---
_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: '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: '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'
...