---
_id: '11561'
abstract:
- lang: eng
  text: We present a sample of ∼1000 emission-line galaxies at z = 0.4–4.7 from the
    ∼0.7deg2 High-z Emission-Line Survey in the Boötes field identified with a suite
    of six narrow-band filters at ≈0.4–2.1 μm. These galaxies have been selected on
    their Ly α (73), [O II] (285), H β/[O III] (387) or H α (362) emission line, and
    have been classified with optical to near-infrared colours. A subsample of 98
    sources have reliable redshifts from multiple narrow-band (e.g. [O II]–H α) detections
    and/or spectroscopy. In this survey paper, we present the observations, selection
    and catalogues of emitters. We measure number densities of Ly α, [O II], H β/[O III]
    and H α and confirm strong luminosity evolution in star-forming galaxies from
    z ∼ 0.4 to ∼5, in agreement with previous results. To demonstrate the usefulness
    of dual-line emitters, we use the sample of dual [O II]–H α emitters to measure
    the observed [O II]/H α ratio at z = 1.47. The observed [O II]/H α ratio increases
    significantly from 0.40 ± 0.01 at z = 0.1 to 0.52 ± 0.05 at z = 1.47, which we
    attribute to either decreasing dust attenuation with redshift, or due to a bias
    in the (typically) fibre measurements in the local Universe that only measure
    the central kpc regions. At the bright end, we find that both the H α and Ly α
    number densities at z ≈ 2.2 deviate significantly from a Schechter form, following
    a power law. We show that this is driven entirely by an increasing X-ray/active
    galactic nucleus fraction with line luminosity, which reaches ≈100 per cent at
    line luminosities L ≳ 3 × 1044 erg s−1.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Philip
  full_name: Best, Philip
  last_name: Best
- first_name: Ian
  full_name: Smail, Ian
  last_name: Smail
- first_name: Fuyan
  full_name: Bian, Fuyan
  last_name: Bian
- first_name: Behnam
  full_name: Darvish, Behnam
  last_name: Darvish
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
- first_name: Xiaohui
  full_name: Fan, Xiaohui
  last_name: Fan
citation:
  ama: 'Matthee JJ, Sobral D, Best P, et al. Boötes-HiZELS: An optical to near-infrared
    survey of emission-line galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal
    Astronomical Society</i>. 2017;471(1):629-649. doi:<a href="https://doi.org/10.1093/mnras/stx1569">10.1093/mnras/stx1569</a>'
  apa: 'Matthee, J. J., Sobral, D., Best, P., Smail, I., Bian, F., Darvish, B., …
    Fan, X. (2017). Boötes-HiZELS: An optical to near-infrared survey of emission-line
    galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx1569">https://doi.org/10.1093/mnras/stx1569</a>'
  chicago: 'Matthee, Jorryt J, David Sobral, Philip Best, Ian Smail, Fuyan Bian, Behnam
    Darvish, Huub Röttgering, and Xiaohui Fan. “Boötes-HiZELS: An Optical to near-Infrared
    Survey of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal
    Astronomical Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx1569">https://doi.org/10.1093/mnras/stx1569</a>.'
  ieee: 'J. J. Matthee <i>et al.</i>, “Boötes-HiZELS: An optical to near-infrared
    survey of emission-line galaxies at z = 0.4–4.7,” <i>Monthly Notices of the Royal
    Astronomical Society</i>, vol. 471, no. 1. Oxford University Press, pp. 629–649,
    2017.'
  ista: 'Matthee JJ, Sobral D, Best P, Smail I, Bian F, Darvish B, Röttgering H, Fan
    X. 2017. Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies
    at z = 0.4–4.7. Monthly Notices of the Royal Astronomical Society. 471(1), 629–649.'
  mla: 'Matthee, Jorryt J., et al. “Boötes-HiZELS: An Optical to near-Infrared Survey
    of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal Astronomical
    Society</i>, vol. 471, no. 1, Oxford University Press, 2017, pp. 629–49, doi:<a
    href="https://doi.org/10.1093/mnras/stx1569">10.1093/mnras/stx1569</a>.'
  short: J.J. Matthee, D. Sobral, P. Best, I. Smail, F. Bian, B. Darvish, H. Röttgering,
    X. Fan, Monthly Notices of the Royal Astronomical Society 471 (2017) 629–649.
date_created: 2022-07-12T11:01:35Z
date_published: 2017-10-01T00:00:00Z
date_updated: 2022-08-19T07:15:14Z
day: '01'
doi: 10.1093/mnras/stx1569
extern: '1'
external_id:
  arxiv:
  - '1702.04721'
intvolume: '       471'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics galaxies
- active
- galaxies
- evolution
- galaxies
- high-redshift
- galaxies
- luminosity function
- mass function
- 'galaxies: star formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1702.04721
month: '10'
oa: 1
oa_version: Preprint
page: 629-649
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies
  at z = 0.4–4.7'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...
---
_id: '11562'
abstract:
- lang: eng
  text: We present the CAlibrating LYMan-α with Hα (CALYMHA) pilot survey and new
    results on Lyman α (Lyα) selected galaxies at z ∼ 2. We use a custom-built Lyα
    narrow-band filter at the Isaac Newton Telescope, designed to provide a matched
    volume coverage to the z = 2.23 Hα HiZELS survey. Here, we present the first results
    for the COSMOS and UDS fields. Our survey currently reaches a 3σ line flux limit
    of ∼4 × 10−17 erg s−1 cm−2, and a Lyα luminosity limit of ∼1042.3 erg s−1. We
    find 188 Lyα emitters over 7.3 × 105 Mpc3, but also find significant numbers of
    other line-emitting sources corresponding to He II, C III] and C IV emission lines.
    These sources are important contaminants, and we carefully remove them, unlike
    most previous studies. We find that the Lyα luminosity function at z = 2.23 is
    very well described by a Schechter function up to LLy α ≈ 1043 erg s−1 with L∗=1042.59+0.16−0.08
    erg s−1, ϕ∗=10−3.09+0.14−0.34 Mpc−3 and α = −1.75 ± 0.25. Above LLy α ≈ 1043 erg
    s−1, the Lyα luminosity function becomes power-law like, driven by X-ray AGN.
    We find that Lyα-selected emitters have a high escape fraction of 37 ± 7 per cent,
    anticorrelated with Lyα luminosity and correlated with Lyα equivalent width. Lyα
    emitters have ubiquitous large (≈40 kpc) Lyα haloes, ∼2 times larger than their
    Hα extents. By directly comparing our Lyα and Hα luminosity functions, we find
    that the global/overall escape fraction of Lyα photons (within a 13 kpc radius)
    from the full population of star-forming galaxies is 5.1 ± 0.2 per cent at the
    peak of the star formation history. An extra 3.3 ± 0.3 per cent of Lyα photons
    likely still escape, but at larger radii.
acknowledgement: 'We thank the reviewer for his/her helpful comments and suggestions
  that have greatly improved this work. DS and JM acknowledge financial support from
  the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship.
  DS also acknowledges funding from FCT through an FCT Investigator Starting Grant
  and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from
  the UK STFC via grant ST/M001229/1. IRS acknowledges support from STFC (ST/L00075X/1),
  the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson
  merit award. We thank Matthew Hayes, Ryan Trainor, Kimihiko Nakajima and Anne Verhamme
  for many helpful discussions and Ana Sobral, Carolina Duarte and Miguel Domingos
  for taking part in observations with the NB392 filter. We also thank Sergio Santos
  for helpful comments. This research is based on observations obtained on the Isaac
  Newton Telescope (INT), programs: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B
  & I15AN008. The authors acknowledge the award of time from programmes: I13AN002,
  I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008 on the INT. INT is operated
  on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio
  del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on
  observations made with ESO Telescopes at the La Silla Paranal Observatory under
  programme ID 098.A 0819. We have benefited greatly from the publicly available programming
  language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages,
  the astronomical imaging tools SEXTRACTOR, SWARP (Bertin & Arnouts 1996; Bertin
  2010), SCAMP (Bertin 2006) and TOPCAT (Taylor 2005). Dedicated to the memory of
  M. L. Nicolau and M. C. Serrano.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: Philip
  full_name: Best, Philip
  last_name: Best
- first_name: Andra
  full_name: Stroe, Andra
  last_name: Stroe
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
- first_name: Iván
  full_name: Oteo, Iván
  last_name: Oteo
- first_name: Ian
  full_name: Smail, Ian
  last_name: Smail
- first_name: Leah
  full_name: Morabito, Leah
  last_name: Morabito
- first_name: Ana
  full_name: Paulino-Afonso, Ana
  last_name: Paulino-Afonso
citation:
  ama: 'Sobral D, Matthee JJ, Best P, et al. The CALYMHA survey: Lyα luminosity function
    and global escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the
    Royal Astronomical Society</i>. 2017;466(1):1242-1258. doi:<a href="https://doi.org/10.1093/mnras/stw3090">10.1093/mnras/stw3090</a>'
  apa: 'Sobral, D., Matthee, J. J., Best, P., Stroe, A., Röttgering, H., Oteo, I.,
    … Paulino-Afonso, A. (2017). The CALYMHA survey: Lyα luminosity function and global
    escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stw3090">https://doi.org/10.1093/mnras/stw3090</a>'
  chicago: 'Sobral, David, Jorryt J Matthee, Philip Best, Andra Stroe, Huub Röttgering,
    Iván Oteo, Ian Smail, Leah Morabito, and Ana Paulino-Afonso. “The CALYMHA Survey:
    Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.”
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press,
    2017. <a href="https://doi.org/10.1093/mnras/stw3090">https://doi.org/10.1093/mnras/stw3090</a>.'
  ieee: 'D. Sobral <i>et al.</i>, “The CALYMHA survey: Lyα luminosity function and
    global escape fraction of Lyα photons at z = 2.23,” <i>Monthly Notices of the
    Royal Astronomical Society</i>, vol. 466, no. 1. Oxford University Press, pp.
    1242–1258, 2017.'
  ista: 'Sobral D, Matthee JJ, Best P, Stroe A, Röttgering H, Oteo I, Smail I, Morabito
    L, Paulino-Afonso A. 2017. The CALYMHA survey: Lyα luminosity function and global
    escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical
    Society. 466(1), 1242–1258.'
  mla: 'Sobral, David, et al. “The CALYMHA Survey: Lyα Luminosity Function and Global
    Escape Fraction of Lyα Photons at z = 2.23.” <i>Monthly Notices of the Royal Astronomical
    Society</i>, vol. 466, no. 1, Oxford University Press, 2017, pp. 1242–58, doi:<a
    href="https://doi.org/10.1093/mnras/stw3090">10.1093/mnras/stw3090</a>.'
  short: D. Sobral, J.J. Matthee, P. Best, A. Stroe, H. Röttgering, I. Oteo, I. Smail,
    L. Morabito, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society
    466 (2017) 1242–1258.
date_created: 2022-07-12T12:04:16Z
date_published: 2017-04-01T00:00:00Z
date_updated: 2022-08-19T07:18:20Z
day: '01'
doi: 10.1093/mnras/stw3090
extern: '1'
external_id:
  arxiv:
  - '1609.05897'
intvolume: '       466'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: haloes'
- 'galaxies: high-redshift'
- 'galaxies: luminosity function'
- mass function
- 'galaxies: statistics'
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1609.05897
month: '04'
oa: 1
oa_version: Preprint
page: 1242-1258
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The CALYMHA survey: Lyα luminosity function and global escape fraction of
  Lyα photons at z = 2.23'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 466
year: '2017'
...
---
_id: '11564'
abstract:
- lang: eng
  text: We study the production rate of ionizing photons of a sample of 588 Hα emitters
    (HAEs) and 160 Lyman-α emitters (LAEs) at z = 2.2 in the COSMOS field in order
    to assess the implied emissivity from galaxies, based on their ultraviolet (UV)
    luminosity. By exploring the rest-frame Lyman Continuum (LyC) with GALEX/NUV data,
    we find fesc < 2.8 (6.4) per cent through median (mean) stacking. By combining
    the Hα luminosity density with intergalactic medium emissivity measurements from
    absorption studies, we find a globally averaged 〈fesc〉 of 5.9+14.5−4.2 per cent
    at z = 2.2 if we assume HAEs are the only source of ionizing photons. We find
    similarly low values of the global 〈fesc〉 at z ≈ 3–5, also ruling out a high 〈fesc〉
    at z < 5. These low escape fractions allow us to measure ξion, the number of produced
    ionizing photons per unit UV luminosity, and investigate how this depends on galaxy
    properties. We find a typical ξion ≈ 1024.77 ± 0.04 Hz erg−1 for HAEs and ξion
    ≈ 1025.14 ± 0.09 Hz erg−1 for LAEs. LAEs and low-mass HAEs at z = 2.2 show similar
    values of ξion as typically assumed in the reionization era, while the typical
    HAE is three times less ionizing. Due to an increasing ξion with increasing EW(Hα),
    ξion likely increases with redshift. This evolution alone is fully in line with
    the observed evolution of ξion between z ≈ 2 and 5, indicating a typical value
    of ξion ≈ 1025.4 Hz erg−1 in the reionization era.
acknowledgement: "We thank the referee for the many helpful and constructive comments
  which have significantly improved this paper. JM acknowledges the support of a Huygens
  PhD fellowship from Leiden University. DS acknowledges financial support from the
  Netherlands Organization for Scientific research (NWO) through a Veni fellowship
  and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010).
  PNB is grateful for support from the UK STFC via grant ST/M001229/1. IO acknowledges
  support from the European Research Council in the form of the Advanced Investigator
  Programme, 321302, COSMICISM. The authors thank Andreas Faisst, Michael Rutkowski
  and Andreas Sandberg for answering questions related to this work and Daniel Schaerer
  and Mark Dijkstra for discussions. We acknowledge the work that has been done by
  both the COSMOS team in assembling such large, state-of-the-art multi-wavelength
  data set, as this has been crucial for the results presented in this paper. We have
  benefited greatly from the public available programming language PYTHON, including
  the NUMPY, MATPLOTLIB, PYFITS, SCIPY (Jones et al. 2001; Hunter 2007; Van Der Walt,
  Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration et al. 2013) packages,
  the astronomical imaging tools SEXTRACTOR and SWARP (Bertin & Arnouts 1996;\r\nBertin
  2010) and the TOPCAT analysis program (Taylor 2013)."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Philip
  full_name: Best, Philip
  last_name: Best
- first_name: Ali Ahmad
  full_name: Khostovan, Ali Ahmad
  last_name: Khostovan
- first_name: Iván
  full_name: Oteo, Iván
  last_name: Oteo
- first_name: Rychard
  full_name: Bouwens, Rychard
  last_name: Bouwens
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
citation:
  ama: Matthee JJ, Sobral D, Best P, et al. The production and escape of Lyman-Continuum
    radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2017;465(3):3637-3655. doi:<a href="https://doi.org/10.1093/mnras/stw2973">10.1093/mnras/stw2973</a>
  apa: Matthee, J. J., Sobral, D., Best, P., Khostovan, A. A., Oteo, I., Bouwens,
    R., &#38; Röttgering, H. (2017). The production and escape of Lyman-Continuum
    radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stw2973">https://doi.org/10.1093/mnras/stw2973</a>
  chicago: Matthee, Jorryt J, David Sobral, Philip Best, Ali Ahmad Khostovan, Iván
    Oteo, Rychard Bouwens, and Huub Röttgering. “The Production and Escape of Lyman-Continuum
    Radiation from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017.
    <a href="https://doi.org/10.1093/mnras/stw2973">https://doi.org/10.1093/mnras/stw2973</a>.
  ieee: J. J. Matthee <i>et al.</i>, “The production and escape of Lyman-Continuum
    radiation from star-forming galaxies at z ∼ 2 and their redshift evolution,” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 465, no. 3. Oxford University
    Press, pp. 3637–3655, 2017.
  ista: Matthee JJ, Sobral D, Best P, Khostovan AA, Oteo I, Bouwens R, Röttgering
    H. 2017. The production and escape of Lyman-Continuum radiation from star-forming
    galaxies at z ∼ 2 and their redshift evolution. Monthly Notices of the Royal Astronomical
    Society. 465(3), 3637–3655.
  mla: Matthee, Jorryt J., et al. “The Production and Escape of Lyman-Continuum Radiation
    from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 465, no. 3, Oxford University
    Press, 2017, pp. 3637–55, doi:<a href="https://doi.org/10.1093/mnras/stw2973">10.1093/mnras/stw2973</a>.
  short: J.J. Matthee, D. Sobral, P. Best, A.A. Khostovan, I. Oteo, R. Bouwens, H.
    Röttgering, Monthly Notices of the Royal Astronomical Society 465 (2017) 3637–3655.
date_created: 2022-07-12T12:12:14Z
date_published: 2017-03-01T00:00:00Z
date_updated: 2022-08-19T07:53:04Z
day: '01'
doi: 10.1093/mnras/stw2973
extern: '1'
external_id:
  arxiv:
  - '1605.08782'
intvolume: '       465'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'cosmology: observations'
- dark ages
- reionization
- first stars
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1605.08782
month: '03'
oa: 1
oa_version: Preprint
page: 3637-3655
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The production and escape of Lyman-Continuum radiation from star-forming galaxies
  at z ∼ 2 and their redshift evolution
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 465
year: '2017'
...
---
_id: '11565'
abstract:
- lang: eng
  text: We use the hydrodynamical EAGLE simulation to study the magnitude and origin
    of the scatter in the stellar mass–halo mass relation for central galaxies. We
    separate cause and effect by correlating stellar masses in the baryonic simulation
    with halo properties in a matched dark matter only (DMO) simulation. The scatter
    in stellar mass increases with redshift and decreases with halo mass. At z = 0.1,
    it declines from 0.25 dex at M200, DMO ≈ 1011 M⊙ to 0.12 dex at M200, DMO ≈ 1013
    M⊙, but the trend is weak above 1012 M⊙. For M200, DMO < 1012.5 M⊙ up to 0.04
    dex of the scatter is due to scatter in the halo concentration. At fixed halo
    mass, a larger stellar mass corresponds to a more concentrated halo. This is likely
    because higher concentrations imply earlier formation times and hence more time
    for accretion and star formation, and/or because feedback is less efficient in
    haloes with higher binding energies. The maximum circular velocity, Vmax, DMO,
    and binding energy are therefore more fundamental properties than halo mass, meaning
    that they are more accurate predictors of stellar mass, and we provide fitting
    formulae for their relations with stellar mass. However, concentration alone cannot
    explain the total scatter in the Mstar−M200,DMO relation, and it does not explain
    the scatter in Mstar–Vmax, DMO. Halo spin, sphericity, triaxiality, substructure
    and environment are also not responsible for the remaining scatter, which thus
    could be due to more complex halo properties or non-linear/stochastic baryonic
    effects.
acknowledgement: We thank the anonymous referee for their comments. JM acknowledges
  the support of a Huygens PhD fellowship from Leiden University. JM thanks David
  Sobral for useful discussions and help with fitting routines and Jonas Chavez Montero
  and Ying Zu for providing data. We thank PRACE for the access to the Curie facility
  in France. We have used the DiRAC system which is a part of National E-Infrastructure
  at Durham University, operated by the Institute for Computational Cosmology on behalf
  of the STFC DiRAC HPC Facility (www.dirac.ac.uk); the equipment was funded by BIS
  National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1,
  STFC DiRAC Operations grant ST/K003267/1 and Durham University. The study was sponsored
  by the Dutch National Computing Facilities Foundation (NCF) for the use of supercomputer
  facilities, with financial support from the Netherlands Organisation for Scientific
  Research (NWO), through VICI grant 639.043.409, and the European Research Council
  under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC Grant
  agreement 278594- GasAroundGalaxies, and from the Belgian Science Policy Office
  ([AP P7/08 CHARM]). We have benefited greatly from the public available programming
  language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY, H5PY and RPY2 packages,
  and the TOPCAT analysis program (Taylor 2005).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: Joop
  full_name: Schaye, Joop
  last_name: Schaye
- first_name: Robert A.
  full_name: Crain, Robert A.
  last_name: Crain
- first_name: Matthieu
  full_name: Schaller, Matthieu
  last_name: Schaller
- first_name: Richard
  full_name: Bower, Richard
  last_name: Bower
- first_name: Tom
  full_name: Theuns, Tom
  last_name: Theuns
citation:
  ama: Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. The origin of
    scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE
    simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;465(2):2381-2396.
    doi:<a href="https://doi.org/10.1093/mnras/stw2884">10.1093/mnras/stw2884</a>
  apa: Matthee, J. J., Schaye, J., Crain, R. A., Schaller, M., Bower, R., &#38; Theuns,
    T. (2017). The origin of scatter in the stellar mass–halo mass relation of central
    galaxies in the EAGLE simulation. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stw2884">https://doi.org/10.1093/mnras/stw2884</a>
  chicago: Matthee, Jorryt J, Joop Schaye, Robert A. Crain, Matthieu Schaller, Richard
    Bower, and Tom Theuns. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation
    of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices of the Royal
    Astronomical Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stw2884">https://doi.org/10.1093/mnras/stw2884</a>.
  ieee: J. J. Matthee, J. Schaye, R. A. Crain, M. Schaller, R. Bower, and T. Theuns,
    “The origin of scatter in the stellar mass–halo mass relation of central galaxies
    in the EAGLE simulation,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 465, no. 2. Oxford University Press, pp. 2381–2396, 2017.
  ista: Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. 2017. The origin
    of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE
    simulation. Monthly Notices of the Royal Astronomical Society. 465(2), 2381–2396.
  mla: Matthee, Jorryt J., et al. “The Origin of Scatter in the Stellar Mass–Halo
    Mass Relation of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 465, no. 2, Oxford University Press,
    2017, pp. 2381–96, doi:<a href="https://doi.org/10.1093/mnras/stw2884">10.1093/mnras/stw2884</a>.
  short: J.J. Matthee, J. Schaye, R.A. Crain, M. Schaller, R. Bower, T. Theuns, Monthly
    Notices of the Royal Astronomical Society 465 (2017) 2381–2396.
date_created: 2022-07-12T12:25:08Z
date_published: 2017-02-01T00:00:00Z
date_updated: 2022-08-19T07:56:07Z
day: '01'
doi: 10.1093/mnras/stw2884
extern: '1'
external_id:
  arxiv:
  - '1608.08218'
intvolume: '       465'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: haloes'
- 'cosmology: theory'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1608.08218
month: '02'
oa: 1
oa_version: Preprint
page: 2381-2396
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The origin of scatter in the stellar mass–halo mass relation of central galaxies
  in the EAGLE simulation
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 465
year: '2017'
...
---
_id: '11566'
abstract:
- lang: eng
  text: While traditionally associated with active galactic nuclei (AGN), the properties
    of the C II] (λ = 2326 Å), C III] (λ, λ = 1907, 1909 Å) and C IV (λ, λ = 1549,
    1551 Å) emission lines are still uncertain as large, unbiased samples of sources
    are scarce. We present the first blind, statistical study of C II], C III] and
    C IV emitters at z ∼ 0.68, 1.05, 1.53, respectively, uniformly selected down to
    a flux limit of ∼4 × 10−17 erg s−1 cm−1 through a narrow-band survey covering
    an area of ∼1.4 deg2 over COSMOS and UDS. We detect 16 C II], 35 C III] and 17
    C IV emitters, whose nature we investigate using optical colours as well as Hubble
    Space Telescope (HST), X-ray, radio and far-infrared data. We find that z ∼ 0.7
    C II] emitters are consistent with a mixture of blue (UV slope β = −2.0 ± 0.4)
    star-forming (SF) galaxies with discy HST structure and AGN with Seyfert-like
    morphologies. Bright C II] emitters have individual X-ray detections as well as
    high average black hole accretion rates (BHARs) of ∼0.1 M⊙ yr−1. C III] emitters
    at z ∼ 1.05 trace a general population of SF galaxies, with β = −0.8 ± 1.1, a
    variety of optical morphologies, including isolated and interacting galaxies and
    low BHAR (<0.02 M⊙ yr−1). Our C IV emitters at z ∼ 1.5 are consistent with young,
    blue quasars (β ∼ −1.9) with point-like optical morphologies, bright X-ray counterparts
    and large BHAR (0.8  M⊙ yr−1). We also find some surprising C II], C III] and
    C IV emitters with rest-frame equivalent widths (EWs) that could be as large as
    50–100 Å. AGN or spatial offsets between the UV continuum stellar disc and the
    line-emitting regions may explain the large EW. These bright C II], C III] and
    C IV emitters are ideal candidates for spectroscopic follow-up to fully unveil
    their nature.
acknowledgement: 'We would like to thank the anonymous referee for her/his valuable
  input that helped improve the clarity and interpretation of our results. DS acknowledges
  financial support from the Netherlands Organisation for Scientific research (NWO),
  through a Veni fellowship. IO acknowledges support from the European Research Council
  in the form of the Advanced Investigator Programme, 321302, COSMICISM. CALYMHA data
  are based on observations made with the Isaac Newton Telescope (proposals 13AN002,
  I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008) operated on the island
  of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los
  Muchachos of the Instituto de Astrofísica de Canarias. Also based on data products
  from observations made with ESO Telescopes at the La Silla Paranal Observatory under
  ESO programme IDs 098.A-0819 and 179.A-2005. We are grateful to E. L. Wright and
  J. Schombert for their cosmology calculator. We would like to thank the authors
  of NUMPY (van der Walt et al. 2011), SCIPY (Jones et al. 2001), MATPLOTLIB (Hunter
  2007) and ASTROPY (Astropy Collaboration et al. 2013) for making these packages
  publicly available. This research has made use of the NASA/IPAC Extragalactic Database
  (NED), which is '
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Andra
  full_name: Stroe, Andra
  last_name: Stroe
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: João
  full_name: Calhau, João
  last_name: Calhau
- first_name: Ivan
  full_name: Oteo, Ivan
  last_name: Oteo
citation:
  ama: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for
    C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent
    widths . <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(3):2558-2574.
    doi:<a href="https://doi.org/10.1093/mnras/stx1712">10.1093/mnras/stx1712</a>
  apa: Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., &#38; Oteo, I. (2017). A
    1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies
    and equivalent widths . <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx1712">https://doi.org/10.1093/mnras/stx1712</a>
  chicago: Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo.
    “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature,
    Morphologies and Equivalent Widths .” <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx1712">https://doi.org/10.1093/mnras/stx1712</a>.
  ieee: A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind
    survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and
    equivalent widths ,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 471, no. 3. Oxford University Press, pp. 2558–2574, 2017.
  ista: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey
    for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent
    widths . Monthly Notices of the Royal Astronomical Society. 471(3), 2558–2574.
  mla: Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at
    z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 471, no. 3, Oxford University Press,
    2017, pp. 2558–74, doi:<a href="https://doi.org/10.1093/mnras/stx1712">10.1093/mnras/stx1712</a>.
  short: A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of
    the Royal Astronomical Society 471 (2017) 2558–2574.
date_created: 2022-07-12T12:33:16Z
date_published: 2017-11-01T00:00:00Z
date_updated: 2022-08-19T07:59:57Z
day: '01'
doi: 10.1093/mnras/stx1712
extern: '1'
external_id:
  arxiv:
  - '1703.10169'
intvolume: '       471'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: active'
- 'galaxies: high-redshift'
- 'quasars: emission lines'
- 'galaxies: star formation'
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1703.10169
month: '11'
oa: 1
oa_version: Preprint
page: 2558-2574
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature,
  morphologies and equivalent widths '
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...
---
_id: '11567'
abstract:
- lang: eng
  text: Recently, the C III] and C IV emission lines have been observed in galaxies
    in the early Universe (z > 5), providing new ways to measure their redshift and
    study their stellar populations and active galactic nuclei (AGN). We explore the
    first blind C II], C III] and C IV survey (z ∼ 0.68, 1.05, 1.53, respectively)
    presented in Stroe et al. (2017). We derive luminosity functions (LF) and study
    properties of C II], C III] and C IV line emitters through comparisons to the
    LFs of H α and Ly α emitters, UV selected star-forming (SF) galaxies and quasars
    at similar redshifts. The C II] LF at z ∼ 0.68 is equally well described by a
    Schechter or a power-law LF, characteristic of a mixture of SF and AGN activity.
    The C III] LF (z ∼ 1.05) is consistent to a scaled down version of the Schechter
    H α and Ly α LF at their redshift, indicating a SF origin. In stark contrast,
    the C IV LF at z ∼ 1.53 is well fit by a power-law, quasar-like LF. We find that
    the brightest UV sources (MUV < −22) will universally have C III] and C IV emission.
    However, on average, C III] and C IV are not as abundant as H α or Ly α emitters
    at the same redshift, with cosmic average ratios of ∼0.02–0.06 to H α and ∼0.01–0.1
    to intrinsic Ly α. We predict that the C III] and C IV lines can only be truly
    competitive in confirming high-redshift candidates when the hosts are intrinsically
    bright and the effective Ly α escape fraction is below 1 per cent. While C III]
    and C IV were proposed as good tracers of young, relatively low-metallicity galaxies
    typical of the early Universe, we find that, at least at z ∼ 1.5, C IV is exclusively
    hosted by AGN/quasars, especially at large line equivalent widths.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Andra
  full_name: Stroe, Andra
  last_name: Stroe
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: João
  full_name: Calhau, João
  last_name: Calhau
- first_name: Ivan
  full_name: Oteo, Ivan
  last_name: Oteo
citation:
  ama: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for
    C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average
    line ratios. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(3):2575-2586.
    doi:<a href="https://doi.org/10.1093/mnras/stx1713">10.1093/mnras/stx1713</a>
  apa: Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., &#38; Oteo, I. (2017). A
    1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity
    functions and cosmic average line ratios. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx1713">https://doi.org/10.1093/mnras/stx1713</a>
  chicago: Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo.
    “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity
    Functions and Cosmic Average Line Ratios.” <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx1713">https://doi.org/10.1093/mnras/stx1713</a>.
  ieee: A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind
    survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and
    cosmic average line ratios,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 471, no. 3. Oxford University Press, pp. 2575–2586, 2017.
  ista: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey
    for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic
    average line ratios. Monthly Notices of the Royal Astronomical Society. 471(3),
    2575–2586.
  mla: Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at
    z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 471, no. 3, Oxford University
    Press, 2017, pp. 2575–86, doi:<a href="https://doi.org/10.1093/mnras/stx1713">10.1093/mnras/stx1713</a>.
  short: A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of
    the Royal Astronomical Society 471 (2017) 2575–2586.
date_created: 2022-07-12T12:54:57Z
date_published: 2017-11-01T00:00:00Z
date_updated: 2022-08-19T08:02:04Z
day: '01'
doi: 10.1093/mnras/stx1713
extern: '1'
external_id:
  arxiv:
  - '1703.10169'
intvolume: '       471'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: active'
- 'galaxies: high redshift'
- 'galaxies: luminosity function'
- mass function
- 'quasars: emission lines'
- star formation
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1703.10169
month: '11'
oa: 1
oa_version: Preprint
page: 2575-2586
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity
  functions and cosmic average line ratios
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...
---
_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: '11573'
abstract:
- lang: eng
  text: We present dynamical measurements from the KMOS (K-band multi-object spectrograph)
    Deep Survey (KDS), which comprises 77 typical star-forming galaxies at z ≃ 3.5
    in the mass range 9.0 < log (M⋆/M⊙) < 10.5. These measurements constrain the internal
    dynamics, the intrinsic velocity dispersions (σint) and rotation velocities (VC)
    of galaxies in the high-redshift Universe. The mean velocity dispersion of the
    galaxies in our sample is σint=70.8+3.3−3.1kms−1⁠, revealing that the increasing
    average σint with increasing redshift, reported for z ≲ 2, continues out to z
    ≃ 3.5. Only 36 ± 8 per cent of our galaxies are rotation-dominated (VC/σint >
    1), with the sample average VC/σint value much smaller than at lower redshift.
    After carefully selecting comparable star-forming samples at multiple epochs,
    we find that the rotation-dominated fraction evolves with redshift with a z−0.2
    dependence. The rotation-dominated KDS galaxies show no clear offset from the
    local rotation velocity–stellar mass (i.e. VC–M⋆) relation, although a smaller
    fraction of the galaxies are on the relation due to the increase in the dispersion-dominated
    fraction. These observations are consistent with a simple equilibrium model picture,
    in which random motions are boosted in high-redshift galaxies by a combination
    of the increasing gas fractions, accretion efficiency, specific star formation
    rate and stellar feedback and which may provide significant pressure support against
    gravity on the galactic disc scale.
acknowledgement: 'We wish to thank the anonymous referee for their comments, which
  have improved the quality and clarity of this work. OJT acknowledges the financial
  support of the Science and Technology Facilities Council through a studentship award.
  MC and OJT acknowledge the KMOS team and all the personnel of the European Southern
  Observatory Very Large Telescope for outstanding support during the KMOS GTO observations.
  CMH, AMS and RMS acknowledge the Science and Technology Facilities Council through
  grant code ST/L00075X/1. RJM acknowledges the support of the European Research Council
  via the award of a Consolidator Grant (PI: McLure). JSD acknowledges the support
  of the European Research Council via the award of an Advanced Grant (PI J. Dunlop),
  and the contribution of the EC FP7 SPACE project ASTRODEEP (Ref.No: 312725). AMS
  acknowledges the Leverhulme Foundation. 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).
  This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program
  with the NASA/ESA HST, which is operated by the Association of Universities for
  Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is based
  on observations taken by the 3D HST Treasury Program (GO 12177 and 12328) with the
  NASA/ESA HST, which is operated by the Association of Universities for Research
  in Astronomy, Inc., under NASA contract NAS5-26555. Based on data obtained with
  the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large
  Program 185.A-0791, and made available by the VUDS team at the CESAM data centre,
  Laboratoire d’Astrophysique de Marseille, France. Based on observations obtained
  at the Very Large Telescope of the European Southern Observatory. Programme IDs:
  092.A 0399(A), 093.A-0122(A,B), 094.A-0214(A,B),095.A0680(A,B),096.A-0315(A,B,C).'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: O. J.
  full_name: Turner, O. J.
  last_name: Turner
- first_name: M.
  full_name: Cirasuolo, M.
  last_name: Cirasuolo
- first_name: C. M.
  full_name: Harrison, C. M.
  last_name: Harrison
- first_name: R. J.
  full_name: McLure, R. J.
  last_name: McLure
- first_name: J. S.
  full_name: Dunlop, J. S.
  last_name: Dunlop
- first_name: A. M.
  full_name: Swinbank, A. M.
  last_name: Swinbank
- first_name: H. L.
  full_name: Johnson, H. L.
  last_name: Johnson
- 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: R. M.
  full_name: Sharples, R. M.
  last_name: Sharples
citation:
  ama: Turner OJ, Cirasuolo M, Harrison CM, et al. The KMOS Deep Survey (KDS) – I.
    Dynamical measurements of typical star-forming galaxies at z ≃ 3.5. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2017;471(2):1280-1320. doi:<a href="https://doi.org/10.1093/mnras/stx1366">10.1093/mnras/stx1366</a>
  apa: Turner, O. J., Cirasuolo, M., Harrison, C. M., McLure, R. J., Dunlop, J. S.,
    Swinbank, A. M., … Sharples, R. M. (2017). The KMOS Deep Survey (KDS) – I. Dynamical
    measurements of typical star-forming galaxies at z ≃ 3.5. <i>Monthly Notices of
    the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx1366">https://doi.org/10.1093/mnras/stx1366</a>
  chicago: Turner, O. J., M. Cirasuolo, C. M. Harrison, R. J. McLure, J. S. Dunlop,
    A. M. Swinbank, H. L. Johnson, D. Sobral, Jorryt J Matthee, and R. M. Sharples.
    “The KMOS Deep Survey (KDS) – I. Dynamical Measurements of Typical Star-Forming
    Galaxies at z ≃ 3.5.” <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx1366">https://doi.org/10.1093/mnras/stx1366</a>.
  ieee: O. J. Turner <i>et al.</i>, “The KMOS Deep Survey (KDS) – I. Dynamical measurements
    of typical star-forming galaxies at z ≃ 3.5,” <i>Monthly Notices of the Royal
    Astronomical Society</i>, vol. 471, no. 2. Oxford University Press, pp. 1280–1320,
    2017.
  ista: Turner OJ, Cirasuolo M, Harrison CM, McLure RJ, Dunlop JS, Swinbank AM, Johnson
    HL, Sobral D, Matthee JJ, Sharples RM. 2017. The KMOS Deep Survey (KDS) – I. Dynamical
    measurements of typical star-forming galaxies at z ≃ 3.5. Monthly Notices of the
    Royal Astronomical Society. 471(2), 1280–1320.
  mla: Turner, O. J., et al. “The KMOS Deep Survey (KDS) – I. Dynamical Measurements
    of Typical Star-Forming Galaxies at z ≃ 3.5.” <i>Monthly Notices of the Royal
    Astronomical Society</i>, vol. 471, no. 2, Oxford University Press, 2017, pp.
    1280–320, doi:<a href="https://doi.org/10.1093/mnras/stx1366">10.1093/mnras/stx1366</a>.
  short: O.J. Turner, M. Cirasuolo, C.M. Harrison, R.J. McLure, J.S. Dunlop, A.M.
    Swinbank, H.L. Johnson, D. Sobral, J.J. Matthee, R.M. Sharples, Monthly Notices
    of the Royal Astronomical Society 471 (2017) 1280–1320.
date_created: 2022-07-13T10:03:01Z
date_published: 2017-10-01T00:00:00Z
date_updated: 2022-08-19T08:07:31Z
day: '01'
doi: 10.1093/mnras/stx1366
extern: '1'
external_id:
  arxiv:
  - '1704.06263'
intvolume: '       471'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: kinematics and dynamics'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1704.06263
month: '10'
oa: 1
oa_version: Preprint
page: 1280-1320
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 KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming
  galaxies at z ≃ 3.5
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...
---
_id: '13476'
abstract:
- lang: eng
  text: Understanding ionizing fluxes of stellar populations is crucial for various
    astrophysical problems including the epoch of reionization. Short-lived massive
    stars are generally considered as the main stellar sources. We examine the potential
    role of less massive stars that lose their envelope through interaction with a
    binary companion. Here, we focus on the role of metallicity (Z). For this purpose
    we used the evolutionary code MESA and created tailored atmosphere models with
    the radiative transfer code CMFGEN. We show that typical progenitors, with initial
    masses of 12 M⊙, produce hot and compact stars (~ 4 M⊙, 60–80 kK, ~1 R⊙). These
    stripped stars copiously produce ionizing photons, emitting 60–85% and 30–60%
    of their energy as HI and HeI ionizing radiation, for Z = 0.0001–0.02, respectively.
    Their output is comparable to what massive stars emit during their Wolf-Rayet
    phase, if we account for their longer lifetimes and the favorable slope of the
    initial mass function. Their relative importance for reionization may be further
    favored since they emit their photons with a time delay (~ 20 Myr after birth
    in our fiducial model). This allows time for the dispersal of the birth clouds,
    allowing the ionizing photons to escape into the intergalactic medium. At low
    Z, we find that Roche stripping fails to fully remove the H-rich envelope, because
    of the reduced opacity in the subsurface layers. This is in sharp contrast with
    the assumption of complete stripping that is made in rapid population synthesis
    simulations, which are widely used to simulate the binary progenitors of supernovae
    and gravitational waves. Finally, we discuss the urgency to increase the observed
    sample of stripped stars to test these models and we discuss how our predictions
    can help to design efficient observational campaigns.
article_number: A11
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Ylva Louise Linsdotter
  full_name: Götberg, Ylva Louise Linsdotter
  id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
  last_name: Götberg
  orcid: 0000-0002-6960-6911
- first_name: S. E.
  full_name: de Mink, S. E.
  last_name: de Mink
- first_name: J. H.
  full_name: Groh, J. H.
  last_name: Groh
citation:
  ama: 'Götberg YLL, de Mink SE, Groh JH. Ionizing spectra of stars that lose their
    envelope through interaction with a binary companion: Role of metallicity. <i>Astronomy
    &#38; Astrophysics</i>. 2017;608. doi:<a href="https://doi.org/10.1051/0004-6361/201730472">10.1051/0004-6361/201730472</a>'
  apa: 'Götberg, Y. L. L., de Mink, S. E., &#38; Groh, J. H. (2017). Ionizing spectra
    of stars that lose their envelope through interaction with a binary companion:
    Role of metallicity. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/201730472">https://doi.org/10.1051/0004-6361/201730472</a>'
  chicago: 'Götberg, Ylva Louise Linsdotter, S. E. de Mink, and J. H. Groh. “Ionizing
    Spectra of Stars That Lose Their Envelope through Interaction with a Binary Companion:
    Role of Metallicity.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2017.
    <a href="https://doi.org/10.1051/0004-6361/201730472">https://doi.org/10.1051/0004-6361/201730472</a>.'
  ieee: 'Y. L. L. Götberg, S. E. de Mink, and J. H. Groh, “Ionizing spectra of stars
    that lose their envelope through interaction with a binary companion: Role of
    metallicity,” <i>Astronomy &#38; Astrophysics</i>, vol. 608. EDP Sciences, 2017.'
  ista: 'Götberg YLL, de Mink SE, Groh JH. 2017. Ionizing spectra of stars that lose
    their envelope through interaction with a binary companion: Role of metallicity.
    Astronomy &#38; Astrophysics. 608, A11.'
  mla: 'Götberg, Ylva Louise Linsdotter, et al. “Ionizing Spectra of Stars That Lose
    Their Envelope through Interaction with a Binary Companion: Role of Metallicity.”
    <i>Astronomy &#38; Astrophysics</i>, vol. 608, A11, EDP Sciences, 2017, doi:<a
    href="https://doi.org/10.1051/0004-6361/201730472">10.1051/0004-6361/201730472</a>.'
  short: Y.L.L. Götberg, S.E. de Mink, J.H. Groh, Astronomy &#38; Astrophysics 608
    (2017).
date_created: 2023-08-03T10:15:09Z
date_published: 2017-12-01T00:00:00Z
date_updated: 2023-08-09T11:27:06Z
day: '01'
doi: 10.1051/0004-6361/201730472
extern: '1'
external_id:
  arxiv:
  - '1701.07439'
intvolume: '       608'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1051/0004-6361/201730472
month: '12'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Ionizing spectra of stars that lose their envelope through interaction with
  a binary companion: Role of metallicity'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 608
year: '2017'
...
---
_id: '13477'
abstract:
- lang: eng
  text: Most massive stars, the progenitors of core-collapse supernovae, are in close
    binary systems and may interact with their companion through mass transfer or
    merging. We undertake a population synthesis study to compute the delay-time distribution
    of core-collapse supernovae, that is, the supernova rate versus time following
    a starburst, taking into account binary interactions. We test the systematic robustness
    of our results by running various simulations to account for the uncertainties
    in our standard assumptions. We find that a significant fraction, 15+9-8%, of
    core-collapse supernovae are “late”, that is, they occur 50–200 Myr after birth,
    when all massive single stars have already exploded. These late events originate
    predominantly from binary systems with at least one, or, in most cases, with both
    stars initially being of intermediate mass (4–8 M⊙). The main evolutionary channels
    that contribute often involve either the merging of the initially more massive
    primary star with its companion or the engulfment of the remaining core of the
    primary by the expanding secondary that has accreted mass at an earlier evolutionary
    stage. Also, the total number of core-collapse supernovae increases by 14+15-14%
    because of binarity for the same initial stellar mass. The high rate implies that
    we should have already observed such late core-collapse supernovae, but have not
    recognized them as such. We argue that φ Persei is a likely progenitor and that
    eccentric neutron star – white dwarf systems are likely descendants. Late events
    can help explain the discrepancy in the delay-time distributions derived from
    supernova remnants in the Magellanic Clouds and extragalactic type Ia events,
    lowering the contribution of prompt Ia events. We discuss ways to test these predictions
    and speculate on the implications for supernova feedback in simulations of galaxy
    evolution.
article_number: A29
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: E.
  full_name: Zapartas, E.
  last_name: Zapartas
- first_name: S. E.
  full_name: de Mink, S. E.
  last_name: de Mink
- first_name: R. G.
  full_name: Izzard, R. G.
  last_name: Izzard
- first_name: S.-C.
  full_name: Yoon, S.-C.
  last_name: Yoon
- first_name: C.
  full_name: Badenes, C.
  last_name: Badenes
- first_name: Ylva Louise Linsdotter
  full_name: Götberg, Ylva Louise Linsdotter
  id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
  last_name: Götberg
  orcid: 0000-0002-6960-6911
- first_name: A.
  full_name: de Koter, A.
  last_name: de Koter
- first_name: C. J.
  full_name: Neijssel, C. J.
  last_name: Neijssel
- first_name: M.
  full_name: Renzo, M.
  last_name: Renzo
- first_name: A.
  full_name: Schootemeijer, A.
  last_name: Schootemeijer
- first_name: T. S.
  full_name: Shrotriya, T. S.
  last_name: Shrotriya
citation:
  ama: Zapartas E, de Mink SE, Izzard RG, et al. Delay-time distribution of core-collapse
    supernovae with late events resulting from binary interaction. <i>Astronomy &#38;
    Astrophysics</i>. 2017;601(A&#38;A). doi:<a href="https://doi.org/10.1051/0004-6361/201629685">10.1051/0004-6361/201629685</a>
  apa: Zapartas, E., de Mink, S. E., Izzard, R. G., Yoon, S.-C., Badenes, C., Götberg,
    Y. L. L., … Shrotriya, T. S. (2017). Delay-time distribution of core-collapse
    supernovae with late events resulting from binary interaction. <i>Astronomy &#38;
    Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/201629685">https://doi.org/10.1051/0004-6361/201629685</a>
  chicago: Zapartas, E., S. E. de Mink, R. G. Izzard, S.-C. Yoon, C. Badenes, Ylva
    Louise Linsdotter Götberg, A. de Koter, et al. “Delay-Time Distribution of Core-Collapse
    Supernovae with Late Events Resulting from Binary Interaction.” <i>Astronomy &#38;
    Astrophysics</i>. EDP Sciences, 2017. <a href="https://doi.org/10.1051/0004-6361/201629685">https://doi.org/10.1051/0004-6361/201629685</a>.
  ieee: E. Zapartas <i>et al.</i>, “Delay-time distribution of core-collapse supernovae
    with late events resulting from binary interaction,” <i>Astronomy &#38; Astrophysics</i>,
    vol. 601, no. A&#38;A. EDP Sciences, 2017.
  ista: Zapartas E, de Mink SE, Izzard RG, Yoon S-C, Badenes C, Götberg YLL, de Koter
    A, Neijssel CJ, Renzo M, Schootemeijer A, Shrotriya TS. 2017. Delay-time distribution
    of core-collapse supernovae with late events resulting from binary interaction.
    Astronomy &#38; Astrophysics. 601(A&#38;A), A29.
  mla: Zapartas, E., et al. “Delay-Time Distribution of Core-Collapse Supernovae with
    Late Events Resulting from Binary Interaction.” <i>Astronomy &#38; Astrophysics</i>,
    vol. 601, no. A&#38;A, A29, EDP Sciences, 2017, doi:<a href="https://doi.org/10.1051/0004-6361/201629685">10.1051/0004-6361/201629685</a>.
  short: E. Zapartas, S.E. de Mink, R.G. Izzard, S.-C. Yoon, C. Badenes, Y.L.L. Götberg,
    A. de Koter, C.J. Neijssel, M. Renzo, A. Schootemeijer, T.S. Shrotriya, Astronomy
    &#38; Astrophysics 601 (2017).
date_created: 2023-08-03T10:15:18Z
date_published: 2017-05-01T00:00:00Z
date_updated: 2023-08-09T11:15:49Z
day: '01'
doi: 10.1051/0004-6361/201629685
extern: '1'
external_id:
  arxiv:
  - '1701.07032'
intvolume: '       601'
issue: A&A
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1051/0004-6361/201629685
month: '05'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Delay-time distribution of core-collapse supernovae with late events resulting
  from binary interaction
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 601
year: '2017'
...
---
_id: '14004'
abstract:
- lang: eng
  text: High-harmonic spectroscopy driven by circularly polarized laser pulses and
    their counterrotating second harmonic is a new branch of attosecond science which
    currently lacks quantitative interpretations. We extend this technique to the
    midinfrared regime and record detailed high-harmonic spectra of several rare-gas
    atoms. These results are compared with the solution of the Schrödinger equation
    in three dimensions and calculations based on the strong-field approximation that
    incorporate accurate scattering-wave recombination matrix elements. A quantum-orbit
    analysis of these results provides a transparent interpretation of the measured
    intensity ratios of symmetry-allowed neighboring harmonics in terms of (i) a set
    of propensity rules related to the angular momentum of the atomic orbitals, (ii)
    atom-specific matrix elements related to their electronic structure, and (iii)
    the interference of the emissions associated with electrons in orbitals corotating
    or counterrotating with the laser fields. These results provide the foundation
    for a quantitative understanding of bicircular high-harmonic spectroscopy.
article_number: '203201'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Denitsa Rangelova
  full_name: Baykusheva, Denitsa Rangelova
  id: 71b4d059-2a03-11ee-914d-dfa3beed6530
  last_name: Baykusheva
- first_name: Simon
  full_name: Brennecke, Simon
  last_name: Brennecke
- first_name: Manfred
  full_name: Lein, Manfred
  last_name: Lein
- first_name: Hans Jakob
  full_name: Wörner, Hans Jakob
  last_name: Wörner
citation:
  ama: Baykusheva DR, Brennecke S, Lein M, Wörner HJ. Signatures of electronic structure
    in bicircular high-harmonic spectroscopy. <i>Physical Review Letters</i>. 2017;119(20).
    doi:<a href="https://doi.org/10.1103/physrevlett.119.203201">10.1103/physrevlett.119.203201</a>
  apa: Baykusheva, D. R., Brennecke, S., Lein, M., &#38; Wörner, H. J. (2017). Signatures
    of electronic structure in bicircular high-harmonic spectroscopy. <i>Physical
    Review Letters</i>. American Physical Society. <a href="https://doi.org/10.1103/physrevlett.119.203201">https://doi.org/10.1103/physrevlett.119.203201</a>
  chicago: Baykusheva, Denitsa Rangelova, Simon Brennecke, Manfred Lein, and Hans
    Jakob Wörner. “Signatures of Electronic Structure in Bicircular High-Harmonic
    Spectroscopy.” <i>Physical Review Letters</i>. American Physical Society, 2017.
    <a href="https://doi.org/10.1103/physrevlett.119.203201">https://doi.org/10.1103/physrevlett.119.203201</a>.
  ieee: D. R. Baykusheva, S. Brennecke, M. Lein, and H. J. Wörner, “Signatures of
    electronic structure in bicircular high-harmonic spectroscopy,” <i>Physical Review
    Letters</i>, vol. 119, no. 20. American Physical Society, 2017.
  ista: Baykusheva DR, Brennecke S, Lein M, Wörner HJ. 2017. Signatures of electronic
    structure in bicircular high-harmonic spectroscopy. Physical Review Letters. 119(20),
    203201.
  mla: Baykusheva, Denitsa Rangelova, et al. “Signatures of Electronic Structure in
    Bicircular High-Harmonic Spectroscopy.” <i>Physical Review Letters</i>, vol. 119,
    no. 20, 203201, American Physical Society, 2017, doi:<a href="https://doi.org/10.1103/physrevlett.119.203201">10.1103/physrevlett.119.203201</a>.
  short: D.R. Baykusheva, S. Brennecke, M. Lein, H.J. Wörner, Physical Review Letters
    119 (2017).
date_created: 2023-08-10T06:35:51Z
date_published: 2017-11-17T00:00:00Z
date_updated: 2023-08-22T08:21:10Z
day: '17'
doi: 10.1103/physrevlett.119.203201
extern: '1'
external_id:
  arxiv:
  - '1710.04474'
intvolume: '       119'
issue: '20'
keyword:
- General Physics and Astronomy
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1710.04474
month: '11'
oa: 1
oa_version: Preprint
publication: Physical Review Letters
publication_identifier:
  eissn:
  - 1079-7114
  issn:
  - 0031-9007
publication_status: published
publisher: American Physical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Signatures of electronic structure in bicircular high-harmonic spectroscopy
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 119
year: '2017'
...
---
_id: '14005'
abstract:
- lang: eng
  text: Strong-field photoelectron holography and laser-induced electron diffraction
    (LIED) are two powerful emerging methods for probing the ultrafast dynamics of
    molecules. However, both of them have remained restricted to static systems and
    to nuclear dynamics induced by strong-field ionization. Here we extend these promising
    methods to image purely electronic valence-shell dynamics in molecules using photoelectron
    holography. In the same experiment, we use LIED and photoelectron holography simultaneously,
    to observe coupled electronic-rotational dynamics taking place on similar timescales.
    These results offer perspectives for imaging ultrafast dynamics of molecules on
    femtosecond to attosecond timescales.
article_number: '15651'
article_processing_charge: No
article_type: original
author:
- first_name: Samuel G.
  full_name: Walt, Samuel G.
  last_name: Walt
- first_name: Niraghatam
  full_name: Bhargava Ram, Niraghatam
  last_name: Bhargava Ram
- first_name: Marcos
  full_name: Atala, Marcos
  last_name: Atala
- first_name: Nikolay I
  full_name: Shvetsov-Shilovski, Nikolay I
  last_name: Shvetsov-Shilovski
- first_name: Aaron
  full_name: von Conta, Aaron
  last_name: von Conta
- first_name: Denitsa Rangelova
  full_name: Baykusheva, Denitsa Rangelova
  id: 71b4d059-2a03-11ee-914d-dfa3beed6530
  last_name: Baykusheva
- first_name: Manfred
  full_name: Lein, Manfred
  last_name: Lein
- first_name: Hans Jakob
  full_name: Wörner, Hans Jakob
  last_name: Wörner
citation:
  ama: Walt SG, Bhargava Ram N, Atala M, et al. Dynamics of valence-shell electrons
    and nuclei probed by strong-field holography and rescattering. <i>Nature Communications</i>.
    2017;8. doi:<a href="https://doi.org/10.1038/ncomms15651">10.1038/ncomms15651</a>
  apa: Walt, S. G., Bhargava Ram, N., Atala, M., Shvetsov-Shilovski, N. I., von Conta,
    A., Baykusheva, D. R., … Wörner, H. J. (2017). Dynamics of valence-shell electrons
    and nuclei probed by strong-field holography and rescattering. <i>Nature Communications</i>.
    Springer Nature. <a href="https://doi.org/10.1038/ncomms15651">https://doi.org/10.1038/ncomms15651</a>
  chicago: Walt, Samuel G., Niraghatam Bhargava Ram, Marcos Atala, Nikolay I Shvetsov-Shilovski,
    Aaron von Conta, Denitsa Rangelova Baykusheva, Manfred Lein, and Hans Jakob Wörner.
    “Dynamics of Valence-Shell Electrons and Nuclei Probed by Strong-Field Holography
    and Rescattering.” <i>Nature Communications</i>. Springer Nature, 2017. <a href="https://doi.org/10.1038/ncomms15651">https://doi.org/10.1038/ncomms15651</a>.
  ieee: S. G. Walt <i>et al.</i>, “Dynamics of valence-shell electrons and nuclei
    probed by strong-field holography and rescattering,” <i>Nature Communications</i>,
    vol. 8. Springer Nature, 2017.
  ista: Walt SG, Bhargava Ram N, Atala M, Shvetsov-Shilovski NI, von Conta A, Baykusheva
    DR, Lein M, Wörner HJ. 2017. Dynamics of valence-shell electrons and nuclei probed
    by strong-field holography and rescattering. Nature Communications. 8, 15651.
  mla: Walt, Samuel G., et al. “Dynamics of Valence-Shell Electrons and Nuclei Probed
    by Strong-Field Holography and Rescattering.” <i>Nature Communications</i>, vol.
    8, 15651, Springer Nature, 2017, doi:<a href="https://doi.org/10.1038/ncomms15651">10.1038/ncomms15651</a>.
  short: S.G. Walt, N. Bhargava Ram, M. Atala, N.I. Shvetsov-Shilovski, A. von Conta,
    D.R. Baykusheva, M. Lein, H.J. Wörner, Nature Communications 8 (2017).
date_created: 2023-08-10T06:36:09Z
date_published: 2017-06-15T00:00:00Z
date_updated: 2023-08-22T08:26:06Z
day: '15'
doi: 10.1038/ncomms15651
extern: '1'
external_id:
  pmid:
  - '28643771'
intvolume: '         8'
keyword:
- General Physics and Astronomy
- General Biochemistry
- Genetics and Molecular Biology
- General Chemistry
- Multidisciplinary
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1038/ncomms15651
month: '06'
oa: 1
oa_version: Published Version
pmid: 1
publication: Nature Communications
publication_identifier:
  eissn:
  - 2041-1723
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
scopus_import: '1'
status: public
title: Dynamics of valence-shell electrons and nuclei probed by strong-field holography
  and rescattering
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 8
year: '2017'
...
---
_id: '14006'
abstract:
- lang: eng
  text: We present a theoretical formalism for the calculation of attosecond delays
    in molecular photoionization. It is shown how delays relevant to one-photon-ionization,
    also known as Eisenbud-Wigner-Smith delays, can be obtained from the complex dipole
    matrix elements provided by molecular quantum scattering theory. These results
    are used to derive formulae for the delays measured by two-photon attosecond interferometry
    based on an attosecond pulse train and a dressing femtosecond infrared pulse.
    These effective delays are first expressed in the molecular frame where maximal
    information about the molecular photoionization dynamics is available. The effects
    of averaging over the emission direction of the electron and the molecular orientation
    are introduced analytically. We illustrate this general formalism for the case
    of two polyatomic molecules. N2O serves as an example of a polar linear molecule
    characterized by complex photoionization dynamics resulting from the presence
    of molecular shape resonances. H2O illustrates the case of a non-linear molecule
    with comparably simple photoionization dynamics resulting from a flat continuum.
    Our theory establishes the foundation for interpreting measurements of the photoionization
    dynamics of all molecules by attosecond metrology.
article_number: '124306'
article_processing_charge: No
article_type: original
author:
- first_name: Denitsa Rangelova
  full_name: Baykusheva, Denitsa Rangelova
  id: 71b4d059-2a03-11ee-914d-dfa3beed6530
  last_name: Baykusheva
- first_name: Hans Jakob
  full_name: Wörner, Hans Jakob
  last_name: Wörner
citation:
  ama: Baykusheva DR, Wörner HJ. Theory of attosecond delays in molecular photoionization.
    <i>The Journal of Chemical Physics</i>. 2017;146(12). doi:<a href="https://doi.org/10.1063/1.4977933">10.1063/1.4977933</a>
  apa: Baykusheva, D. R., &#38; Wörner, H. J. (2017). Theory of attosecond delays
    in molecular photoionization. <i>The Journal of Chemical Physics</i>. AIP Publishing.
    <a href="https://doi.org/10.1063/1.4977933">https://doi.org/10.1063/1.4977933</a>
  chicago: Baykusheva, Denitsa Rangelova, and Hans Jakob Wörner. “Theory of Attosecond
    Delays in Molecular Photoionization.” <i>The Journal of Chemical Physics</i>.
    AIP Publishing, 2017. <a href="https://doi.org/10.1063/1.4977933">https://doi.org/10.1063/1.4977933</a>.
  ieee: D. R. Baykusheva and H. J. Wörner, “Theory of attosecond delays in molecular
    photoionization,” <i>The Journal of Chemical Physics</i>, vol. 146, no. 12. AIP
    Publishing, 2017.
  ista: Baykusheva DR, Wörner HJ. 2017. Theory of attosecond delays in molecular photoionization.
    The Journal of Chemical Physics. 146(12), 124306.
  mla: Baykusheva, Denitsa Rangelova, and Hans Jakob Wörner. “Theory of Attosecond
    Delays in Molecular Photoionization.” <i>The Journal of Chemical Physics</i>,
    vol. 146, no. 12, 124306, AIP Publishing, 2017, doi:<a href="https://doi.org/10.1063/1.4977933">10.1063/1.4977933</a>.
  short: D.R. Baykusheva, H.J. Wörner, The Journal of Chemical Physics 146 (2017).
date_created: 2023-08-10T06:36:19Z
date_published: 2017-03-28T00:00:00Z
date_updated: 2023-08-22T08:30:59Z
day: '28'
doi: 10.1063/1.4977933
extern: '1'
external_id:
  pmid:
  - '28388142'
intvolume: '       146'
issue: '12'
keyword:
- Physical and Theoretical Chemistry
- General Physics and Astronomy
language:
- iso: eng
month: '03'
oa_version: None
pmid: 1
publication: The Journal of Chemical Physics
publication_identifier:
  eissn:
  - 1089-7690
  issn:
  - 0021-9606
publication_status: published
publisher: AIP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Theory of attosecond delays in molecular photoionization
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 146
year: '2017'
...
---
_id: '14031'
abstract:
- lang: eng
  text: High-harmonic spectroscopy driven by circularly polarized laser pulses and
    their counterrotating second harmonic is a new branch of attosecond science which
    currently lacks quantitative interpretations. We extend this technique to the
    midinfrared regime and record detailed high-harmonic spectra of several rare-gas
    atoms. These results are compared with the solution of the Schrödinger equation
    in three dimensions and calculations based on the strong-field approximation that
    incorporate accurate scattering-wave recombination matrix elements. A quantum-orbit
    analysis of these results provides a transparent interpretation of the measured
    intensity ratios of symmetry-allowed neighboring harmonics in terms of (i) a set
    of propensity rules related to the angular momentum of the atomic orbitals, (ii)
    atom-specific matrix elements related to their electronic structure, and (iii)
    the interference of the emissions associated with electrons in orbitals corotating
    or counterrotating with the laser fields. These results provide the foundation
    for a quantitative understanding of bicircular high-harmonic spectroscopy.
article_number: '203201'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Denitsa Rangelova
  full_name: Baykusheva, Denitsa Rangelova
  id: 71b4d059-2a03-11ee-914d-dfa3beed6530
  last_name: Baykusheva
- first_name: Simon
  full_name: Brennecke, Simon
  last_name: Brennecke
- first_name: Manfred
  full_name: Lein, Manfred
  last_name: Lein
- first_name: Hans Jakob
  full_name: Wörner, Hans Jakob
  last_name: Wörner
citation:
  ama: Baykusheva DR, Brennecke S, Lein M, Wörner HJ. Signatures of electronic structure
    in bicircular high-harmonic spectroscopy. <i>Physical Review Letters</i>. 2017;119(20).
    doi:<a href="https://doi.org/10.1103/physrevlett.119.203201">10.1103/physrevlett.119.203201</a>
  apa: Baykusheva, D. R., Brennecke, S., Lein, M., &#38; Wörner, H. J. (2017). Signatures
    of electronic structure in bicircular high-harmonic spectroscopy. <i>Physical
    Review Letters</i>. American Physical Society. <a href="https://doi.org/10.1103/physrevlett.119.203201">https://doi.org/10.1103/physrevlett.119.203201</a>
  chicago: Baykusheva, Denitsa Rangelova, Simon Brennecke, Manfred Lein, and Hans
    Jakob Wörner. “Signatures of Electronic Structure in Bicircular High-Harmonic
    Spectroscopy.” <i>Physical Review Letters</i>. American Physical Society, 2017.
    <a href="https://doi.org/10.1103/physrevlett.119.203201">https://doi.org/10.1103/physrevlett.119.203201</a>.
  ieee: D. R. Baykusheva, S. Brennecke, M. Lein, and H. J. Wörner, “Signatures of
    electronic structure in bicircular high-harmonic spectroscopy,” <i>Physical Review
    Letters</i>, vol. 119, no. 20. American Physical Society, 2017.
  ista: Baykusheva DR, Brennecke S, Lein M, Wörner HJ. 2017. Signatures of electronic
    structure in bicircular high-harmonic spectroscopy. Physical Review Letters. 119(20),
    203201.
  mla: Baykusheva, Denitsa Rangelova, et al. “Signatures of Electronic Structure in
    Bicircular High-Harmonic Spectroscopy.” <i>Physical Review Letters</i>, vol. 119,
    no. 20, 203201, American Physical Society, 2017, doi:<a href="https://doi.org/10.1103/physrevlett.119.203201">10.1103/physrevlett.119.203201</a>.
  short: D.R. Baykusheva, S. Brennecke, M. Lein, H.J. Wörner, Physical Review Letters
    119 (2017).
date_created: 2023-08-10T06:48:12Z
date_published: 2017-11-17T00:00:00Z
date_updated: 2023-08-22T06:48:28Z
day: '17'
doi: 10.1103/physrevlett.119.203201
extern: '1'
external_id:
  arxiv:
  - '1710.04474'
  pmid:
  - '29219334'
intvolume: '       119'
issue: '20'
keyword:
- General Physics and Astronomy
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1710.04474
month: '11'
oa: 1
oa_version: Preprint
pmid: 1
publication: Physical Review Letters
publication_identifier:
  eissn:
  - 1079-7114
  issn:
  - 0031-9007
publication_status: published
publisher: American Physical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Signatures of electronic structure in bicircular high-harmonic spectroscopy
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 119
year: '2017'
...
---
_id: '11072'
abstract:
- lang: eng
  text: "Spatiotemporal activation of RhoA and actomyosin contraction underpins cellular
    adhesion and division. Loss of cell–cell adhesion and chromosomal instability
    are cardinal events that drive tumour progression. Here, we show that p120-catenin
    (p120) not only controls cell–cell adhesion, but also acts as a critical regulator
    of cytokinesis. We find that p120 regulates actomyosin contractility through concomitant
    binding to RhoA and the centralspindlin component MKLP1, independent of cadherin
    association. In anaphase, p120 is enriched at the cleavage furrow where it binds
    MKLP1 to spatially control RhoA GTPase cycling. Binding of p120 to MKLP1 during
    cytokinesis depends on the N-terminal coiled-coil domain of p120 isoform 1A. Importantly,
    clinical data show that loss of p120 expression is a common event in breast cancer
    that strongly correlates with multinucleation and adverse patient survival. In
    summary, our study identifies p120 loss as a driver event of chromosomal instability
    in cancer.\r\n"
article_number: '13874'
article_processing_charge: No
article_type: original
author:
- first_name: Robert A.H.
  full_name: van de Ven, Robert A.H.
  last_name: van de Ven
- first_name: Jolien S.
  full_name: de Groot, Jolien S.
  last_name: de Groot
- first_name: Danielle
  full_name: Park, Danielle
  last_name: Park
- first_name: Robert
  full_name: van Domselaar, Robert
  last_name: van Domselaar
- first_name: Danielle
  full_name: de Jong, Danielle
  last_name: de Jong
- first_name: Karoly
  full_name: Szuhai, Karoly
  last_name: Szuhai
- first_name: Elsken
  full_name: van der Wall, Elsken
  last_name: van der Wall
- first_name: Oscar M.
  full_name: Rueda, Oscar M.
  last_name: Rueda
- first_name: H. Raza
  full_name: Ali, H. Raza
  last_name: Ali
- first_name: Carlos
  full_name: Caldas, Carlos
  last_name: Caldas
- first_name: Paul J.
  full_name: van Diest, Paul J.
  last_name: van Diest
- first_name: Martin W
  full_name: HETZER, Martin W
  id: 86c0d31b-b4eb-11ec-ac5a-eae7b2e135ed
  last_name: HETZER
  orcid: 0000-0002-2111-992X
- first_name: Erik
  full_name: Sahai, Erik
  last_name: Sahai
- first_name: Patrick W.B.
  full_name: Derksen, Patrick W.B.
  last_name: Derksen
citation:
  ama: van de Ven RAH, de Groot JS, Park D, et al. p120-catenin prevents multinucleation
    through control of MKLP1-dependent RhoA activity during cytokinesis. <i>Nature
    Communications</i>. 2016;7. doi:<a href="https://doi.org/10.1038/ncomms13874">10.1038/ncomms13874</a>
  apa: van de Ven, R. A. H., de Groot, J. S., Park, D., van Domselaar, R., de Jong,
    D., Szuhai, K., … Derksen, P. W. B. (2016). p120-catenin prevents multinucleation
    through control of MKLP1-dependent RhoA activity during cytokinesis. <i>Nature
    Communications</i>. Springer Nature. <a href="https://doi.org/10.1038/ncomms13874">https://doi.org/10.1038/ncomms13874</a>
  chicago: Ven, Robert A.H. van de, Jolien S. de Groot, Danielle Park, Robert van
    Domselaar, Danielle de Jong, Karoly Szuhai, Elsken van der Wall, et al. “P120-Catenin
    Prevents Multinucleation through Control of MKLP1-Dependent RhoA Activity during
    Cytokinesis.” <i>Nature Communications</i>. Springer Nature, 2016. <a href="https://doi.org/10.1038/ncomms13874">https://doi.org/10.1038/ncomms13874</a>.
  ieee: R. A. H. van de Ven <i>et al.</i>, “p120-catenin prevents multinucleation
    through control of MKLP1-dependent RhoA activity during cytokinesis,” <i>Nature
    Communications</i>, vol. 7. Springer Nature, 2016.
  ista: van de Ven RAH, de Groot JS, Park D, van Domselaar R, de Jong D, Szuhai K,
    van der Wall E, Rueda OM, Ali HR, Caldas C, van Diest PJ, Hetzer M, Sahai E, Derksen
    PWB. 2016. p120-catenin prevents multinucleation through control of MKLP1-dependent
    RhoA activity during cytokinesis. Nature Communications. 7, 13874.
  mla: van de Ven, Robert A. H., et al. “P120-Catenin Prevents Multinucleation through
    Control of MKLP1-Dependent RhoA Activity during Cytokinesis.” <i>Nature Communications</i>,
    vol. 7, 13874, Springer Nature, 2016, doi:<a href="https://doi.org/10.1038/ncomms13874">10.1038/ncomms13874</a>.
  short: R.A.H. van de Ven, J.S. de Groot, D. Park, R. van Domselaar, D. de Jong,
    K. Szuhai, E. van der Wall, O.M. Rueda, H.R. Ali, C. Caldas, P.J. van Diest, M.
    Hetzer, E. Sahai, P.W.B. Derksen, Nature Communications 7 (2016).
date_created: 2022-04-07T07:48:34Z
date_published: 2016-12-22T00:00:00Z
date_updated: 2022-07-18T08:34:32Z
day: '22'
doi: 10.1038/ncomms13874
extern: '1'
external_id:
  pmid:
  - '28004812'
intvolume: '         7'
keyword:
- General Physics and Astronomy
- General Biochemistry
- Genetics and Molecular Biology
- General Chemistry
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1038/ncomms13874
month: '12'
oa: 1
oa_version: Published Version
pmid: 1
publication: Nature Communications
publication_identifier:
  issn:
  - 2041-1723
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
related_material:
  link:
  - relation: erratum
    url: https://doi.org/10.1038/ncomms16030
scopus_import: '1'
status: public
title: p120-catenin prevents multinucleation through control of MKLP1-dependent RhoA
  activity during cytokinesis
type: journal_article
user_id: 72615eeb-f1f3-11ec-aa25-d4573ddc34fd
volume: 7
year: '2016'
...
---
_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: '11576'
abstract:
- lang: eng
  text: We use new near-infrared spectroscopic observations to investigate the nature
    and evolution of the most luminous Hα emitters at z ∼ 0.8–2.23, which evolve strongly
    in number density over this period, and compare them to more typical Hα emitters.
    We study 59 luminous Hα emitters with LHα > L∗Hα⁠, roughly equally split per redshift
    slice at z ∼ 0.8, 1.47 and 2.23 from the HiZELS and CF-HiZELS surveys. We find
    that, overall, 30 ± 8 per cent are active galactic nuclei [AGNs; 80 ± 30 per cent
    of these AGNs are broad-line AGNs, BL-AGNs], and we find little to no evolution
    in the AGN fraction with redshift, within the errors. However, the AGN fraction
    increases strongly with Hα luminosity and correlates best with LHα/L∗Hα(z)⁠. While
    LHα ≤ L∗Hα(z) Hα emitters are largely dominated by star-forming galaxies (>80
    per cent), the most luminous Hα emitters (⁠LHα>10L∗Hα(z)⁠) at any cosmic time
    are essentially all BL-AGN. Using our AGN-decontaminated sample of luminous star-forming
    galaxies, and integrating down to a fixed Hα luminosity, we find a factor of ∼1300
    evolution in the star formation rate density from z = 0 to 2.23. This is much
    stronger than the evolution from typical Hα star-forming galaxies and in line
    with the evolution seen for constant luminosity cuts used to select ‘ultraluminous’
    infrared galaxies and/or sub-millimetre galaxies. By taking into account the evolution
    in the typical Hα luminosity, we show that the most strongly star-forming Hα-selected
    galaxies at any epoch (⁠LHα>L∗Hα(z)⁠) contribute the same fractional amount of
    ≈15 per cent to the total star formation rate density, at least up to z = 2.23.
acknowledgement: "The authors would like to thank the anonymous reviewer for the many
  helpful comments and suggestions which greatly improved the clarity and quality
  of this work. DS and SAK acknowledge financial support from the Netherlands Organisation
  for Scientific research (NWO) through a Veni fellowship. DS also acknowledges funding
  from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010)
  and from FCT grant PEst-OE/FIS/UI2751/2014. Part of this project was undertaken
  during the inaugural Leiden/ESA Astrophysics Program for Summer Students (LEAPS).
  IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator
  programme DUSTYGAL 321334 and a Royal Society/Wolfson merit award. CH acknowledges
  support from STFC. Based on observations made with ESO Telescopes at the La Silla
  Paranal Observatory under programme ID 087.A-0337 and ID 089.A-0965. Also based
  on data from the Telescopio Nazionale Galileo, with time awarded through OPTICON
  programmes 2011A/026 and 2012A020 and the William Herschel Telescope under programme
  W12BN007. The William Herschel Telescope is operated on the island of La Palma by
  the Isaac Newton Group in the Spanish\r\nObservatorio del Roque de los Muchachos
  of the Instituto de Astrofisica de Canarias. The authors wish to thank all the help
  given by the telescope staff from all the observatories used in this study: ESO
  staff in La Silla, and the TNG and WHT staff in La Palma. This publication makes
  use of data products from the Two Micron All-Sky Survey, which is a joint project
  of the University of Massachusetts and the Infrared Processing and Analysis Center/California
  Institute of Technology, funded by the National Aeronautics and Space Administration
  and the National Science Foundation."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Saul A.
  full_name: Kohn, Saul A.
  last_name: Kohn
- first_name: Philip N.
  full_name: Best, Philip N.
  last_name: Best
- first_name: Ian
  full_name: Smail, Ian
  last_name: Smail
- first_name: Chris M.
  full_name: Harrison, Chris M.
  last_name: Harrison
- first_name: John
  full_name: Stott, John
  last_name: Stott
- first_name: João
  full_name: Calhau, João
  last_name: Calhau
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
citation:
  ama: 'Sobral D, Kohn SA, Best PN, et al. The most luminous H α emitters at z ∼ 0.8–2.23
    from HiZELS: Evolution of AGN and star-forming galaxies. <i>Monthly Notices of
    the Royal Astronomical Society</i>. 2016;457(2):1739-1752. doi:<a href="https://doi.org/10.1093/mnras/stw022">10.1093/mnras/stw022</a>'
  apa: 'Sobral, D., Kohn, S. A., Best, P. N., Smail, I., Harrison, C. M., Stott, J.,
    … Matthee, J. J. (2016). The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS:
    Evolution of AGN and star-forming galaxies. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stw022">https://doi.org/10.1093/mnras/stw022</a>'
  chicago: 'Sobral, David, Saul A. Kohn, Philip N. Best, Ian Smail, Chris M. Harrison,
    John Stott, João Calhau, and Jorryt J Matthee. “The Most Luminous H α Emitters
    at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and Star-Forming Galaxies.” <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press, 2016.
    <a href="https://doi.org/10.1093/mnras/stw022">https://doi.org/10.1093/mnras/stw022</a>.'
  ieee: 'D. Sobral <i>et al.</i>, “The most luminous H α emitters at z ∼ 0.8–2.23
    from HiZELS: Evolution of AGN and star-forming galaxies,” <i>Monthly Notices of
    the Royal Astronomical Society</i>, vol. 457, no. 2. Oxford University Press,
    pp. 1739–1752, 2016.'
  ista: 'Sobral D, Kohn SA, Best PN, Smail I, Harrison CM, Stott J, Calhau J, Matthee
    JJ. 2016. The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution
    of AGN and star-forming galaxies. Monthly Notices of the Royal Astronomical Society.
    457(2), 1739–1752.'
  mla: 'Sobral, David, et al. “The Most Luminous H α Emitters at z ∼ 0.8–2.23 from
    HiZELS: Evolution of AGN and Star-Forming Galaxies.” <i>Monthly Notices of the
    Royal Astronomical Society</i>, vol. 457, no. 2, Oxford University Press, 2016,
    pp. 1739–52, doi:<a href="https://doi.org/10.1093/mnras/stw022">10.1093/mnras/stw022</a>.'
  short: D. Sobral, S.A. Kohn, P.N. Best, I. Smail, C.M. Harrison, J. Stott, J. Calhau,
    J.J. Matthee, Monthly Notices of the Royal Astronomical Society 457 (2016) 1739–1752.
date_created: 2022-07-13T12:50:36Z
date_published: 2016-04-01T00:00:00Z
date_updated: 2022-08-19T08:15:21Z
day: '01'
doi: 10.1093/mnras/stw022
extern: '1'
external_id:
  arxiv:
  - '1601.02266'
intvolume: '       457'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1601.02266
month: '04'
oa: 1
oa_version: Preprint
page: 1739-1752
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 most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN
  and star-forming galaxies'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 457
year: '2016'
...
---
_id: '11578'
abstract:
- lang: eng
  text: We present the first results from our CAlibrating LYMan α with Hα (CALYMHA)
    pilot survey at the Isaac Newton Telescope. We measure Lyα emission for 488 Hα
    selected galaxies at z = 2.23 from High-z Emission Line Survey in the COSMOS and
    UDS fields with a specially designed narrow-band filter (λc = 3918 Å, Δλ = 52
    Å). We find 17 dual Hα-Lyα emitters [fLyα > 5 × 10−17 erg s−1 cm−2, of which five
    are X-ray active galactic nuclei (AGN)]. For star-forming galaxies, we find a
    range of Lyα escape fractions (fesc, measured with 3 arcsec apertures) from 2
    to 30 per cent. These galaxies have masses from 3 × 108 M⊙ to 1011 M⊙ and dust
    attenuations E(B − V) = 0–0.5. Using stacking, we measure a median escape fraction
    of 1.6 ± 0.5 per cent (4.0 ± 1.0 per cent without correcting Hα for dust), but
    show that this depends on galaxy properties. The stacked fesc tends to decrease
    with increasing star formation rate and dust attenuation. However, at the highest
    masses and dust attenuations, we detect individual galaxies with fesc much higher
    than the typical values from stacking, indicating significant scatter in the values
    of fesc. Relations between fesc and UV slope are bimodal, with high fesc for either
    the bluest or reddest galaxies. We speculate that this bimodality and large scatter
    in the values of fesc is due to additional physical mechanisms such as outflows
    facilitating fesc for dusty/massive systems. Lyα is significantly more extended
    than Hα and the UV. fesc continues to increase up to at least 20 kpc (3σ, 40 kpc
    [2σ]) for typical star-forming galaxies and thus the aperture is the most important
    predictor of fesc.
acknowledgement: "We thank the anonymous referee for constructive comments and suggestions
  which have improved the quality of this work. JM acknowledges the support of a Huygens
  PhD fellowship from Leiden University. DS and JM acknowledge financial support from
  the Netherlands Organization for Scientific research (NWO) through a Veni fellowship,
  and DS from FCT through a FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010)
  and from FCT grant PEst-OE/FIS/UI2751/2014. IO acknowledges support from the European
  Research Council (ERC) in the form of Advanced Investigator Programme, COSMICISM,
  321302. HR acknowledges support from the ERC Advanced Investigator programme NewClusters
  321271. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator
  programme DUSTYGAL 321334 and a Royal Society/Wolfson Merit Award. APA acknowledges
  support from the Fundac¸ao para a Ciencia e para a Tecnologia (FCT) through the
  Fellowship SFRH/BD/52706/2014.\r\nBased on observations made with the Isaac Newton
  Telescope (proposals 2013AN002, 2013BN008, 2014AC88, 2014AN002, 2014BN006, 2014BC118)
  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 Astrof´ısica de Canarias. We acknowledge
  the tremendous work that has been done by both COSMOS and UKIDSS UDS/SXDF teams
  in assembling such large, state-ofthe-art multi-wavelength data sets over such wide
  areas, as those have been crucial for the results presented in this paper. The sample
  of HAEs is publicly available from Sobral et al. (2013).\r\nWe have benefited greatly
  from the publically 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
  imaging tools SEXTRACTOR, SWARP and SCAMP (Bertin & Arnouts 1996; Bertin 2006, 2010)
  and the TOPCAT analysis program (Taylor 2005)."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Iván
  full_name: Oteo, Iván
  last_name: Oteo
- first_name: Philip
  full_name: Best, Philip
  last_name: Best
- first_name: Ian
  full_name: Smail, Ian
  last_name: Smail
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
- first_name: Ana
  full_name: Paulino-Afonso, Ana
  last_name: Paulino-Afonso
citation:
  ama: 'Matthee JJ, Sobral D, Oteo I, et al. The CALYMHA survey: Lyα escape fraction
    and its dependence on galaxy properties at z = 2.23. <i>Monthly Notices of the
    Royal Astronomical Society</i>. 2016;458(1):449-467. doi:<a href="https://doi.org/10.1093/mnras/stw322">10.1093/mnras/stw322</a>'
  apa: 'Matthee, J. J., Sobral, D., Oteo, I., Best, P., Smail, I., Röttgering, H.,
    &#38; Paulino-Afonso, A. (2016). The CALYMHA survey: Lyα escape fraction and its
    dependence on galaxy properties at z = 2.23. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stw322">https://doi.org/10.1093/mnras/stw322</a>'
  chicago: 'Matthee, Jorryt J, David Sobral, Iván Oteo, Philip Best, Ian Smail, Huub
    Röttgering, and Ana Paulino-Afonso. “The CALYMHA Survey: Lyα Escape Fraction and
    Its Dependence on Galaxy Properties at z = 2.23.” <i>Monthly Notices of the Royal
    Astronomical Society</i>. Oxford University Press, 2016. <a href="https://doi.org/10.1093/mnras/stw322">https://doi.org/10.1093/mnras/stw322</a>.'
  ieee: 'J. J. Matthee <i>et al.</i>, “The CALYMHA survey: Lyα escape fraction and
    its dependence on galaxy properties at z = 2.23,” <i>Monthly Notices of the Royal
    Astronomical Society</i>, vol. 458, no. 1. Oxford University Press, pp. 449–467,
    2016.'
  ista: 'Matthee JJ, Sobral D, Oteo I, Best P, Smail I, Röttgering H, Paulino-Afonso
    A. 2016. The CALYMHA survey: Lyα escape fraction and its dependence on galaxy
    properties at z = 2.23. Monthly Notices of the Royal Astronomical Society. 458(1),
    449–467.'
  mla: 'Matthee, Jorryt J., et al. “The CALYMHA Survey: Lyα Escape Fraction and Its
    Dependence on Galaxy Properties at z = 2.23.” <i>Monthly Notices of the Royal
    Astronomical Society</i>, vol. 458, no. 1, Oxford University Press, 2016, pp.
    449–67, doi:<a href="https://doi.org/10.1093/mnras/stw322">10.1093/mnras/stw322</a>.'
  short: J.J. Matthee, D. Sobral, I. Oteo, P. Best, I. Smail, H. Röttgering, A. Paulino-Afonso,
    Monthly Notices of the Royal Astronomical Society 458 (2016) 449–467.
date_created: 2022-07-14T08:51:37Z
date_published: 2016-05-01T00:00:00Z
date_updated: 2022-08-19T08:17:19Z
day: '01'
doi: 10.1093/mnras/stw322
extern: '1'
external_id:
  arxiv:
  - '1602.02756'
intvolume: '       458'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: ISM'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1602.02756
month: '05'
oa: 1
oa_version: Preprint
page: 449-467
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties
  at z = 2.23'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 458
year: '2016'
...
---
_id: '13478'
abstract:
- lang: eng
  text: HR 8799 is a star accompanied by four massive planets on wide orbits. The
    observed planetary configuration has been shown to be unstable on a timescale
    much shorter than the estimated age of the system (~30 Myr) unless the planets
    are locked into mean motion resonances. This condition is characterised by small-amplitude
    libration of one or more resonant angles that stabilise the system by preventing
    close encounters. We simulate planetary systems similar to the HR 8799 planetary
    system, exploring the parameter space in separation between the orbits, planetary
    masses and distance from the Sun to the star. We find systems that look like HR
    8799 and remain stable for longer than the estimated age of HR 8799. None of our
    systems are forced into resonances. We find, with nominal masses (Mb = 5 MJup
    and Mc,d,e = 7 MJup) and in a narrow range of orbit separations, that 5 of 100
    systems match the observations and lifetime. Considering a broad range of orbit
    separations, we find 12 of 900 similar systems. The systems survive significantly
    longer because of their slightly increased initial orbit separations compared
    to assuming circular orbits from the observed positions. A small increase in separation
    leads to a significant increase in survival time. The low eccentricity the orbits
    develop from gravitational interaction is enough for the planets to match the
    observations. With lower masses, but still comfortably within the estimated planet
    mass uncertainty, we find 18 of 100 matching and long-lived systems in a narrow
    orbital separation range. In the broad separation range, we find 82 of 900 matching
    systems. Our results imply that the planets in the HR 8799 system do not have
    to be in strong mean motion resonances. We also investigate the future of wide-orbit
    planetary systems using our HR 8799 analogues. We find that 80% of the systems
    have two planets left after strong planet-planet scattering and these are on eccentric
    orbits with semi-major axes of a1 ~ 10 AU and a2 ~ 30−1000 AU. We speculate that
    other wide-orbit planetary systems, such as AB Pic and HD 106906, are the remnants
    of HR 8799 analogues that underwent close encounters and dynamical instability.
article_number: A147
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Ylva Louise Linsdotter
  full_name: Götberg, Ylva Louise Linsdotter
  id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
  last_name: Götberg
  orcid: 0000-0002-6960-6911
- first_name: Melvyn B.
  full_name: Davies, Melvyn B.
  last_name: Davies
- first_name: Alexander J.
  full_name: Mustill, Alexander J.
  last_name: Mustill
- first_name: Anders
  full_name: Johansen, Anders
  last_name: Johansen
- first_name: Ross P.
  full_name: Church, Ross P.
  last_name: Church
citation:
  ama: Götberg YLL, Davies MB, Mustill AJ, Johansen A, Church RP. Long-term stability
    of the HR 8799 planetary system without resonant lock. <i>Astronomy &#38; Astrophysics</i>.
    2016;592. doi:<a href="https://doi.org/10.1051/0004-6361/201526309">10.1051/0004-6361/201526309</a>
  apa: Götberg, Y. L. L., Davies, M. B., Mustill, A. J., Johansen, A., &#38; Church,
    R. P. (2016). Long-term stability of the HR 8799 planetary system without resonant
    lock. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/201526309">https://doi.org/10.1051/0004-6361/201526309</a>
  chicago: Götberg, Ylva Louise Linsdotter, Melvyn B. Davies, Alexander J. Mustill,
    Anders Johansen, and Ross P. Church. “Long-Term Stability of the HR 8799 Planetary
    System without Resonant Lock.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences,
    2016. <a href="https://doi.org/10.1051/0004-6361/201526309">https://doi.org/10.1051/0004-6361/201526309</a>.
  ieee: Y. L. L. Götberg, M. B. Davies, A. J. Mustill, A. Johansen, and R. P. Church,
    “Long-term stability of the HR 8799 planetary system without resonant lock,” <i>Astronomy
    &#38; Astrophysics</i>, vol. 592. EDP Sciences, 2016.
  ista: Götberg YLL, Davies MB, Mustill AJ, Johansen A, Church RP. 2016. Long-term
    stability of the HR 8799 planetary system without resonant lock. Astronomy &#38;
    Astrophysics. 592, A147.
  mla: Götberg, Ylva Louise Linsdotter, et al. “Long-Term Stability of the HR 8799
    Planetary System without Resonant Lock.” <i>Astronomy &#38; Astrophysics</i>,
    vol. 592, A147, EDP Sciences, 2016, doi:<a href="https://doi.org/10.1051/0004-6361/201526309">10.1051/0004-6361/201526309</a>.
  short: Y.L.L. Götberg, M.B. Davies, A.J. Mustill, A. Johansen, R.P. Church, Astronomy
    &#38; Astrophysics 592 (2016).
date_created: 2023-08-03T10:15:28Z
date_published: 2016-08-18T00:00:00Z
date_updated: 2023-08-09T11:09:50Z
day: '18'
doi: 10.1051/0004-6361/201526309
extern: '1'
external_id:
  arxiv:
  - '1606.07819'
intvolume: '       592'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1051/0004-6361/201526309
month: '08'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Long-term stability of the HR 8799 planetary system without resonant lock
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 592
year: '2016'
...