075</a>.'
  short: D. Sobral, J.J. Matthee, Astronomy &#38; Astrophysics 623 (2019).
date_created: 2022-07-06T11:08:16Z
date_published: 2019-03-26T00:00:00Z
date_updated: 2022-07-19T09:37:20Z
day: '26'
doi: 10.1051/0004-6361/201833075
extern: '1'
external_id:
  arxiv:
  - '1803.08923'
intvolume: '       623'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / galaxies: star formation / galaxies: statistics / galaxies:
  evolution / galaxies: formation / galaxies: ISM'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1803.08923
month: '03'
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: 'Predicting Lyα escape fractions with a simple observable: Lyα in emission
  as an empirically calibrated star formation rate indicator'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 623
year: '2019'
...
---
_id: '11535'
abstract:
- lang: eng
  text: We investigate the clustering and halo properties of ∼5000 Ly α-selected emission-line
    galaxies (LAEs) from the Slicing COSMOS 4K (SC4K) and from archival NB497 imaging
    of SA22 split in 15 discrete redshift slices between z ∼ 2.5 and 6. We measure
    clustering lengths of r0 ∼ 3–6 h−1 Mpc and typical halo masses of ∼1011 M⊙ for
    our narrowband-selected LAEs with typical LLy α ∼ 1042–43 erg s−1. The intermediate-band-selected
    LAEs are observed to have r0 ∼ 3.5–15 h−1 Mpc with typical halo masses of ∼1011–12
    M⊙ and typical LLy α ∼ 1043–43.6 erg s−1. We find a strong, redshift-independent
    correlation between halo mass and Ly α luminosity normalized by the characteristic
    Ly α luminosity, L⋆(z). The faintest LAEs (L ∼ 0.1 L⋆(z)) typically identified
    by deep narrowband surveys are found in 1010 M⊙ haloes and the brightest LAEs
    (L ∼ 7 L⋆(z)) are found in ∼5 × 1012 M⊙ haloes. A dependency on the rest-frame
    1500 Å UV luminosity, MUV, is also observed where the halo masses increase from
    1011 to 1013 M⊙ for MUV ∼ −19 to −23.5 mag. Halo mass is also observed to increase
    from 109.8 to 1012 M⊙ for dust-corrected UV star formation rates from ∼0.6 to
    10 M⊙ yr−1 and continues to increase up to 1013 M⊙ in halo mass, where the majority
    of those sources are active galactic nuclei. All the trends we observe are found
    to be redshift independent. Our results reveal that LAEs are the likely progenitors
    of a wide range of galaxies depending on their luminosity, from dwarf-like, to
    Milky Way-type, to bright cluster galaxies. LAEs therefore provide unique insight
    into the early formation and evolution of the galaxies we observe in the local
    Universe.
acknowledgement: We thank the anonymous referee for their useful comments and suggestions
  that helped improve this study. AAK acknowledges that this work was supported by
  NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant
  NNX16AO92H. JM acknowledges support from the ETH Zwicky fellowship. RKC acknowledges
  funding from STFC via a studentship. APA acknowledges support from the Fundac¸ao
  para a Ci ˜ encia e a Tecnologia FCT through the fellowship PD/BD/52706/2014 and
  the research grant UID/FIS/04434/2013. JC and SS both acknowledge their support
  from the Lancaster University PhD Fellowship. We have benefited greatly from the
  publicly available programming language PYTHON, including the NUMPY, SCIPY, MATPLOTLIB,
  SCIKIT-LEARN, and ASTROPY packages, as well as the TOPCAT analysis program. The
  SC4K samples used in this paper are all publicly available for use by the community
  (Sobral et al. 2018a). The catalogue is also available on the COSMOS IPAC website
  (https://irsa.ipac.caltech.edu/data/COSMOS/overview.html).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: A A
  full_name: Khostovan, A A
  last_name: Khostovan
- first_name: D
  full_name: Sobral, D
  last_name: Sobral
- first_name: B
  full_name: Mobasher, B
  last_name: Mobasher
- 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: R K
  full_name: Cochrane, R K
  last_name: Cochrane
- first_name: N
  full_name: Chartab, N
  last_name: Chartab
- first_name: M
  full_name: Jafariyazani, M
  last_name: Jafariyazani
- first_name: A
  full_name: Paulino-Afonso, A
  last_name: Paulino-Afonso
- first_name: S
  full_name: Santos, S
  last_name: Santos
- first_name: J
  full_name: Calhau, J
  last_name: Calhau
citation:
  ama: 'Khostovan AA, Sobral D, Mobasher B, et al. The clustering of typical Ly α emitters
    from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2019;489(1):555-573. doi:<a href="https://doi.org/10.1093/mnras/stz2149">10.1093/mnras/stz2149</a>'
  apa: 'Khostovan, A. A., Sobral, D., Mobasher, B., Matthee, J. J., Cochrane, R. K.,
    Chartab, N., … Calhau, J. (2019). The clustering of typical Ly α emitters from
    z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. <i>Monthly Notices
    of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stz2149">https://doi.org/10.1093/mnras/stz2149</a>'
  chicago: 'Khostovan, A A, D Sobral, B Mobasher, Jorryt J Matthee, R K Cochrane,
    N Chartab, M Jafariyazani, A Paulino-Afonso, S Santos, and J Calhau. “The Clustering
    of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV
    Luminosities.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford
    University Press, 2019. <a href="https://doi.org/10.1093/mnras/stz2149">https://doi.org/10.1093/mnras/stz2149</a>.'
  ieee: 'A. A. Khostovan <i>et al.</i>, “The clustering of typical Ly α emitters from
    z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities,” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 489, no. 1. Oxford University Press,
    pp. 555–573, 2019.'
  ista: 'Khostovan AA, Sobral D, Mobasher B, Matthee JJ, Cochrane RK, Chartab N, Jafariyazani
    M, Paulino-Afonso A, Santos S, Calhau J. 2019. The clustering of typical Ly α emitters
    from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices
    of the Royal Astronomical Society. 489(1), 555–573.'
  mla: 'Khostovan, A. A., et al. “The Clustering of Typical Ly α Emitters from z ∼
    2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 489, no. 1, Oxford University Press,
    2019, pp. 555–73, doi:<a href="https://doi.org/10.1093/mnras/stz2149">10.1093/mnras/stz2149</a>.'
  short: A.A. Khostovan, D. Sobral, B. Mobasher, J.J. Matthee, R.K. Cochrane, N. Chartab,
    M. Jafariyazani, A. Paulino-Afonso, S. Santos, J. Calhau, Monthly Notices of the
    Royal Astronomical Society 489 (2019) 555–573.
date_created: 2022-07-07T13:01:03Z
date_published: 2019-10-01T00:00:00Z
date_updated: 2022-08-19T06:38:42Z
day: '01'
doi: 10.1093/mnras/stz2149
extern: '1'
external_id:
  arxiv:
  - '1811.00556'
intvolume: '       489'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: haloes'
- 'galaxies: high-redshift'
- 'galaxies: star formation'
- 'cosmology: observations'
- large-scale structure of Universe
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1811.00556
month: '10'
oa: 1
oa_version: Preprint
page: 555-573
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: 'The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend
  on Ly α and UV luminosities'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 489
year: '2019'
...
---
_id: '11540'
abstract:
- lang: eng
  text: Observations have revealed that the star formation rate (SFR) and stellar
    mass (Mstar) of star-forming galaxies follow a tight relation known as the galaxy
    main sequence. However, what physical information is encoded in this relation
    is under debate. Here, we use the EAGLE cosmological hydrodynamical simulation
    to study the mass dependence, evolution, and origin of scatter in the SFR–Mstar
    relation. At z = 0, we find that the scatter decreases slightly with stellar mass
    from 0.35 dex at Mstar ≈ 109 M⊙ to 0.30 dex at Mstar ≳ 1010.5 M⊙. The scatter
    decreases from z = 0 to z = 5 by 0.05 dex at Mstar ≳ 1010 M⊙ and by 0.15 dex for
    lower masses. We show that the scatter at z = 0.1 originates from a combination
    of fluctuations on short time-scales (ranging from 0.2–2 Gyr) that are presumably
    associated with self-regulation from cooling, star formation, and outflows, but
    is dominated by long time-scale (∼10 Gyr) variations related to differences in
    halo formation times. Shorter time-scale fluctuations are relatively more important
    for lower mass galaxies. At high masses, differences in black hole formation efficiency
    cause additional scatter, but also diminish the scatter caused by different halo
    formation times. While individual galaxies cross the main sequence multiple times
    during their evolution, they fluctuate around tracks associated with their halo
    properties, i.e. galaxies above/below the main sequence at z = 0.1 tend to have
    been above/below the main sequence for ≫1 Gyr.
acknowledgement: JM acknowledges the support of a Huygens PhD fellowship from Leiden
  University. We thank Camila Correa for help analysing snipshot merger trees. We
  thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann,
  Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and
  suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade
  of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and
  ideas. We have benefited from the public available programming language PYTHON,
  including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT
  analysis tool (Taylor 2013).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- 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
citation:
  ama: Matthee JJ, Schaye J. The origin of scatter in the star formation rate–stellar
    mass relation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;484(1):915-932.
    doi:<a href="https://doi.org/10.1093/mnras/stz030">10.1093/mnras/stz030</a>
  apa: Matthee, J. J., &#38; Schaye, J. (2019). The origin of scatter in the star
    formation rate–stellar mass relation. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stz030">https://doi.org/10.1093/mnras/stz030</a>
  chicago: Matthee, Jorryt J, and Joop Schaye. “The Origin of Scatter in the Star
    Formation Rate–Stellar Mass Relation.” <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press, 2019. <a href="https://doi.org/10.1093/mnras/stz030">https://doi.org/10.1093/mnras/stz030</a>.
  ieee: J. J. Matthee and J. Schaye, “The origin of scatter in the star formation
    rate–stellar mass relation,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 484, no. 1. Oxford University Press, pp. 915–932, 2019.
  ista: Matthee JJ, Schaye J. 2019. The origin of scatter in the star formation rate–stellar
    mass relation. Monthly Notices of the Royal Astronomical Society. 484(1), 915–932.
  mla: Matthee, Jorryt J., and Joop Schaye. “The Origin of Scatter in the Star Formation
    Rate–Stellar Mass Relation.” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 484, no. 1, Oxford University Press, 2019, pp. 915–32, doi:<a href="https://doi.org/10.1093/mnras/stz030">10.1093/mnras/stz030</a>.
  short: J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society
    484 (2019) 915–932.
date_created: 2022-07-08T07:48:31Z
date_published: 2019-03-01T00:00:00Z
date_updated: 2022-08-19T06:42:43Z
day: '01'
doi: 10.1093/mnras/stz030
extern: '1'
external_id:
  arxiv:
  - '1805.05956'
intvolume: '       484'
issue: '1'
keyword:
- Space and Planetary Science
- 'Astronomy and Astrophysics : galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: star formation'
- 'cosmology: theory'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1805.05956
month: '03'
oa: 1
oa_version: Preprint
page: 915-932
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: The origin of scatter in the star formation rate–stellar mass relation
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 484
year: '2019'
...
---
_id: '11541'
abstract:
- lang: eng
  text: We present new Hubble Space Telescope (HST)/WFC3 observations and re-analyse
    VLT data to unveil the continuum, variability, and rest-frame ultraviolet (UV)
    lines of the multiple UV clumps of the most luminous Lyα emitter at z = 6.6, CR7
    (COSMOS Redshift 7). Our re-reduced, flux-calibrated X-SHOOTER spectra of CR7
    reveal an He II emission line in observations obtained along the major axis of
    Lyα emission with the best seeing conditions. He II is spatially offset by ≈+0.8
    arcsec from the peak of Lyα emission, and it is found towards clump B. Our WFC3
    grism spectra detects the UV continuum of CR7’s clump A, yielding a power law
    with β=−2.5+0.6−0.7 and MUV=−21.87+0.25−0.20⁠. No significant variability is found
    for any of the UV clumps on their own, but there is tentative (≈2.2 σ) brightening
    of CR7 in F110W as a whole from 2012 to 2017. HST grism data fail to robustly
    detect rest-frame UV lines in any of the clumps, implying fluxes ≲2×10−17 erg s−1 cm−2
    (3σ). We perform CLOUDY modelling to constrain the metallicity and the ionizing
    nature of CR7. CR7 seems to be actively forming stars without any clear active
    galactic nucleus activity in clump A, consistent with a metallicity of ∼0.05–0.2 Z⊙.
    Component C or an interclump component between B and C may host a high ionization
    source. Our results highlight the need for spatially resolved information to study
    the formation and assembly of early galaxies.
acknowledgement: We thank the anonymous reviewer for the numerous detailed comments
  that led us to greatly improve the quality, extent, and statistical robustness of
  this work. DS acknowledges financial support from the Netherlands Organisation for
  Scientific research through a Veni fellowship. JM acknowledges the support of a
  Huygens PhD fellowship from Leiden University. AF acknowledges support from the
  ERC Advanced Grant INTERSTELLAR H2020/740120. BD acknowledges financial support
  from NASA through the Astrophysics Data Analysis Program, grant number NNX12AE20G
  and the National Science Foundation, grant number 1716907. We are thankful for several
  discussions and constructive comments from Johannes Zabl, Eros Vanzella, Bo Milvang-Jensen,
  Henry McCracken, Max Gronke, Mark Dijkstra, Richard Ellis, and Nicolas Laporte.
  We also thank Umar Burhanudin and Izzy Garland for taking part in the XGAL internship
  in Lancaster and for exploring the HST grism data independently. Based on observations
  obtained with HST/WFC3 programs 12578, 14495, and 14596. Based on observations of
  the National Japanese Observatory with the Suprime-Cam on the Subaru telescope (S14A-086)
  on the big island of Hawaii. This work is based in part on data products produced
  at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France–Hawaii
  Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on data
  products from observations made with ESO Telescopes at the La Silla Paranal Observatory
  under ESO programme IDs 294.A-5018, 294.A-5039, 092.A 0786, 093.A-0561, 097.A0043,
  097.A-0943, 098.A-0819, 298.A-5012, and 179.A-2005, and on data products produced
  by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.
  The authors acknowledge the award of service time (SW2014b20) on the William Herschel
  Telescope (WHT). WHT and its service programme are operated on the island of La
  Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos
  of the Instituto de Astrofisica de Canarias. This research was supported by the
  Munich Institute for Astro- and Particle Physics of the DFG cluster of excellence
  ‘Origin and Structure of the Universe’. We have benefitted immensely from the public
  available programming language PYTHON, including NUMPY and SCIPY (Jones et al. 2001;
  Van Der Walt, Colbert & Varoquaux 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy
  Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This
  research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France.
  All data used for this paper are publicly available, and we make all reduced data
  available with the refereed paper.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- 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: Gabriel
  full_name: Brammer, Gabriel
  last_name: Brammer
- first_name: Andrea
  full_name: Ferrara, Andrea
  last_name: Ferrara
- first_name: Lara
  full_name: Alegre, Lara
  last_name: Alegre
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
- first_name: Daniel
  full_name: Schaerer, Daniel
  last_name: Schaerer
- first_name: Bahram
  full_name: Mobasher, Bahram
  last_name: Mobasher
- first_name: Behnam
  full_name: Darvish, Behnam
  last_name: Darvish
citation:
  ama: Sobral D, Matthee JJ, Brammer G, et al. On the nature and physical conditions
    of the luminous Ly α emitter CR7 and its rest-frame UV components. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2019;482(2):2422-2441. doi:<a href="https://doi.org/10.1093/mnras/sty2779">10.1093/mnras/sty2779</a>
  apa: Sobral, D., Matthee, J. J., Brammer, G., Ferrara, A., Alegre, L., Röttgering,
    H., … Darvish, B. (2019). On the nature and physical conditions of the luminous
    Ly α emitter CR7 and its rest-frame UV components. <i>Monthly Notices of the Royal
    Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/sty2779">https://doi.org/10.1093/mnras/sty2779</a>
  chicago: Sobral, David, Jorryt J Matthee, Gabriel Brammer, Andrea Ferrara, Lara
    Alegre, Huub Röttgering, Daniel Schaerer, Bahram Mobasher, and Behnam Darvish.
    “On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its
    Rest-Frame UV Components.” <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press, 2019. <a href="https://doi.org/10.1093/mnras/sty2779">https://doi.org/10.1093/mnras/sty2779</a>.
  ieee: D. Sobral <i>et al.</i>, “On the nature and physical conditions of the luminous
    Ly α emitter CR7 and its rest-frame UV components,” <i>Monthly Notices of the
    Royal Astronomical Society</i>, vol. 482, no. 2. Oxford University Press, pp.
    2422–2441, 2019.
  ista: Sobral D, Matthee JJ, Brammer G, Ferrara A, Alegre L, Röttgering H, Schaerer
    D, Mobasher B, Darvish B. 2019. On the nature and physical conditions of the luminous
    Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal
    Astronomical Society. 482(2), 2422–2441.
  mla: Sobral, David, et al. “On the Nature and Physical Conditions of the Luminous
    Ly α Emitter CR7 and Its Rest-Frame UV Components.” <i>Monthly Notices of the
    Royal Astronomical Society</i>, vol. 482, no. 2, Oxford University Press, 2019,
    pp. 2422–41, doi:<a href="https://doi.org/10.1093/mnras/sty2779">10.1093/mnras/sty2779</a>.
  short: D. Sobral, J.J. Matthee, G. Brammer, A. Ferrara, L. Alegre, H. Röttgering,
    D. Schaerer, B. Mobasher, B. Darvish, Monthly Notices of the Royal Astronomical
    Society 482 (2019) 2422–2441.
date_created: 2022-07-08T10:40:05Z
date_published: 2019-01-01T00:00:00Z
date_updated: 2022-08-19T06:49:36Z
day: '01'
doi: 10.1093/mnras/sty2779
extern: '1'
external_id:
  arxiv:
  - '1710.08422'
intvolume: '       482'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: ISM'
- 'cosmology: observations'
- dark ages
- reionization
- first stars
- early Universe
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1710.08422
month: '01'
oa: 1
oa_version: Preprint
page: 2422-2441
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: On the nature and physical conditions of the luminous Ly α emitter CR7 and
  its rest-frame UV components
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 482
year: '2019'
...
---
_id: '11508'
abstract:
- lang: eng
  text: Distant luminous Lyman-α emitters (LAEs) are excellent targets for spectroscopic
    observations of galaxies in the epoch of reionisation (EoR). We present deep high-resolution
    (R = 5000) VLT/X-shooter observations, along with an extensive collection of photometric
    data of COLA1, a proposed double peaked LAE at z = 6.6. We rule out the possibility
    that COLA1’s emission line is an [OII] doublet at z = 1.475 on the basis of i)
    the asymmetric red line-profile and flux ratio of the peaks (blue/red=0.31 ± 0.03)
    and ii) an unphysical [OII]/Hα ratio ([OII]/Hα >  22). We show that COLA1’s observed
    B-band flux is explained by a faint extended foreground LAE, for which we detect
    Lyα and [OIII] at z = 2.142. We thus conclude that COLA1 is a real double-peaked
    LAE at z = 6.593, the first discovered at z >  6. COLA1 is UV luminous (M1500 = −21.6 ± 0.3),
    has a high equivalent width (EW0,Lyα = 120−40+50 Å) and very compact Lyα emission
    (r50,Lyα = 0.33−0.04+0.07 kpc). Relatively weak inferred Hβ+[OIII] line-emission
    from Spitzer/IRAC indicates an extremely low metallicity of Z <  1/20 Z⊙ or reduced
    strength of nebular lines due to high escape of ionising photons. The small Lyα
    peak separation of 220 ± 20 km s−1 implies a low HI column density and an ionising
    photon escape fraction of ≈15 − 30%, providing the first direct evidence that
    such galaxies contribute actively to the reionisation of the Universe at z >  6.
    Based on simple estimates, we find that COLA1 could have provided just enough
    photons to reionise its own ≈0.3 pMpc (2.3 cMpc) bubble, allowing the blue Lyα
    line to be observed. However, we also discuss alternative scenarios explaining
    the detected double peaked nature of COLA1. Our results show that future high-resolution
    observations of statistical samples of double peaked LAEs at z >  5 are a promising
    probe of the occurrence of ionised regions around galaxies in the EoR.
acknowledgement: JM acknowledges the award of a Huygens PhD fellowship from Leiden
  University. MG acknowledges support from NASA grant NNX17AK58G. APA, PhD::SPACE
  fellow, acknowledges support from the FCT through the fellowship PD/BD/52706/2014.
  Based on observations made with ESO Telescopes at the La Silla Paranal Observatory
  under programme IDs 294.A-5018, 098.A-0819, 099.A-0254 and 0100.A-0213. We are grateful
  for the excellent data-sets from the COSMOS and UltraVISTA survey teams. This research
  was supported by the Munich Institute for Astro- and Particle Physics (MIAPP) of
  the DFG cluster of excellence “Origin and Structure of the Universe”. We thank the
  referee for their comments that improved the paper. We also thank Christoph Behrens,
  Len Cowie, Koki Kakiichi, Peter Laursen, Charlotte Mason, Eros Vanzella, Lewis Weinberger
  and Johannes Zabl for discussions. We have benefited from the public available programming
  language Python, including the numpy, matplotlib, scipy and astropy packages (Hunter
  2007; Astropy Collaboration 2013), the astronomical imaging tools Swarp (Bertin
  2010) and ds9 and the Topcat analysis tool (Taylor 2013).
article_number: A136
article_processing_charge: No
article_type: original
arxiv: 1
author:
- 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: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Max
  full_name: Gronke, Max
  last_name: Gronke
- first_name: Ana
  full_name: Paulino-Afonso, Ana
  last_name: Paulino-Afonso
- first_name: Mauro
  full_name: Stefanon, Mauro
  last_name: Stefanon
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
citation:
  ama: 'Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H.
    Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly
    contributing to the reionisation of the universe. <i>Astronomy &#38; Astrophysics</i>.
    2018;619. doi:<a href="https://doi.org/10.1051/0004-6361/201833528">10.1051/0004-6361/201833528</a>'
  apa: 'Matthee, J. J., Sobral, D., Gronke, M., Paulino-Afonso, A., Stefanon, M.,
    &#38; Röttgering, H. (2018). Confirmation of double peaked Lyα emission at z =
    6.593: Witnessing a galaxy directly contributing to the reionisation of the universe.
    <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/201833528">https://doi.org/10.1051/0004-6361/201833528</a>'
  chicago: 'Matthee, Jorryt J, David Sobral, Max Gronke, Ana Paulino-Afonso, Mauro
    Stefanon, and Huub Röttgering. “Confirmation of Double Peaked Lyα Emission at
    z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the
    Universe.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2018. <a href="https://doi.org/10.1051/0004-6361/201833528">https://doi.org/10.1051/0004-6361/201833528</a>.'
  ieee: 'J. J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, and
    H. Röttgering, “Confirmation of double peaked Lyα emission at z = 6.593: Witnessing
    a galaxy directly contributing to the reionisation of the universe,” <i>Astronomy
    &#38; Astrophysics</i>, vol. 619. EDP Sciences, 2018.'
  ista: 'Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering
    H. 2018. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a
    galaxy directly contributing to the reionisation of the universe. Astronomy &#38;
    Astrophysics. 619, A136.'
  mla: 'Matthee, Jorryt J., et al. “Confirmation of Double Peaked Lyα Emission at
    z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the
    Universe.” <i>Astronomy &#38; Astrophysics</i>, vol. 619, A136, EDP Sciences,
    2018, doi:<a href="https://doi.org/10.1051/0004-6361/201833528">10.1051/0004-6361/201833528</a>.'
  short: J.J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, H. Röttgering,
    Astronomy &#38; Astrophysics 619 (2018).
date_created: 2022-07-06T11:14:23Z
date_published: 2018-11-19T00:00:00Z
date_updated: 2022-07-19T09:32:08Z
day: '19'
doi: 10.1051/0004-6361/201833528
extern: '1'
external_id:
  arxiv:
  - '1805.11621'
intvolume: '       619'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / galaxies: formation / dark ages / reionization / first
  stars / techniques: spectroscopic / intergalactic medium'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1805.11621
month: '11'
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: 'Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy
  directly contributing to the reionisation of the universe'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 619
year: '2018'
...
---
_id: '11549'
abstract:
- lang: eng
  text: We investigate the clustering properties of ∼7000 H β + [O III] and [O II]
    narrowband-selected emitters at z ∼ 0.8–4.7 from the High-z Emission Line Survey.
    We find clustering lengths, r0, of 1.5–4.0 h−1 Mpc and minimum dark matter halo
    masses of 1010.7–12.1 M⊙ for our z = 0.8–3.2 H β + [O III] emitters and r0 ∼ 2.0–8.3
    h−1 Mpc and halo masses of 1011.5–12.6 M⊙ for our z = 1.5–4.7 [O II] emitters.
    We find r0 to strongly increase both with increasing line luminosity and redshift.
    By taking into account the evolution of the characteristic line luminosity, L⋆(z),
    and using our model predictions of halo mass given r0, we find a strong, redshift-independent
    increasing trend between L/L⋆(z) and minimum halo mass. The faintest H β + [O III]
    emitters are found to reside in 109.5 M⊙ haloes and the brightest emitters in
    1013.0 M⊙ haloes. For [O II] emitters, the faintest emitters are found in 1010.5
    M⊙ haloes and the brightest emitters in 1012.6 M⊙ haloes. A redshift-independent
    stellar mass dependency is also observed where the halo mass increases from 1011
    to 1012.5 M⊙ for stellar masses of 108.5 to 1011.5 M⊙, respectively. We investigate
    the interdependencies of these trends by repeating our analysis in a Lline−Mstar
    grid space for our most populated samples (H β + [O III] z = 0.84 and [O II] z
    = 1.47) and find that the line luminosity dependency is stronger than the stellar
    mass dependency on halo mass. For L > L⋆ emitters at all epochs, we find a relatively
    flat trend with halo masses of 1012.5–13 M⊙, which may be due to quenching mechanisms
    in massive haloes that is consistent with a transitional halo mass predicted by
    models.
acknowledgement: We thank the anonymous referee for their useful comments and suggestions
  that improved this study. AAK thanks Anahita Alavi and Irene Shivaei for useful
  discussion in the making of this paper. AAK acknowledges that this work was supported
  by NASA Headquarters under the NASA Earth and Space Science Fellowship Program –
  Grant NNX16AO92H. DS acknowledges financial support from the Netherlands Organization
  for Scientific Research (NWO) through a Veni fellowship and from Lancaster University
  through an Early Career Internal Grant A100679. PNB is grateful for support from
  STFC via grant STM001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the
  ERC Advanced Grant DUSTYGAL (321334), and a Royal Society/Wolfson Merit award. JM
  acknowledges the support of a Huygens PhD fellowship from Leiden University. BD
  acknowledges financial support from NASA through the Astrophysics Data Analysis
  Program (ADAP), grant number NNX12AE20G.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: A A
  full_name: Khostovan, A A
  last_name: Khostovan
- first_name: D
  full_name: Sobral, D
  last_name: Sobral
- first_name: B
  full_name: Mobasher, B
  last_name: Mobasher
- first_name: P N
  full_name: Best, P N
  last_name: Best
- first_name: I
  full_name: Smail, I
  last_name: Smail
- 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: B
  full_name: Darvish, B
  last_name: Darvish
- first_name: H
  full_name: Nayyeri, H
  last_name: Nayyeri
- first_name: S
  full_name: Hemmati, S
  last_name: Hemmati
- first_name: J P
  full_name: Stott, J P
  last_name: Stott
citation:
  ama: 'Khostovan AA, Sobral D, Mobasher B, et al. The clustering of H β + [O III]
    and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar
    mass. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;478(3):2999-3015.
    doi:<a href="https://doi.org/10.1093/mnras/sty925">10.1093/mnras/sty925</a>'
  apa: 'Khostovan, A. A., Sobral, D., Mobasher, B., Best, P. N., Smail, I., Matthee,
    J. J., … Stott, J. P. (2018). The clustering of H β + [O III] and [O II] emitters
    since z ∼ 5: Dependencies with line luminosity and stellar mass. <i>Monthly Notices
    of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/sty925">https://doi.org/10.1093/mnras/sty925</a>'
  chicago: 'Khostovan, A A, D Sobral, B Mobasher, P N Best, I Smail, Jorryt J Matthee,
    B Darvish, H Nayyeri, S Hemmati, and J P Stott. “The Clustering of H β + [O III]
    and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar
    Mass.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University
    Press, 2018. <a href="https://doi.org/10.1093/mnras/sty925">https://doi.org/10.1093/mnras/sty925</a>.'
  ieee: 'A. A. Khostovan <i>et al.</i>, “The clustering of H β + [O III] and [O II]
    emitters since z ∼ 5: Dependencies with line luminosity and stellar mass,” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 478, no. 3. Oxford University
    Press, pp. 2999–3015, 2018.'
  ista: 'Khostovan AA, Sobral D, Mobasher B, Best PN, Smail I, Matthee JJ, Darvish
    B, Nayyeri H, Hemmati S, Stott JP. 2018. The clustering of H β + [O III] and [O II]
    emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly
    Notices of the Royal Astronomical Society. 478(3), 2999–3015.'
  mla: 'Khostovan, A. A., et al. “The Clustering of H β + [O III] and [O II] Emitters
    since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 478, no. 3, Oxford University Press,
    2018, pp. 2999–3015, doi:<a href="https://doi.org/10.1093/mnras/sty925">10.1093/mnras/sty925</a>.'
  short: A.A. Khostovan, D. Sobral, B. Mobasher, P.N. Best, I. Smail, J.J. Matthee,
    B. Darvish, H. Nayyeri, S. Hemmati, J.P. Stott, Monthly Notices of the Royal Astronomical
    Society 478 (2018) 2999–3015.
date_created: 2022-07-08T11:48:48Z
date_published: 2018-08-01T00:00:00Z
date_updated: 2022-08-19T06:53:39Z
day: '01'
doi: 10.1093/mnras/sty925
extern: '1'
external_id:
  arxiv:
  - '1705.01101'
intvolume: '       478'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: haloes'
- 'galaxies: high-redshift'
- 'galaxies: star formation'
- 'cosmology: observations'
- large-scale structure of Universe
language:
- iso: eng
main_file_link:
- url: https://arxiv.org/abs/1705.01101
month: '08'
oa_version: Published Version
page: 2999-3015
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: 'The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies
  with line luminosity and stellar mass'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 478
year: '2018'
...
---
_id: '11555'
abstract:
- lang: eng
  text: We investigate the morphology of the [C II] emission in a sample of ‘normal’
    star-forming galaxies at 5 < z < 7.2 in relation to their UV (rest-frame) counterpart.
    We use new Atacama Large Millimetre/submillimetre Array (ALMA) observations of
    galaxies at z ∼ 6–7, as well as a careful re-analysis of archival ALMA data. In
    total 29 galaxies were analysed, 21 of which are detected in [C II]. For several
    of the latter the [C II] emission breaks into multiple components. Only a fraction
    of these [C II] components, if any, is associated with the primary UV systems,
    while the bulk of the [C II] emission is associated either with fainter UV components,
    or not associated with any UV counterpart at the current limits. By taking into
    account the presence of all these components, we find that the L[CII]–SFR (star
    formation rate) relation at early epochs is fully consistent with the local relation,
    but it has a dispersion of 0.48 ± 0.07 dex, which is about two times larger than
    observed locally. We also find that the deviation from the local L[CII]–SFR relation
    has a weak anticorrelation with the EW(Ly α). The morphological analysis also
    reveals that [C II] emission is generally much more extended than the UV emission.
    As a consequence, these primordial galaxies are characterized by a [C II] surface
    brightness generally much lower than expected from the local Σ[CII]−ΣSFR relation.
    These properties are likely a consequence of a combination of different effects,
    namely gas metallicity, [C II] emission from obscured star-forming regions, strong
    variations of the ionization parameter, and circumgalactic gas in accretion or
    ejected by these primeval galaxies.
acknowledgement: "This paper makes use of the following ALMA data:\r\nADS/JAO.ALMA#2012.1.00719.S,
  ADS/JAO.ALMA#2012.A.00040.S,\r\nADS/JAO.ALMA#2013.A.00433.S, ADS/JAO.ALMA#2011.0.00115.S,\r\nADS/JAO.ALMA#2012.1.00033.S,
  ADS/JAO.ALMA#2012.1.00523.S,\r\nADS/JAO.ALMA#2013.1.00815.S, ADS/JAO.ALMA#2015.1.00834.S.,\r\nADS/JAO.ALMA#2015.1.01105.S,
  AND ADS/JAO.ALMA#2016.1.01240.S\r\nwhich can be retrieved from the ALMA data archive:\r\nhttps://almascience.eso.org/
  alma-data/archive. ALMA is a partnership of ESO (representing its member states),
  NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan),
  in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated
  by ESO, AUI/NRAO, and NAOJ. We are grateful to G. Jones to for providing his [C
  II] flux maps. RM and SC acknowledge support by the Science and Technology Facilities
  Council (STFC). RM acknowledges ERC Advanced Grant 695671 ‘QUENCH’. AF acknowledges
  support from the ERC Advanced Grant INTERSTELLAR H2020/740120."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: S
  full_name: Carniani, S
  last_name: Carniani
- first_name: R
  full_name: Maiolino, R
  last_name: Maiolino
- first_name: R
  full_name: Amorin, R
  last_name: Amorin
- first_name: L
  full_name: Pentericci, L
  last_name: Pentericci
- first_name: A
  full_name: Pallottini, A
  last_name: Pallottini
- first_name: A
  full_name: Ferrara, A
  last_name: Ferrara
- first_name: C J
  full_name: Willott, C J
  last_name: Willott
- first_name: R
  full_name: Smit, R
  last_name: Smit
- 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: D
  full_name: Sobral, D
  last_name: Sobral
- first_name: P
  full_name: Santini, P
  last_name: Santini
- first_name: M
  full_name: Castellano, M
  last_name: Castellano
- first_name: S
  full_name: De Barros, S
  last_name: De Barros
- first_name: A
  full_name: Fontana, A
  last_name: Fontana
- first_name: A
  full_name: Grazian, A
  last_name: Grazian
- first_name: L
  full_name: Guaita, L
  last_name: Guaita
citation:
  ama: Carniani S, Maiolino R, Amorin R, et al. Kiloparsec-scale gaseous clumps and
    star formation at z = 5–7. <i>Monthly Notices of the Royal Astronomical Society</i>.
    2018;478(1):1170-1184. doi:<a href="https://doi.org/10.1093/mnras/sty1088">10.1093/mnras/sty1088</a>
  apa: Carniani, S., Maiolino, R., Amorin, R., Pentericci, L., Pallottini, A., Ferrara,
    A., … Guaita, L. (2018). Kiloparsec-scale gaseous clumps and star formation at
    z = 5–7. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University
    Press. <a href="https://doi.org/10.1093/mnras/sty1088">https://doi.org/10.1093/mnras/sty1088</a>
  chicago: Carniani, S, R Maiolino, R Amorin, L Pentericci, A Pallottini, A Ferrara,
    C J Willott, et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at z = 5–7.”
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press,
    2018. <a href="https://doi.org/10.1093/mnras/sty1088">https://doi.org/10.1093/mnras/sty1088</a>.
  ieee: S. Carniani <i>et al.</i>, “Kiloparsec-scale gaseous clumps and star formation
    at z = 5–7,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478,
    no. 1. Oxford University Press, pp. 1170–1184, 2018.
  ista: Carniani S, Maiolino R, Amorin R, Pentericci L, Pallottini A, Ferrara A, Willott
    CJ, Smit R, Matthee JJ, Sobral D, Santini P, Castellano M, De Barros S, Fontana
    A, Grazian A, Guaita L. 2018. Kiloparsec-scale gaseous clumps and star formation
    at z = 5–7. Monthly Notices of the Royal Astronomical Society. 478(1), 1170–1184.
  mla: Carniani, S., et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at
    z = 5–7.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478,
    no. 1, Oxford University Press, 2018, pp. 1170–84, doi:<a href="https://doi.org/10.1093/mnras/sty1088">10.1093/mnras/sty1088</a>.
  short: S. Carniani, R. Maiolino, R. Amorin, L. Pentericci, A. Pallottini, A. Ferrara,
    C.J. Willott, R. Smit, J.J. Matthee, D. Sobral, P. Santini, M. Castellano, S.
    De Barros, A. Fontana, A. Grazian, L. Guaita, Monthly Notices of the Royal Astronomical
    Society 478 (2018) 1170–1184.
date_created: 2022-07-11T08:05:42Z
date_published: 2018-07-01T00:00:00Z
date_updated: 2022-08-19T06:58:06Z
day: '01'
doi: 10.1093/mnras/sty1088
extern: '1'
external_id:
  arxiv:
  - '1712.03985'
intvolume: '       478'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: ISM'
- 'galaxies: formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1712.03985
month: '07'
oa: 1
oa_version: Preprint
page: 1170-1184
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: Kiloparsec-scale gaseous clumps and star formation at z = 5–7
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 478
year: '2018'
...
---
_id: '11557'
abstract:
- lang: eng
  text: Deep narrow-band surveys have revealed a large population of faint Ly α emitters
    (LAEs) in the distant Universe, but relatively little is known about the most
    luminous sources (⁠LLyα≳1042.7 erg s−1; LLyα≳L∗Lyα⁠). Here we present the spectroscopic
    follow-up of 21 luminous LAEs at z ∼ 2–3 found with panoramic narrow-band surveys
    over five independent extragalactic fields (≈4 × 106 Mpc3 surveyed at z ∼ 2.2
    and z ∼ 3.1). We use WHT/ISIS, Keck/DEIMOS, and VLT/X-SHOOTER to study these sources
    using high ionization UV lines. Luminous LAEs at z ∼ 2–3 have blue UV slopes (⁠β=−2.0+0.3−0.1⁠)
    and high Ly α escape fractions (⁠50+20−15 per cent) and span five orders of magnitude
    in UV luminosity (MUV ≈ −19 to −24). Many (70 per cent) show at least one high
    ionization rest-frame UV line such as C IV, N V, C III], He II or O III], typically
    blue-shifted by ≈100–200 km s−1 relative to Ly α. Their Ly α profiles reveal a
    wide variety of shapes, including significant blue-shifted components and widths
    from 200 to 4000 km s−1. Overall, 60 ± 11  per cent appear to be active galactic
    nucleus (AGN) dominated, and at LLyα > 1043.3 erg s−1 and/or MUV < −21.5 virtually
    all LAEs are AGNs with high ionization parameters (log U = 0.6 ± 0.5) and with
    metallicities of ≈0.5 − 1 Z⊙. Those lacking signatures of AGNs (40 ± 11  per cent)
    have lower ionization parameters (⁠logU=−3.0+1.6−0.9 and log ξion = 25.4 ± 0.2)
    and are apparently metal-poor sources likely powered by young, dust-poor ‘maximal’
    starbursts. Our results show that luminous LAEs at z ∼ 2–3 are a diverse population
    and that 2×L∗Lyα and 2×M∗UV mark a sharp transition in the nature of LAEs, from
    star formation dominated to AGN dominated.
acknowledgement: 'We thank the anonymous reviewer for their timely and constructive
  comments that greatly helped us to improve the manuscript. DS acknowledges financial
  support from the Netherlands Organization for Scientific research (NWO) through
  a Veni fellowship and from Lancaster University through an Early Career Internal
  Grant A100679. JM acknowledges the support of a Huygens PhD fellowship from Leiden
  University. BD acknowledges financial support from NASA through the Astrophysics
  Data Analysis Program (ADAP), grant number NNX12AE20G, and the National Science
  Foundation, grant number 1716907. IRS acknowledges support from the ERC Advanced
  Grant DUSTYGAL (321334), STFC (ST/P000541/1), and a Royal Society/Wolfson Merit
  Award. PNB is grateful for support from STFC via grant ST/M001229/1. We thank Anne
  Verhamme, Kimihiko Nakajima, Ryan Trainor, Sangeeta Malhotra, Max Gronke, James
  Rhoads, Fang Xia An, Matthew Hayes, Takashi Kojima, Mark Dijkstra, and Anne Jaskot
  for many helpful and engaging discussions, particularly during the SnowCLAW Ly α
  workshop. We thank Bruno Ribeiro, Stephane Charlot, and Joseph Caruana for comments
  on the manuscript. The authors would also like to thank Ingrid Tengs, Meg Singleton,
  Ali Khostovan, and Sara Perez for participating in part of the observations. We
  also thank Joao Calhau, Leah Morabito, Sergio Santos, and Aayush Saxena for their
  assistance with the narrow-band observations which allowed to select some of the
  sour ces. Based on observations obtained with the William Herschel Telescope, program:
  W16AN004; the Very Large Telescope, programs: 098.A-0819 & 099.A-0254; and the Keck
  II telescope, program: C267D. Based on data products from observations made with
  ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018,
  294.A-5039, 092.A-0786, 093.A-0561, 097.A-0943, 098.A-0819, 099.A-0254 and 179.A-2005.
  The authors acknowledge the award of service time (SW2014b20) on the WHT. WHT and
  its service programme are operated on the island of La Palma by the Isaac Newton
  Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de
  Astrofisica de Canarias. The authors would also like to thank all the extremely
  helpful observatory staff that have greatly contributed towards our observations,
  particularly Fiona Riddick, Lilian Dominguez, Florencia Jimenez, and Ian Skillen.
  We have benefited greatly from the publicly available programming language PYTHON,
  including the NUMPY & SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al.
  2001), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and
  the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR
  catalogue access tool, CDS, Strasbourg, France.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- 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: Behnam
  full_name: Darvish, Behnam
  last_name: Darvish
- first_name: Ian
  full_name: Smail, Ian
  last_name: Smail
- first_name: Philip N
  full_name: Best, Philip N
  last_name: Best
- first_name: Lara
  full_name: Alegre, Lara
  last_name: Alegre
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
- first_name: Bahram
  full_name: Mobasher, Bahram
  last_name: Mobasher
- first_name: Ana
  full_name: Paulino-Afonso, Ana
  last_name: Paulino-Afonso
- first_name: Andra
  full_name: Stroe, Andra
  last_name: Stroe
- first_name: Iván
  full_name: Oteo, Iván
  last_name: Oteo
citation:
  ama: 'Sobral D, Matthee JJ, Darvish B, et al. The nature of luminous Ly α emitters
    at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. <i>Monthly Notices
    of the Royal Astronomical Society</i>. 2018;477(2):2817-2840. doi:<a href="https://doi.org/10.1093/mnras/sty782">10.1093/mnras/sty782</a>'
  apa: 'Sobral, D., Matthee, J. J., Darvish, B., Smail, I., Best, P. N., Alegre, L.,
    … Oteo, I. (2018). The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor
    starbursts and highly ionizing AGN. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/sty782">https://doi.org/10.1093/mnras/sty782</a>'
  chicago: 'Sobral, David, Jorryt J Matthee, Behnam Darvish, Ian Smail, Philip N Best,
    Lara Alegre, Huub Röttgering, et al. “The Nature of Luminous Ly α Emitters at
    z ∼ 2–3: Maximal Dust-Poor Starbursts and Highly Ionizing AGN.” <i>Monthly Notices
    of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href="https://doi.org/10.1093/mnras/sty782">https://doi.org/10.1093/mnras/sty782</a>.'
  ieee: 'D. Sobral <i>et al.</i>, “The nature of luminous Ly α emitters at z ∼ 2–3:
    Maximal dust-poor starbursts and highly ionizing AGN,” <i>Monthly Notices of the
    Royal Astronomical Society</i>, vol. 477, no. 2. Oxford University Press, pp.
    2817–2840, 2018.'
  ista: 'Sobral D, Matthee JJ, Darvish B, Smail I, Best PN, Alegre L, Röttgering H,
    Mobasher B, Paulino-Afonso A, Stroe A, Oteo I. 2018. The nature of luminous Ly
    α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly
    Notices of the Royal Astronomical Society. 477(2), 2817–2840.'
  mla: 'Sobral, David, et al. “The Nature of Luminous Ly α Emitters at z ∼ 2–3: Maximal
    Dust-Poor Starbursts and Highly Ionizing AGN.” <i>Monthly Notices of the Royal
    Astronomical Society</i>, vol. 477, no. 2, Oxford University Press, 2018, pp.
    2817–40, doi:<a href="https://doi.org/10.1093/mnras/sty782">10.1093/mnras/sty782</a>.'
  short: D. Sobral, J.J. Matthee, B. Darvish, I. Smail, P.N. Best, L. Alegre, H. Röttgering,
    B. Mobasher, A. Paulino-Afonso, A. Stroe, I. Oteo, Monthly Notices of the Royal
    Astronomical Society 477 (2018) 2817–2840.
date_created: 2022-07-12T07:18:02Z
date_published: 2018-06-01T00:00:00Z
date_updated: 2022-08-19T07:01:08Z
day: '01'
doi: 10.1093/mnras/sty782
extern: '1'
external_id:
  arxiv:
  - '1802.10102'
intvolume: '       477'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: active'
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: ISM'
- 'galaxies: starburst'
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1802.10102
month: '06'
oa: 1
oa_version: Preprint
page: 2817-2840
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: 'The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts
  and highly ionizing AGN'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 477
year: '2018'
...
---
_id: '11558'
abstract:
- lang: eng
  text: We present and explore deep narrow- and medium-band data obtained with the
    Subaru and the Isaac Newton Telescopes in the ∼2 deg2 COSMOS field. We use these
    data as an extremely wide, low-resolution (R ∼ 20–80) Integral Field Unit survey
    to slice through the COSMOS field and obtain a large sample of ∼4000 Ly α emitters
    (LAEs) from z ∼ 2 to 6 in 16 redshift slices (SC4K). We present new Ly α luminosity
    functions (LFs) covering a comoving volume of ∼108 Mpc3. SC4K extensively complements
    ultradeep surveys, jointly covering over 4 dex in Ly α luminosity and revealing
    a global (2.5 < z < 6) synergy LF with α=−1.93+0.12−0.12⁠, log10Φ∗Lyα=−3.45+0.22−0.29 Mpc−3,
    and log10L∗Lyα=42.93+0.15−0.11 erg s−1. The Schechter component of the Ly α LF
    reveals a factor ∼5 rise in L∗Lyα and a ∼7 × decline in Φ∗Lyα from z ∼ 2 to 6.
    The data reveal an extra power-law (or Schechter) component above LLy α ≈ 1043.3 erg s−1
    at z ∼ 2.2–3.5 and we show that it is partially driven by X-ray and radio active
    galactic nucleus (AGN), as their Ly α LF resembles the excess. The power-law component
    vanishes and/or is below our detection limits above z > 3.5, likely linked with
    the evolution of the AGN population. The Ly α luminosity density rises by a factor
    ∼2 from z ∼ 2 to 3 but is then found to be roughly constant (⁠1.1+0.2−0.2×1040 erg s−1 Mpc−3)
    to z ∼ 6, despite the ∼0.7 dex drop in ultraviolet (UV) luminosity density. The
    Ly α/UV luminosity density ratio rises from 4 ± 1 per cent to 30 ± 6 per cent
    from z ∼ 2.2 to 6. Our results imply a rise of a factor of ≈2 in the global ionization
    efficiency (ξion) and a factor ≈4 ± 1 in the Ly α escape fraction from z ∼ 2 to
    6, hinting for evolution in both the typical burstiness/stellar populations and
    even more so in the typical interstellar medium conditions allowing Ly α photons
    to escape.
acknowledgement: "We thank the anonymous referee for their constructive comments that
  helped us improve the manuscript. DS acknowledges the hospitality of the IAC and
  a Severo Ochoa visiting grant. SS and JC acknowledge studentships from the Lancaster
  University. JM acknowledges a Huygens PhD fellowship from Leiden University. APA
  acknowledges financial support from the Science and Technology Foundation (FCT,
  Portugal) through research grants UID/FIS/04434/2013 and fellowship PD/BD/52706/2014.
  The authors thank Alyssa Drake, Kimihiko Nakajima, Yuichi Harikane, Max Gronke,
  Irene Shivaei, Helmut Dannerbauer, Huub Rottgering, ¨ Marius Eide, and Masami Ouchi
  for many engaging and stimulating discussions. We also thank Sara Perez, Alex Bennett,
  and Tom Rose for their involvement in the early stages of this project. Based on
  data products from observations made with European Southern Observatory (ESO) Telescopes
  at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 097.A 0943,\r\n098.A-0819,
  099.A-0254, and 179.A-2005 and on data products produced by TERAPIX and the Cambridge
  Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations
  using the WFC on the 2.5 m INT, as part of programmes 2013AN002, 2013BN008, 2014AC88,
  2014AN002, 2014BN006, 2014BC118, and 2016AN001. The INT is operated on the island
  of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los
  Muchachos of the Instituto de Astrofisica de Canarias. This work is based in part
  on data products produced at TERAPIX available at the Canadian Astronomy Data Centre
  as part of the Canada–France– Hawaii Telescope Legacy Survey (CFHTLS), a collaborative
  project of NRC and CNRS.\r\nWe are grateful to the CFHTLS, COSMOS-UltraVISTA, and
  COSMOS survey teams. We are also unmeasurably thankful to the pioneering and continuous
  work from previous Ly α surveys’ teams. Without these previous Ly α and the wider
  reach legacy surveys, this research would have been impossible. We also thank the
  VUDS team for making available spectroscopic redshifts from data obtained with VIMOS
  at the European Southern Observatory Very Large Telescope, Paranal, Chile, under
  Large Programme 185.A-0791. Finally, the authors acknowledge the unique value of
  the publicly available programming language PYTHON, including the NUMPY and SCIPY
  (Van Der Walt, Colbert & Varoquaux 2011; Jones et al. 2001), MATPLOTLIB (Hunter
  2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program
  (Taylor 2005). We publicly release a catalogue with all LAEs used in this paper
  (SC4K), so it can be freely explored by the community (see five example entries
  in Table A1)."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Sérgio
  full_name: Santos, Sérgio
  last_name: Santos
- 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: Ana
  full_name: Paulino-Afonso, Ana
  last_name: Paulino-Afonso
- first_name: Bruno
  full_name: Ribeiro, Bruno
  last_name: Ribeiro
- first_name: João
  full_name: Calhau, João
  last_name: Calhau
- first_name: Ali A
  full_name: Khostovan, Ali A
  last_name: Khostovan
citation:
  ama: 'Sobral D, Santos S, Matthee JJ, et al. Slicing COSMOS with SC4K: The evolution
    of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2018;476(4):4725-4752. doi:<a href="https://doi.org/10.1093/mnras/sty378">10.1093/mnras/sty378</a>'
  apa: 'Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Ribeiro, B., Calhau,
    J., &#38; Khostovan, A. A. (2018). Slicing COSMOS with SC4K: The evolution of
    typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/sty378">https://doi.org/10.1093/mnras/sty378</a>'
  chicago: 'Sobral, David, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso, Bruno
    Ribeiro, João Calhau, and Ali A Khostovan. “Slicing COSMOS with SC4K: The Evolution
    of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018.
    <a href="https://doi.org/10.1093/mnras/sty378">https://doi.org/10.1093/mnras/sty378</a>.'
  ieee: 'D. Sobral <i>et al.</i>, “Slicing COSMOS with SC4K: The evolution of typical
    Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6,” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 476, no. 4. Oxford University Press,
    pp. 4725–4752, 2018.'
  ista: 'Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Ribeiro B, Calhau J, Khostovan
    AA. 2018. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and
    the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical
    Society. 476(4), 4725–4752.'
  mla: 'Sobral, David, et al. “Slicing COSMOS with SC4K: The Evolution of Typical
    Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 476, no. 4, Oxford University Press,
    2018, pp. 4725–52, doi:<a href="https://doi.org/10.1093/mnras/sty378">10.1093/mnras/sty378</a>.'
  short: D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, B. Ribeiro, J. Calhau,
    A.A. Khostovan, Monthly Notices of the Royal Astronomical Society 476 (2018) 4725–4752.
date_created: 2022-07-12T10:41:08Z
date_published: 2018-06-01T00:00:00Z
date_updated: 2022-08-19T07:04:45Z
day: '01'
doi: 10.1093/mnras/sty378
extern: '1'
external_id:
  arxiv:
  - '1712.04451'
intvolume: '       476'
issue: '4'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: high-redshift'
- 'galaxies: luminosity function'
- mass function
- 'galaxies: statistics'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1712.04451
month: '06'
oa: 1
oa_version: Preprint
page: 4725-4752
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: 'Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α
  escape fraction from z ∼ 2 to 6'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 476
year: '2018'
...
---
_id: '11584'
abstract:
- lang: eng
  text: Observations show that star-forming galaxies reside on a tight 3D plane between
    mass, gas-phase metallicity, and star formation rate (SFR), which can be explained
    by the interplay between metal-poor gas inflows, SFR and outflows. However, different
    metals are released on different time-scales, which may affect the slope of this
    relation. Here, we use central, star-forming galaxies with Mstar = 109.0–10.5
    M⊙ from the EAGLE hydrodynamical simulation to examine 3D relations between mass,
    SFR, and chemical enrichment using absolute and relative C, N, O, and Fe abundances.
    We show that the scatter is smaller when gas-phase α-enhancement is used rather
    than metallicity. A similar plane also exists for stellar α-enhancement, implying
    that present-day specific SFRs are correlated with long time-scale star formation
    histories. Between z = 0 and 1, the α-enhancement plane is even more insensitive
    to redshift than the plane using metallicity. However, it evolves at z > 1 due
    to lagging iron yields. At fixed mass, galaxies with higher SFRs have star formation
    histories shifted towards late times, are more α-enhanced, and this α-enhancement
    increases with redshift as observed. These findings suggest that relations between
    physical properties inferred from observations may be affected by systematic variations
    in α-enhancements.
acknowledgement: We thank the anonymous referee for their constructive comments. JM
  acknowledges the support of a Huygens PhD fellowship from Leiden University. We
  thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge
  the use of the TOPCAT software (Taylor 2013) for assisting in rapid exploration
  of multidimensional data sets and the use of PYTHON and its NUMPY, MATPLOTLIB, and
  PANDAS packages.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- 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
citation:
  ama: 'Matthee JJ, Schaye J. Star-forming galaxies are predicted to lie on a fundamental
    plane of mass, star formation rate, and α-enhancement. <i>Monthly Notices of the
    Royal Astronomical Society: Letters</i>. 2018;479(1):L34-L39. doi:<a href="https://doi.org/10.1093/mnrasl/sly093">10.1093/mnrasl/sly093</a>'
  apa: 'Matthee, J. J., &#38; Schaye, J. (2018). Star-forming galaxies are predicted
    to lie on a fundamental plane of mass, star formation rate, and α-enhancement.
    <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University
    Press. <a href="https://doi.org/10.1093/mnrasl/sly093">https://doi.org/10.1093/mnrasl/sly093</a>'
  chicago: 'Matthee, Jorryt J, and Joop Schaye. “Star-Forming Galaxies Are Predicted
    to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.”
    <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University
    Press, 2018. <a href="https://doi.org/10.1093/mnrasl/sly093">https://doi.org/10.1093/mnrasl/sly093</a>.'
  ieee: 'J. J. Matthee and J. Schaye, “Star-forming galaxies are predicted to lie
    on a fundamental plane of mass, star formation rate, and α-enhancement,” <i>Monthly
    Notices of the Royal Astronomical Society: Letters</i>, vol. 479, no. 1. Oxford
    University Press, pp. L34–L39, 2018.'
  ista: 'Matthee JJ, Schaye J. 2018. Star-forming galaxies are predicted to lie on
    a fundamental plane of mass, star formation rate, and α-enhancement. Monthly Notices
    of the Royal Astronomical Society: Letters. 479(1), L34–L39.'
  mla: 'Matthee, Jorryt J., and Joop Schaye. “Star-Forming Galaxies Are Predicted
    to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.”
    <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 479, no.
    1, Oxford University Press, 2018, pp. L34–39, doi:<a href="https://doi.org/10.1093/mnrasl/sly093">10.1093/mnrasl/sly093</a>.'
  short: 'J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society:
    Letters 479 (2018) L34–L39.'
date_created: 2022-07-14T12:49:47Z
date_published: 2018-09-01T00:00:00Z
date_updated: 2022-08-19T08:35:45Z
day: '01'
doi: 10.1093/mnrasl/sly093
extern: '1'
external_id:
  arxiv:
  - '1802.06786'
intvolume: '       479'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: abundances'
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: star formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1802.06786
month: '09'
oa: 1
oa_version: Preprint
page: L34 - L39
publication: 'Monthly Notices of the Royal Astronomical Society: Letters'
publication_identifier:
  eissn:
  - 1745-3933
  issn:
  - 1745-3925
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Star-forming galaxies are predicted to lie on a fundamental plane of mass,
  star formation rate, and α-enhancement
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 479
year: '2018'
...
---
_id: '11518'
abstract:
- lang: eng
  text: "We present spectroscopic follow-up observations of CR7 with ALMA, targeted
    at constraining the infrared (IR) continuum and [C II]158 mm line-emission at
    high spatial resolution matched to the HST/WFC3 imaging. CR7 is a luminous Lyα
    emitting galaxy at z = 6.6 that consists of three separated UV-continuum components.
    Our observations reveal several well-separated components of [C II] emission.
    The two most luminous components in [C II] coincide with the brightest UV components
    (A and B), blueshifted by »150 km s−1 with respect to the\r\npeak of Lyα emission.
    Other [C II] components are observed close to UV clumps B and C and are blueshifted
    by »300 and ≈80 km s−1 with respect to the systemic redshift. We do not detect
    FIR continuum emission due to dust with a 3σ limiting luminosity LIR T L d 35
    K 3.1 10 = <´ 10 ( ) . This allows us to mitigate uncertainties in the dust-corrected
    SFR and derive SFRs for the three UV clumps A, B, and C of 28, 5, and 7 M yr−1.
    All clumps have [C II] luminosities consistent within the scatter observed in
    the local relation between SFR and L[ ] C II , implying that strong Lyα emission
    does not necessarily anti-correlate with [C II] luminosity. Combining\r\nour measurements
    with the literature, we show that galaxies with blue UV slopes have weaker [C
    II] emission at fixed SFR, potentially due to their lower metallicities and/or
    higher photoionization. Comparison with hydrodynamical simulations suggests that
    CR7ʼs clumps have metallicities of 0.1 Z Z 0.2 < < . The observed ISM structure
    of CR7 indicates that we are likely witnessing the build up of a central galaxy
    in the early universe through complex accretion of satellites."
acknowledgement: 'We thank the referee for their constructive comments, which have
  helped improve the quality and clarity of this work. We thank Raffaella Schneider
  for comments on an earlier version of this paper. We thank Leindert Boogaard, Steven
  Bos, Rychard Bouwens, and Renske Smit for discussions. J.M. acknowledges the support
  of a Huygens PhD fellowship from Leiden University. D.S. acknowledges financial
  support from the Netherlands Organisation for Scientific research (NWO) through
  a Veni fellowship and from Lancaster University through an Early Career Internal
  Grant A100679. A.F. acknowledges support from the ERC Advanced Grant INTERSTELLAR
  H2020/740120. B.D. acknowledges financial support from NASA through the Astrophysics
  Data Analysis Program (ADAP), grant number NNX12AE20G. Based on observations made
  with ESO Telescopes at the La Silla Paranal Observatory under programme ID 294.A-5018.
  This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00122.S. ALMA
  is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan),
  together with NRC (Canada) and NSC and ASIAA (Taiwan), and KASI (Republic of Korea),
  in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated
  by ESO, AUI/NRAO, and NAOJ.'
article_number: '145'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- 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: D.
  full_name: Sobral, D.
  last_name: Sobral
- first_name: F.
  full_name: Boone, F.
  last_name: Boone
- first_name: H.
  full_name: Röttgering, H.
  last_name: Röttgering
- first_name: D.
  full_name: Schaerer, D.
  last_name: Schaerer
- first_name: M.
  full_name: Girard, M.
  last_name: Girard
- first_name: A.
  full_name: Pallottini, A.
  last_name: Pallottini
- first_name: L.
  full_name: Vallini, L.
  last_name: Vallini
- first_name: A.
  full_name: Ferrara, A.
  last_name: Ferrara
- first_name: B.
  full_name: Darvish, B.
  last_name: Darvish
- first_name: B.
  full_name: Mobasher, B.
  last_name: Mobasher
citation:
  ama: Matthee JJ, Sobral D, Boone F, et al. ALMA reveals metals yet no dust within
    multiple components in CR7. <i>The Astrophysical Journal</i>. 2017;851(2). doi:<a
    href="https://doi.org/10.3847/1538-4357/aa9931">10.3847/1538-4357/aa9931</a>
  apa: Matthee, J. J., Sobral, D., Boone, F., Röttgering, H., Schaerer, D., Girard,
    M., … Mobasher, B. (2017). ALMA reveals metals yet no dust within multiple components
    in CR7. <i>The Astrophysical Journal</i>. IOP Publishing. <a href="https://doi.org/10.3847/1538-4357/aa9931">https://doi.org/10.3847/1538-4357/aa9931</a>
  chicago: Matthee, Jorryt J, D. Sobral, F. Boone, H. Röttgering, D. Schaerer, M.
    Girard, A. Pallottini, et al. “ALMA Reveals Metals yet No Dust within Multiple
    Components in CR7.” <i>The Astrophysical Journal</i>. IOP Publishing, 2017. <a
    href="https://doi.org/10.3847/1538-4357/aa9931">https://doi.org/10.3847/1538-4357/aa9931</a>.
  ieee: J. J. Matthee <i>et al.</i>, “ALMA reveals metals yet no dust within multiple
    components in CR7,” <i>The Astrophysical Journal</i>, vol. 851, no. 2. IOP Publishing,
    2017.
  ista: Matthee JJ, Sobral D, Boone F, Röttgering H, Schaerer D, Girard M, Pallottini
    A, Vallini L, Ferrara A, Darvish B, Mobasher B. 2017. ALMA reveals metals yet
    no dust within multiple components in CR7. The Astrophysical Journal. 851(2),
    145.
  mla: Matthee, Jorryt J., et al. “ALMA Reveals Metals yet No Dust within Multiple
    Components in CR7.” <i>The Astrophysical Journal</i>, vol. 851, no. 2, 145, IOP
    Publishing, 2017, doi:<a href="https://doi.org/10.3847/1538-4357/aa9931">10.3847/1538-4357/aa9931</a>.
  short: J.J. Matthee, D. Sobral, F. Boone, H. Röttgering, D. Schaerer, M. Girard,
    A. Pallottini, L. Vallini, A. Ferrara, B. Darvish, B. Mobasher, The Astrophysical
    Journal 851 (2017).
date_created: 2022-07-07T08:48:04Z
date_published: 2017-12-21T00:00:00Z
date_updated: 2022-08-18T10:23:35Z
day: '21'
doi: 10.3847/1538-4357/aa9931
extern: '1'
external_id:
  arxiv:
  - '1709.06569'
intvolume: '       851'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- dark ages
- reionization
- 'first stars – galaxies: formation – galaxies: high-redshift – galaxies: ISM – galaxies:
  kinematics and dynamics'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1709.06569
month: '12'
oa: 1
oa_version: Preprint
publication: The Astrophysical Journal
publication_identifier:
  eissn:
  - 1538-4357
  issn:
  - 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: ALMA reveals metals yet no dust within multiple components in CR7
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 851
year: '2017'
...
---
_id: '11561'
abstract:
- lang: eng
  text: 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.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- 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: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Philip
  full_name: Best, Philip
  last_name: Best
- first_name: Ian
  full_name: Smail, Ian
  last_name: Smail
- first_name: Fuyan
  full_name: Bian, Fuyan
  last_name: Bian
- first_name: Behnam
  full_name: Darvish, Behnam
  last_name: Darvish
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
- first_name: Xiaohui
  full_name: Fan, Xiaohui
  last_name: Fan
citation:
  ama: '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>'
  apa: '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>'
  chicago: '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>.'
  ieee: '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.'
  ista: '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.'
  mla: '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>.'
  short: 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.
date_created: 2022-07-12T11:01:35Z
date_published: 2017-10-01T00:00:00Z
date_updated: 2022-08-19T07:15:14Z
day: '01'
doi: 10.1093/mnras/stx1569
extern: '1'
external_id:
  arxiv:
  - '1702.04721'
intvolume: '       471'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics galaxies
- active
- galaxies
- evolution
- galaxies
- high-redshift
- galaxies
- luminosity function
- mass function
- 'galaxies: star formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1702.04721
month: '10'
oa: 1
oa_version: Preprint
page: 629-649
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies
  at z = 0.4–4.7'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...
---
_id: '11562'
abstract:
- lang: eng
  text: We present the CAlibrating LYMan-α with Hα (CALYMHA) pilot survey and new
    results on Lyman α (Lyα) selected galaxies at z ∼ 2. We use a custom-built Lyα
    narrow-band filter at the Isaac Newton Telescope, designed to provide a matched
    volume coverage to the z = 2.23 Hα HiZELS survey. Here, we present the first results
    for the COSMOS and UDS fields. Our survey currently reaches a 3σ line flux limit
    of ∼4 × 10−17 erg s−1 cm−2, and a Lyα luminosity limit of ∼1042.3 erg s−1. We
    find 188 Lyα emitters over 7.3 × 105 Mpc3, but also find significant numbers of
    other line-emitting sources corresponding to He II, C III] and C IV emission lines.
    These sources are important contaminants, and we carefully remove them, unlike
    most previous studies. We find that the Lyα luminosity function at z = 2.23 is
    very well described by a Schechter function up to LLy α ≈ 1043 erg s−1 with L∗=1042.59+0.16−0.08
    erg s−1, ϕ∗=10−3.09+0.14−0.34 Mpc−3 and α = −1.75 ± 0.25. Above LLy α ≈ 1043 erg
    s−1, the Lyα luminosity function becomes power-law like, driven by X-ray AGN.
    We find that Lyα-selected emitters have a high escape fraction of 37 ± 7 per cent,
    anticorrelated with Lyα luminosity and correlated with Lyα equivalent width. Lyα
    emitters have ubiquitous large (≈40 kpc) Lyα haloes, ∼2 times larger than their
    Hα extents. By directly comparing our Lyα and Hα luminosity functions, we find
    that the global/overall escape fraction of Lyα photons (within a 13 kpc radius)
    from the full population of star-forming galaxies is 5.1 ± 0.2 per cent at the
    peak of the star formation history. An extra 3.3 ± 0.3 per cent of Lyα photons
    likely still escape, but at larger radii.
acknowledgement: 'We thank the reviewer for his/her helpful comments and suggestions
  that have greatly improved this work. DS and JM acknowledge financial support from
  the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship.
  DS also acknowledges funding from FCT through an FCT Investigator Starting Grant
  and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from
  the UK STFC via grant ST/M001229/1. IRS acknowledges support from STFC (ST/L00075X/1),
  the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson
  merit award. We thank Matthew Hayes, Ryan Trainor, Kimihiko Nakajima and Anne Verhamme
  for many helpful discussions and Ana Sobral, Carolina Duarte and Miguel Domingos
  for taking part in observations with the NB392 filter. We also thank Sergio Santos
  for helpful comments. This research is based on observations obtained on the Isaac
  Newton Telescope (INT), programs: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B
  & I15AN008. The authors acknowledge the award of time from programmes: I13AN002,
  I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008 on the INT. INT is operated
  on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio
  del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on
  observations made with ESO Telescopes at the La Silla Paranal Observatory under
  programme ID 098.A 0819. We have benefited greatly from the publicly available programming
  language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages,
  the astronomical imaging tools SEXTRACTOR, SWARP (Bertin & Arnouts 1996; Bertin
  2010), SCAMP (Bertin 2006) and TOPCAT (Taylor 2005). Dedicated to the memory of
  M. L. Nicolau and M. C. Serrano.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- 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: Philip
  full_name: Best, Philip
  last_name: Best
- first_name: Andra
  full_name: Stroe, Andra
  last_name: Stroe
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
- first_name: Iván
  full_name: Oteo, Iván
  last_name: Oteo
- first_name: Ian
  full_name: Smail, Ian
  last_name: Smail
- first_name: Leah
  full_name: Morabito, Leah
  last_name: Morabito
- first_name: Ana
  full_name: Paulino-Afonso, Ana
  last_name: Paulino-Afonso
citation:
  ama: 'Sobral D, Matthee JJ, Best P, et al. The CALYMHA survey: Lyα luminosity function
    and global escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the
    Royal Astronomical Society</i>. 2017;466(1):1242-1258. doi:<a href="https://doi.org/10.1093/mnras/stw3090">10.1093/mnras/stw3090</a>'
  apa: 'Sobral, D., Matthee, J. J., Best, P., Stroe, A., Röttgering, H., Oteo, I.,
    … Paulino-Afonso, A. (2017). The CALYMHA survey: Lyα luminosity function and global
    escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stw3090">https://doi.org/10.1093/mnras/stw3090</a>'
  chicago: 'Sobral, David, Jorryt J Matthee, Philip Best, Andra Stroe, Huub Röttgering,
    Iván Oteo, Ian Smail, Leah Morabito, and Ana Paulino-Afonso. “The CALYMHA Survey:
    Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.”
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press,
    2017. <a href="https://doi.org/10.1093/mnras/stw3090">https://doi.org/10.1093/mnras/stw3090</a>.'
  ieee: 'D. Sobral <i>et al.</i>, “The CALYMHA survey: Lyα luminosity function and
    global escape fraction of Lyα photons at z = 2.23,” <i>Monthly Notices of the
    Royal Astronomical Society</i>, vol. 466, no. 1. Oxford University Press, pp.
    1242–1258, 2017.'
  ista: 'Sobral D, Matthee JJ, Best P, Stroe A, Röttgering H, Oteo I, Smail I, Morabito
    L, Paulino-Afonso A. 2017. The CALYMHA survey: Lyα luminosity function and global
    escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical
    Society. 466(1), 1242–1258.'
  mla: 'Sobral, David, et al. “The CALYMHA Survey: Lyα Luminosity Function and Global
    Escape Fraction of Lyα Photons at z = 2.23.” <i>Monthly Notices of the Royal Astronomical
    Society</i>, vol. 466, no. 1, Oxford University Press, 2017, pp. 1242–58, doi:<a
    href="https://doi.org/10.1093/mnras/stw3090">10.1093/mnras/stw3090</a>.'
  short: D. Sobral, J.J. Matthee, P. Best, A. Stroe, H. Röttgering, I. Oteo, I. Smail,
    L. Morabito, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society
    466 (2017) 1242–1258.
date_created: 2022-07-12T12:04:16Z
date_published: 2017-04-01T00:00:00Z
date_updated: 2022-08-19T07:18:20Z
day: '01'
doi: 10.1093/mnras/stw3090
extern: '1'
external_id:
  arxiv:
  - '1609.05897'
intvolume: '       466'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: haloes'
- 'galaxies: high-redshift'
- 'galaxies: luminosity function'
- mass function
- 'galaxies: statistics'
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1609.05897
month: '04'
oa: 1
oa_version: Preprint
page: 1242-1258
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: 'The CALYMHA survey: Lyα luminosity function and global escape fraction of
  Lyα photons at z = 2.23'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 466
year: '2017'
...
---
_id: '11564'
abstract:
- lang: eng
  text: We study the production rate of ionizing photons of a sample of 588 Hα emitters
    (HAEs) and 160 Lyman-α emitters (LAEs) at z = 2.2 in the COSMOS field in order
    to assess the implied emissivity from galaxies, based on their ultraviolet (UV)
    luminosity. By exploring the rest-frame Lyman Continuum (LyC) with GALEX/NUV data,
    we find fesc < 2.8 (6.4) per cent through median (mean) stacking. By combining
    the Hα luminosity density with intergalactic medium emissivity measurements from
    absorption studies, we find a globally averaged 〈fesc〉 of 5.9+14.5−4.2 per cent
    at z = 2.2 if we assume HAEs are the only source of ionizing photons. We find
    similarly low values of the global 〈fesc〉 at z ≈ 3–5, also ruling out a high 〈fesc〉
    at z < 5. These low escape fractions allow us to measure ξion, the number of produced
    ionizing photons per unit UV luminosity, and investigate how this depends on galaxy
    properties. We find a typical ξion ≈ 1024.77 ± 0.04 Hz erg−1 for HAEs and ξion
    ≈ 1025.14 ± 0.09 Hz erg−1 for LAEs. LAEs and low-mass HAEs at z = 2.2 show similar
    values of ξion as typically assumed in the reionization era, while the typical
    HAE is three times less ionizing. Due to an increasing ξion with increasing EW(Hα),
    ξion likely increases with redshift. This evolution alone is fully in line with
    the observed evolution of ξion between z ≈ 2 and 5, indicating a typical value
    of ξion ≈ 1025.4 Hz erg−1 in the reionization era.
acknowledgement: "We thank the referee for the many helpful and constructive comments
  which have significantly improved this paper. JM acknowledges the support of a Huygens
  PhD fellowship from Leiden University. DS acknowledges financial support from the
  Netherlands Organization for Scientific research (NWO) through a Veni fellowship
  and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010).
  PNB is grateful for support from the UK STFC via grant ST/M001229/1. IO acknowledges
  support from the European Research Council in the form of the Advanced Investigator
  Programme, 321302, COSMICISM. The authors thank Andreas Faisst, Michael Rutkowski
  and Andreas Sandberg for answering questions related to this work and Daniel Schaerer
  and Mark Dijkstra for discussions. We acknowledge the work that has been done by
  both the COSMOS team in assembling such large, state-of-the-art multi-wavelength
  data set, as this has been crucial for the results presented in this paper. We have
  benefited greatly from the public available programming language PYTHON, including
  the NUMPY, MATPLOTLIB, PYFITS, SCIPY (Jones et al. 2001; Hunter 2007; Van Der Walt,
  Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration et al. 2013) packages,
  the astronomical imaging tools SEXTRACTOR and SWARP (Bertin & Arnouts 1996;\r\nBertin
  2010) and the TOPCAT analysis program (Taylor 2013)."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- 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: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Philip
  full_name: Best, Philip
  last_name: Best
- first_name: Ali Ahmad
  full_name: Khostovan, Ali Ahmad
  last_name: Khostovan
- first_name: Iván
  full_name: Oteo, Iván
  last_name: Oteo
- first_name: Rychard
  full_name: Bouwens, Rychard
  last_name: Bouwens
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
citation:
  ama: Matthee JJ, Sobral D, Best P, et al. The production and escape of Lyman-Continuum
    radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2017;465(3):3637-3655. doi:<a href="https://doi.org/10.1093/mnras/stw2973">10.1093/mnras/stw2973</a>
  apa: Matthee, J. J., Sobral, D., Best, P., Khostovan, A. A., Oteo, I., Bouwens,
    R., &#38; Röttgering, H. (2017). The production and escape of Lyman-Continuum
    radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stw2973">https://doi.org/10.1093/mnras/stw2973</a>
  chicago: Matthee, Jorryt J, David Sobral, Philip Best, Ali Ahmad Khostovan, Iván
    Oteo, Rychard Bouwens, and Huub Röttgering. “The Production and Escape of Lyman-Continuum
    Radiation from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017.
    <a href="https://doi.org/10.1093/mnras/stw2973">https://doi.org/10.1093/mnras/stw2973</a>.
  ieee: J. J. Matthee <i>et al.</i>, “The production and escape of Lyman-Continuum
    radiation from star-forming galaxies at z ∼ 2 and their redshift evolution,” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 465, no. 3. Oxford University
    Press, pp. 3637–3655, 2017.
  ista: Matthee JJ, Sobral D, Best P, Khostovan AA, Oteo I, Bouwens R, Röttgering
    H. 2017. The production and escape of Lyman-Continuum radiation from star-forming
    galaxies at z ∼ 2 and their redshift evolution. Monthly Notices of the Royal Astronomical
    Society. 465(3), 3637–3655.
  mla: Matthee, Jorryt J., et al. “The Production and Escape of Lyman-Continuum Radiation
    from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 465, no. 3, Oxford University
    Press, 2017, pp. 3637–55, doi:<a href="https://doi.org/10.1093/mnras/stw2973">10.1093/mnras/stw2973</a>.
  short: J.J. Matthee, D. Sobral, P. Best, A.A. Khostovan, I. Oteo, R. Bouwens, H.
    Röttgering, Monthly Notices of the Royal Astronomical Society 465 (2017) 3637–3655.
date_created: 2022-07-12T12:12:14Z
date_published: 2017-03-01T00:00:00Z
date_updated: 2022-08-19T07:53:04Z
day: '01'
doi: 10.1093/mnras/stw2973
extern: '1'
external_id:
  arxiv:
  - '1605.08782'
intvolume: '       465'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'cosmology: observations'
- dark ages
- reionization
- first stars
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1605.08782
month: '03'
oa: 1
oa_version: Preprint
page: 3637-3655
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: The production and escape of Lyman-Continuum radiation from star-forming galaxies
  at z ∼ 2 and their redshift evolution
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 465
year: '2017'
...
---
_id: '11565'
abstract:
- lang: eng
  text: We use the hydrodynamical EAGLE simulation to study the magnitude and origin
    of the scatter in the stellar mass–halo mass relation for central galaxies. We
    separate cause and effect by correlating stellar masses in the baryonic simulation
    with halo properties in a matched dark matter only (DMO) simulation. The scatter
    in stellar mass increases with redshift and decreases with halo mass. At z = 0.1,
    it declines from 0.25 dex at M200, DMO ≈ 1011 M⊙ to 0.12 dex at M200, DMO ≈ 1013
    M⊙, but the trend is weak above 1012 M⊙. For M200, DMO < 1012.5 M⊙ up to 0.04
    dex of the scatter is due to scatter in the halo concentration. At fixed halo
    mass, a larger stellar mass corresponds to a more concentrated halo. This is likely
    because higher concentrations imply earlier formation times and hence more time
    for accretion and star formation, and/or because feedback is less efficient in
    haloes with higher binding energies. The maximum circular velocity, Vmax, DMO,
    and binding energy are therefore more fundamental properties than halo mass, meaning
    that they are more accurate predictors of stellar mass, and we provide fitting
    formulae for their relations with stellar mass. However, concentration alone cannot
    explain the total scatter in the Mstar−M200,DMO relation, and it does not explain
    the scatter in Mstar–Vmax, DMO. Halo spin, sphericity, triaxiality, substructure
    and environment are also not responsible for the remaining scatter, which thus
    could be due to more complex halo properties or non-linear/stochastic baryonic
    effects.
acknowledgement: We thank the anonymous referee for their comments. JM acknowledges
  the support of a Huygens PhD fellowship from Leiden University. JM thanks David
  Sobral for useful discussions and help with fitting routines and Jonas Chavez Montero
  and Ying Zu for providing data. We thank PRACE for the access to the Curie facility
  in France. We have used the DiRAC system which is a part of National E-Infrastructure
  at Durham University, operated by the Institute for Computational Cosmology on behalf
  of the STFC DiRAC HPC Facility (www.dirac.ac.uk); the equipment was funded by BIS
  National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1,
  STFC DiRAC Operations grant ST/K003267/1 and Durham University. The study was sponsored
  by the Dutch National Computing Facilities Foundation (NCF) for the use of supercomputer
  facilities, with financial support from the Netherlands Organisation for Scientific
  Research (NWO), through VICI grant 639.043.409, and the European Research Council
  under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC Grant
  agreement 278594- GasAroundGalaxies, and from the Belgian Science Policy Office
  ([AP P7/08 CHARM]). We have benefited greatly from the public available programming
  language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY, H5PY and RPY2 packages,
  and the TOPCAT analysis program (Taylor 2005).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- 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: Robert A.
  full_name: Crain, Robert A.
  last_name: Crain
- first_name: Matthieu
  full_name: Schaller, Matthieu
  last_name: Schaller
- first_name: Richard
  full_name: Bower, Richard
  last_name: Bower
- first_name: Tom
  full_name: Theuns, Tom
  last_name: Theuns
citation:
  ama: Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. The origin of
    scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE
    simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;465(2):2381-2396.
    doi:<a href="https://doi.org/10.1093/mnras/stw2884">10.1093/mnras/stw2884</a>
  apa: Matthee, J. J., Schaye, J., Crain, R. A., Schaller, M., Bower, R., &#38; Theuns,
    T. (2017). The origin of scatter in the stellar mass–halo mass relation of central
    galaxies in the EAGLE simulation. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stw2884">https://doi.org/10.1093/mnras/stw2884</a>
  chicago: Matthee, Jorryt J, Joop Schaye, Robert A. Crain, Matthieu Schaller, Richard
    Bower, and Tom Theuns. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation
    of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices of the Royal
    Astronomical Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stw2884">https://doi.org/10.1093/mnras/stw2884</a>.
  ieee: J. J. Matthee, J. Schaye, R. A. Crain, M. Schaller, R. Bower, and T. Theuns,
    “The origin of scatter in the stellar mass–halo mass relation of central galaxies
    in the EAGLE simulation,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 465, no. 2. Oxford University Press, pp. 2381–2396, 2017.
  ista: Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. 2017. The origin
    of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE
    simulation. Monthly Notices of the Royal Astronomical Society. 465(2), 2381–2396.
  mla: Matthee, Jorryt J., et al. “The Origin of Scatter in the Stellar Mass–Halo
    Mass Relation of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 465, no. 2, Oxford University Press,
    2017, pp. 2381–96, doi:<a href="https://doi.org/10.1093/mnras/stw2884">10.1093/mnras/stw2884</a>.
  short: J.J. Matthee, J. Schaye, R.A. Crain, M. Schaller, R. Bower, T. Theuns, Monthly
    Notices of the Royal Astronomical Society 465 (2017) 2381–2396.
date_created: 2022-07-12T12:25:08Z
date_published: 2017-02-01T00:00:00Z
date_updated: 2022-08-19T07:56:07Z
day: '01'
doi: 10.1093/mnras/stw2884
extern: '1'
external_id:
  arxiv:
  - '1608.08218'
intvolume: '       465'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: haloes'
- 'cosmology: theory'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1608.08218
month: '02'
oa: 1
oa_version: Preprint
page: 2381-2396
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: The origin of scatter in the stellar mass–halo mass relation of central galaxies
  in the EAGLE simulation
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 465
year: '2017'
...
---
_id: '11566'
abstract:
- lang: eng
  text: While traditionally associated with active galactic nuclei (AGN), the properties
    of the C II] (λ = 2326 Å), C III] (λ, λ = 1907, 1909 Å) and C IV (λ, λ = 1549,
    1551 Å) emission lines are still uncertain as large, unbiased samples of sources
    are scarce. We present the first blind, statistical study of C II], C III] and
    C IV emitters at z ∼ 0.68, 1.05, 1.53, respectively, uniformly selected down to
    a flux limit of ∼4 × 10−17 erg s−1 cm−1 through a narrow-band survey covering
    an area of ∼1.4 deg2 over COSMOS and UDS. We detect 16 C II], 35 C III] and 17
    C IV emitters, whose nature we investigate using optical colours as well as Hubble
    Space Telescope (HST), X-ray, radio and far-infrared data. We find that z ∼ 0.7
    C II] emitters are consistent with a mixture of blue (UV slope β = −2.0 ± 0.4)
    star-forming (SF) galaxies with discy HST structure and AGN with Seyfert-like
    morphologies. Bright C II] emitters have individual X-ray detections as well as
    high average black hole accretion rates (BHARs) of ∼0.1 M⊙ yr−1. C III] emitters
    at z ∼ 1.05 trace a general population of SF galaxies, with β = −0.8 ± 1.1, a
    variety of optical morphologies, including isolated and interacting galaxies and
    low BHAR (<0.02 M⊙ yr−1). Our C IV emitters at z ∼ 1.5 are consistent with young,
    blue quasars (β ∼ −1.9) with point-like optical morphologies, bright X-ray counterparts
    and large BHAR (0.8  M⊙ yr−1). We also find some surprising C II], C III] and
    C IV emitters with rest-frame equivalent widths (EWs) that could be as large as
    50–100 Å. AGN or spatial offsets between the UV continuum stellar disc and the
    line-emitting regions may explain the large EW. These bright C II], C III] and
    C IV emitters are ideal candidates for spectroscopic follow-up to fully unveil
    their nature.
acknowledgement: 'We would like to thank the anonymous referee for her/his valuable
  input that helped improve the clarity and interpretation of our results. DS acknowledges
  financial support from the Netherlands Organisation for Scientific research (NWO),
  through a Veni fellowship. IO acknowledges support from the European Research Council
  in the form of the Advanced Investigator Programme, 321302, COSMICISM. CALYMHA data
  are based on observations made with the Isaac Newton Telescope (proposals 13AN002,
  I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008) operated on the island
  of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los
  Muchachos of the Instituto de Astrofísica de Canarias. Also based on data products
  from observations made with ESO Telescopes at the La Silla Paranal Observatory under
  ESO programme IDs 098.A-0819 and 179.A-2005. We are grateful to E. L. Wright and
  J. Schombert for their cosmology calculator. We would like to thank the authors
  of NUMPY (van der Walt et al. 2011), SCIPY (Jones et al. 2001), MATPLOTLIB (Hunter
  2007) and ASTROPY (Astropy Collaboration et al. 2013) for making these packages
  publicly available. This research has made use of the NASA/IPAC Extragalactic Database
  (NED), which is '
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Andra
  full_name: Stroe, Andra
  last_name: Stroe
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- 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: João
  full_name: Calhau, João
  last_name: Calhau
- first_name: Ivan
  full_name: Oteo, Ivan
  last_name: Oteo
citation:
  ama: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for
    C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent
    widths . <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(3):2558-2574.
    doi:<a href="https://doi.org/10.1093/mnras/stx1712">10.1093/mnras/stx1712</a>
  apa: Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., &#38; Oteo, I. (2017). A
    1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies
    and equivalent widths . <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx1712">https://doi.org/10.1093/mnras/stx1712</a>
  chicago: Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo.
    “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature,
    Morphologies and Equivalent Widths .” <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx1712">https://doi.org/10.1093/mnras/stx1712</a>.
  ieee: A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind
    survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and
    equivalent widths ,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 471, no. 3. Oxford University Press, pp. 2558–2574, 2017.
  ista: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey
    for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent
    widths . Monthly Notices of the Royal Astronomical Society. 471(3), 2558–2574.
  mla: Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at
    z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 471, no. 3, Oxford University Press,
    2017, pp. 2558–74, doi:<a href="https://doi.org/10.1093/mnras/stx1712">10.1093/mnras/stx1712</a>.
  short: A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of
    the Royal Astronomical Society 471 (2017) 2558–2574.
date_created: 2022-07-12T12:33:16Z
date_published: 2017-11-01T00:00:00Z
date_updated: 2022-08-19T07:59:57Z
day: '01'
doi: 10.1093/mnras/stx1712
extern: '1'
external_id:
  arxiv:
  - '1703.10169'
intvolume: '       471'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: active'
- 'galaxies: high-redshift'
- 'quasars: emission lines'
- 'galaxies: star formation'
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1703.10169
month: '11'
oa: 1
oa_version: Preprint
page: 2558-2574
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: 'A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature,
  morphologies and equivalent widths '
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...
---
_id: '11567'
abstract:
- lang: eng
  text: Recently, the C III] and C IV emission lines have been observed in galaxies
    in the early Universe (z > 5), providing new ways to measure their redshift and
    study their stellar populations and active galactic nuclei (AGN). We explore the
    first blind C II], C III] and C IV survey (z ∼ 0.68, 1.05, 1.53, respectively)
    presented in Stroe et al. (2017). We derive luminosity functions (LF) and study
    properties of C II], C III] and C IV line emitters through comparisons to the
    LFs of H α and Ly α emitters, UV selected star-forming (SF) galaxies and quasars
    at similar redshifts. The C II] LF at z ∼ 0.68 is equally well described by a
    Schechter or a power-law LF, characteristic of a mixture of SF and AGN activity.
    The C III] LF (z ∼ 1.05) is consistent to a scaled down version of the Schechter
    H α and Ly α LF at their redshift, indicating a SF origin. In stark contrast,
    the C IV LF at z ∼ 1.53 is well fit by a power-law, quasar-like LF. We find that
    the brightest UV sources (MUV < −22) will universally have C III] and C IV emission.
    However, on average, C III] and C IV are not as abundant as H α or Ly α emitters
    at the same redshift, with cosmic average ratios of ∼0.02–0.06 to H α and ∼0.01–0.1
    to intrinsic Ly α. We predict that the C III] and C IV lines can only be truly
    competitive in confirming high-redshift candidates when the hosts are intrinsically
    bright and the effective Ly α escape fraction is below 1 per cent. While C III]
    and C IV were proposed as good tracers of young, relatively low-metallicity galaxies
    typical of the early Universe, we find that, at least at z ∼ 1.5, C IV is exclusively
    hosted by AGN/quasars, especially at large line equivalent widths.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Andra
  full_name: Stroe, Andra
  last_name: Stroe
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- 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: João
  full_name: Calhau, João
  last_name: Calhau
- first_name: Ivan
  full_name: Oteo, Ivan
  last_name: Oteo
citation:
  ama: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for
    C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average
    line ratios. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(3):2575-2586.
    doi:<a href="https://doi.org/10.1093/mnras/stx1713">10.1093/mnras/stx1713</a>
  apa: Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., &#38; Oteo, I. (2017). A
    1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity
    functions and cosmic average line ratios. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx1713">https://doi.org/10.1093/mnras/stx1713</a>
  chicago: Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo.
    “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity
    Functions and Cosmic Average Line Ratios.” <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx1713">https://doi.org/10.1093/mnras/stx1713</a>.
  ieee: A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind
    survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and
    cosmic average line ratios,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 471, no. 3. Oxford University Press, pp. 2575–2586, 2017.
  ista: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey
    for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic
    average line ratios. Monthly Notices of the Royal Astronomical Society. 471(3),
    2575–2586.
  mla: Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at
    z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 471, no. 3, Oxford University
    Press, 2017, pp. 2575–86, doi:<a href="https://doi.org/10.1093/mnras/stx1713">10.1093/mnras/stx1713</a>.
  short: A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of
    the Royal Astronomical Society 471 (2017) 2575–2586.
date_created: 2022-07-12T12:54:57Z
date_published: 2017-11-01T00:00:00Z
date_updated: 2022-08-19T08:02:04Z
day: '01'
doi: 10.1093/mnras/stx1713
extern: '1'
external_id:
  arxiv:
  - '1703.10169'
intvolume: '       471'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: active'
- 'galaxies: high redshift'
- 'galaxies: luminosity function'
- mass function
- 'quasars: emission lines'
- star formation
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1703.10169
month: '11'
oa: 1
oa_version: Preprint
page: 2575-2586
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: A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity
  functions and cosmic average line ratios
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...