---
_id: '11524'
abstract:
- lang: eng
  text: We measure the evolution of the rest-frame UV luminosity function (LF) and
    the stellar mass function (SMF) of Lyman-α (Ly α) emitters (LAEs) from z ∼ 2 to
    z ∼ 6 by exploring ∼4000 LAEs from the SC4K sample. We find a correlation between
    Ly α luminosity (LLy α) and rest-frame UV (MUV), with best fit MUV=−1.6+0.2−0.3log10(LLyα/ergs−1)+47+12−11
    and a shallower relation between LLy α and stellar mass (M⋆), with best fit log10(M⋆/M⊙)=0.9+0.1−0.1log10(LLyα/ergs−1)−28+4.0−3.8⁠.
    An increasing LLy α cut predominantly lowers the number density of faint MUV and
    low M⋆ LAEs. We estimate a proxy for the full UV LFs and SMFs of LAEs with simple
    assumptions of the faint end slope. For the UV LF, we find a brightening of the
    characteristic UV luminosity (M∗UV⁠) with increasing redshift and a decrease of
    the characteristic number density (Φ*). For the SMF, we measure a characteristic
    stellar mass (⁠M∗⋆/M⊙⁠) increase with increasing redshift, and a Φ* decline. However,
    if we apply a uniform luminosity cut of log10(LLyα/ergs−1)≥43.0⁠, we find much
    milder to no evolution in the UV and SMF of LAEs. The UV luminosity density (ρUV)
    of the full sample of LAEs shows moderate evolution and the stellar mass density
    (ρM) decreases, with both being always lower than the total ρUV and ρM of more
    typical galaxies but slowly approaching them with increasing redshift. Overall,
    our results indicate that both ρUV and ρM of LAEs slowly approach the measurements
    of continuum-selected galaxies at z > 6, which suggests a key role of LAEs in
    the epoch of reionization.
acknowledgement: This research made use of Astropy, a community developed core Python
  package for Astronomy (Astropy Collaboration et al. 2013). topcat, a graphical tool
  for manipulating tabular data, was also utilized in this analysis (Taylor 2005).
  SG would like to thank Nastasha Wijers for the discussion on the column density
  distribution in EAGLE. SC gratefully acknowledges support from Swiss National Science
  Foundation grants PP00P2 163824 and PP00P2 190092, and from the European Research
  Council (ERC) under the European Union’s Horizon 2020 research and innovation programme
  grant agreement No 864361. GP acknowledges support from the Swiss National Science
  Foundation (SNF) and from the Netherlands Research School for Astronomy (NOVA).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: S
  full_name: Santos, S
  last_name: Santos
- first_name: D
  full_name: Sobral, D
  last_name: Sobral
- first_name: J
  full_name: Butterworth, J
  last_name: Butterworth
- first_name: A
  full_name: Paulino-Afonso, A
  last_name: Paulino-Afonso
- first_name: B
  full_name: Ribeiro, B
  last_name: Ribeiro
- first_name: E
  full_name: da Cunha, E
  last_name: da Cunha
- first_name: J
  full_name: Calhau, J
  last_name: Calhau
- first_name: A A
  full_name: Khostovan, A A
  last_name: Khostovan
- 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: P
  full_name: Arrabal Haro, P
  last_name: Arrabal Haro
citation:
  ama: Santos S, Sobral D, Butterworth J, et al. The evolution of the UV luminosity
    and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2021;505(1):1117-1134. doi:<a href="https://doi.org/10.1093/mnras/stab1218">10.1093/mnras/stab1218</a>
  apa: Santos, S., Sobral, D., Butterworth, J., Paulino-Afonso, A., Ribeiro, B., da Cunha,
    E., … Arrabal Haro, P. (2021). The evolution of the UV luminosity and stellar
    mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. <i>Monthly Notices of
    the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stab1218">https://doi.org/10.1093/mnras/stab1218</a>
  chicago: Santos, S, D Sobral, J Butterworth, A Paulino-Afonso, B Ribeiro, E da Cunha,
    J Calhau, A A Khostovan, Jorryt J Matthee, and P Arrabal Haro. “The Evolution
    of the UV Luminosity and Stellar Mass Functions of Lyman-α Emitters from z ∼ 2
    to z ∼ 6.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University
    Press, 2021. <a href="https://doi.org/10.1093/mnras/stab1218">https://doi.org/10.1093/mnras/stab1218</a>.
  ieee: S. Santos <i>et al.</i>, “The evolution of the UV luminosity and stellar mass
    functions of Lyman-α emitters from z ∼ 2 to z ∼ 6,” <i>Monthly Notices of the
    Royal Astronomical Society</i>, vol. 505, no. 1. Oxford University Press, pp.
    1117–1134, 2021.
  ista: Santos S, Sobral D, Butterworth J, Paulino-Afonso A, Ribeiro B, da Cunha E,
    Calhau J, Khostovan AA, Matthee JJ, Arrabal Haro P. 2021. The evolution of the
    UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼
    6. Monthly Notices of the Royal Astronomical Society. 505(1), 1117–1134.
  mla: Santos, S., et al. “The Evolution of the UV Luminosity and Stellar Mass Functions
    of Lyman-α Emitters from z ∼ 2 to z ∼ 6.” <i>Monthly Notices of the Royal Astronomical
    Society</i>, vol. 505, no. 1, Oxford University Press, 2021, pp. 1117–34, doi:<a
    href="https://doi.org/10.1093/mnras/stab1218">10.1093/mnras/stab1218</a>.
  short: S. Santos, D. Sobral, J. Butterworth, A. Paulino-Afonso, B. Ribeiro, E. da Cunha,
    J. Calhau, A.A. Khostovan, J.J. Matthee, P. Arrabal Haro, Monthly Notices of the
    Royal Astronomical Society 505 (2021) 1117–1134.
date_created: 2022-07-07T10:02:59Z
date_published: 2021-07-01T00:00:00Z
date_updated: 2022-08-18T10:51:47Z
day: '01'
doi: 10.1093/mnras/stab1218
extern: '1'
external_id:
  arxiv:
  - '2105.00007'
intvolume: '       505'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: luminosity function'
- mass function
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/2105.00007
month: '07'
oa: 1
oa_version: Preprint
page: 1117-1134
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 evolution of the UV luminosity and stellar mass functions of Lyman-α emitters
  from z ∼ 2 to z ∼ 6
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 505
year: '2021'
...
---
_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: '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: '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: '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'
...
---
_id: '11574'
abstract:
- lang: eng
  text: We present new results from the widest narrow-band survey search for Lyα emitters
    at z = 5.7, just after reionization. We survey a total of 7 deg2 spread over the
    COSMOS, UDS and SA22 fields. We find over 11 000 line emitters, out of which 514
    are robust Lyα candidates at z = 5.7 within a volume of 6.3 × 106 Mpc3. Our Lyα
    emitters span a wide range in Lyα luminosities, from faint to bright (LLyα ∼ 1042.5–44
    erg s−1) and rest-frame equivalent widths (EW0 ∼ 25–1000 Å) in a single, homogeneous
    data set. By combining all our fields, we find that the faint end slope of the
    z = 5.7 Lyα luminosity function is very steep, with α=−2.3+0.4−0.3⁠. We also present
    an updated z = 6.6 Lyα luminosity function, based on comparable volumes and obtained
    with the same methods, which we directly compare with that at z = 5.7. We find
    a significant decline of the number density of faint Lyα emitters from z = 5.7
    to 6.6 (by 0.5 ± 0.1 dex), but no evolution at the bright end/no evolution in
    L*. Faint Lyα emitters at z = 6.6 show much more extended haloes than those at
    z = 5.7, suggesting that neutral Hydrogen plays an important role, increasing
    the scattering and leading to observations missing faint Lyα emission within the
    epoch of reionization. Altogether, our results suggest that we are observing patchy
    reionization which happens first around the brightest Lyα emitters, allowing the
    number densities of those sources to remain unaffected by the increase of neutral
    Hydrogen fraction from z ∼ 5 to 7.
acknowledgement: 'We thank the anonymous referee for useful and constructive comments
  and suggestions which greatly improved the quality and clarity of our work. The
  authors acknowledge financial support from the Netherlands Organisation for Scientific
  research (NWO) through a Veni fellowship. SS and DS acknowledge funding from FCT
  through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010).
  SS also acknowledges support from FCT through the research grants UID/FIS/04434/2013
  and PTDC/FIS-AST/2194/2012. JM acknowledges a Huygens PhD fellowship from Leiden
  University. Based on observations with the Subaru Telescope (Program IDs: S05B-027,
  S06A-025, S06B-010, S07A-013, S07B-008, S08B-008, S09A-017, S14A-086). Based on
  observations made with ESO Telescopes at the La Silla Paranal Observatory under
  programme ID 294.A-5018. Based on observations obtained with MegaPrime/Megacam,
  a joint project of CFHT and CEA/IRFU, at the Canada–France–Hawaii Telescope (CFHT)
  which is operated by the National Research Council (NRC) of Canada, the Institut
  National des Science de l’Univers of the Centre National de la Recherche Scientifique
  (CNRS) of France, and the University 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 ID 179.A-2005 and on data
  products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of
  the UltraVISTA consortium. We are grateful to the CFHTLS, COSMOS-UltraVISTA, UKIDSS,
  SXDF and COSMOS survey teams. Without these legacy surveys, this research would
  have been impossible. The authors wish to recognize and acknowledge the very significant
  cultural role and reverence that the summit of Mauna Kea has always had within the
  indigenous Hawaiian community. We are most fortunate to have the opportunity to
  conduct and explore observations from this mountain. Finally, the authors acknowledge
  the unique value of the publicly available programming language PYTHON, including
  the NUMPY, PYFITS, MATPLOTLIB, SCIPY and ASTROPY (Astropy Collaboration et al.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Sérgio
  full_name: Santos, Sérgio
  last_name: Santos
- 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: 'Santos S, Sobral D, Matthee JJ. The Lyα luminosity function at z= 5.7–6.6
    and the steep drop of the faint end: Implications for reionization. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2016;463(2):1678-1691. doi:<a href="https://doi.org/10.1093/mnras/stw2076">10.1093/mnras/stw2076</a>'
  apa: 'Santos, S., Sobral, D., &#38; Matthee, J. J. (2016). The Lyα luminosity function
    at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization.
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press.
    <a href="https://doi.org/10.1093/mnras/stw2076">https://doi.org/10.1093/mnras/stw2076</a>'
  chicago: 'Santos, Sérgio, David Sobral, and Jorryt J Matthee. “The Lyα Luminosity
    Function at Z= 5.7–6.6 and the Steep Drop of the Faint End: Implications for Reionization.”
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press,
    2016. <a href="https://doi.org/10.1093/mnras/stw2076">https://doi.org/10.1093/mnras/stw2076</a>.'
  ieee: 'S. Santos, D. Sobral, and J. J. Matthee, “The Lyα luminosity function at
    z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization,”
    <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 463, no. 2. Oxford
    University Press, pp. 1678–1691, 2016.'
  ista: 'Santos S, Sobral D, Matthee JJ. 2016. The Lyα luminosity function at z= 5.7–6.6
    and the steep drop of the faint end: Implications for reionization. Monthly Notices
    of the Royal Astronomical Society. 463(2), 1678–1691.'
  mla: 'Santos, Sérgio, et al. “The Lyα Luminosity Function at Z= 5.7–6.6 and the
    Steep Drop of the Faint End: Implications for Reionization.” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 463, no. 2, Oxford University Press,
    2016, pp. 1678–91, doi:<a href="https://doi.org/10.1093/mnras/stw2076">10.1093/mnras/stw2076</a>.'
  short: S. Santos, D. Sobral, J.J. Matthee, Monthly Notices of the Royal Astronomical
    Society 463 (2016) 1678–1691.
date_created: 2022-07-13T10:08:20Z
date_published: 2016-12-01T00:00:00Z
date_updated: 2022-08-19T08:09:54Z
day: '01'
doi: 10.1093/mnras/stw2076
extern: '1'
external_id:
  arxiv:
  - '1606.07435'
intvolume: '       463'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift'
- 'galaxies: luminosity function'
- mass function
- 'cosmology: observations'
- dark ages
- reionization
- first stars
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1606.07435
month: '12'
oa: 1
oa_version: Preprint
page: 1678-1691
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 Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint
  end: Implications for reionization'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 463
year: '2016'
...
---
_id: '11580'
abstract:
- lang: eng
  text: 'We present results from the largest contiguous narrow-band survey in the
    near-infrared. We have used the wide-field infrared camera/Canada–France–Hawaii
    Telescope and the lowOH2 filter (1.187 ± 0.005 μm) to survey ≈10 deg2 of contiguous
    extragalactic sky in the SA22 field. A total of ∼6000 candidate emission-line
    galaxies are found. We use deep ugrizJK data to obtain robust photometric redshifts.
    We combine our data with the High-redshift(Z) Emission Line Survey (HiZELS), explore
    spectroscopic surveys (VVDS, VIPERS) and obtain our own spectroscopic follow-up
    with KMOS, FMOS and MOSFIRE to derive large samples of high-redshift emission-line
    selected galaxies: 3471 Hα emitters at z = 0.8, 1343 [O III] + Hβ emitters at
    z = 1.4 and 572 [O II] emitters at z = 2.2. We probe comoving volumes of >106
    Mpc3 and find significant overdensities, including an 8.5σ (spectroscopically
    confirmed) overdensity of Hα emitters at z = 0.81. We derive Hα, [O III] + Hβ
    and [O II] luminosity functions at z = 0.8, 1.4, 2.2, respectively, and present
    implications for future surveys such as Euclid. Our uniquely large volumes/areas
    allow us to subdivide the samples in thousands of randomized combinations of areas
    and provide a robust empirical measurement of sample/cosmic variance. We show
    that surveys for star-forming/emission-line galaxies at a depth similar to ours
    can only overcome cosmic-variance (errors <10 per cent) if they are based on volumes
    >5 × 105 Mpc3; errors on L* and ϕ* due to sample (cosmic) variance on surveys
    probing ∼104 and ∼105 Mpc3 are typically very high: ∼300 and ∼40–60 per cent,
    respectively.'
acknowledgement: The authors wish to thank the anonymous reviewer for many helpful
  comments and suggestions which greatly improved the clarity and quality of this
  work. DS acknowledges financial support from the Netherlands Organization for Scientific
  research (NWO) through a Veni fellowship, from FCT through an FCT Investigator Starting
  Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010), from FCT grant PEst-OE/FIS/UI2751/2014,
  and from LSF and LKBF. JM acknowledges the award of a Huygens PhD fellowship. PNB
  is grateful for support from STFC. IRS acknowledges support from STFC, a Leverhulme
  Fellowship, the ERC Advanced Investigator programme DUSTYGAL and a Royal Society/Wolfson
  Merit Award. BMJ acknowledges support from the ERC-StG grant EGGS-278202. The Dark
  Cosmology Centre is funded by the DNRF. The Dark Cosmology Centre is funded by the
  DNRF. JWK acknowledges support from the National Research Foundation of Korea (NRF)
  grant, no. 2008-0060544, funded by the Korea government (MSIP). JPS acknowledges
  support from STFC (ST/I001573/1). JC acknowledges support from the FCT-IF grant
  IF/01154/2012/CP0189/CT0010. The work was only possible due to OPTICON/FP7 and the
  invaluable access that it granted to the CFHT telescope. We would also like to acknowledge
  the excellent work done by CFHT staff in conducting the observations in service
  mode, and on delivering truly excellent data. We are also tremendously thankful
  to Kentaro Aoki for the incredible support while observing at Subaru with FMOS,
  and also to the Keck staff for the help with the observations with MOSFIRE. This
  work is based on observations obtained with WIRCam on the CFHT, OPTICON programme
  2011B/029, 2012A019 and 2012B/016. Based on observations made with ESO telescopes
  at the La Silla Paranal Observatory under programmes IDs 60.A-9460 (data can be
  accessed through the ESO data archive), 087.A 0337 and 089.A-0965. Based on observations
  done with FMOS on Subaru under programme S14A-084, and on MOSFIRE/Keck observations
  under programme U066M. Part of the data on which this analysis is based are available
  from Sobral et al. (2013a). Dedicated to the memory of C. M. Sobral (1953-2014).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: D.
  full_name: Sobral, D.
  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: P. N.
  full_name: Best, P. N.
  last_name: Best
- first_name: I.
  full_name: Smail, I.
  last_name: Smail
- first_name: A. A.
  full_name: Khostovan, A. A.
  last_name: Khostovan
- first_name: B.
  full_name: Milvang-Jensen, B.
  last_name: Milvang-Jensen
- first_name: J.-W.
  full_name: Kim, J.-W.
  last_name: Kim
- first_name: J.
  full_name: Stott, J.
  last_name: Stott
- first_name: J.
  full_name: Calhau, J.
  last_name: Calhau
- first_name: H.
  full_name: Nayyeri, H.
  last_name: Nayyeri
- first_name: B.
  full_name: Mobasher, B.
  last_name: Mobasher
citation:
  ama: 'Sobral D, Matthee JJ, Best PN, et al. CF-HiZELS, an ∼10 deg2 emission-line
    survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions
    at z = 0.8, 1.4 and 2.2 . <i>Monthly Notices of the Royal Astronomical Society</i>.
    2015;451(3):2303-2323. doi:<a href="https://doi.org/10.1093/mnras/stv1076">10.1093/mnras/stv1076</a>'
  apa: 'Sobral, D., Matthee, J. J., Best, P. N., Smail, I., Khostovan, A. A., Milvang-Jensen,
    B., … Mobasher, B. (2015). CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic
    follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and
    2.2 . <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University
    Press. <a href="https://doi.org/10.1093/mnras/stv1076">https://doi.org/10.1093/mnras/stv1076</a>'
  chicago: 'Sobral, D., Jorryt J Matthee, P. N. Best, I. Smail, A. A. Khostovan, B.
    Milvang-Jensen, J.-W. Kim, et al. “CF-HiZELS, an ∼10 Deg2 Emission-Line Survey
    with Spectroscopic Follow-up: Hα, [O III] + Hβ and [O II] Luminosity Functions
    at z = 0.8, 1.4 and 2.2 .” <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press, 2015. <a href="https://doi.org/10.1093/mnras/stv1076">https://doi.org/10.1093/mnras/stv1076</a>.'
  ieee: 'D. Sobral <i>et al.</i>, “CF-HiZELS, an ∼10 deg2 emission-line survey with
    spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z
    = 0.8, 1.4 and 2.2 ,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 451, no. 3. Oxford University Press, pp. 2303–2323, 2015.'
  ista: 'Sobral D, Matthee JJ, Best PN, Smail I, Khostovan AA, Milvang-Jensen B, Kim
    J-W, Stott J, Calhau J, Nayyeri H, Mobasher B. 2015. CF-HiZELS, an ∼10 deg2 emission-line
    survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions
    at z = 0.8, 1.4 and 2.2 . Monthly Notices of the Royal Astronomical Society. 451(3),
    2303–2323.'
  mla: 'Sobral, D., et al. “CF-HiZELS, an ∼10 Deg2 Emission-Line Survey with Spectroscopic
    Follow-up: Hα, [O III] + Hβ and [O II] Luminosity Functions at z = 0.8, 1.4 and
    2.2 .” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 451, no.
    3, Oxford University Press, 2015, pp. 2303–23, doi:<a href="https://doi.org/10.1093/mnras/stv1076">10.1093/mnras/stv1076</a>.'
  short: D. Sobral, J.J. Matthee, P.N. Best, I. Smail, A.A. Khostovan, B. Milvang-Jensen,
    J.-W. Kim, J. Stott, J. Calhau, H. Nayyeri, B. Mobasher, Monthly Notices of the
    Royal Astronomical Society 451 (2015) 2303–2323.
date_created: 2022-07-14T09:02:22Z
date_published: 2015-08-11T00:00:00Z
date_updated: 2022-08-19T08:23:18Z
day: '11'
doi: 10.1093/mnras/stv1076
extern: '1'
external_id:
  arxiv:
  - '1502.06602'
intvolume: '       451'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: luminosity function'
- mass function
- 'cosmology: observations'
- early Universe
- large-scale structure of Universe
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1502.06602
month: '08'
oa: 1
oa_version: Preprint
page: 2303-2323
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: 'CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up:
  Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 '
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 451
year: '2015'
...