---
_id: '11619'
abstract:
- lang: eng
  text: We report on the confirmation and mass determination of π Men c, the first
    transiting planet discovered by NASA’s TESS space mission. π Men is a naked-eye
    (V = 5.65 mag), quiet G0 V star that was previously known to host a sub-stellar
    companion (π Men b) on a longperiod (Porb = 2091 days), eccentric (e = 0.64) orbit.
    Using TESS time-series photometry, combined with Gaia data, published UCLES at
    AAT Doppler measurements, and archival HARPS at ESO-3.6m radial velocities, we
    found that π Men c is a close-in planet with an orbital period of Porb = 6.27
    days, a mass of Mc = 4.52 ± 0.81 M⊕, and a radius of Rc = 2.06 ± 0.03 R⊕. Based
    on the planet’s orbital period and size, π Men c is a super-Earth located at,
    or close to, the radius gap, while its mass and bulk density suggest it may have
    held on to a significant atmosphere. Because of the brightness of the host star,
    this system is highly suitable for a wide range of further studies to characterize
    the planetary atmosphere and dynamical properties. We also performed an asteroseismic
    analysis of the TESS data and detected a hint of power excess consistent with
    the seismic values expected for this star, although this result depends on the
    photometric aperture used to extract the light curve. This marginal detection
    is expected from pre-launch simulations hinting at the asteroseismic potential
    of the TESS mission for longer, multi-sector observations and/or for more evolved
    bright stars.
article_number: L10
article_processing_charge: No
article_type: letter_note
arxiv: 1
author:
- first_name: D.
  full_name: Gandolfi, D.
  last_name: Gandolfi
- first_name: O.
  full_name: Barragán, O.
  last_name: Barragán
- first_name: J. H.
  full_name: Livingston, J. H.
  last_name: Livingston
- first_name: M.
  full_name: Fridlund, M.
  last_name: Fridlund
- first_name: A. B.
  full_name: Justesen, A. B.
  last_name: Justesen
- first_name: S.
  full_name: Redfield, S.
  last_name: Redfield
- first_name: L.
  full_name: Fossati, L.
  last_name: Fossati
- first_name: S.
  full_name: Mathur, S.
  last_name: Mathur
- first_name: S.
  full_name: Grziwa, S.
  last_name: Grziwa
- first_name: J.
  full_name: Cabrera, J.
  last_name: Cabrera
- first_name: R. A.
  full_name: García, R. A.
  last_name: García
- first_name: C. M.
  full_name: Persson, C. M.
  last_name: Persson
- first_name: V.
  full_name: Van Eylen, V.
  last_name: Van Eylen
- first_name: A. P.
  full_name: Hatzes, A. P.
  last_name: Hatzes
- first_name: D.
  full_name: Hidalgo, D.
  last_name: Hidalgo
- first_name: S.
  full_name: Albrecht, S.
  last_name: Albrecht
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
- first_name: W. D.
  full_name: Cochran, W. D.
  last_name: Cochran
- first_name: Sz.
  full_name: Csizmadia, Sz.
  last_name: Csizmadia
- first_name: H.
  full_name: Deeg, H.
  last_name: Deeg
- first_name: Ph.
  full_name: Eigmüller, Ph.
  last_name: Eigmüller
- first_name: M.
  full_name: Endl, M.
  last_name: Endl
- first_name: A.
  full_name: Erikson, A.
  last_name: Erikson
- first_name: M.
  full_name: Esposito, M.
  last_name: Esposito
- first_name: E.
  full_name: Guenther, E.
  last_name: Guenther
- first_name: J.
  full_name: Korth, J.
  last_name: Korth
- first_name: R.
  full_name: Luque, R.
  last_name: Luque
- first_name: P.
  full_name: Montañes Rodríguez, P.
  last_name: Montañes Rodríguez
- first_name: D.
  full_name: Nespral, D.
  last_name: Nespral
- first_name: G.
  full_name: Nowak, G.
  last_name: Nowak
- first_name: M.
  full_name: Pätzold, M.
  last_name: Pätzold
- first_name: J.
  full_name: Prieto-Arranz, J.
  last_name: Prieto-Arranz
citation:
  ama: 'Gandolfi D, Barragán O, Livingston JH, et al. TESS’s first planet: A super-Earth
    transiting the naked-eye star π Mensae. <i>Astronomy &#38; Astrophysics</i>. 2018;619.
    doi:<a href="https://doi.org/10.1051/0004-6361/201834289">10.1051/0004-6361/201834289</a>'
  apa: 'Gandolfi, D., Barragán, O., Livingston, J. H., Fridlund, M., Justesen, A.
    B., Redfield, S., … Prieto-Arranz, J. (2018). TESS’s first planet: A super-Earth
    transiting the naked-eye star π Mensae. <i>Astronomy &#38; Astrophysics</i>. EDP
    Sciences. <a href="https://doi.org/10.1051/0004-6361/201834289">https://doi.org/10.1051/0004-6361/201834289</a>'
  chicago: 'Gandolfi, D., O. Barragán, J. H. Livingston, M. Fridlund, A. B. Justesen,
    S. Redfield, L. Fossati, et al. “TESS’s First Planet: A Super-Earth Transiting
    the Naked-Eye Star π Mensae.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences,
    2018. <a href="https://doi.org/10.1051/0004-6361/201834289">https://doi.org/10.1051/0004-6361/201834289</a>.'
  ieee: 'D. Gandolfi <i>et al.</i>, “TESS’s first planet: A super-Earth transiting
    the naked-eye star π Mensae,” <i>Astronomy &#38; Astrophysics</i>, vol. 619. EDP
    Sciences, 2018.'
  ista: 'Gandolfi D, Barragán O, Livingston JH, Fridlund M, Justesen AB, Redfield
    S, Fossati L, Mathur S, Grziwa S, Cabrera J, García RA, Persson CM, Van Eylen
    V, Hatzes AP, Hidalgo D, Albrecht S, Bugnet LA, Cochran WD, Csizmadia S, Deeg
    H, Eigmüller P, Endl M, Erikson A, Esposito M, Guenther E, Korth J, Luque R, Montañes
    Rodríguez P, Nespral D, Nowak G, Pätzold M, Prieto-Arranz J. 2018. TESS’s first
    planet: A super-Earth transiting the naked-eye star π Mensae. Astronomy &#38;
    Astrophysics. 619, L10.'
  mla: 'Gandolfi, D., et al. “TESS’s First Planet: A Super-Earth Transiting the Naked-Eye
    Star π Mensae.” <i>Astronomy &#38; Astrophysics</i>, vol. 619, L10, EDP Sciences,
    2018, doi:<a href="https://doi.org/10.1051/0004-6361/201834289">10.1051/0004-6361/201834289</a>.'
  short: D. Gandolfi, O. Barragán, J.H. Livingston, M. Fridlund, A.B. Justesen, S.
    Redfield, L. Fossati, S. Mathur, S. Grziwa, J. Cabrera, R.A. García, C.M. Persson,
    V. Van Eylen, A.P. Hatzes, D. Hidalgo, S. Albrecht, L.A. Bugnet, W.D. Cochran,
    S. Csizmadia, H. Deeg, P. Eigmüller, M. Endl, A. Erikson, M. Esposito, E. Guenther,
    J. Korth, R. Luque, P. Montañes Rodríguez, D. Nespral, G. Nowak, M. Pätzold, J.
    Prieto-Arranz, Astronomy &#38; Astrophysics 619 (2018).
date_created: 2022-07-18T14:41:16Z
date_published: 2018-11-22T00:00:00Z
date_updated: 2022-08-22T07:43:29Z
day: '22'
doi: 10.1051/0004-6361/201834289
extern: '1'
external_id:
  arxiv:
  - '1809.07573'
intvolume: '       619'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- planetary systems / planets and satellites
- detection / planets and satellites
- fundamental parameters / planets and satellites
- terrestrial planets / stars
- fundamental parameters
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1809.07573
month: '11'
oa: 1
oa_version: Preprint
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: 'TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 619
year: '2018'
...
---
_id: '11631'
abstract:
- lang: eng
  text: "The recently launched NASA Transiting Exoplanet Survey Satellite (TESS) mission
    is going to collect lightcurves for a few hundred million of stars and we expect
    to increase the number of pulsating stars to analyze compared to the few thousand
    stars observed by the CoRoT, Kepler and K2 missions. However, most of the TESS
    targets have not yet been properly classified and characterized. In order to improve
    the analysis of the TESS data, it is crucial to determine the type of stellar
    pulsations in a timely manner. We propose an automatic method to classify stars
    attending to their pulsation properties, in particular, to identify solar-like
    pulsators among all TESS targets. It relies on the use of the global amount of
    power contained in the power spectrum (already known as the FliPer method) as
    a key parameter, along with\r\nthe effective temperature, to feed into a machine
    learning classifier. Our study, based on TESS simulated datasets, shows that we
    are able to classify pulsators with a 98% accuracy."
article_number: '1811.12140'
article_processing_charge: No
arxiv: 1
author:
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
- first_name: R. A.
  full_name: García, R. A.
  last_name: García
- first_name: G. R.
  full_name: Davies, G. R.
  last_name: Davies
- first_name: S.
  full_name: Mathur, S.
  last_name: Mathur
- first_name: O. J.
  full_name: Hall, O. J.
  last_name: Hall
- first_name: B. M.
  full_name: Rendle, B. M.
  last_name: Rendle
citation:
  ama: 'Bugnet LA, García RA, Davies GR, Mathur S, Hall OJ, Rendle BM. FliPer: Classifying
    TESS pulsating stars. <i>arXiv</i>. doi:<a href="https://doi.org/10.48550/arXiv.1811.12140">10.48550/arXiv.1811.12140</a>'
  apa: 'Bugnet, L. A., García, R. A., Davies, G. R., Mathur, S., Hall, O. J., &#38;
    Rendle, B. M. (n.d.). FliPer: Classifying TESS pulsating stars. <i>arXiv</i>.
    <a href="https://doi.org/10.48550/arXiv.1811.12140">https://doi.org/10.48550/arXiv.1811.12140</a>'
  chicago: 'Bugnet, Lisa Annabelle, R. A. García, G. R. Davies, S. Mathur, O. J. Hall,
    and B. M. Rendle. “FliPer: Classifying TESS Pulsating Stars.” <i>ArXiv</i>, n.d.
    <a href="https://doi.org/10.48550/arXiv.1811.12140">https://doi.org/10.48550/arXiv.1811.12140</a>.'
  ieee: 'L. A. Bugnet, R. A. García, G. R. Davies, S. Mathur, O. J. Hall, and B. M.
    Rendle, “FliPer: Classifying TESS pulsating stars,” <i>arXiv</i>. .'
  ista: 'Bugnet LA, García RA, Davies GR, Mathur S, Hall OJ, Rendle BM. FliPer: Classifying
    TESS pulsating stars. arXiv, 1811.12140.'
  mla: 'Bugnet, Lisa Annabelle, et al. “FliPer: Classifying TESS Pulsating Stars.”
    <i>ArXiv</i>, 1811.12140, doi:<a href="https://doi.org/10.48550/arXiv.1811.12140">10.48550/arXiv.1811.12140</a>.'
  short: L.A. Bugnet, R.A. García, G.R. Davies, S. Mathur, O.J. Hall, B.M. Rendle,
    ArXiv (n.d.).
date_created: 2022-07-21T07:05:23Z
date_published: 2018-11-29T00:00:00Z
date_updated: 2022-08-22T08:41:55Z
day: '29'
doi: 10.48550/arXiv.1811.12140
extern: '1'
external_id:
  arxiv:
  - '1811.12140'
keyword:
- asteroseismology - methods
- data analysis - stars
- oscillations
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: ' https://doi.org/10.48550/arXiv.1811.12140'
month: '11'
oa: 1
oa_version: Preprint
publication: arXiv
publication_status: submitted
status: public
title: 'FliPer: Classifying TESS pulsating stars'
type: preprint
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
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: '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: '11572'
abstract:
- lang: eng
  text: We present spectroscopic follow-up of candidate luminous Ly α emitters (LAEs)
    at z = 5.7–6.6 in the SA22 field with VLT/X-SHOOTER. We confirm two new luminous
    LAEs at z = 5.676 (SR6) and z = 6.532 (VR7), and also present HST follow-up of
    both sources. These sources have luminosities LLy α ≈ 3 × 1043 erg s−1, very high
    rest-frame equivalent widths of EW0 ≳ 200 Å and narrow Ly α lines (200–340 km s−1).
    VR7 is the most UV-luminous LAE at z > 6.5, with M1500 = −22.5, even brighter
    in the UV than CR7. Besides Ly α, we do not detect any other rest-frame UV lines
    in the spectra of SR6 and VR7, and argue that rest-frame UV lines are easier to
    observe in bright galaxies with low Ly α equivalent widths. We confirm that Ly α
    line widths increase with Ly α luminosity at z = 5.7, while there are indications
    that Ly α lines of faint LAEs become broader at z = 6.6, potentially due to reionization.
    We find a large spread of up to 3 dex in UV luminosity for >L⋆ LAEs, but find
    that the Ly α luminosity of the brightest LAEs is strongly related to UV luminosity
    at z = 6.6. Under basic assumptions, we find that several LAEs at z ≈ 6–7 have
    Ly α escape fractions ≳ 100  per cent, indicating bursty star formation histories,
    alternative Ly α production mechanisms, or dust attenuating Ly α emission differently
    than UV emission. Finally, we present a method to compute ξion, the production
    efficiency of ionizing photons, and find that LAEs at z ≈ 6–7 have high values
    of log10(ξion/Hz erg−1) ≈ 25.51 ± 0.09 that may alleviate the need for high Lyman-Continuum
    escape fractions required for reionization.
acknowledgement: 'We thank the referee for a constructive report that has improved
  the quality and clarity of this work. The authors thank Grecco Oyarzún for discussions.
  JM acknowledges the support of a Huygens PhD fellowship from Leiden University.
  DS 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. BD acknowledges financial support from NASA
  through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G.
  We thank Kasper Schmidt for providing measurements. Based on observations with the
  W.M. Keck Observatory through programme C267D. The W.M. Keck Observatory is operated
  as a scientific partnership amongst the California Institute of Technology, the
  University of California and the National Aeronautics and Space Administration.
  Based on observations made with ESO Telescopes at the La Silla Paranal Observatory
  under programme IDs 097.A-0943, 294.A 5018 and 098.A-0819 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 observing time (W16AN004) and 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.
  Based on observations made with the NASA/ESA HST, obtained (from the Data Archive)
  at the Space Telescope Science Institute, which is operated by the Association of
  Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These
  observations are associated with programme #14699. We are grateful for the excellent
  data sets from the COSMOS, UltraVISTA, SXDS, UDS and CFHTLS survey teams; without
  these legacy surveys, this research would have been impossible. We have benefited
  from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB,
  PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP
  and SCAMP 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: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Behnam
  full_name: Darvish, Behnam
  last_name: Darvish
- first_name: Sérgio
  full_name: Santos, Sérgio
  last_name: Santos
- first_name: Bahram
  full_name: Mobasher, Bahram
  last_name: Mobasher
- first_name: Ana
  full_name: Paulino-Afonso, Ana
  last_name: Paulino-Afonso
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
- first_name: Lara
  full_name: Alegre, Lara
  last_name: Alegre
citation:
  ama: Matthee JJ, Sobral D, Darvish B, et al. Spectroscopic properties of luminous
    Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2017;472(1):772-787. doi:<a href="https://doi.org/10.1093/mnras/stx2061">10.1093/mnras/stx2061</a>
  apa: Matthee, J. J., Sobral, D., Darvish, B., Santos, S., Mobasher, B., Paulino-Afonso,
    A., … Alegre, L. (2017). Spectroscopic properties of luminous Ly α emitters at
    z ≈ 6–7 and comparison to the Lyman-break population. <i>Monthly Notices of the
    Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx2061">https://doi.org/10.1093/mnras/stx2061</a>
  chicago: Matthee, Jorryt J, David Sobral, Behnam Darvish, Sérgio Santos, Bahram
    Mobasher, Ana Paulino-Afonso, Huub Röttgering, and Lara Alegre. “Spectroscopic
    Properties of Luminous Ly α Emitters at z ≈ 6–7 and Comparison to the Lyman-Break
    Population.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford
    University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx2061">https://doi.org/10.1093/mnras/stx2061</a>.
  ieee: J. J. Matthee <i>et al.</i>, “Spectroscopic properties of luminous Ly α emitters
    at z ≈ 6–7 and comparison to the Lyman-break population,” <i>Monthly Notices of
    the Royal Astronomical Society</i>, vol. 472, no. 1. Oxford University Press,
    pp. 772–787, 2017.
  ista: Matthee JJ, Sobral D, Darvish B, Santos S, Mobasher B, Paulino-Afonso A, Röttgering
    H, Alegre L. 2017. Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7
    and comparison to the Lyman-break population. Monthly Notices of the Royal Astronomical
    Society. 472(1), 772–787.
  mla: Matthee, Jorryt J., et al. “Spectroscopic Properties of Luminous Ly α Emitters
    at z ≈ 6–7 and Comparison to the Lyman-Break Population.” <i>Monthly Notices of
    the Royal Astronomical Society</i>, vol. 472, no. 1, Oxford University Press,
    2017, pp. 772–87, doi:<a href="https://doi.org/10.1093/mnras/stx2061">10.1093/mnras/stx2061</a>.
  short: J.J. Matthee, D. Sobral, B. Darvish, S. Santos, B. Mobasher, A. Paulino-Afonso,
    H. Röttgering, L. Alegre, Monthly Notices of the Royal Astronomical Society 472
    (2017) 772–787.
date_created: 2022-07-13T09:47:39Z
date_published: 2017-11-01T00:00:00Z
date_updated: 2022-08-19T08:05:37Z
day: '01'
doi: 10.1093/mnras/stx2061
extern: '1'
external_id:
  arxiv:
  - '1706.06591'
intvolume: '       472'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution – galaxies: high-redshift'
- dark ages
- reionization
- first stars
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1706.06591
month: '11'
oa: 1
oa_version: Preprint
page: 772-787
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: Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison
  to the Lyman-break population
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 472
year: '2017'
...
---
_id: '11633'
abstract:
- lang: eng
  text: Our understanding of stars through asteroseismic data analysis is limited
    by our ability to take advantage of the huge amount of observed stars provided
    by space missions such as CoRoT, Kepler , K2, and soon TESS and PLATO. Global
    seismic pipelines provide global stellar parameters such as mass and radius using
    the mean seismic parameters, as well as the effective temperature. These pipelines
    are commonly used automatically on thousands of stars observed by K2 for 3 months
    (and soon TESS for at least ∼ 1 month). However, pipelines are not immune from
    misidentifying noise peaks and stellar oscillations. Therefore, new validation
    techniques are required to assess the quality of these results. We present a new
    metric called FliPer (Flicker in Power), which takes into account the average
    variability at all measured time scales. The proper calibration of FliPer enables
    us to obtain good estimations of global stellar parameters such as surface gravity
    that are robust against the influence of noise peaks and hence are an excellent
    way to find faults in asteroseismic pipelines.
article_number: '1711.02890'
article_processing_charge: No
arxiv: 1
author:
- first_name: Lisa Annabelle
  full_name: Bugnet, Lisa Annabelle
  id: d9edb345-f866-11ec-9b37-d119b5234501
  last_name: Bugnet
  orcid: 0000-0003-0142-4000
- first_name: R. A.
  full_name: Garcia, R. A.
  last_name: Garcia
- first_name: G. R.
  full_name: Davies, G. R.
  last_name: Davies
- first_name: S.
  full_name: Mathur, S.
  last_name: Mathur
- first_name: E.
  full_name: Corsaro, E.
  last_name: Corsaro
citation:
  ama: 'Bugnet LA, Garcia RA, Davies GR, Mathur S, Corsaro E. FliPer: Checking the
    reliability of global seismic parameters from automatic pipelines. <i>arXiv</i>.
    doi:<a href="https://doi.org/10.48550/arXiv.1711.02890">10.48550/arXiv.1711.02890</a>'
  apa: 'Bugnet, L. A., Garcia, R. A., Davies, G. R., Mathur, S., &#38; Corsaro, E.
    (n.d.). FliPer: Checking the reliability of global seismic parameters from automatic
    pipelines. <i>arXiv</i>. <a href="https://doi.org/10.48550/arXiv.1711.02890">https://doi.org/10.48550/arXiv.1711.02890</a>'
  chicago: 'Bugnet, Lisa Annabelle, R. A. Garcia, G. R. Davies, S. Mathur, and E.
    Corsaro. “FliPer: Checking the Reliability of Global Seismic Parameters from Automatic
    Pipelines.” <i>ArXiv</i>, n.d. <a href="https://doi.org/10.48550/arXiv.1711.02890">https://doi.org/10.48550/arXiv.1711.02890</a>.'
  ieee: 'L. A. Bugnet, R. A. Garcia, G. R. Davies, S. Mathur, and E. Corsaro, “FliPer:
    Checking the reliability of global seismic parameters from automatic pipelines,”
    <i>arXiv</i>. .'
  ista: 'Bugnet LA, Garcia RA, Davies GR, Mathur S, Corsaro E. FliPer: Checking the
    reliability of global seismic parameters from automatic pipelines. arXiv, 1711.02890.'
  mla: 'Bugnet, Lisa Annabelle, et al. “FliPer: Checking the Reliability of Global
    Seismic Parameters from Automatic Pipelines.” <i>ArXiv</i>, 1711.02890, doi:<a
    href="https://doi.org/10.48550/arXiv.1711.02890">10.48550/arXiv.1711.02890</a>.'
  short: L.A. Bugnet, R.A. Garcia, G.R. Davies, S. Mathur, E. Corsaro, ArXiv (n.d.).
date_created: 2022-07-21T07:13:13Z
date_published: 2017-11-08T00:00:00Z
date_updated: 2022-08-22T08:45:42Z
day: '08'
doi: 10.48550/arXiv.1711.02890
extern: '1'
external_id:
  arxiv:
  - '1711.02890'
keyword:
- asteroseismology - methods
- data analysis - stars
- oscillations
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.48550/arXiv.1711.02890
month: '11'
oa: 1
oa_version: Preprint
publication: arXiv
publication_status: submitted
status: public
title: 'FliPer: Checking the reliability of global seismic parameters from automatic
  pipelines'
type: preprint
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
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: '11575'
abstract:
- lang: eng
  text: We investigate correlations between different physical properties of star-forming
    galaxies in the ‘Evolution and Assembly of GaLaxies and their Environments’ (EAGLE)
    cosmological hydrodynamical simulation suite over the redshift range 0 ≤ z ≤ 4.5.
    A principal component analysis reveals that neutral gas fraction (fgas,neutral),
    stellar mass (Mstellar) and star formation rate (SFR) account for most of the
    variance seen in the population, with galaxies tracing a two-dimensional, nearly
    flat, surface in the three-dimensional space of fgas, neutral–Mstellar–SFR with
    little scatter. The location of this plane varies little with redshift, whereas
    galaxies themselves move along the plane as their fgas, neutral and SFR drop with
    redshift. The positions of galaxies along the plane are highly correlated with
    gas metallicity. The metallicity can therefore be robustly predicted from fgas,
    neutral, or from the Mstellar and SFR. We argue that the appearance of this ‘Fundamental
    Plane of star formation’ is a consequence of self-regulation, with the plane's
    curvature set by the dependence of the SFR on gas density and metallicity. We
    analyse a large compilation of observations spanning the redshift range 0 ≲ z
    ≲ 3, and find that such a plane is also present in the data. The properties of
    the observed Fundamental Plane of star formation are in good agreement with EAGLE's
    predictions.
acknowledgement: We thank Luca Cortese, Matt Bothwell, Paola Santini and Tim Davis
  for providing observational data sets, and Aaron Robotham, Luca Cortese and Barbara
  Catinella for useful discussions. CdPL is funded by a Discovery Early Career Researcher
  Award (DE150100618). CdPL also thanks the MERAC Foundation for a Postdoctoral Research
  Award. This work used the DiRAC Data Centric system at Durham University, operated
  by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility
  (www.dirac.ac.uk). This equipment was funded by BIS National E-infrastructure capital
  grant ST/K00042X/1, STFC capital grant ST/H008519/1, and STFC DiRAC Operations grant
  ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure.
  Support was also received via the Interuniversity Attraction Poles Programme initiated
  by the Belgian Science Policy Office ([AP P7/08 CHARM]), the National Science Foundation
  under grant no. NSF PHY11-25915, and the UK Science and Technology Facilities Council
  (grant numbers ST/F001166/1 and ST/I000976/1) via rolling and consolidating grants
  awarded to the ICC. The research was supported in part by the European Research
  Council under the European Union‘s Seventh Framework Programme (FP7/2007-2013)/ERC
  grant agreement 278594-GasAroundGalaxies.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Claudia del P.
  full_name: Lagos, Claudia del P.
  last_name: Lagos
- first_name: Tom
  full_name: Theuns, Tom
  last_name: Theuns
- first_name: Joop
  full_name: Schaye, Joop
  last_name: Schaye
- first_name: Michelle
  full_name: Furlong, Michelle
  last_name: Furlong
- first_name: Richard G.
  full_name: Bower, Richard G.
  last_name: Bower
- first_name: Matthieu
  full_name: Schaller, Matthieu
  last_name: Schaller
- first_name: Robert A.
  full_name: Crain, Robert A.
  last_name: Crain
- first_name: James W.
  full_name: Trayford, James W.
  last_name: Trayford
- 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: Lagos C del P, Theuns T, Schaye J, et al. The Fundamental Plane of star formation
    in galaxies revealed by the EAGLE hydrodynamical simulations. <i>Monthly Notices
    of the Royal Astronomical Society</i>. 2016;459(3):2632-2650. doi:<a href="https://doi.org/10.1093/mnras/stw717">10.1093/mnras/stw717</a>
  apa: Lagos, C. del P., Theuns, T., Schaye, J., Furlong, M., Bower, R. G., Schaller,
    M., … Matthee, J. J. (2016). The Fundamental Plane of star formation in galaxies
    revealed by the EAGLE hydrodynamical simulations. <i>Monthly Notices of the Royal
    Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stw717">https://doi.org/10.1093/mnras/stw717</a>
  chicago: Lagos, Claudia del P., Tom Theuns, Joop Schaye, Michelle Furlong, Richard
    G. Bower, Matthieu Schaller, Robert A. Crain, James W. Trayford, and Jorryt J
    Matthee. “The Fundamental Plane of Star Formation in Galaxies Revealed by the
    EAGLE Hydrodynamical Simulations.” <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press, 2016. <a href="https://doi.org/10.1093/mnras/stw717">https://doi.org/10.1093/mnras/stw717</a>.
  ieee: C. del P. Lagos <i>et al.</i>, “The Fundamental Plane of star formation in
    galaxies revealed by the EAGLE hydrodynamical simulations,” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 459, no. 3. Oxford University Press,
    pp. 2632–2650, 2016.
  ista: Lagos C del P, Theuns T, Schaye J, Furlong M, Bower RG, Schaller M, Crain
    RA, Trayford JW, Matthee JJ. 2016. The Fundamental Plane of star formation in
    galaxies revealed by the EAGLE hydrodynamical simulations. Monthly Notices of
    the Royal Astronomical Society. 459(3), 2632–2650.
  mla: Lagos, Claudia del P., et al. “The Fundamental Plane of Star Formation in Galaxies
    Revealed by the EAGLE Hydrodynamical Simulations.” <i>Monthly Notices of the Royal
    Astronomical Society</i>, vol. 459, no. 3, Oxford University Press, 2016, pp.
    2632–50, doi:<a href="https://doi.org/10.1093/mnras/stw717">10.1093/mnras/stw717</a>.
  short: C. del P. Lagos, T. Theuns, J. Schaye, M. Furlong, R.G. Bower, M. Schaller,
    R.A. Crain, J.W. Trayford, J.J. Matthee, Monthly Notices of the Royal Astronomical
    Society 459 (2016) 2632–2650.
date_created: 2022-07-13T10:21:24Z
date_published: 2016-07-01T00:00:00Z
date_updated: 2022-08-19T08:12:07Z
day: '01'
doi: 10.1093/mnras/stw717
extern: '1'
external_id:
  arxiv:
  - '1510.08067'
intvolume: '       459'
issue: '3'
keyword:
- Space and Planetary Science
- 'Astronomy and Astrophysics  stars: formation'
- 'ISM: evolution'
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: ISM'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1510.08067
month: '07'
oa: 1
oa_version: Preprint
page: 2632-2650
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 Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical
  simulations
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 459
year: '2016'
...
---
_id: '11519'
abstract:
- lang: eng
  text: 'Faint Lyα emitters become increasingly rarer toward the reionization epoch
    (z ∼ 6–7). However, observations from a very large (∼5 deg2) Lyα narrow-band survey
    at z = 6.6 show that this is not the case for the most luminous emitters, capable
    of ionizing their own local bubbles. Here we present follow-up observations of
    the two most luminous Lyα candidates in the COSMOS field: “MASOSA” and “CR7.”
    We used X-SHOOTER, SINFONI, and FORS2 on the Very Large Telescope, and DEIMOS
    on Keck, to confirm both candidates beyond any doubt. We find redshifts of z =
    6.541 and z = 6.604 for “MASOSA” and “CR7,” respectively. MASOSA has a strong
    detection in Lyα with a line width of 386 ± 30 km s−1 (FWHM) and with very high
    EW0 (>200 Å), but undetected in the continuum, implying very low stellar mass
    and a likely young, metal-poor stellar population. “CR7,” with an observed Lyα
    luminosity of 1043.92±0.05 erg s−1 is the most luminous Lyα emitter ever found
    at z > 6 and is spatially extended (∼16 kpc). “CR7” reveals a narrow Lyα line
    with 266 ± 15 km s−1 FWHM, being detected in the near-infrared (NIR) (rest-frame
    UV; β = −2.3 ± 0.1) and in IRAC/Spitzer. We detect a narrow He II 1640 Å emission
    line (6σ, FWHM = 130 ± 30 km s−1 ) in CR7 which can explain the clear excess seen
    in the J-band photometry (EW0 ∼ 80 Å). We find no other emission lines from the
    UV to the NIR in our X-SHOOTER spectra (He II/O III] 1663 Å > 3 and He II/C III]
    1908 Å > 2.5). We conclude that CR7 is best explained by a combination of a PopIII-like
    population, which dominates the rest-frame UV and the nebular emission, and a
    more normal stellar population, which presumably dominates the mass. Hubble Space
    Telescope/WFC3 observations show that the light is indeed spatially separated
    between a very blue component, coincident with Lyα and He II emission, and two
    red components (∼5 kpc away), which dominate the mass. Our findings are consistent
    with theoretical predictions of a PopIII wave, with PopIII star formation migrating
    away from the original sites of star formation.'
acknowledgement: We thank the anonymous reviewer for useful and constructive comments
  and suggestions which greatly improved the quality and clarity of our work. D.S.
  acknowledges financial support from the Netherlands Organisation for Scientific
  research (NWO) through a Veni fellowship, from FCT through a FCT Investigator Starting
  Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010), from FCT grant UID/FIS/04434/2013,
  and from LSF and LKBF. J.M. acknowledges the award of a Huygens PhD fellowship.
  H.R. acknowledges support from the ERC Advanced Investigator program NewClusters
  321271. The authors thank Mark Dijkstra, Bhaskar Agarwal, Jarrett Johnson, Andrea
  Ferrara, Jarle Brinchmann, Rebecca Bowler, George Becker, Emma Curtis-Lake, Milos
  Milosavljevic, Raffaella Schneider, Paul Shapiro, and Erik Zackrisson for interesting,
  stimulating and helpful discussions. The authors are extremely grateful to ESO for
  the award of ESO DDT time (294.A-5018 and 294.A-5039) which allowed the spectroscopic
  confirmation of both sources and the detailed investigation of their nature. Observations
  are also based on data from W.M. Keck Observatory. The W.M. Keck Observatory is
  operated as a scientific partnership of Caltech, the University of California and
  the National Aeronautics and Space Administration. 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 lUnivers 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 IDs 294.A-5018,
  294.A-5039, 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.
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: Daniel
  full_name: Schaerer, Daniel
  last_name: Schaerer
- first_name: Bahram
  full_name: Mobasher, Bahram
  last_name: Mobasher
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
- first_name: Sérgio
  full_name: Santos, Sérgio
  last_name: Santos
- first_name: Shoubaneh
  full_name: Hemmati, Shoubaneh
  last_name: Hemmati
citation:
  ama: 'Sobral D, Matthee JJ, Darvish B, et al. Evidence for PopIII-like stellar populations
    in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic
    confirmation. <i>The Astrophysical Journal</i>. 2015;808(2):139. doi:<a href="https://doi.org/10.1088/0004-637X/808/2/139">10.1088/0004-637X/808/2/139</a>'
  apa: 'Sobral, D., Matthee, J. J., Darvish, B., Schaerer, D., Mobasher, B., Röttgering,
    H., … Hemmati, S. (2015). Evidence for PopIII-like stellar populations in the
    most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation.
    <i>The Astrophysical Journal</i>. IOP Publishing. <a href="https://doi.org/10.1088/0004-637X/808/2/139">https://doi.org/10.1088/0004-637X/808/2/139</a>'
  chicago: 'Sobral, David, Jorryt J Matthee, Behnam Darvish, Daniel Schaerer, Bahram
    Mobasher, Huub Röttgering, Sérgio Santos, and Shoubaneh Hemmati. “Evidence for
    PopIII-like Stellar Populations in the Most Luminous Lyα Emitters at the Epoch
    of Reionisation: Spectroscopic Confirmation.” <i>The Astrophysical Journal</i>.
    IOP Publishing, 2015. <a href="https://doi.org/10.1088/0004-637X/808/2/139">https://doi.org/10.1088/0004-637X/808/2/139</a>.'
  ieee: 'D. Sobral <i>et al.</i>, “Evidence for PopIII-like stellar populations in
    the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation,”
    <i>The Astrophysical Journal</i>, vol. 808, no. 2. IOP Publishing, p. 139, 2015.'
  ista: 'Sobral D, Matthee JJ, Darvish B, Schaerer D, Mobasher B, Röttgering H, Santos
    S, Hemmati S. 2015. Evidence for PopIII-like stellar populations in the most luminous
    Lyα emitters at the epoch of reionisation: Spectroscopic confirmation. The Astrophysical
    Journal. 808(2), 139.'
  mla: 'Sobral, David, et al. “Evidence for PopIII-like Stellar Populations in the
    Most Luminous Lyα Emitters at the Epoch of Reionisation: Spectroscopic Confirmation.”
    <i>The Astrophysical Journal</i>, vol. 808, no. 2, IOP Publishing, 2015, p. 139,
    doi:<a href="https://doi.org/10.1088/0004-637X/808/2/139">10.1088/0004-637X/808/2/139</a>.'
  short: D. Sobral, J.J. Matthee, B. Darvish, D. Schaerer, B. Mobasher, H. Röttgering,
    S. Santos, S. Hemmati, The Astrophysical Journal 808 (2015) 139.
date_created: 2022-07-07T09:00:58Z
date_published: 2015-07-28T00:00:00Z
date_updated: 2022-08-18T10:30:13Z
day: '28'
doi: 10.1088/0004-637X/808/2/139
extern: '1'
external_id:
  arxiv:
  - '1504.01734'
intvolume: '       808'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- dark ages
- reionization
- 'first stars – early universe – galaxies: evolution'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1504.01734
month: '07'
oa: 1
oa_version: Preprint
page: '139'
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: 'Evidence for PopIII-like stellar populations in the most luminous Lyα emitters
  at the epoch of reionisation: Spectroscopic confirmation'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 808
year: '2015'
...
---
_id: '11579'
abstract:
- lang: eng
  text: CR7 is the brightest z = 6.6 Ly α emitter (LAE) known to date, and spectroscopic
    follow-up by Sobral et al. suggests that CR7 might host Population (Pop) III stars.
    We examine this interpretation using cosmological hydrodynamical simulations.
    Several simulated galaxies show the same ‘Pop III wave’ pattern observed in CR7.
    However, to reproduce the extreme CR7 Ly α/He II1640 line luminosities (⁠Lα/HeII⁠)
    a top-heavy initial mass function and a massive ( ≳ 107 M⊙) Pop III burst with
    age ≲ 2 Myr are required. Assuming that the observed properties of Ly α and He II
    emission are typical for Pop III, we predict that in the COSMOS/UDS/SA22 fields,
    14 out of the 30 LAEs at z = 6.6 with Lα > 1043.3 erg s−1 should also host Pop
    III stars producing an observable LHeII≳1042.7ergs−1⁠. As an alternate explanation,
    we explore the possibility that CR7 is instead powered by accretion on to a direct
    collapse black hole. Our model predicts Lα, LHeII⁠, and X-ray luminosities that
    are in agreement with the observations. In any case, the observed properties of
    CR7 indicate that this galaxy is most likely powered by sources formed from pristine
    gas. We propose that further X-ray observations can distinguish between the two
    above scenarios.
acknowledgement: SS acknowledges support from the Netherlands Organization for Scientific
  research (NWO), VENI grant 639.041.233. RS acknowledges support from the European
  Research Council under the European Union (FP/2007-2013)/ERC grant agreement no.
  306476. DS acknowledges (i) financial support from the NWO through a Veni fellowship
  and (ii) funding from FCT through a FCT Investigator Starting Grant and Start-up
  Grant (IF/01154/2012/CP0189/CT0010) and from FCT grant PEstOE/FIS/UI2751/2014.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: A.
  full_name: Pallottini, A.
  last_name: Pallottini
- first_name: A.
  full_name: Ferrara, A.
  last_name: Ferrara
- first_name: F.
  full_name: Pacucci, F.
  last_name: Pacucci
- first_name: S.
  full_name: Gallerani, S.
  last_name: Gallerani
- first_name: S.
  full_name: Salvadori, S.
  last_name: Salvadori
- first_name: R.
  full_name: Schneider, R.
  last_name: Schneider
- first_name: D.
  full_name: Schaerer, D.
  last_name: Schaerer
- 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
citation:
  ama: 'Pallottini A, Ferrara A, Pacucci F, et al. The brightest Lyα emitter: Pop
    III or black hole? <i>Monthly Notices of the Royal Astronomical Society</i>. 2015;453(3):2465-2470.
    doi:<a href="https://doi.org/10.1093/mnras/stv1795">10.1093/mnras/stv1795</a>'
  apa: 'Pallottini, A., Ferrara, A., Pacucci, F., Gallerani, S., Salvadori, S., Schneider,
    R., … Matthee, J. J. (2015). The brightest Lyα emitter: Pop III or black hole?
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press.
    <a href="https://doi.org/10.1093/mnras/stv1795">https://doi.org/10.1093/mnras/stv1795</a>'
  chicago: 'Pallottini, A., A. Ferrara, F. Pacucci, S. Gallerani, S. Salvadori, R.
    Schneider, D. Schaerer, D. Sobral, and Jorryt J Matthee. “The Brightest Lyα Emitter:
    Pop III or Black Hole?” <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press, 2015. <a href="https://doi.org/10.1093/mnras/stv1795">https://doi.org/10.1093/mnras/stv1795</a>.'
  ieee: 'A. Pallottini <i>et al.</i>, “The brightest Lyα emitter: Pop III or black
    hole?,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 453, no.
    3. Oxford University Press, pp. 2465–2470, 2015.'
  ista: 'Pallottini A, Ferrara A, Pacucci F, Gallerani S, Salvadori S, Schneider R,
    Schaerer D, Sobral D, Matthee JJ. 2015. The brightest Lyα emitter: Pop III or
    black hole? Monthly Notices of the Royal Astronomical Society. 453(3), 2465–2470.'
  mla: 'Pallottini, A., et al. “The Brightest Lyα Emitter: Pop III or Black Hole?”
    <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 453, no. 3, Oxford
    University Press, 2015, pp. 2465–70, doi:<a href="https://doi.org/10.1093/mnras/stv1795">10.1093/mnras/stv1795</a>.'
  short: A. Pallottini, A. Ferrara, F. Pacucci, S. Gallerani, S. Salvadori, R. Schneider,
    D. Schaerer, D. Sobral, J.J. Matthee, Monthly Notices of the Royal Astronomical
    Society 453 (2015) 2465–2470.
date_created: 2022-07-14T08:58:36Z
date_published: 2015-11-01T00:00:00Z
date_updated: 2022-08-19T08:19:23Z
day: '01'
doi: 10.1093/mnras/stv1795
extern: '1'
external_id:
  arxiv:
  - '1506.07173'
intvolume: '       453'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- black hole physics
- 'stars: Population III'
- 'galaxies: high-redshift'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1506.07173
month: '11'
oa: 1
oa_version: Preprint
page: 2465-2470
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 brightest Lyα emitter: Pop III or black hole?'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 453
year: '2015'
...
---
_id: '11583'
abstract:
- lang: eng
  text: 'Candidate galaxies at redshifts of z ∼ 10 are now being found in extremely
    deep surveys, probing very small areas. As a consequence, candidates are very
    faint, making spectroscopic confirmation practically impossible. In order to overcome
    such limitations, we have undertaken the CF-HiZELS survey, which is a large-area,
    medium-depth near-infrared narrow-band survey targeted at z = 8.8 Lyman α (Lyα)
    emitters (LAEs) and covering 10 deg2 in part of the SSA22 field with the Canada–France–Hawaii
    Telescope (CFHT). We surveyed a comoving volume of 4.7 × 106 Mpc3 to a Lyα luminosity
    limit of 6.3 × 1043舁erg舁s−1. We look for Lyα candidates by applying the following
    criteria: (i) clear emission-line source, (ii) no optical detections (ugriz from
    CFHTLS), (iii) no visible detection in the optical stack (ugriz > 27), (iv) visually
    checked reliable NBJ and J detections and (v) J − K ≤ 0. We compute photometric
    redshifts and remove a significant amount of dusty lower redshift line-emitters
    at z ∼ 1.4 or 2.2. A total of 13 Lyα candidates were found, of which two are marked
    as strong candidates, but the majority have very weak constraints on their spectral
    energy distributions. Using follow-up observations with SINFONI/VLT, we are able
    to exclude the most robust candidates as LAEs. We put a strong constraint on the
    Lyα luminosity function at z ∼ 9 and make realistic predictions for ongoing and
    future surveys. Our results show that surveys for the highest redshift LAEs are
    susceptible of multiple contaminations and that spectroscopic follow-up is absolutely
    necessary.'
acknowledgement: We thank the anonymous referee for the comments and suggestions which
  improved both the quality and clarity of this work. DS acknowledges financial support
  from the Netherlands Organisation for Scientific Research (NWO) through a Veni fellowship.
  IRS acknowledges support from STFC (ST/I001573/1), a Leverhulme Fellowship, the
  ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson
  Merit Award. PNB acknowledges support from the Leverhulme Trust. JWK acknowledges
  the support from the Creative Research Initiative Program, no. 2008- 0060544, of
  the National Research Foundation of Korea (NRF) funded by the Korean government
  (MSIP). JPUF and BMJ acknowledge support from the ERC-StG grant EGGS-278202. The
  Dark Cosmology Centre is funded by the Danish National Research Foundation. This
  work is based in part on data obtained as part of the UKIRT Infrared Deep Sky Survey.
  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. This work was
  only possible due to OPTICON/FP7 and the access that it granted to the CFHT telescope.
  The authors also wish to acknowledge the CFHTLS and UKIDSS surveys for their excellent
  legacy and complementary value – without such high-quality data sets, this research
  would not have been possible.
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: A. M.
  full_name: Swinbank, A. M.
  last_name: Swinbank
- first_name: Ian
  full_name: Smail, Ian
  last_name: Smail
- first_name: P. N.
  full_name: Best, P. N.
  last_name: Best
- first_name: Jae-Woo
  full_name: Kim, Jae-Woo
  last_name: Kim
- first_name: Marijn
  full_name: Franx, Marijn
  last_name: Franx
- first_name: Bo
  full_name: Milvang-Jensen, Bo
  last_name: Milvang-Jensen
- first_name: Johan
  full_name: Fynbo, Johan
  last_name: Fynbo
citation:
  ama: 'Matthee JJ, Sobral D, Swinbank AM, et al. A 10 deg2 Lyman α survey at z=8.8
    with spectroscopic follow-up: Strong constraints on the luminosity function and
    implications for other surveys. <i>Monthly Notices of the Royal Astronomical Society</i>.
    2014;440(3):2375-2387. doi:<a href="https://doi.org/10.1093/mnras/stu392">10.1093/mnras/stu392</a>'
  apa: 'Matthee, J. J., Sobral, D., Swinbank, A. M., Smail, I., Best, P. N., Kim,
    J.-W., … Fynbo, J. (2014). A 10 deg2 Lyman α survey at z=8.8 with spectroscopic
    follow-up: Strong constraints on the luminosity function and implications for
    other surveys. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford
    University Press. <a href="https://doi.org/10.1093/mnras/stu392">https://doi.org/10.1093/mnras/stu392</a>'
  chicago: 'Matthee, Jorryt J, David Sobral, A. M. Swinbank, Ian Smail, P. N. Best,
    Jae-Woo Kim, Marijn Franx, Bo Milvang-Jensen, and Johan Fynbo. “A 10 Deg2 Lyman
    α Survey at Z=8.8 with Spectroscopic Follow-up: Strong Constraints on the Luminosity
    Function and Implications for Other Surveys.” <i>Monthly Notices of the Royal
    Astronomical Society</i>. Oxford University Press, 2014. <a href="https://doi.org/10.1093/mnras/stu392">https://doi.org/10.1093/mnras/stu392</a>.'
  ieee: 'J. J. Matthee <i>et al.</i>, “A 10 deg2 Lyman α survey at z=8.8 with spectroscopic
    follow-up: Strong constraints on the luminosity function and implications for
    other surveys,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol.
    440, no. 3. Oxford University Press, pp. 2375–2387, 2014.'
  ista: 'Matthee JJ, Sobral D, Swinbank AM, Smail I, Best PN, Kim J-W, Franx M, Milvang-Jensen
    B, Fynbo J. 2014. A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up:
    Strong constraints on the luminosity function and implications for other surveys.
    Monthly Notices of the Royal Astronomical Society. 440(3), 2375–2387.'
  mla: 'Matthee, Jorryt J., et al. “A 10 Deg2 Lyman α Survey at Z=8.8 with Spectroscopic
    Follow-up: Strong Constraints on the Luminosity Function and Implications for
    Other Surveys.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol.
    440, no. 3, Oxford University Press, 2014, pp. 2375–87, doi:<a href="https://doi.org/10.1093/mnras/stu392">10.1093/mnras/stu392</a>.'
  short: J.J. Matthee, D. Sobral, A.M. Swinbank, I. Smail, P.N. Best, J.-W. Kim, M.
    Franx, B. Milvang-Jensen, J. Fynbo, Monthly Notices of the Royal Astronomical
    Society 440 (2014) 2375–2387.
date_created: 2022-07-14T12:33:24Z
date_published: 2014-05-21T00:00:00Z
date_updated: 2022-08-19T08:30:30Z
day: '21'
doi: 10.1093/mnras/stu392
extern: '1'
external_id:
  arxiv:
  - '1402.6697'
intvolume: '       440'
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/1402.6697
month: '05'
oa: 1
oa_version: Preprint
page: 2375-2387
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 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints
  on the luminosity function and implications for other surveys'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 440
year: '2014'
...