---
_id: '11503'
abstract:
- lang: eng
text: "Context. The Lyα emitter (LAE) fraction, XLAE, is a potentially powerful
probe of the evolution of the intergalactic neutral hydrogen gas fraction. However,
uncertainties in the measurement of XLAE are still under debate.\r\nAims. Thanks
to deep data obtained with the integral field spectrograph Multi Unit Spectroscopic
Explorer (MUSE), we can measure the evolution of the LAE fraction homogeneously
over a wide redshift range of z ≈ 3–6 for UV-faint galaxies (down to UV magnitudes
of M1500 ≈ −17.75). This is a significantly fainter range than in former studies
(M1500 ≤ −18.75) and it allows us to probe the bulk of the population of high-redshift
star-forming galaxies.\r\nMethods. We constructed a UV-complete photometric-redshift
sample following UV luminosity functions and measured the Lyα emission with MUSE
using the latest (second) data release from the MUSE Hubble Ultra Deep Field Survey.\r\nResults.
We derived the redshift evolution of XLAE for M1500 ∈ [ − 21.75; −17.75] for the
first time with a equivalent width range EW(Lyα) ≥ 65 Å and found low values of
XLAE ≲ 30% at z ≲ 6. The best-fit linear relation is XLAE = 0.07+0.06−0.03z −
0.22+0.12−0.24. For M1500 ∈ [ − 20.25; −18.75] and EW(Lyα) ≥ 25 Å, our XLAE values
are consistent with those in the literature within 1σ at z ≲ 5, but our median
values are systematically lower than reported values over the whole redshift range.
In addition, we do not find a significant dependence of XLAE on M1500 for EW(Lyα)
≥ 50 Å at z ≈ 3–4, in contrast with previous work. The differences in XLAE mainly
arise from selection biases for Lyman Break Galaxies (LBGs) in the literature:
UV-faint LBGs are more easily selected if they have strong Lyα emission, hence
XLAE is biased towards higher values when those samples are used.\r\nConclusions.
Our results suggest either a lower increase of XLAE towards z ≈ 6 than previously
suggested, or even a turnover of XLAE at z ≈ 5.5, which may be the signature of
a late or patchy reionization process. We compared our results with predictions
from a cosmological galaxy evolution model. We find that a model with a bursty
star formation (SF) can reproduce our observed LAE fractions much better than
models where SF is a smooth function of time."
acknowledgement: We thank the anonymous referee for constructive comments and suggestions.
We would like to express our gratitude to Stephane De Barros and Pablo Arrabal Haro
for kindly providing their data plotted in Figs. 1, 2, and 8. We are grateful to
Kazuhiro Shimasaku, Masami Ouchi, Rieko Momose, Daniel Schaerer, Hidenobu Yajima,
Taku Okamura, Makoto Ando, and Hinako Goto for giving insightful comments and suggestions.
This work is based on observations taken by VLT, which is operated by European Southern
Observatory. This research made use of Astropy (http://www.astropy.org), which is
a community-developed core Python package for Astronomy (Astropy Collaboration 2013,
2018), MARZ, MPDAF, and matplotlib (Hunter 2007). H.K. acknowledges support from
Japan Society for the Promotion of Science (JSPS) through the JSPS Research Fellowship
for Young Scientists and Overseas Challenge Program for Young Researchers. AV acknowledges
support from the ERC starting grant 757258-TRIPLE and the SNF Professorship 176808-TRIPLE.
This work was supported by the project FOGHAR (Agence Nationale de la Recherche,
ANR-13-BS05-0010-02). JB acknowledges support from the ORAGE project from the Agence
Nationale de la Recherche under grant ANR-14-CE33-0016-03. JR acknowledges support
from the ERC starting grant 336736-CALENDS. T. H. acknowledges supports by the Grant-inAid
for Scientic Research 19J01620.
article_number: A12
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- first_name: Jérémy
full_name: Blaizot, Jérémy
last_name: Blaizot
- first_name: Thibault
full_name: Garel, Thibault
last_name: Garel
- first_name: Anne
full_name: Verhamme, Anne
last_name: Verhamme
- first_name: Roland
full_name: Bacon, Roland
last_name: Bacon
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Takuya
full_name: Hashimoto, Takuya
last_name: Hashimoto
- first_name: Hanae
full_name: Inami, Hanae
last_name: Inami
- first_name: Simon
full_name: Conseil, Simon
last_name: Conseil
- first_name: Bruno
full_name: Guiderdoni, Bruno
last_name: Guiderdoni
- first_name: Alyssa B.
full_name: Drake, Alyssa B.
last_name: Drake
- first_name: Edmund
full_name: Christian Herenz, Edmund
last_name: Christian Herenz
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Pascal
full_name: Oesch, Pascal
last_name: Oesch
- 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: Raffaella
full_name: Anna Marino, Raffaella
last_name: Anna Marino
- first_name: Kasper
full_name: Borello Schmidt, Kasper
last_name: Borello Schmidt
- first_name: Roser
full_name: Pelló, Roser
last_name: Pelló
- first_name: Michael
full_name: Maseda, Michael
last_name: Maseda
- first_name: Floriane
full_name: Leclercq, Floriane
last_name: Leclercq
- first_name: Josephine
full_name: Kerutt, Josephine
last_name: Kerutt
- first_name: Guillaume
full_name: Mahler, Guillaume
last_name: Mahler
citation:
ama: 'Kusakabe H, Blaizot J, Garel T, et al. The MUSE Hubble Ultra Deep Field Survey:
XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy &
Astrophysics. 2020;638. doi:10.1051/0004-6361/201937340'
apa: 'Kusakabe, H., Blaizot, J., Garel, T., Verhamme, A., Bacon, R., Richard, J.,
… Mahler, G. (2020). The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of
the Lyα emitter fraction from z = 3 to z = 6. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/201937340'
chicago: 'Kusakabe, Haruka, Jérémy Blaizot, Thibault Garel, Anne Verhamme, Roland
Bacon, Johan Richard, Takuya Hashimoto, et al. “The MUSE Hubble Ultra Deep Field
Survey: XIV. Evolution of the Lyα Emitter Fraction from z = 3 to z = 6.” Astronomy
& Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/201937340.'
ieee: 'H. Kusakabe et al., “The MUSE Hubble Ultra Deep Field Survey: XIV.
Evolution of the Lyα emitter fraction from z = 3 to z = 6,” Astronomy &
Astrophysics, vol. 638. EDP Sciences, 2020.'
ista: 'Kusakabe H, Blaizot J, Garel T, Verhamme A, Bacon R, Richard J, Hashimoto
T, Inami H, Conseil S, Guiderdoni B, Drake AB, Christian Herenz E, Schaye J, Oesch
P, Matthee JJ, Anna Marino R, Borello Schmidt K, Pelló R, Maseda M, Leclercq F,
Kerutt J, Mahler G. 2020. The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution
of the Lyα emitter fraction from z = 3 to z = 6. Astronomy & Astrophysics.
638, A12.'
mla: 'Kusakabe, Haruka, et al. “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution
of the Lyα Emitter Fraction from z = 3 to z = 6.” Astronomy & Astrophysics,
vol. 638, A12, EDP Sciences, 2020, doi:10.1051/0004-6361/201937340.'
short: H. Kusakabe, J. Blaizot, T. Garel, A. Verhamme, R. Bacon, J. Richard, T.
Hashimoto, H. Inami, S. Conseil, B. Guiderdoni, A.B. Drake, E. Christian Herenz,
J. Schaye, P. Oesch, J.J. Matthee, R. Anna Marino, K. Borello Schmidt, R. Pelló,
M. Maseda, F. Leclercq, J. Kerutt, G. Mahler, Astronomy & Astrophysics 638
(2020).
date_created: 2022-07-06T09:50:48Z
date_published: 2020-06-03T00:00:00Z
date_updated: 2022-07-19T09:35:20Z
day: '03'
doi: 10.1051/0004-6361/201937340
extern: '1'
external_id:
arxiv:
- '2003.12083'
intvolume: ' 638'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'dark ages / reionization / first stars / early Universe / cosmology: observations
/ galaxies: evolution / galaxies: high-redshift / intergalactic medium'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2003.12083
month: '06'
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: 'The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter
fraction from z = 3 to z = 6'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 638
year: '2020'
...
---
_id: '11541'
abstract:
- lang: eng
text: We present new Hubble Space Telescope (HST)/WFC3 observations and re-analyse
VLT data to unveil the continuum, variability, and rest-frame ultraviolet (UV)
lines of the multiple UV clumps of the most luminous Lyα emitter at z = 6.6, CR7
(COSMOS Redshift 7). Our re-reduced, flux-calibrated X-SHOOTER spectra of CR7
reveal an He II emission line in observations obtained along the major axis of
Lyα emission with the best seeing conditions. He II is spatially offset by ≈+0.8
arcsec from the peak of Lyα emission, and it is found towards clump B. Our WFC3
grism spectra detects the UV continuum of CR7’s clump A, yielding a power law
with β=−2.5+0.6−0.7 and MUV=−21.87+0.25−0.20. No significant variability is found
for any of the UV clumps on their own, but there is tentative (≈2.2 σ) brightening
of CR7 in F110W as a whole from 2012 to 2017. HST grism data fail to robustly
detect rest-frame UV lines in any of the clumps, implying fluxes ≲2×10−17 erg s−1 cm−2
(3σ). We perform CLOUDY modelling to constrain the metallicity and the ionizing
nature of CR7. CR7 seems to be actively forming stars without any clear active
galactic nucleus activity in clump A, consistent with a metallicity of ∼0.05–0.2 Z⊙.
Component C or an interclump component between B and C may host a high ionization
source. Our results highlight the need for spatially resolved information to study
the formation and assembly of early galaxies.
acknowledgement: We thank the anonymous reviewer for the numerous detailed comments
that led us to greatly improve the quality, extent, and statistical robustness of
this work. DS acknowledges financial support from the Netherlands Organisation for
Scientific research through a Veni fellowship. JM acknowledges the support of a
Huygens PhD fellowship from Leiden University. AF acknowledges support from the
ERC Advanced Grant INTERSTELLAR H2020/740120. BD acknowledges financial support
from NASA through the Astrophysics Data Analysis Program, grant number NNX12AE20G
and the National Science Foundation, grant number 1716907. We are thankful for several
discussions and constructive comments from Johannes Zabl, Eros Vanzella, Bo Milvang-Jensen,
Henry McCracken, Max Gronke, Mark Dijkstra, Richard Ellis, and Nicolas Laporte.
We also thank Umar Burhanudin and Izzy Garland for taking part in the XGAL internship
in Lancaster and for exploring the HST grism data independently. Based on observations
obtained with HST/WFC3 programs 12578, 14495, and 14596. Based on observations of
the National Japanese Observatory with the Suprime-Cam on the Subaru telescope (S14A-086)
on the big island of Hawaii. This work is based in part on data products produced
at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France–Hawaii
Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on data
products from observations made with ESO Telescopes at the La Silla Paranal Observatory
under ESO programme IDs 294.A-5018, 294.A-5039, 092.A 0786, 093.A-0561, 097.A0043,
097.A-0943, 098.A-0819, 298.A-5012, and 179.A-2005, and on data products produced
by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.
The authors acknowledge the award of service time (SW2014b20) on the William Herschel
Telescope (WHT). WHT and its service programme are operated on the island of La
Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos
of the Instituto de Astrofisica de Canarias. This research was supported by the
Munich Institute for Astro- and Particle Physics of the DFG cluster of excellence
‘Origin and Structure of the Universe’. We have benefitted immensely from the public
available programming language PYTHON, including NUMPY and SCIPY (Jones et al. 2001;
Van Der Walt, Colbert & Varoquaux 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy
Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This
research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France.
All data used for this paper are publicly available, and we make all reduced data
available with the refereed paper.
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: Gabriel
full_name: Brammer, Gabriel
last_name: Brammer
- first_name: Andrea
full_name: Ferrara, Andrea
last_name: Ferrara
- first_name: Lara
full_name: Alegre, Lara
last_name: Alegre
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
- first_name: Daniel
full_name: Schaerer, Daniel
last_name: Schaerer
- first_name: Bahram
full_name: Mobasher, Bahram
last_name: Mobasher
- first_name: Behnam
full_name: Darvish, Behnam
last_name: Darvish
citation:
ama: Sobral D, Matthee JJ, Brammer G, et al. On the nature and physical conditions
of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly
Notices of the Royal Astronomical Society. 2019;482(2):2422-2441. doi:10.1093/mnras/sty2779
apa: Sobral, D., Matthee, J. J., Brammer, G., Ferrara, A., Alegre, L., Röttgering,
H., … Darvish, B. (2019). On the nature and physical conditions of the luminous
Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal
Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty2779
chicago: Sobral, David, Jorryt J Matthee, Gabriel Brammer, Andrea Ferrara, Lara
Alegre, Huub Röttgering, Daniel Schaerer, Bahram Mobasher, and Behnam Darvish.
“On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its
Rest-Frame UV Components.” Monthly Notices of the Royal Astronomical Society.
Oxford University Press, 2019. https://doi.org/10.1093/mnras/sty2779.
ieee: D. Sobral et al., “On the nature and physical conditions of the luminous
Ly α emitter CR7 and its rest-frame UV components,” Monthly Notices of the
Royal Astronomical Society, vol. 482, no. 2. Oxford University Press, pp.
2422–2441, 2019.
ista: Sobral D, Matthee JJ, Brammer G, Ferrara A, Alegre L, Röttgering H, Schaerer
D, Mobasher B, Darvish B. 2019. On the nature and physical conditions of the luminous
Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal
Astronomical Society. 482(2), 2422–2441.
mla: Sobral, David, et al. “On the Nature and Physical Conditions of the Luminous
Ly α Emitter CR7 and Its Rest-Frame UV Components.” Monthly Notices of the
Royal Astronomical Society, vol. 482, no. 2, Oxford University Press, 2019,
pp. 2422–41, doi:10.1093/mnras/sty2779.
short: D. Sobral, J.J. Matthee, G. Brammer, A. Ferrara, L. Alegre, H. Röttgering,
D. Schaerer, B. Mobasher, B. Darvish, Monthly Notices of the Royal Astronomical
Society 482 (2019) 2422–2441.
date_created: 2022-07-08T10:40:05Z
date_published: 2019-01-01T00:00:00Z
date_updated: 2022-08-19T06:49:36Z
day: '01'
doi: 10.1093/mnras/sty2779
extern: '1'
external_id:
arxiv:
- '1710.08422'
intvolume: ' 482'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: ISM'
- 'cosmology: observations'
- dark ages
- reionization
- first stars
- early Universe
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1710.08422
month: '01'
oa: 1
oa_version: Preprint
page: 2422-2441
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: On the nature and physical conditions of the luminous Ly α emitter CR7 and
its rest-frame UV components
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 482
year: '2019'
...
---
_id: '11519'
abstract:
- lang: eng
text: 'Faint Lyα emitters become increasingly rarer toward the reionization epoch
(z ∼ 6–7). However, observations from a very large (∼5 deg2) Lyα narrow-band survey
at z = 6.6 show that this is not the case for the most luminous emitters, capable
of ionizing their own local bubbles. Here we present follow-up observations of
the two most luminous Lyα candidates in the COSMOS field: “MASOSA” and “CR7.”
We used X-SHOOTER, SINFONI, and FORS2 on the Very Large Telescope, and DEIMOS
on Keck, to confirm both candidates beyond any doubt. We find redshifts of z =
6.541 and z = 6.604 for “MASOSA” and “CR7,” respectively. MASOSA has a strong
detection in Lyα with a line width of 386 ± 30 km s−1 (FWHM) and with very high
EW0 (>200 Å), but undetected in the continuum, implying very low stellar mass
and a likely young, metal-poor stellar population. “CR7,” with an observed Lyα
luminosity of 1043.92±0.05 erg s−1 is the most luminous Lyα emitter ever found
at z > 6 and is spatially extended (∼16 kpc). “CR7” reveals a narrow Lyα line
with 266 ± 15 km s−1 FWHM, being detected in the near-infrared (NIR) (rest-frame
UV; β = −2.3 ± 0.1) and in IRAC/Spitzer. We detect a narrow He II 1640 Å emission
line (6σ, FWHM = 130 ± 30 km s−1 ) in CR7 which can explain the clear excess seen
in the J-band photometry (EW0 ∼ 80 Å). We find no other emission lines from the
UV to the NIR in our X-SHOOTER spectra (He II/O III] 1663 Å > 3 and He II/C III]
1908 Å > 2.5). We conclude that CR7 is best explained by a combination of a PopIII-like
population, which dominates the rest-frame UV and the nebular emission, and a
more normal stellar population, which presumably dominates the mass. Hubble Space
Telescope/WFC3 observations show that the light is indeed spatially separated
between a very blue component, coincident with Lyα and He II emission, and two
red components (∼5 kpc away), which dominate the mass. Our findings are consistent
with theoretical predictions of a PopIII wave, with PopIII star formation migrating
away from the original sites of star formation.'
acknowledgement: We thank the anonymous reviewer for useful and constructive comments
and suggestions which greatly improved the quality and clarity of our work. D.S.
acknowledges financial support from the Netherlands Organisation for Scientific
research (NWO) through a Veni fellowship, from FCT through a FCT Investigator Starting
Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010), from FCT grant UID/FIS/04434/2013,
and from LSF and LKBF. J.M. acknowledges the award of a Huygens PhD fellowship.
H.R. acknowledges support from the ERC Advanced Investigator program NewClusters
321271. The authors thank Mark Dijkstra, Bhaskar Agarwal, Jarrett Johnson, Andrea
Ferrara, Jarle Brinchmann, Rebecca Bowler, George Becker, Emma Curtis-Lake, Milos
Milosavljevic, Raffaella Schneider, Paul Shapiro, and Erik Zackrisson for interesting,
stimulating and helpful discussions. The authors are extremely grateful to ESO for
the award of ESO DDT time (294.A-5018 and 294.A-5039) which allowed the spectroscopic
confirmation of both sources and the detailed investigation of their nature. Observations
are also based on data from W.M. Keck Observatory. The W.M. Keck Observatory is
operated as a scientific partnership of Caltech, the University of California and
the National Aeronautics and Space Administration. Based on observations obtained
with MegaPrime/Megacam, a joint project of CFHT and CEA/IRFU, at the Canada–France–Hawaii
Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada,
the Institut National des Science de lUnivers of the Centre National de la Recherche
Scientifique (CNRS) of France, and the University of Hawaii. This work is based
in part on data products produced at Terapix available at the Canadian Astronomy
Data Centre as part of the Canada–France–Hawaii Telescope Legacy Survey, a collaborative
project of NRC and CNRS. Based on data products from observations made with ESO
Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018,
294.A-5039, and 179.A-2005, and on data products produced by TERAPIX and the Cambridge
Astronomy Survey Unit on behalf of the UltraVISTA consortium. The authors acknowledge
the award of service time (SW2014b20) on the William Herschel Telescope (WHT). WHT
and its service programme are operated on the island of La Palma by the Isaac Newton
Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de
Astrofisica de Canarias.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Behnam
full_name: Darvish, Behnam
last_name: Darvish
- first_name: Daniel
full_name: Schaerer, Daniel
last_name: Schaerer
- first_name: Bahram
full_name: Mobasher, Bahram
last_name: Mobasher
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
- first_name: Sérgio
full_name: Santos, Sérgio
last_name: Santos
- first_name: Shoubaneh
full_name: Hemmati, Shoubaneh
last_name: Hemmati
citation:
ama: 'Sobral D, Matthee JJ, Darvish B, et al. Evidence for PopIII-like stellar populations
in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic
confirmation. The Astrophysical Journal. 2015;808(2):139. doi:10.1088/0004-637X/808/2/139'
apa: 'Sobral, D., Matthee, J. J., Darvish, B., Schaerer, D., Mobasher, B., Röttgering,
H., … Hemmati, S. (2015). Evidence for PopIII-like stellar populations in the
most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation.
The Astrophysical Journal. IOP Publishing. https://doi.org/10.1088/0004-637X/808/2/139'
chicago: 'Sobral, David, Jorryt J Matthee, Behnam Darvish, Daniel Schaerer, Bahram
Mobasher, Huub Röttgering, Sérgio Santos, and Shoubaneh Hemmati. “Evidence for
PopIII-like Stellar Populations in the Most Luminous Lyα Emitters at the Epoch
of Reionisation: Spectroscopic Confirmation.” The Astrophysical Journal.
IOP Publishing, 2015. https://doi.org/10.1088/0004-637X/808/2/139.'
ieee: 'D. Sobral et al., “Evidence for PopIII-like stellar populations in
the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation,”
The Astrophysical Journal, vol. 808, no. 2. IOP Publishing, p. 139, 2015.'
ista: 'Sobral D, Matthee JJ, Darvish B, Schaerer D, Mobasher B, Röttgering H, Santos
S, Hemmati S. 2015. Evidence for PopIII-like stellar populations in the most luminous
Lyα emitters at the epoch of reionisation: Spectroscopic confirmation. The Astrophysical
Journal. 808(2), 139.'
mla: 'Sobral, David, et al. “Evidence for PopIII-like Stellar Populations in the
Most Luminous Lyα Emitters at the Epoch of Reionisation: Spectroscopic Confirmation.”
The Astrophysical Journal, vol. 808, no. 2, IOP Publishing, 2015, p. 139,
doi:10.1088/0004-637X/808/2/139.'
short: D. Sobral, J.J. Matthee, B. Darvish, D. Schaerer, B. Mobasher, H. Röttgering,
S. Santos, S. Hemmati, The Astrophysical Journal 808 (2015) 139.
date_created: 2022-07-07T09:00:58Z
date_published: 2015-07-28T00:00:00Z
date_updated: 2022-08-18T10:30:13Z
day: '28'
doi: 10.1088/0004-637X/808/2/139
extern: '1'
external_id:
arxiv:
- '1504.01734'
intvolume: ' 808'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- dark ages
- reionization
- 'first stars – early universe – galaxies: evolution'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1504.01734
month: '07'
oa: 1
oa_version: Preprint
page: '139'
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Evidence for PopIII-like stellar populations in the most luminous Lyα emitters
at the epoch of reionisation: Spectroscopic confirmation'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 808
year: '2015'
...
---
_id: '11580'
abstract:
- lang: eng
text: 'We present results from the largest contiguous narrow-band survey in the
near-infrared. We have used the wide-field infrared camera/Canada–France–Hawaii
Telescope and the lowOH2 filter (1.187 ± 0.005 μm) to survey ≈10 deg2 of contiguous
extragalactic sky in the SA22 field. A total of ∼6000 candidate emission-line
galaxies are found. We use deep ugrizJK data to obtain robust photometric redshifts.
We combine our data with the High-redshift(Z) Emission Line Survey (HiZELS), explore
spectroscopic surveys (VVDS, VIPERS) and obtain our own spectroscopic follow-up
with KMOS, FMOS and MOSFIRE to derive large samples of high-redshift emission-line
selected galaxies: 3471 Hα emitters at z = 0.8, 1343 [O III] + Hβ emitters at
z = 1.4 and 572 [O II] emitters at z = 2.2. We probe comoving volumes of >106
Mpc3 and find significant overdensities, including an 8.5σ (spectroscopically
confirmed) overdensity of Hα emitters at z = 0.81. We derive Hα, [O III] + Hβ
and [O II] luminosity functions at z = 0.8, 1.4, 2.2, respectively, and present
implications for future surveys such as Euclid. Our uniquely large volumes/areas
allow us to subdivide the samples in thousands of randomized combinations of areas
and provide a robust empirical measurement of sample/cosmic variance. We show
that surveys for star-forming/emission-line galaxies at a depth similar to ours
can only overcome cosmic-variance (errors <10 per cent) if they are based on volumes
>5 × 105 Mpc3; errors on L* and ϕ* due to sample (cosmic) variance on surveys
probing ∼104 and ∼105 Mpc3 are typically very high: ∼300 and ∼40–60 per cent,
respectively.'
acknowledgement: The authors wish to thank the anonymous reviewer for many helpful
comments and suggestions which greatly improved the clarity and quality of this
work. DS acknowledges financial support from the Netherlands Organization for Scientific
research (NWO) through a Veni fellowship, from FCT through an FCT Investigator Starting
Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010), from FCT grant PEst-OE/FIS/UI2751/2014,
and from LSF and LKBF. JM acknowledges the award of a Huygens PhD fellowship. PNB
is grateful for support from STFC. IRS acknowledges support from STFC, a Leverhulme
Fellowship, the ERC Advanced Investigator programme DUSTYGAL and a Royal Society/Wolfson
Merit Award. BMJ acknowledges support from the ERC-StG grant EGGS-278202. The Dark
Cosmology Centre is funded by the DNRF. The Dark Cosmology Centre is funded by the
DNRF. JWK acknowledges support from the National Research Foundation of Korea (NRF)
grant, no. 2008-0060544, funded by the Korea government (MSIP). JPS acknowledges
support from STFC (ST/I001573/1). JC acknowledges support from the FCT-IF grant
IF/01154/2012/CP0189/CT0010. The work was only possible due to OPTICON/FP7 and the
invaluable access that it granted to the CFHT telescope. We would also like to acknowledge
the excellent work done by CFHT staff in conducting the observations in service
mode, and on delivering truly excellent data. We are also tremendously thankful
to Kentaro Aoki for the incredible support while observing at Subaru with FMOS,
and also to the Keck staff for the help with the observations with MOSFIRE. This
work is based on observations obtained with WIRCam on the CFHT, OPTICON programme
2011B/029, 2012A019 and 2012B/016. Based on observations made with ESO telescopes
at the La Silla Paranal Observatory under programmes IDs 60.A-9460 (data can be
accessed through the ESO data archive), 087.A 0337 and 089.A-0965. Based on observations
done with FMOS on Subaru under programme S14A-084, and on MOSFIRE/Keck observations
under programme U066M. Part of the data on which this analysis is based are available
from Sobral et al. (2013a). Dedicated to the memory of C. M. Sobral (1953-2014).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: D.
full_name: Sobral, D.
last_name: Sobral
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: P. N.
full_name: Best, P. N.
last_name: Best
- first_name: I.
full_name: Smail, I.
last_name: Smail
- first_name: A. A.
full_name: Khostovan, A. A.
last_name: Khostovan
- first_name: B.
full_name: Milvang-Jensen, B.
last_name: Milvang-Jensen
- first_name: J.-W.
full_name: Kim, J.-W.
last_name: Kim
- first_name: J.
full_name: Stott, J.
last_name: Stott
- first_name: J.
full_name: Calhau, J.
last_name: Calhau
- first_name: H.
full_name: Nayyeri, H.
last_name: Nayyeri
- first_name: B.
full_name: Mobasher, B.
last_name: Mobasher
citation:
ama: 'Sobral D, Matthee JJ, Best PN, et al. CF-HiZELS, an ∼10 deg2 emission-line
survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions
at z = 0.8, 1.4 and 2.2 . Monthly Notices of the Royal Astronomical Society.
2015;451(3):2303-2323. doi:10.1093/mnras/stv1076'
apa: 'Sobral, D., Matthee, J. J., Best, P. N., Smail, I., Khostovan, A. A., Milvang-Jensen,
B., … Mobasher, B. (2015). CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic
follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and
2.2 . Monthly Notices of the Royal Astronomical Society. Oxford University
Press. https://doi.org/10.1093/mnras/stv1076'
chicago: 'Sobral, D., Jorryt J Matthee, P. N. Best, I. Smail, A. A. Khostovan, B.
Milvang-Jensen, J.-W. Kim, et al. “CF-HiZELS, an ∼10 Deg2 Emission-Line Survey
with Spectroscopic Follow-up: Hα, [O III] + Hβ and [O II] Luminosity Functions
at z = 0.8, 1.4 and 2.2 .” Monthly Notices of the Royal Astronomical Society.
Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv1076.'
ieee: 'D. Sobral et al., “CF-HiZELS, an ∼10 deg2 emission-line survey with
spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z
= 0.8, 1.4 and 2.2 ,” Monthly Notices of the Royal Astronomical Society,
vol. 451, no. 3. Oxford University Press, pp. 2303–2323, 2015.'
ista: 'Sobral D, Matthee JJ, Best PN, Smail I, Khostovan AA, Milvang-Jensen B, Kim
J-W, Stott J, Calhau J, Nayyeri H, Mobasher B. 2015. CF-HiZELS, an ∼10 deg2 emission-line
survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions
at z = 0.8, 1.4 and 2.2 . Monthly Notices of the Royal Astronomical Society. 451(3),
2303–2323.'
mla: 'Sobral, D., et al. “CF-HiZELS, an ∼10 Deg2 Emission-Line Survey with Spectroscopic
Follow-up: Hα, [O III] + Hβ and [O II] Luminosity Functions at z = 0.8, 1.4 and
2.2 .” Monthly Notices of the Royal Astronomical Society, vol. 451, no.
3, Oxford University Press, 2015, pp. 2303–23, doi:10.1093/mnras/stv1076.'
short: D. Sobral, J.J. Matthee, P.N. Best, I. Smail, A.A. Khostovan, B. Milvang-Jensen,
J.-W. Kim, J. Stott, J. Calhau, H. Nayyeri, B. Mobasher, Monthly Notices of the
Royal Astronomical Society 451 (2015) 2303–2323.
date_created: 2022-07-14T09:02:22Z
date_published: 2015-08-11T00:00:00Z
date_updated: 2022-08-19T08:23:18Z
day: '11'
doi: 10.1093/mnras/stv1076
extern: '1'
external_id:
arxiv:
- '1502.06602'
intvolume: ' 451'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: luminosity function'
- mass function
- 'cosmology: observations'
- early Universe
- large-scale structure of Universe
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1502.06602
month: '08'
oa: 1
oa_version: Preprint
page: 2303-2323
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up:
Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 '
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 451
year: '2015'
...