---
_id: '11585'
abstract:
- lang: eng
  text: "Observations show that star-forming galaxies reside on a tight three-dimensional
    plane between mass, gas-phase metallicity and star formation rate (SFR), which
    can be explained by the interplay between metal-poor gas inflows, SFR and outflows.
    However, different metals are released on different time-scales, which may affect
    the slope of this relation. Here, we use central, star-forming galaxies with Mstar
    = 109.0−10.5 M\f from the EAGLE hydrodynamical simulation to examine three-dimensional
    relations between mass, SFR and chemical enrichment using absolute and relative
    C, N, O and Fe abundances. We show that the scatter is smaller when gas-phase
    α-enhancement is used rather than metallicity. A similar plane also exists for
    stellar α-enhancement, implying that present-day specific SFRs are correlated
    with long time-scale star formation histories. Between z = 0 and 1, the α-enhancement
    plane is even more insensitive to redshift than the plane using metallicity. However,
    it evolves at z > 1 due to lagging iron yields. At fixed mass, galaxies with higher
    SFRs have star formation histories shifted toward late times, are more α-enhanced
    and this α-enhancement increases with redshift as observed. These findings suggest
    that relations between physical properties inferred from observations may be affected
    by systematic variations in α-enhancements."
acknowledgement: We thank the anonymous referee for their constructive comments. JM
  acknowledges the support of a Huygens PhD fellowship from Leiden University. We
  thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge
  the use of the Topcat software (Taylor 2013) for assisting in rapid exploration
  of multi-dimensional datasets and the use of Python and its numpy, matplotlib and
  pandas packages.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
citation:
  ama: Matthee JJ. Differences in galaxy colours are not just about the mass. <i>Nature
    Astronomy</i>. 2021;5:984-985. doi:<a href="https://doi.org/10.1038/s41550-021-01415-y">10.1038/s41550-021-01415-y</a>
  apa: Matthee, J. J. (2021). Differences in galaxy colours are not just about the
    mass. <i>Nature Astronomy</i>. Springer Nature. <a href="https://doi.org/10.1038/s41550-021-01415-y">https://doi.org/10.1038/s41550-021-01415-y</a>
  chicago: Matthee, Jorryt J. “Differences in Galaxy Colours Are Not Just about the
    Mass.” <i>Nature Astronomy</i>. Springer Nature, 2021. <a href="https://doi.org/10.1038/s41550-021-01415-y">https://doi.org/10.1038/s41550-021-01415-y</a>.
  ieee: J. J. Matthee, “Differences in galaxy colours are not just about the mass,”
    <i>Nature Astronomy</i>, vol. 5. Springer Nature, pp. 984–985, 2021.
  ista: Matthee JJ. 2021. Differences in galaxy colours are not just about the mass.
    Nature Astronomy. 5, 984–985.
  mla: Matthee, Jorryt J. “Differences in Galaxy Colours Are Not Just about the Mass.”
    <i>Nature Astronomy</i>, vol. 5, Springer Nature, 2021, pp. 984–85, doi:<a href="https://doi.org/10.1038/s41550-021-01415-y">10.1038/s41550-021-01415-y</a>.
  short: J.J. Matthee, Nature Astronomy 5 (2021) 984–985.
date_created: 2022-07-14T13:13:39Z
date_published: 2021-07-05T00:00:00Z
date_updated: 2022-08-19T08:37:58Z
day: '05'
doi: 10.1038/s41550-021-01415-y
extern: '1'
external_id:
  arxiv:
  - '1802.06786'
intvolume: '         5'
keyword:
- Astronomy and Astrophysics
- galaxies
- formation - galaxies
- evolution - galaxies
- star formation - galaxies
- abundances
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1802.06786
month: '07'
oa: 1
oa_version: Preprint
page: 984-985
publication: Nature Astronomy
publication_identifier:
  eissn:
  - 2397-3366
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
scopus_import: '1'
status: public
title: Differences in galaxy colours are not just about the mass
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 5
year: '2021'
...
---
_id: '11533'
abstract:
- lang: eng
  text: We explore deep rest-frame UV to FIR data in the COSMOS field to measure the
    individual spectral energy distributions (SED) of the ∼4000 SC4K (Sobral et al.)
    Lyman α (Ly α) emitters (LAEs) at z ∼ 2–6. We find typical stellar masses of 109.3
    ± 0.6 M⊙ and star formation rates (SFR) of SFRSED=4.4+10.5−2.4 M⊙ yr−1 and SFRLyα=5.9+6.3−2.6 M⊙ yr−1,
    combined with very blue UV slopes of β=−2.1+0.5−0.4⁠, but with significant variations
    within the population. MUV and β are correlated in a similar way to UV-selected
    sources, but LAEs are consistently bluer. This suggests that LAEs are the youngest
    and/or most dust-poor subset of the UV-selected population. We also study the
    Ly α rest-frame equivalent width (EW0) and find 45 ‘extreme’ LAEs with EW0 > 240 Å
    (3σ), implying a low number density of (7 ± 1) × 10−7 Mpc−3. Overall, we measure
    little to no evolution of the Ly α EW0 and scale length parameter (w0), which
    are consistently high (EW0=140+280−70 Å, w0=129+11−11 Å) from z ∼ 6 to z ∼ 2 and
    below. However, w0 is anticorrelated with MUV and stellar mass. Our results imply
    that sources selected as LAEs have a high Ly α escape fraction (fesc,Ly α) irrespective
    of cosmic time, but fesc,Ly α is still higher for UV-fainter and lower mass LAEs.
    The least massive LAEs (<109.5 M⊙) are typically located above the star formation
    ‘main sequence’ (MS), but the offset from the MS decreases towards z ∼ 6 and towards
    1010 M⊙. Our results imply a lack of evolution in the properties of LAEs across
    time and reveals the increasing overlap in properties of LAEs and UV-continuum
    selected galaxies as typical star-forming galaxies at high redshift effectively
    become LAEs.
acknowledgement: We thank the anonymous referee for the valuable feedback that significantly
  improved the quality and clarity of this paper. SS and JC acknowledge studentships
  from Lancaster University. APA acknowledges support from Fundação para a Ciência
  e a Tecnologia through the project PTDC/FISAST/31546/2017. The authors would like
  to thank Ali Khostovan, Sara Perez Sanchez, Alex Bennett and Tom Rose for contributions
  and discussions in the early stages of this work. 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 CALET and the Cambridge Astronomy
  Survey Unit on behalf of the UltraVISTA consortium. Finally, the authors acknowledge
  the unique value of the publicly available analysis software TOPCAT (Taylor 2005)
  and publicly available programming language Python, including the numpy, pyfits,
  matplotlib, scipy and astropy (Astropy Collaboration et al. 2013) packages. This
  work is based on the public SC4K sample of LAEs (Sobral et al. 2018a) and we release
  the full catalogue with all the photometry and properties derived in this paper,
  in electronic format, along with the relevant tables.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: S
  full_name: Santos, S
  last_name: Santos
- first_name: D
  full_name: Sobral, D
  last_name: Sobral
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: J
  full_name: Calhau, J
  last_name: Calhau
- first_name: E
  full_name: da Cunha, E
  last_name: da Cunha
- first_name: B
  full_name: Ribeiro, B
  last_name: Ribeiro
- first_name: A
  full_name: Paulino-Afonso, A
  last_name: Paulino-Afonso
- first_name: P
  full_name: Arrabal Haro, P
  last_name: Arrabal Haro
- first_name: J
  full_name: Butterworth, J
  last_name: Butterworth
citation:
  ama: Santos S, Sobral D, Matthee JJ, et al. The evolution of rest-frame UV properties,
    Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2020;493(1):141-160. doi:<a href="https://doi.org/10.1093/mnras/staa093">10.1093/mnras/staa093</a>
  apa: Santos, S., Sobral, D., Matthee, J. J., Calhau, J., da Cunha, E., Ribeiro,
    B., … Butterworth, J. (2020). The evolution of rest-frame UV properties, Ly α
    EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. <i>Monthly Notices
    of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/staa093">https://doi.org/10.1093/mnras/staa093</a>
  chicago: Santos, S, D Sobral, Jorryt J Matthee, J Calhau, E da Cunha, B Ribeiro,
    A Paulino-Afonso, P Arrabal Haro, and J Butterworth. “The Evolution of Rest-Frame
    UV Properties, Ly α EWs, and the SFR–Stellar Mass Relation at z ∼ 2–6 for SC4K
    LAEs.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University
    Press, 2020. <a href="https://doi.org/10.1093/mnras/staa093">https://doi.org/10.1093/mnras/staa093</a>.
  ieee: S. Santos <i>et al.</i>, “The evolution of rest-frame UV properties, Ly α
    EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs,” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 493, no. 1. Oxford University Press,
    pp. 141–160, 2020.
  ista: Santos S, Sobral D, Matthee JJ, Calhau J, da Cunha E, Ribeiro B, Paulino-Afonso
    A, Arrabal Haro P, Butterworth J. 2020. The evolution of rest-frame UV properties,
    Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. Monthly
    Notices of the Royal Astronomical Society. 493(1), 141–160.
  mla: Santos, S., et al. “The Evolution of Rest-Frame UV Properties, Ly α EWs, and
    the SFR–Stellar Mass Relation at z ∼ 2–6 for SC4K LAEs.” <i>Monthly Notices of
    the Royal Astronomical Society</i>, vol. 493, no. 1, Oxford University Press,
    2020, pp. 141–60, doi:<a href="https://doi.org/10.1093/mnras/staa093">10.1093/mnras/staa093</a>.
  short: S. Santos, D. Sobral, J.J. Matthee, J. Calhau, E. da Cunha, B. Ribeiro, A.
    Paulino-Afonso, P. Arrabal Haro, J. Butterworth, Monthly Notices of the Royal
    Astronomical Society 493 (2020) 141–160.
date_created: 2022-07-07T12:05:23Z
date_published: 2020-03-01T00:00:00Z
date_updated: 2022-08-18T11:27:43Z
day: '01'
doi: 10.1093/mnras/staa093
extern: '1'
external_id:
  arxiv:
  - '1910.02959'
intvolume: '       493'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: high-redshift'
- 'galaxies: star formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1910.02959
month: '03'
oa: 1
oa_version: Preprint
page: 141-160
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass
  relation at z ∼ 2–6 for SC4K LAEs
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 493
year: '2020'
...
---
_id: '11539'
abstract:
- lang: eng
  text: 'Despite recent progress in understanding Ly α emitters (LAEs), relatively
    little is known regarding their typical black hole activity across cosmic time.
    Here, we study the X-ray and radio properties of ∼4000 LAEs at 2.2 < z < 6 from
    the SC4K survey in the COSMOS field. We detect 254 (⁠6.8per cent±0.4per cent⁠)
    LAEs individually in the X-rays (S/N > 3) with an average luminosity of 1044.31±0.01ergs−1
    and average black hole accretion rate (BHAR) of 0.72±0.01 M⊙ yr−1, consistent
    with moderate to high accreting active galactic neuclei (AGNs). We detect 120
    sources in deep radio data (radio AGN fraction of 3.2per cent±0.3per cent⁠). The
    global AGN fraction (⁠8.6per cent±0.4per cent⁠) rises with Ly α luminosity and
    declines with increasing redshift. For X-ray-detected LAEs, Ly α luminosities
    correlate with the BHARs, suggesting that Ly α luminosity becomes a BHAR indicator.
    Most LAEs (⁠93.1per cent±0.6per cent⁠) at 2 < z < 6 have no detectable X-ray emission
    (BHARs < 0.017 M⊙ yr−1). The median star formation rate (SFR) of star-forming
    LAEs from Ly α and radio luminosities is 7.6+6.6−2.8 M⊙ yr−1. The black hole to
    galaxy growth ratio (BHAR/SFR) for LAEs is <0.0022, consistent with typical star-forming
    galaxies and the local BHAR/SFR relation. We conclude that LAEs at 2 < z < 6 include
    two different populations: an AGN population, where Ly α luminosity traces BHAR,
    and another with low SFRs which remain undetected in even the deepest X-ray stacks
    but is detected in the radio stacks.'
acknowledgement: JM acknowledges the support of a Huygens PhD fellowship from Leiden
  University. We thank Camila Correa for help analysing snipshot merger trees. We
  thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann,
  Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and
  suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade
  of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and
  ideas. We have benefited from the public available programming language PYTHON,
  including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT
  analysis tool (Taylor 2013).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: João
  full_name: Calhau, João
  last_name: Calhau
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Sérgio
  full_name: Santos, Sérgio
  last_name: Santos
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: Ana
  full_name: Paulino-Afonso, Ana
  last_name: Paulino-Afonso
- first_name: Andra
  full_name: Stroe, Andra
  last_name: Stroe
- first_name: Brooke
  full_name: Simmons, Brooke
  last_name: Simmons
- first_name: Cassandra
  full_name: Barlow-Hall, Cassandra
  last_name: Barlow-Hall
- first_name: Benjamin
  full_name: Adams, Benjamin
  last_name: Adams
citation:
  ama: 'Calhau J, Sobral D, Santos S, et al. The X-ray and radio activity of typical
    and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving
    population. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;493(3):3341-3362.
    doi:<a href="https://doi.org/10.1093/mnras/staa476">10.1093/mnras/staa476</a>'
  apa: 'Calhau, J., Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Stroe,
    A., … Adams, B. (2020). The X-ray and radio activity of typical and luminous Ly α
    emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/staa476">https://doi.org/10.1093/mnras/staa476</a>'
  chicago: 'Calhau, João, David Sobral, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso,
    Andra Stroe, Brooke Simmons, Cassandra Barlow-Hall, and Benjamin Adams. “The X-Ray
    and Radio Activity of Typical and Luminous Ly α Emitters from z ∼ 2 to z ∼ 6:
    Evidence for a Diverse, Evolving Population.” <i>Monthly Notices of the Royal
    Astronomical Society</i>. Oxford University Press, 2020. <a href="https://doi.org/10.1093/mnras/staa476">https://doi.org/10.1093/mnras/staa476</a>.'
  ieee: 'J. Calhau <i>et al.</i>, “The X-ray and radio activity of typical and luminous
    Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population,”
    <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 3. Oxford
    University Press, pp. 3341–3362, 2020.'
  ista: 'Calhau J, Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Stroe A, Simmons
    B, Barlow-Hall C, Adams B. 2020. The X-ray and radio activity of typical and luminous
    Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population.
    Monthly Notices of the Royal Astronomical Society. 493(3), 3341–3362.'
  mla: 'Calhau, João, et al. “The X-Ray and Radio Activity of Typical and Luminous
    Ly α Emitters from z ∼ 2 to z ∼ 6: Evidence for a Diverse, Evolving Population.”
    <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 3, Oxford
    University Press, 2020, pp. 3341–62, doi:<a href="https://doi.org/10.1093/mnras/staa476">10.1093/mnras/staa476</a>.'
  short: J. Calhau, D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, A. Stroe,
    B. Simmons, C. Barlow-Hall, B. Adams, Monthly Notices of the Royal Astronomical
    Society 493 (2020) 3341–3362.
date_created: 2022-07-08T07:34:10Z
date_published: 2020-04-01T00:00:00Z
date_updated: 2022-08-18T11:25:31Z
day: '01'
doi: 10.1093/mnras/staa476
extern: '1'
external_id:
  arxiv:
  - '1909.11672'
intvolume: '       493'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: active'
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'quasars: supermassive black holes'
- 'galaxies: star formation'
- 'cosmology: observations'
- 'X-rays: galaxies'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1909.11672
month: '04'
oa: 1
oa_version: Preprint
page: 3341-3362
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 X-ray and radio activity of typical and luminous Ly α emitters from z
  ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 493
year: '2020'
...
---
_id: '11499'
abstract:
- lang: eng
  text: Deep optical spectroscopic surveys of galaxies provide a unique opportunity
    to investigate rest-frame ultra-violet (UV) emission line properties of galaxies
    at z ∼ 2 − 4.5. Here we combine VLT/MUSE Guaranteed Time Observations of the Hubble
    Deep Field South, Ultra Deep Field, COSMOS, and several quasar fields with other
    publicly available data from VLT/VIMOS and VLT/FORS2 to construct a catalogue
    of He II λ1640 emitters at z ≳ 2. The deepest areas of our MUSE pointings reach
    a 3σ line flux limit of 3.1 × 10−19 erg s−1 cm−2. After discarding broad-line
    active galactic nuclei, we find 13 He II λ1640 detections from MUSE with a median
    MUV = −20.1 and 21 tentative He II λ1640 detections from other public surveys.
    Excluding Lyα, all except two galaxies in our sample show at least one other rest-UV
    emission line, with C III] λ1907, λ1909 being the most prominent. We use multi-wavelength
    data available in the Hubble legacy fields to derive basic galaxy properties of
    our sample through spectral energy distribution fitting techniques. Taking advantage
    of the high-quality spectra obtained by MUSE (∼10 − 30 h of exposure time per
    pointing), we use photo-ionisation models to study the rest-UV emission line diagnostics
    of the He II λ1640 emitters. Line ratios of our sample can be reproduced by moderately
    sub-solar photo-ionisation models, however, we find that including effects of
    binary stars lead to degeneracies in most free parameters. Even after considering
    extra ionising photons produced by extreme sub-solar metallicity binary stellar
    models, photo-ionisation models are unable to reproduce rest-frame He II λ1640
    equivalent widths (∼0.2 − 10 Å), thus additional mechanisms are necessary in models
    to match the observed He II λ1640 properties.
acknowledgement: 'The authors wish to thank the referee for constructive comments
  that improved the paper substantially. We thank the BPASS team for making the stellar
  population models available. We thank Elizabeth Stanway, Claus Leitherer, Daniel
  Schaerer, Jorick Vink, and Nell Byler for insightful discussions. We thank the Lorentz
  Centre and the scientific organizers of the Characterizing galaxies with spectroscopy
  with a view for JWST workshop held at the Lorentz Centre in 2017 October, which
  promoted useful discussions in the wider community. TN, JB, and RB acknowledges
  the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) top grant TOP1.16.057.
  AF acknowledges support from the ERC via an Advanced Grant under grant agreement
  no. 339659-MUSICOS. JB acknowledges support by Fundação para a Ciência e a Tecnologia
  (FCT) through national funds (UID/FIS/04434/2013) and Investigador FCT contract
  IF/01654/2014/CP1215/CT0003, and by FEDER through COMPETE2020 (POCI-01-0145-FEDER-007672).
  JR acknowledges support from the ERC Starting grant 336736 (CALENDS). This research
  made use of astropy (http://www.astropy.org) a community-developed core Python package
  for Astronomy (Astropy Collaboration 2013, 2018) and pandas (McKinney 2010). Figures
  were generated using matplotlib (Hunter 2007) and seaborn (https://seaborn.pydata.org).
  Facilities: VLT (MUSE).'
article_number: A89
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Themiya
  full_name: Nanayakkara, Themiya
  last_name: Nanayakkara
- first_name: Jarle
  full_name: Brinchmann, Jarle
  last_name: Brinchmann
- first_name: Leindert
  full_name: Boogaard, Leindert
  last_name: Boogaard
- first_name: Rychard
  full_name: Bouwens, Rychard
  last_name: Bouwens
- first_name: Sebastiano
  full_name: Cantalupo, Sebastiano
  last_name: Cantalupo
- first_name: Anna
  full_name: Feltre, Anna
  last_name: Feltre
- first_name: Wolfram
  full_name: Kollatschny, Wolfram
  last_name: Kollatschny
- first_name: Raffaella Anna
  full_name: Marino, Raffaella Anna
  last_name: Marino
- first_name: Michael
  full_name: Maseda, Michael
  last_name: Maseda
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: Mieke
  full_name: Paalvast, Mieke
  last_name: Paalvast
- first_name: Johan
  full_name: Richard, Johan
  last_name: Richard
- first_name: Anne
  full_name: Verhamme, Anne
  last_name: Verhamme
citation:
  ama: Nanayakkara T, Brinchmann J, Boogaard L, et al. Exploring He II λ1640 emission
    line properties at z ∼2−4. <i>Astronomy &#38; Astrophysics</i>. 2019;648. doi:<a
    href="https://doi.org/10.1051/0004-6361/201834565">10.1051/0004-6361/201834565</a>
  apa: Nanayakkara, T., Brinchmann, J., Boogaard, L., Bouwens, R., Cantalupo, S.,
    Feltre, A., … Verhamme, A. (2019). Exploring He II λ1640 emission line properties
    at z ∼2−4. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/201834565">https://doi.org/10.1051/0004-6361/201834565</a>
  chicago: Nanayakkara, Themiya, Jarle Brinchmann, Leindert Boogaard, Rychard Bouwens,
    Sebastiano Cantalupo, Anna Feltre, Wolfram Kollatschny, et al. “Exploring He II Λ1640
    Emission Line Properties at z ∼2−4.” <i>Astronomy &#38; Astrophysics</i>. EDP
    Sciences, 2019. <a href="https://doi.org/10.1051/0004-6361/201834565">https://doi.org/10.1051/0004-6361/201834565</a>.
  ieee: T. Nanayakkara <i>et al.</i>, “Exploring He II λ1640 emission line properties
    at z ∼2−4,” <i>Astronomy &#38; Astrophysics</i>, vol. 648. EDP Sciences, 2019.
  ista: Nanayakkara T, Brinchmann J, Boogaard L, Bouwens R, Cantalupo S, Feltre A,
    Kollatschny W, Marino RA, Maseda M, Matthee JJ, Paalvast M, Richard J, Verhamme
    A. 2019. Exploring He II λ1640 emission line properties at z ∼2−4. Astronomy &#38;
    Astrophysics. 648, A89.
  mla: Nanayakkara, Themiya, et al. “Exploring He II Λ1640 Emission Line Properties
    at z ∼2−4.” <i>Astronomy &#38; Astrophysics</i>, vol. 648, A89, EDP Sciences,
    2019, doi:<a href="https://doi.org/10.1051/0004-6361/201834565">10.1051/0004-6361/201834565</a>.
  short: T. Nanayakkara, J. Brinchmann, L. Boogaard, R. Bouwens, S. Cantalupo, A.
    Feltre, W. Kollatschny, R.A. Marino, M. Maseda, J.J. Matthee, M. Paalvast, J.
    Richard, A. Verhamme, Astronomy &#38; Astrophysics 648 (2019).
date_created: 2022-07-06T09:07:06Z
date_published: 2019-04-16T00:00:00Z
date_updated: 2022-07-19T09:36:08Z
day: '16'
doi: 10.1051/0004-6361/201834565
extern: '1'
external_id:
  arxiv:
  - '1902.05960'
intvolume: '       648'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: ISM / galaxies: star formation / galaxies: evolution / galaxies: high-redshift'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1902.05960
month: '04'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
related_material:
  link:
  - relation: erratum
    url: https://doi.org/10.1051/0004-6361/201834565e
scopus_import: '1'
status: public
title: Exploring He II λ1640 emission line properties at z ∼2−4
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 648
year: '2019'
...
---
_id: '11507'
abstract:
- lang: eng
  text: 'Lyman-α (Lyα) is intrinsically the brightest line emitted from active galaxies.
    While it originates from many physical processes, for star-forming galaxies the
    intrinsic Lyα luminosity is a direct tracer of the Lyman-continuum (LyC) radiation
    produced by the most massive O- and early-type B-stars (M⋆ ≳ 10 M⊙) with lifetimes
    of a few Myrs. As such, Lyα luminosity should be an excellent instantaneous star
    formation rate (SFR) indicator. However, its resonant nature and susceptibility
    to dust as a rest-frame UV photon makes Lyα very hard to interpret due to the
    uncertain Lyα escape fraction, fesc, Lyα. Here we explore results from the CAlibrating
    LYMan-α with Hα (CALYMHA) survey at z = 2.2, follow-up of Lyα emitters (LAEs)
    at z = 2.2 − 2.6 and a z ∼ 0−0.3 compilation of LAEs to directly measure fesc, Lyα
    with Hα. We derive a simple empirical relation that robustly retrieves fesc, Lyα
    as a function of Lyα rest-frame EW (EW0): fesc,Lyα = 0.0048 EW0[Å] ± 0.05 and
    we show that it constrains a well-defined anti-correlation between ionisation
    efficiency (ξion) and dust extinction in LAEs. Observed Lyα luminosities and EW0
    are easy measurable quantities at high redshift, thus making our relation a practical
    tool to estimate intrinsic Lyα and LyC luminosities under well controlled and
    simple assumptions. Our results allow observed Lyα luminosities to be used to
    compute SFRs for LAEs at z ∼ 0−2.6 within ±0.2 dex of the Hα dust corrected SFRs.
    We apply our empirical SFR(Lyα,EW0) calibration to several sources at z ≥ 2.6
    to find that star-forming LAEs have SFRs typically ranging from 0.1 to 20 M⊙ yr−1
    and that our calibration might be even applicable for the most luminous LAEs within
    the epoch of re-ionisation. Our results imply high ionisation efficiencies (log10[ξion/Hz erg−1]
    = 25.4−25.6) and low dust content in LAEs across cosmic time, and will be easily
    tested with future observations with JWST which can obtain Hα and Hβ measurements
    for high-redshift LAEs.'
acknowledgement: We thank the anonymous referees for multiple comments and suggestions
  which have improved the manuscript. JM acknowledges the support of a Huygens PhD
  fellowship from Leiden University. We have benefited greatly from the publicly available
  programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt et al. 2011;
  Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration
  2013) packages, and the TOPCAT analysis program (Taylor 2013). The results and samples
  of LAEs used for this paper are publicly available (see e.g. Sobral et al. 2017,
  2018a) and we also provide the toy model used as a PYTHON script.
article_number: A157
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
citation:
  ama: 'Sobral D, Matthee JJ. Predicting Lyα escape fractions with a simple observable:
    Lyα in emission as an empirically calibrated star formation rate indicator. <i>Astronomy
    &#38; Astrophysics</i>. 2019;623. doi:<a href="https://doi.org/10.1051/0004-6361/201833075">10.1051/0004-6361/201833075</a>'
  apa: 'Sobral, D., &#38; Matthee, J. J. (2019). Predicting Lyα escape fractions with
    a simple observable: Lyα in emission as an empirically calibrated star formation
    rate indicator. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href="https://doi.org/10.1051/0004-6361/201833075">https://doi.org/10.1051/0004-6361/201833075</a>'
  chicago: 'Sobral, David, and Jorryt J Matthee. “Predicting Lyα Escape Fractions
    with a Simple Observable: Lyα in Emission as an Empirically Calibrated Star Formation
    Rate Indicator.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href="https://doi.org/10.1051/0004-6361/201833075">https://doi.org/10.1051/0004-6361/201833075</a>.'
  ieee: 'D. Sobral and J. J. Matthee, “Predicting Lyα escape fractions with a simple
    observable: Lyα in emission as an empirically calibrated star formation rate indicator,”
    <i>Astronomy &#38; Astrophysics</i>, vol. 623. EDP Sciences, 2019.'
  ista: 'Sobral D, Matthee JJ. 2019. Predicting Lyα escape fractions with a simple
    observable: Lyα in emission as an empirically calibrated star formation rate indicator.
    Astronomy &#38; Astrophysics. 623, A157.'
  mla: 'Sobral, David, and Jorryt J. Matthee. “Predicting Lyα Escape Fractions with
    a Simple Observable: Lyα in Emission as an Empirically Calibrated Star Formation
    Rate Indicator.” <i>Astronomy &#38; Astrophysics</i>, vol. 623, A157, EDP Sciences,
    2019, doi:<a href="https://doi.org/10.1051/0004-6361/201833075">10.1051/0004-6361/201833075</a>.'
  short: D. Sobral, J.J. Matthee, Astronomy &#38; Astrophysics 623 (2019).
date_created: 2022-07-06T11:08:16Z
date_published: 2019-03-26T00:00:00Z
date_updated: 2022-07-19T09:37:20Z
day: '26'
doi: 10.1051/0004-6361/201833075
extern: '1'
external_id:
  arxiv:
  - '1803.08923'
intvolume: '       623'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / galaxies: star formation / galaxies: statistics / galaxies:
  evolution / galaxies: formation / galaxies: ISM'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1803.08923
month: '03'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
  eissn:
  - 1432-0746
  issn:
  - 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Predicting Lyα escape fractions with a simple observable: Lyα in emission
  as an empirically calibrated star formation rate indicator'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 623
year: '2019'
...
---
_id: '11535'
abstract:
- lang: eng
  text: We investigate the clustering and halo properties of ∼5000 Ly α-selected emission-line
    galaxies (LAEs) from the Slicing COSMOS 4K (SC4K) and from archival NB497 imaging
    of SA22 split in 15 discrete redshift slices between z ∼ 2.5 and 6. We measure
    clustering lengths of r0 ∼ 3–6 h−1 Mpc and typical halo masses of ∼1011 M⊙ for
    our narrowband-selected LAEs with typical LLy α ∼ 1042–43 erg s−1. The intermediate-band-selected
    LAEs are observed to have r0 ∼ 3.5–15 h−1 Mpc with typical halo masses of ∼1011–12
    M⊙ and typical LLy α ∼ 1043–43.6 erg s−1. We find a strong, redshift-independent
    correlation between halo mass and Ly α luminosity normalized by the characteristic
    Ly α luminosity, L⋆(z). The faintest LAEs (L ∼ 0.1 L⋆(z)) typically identified
    by deep narrowband surveys are found in 1010 M⊙ haloes and the brightest LAEs
    (L ∼ 7 L⋆(z)) are found in ∼5 × 1012 M⊙ haloes. A dependency on the rest-frame
    1500 Å UV luminosity, MUV, is also observed where the halo masses increase from
    1011 to 1013 M⊙ for MUV ∼ −19 to −23.5 mag. Halo mass is also observed to increase
    from 109.8 to 1012 M⊙ for dust-corrected UV star formation rates from ∼0.6 to
    10 M⊙ yr−1 and continues to increase up to 1013 M⊙ in halo mass, where the majority
    of those sources are active galactic nuclei. All the trends we observe are found
    to be redshift independent. Our results reveal that LAEs are the likely progenitors
    of a wide range of galaxies depending on their luminosity, from dwarf-like, to
    Milky Way-type, to bright cluster galaxies. LAEs therefore provide unique insight
    into the early formation and evolution of the galaxies we observe in the local
    Universe.
acknowledgement: We thank the anonymous referee for their useful comments and suggestions
  that helped improve this study. AAK acknowledges that this work was supported by
  NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant
  NNX16AO92H. JM acknowledges support from the ETH Zwicky fellowship. RKC acknowledges
  funding from STFC via a studentship. APA acknowledges support from the Fundac¸ao
  para a Ci ˜ encia e a Tecnologia FCT through the fellowship PD/BD/52706/2014 and
  the research grant UID/FIS/04434/2013. JC and SS both acknowledge their support
  from the Lancaster University PhD Fellowship. We have benefited greatly from the
  publicly available programming language PYTHON, including the NUMPY, SCIPY, MATPLOTLIB,
  SCIKIT-LEARN, and ASTROPY packages, as well as the TOPCAT analysis program. The
  SC4K samples used in this paper are all publicly available for use by the community
  (Sobral et al. 2018a). The catalogue is also available on the COSMOS IPAC website
  (https://irsa.ipac.caltech.edu/data/COSMOS/overview.html).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: A A
  full_name: Khostovan, A A
  last_name: Khostovan
- first_name: D
  full_name: Sobral, D
  last_name: Sobral
- first_name: B
  full_name: Mobasher, B
  last_name: Mobasher
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: R K
  full_name: Cochrane, R K
  last_name: Cochrane
- first_name: N
  full_name: Chartab, N
  last_name: Chartab
- first_name: M
  full_name: Jafariyazani, M
  last_name: Jafariyazani
- first_name: A
  full_name: Paulino-Afonso, A
  last_name: Paulino-Afonso
- first_name: S
  full_name: Santos, S
  last_name: Santos
- first_name: J
  full_name: Calhau, J
  last_name: Calhau
citation:
  ama: 'Khostovan AA, Sobral D, Mobasher B, et al. The clustering of typical Ly α emitters
    from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2019;489(1):555-573. doi:<a href="https://doi.org/10.1093/mnras/stz2149">10.1093/mnras/stz2149</a>'
  apa: 'Khostovan, A. A., Sobral, D., Mobasher, B., Matthee, J. J., Cochrane, R. K.,
    Chartab, N., … Calhau, J. (2019). The clustering of typical Ly α emitters from
    z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. <i>Monthly Notices
    of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stz2149">https://doi.org/10.1093/mnras/stz2149</a>'
  chicago: 'Khostovan, A A, D Sobral, B Mobasher, Jorryt J Matthee, R K Cochrane,
    N Chartab, M Jafariyazani, A Paulino-Afonso, S Santos, and J Calhau. “The Clustering
    of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV
    Luminosities.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford
    University Press, 2019. <a href="https://doi.org/10.1093/mnras/stz2149">https://doi.org/10.1093/mnras/stz2149</a>.'
  ieee: 'A. A. Khostovan <i>et al.</i>, “The clustering of typical Ly α emitters from
    z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities,” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 489, no. 1. Oxford University Press,
    pp. 555–573, 2019.'
  ista: 'Khostovan AA, Sobral D, Mobasher B, Matthee JJ, Cochrane RK, Chartab N, Jafariyazani
    M, Paulino-Afonso A, Santos S, Calhau J. 2019. The clustering of typical Ly α emitters
    from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices
    of the Royal Astronomical Society. 489(1), 555–573.'
  mla: 'Khostovan, A. A., et al. “The Clustering of Typical Ly α Emitters from z ∼
    2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 489, no. 1, Oxford University Press,
    2019, pp. 555–73, doi:<a href="https://doi.org/10.1093/mnras/stz2149">10.1093/mnras/stz2149</a>.'
  short: A.A. Khostovan, D. Sobral, B. Mobasher, J.J. Matthee, R.K. Cochrane, N. Chartab,
    M. Jafariyazani, A. Paulino-Afonso, S. Santos, J. Calhau, Monthly Notices of the
    Royal Astronomical Society 489 (2019) 555–573.
date_created: 2022-07-07T13:01:03Z
date_published: 2019-10-01T00:00:00Z
date_updated: 2022-08-19T06:38:42Z
day: '01'
doi: 10.1093/mnras/stz2149
extern: '1'
external_id:
  arxiv:
  - '1811.00556'
intvolume: '       489'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: haloes'
- 'galaxies: high-redshift'
- 'galaxies: star formation'
- 'cosmology: observations'
- large-scale structure of Universe
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1811.00556
month: '10'
oa: 1
oa_version: Preprint
page: 555-573
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend
  on Ly α and UV luminosities'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 489
year: '2019'
...
---
_id: '11540'
abstract:
- lang: eng
  text: Observations have revealed that the star formation rate (SFR) and stellar
    mass (Mstar) of star-forming galaxies follow a tight relation known as the galaxy
    main sequence. However, what physical information is encoded in this relation
    is under debate. Here, we use the EAGLE cosmological hydrodynamical simulation
    to study the mass dependence, evolution, and origin of scatter in the SFR–Mstar
    relation. At z = 0, we find that the scatter decreases slightly with stellar mass
    from 0.35 dex at Mstar ≈ 109 M⊙ to 0.30 dex at Mstar ≳ 1010.5 M⊙. The scatter
    decreases from z = 0 to z = 5 by 0.05 dex at Mstar ≳ 1010 M⊙ and by 0.15 dex for
    lower masses. We show that the scatter at z = 0.1 originates from a combination
    of fluctuations on short time-scales (ranging from 0.2–2 Gyr) that are presumably
    associated with self-regulation from cooling, star formation, and outflows, but
    is dominated by long time-scale (∼10 Gyr) variations related to differences in
    halo formation times. Shorter time-scale fluctuations are relatively more important
    for lower mass galaxies. At high masses, differences in black hole formation efficiency
    cause additional scatter, but also diminish the scatter caused by different halo
    formation times. While individual galaxies cross the main sequence multiple times
    during their evolution, they fluctuate around tracks associated with their halo
    properties, i.e. galaxies above/below the main sequence at z = 0.1 tend to have
    been above/below the main sequence for ≫1 Gyr.
acknowledgement: JM acknowledges the support of a Huygens PhD fellowship from Leiden
  University. We thank Camila Correa for help analysing snipshot merger trees. We
  thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann,
  Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and
  suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade
  of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and
  ideas. We have benefited from the public available programming language PYTHON,
  including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT
  analysis tool (Taylor 2013).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: Joop
  full_name: Schaye, Joop
  last_name: Schaye
citation:
  ama: Matthee JJ, Schaye J. The origin of scatter in the star formation rate–stellar
    mass relation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;484(1):915-932.
    doi:<a href="https://doi.org/10.1093/mnras/stz030">10.1093/mnras/stz030</a>
  apa: Matthee, J. J., &#38; Schaye, J. (2019). The origin of scatter in the star
    formation rate–stellar mass relation. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stz030">https://doi.org/10.1093/mnras/stz030</a>
  chicago: Matthee, Jorryt J, and Joop Schaye. “The Origin of Scatter in the Star
    Formation Rate–Stellar Mass Relation.” <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press, 2019. <a href="https://doi.org/10.1093/mnras/stz030">https://doi.org/10.1093/mnras/stz030</a>.
  ieee: J. J. Matthee and J. Schaye, “The origin of scatter in the star formation
    rate–stellar mass relation,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 484, no. 1. Oxford University Press, pp. 915–932, 2019.
  ista: Matthee JJ, Schaye J. 2019. The origin of scatter in the star formation rate–stellar
    mass relation. Monthly Notices of the Royal Astronomical Society. 484(1), 915–932.
  mla: Matthee, Jorryt J., and Joop Schaye. “The Origin of Scatter in the Star Formation
    Rate–Stellar Mass Relation.” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 484, no. 1, Oxford University Press, 2019, pp. 915–32, doi:<a href="https://doi.org/10.1093/mnras/stz030">10.1093/mnras/stz030</a>.
  short: J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society
    484 (2019) 915–932.
date_created: 2022-07-08T07:48:31Z
date_published: 2019-03-01T00:00:00Z
date_updated: 2022-08-19T06:42:43Z
day: '01'
doi: 10.1093/mnras/stz030
extern: '1'
external_id:
  arxiv:
  - '1805.05956'
intvolume: '       484'
issue: '1'
keyword:
- Space and Planetary Science
- 'Astronomy and Astrophysics : galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: star formation'
- 'cosmology: theory'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1805.05956
month: '03'
oa: 1
oa_version: Preprint
page: 915-932
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The origin of scatter in the star formation rate–stellar mass relation
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 484
year: '2019'
...
---
_id: '11549'
abstract:
- lang: eng
  text: We investigate the clustering properties of ∼7000 H β + [O III] and [O II]
    narrowband-selected emitters at z ∼ 0.8–4.7 from the High-z Emission Line Survey.
    We find clustering lengths, r0, of 1.5–4.0 h−1 Mpc and minimum dark matter halo
    masses of 1010.7–12.1 M⊙ for our z = 0.8–3.2 H β + [O III] emitters and r0 ∼ 2.0–8.3
    h−1 Mpc and halo masses of 1011.5–12.6 M⊙ for our z = 1.5–4.7 [O II] emitters.
    We find r0 to strongly increase both with increasing line luminosity and redshift.
    By taking into account the evolution of the characteristic line luminosity, L⋆(z),
    and using our model predictions of halo mass given r0, we find a strong, redshift-independent
    increasing trend between L/L⋆(z) and minimum halo mass. The faintest H β + [O III]
    emitters are found to reside in 109.5 M⊙ haloes and the brightest emitters in
    1013.0 M⊙ haloes. For [O II] emitters, the faintest emitters are found in 1010.5
    M⊙ haloes and the brightest emitters in 1012.6 M⊙ haloes. A redshift-independent
    stellar mass dependency is also observed where the halo mass increases from 1011
    to 1012.5 M⊙ for stellar masses of 108.5 to 1011.5 M⊙, respectively. We investigate
    the interdependencies of these trends by repeating our analysis in a Lline−Mstar
    grid space for our most populated samples (H β + [O III] z = 0.84 and [O II] z
    = 1.47) and find that the line luminosity dependency is stronger than the stellar
    mass dependency on halo mass. For L > L⋆ emitters at all epochs, we find a relatively
    flat trend with halo masses of 1012.5–13 M⊙, which may be due to quenching mechanisms
    in massive haloes that is consistent with a transitional halo mass predicted by
    models.
acknowledgement: We thank the anonymous referee for their useful comments and suggestions
  that improved this study. AAK thanks Anahita Alavi and Irene Shivaei for useful
  discussion in the making of this paper. AAK acknowledges that this work was supported
  by NASA Headquarters under the NASA Earth and Space Science Fellowship Program –
  Grant NNX16AO92H. DS acknowledges financial support from the Netherlands Organization
  for Scientific Research (NWO) through a Veni fellowship and from Lancaster University
  through an Early Career Internal Grant A100679. PNB is grateful for support from
  STFC via grant STM001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the
  ERC Advanced Grant DUSTYGAL (321334), and a Royal Society/Wolfson Merit award. JM
  acknowledges the support of a Huygens PhD fellowship from Leiden University. BD
  acknowledges financial support from NASA through the Astrophysics Data Analysis
  Program (ADAP), grant number NNX12AE20G.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: A A
  full_name: Khostovan, A A
  last_name: Khostovan
- first_name: D
  full_name: Sobral, D
  last_name: Sobral
- first_name: B
  full_name: Mobasher, B
  last_name: Mobasher
- first_name: P N
  full_name: Best, P N
  last_name: Best
- first_name: I
  full_name: Smail, I
  last_name: Smail
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: B
  full_name: Darvish, B
  last_name: Darvish
- first_name: H
  full_name: Nayyeri, H
  last_name: Nayyeri
- first_name: S
  full_name: Hemmati, S
  last_name: Hemmati
- first_name: J P
  full_name: Stott, J P
  last_name: Stott
citation:
  ama: 'Khostovan AA, Sobral D, Mobasher B, et al. The clustering of H β + [O III]
    and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar
    mass. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;478(3):2999-3015.
    doi:<a href="https://doi.org/10.1093/mnras/sty925">10.1093/mnras/sty925</a>'
  apa: 'Khostovan, A. A., Sobral, D., Mobasher, B., Best, P. N., Smail, I., Matthee,
    J. J., … Stott, J. P. (2018). The clustering of H β + [O III] and [O II] emitters
    since z ∼ 5: Dependencies with line luminosity and stellar mass. <i>Monthly Notices
    of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/sty925">https://doi.org/10.1093/mnras/sty925</a>'
  chicago: 'Khostovan, A A, D Sobral, B Mobasher, P N Best, I Smail, Jorryt J Matthee,
    B Darvish, H Nayyeri, S Hemmati, and J P Stott. “The Clustering of H β + [O III]
    and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar
    Mass.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University
    Press, 2018. <a href="https://doi.org/10.1093/mnras/sty925">https://doi.org/10.1093/mnras/sty925</a>.'
  ieee: 'A. A. Khostovan <i>et al.</i>, “The clustering of H β + [O III] and [O II]
    emitters since z ∼ 5: Dependencies with line luminosity and stellar mass,” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 478, no. 3. Oxford University
    Press, pp. 2999–3015, 2018.'
  ista: 'Khostovan AA, Sobral D, Mobasher B, Best PN, Smail I, Matthee JJ, Darvish
    B, Nayyeri H, Hemmati S, Stott JP. 2018. The clustering of H β + [O III] and [O II]
    emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly
    Notices of the Royal Astronomical Society. 478(3), 2999–3015.'
  mla: 'Khostovan, A. A., et al. “The Clustering of H β + [O III] and [O II] Emitters
    since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 478, no. 3, Oxford University Press,
    2018, pp. 2999–3015, doi:<a href="https://doi.org/10.1093/mnras/sty925">10.1093/mnras/sty925</a>.'
  short: A.A. Khostovan, D. Sobral, B. Mobasher, P.N. Best, I. Smail, J.J. Matthee,
    B. Darvish, H. Nayyeri, S. Hemmati, J.P. Stott, Monthly Notices of the Royal Astronomical
    Society 478 (2018) 2999–3015.
date_created: 2022-07-08T11:48:48Z
date_published: 2018-08-01T00:00:00Z
date_updated: 2022-08-19T06:53:39Z
day: '01'
doi: 10.1093/mnras/sty925
extern: '1'
external_id:
  arxiv:
  - '1705.01101'
intvolume: '       478'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: haloes'
- 'galaxies: high-redshift'
- 'galaxies: star formation'
- 'cosmology: observations'
- large-scale structure of Universe
language:
- iso: eng
main_file_link:
- url: https://arxiv.org/abs/1705.01101
month: '08'
oa_version: Published Version
page: 2999-3015
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies
  with line luminosity and stellar mass'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 478
year: '2018'
...
---
_id: '11584'
abstract:
- lang: eng
  text: Observations show that star-forming galaxies reside on a tight 3D plane between
    mass, gas-phase metallicity, and star formation rate (SFR), which can be explained
    by the interplay between metal-poor gas inflows, SFR and outflows. However, different
    metals are released on different time-scales, which may affect the slope of this
    relation. Here, we use central, star-forming galaxies with Mstar = 109.0–10.5
    M⊙ from the EAGLE hydrodynamical simulation to examine 3D relations between mass,
    SFR, and chemical enrichment using absolute and relative C, N, O, and Fe abundances.
    We show that the scatter is smaller when gas-phase α-enhancement is used rather
    than metallicity. A similar plane also exists for stellar α-enhancement, implying
    that present-day specific SFRs are correlated with long time-scale star formation
    histories. Between z = 0 and 1, the α-enhancement plane is even more insensitive
    to redshift than the plane using metallicity. However, it evolves at z > 1 due
    to lagging iron yields. At fixed mass, galaxies with higher SFRs have star formation
    histories shifted towards late times, are more α-enhanced, and this α-enhancement
    increases with redshift as observed. These findings suggest that relations between
    physical properties inferred from observations may be affected by systematic variations
    in α-enhancements.
acknowledgement: We thank the anonymous referee for their constructive comments. JM
  acknowledges the support of a Huygens PhD fellowship from Leiden University. We
  thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge
  the use of the TOPCAT software (Taylor 2013) for assisting in rapid exploration
  of multidimensional data sets and the use of PYTHON and its NUMPY, MATPLOTLIB, and
  PANDAS packages.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: Joop
  full_name: Schaye, Joop
  last_name: Schaye
citation:
  ama: 'Matthee JJ, Schaye J. Star-forming galaxies are predicted to lie on a fundamental
    plane of mass, star formation rate, and α-enhancement. <i>Monthly Notices of the
    Royal Astronomical Society: Letters</i>. 2018;479(1):L34-L39. doi:<a href="https://doi.org/10.1093/mnrasl/sly093">10.1093/mnrasl/sly093</a>'
  apa: 'Matthee, J. J., &#38; Schaye, J. (2018). Star-forming galaxies are predicted
    to lie on a fundamental plane of mass, star formation rate, and α-enhancement.
    <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University
    Press. <a href="https://doi.org/10.1093/mnrasl/sly093">https://doi.org/10.1093/mnrasl/sly093</a>'
  chicago: 'Matthee, Jorryt J, and Joop Schaye. “Star-Forming Galaxies Are Predicted
    to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.”
    <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University
    Press, 2018. <a href="https://doi.org/10.1093/mnrasl/sly093">https://doi.org/10.1093/mnrasl/sly093</a>.'
  ieee: 'J. J. Matthee and J. Schaye, “Star-forming galaxies are predicted to lie
    on a fundamental plane of mass, star formation rate, and α-enhancement,” <i>Monthly
    Notices of the Royal Astronomical Society: Letters</i>, vol. 479, no. 1. Oxford
    University Press, pp. L34–L39, 2018.'
  ista: 'Matthee JJ, Schaye J. 2018. Star-forming galaxies are predicted to lie on
    a fundamental plane of mass, star formation rate, and α-enhancement. Monthly Notices
    of the Royal Astronomical Society: Letters. 479(1), L34–L39.'
  mla: 'Matthee, Jorryt J., and Joop Schaye. “Star-Forming Galaxies Are Predicted
    to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.”
    <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 479, no.
    1, Oxford University Press, 2018, pp. L34–39, doi:<a href="https://doi.org/10.1093/mnrasl/sly093">10.1093/mnrasl/sly093</a>.'
  short: 'J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society:
    Letters 479 (2018) L34–L39.'
date_created: 2022-07-14T12:49:47Z
date_published: 2018-09-01T00:00:00Z
date_updated: 2022-08-19T08:35:45Z
day: '01'
doi: 10.1093/mnrasl/sly093
extern: '1'
external_id:
  arxiv:
  - '1802.06786'
intvolume: '       479'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: abundances'
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: star formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1802.06786
month: '09'
oa: 1
oa_version: Preprint
page: L34 - L39
publication: 'Monthly Notices of the Royal Astronomical Society: Letters'
publication_identifier:
  eissn:
  - 1745-3933
  issn:
  - 1745-3925
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Star-forming galaxies are predicted to lie on a fundamental plane of mass,
  star formation rate, and α-enhancement
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 479
year: '2018'
...
---
_id: '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: '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'
...