---
_id: '11488'
abstract:
- lang: eng
text: Hydrogen Lyα haloes (LAHs) are commonly used as a tracer of the circumgalactic
medium (CGM) at high redshifts. In this work, we aim to explore the existence
of Lyα haloes around individual UV-selected galaxies, rather than around Lyα emitters
(LAEs), at high redshifts. Our sample was continuum-selected with F775W ≤ 27.5,
and spectroscopic redshifts were assigned or constrained for all the sources thanks
to the deepest (100- to 140-h) existing Very Large Telescope (VLT)/Multi-Unit
Spectroscopic Explorer (MUSE) data with adaptive optics. The final sample includes
21 galaxies that are purely F775W-magnitude selected within the redshift range
z ≈ 2.9 − 4.4 and within a UV magnitude range −20 ≤ M1500 ≤ −18, thus avoiding
any bias toward LAEs. We tested whether galaxy’s Lyα emission is significantly
more extended than the MUSE PSF-convolved continuum component. We find 17 LAHs
and four non-LAHs. We report the first individual detections of extended Lyα emission
around non-LAEs. The Lyα halo fraction is thus as high as 81.0−11.2+10.3%, which
is close to that for LAEs at z = 3 − 6 in the literature. This implies that UV-selected
galaxies generally have a large amount of hydrogen in their CGM. We derived the
mean surface brightness (SB) profile for our LAHs with cosmic dimming corrections
and find that Lyα emission extends to 5.4 arcsec (≃40 physical kpc at the midpoint
redshift z = 3.6) above the typical 1σ SB limit. The incidence rate of surrounding
gas detected in Lyα per one-dimensional line of sight per unit redshift, dn/dz,
is estimated to be 0.76−0.09+0.09 for galaxies with M1500 ≤ −18 mag at z ≃ 3.7.
Assuming that Lyα emission and absorption arise in the same gas, this suggests,
based on abundance matching, that LAHs trace the same gas as damped Lyα systems
(DLAs) and sub-DLAs.
acknowledgement: 'We thank the anonymous referee for constructive comments and suggestions.
We would like to express our gratitude to Edmund Christian Herenz, Leindert Boogard,
Miroslava Dessauges, Moupiya Maji, Valentin Mauerhofer, Charlotte Paola Simmonds
Wagemann, Masami Ouchi, Kazuhiro Shimasaku, Akio Inoue, and Rieko Momose for giving
insightful comments and suggestions. H.K. is grateful to Liam McCarney for useful
suggestions on English writing through the UniGE’s Tandems linguistiques. H.K. acknowledges
support from Swiss Government Excellence Scholarships and Japan Society for the
Promotion of Science (JSPS) Overseas Research Fellowship. H.K., F.L., and A.V. are
supported by the SNF grant PP00P2 176808. A.V. and T.G. are supported by the ERC
Starting Grant 757258“TRIPLE”. This work was supported by the Programme National
Cosmology et Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and
CNES. This work is based on observations taken by VLT, which is operated by European
Southern Observatory. This research made use of Astropy, which is a community-developed
core Python package for Astronomy (Astropy Collaboration 2013, 2018), and other
software and packages: MARZ, MPDAF (Piqueras et al. 2019), PHOTUTILS, Numpy (Harris
et al. 2020), Scipy (Virtanen et al. 2020), and matplotlib (Hunter 2007).'
article_number: A44
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- first_name: Anne
full_name: Verhamme, Anne
last_name: Verhamme
- first_name: Jérémy
full_name: Blaizot, Jérémy
last_name: Blaizot
- first_name: Thibault
full_name: Garel, Thibault
last_name: Garel
- first_name: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
- first_name: Floriane
full_name: Leclercq, Floriane
last_name: Leclercq
- first_name: Roland
full_name: Bacon, Roland
last_name: Bacon
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Sofia G.
full_name: Gallego, Sofia G.
last_name: Gallego
- first_name: Josephine
full_name: Kerutt, Josephine
last_name: Kerutt
- 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: Michael
full_name: Maseda, Michael
last_name: Maseda
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
- first_name: Roser
full_name: Pelló, Roser
last_name: Pelló
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Laurence
full_name: Tresse, Laurence
last_name: Tresse
- first_name: Tanya
full_name: Urrutia, Tanya
last_name: Urrutia
- first_name: Eloïse
full_name: Vitte, Eloïse
last_name: Vitte
citation:
ama: 'Kusakabe H, Verhamme A, Blaizot J, et al. The MUSE eXtremely Deep Field: Individual
detections of Lyα haloes around rest-frame UV-selected galaxies at z
≃ 2.9–4.4. Astronomy & Astrophysics. 2022;660. doi:10.1051/0004-6361/202142302'
apa: 'Kusakabe, H., Verhamme, A., Blaizot, J., Garel, T., Wisotzki, L., Leclercq,
F., … Vitte, E. (2022). The MUSE eXtremely Deep Field: Individual detections of
Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4.
Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202142302'
chicago: 'Kusakabe, Haruka, Anne Verhamme, Jérémy Blaizot, Thibault Garel, Lutz
Wisotzki, Floriane Leclercq, Roland Bacon, et al. “The MUSE EXtremely Deep Field:
Individual Detections of Lyα Haloes around Rest-Frame UV-Selected Galaxies
at z ≃ 2.9–4.4.” Astronomy & Astrophysics. EDP Sciences, 2022.
https://doi.org/10.1051/0004-6361/202142302.'
ieee: 'H. Kusakabe et al., “The MUSE eXtremely Deep Field: Individual detections
of Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4,”
Astronomy & Astrophysics, vol. 660. EDP Sciences, 2022.'
ista: 'Kusakabe H, Verhamme A, Blaizot J, Garel T, Wisotzki L, Leclercq F, Bacon
R, Schaye J, Gallego SG, Kerutt J, Matthee JJ, Maseda M, Nanayakkara T, Pelló
R, Richard J, Tresse L, Urrutia T, Vitte E. 2022. The MUSE eXtremely Deep Field:
Individual detections of Lyα haloes around rest-frame UV-selected galaxies
at z ≃ 2.9–4.4. Astronomy & Astrophysics. 660, A44.'
mla: 'Kusakabe, Haruka, et al. “The MUSE EXtremely Deep Field: Individual Detections
of Lyα Haloes around Rest-Frame UV-Selected Galaxies at z ≃ 2.9–4.4.”
Astronomy & Astrophysics, vol. 660, A44, EDP Sciences, 2022, doi:10.1051/0004-6361/202142302.'
short: H. Kusakabe, A. Verhamme, J. Blaizot, T. Garel, L. Wisotzki, F. Leclercq,
R. Bacon, J. Schaye, S.G. Gallego, J. Kerutt, J.J. Matthee, M. Maseda, T. Nanayakkara,
R. Pelló, J. Richard, L. Tresse, T. Urrutia, E. Vitte, Astronomy & Astrophysics
660 (2022).
date_created: 2022-07-05T14:27:26Z
date_published: 2022-04-07T00:00:00Z
date_updated: 2022-07-19T09:33:24Z
day: '07'
doi: 10.1051/0004-6361/202142302
extern: '1'
external_id:
arxiv:
- '2201.07257'
intvolume: ' 660'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology:
observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2201.07257
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'
scopus_import: '1'
status: public
title: 'The MUSE eXtremely Deep Field: Individual detections of Lyα haloes
around rest-frame UV-selected galaxies at z ≃ 2.9–4.4'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 660
year: '2022'
...
---
_id: '11497'
abstract:
- lang: eng
text: "Context. The hydrogen Lyman α line is often the only measurable feature in
optical spectra of high-redshift galaxies. Its shape and strength are influenced
by radiative transfer processes and the properties of the underlying stellar population.
High equivalent widths of several hundred Å are especially hard to explain by
models and could point towards unusual stellar populations, for example with low
metallicities, young stellar ages, and a top-heavy initial mass function. Other
aspects influencing equivalent widths are the morphology of the galaxy and its
gas properties.\r\nAims. The aim of this study is to better understand the connection
between the Lyman α rest-frame equivalent width (EW0) and spectral properties
as well as ultraviolet (UV) continuum morphology by obtaining reliable EW0 histograms
for a statistical sample of galaxies and by assessing the fraction of objects
with large equivalent widths.\r\nMethods. We used integral field spectroscopy
from the Multi Unit Spectroscopic Explorer (MUSE) combined with broad-band data
from the Hubble Space Telescope (HST) to measure EW0. We analysed the emission
lines of 1920 Lyman α emitters (LAEs) detected in the full MUSE-Wide (one hour
exposure time) and MUSE-Deep (ten hour exposure time) surveys and found UV continuum
counterparts in archival HST data. We fitted the UV continuum photometric images
using the Galfit software to gain morphological information on the rest-UV emission
and fitted the spectra obtained from MUSE to determine the double peak fraction,
asymmetry, full-width at half maximum, and flux of the Lyman α line.\r\nResults.
The two surveys show different histograms of Lyman α EW0. In MUSE-Wide, 20% of
objects have EW0 > 240 Å, while this fraction is only 11% in MUSE-Deep and ≈16%
for the full sample. This includes objects without HST continuum counterparts
(one-third of our sample), for which we give lower limits for EW0. The object
with the highest securely measured EW0 has EW0 = 589 ± 193 Å (the highest lower
limit being EW0 = 4464 Å). We investigate the connection between EW0 and Lyman
α spectral or UV continuum morphological properties.\r\nConclusions. The survey
depth has to be taken into account when studying EW0 distributions. We find that
in general, high EW0 objects can have a wide range of spectral and UV morphological
properties, which might reflect that the underlying causes for high EW0 values
are equally varied."
acknowledgement: We thank the referee for thoughtful and constructive comments that
have improved the quality of this manuscript. Based on observations collected at
the European Southern Observatory under ESO programme 1101.A-0127. This work made
use of v2.2.1 of the Binary Population and Spectral Synthesis (BPASS) models as
described in Eldridge et al. (2017) and Stanway & Eldridge (2018). A.F. acknowledges
the support from grant PRIN MIUR2017-20173ML3WW_001. T.N. acknowledges support from
Australian Research Council Laureate Fellowship FL180100060.
article_number: '183'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: J.
full_name: Kerutt, J.
last_name: Kerutt
- first_name: L.
full_name: Wisotzki, L.
last_name: Wisotzki
- first_name: A.
full_name: Verhamme, A.
last_name: Verhamme
- first_name: K. B.
full_name: Schmidt, K. B.
last_name: Schmidt
- first_name: F.
full_name: Leclercq, F.
last_name: Leclercq
- first_name: E. C.
full_name: Herenz, E. C.
last_name: Herenz
- first_name: T.
full_name: Urrutia, T.
last_name: Urrutia
- first_name: T.
full_name: Garel, T.
last_name: Garel
- first_name: T.
full_name: Hashimoto, T.
last_name: Hashimoto
- first_name: M.
full_name: Maseda, M.
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: H.
full_name: Kusakabe, H.
last_name: Kusakabe
- first_name: J.
full_name: Schaye, J.
last_name: Schaye
- first_name: J.
full_name: Richard, J.
last_name: Richard
- first_name: B.
full_name: Guiderdoni, B.
last_name: Guiderdoni
- first_name: V.
full_name: Mauerhofer, V.
last_name: Mauerhofer
- first_name: T.
full_name: Nanayakkara, T.
last_name: Nanayakkara
- first_name: E.
full_name: Vitte, E.
last_name: Vitte
citation:
ama: Kerutt J, Wisotzki L, Verhamme A, et al. Equivalent widths of Lyman α emitters
in MUSE-Wide and MUSE-Deep. Astronomy & Astrophysics. 2022;659. doi:10.1051/0004-6361/202141900
apa: Kerutt, J., Wisotzki, L., Verhamme, A., Schmidt, K. B., Leclercq, F., Herenz,
E. C., … Vitte, E. (2022). Equivalent widths of Lyman α emitters in MUSE-Wide
and MUSE-Deep. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202141900
chicago: Kerutt, J., L. Wisotzki, A. Verhamme, K. B. Schmidt, F. Leclercq, E. C.
Herenz, T. Urrutia, et al. “Equivalent Widths of Lyman α Emitters in MUSE-Wide
and MUSE-Deep.” Astronomy & Astrophysics. EDP Sciences, 2022. https://doi.org/10.1051/0004-6361/202141900.
ieee: J. Kerutt et al., “Equivalent widths of Lyman α emitters in MUSE-Wide
and MUSE-Deep,” Astronomy & Astrophysics, vol. 659. EDP Sciences, 2022.
ista: Kerutt J, Wisotzki L, Verhamme A, Schmidt KB, Leclercq F, Herenz EC, Urrutia
T, Garel T, Hashimoto T, Maseda M, Matthee JJ, Kusakabe H, Schaye J, Richard J,
Guiderdoni B, Mauerhofer V, Nanayakkara T, Vitte E. 2022. Equivalent widths of
Lyman α emitters in MUSE-Wide and MUSE-Deep. Astronomy & Astrophysics. 659,
183.
mla: Kerutt, J., et al. “Equivalent Widths of Lyman α Emitters in MUSE-Wide and
MUSE-Deep.” Astronomy & Astrophysics, vol. 659, 183, EDP Sciences,
2022, doi:10.1051/0004-6361/202141900.
short: J. Kerutt, L. Wisotzki, A. Verhamme, K.B. Schmidt, F. Leclercq, E.C. Herenz,
T. Urrutia, T. Garel, T. Hashimoto, M. Maseda, J.J. Matthee, H. Kusakabe, J. Schaye,
J. Richard, B. Guiderdoni, V. Mauerhofer, T. Nanayakkara, E. Vitte, Astronomy
& Astrophysics 659 (2022).
date_created: 2022-07-06T08:17:27Z
date_published: 2022-03-25T00:00:00Z
date_updated: 2022-07-19T09:47:16Z
day: '25'
doi: 10.1051/0004-6361/202141900
extern: '1'
external_id:
arxiv:
- '2202.06642'
intvolume: ' 659'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology:
observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2202.06642
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: Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 659
year: '2022'
...
---
_id: '11521'
abstract:
- lang: eng
text: 'The cosmic ionizing emissivity from star-forming galaxies has long been anchored
to UV luminosity functions. Here, we introduce an emissivity framework based on
Lyα emitters (LAEs), which naturally hones in on the subset of galaxies responsible
for the ionizing background due to the intimate connection between production
and escape of Lyα and LyC photons. Using constraints on the escape fractions of
bright LAEs (LLyα > 0.2L*) at z ≈ 2 obtained from resolved Lyα profiles, and arguing
for their redshift-invariance, we show that: (i) quasars and LAEs together reproduce
the relatively flat emissivity at z ≈ 2–6, which is non-trivial given the strong
evolution in both the star formation density and quasar number density at these
epochs and (ii) LAEs produce late and rapid reionization between z ≈ 6−9 under
plausible assumptions. Within this framework, the >10 × rise in the UV population-averaged
fesc between z ≈ 3–7 naturally arises due to the same phenomena that drive the
growing LAE fraction with redshift. Generally, a LAE dominated emissivity yields
a peak in the distribution of the ionizing budget with UV luminosity as reported
in latest simulations. Using our adopted parameters (fesc=50 per cent, ξion
= 1025.9 Hz erg−1 for half the bright LAEs), a highly ionizing minority of galaxies
with MUV < −17 accounts for the entire ionizing budget from star-forming galaxies.
Rapid flashes of LyC from such rare galaxies produce a ‘disco’ ionizing background.
We conclude proposing tests to further develop our suggested Lyα-anchored formalism.'
acknowledgement: We thank an anonymous referee for an encouraging and constructive
report that helped improving the quality of this work. We acknowledge illuminating
conversations with Xiaohan Wu, Chris Cain, Anna-Christina Eilers, Simon Lilly and
Ruari Mackenzie. RPN gratefully acknowledges an Ashford Fellowship granted by Harvard
University. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409.
PO acknowledges support from the Swiss National Science Foundation through the SNSF
Professorship grant 190079. GP acknowledges support from the Netherlands Research
School for Astronomy (NOVA). MH is fellow of the Knut and Alice Wallenberg Foundation.
DE is supported by the US National Science Foundation (NSF) through Astronomy &
Astrophysics grant AST-1909198. The Cosmic Dawn Center (DAWN) is funded by the Danish
National Research Foundation under grant No. 140. RA acknowledges support from Fondecyt
Regular Grant 1202007. ST is supported by the 2021 Research Fund 1.210134.01 of
UNIST (Ulsan National Institute of Science & Technology). MLl acknowledges support
from the ANID/Scholarship Program/Doctorado Nacional/2019-21191036. JC acknowledges
support from the Spanish Ministry of Science and Innovation, project PID2019-107408GB-C43
(ESTALLIDOS) and from Gobierno de Canarias through EU FEDER funding, project PID2020010050.
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: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Matthew
full_name: Hayes, Matthew
last_name: Hayes
- first_name: Dawn
full_name: Erb, Dawn
last_name: Erb
- first_name: Daniel
full_name: Schaerer, Daniel
last_name: Schaerer
- first_name: Ricardo
full_name: Amorín, Ricardo
last_name: Amorín
- first_name: Sandro
full_name: Tacchella, Sandro
last_name: Tacchella
- first_name: Ana Paulino-Afonso
full_name: Ana Paulino-Afonso, Ana Paulino-Afonso
last_name: Ana Paulino-Afonso
- first_name: Mario
full_name: Llerena, Mario
last_name: Llerena
- first_name: João
full_name: Calhau, João
last_name: Calhau
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
citation:
ama: 'Matthee JJ, Naidu RP, Pezzulli G, et al. (Re)Solving reionization with Lyα:
How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background.
Monthly Notices of the Royal Astronomical Society. 2022;512(4):5960-5977.
doi:10.1093/mnras/stac801'
apa: 'Matthee, J. J., Naidu, R. P., Pezzulli, G., Gronke, M., Sobral, D., Oesch,
P. A., … Röttgering, H. (2022). (Re)Solving reionization with Lyα: How bright
Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly
Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stac801'
chicago: 'Matthee, Jorryt J, Rohan P. Naidu, Gabriele Pezzulli, Max Gronke, David
Sobral, Pascal A. Oesch, Matthew Hayes, et al. “(Re)Solving Reionization with
Lyα: How Bright Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.”
Monthly Notices of the Royal Astronomical Society. Oxford University Press,
2022. https://doi.org/10.1093/mnras/stac801.'
ieee: 'J. J. Matthee et al., “(Re)Solving reionization with Lyα: How bright
Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background,” Monthly
Notices of the Royal Astronomical Society, vol. 512, no. 4. Oxford University
Press, pp. 5960–5977, 2022.'
ista: 'Matthee JJ, Naidu RP, Pezzulli G, Gronke M, Sobral D, Oesch PA, Hayes M,
Erb D, Schaerer D, Amorín R, Tacchella S, Ana Paulino-Afonso AP-A, Llerena M,
Calhau J, Röttgering H. 2022. (Re)Solving reionization with Lyα: How bright Lyα
emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly Notices
of the Royal Astronomical Society. 512(4), 5960–5977.'
mla: 'Matthee, Jorryt J., et al. “(Re)Solving Reionization with Lyα: How Bright
Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.” Monthly
Notices of the Royal Astronomical Society, vol. 512, no. 4, Oxford University
Press, 2022, pp. 5960–77, doi:10.1093/mnras/stac801.'
short: J.J. Matthee, R.P. Naidu, G. Pezzulli, M. Gronke, D. Sobral, P.A. Oesch,
M. Hayes, D. Erb, D. Schaerer, R. Amorín, S. Tacchella, A.P.-A. Ana Paulino-Afonso,
M. Llerena, J. Calhau, H. Röttgering, Monthly Notices of the Royal Astronomical
Society 512 (2022) 5960–5977.
date_created: 2022-07-07T09:21:30Z
date_published: 2022-06-01T00:00:00Z
date_updated: 2022-08-18T10:42:47Z
day: '01'
doi: 10.1093/mnras/stac801
extern: '1'
external_id:
arxiv:
- '2110.11967'
intvolume: ' 512'
issue: '4'
keyword:
- 'galaxies: high-redshift'
- intergalactic medium
- 'cosmology: observations'
- dark ages
- reionization
- first stars
- 'ultraviolet: galaxies'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2110.11967
month: '06'
oa: 1
oa_version: Preprint
page: 5960-5977
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: '(Re)Solving reionization with Lyα: How bright Lyα emitters account for the
z ≈ 2 − 8 cosmic ionizing background'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 512
year: '2022'
...
---
_id: '11500'
abstract:
- lang: eng
text: We report the discovery of diffuse extended Lyα emission from redshift 3.1
to 4.5, tracing cosmic web filaments on scales of 2.5−4 cMpc. These structures
have been observed in overdensities of Lyα emitters in the MUSE Extremely Deep
Field, a 140 h deep MUSE observation located in the Hubble Ultra-Deep Field. Among
the 22 overdense regions identified, five are likely to harbor very extended Lyα
emission at high significance with an average surface brightness of 5 × 10−20
erg s−1 cm−2 arcsec−2. Remarkably, 70% of the total Lyα luminosity from these
filaments comes from beyond the circumgalactic medium of any identified Lyα emitter.
Fluorescent Lyα emission powered by the cosmic UV background can only account
for less than 34% of this emission at z ≈ 3 and for not more than 10% at higher
redshift. We find that the bulk of this diffuse emission can be reproduced by
the unresolved Lyα emission of a large population of ultra low-luminosity Lyα
emitters (< 1040 erg s−1), provided that the faint end of the Lyα luminosity function
is steep (α ⪅ −1.8), it extends down to luminosities lower than 1038 − 1037 erg
s−1, and the clustering of these Lyα emitters is significant (filling factor <
1/6). If these Lyα emitters are powered by star formation, then this implies their
luminosity function needs to extend down to star formation rates < 10−4 M⊙ yr−1.
These observations provide the first detection of the cosmic web in Lyα emission
in typical filamentary environments and the first observational clue indicating
the existence of a large population of ultra low-luminosity Lyα emitters at high
redshift.
acknowledgement: 'We warmly thank ESO Paranal staff for their great professional support
during all MXDF GTO observing runs. We thank the anonymous referee for a careful
reading of the manuscript and helpful comments. We also thank Matthew Lehnert for
fruitful discussions. RB, AF, SC acknowledge support from the ERC advanced grant
339659-MUSICOS. JB acknowledges support by Fundação para a Ciência e a Tecnologia
(FCT) through the research grants UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020
and through the Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. TG, AV
acknowledges support from the European Research Council under grant agreement ERC-stg-757258
(TRIPLE). DM acknowledges A. Dabbech for useful interactions about IUWT and support
from the GDR ISIS through the Projets exploratoires program (project TASTY). AF
acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. SLZ acknowledges
support by The Netherlands Organisation for Scientific Research (NWO) through a
TOP Grant Module 1 under project number 614.001.652. This research made use of the
following open-source software and we are thankful to the developers of these: GNU
Octave (Eaton et al. 2018) and its statistics, signal and image packages, the Python
packages Matplotlib (Hunter 2007), Numpy (van der Walt et al. 2010), MPDAF (Piqueras
et al. 2017), Astropy (Astropy Collaboration 2018), PyWavelets (Lee et al. 2019).'
article_number: A107
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: R.
full_name: Bacon, R.
last_name: Bacon
- first_name: D.
full_name: Mary, D.
last_name: Mary
- first_name: T.
full_name: Garel, T.
last_name: Garel
- first_name: J.
full_name: Blaizot, J.
last_name: Blaizot
- first_name: M.
full_name: Maseda, M.
last_name: Maseda
- first_name: J.
full_name: Schaye, J.
last_name: Schaye
- first_name: L.
full_name: Wisotzki, L.
last_name: Wisotzki
- first_name: S.
full_name: Conseil, S.
last_name: Conseil
- first_name: J.
full_name: Brinchmann, J.
last_name: Brinchmann
- first_name: F.
full_name: Leclercq, F.
last_name: Leclercq
- first_name: V.
full_name: Abril-Melgarejo, V.
last_name: Abril-Melgarejo
- first_name: L.
full_name: Boogaard, L.
last_name: Boogaard
- first_name: N. F.
full_name: Bouché, N. F.
last_name: Bouché
- first_name: T.
full_name: Contini, T.
last_name: Contini
- first_name: A.
full_name: Feltre, A.
last_name: Feltre
- first_name: B.
full_name: Guiderdoni, B.
last_name: Guiderdoni
- first_name: C.
full_name: Herenz, C.
last_name: Herenz
- first_name: W.
full_name: Kollatschny, W.
last_name: Kollatschny
- first_name: H.
full_name: Kusakabe, H.
last_name: Kusakabe
- 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: L.
full_name: Michel-Dansac, L.
last_name: Michel-Dansac
- first_name: T.
full_name: Nanayakkara, T.
last_name: Nanayakkara
- first_name: J.
full_name: Richard, J.
last_name: Richard
- first_name: M.
full_name: Roth, M.
last_name: Roth
- first_name: K. B.
full_name: Schmidt, K. B.
last_name: Schmidt
- first_name: M.
full_name: Steinmetz, M.
last_name: Steinmetz
- first_name: L.
full_name: Tresse, L.
last_name: Tresse
- first_name: T.
full_name: Urrutia, T.
last_name: Urrutia
- first_name: A.
full_name: Verhamme, A.
last_name: Verhamme
- first_name: P. M.
full_name: Weilbacher, P. M.
last_name: Weilbacher
- first_name: J.
full_name: Zabl, J.
last_name: Zabl
- first_name: S. L.
full_name: Zoutendijk, S. L.
last_name: Zoutendijk
citation:
ama: 'Bacon R, Mary D, Garel T, et al. The MUSE Extremely Deep Field: The cosmic
web in emission at high redshift. Astronomy & Astrophysics. 2021;647.
doi:10.1051/0004-6361/202039887'
apa: 'Bacon, R., Mary, D., Garel, T., Blaizot, J., Maseda, M., Schaye, J., … Zoutendijk,
S. L. (2021). The MUSE Extremely Deep Field: The cosmic web in emission at high
redshift. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202039887'
chicago: 'Bacon, R., D. Mary, T. Garel, J. Blaizot, M. Maseda, J. Schaye, L. Wisotzki,
et al. “The MUSE Extremely Deep Field: The Cosmic Web in Emission at High Redshift.”
Astronomy & Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202039887.'
ieee: 'R. Bacon et al., “The MUSE Extremely Deep Field: The cosmic web in
emission at high redshift,” Astronomy & Astrophysics, vol. 647. EDP
Sciences, 2021.'
ista: 'Bacon R, Mary D, Garel T, Blaizot J, Maseda M, Schaye J, Wisotzki L, Conseil
S, Brinchmann J, Leclercq F, Abril-Melgarejo V, Boogaard L, Bouché NF, Contini
T, Feltre A, Guiderdoni B, Herenz C, Kollatschny W, Kusakabe H, Matthee JJ, Michel-Dansac
L, Nanayakkara T, Richard J, Roth M, Schmidt KB, Steinmetz M, Tresse L, Urrutia
T, Verhamme A, Weilbacher PM, Zabl J, Zoutendijk SL. 2021. The MUSE Extremely
Deep Field: The cosmic web in emission at high redshift. Astronomy & Astrophysics.
647, A107.'
mla: 'Bacon, R., et al. “The MUSE Extremely Deep Field: The Cosmic Web in Emission
at High Redshift.” Astronomy & Astrophysics, vol. 647, A107, EDP Sciences,
2021, doi:10.1051/0004-6361/202039887.'
short: R. Bacon, D. Mary, T. Garel, J. Blaizot, M. Maseda, J. Schaye, L. Wisotzki,
S. Conseil, J. Brinchmann, F. Leclercq, V. Abril-Melgarejo, L. Boogaard, N.F.
Bouché, T. Contini, A. Feltre, B. Guiderdoni, C. Herenz, W. Kollatschny, H. Kusakabe,
J.J. Matthee, L. Michel-Dansac, T. Nanayakkara, J. Richard, M. Roth, K.B. Schmidt,
M. Steinmetz, L. Tresse, T. Urrutia, A. Verhamme, P.M. Weilbacher, J. Zabl, S.L.
Zoutendijk, Astronomy & Astrophysics 647 (2021).
date_created: 2022-07-06T09:31:50Z
date_published: 2021-03-18T00:00:00Z
date_updated: 2022-07-19T09:34:57Z
day: '18'
doi: 10.1051/0004-6361/202039887
extern: '1'
external_id:
arxiv:
- '2102.05516'
intvolume: ' 647'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / galaxies: groups: general / cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2102.05516
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: 'The MUSE Extremely Deep Field: The cosmic web in emission at high redshift'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 647
year: '2021'
...
---
_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: '11504'
abstract:
- lang: eng
text: We present spatially resolved maps of six individually-detected Lyman α haloes
(LAHs) as well as a first statistical analysis of the Lyman α (Lyα) spectral signature
in the circum-galactic medium of high-redshift star-forming galaxies (−17.5 >
MUV > −21.5) using the Multi-Unit Spectroscopic Explorer. Our resolved spectroscopic
analysis of the LAHs reveals significant intrahalo variations of the Lyα line
profile. Using a three-dimensional two-component model for the Lyα emission, we
measured the full width at half maximum (FWHM), the peak velocity shift, and the
asymmetry of the Lyα line in the core and in the halo of 19 galaxies. We find
that the Lyα line shape is statistically different in the halo compared to the
core (in terms of width, peak wavelength, and asymmetry) for ≈40% of our galaxies.
Similarly to object-by-object based studies and a recent resolved study using
lensing, we find a correlation between the peak velocity shift and the width of
the Lyα line both at the interstellar and circum-galactic scales. This trend has
been predicted by radiative transfer simulations of galactic winds as a result
of resonant scattering in outflows. While there is a lack of correlation between
the spectral properties and the spatial scale lengths of our LAHs, we find a correlation
between the width of the line in the LAH and the halo flux fraction. Interestingly,
UV bright galaxies (MUV < −20) show broader, more redshifted, and less asymmetric
Lyα lines in their haloes. The most significant correlation found is for the FWHM
of the line and the UV continuum slope of the galaxy, suggesting that the redder
galaxies have broader Lyα lines. The generally broad and red line shapes found
in the halo component suggest that the Lyα haloes are powered either by scattering
processes through an outflowing medium, fluorescent emission from outflowing cold
clumps of gas, or a mix of both. Considering the large diversity of the Lyα line
profiles observed in our sample and the lack of strong correlation, the interpretation
of our results is still broadly open and underlines the need for realistic spatially
resolved models of the LAHs.
acknowledgement: F.L., R.B., and S.C. acknowledge support from the ERC advanced grant
339659-MUSICOS. F.L., T.G., H.K., and A.V. acknowledge support from the ERC starting
grant ERC-757258-TRIPLE. A.C. and J.R. acknowledge support from the ERC starting
grant 336736-CALENDS. J.B. acknowledges support by FCT/MCTES through national funds
(PID-DAC) by grant UID/FIS/04434/2019 and through Investigador FCT Contract No.IF/01654/2014/CP1215/CT0003.
T.H. was supported by Leading Initiative for Excellent Young Researchers, MEXT,
Japan.
article_number: A82
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Floriane
full_name: Leclercq, Floriane
last_name: Leclercq
- first_name: Roland
full_name: Bacon, Roland
last_name: Bacon
- first_name: Anne
full_name: Verhamme, Anne
last_name: Verhamme
- first_name: Thibault
full_name: Garel, Thibault
last_name: Garel
- first_name: Jérémy
full_name: Blaizot, Jérémy
last_name: Blaizot
- first_name: Jarle
full_name: Brinchmann, Jarle
last_name: Brinchmann
- first_name: Sebastiano
full_name: Cantalupo, Sebastiano
last_name: Cantalupo
- first_name: Adélaïde
full_name: Claeyssens, Adélaïde
last_name: Claeyssens
- first_name: Simon
full_name: Conseil, Simon
last_name: Conseil
- first_name: Thierry
full_name: Contini, Thierry
last_name: Contini
- first_name: Takuya
full_name: Hashimoto, Takuya
last_name: Hashimoto
- first_name: Edmund Christian
full_name: Herenz, Edmund Christian
last_name: Herenz
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- 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: Peter
full_name: Mitchell, Peter
last_name: Mitchell
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Kasper Borello
full_name: Schmidt, Kasper Borello
last_name: Schmidt
- first_name: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
citation:
ama: 'Leclercq F, Bacon R, Verhamme A, et al. The MUSE Hubble Ultra Deep field survey:
XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming
galaxies at z > 3. Astronomy & Astrophysics. 2020;635. doi:10.1051/0004-6361/201937339'
apa: 'Leclercq, F., Bacon, R., Verhamme, A., Garel, T., Blaizot, J., Brinchmann,
J., … Wisotzki, L. (2020). The MUSE Hubble Ultra Deep field survey: XIII. Spatially
resolved spectral properties of Lyman α haloes around star-forming galaxies at
z > 3. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201937339'
chicago: 'Leclercq, Floriane, Roland Bacon, Anne Verhamme, Thibault Garel, Jérémy
Blaizot, Jarle Brinchmann, Sebastiano Cantalupo, et al. “The MUSE Hubble Ultra
Deep Field Survey: XIII. Spatially Resolved Spectral Properties of Lyman α Haloes
around Star-Forming Galaxies at z > 3.” Astronomy & Astrophysics.
EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/201937339.'
ieee: 'F. Leclercq et al., “The MUSE Hubble Ultra Deep field survey: XIII.
Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies
at z > 3,” Astronomy & Astrophysics, vol. 635. EDP Sciences, 2020.'
ista: 'Leclercq F, Bacon R, Verhamme A, Garel T, Blaizot J, Brinchmann J, Cantalupo
S, Claeyssens A, Conseil S, Contini T, Hashimoto T, Herenz EC, Kusakabe H, Marino
RA, Maseda M, Matthee JJ, Mitchell P, Pezzulli G, Richard J, Schmidt KB, Wisotzki
L. 2020. The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral
properties of Lyman α haloes around star-forming galaxies at z > 3. Astronomy
& Astrophysics. 635, A82.'
mla: 'Leclercq, Floriane, et al. “The MUSE Hubble Ultra Deep Field Survey: XIII.
Spatially Resolved Spectral Properties of Lyman α Haloes around Star-Forming Galaxies
at z > 3.” Astronomy & Astrophysics, vol. 635, A82, EDP Sciences,
2020, doi:10.1051/0004-6361/201937339.'
short: F. Leclercq, R. Bacon, A. Verhamme, T. Garel, J. Blaizot, J. Brinchmann,
S. Cantalupo, A. Claeyssens, S. Conseil, T. Contini, T. Hashimoto, E.C. Herenz,
H. Kusakabe, R.A. Marino, M. Maseda, J.J. Matthee, P. Mitchell, G. Pezzulli, J.
Richard, K.B. Schmidt, L. Wisotzki, Astronomy & Astrophysics 635 (2020).
date_created: 2022-07-06T09:56:20Z
date_published: 2020-03-11T00:00:00Z
date_updated: 2022-07-19T09:36:58Z
day: '11'
doi: 10.1051/0004-6361/201937339
extern: '1'
external_id:
arxiv:
- '2002.05731'
intvolume: ' 635'
keyword:
- Space and Planetary Science
- 'Astronomy and Astrophysics galaxies: high-redshift / galaxies: formation / galaxies:
evolution / cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2002.05731
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: 'The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral
properties of Lyman α haloes around star-forming galaxies at z > 3'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 635
year: '2020'
...
---
_id: '11529'
abstract:
- lang: eng
text: CR7 is among the most luminous Ly α emitters (LAEs) known at z = 6.6 and consists
of at least three UV components that are surrounded by Ly α emission. Previous
studies have suggested that it may host an extreme ionizing source. Here, we present
deep integral field spectroscopy of CR7 with VLT/Multi Unit Spectroscopic Explorer
(MUSE). We measure extended emission with a similar halo scale length as typical
LAEs at z ≈ 5. CR7’s Ly α halo is clearly elongated along the direction connecting
the multiple components, likely tracing the underlying gas distribution. The Ly α
emission originates almost exclusively from the brightest UV component, but we
also identify a faint kinematically distinct Ly α emitting region nearby a fainter
component. Combined with new near-infrared data, the MUSE data show that the rest-frame
Ly α equivalent width (EW) is ≈100 Å. This is a factor 4 higher than the EW measured
in low-redshift analogues with carefully matched Ly α profiles (and thus arguably
H I column density), but this EW can plausibly be explained by star formation.
Alternative scenarios requiring active galactic nucleus (AGN) powering are also
disfavoured by the narrower and steeper Ly α spectrum and much smaller IR to UV
ratio compared to obscured AGN in other Ly α blobs. CR7’s Ly α emission, while
extremely luminous, resembles the emission in more common LAEs at lower redshifts
very well and is likely powered by a young metal-poor starburst.
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: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Ruari
full_name: Mackenzie, Ruari
last_name: Mackenzie
- first_name: Sebastiano
full_name: Cantalupo, Sebastiano
last_name: Cantalupo
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- first_name: Floriane
full_name: Leclercq, Floriane
last_name: Leclercq
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
- first_name: Simon
full_name: Lilly, Simon
last_name: Lilly
- first_name: Leindert
full_name: Boogaard, Leindert
last_name: Boogaard
- first_name: Raffaella
full_name: Marino, Raffaella
last_name: Marino
- first_name: Michael
full_name: Maseda, Michael
last_name: Maseda
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
citation:
ama: 'Matthee JJ, Pezzulli G, Mackenzie R, et al. The nature of CR7 revealed with
MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly
Notices of the Royal Astronomical Society. 2020;498(2):3043-3059. doi:10.1093/mnras/staa2550'
apa: 'Matthee, J. J., Pezzulli, G., Mackenzie, R., Cantalupo, S., Kusakabe, H.,
Leclercq, F., … Nanayakkara, T. (2020). The nature of CR7 revealed with MUSE:
A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices
of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa2550'
chicago: 'Matthee, Jorryt J, Gabriele Pezzulli, Ruari Mackenzie, Sebastiano Cantalupo,
Haruka Kusakabe, Floriane Leclercq, David Sobral, et al. “The Nature of CR7 Revealed
with MUSE: A Young Starburst Powering Extended Ly α Emission at z = 6.6.” Monthly
Notices of the Royal Astronomical Society. Oxford University Press, 2020.
https://doi.org/10.1093/mnras/staa2550.'
ieee: 'J. J. Matthee et al., “The nature of CR7 revealed with MUSE: A young
starburst powering extended Ly α emission at z = 6.6,” Monthly Notices of the
Royal Astronomical Society, vol. 498, no. 2. Oxford University Press, pp.
3043–3059, 2020.'
ista: 'Matthee JJ, Pezzulli G, Mackenzie R, Cantalupo S, Kusakabe H, Leclercq F,
Sobral D, Richard J, Wisotzki L, Lilly S, Boogaard L, Marino R, Maseda M, Nanayakkara
T. 2020. The nature of CR7 revealed with MUSE: A young starburst powering extended
Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. 498(2),
3043–3059.'
mla: 'Matthee, Jorryt J., et al. “The Nature of CR7 Revealed with MUSE: A Young
Starburst Powering Extended Ly α Emission at z = 6.6.” Monthly Notices of the
Royal Astronomical Society, vol. 498, no. 2, Oxford University Press, 2020,
pp. 3043–59, doi:10.1093/mnras/staa2550.'
short: J.J. Matthee, G. Pezzulli, R. Mackenzie, S. Cantalupo, H. Kusakabe, F. Leclercq,
D. Sobral, J. Richard, L. Wisotzki, S. Lilly, L. Boogaard, R. Marino, M. Maseda,
T. Nanayakkara, Monthly Notices of the Royal Astronomical Society 498 (2020) 3043–3059.
date_created: 2022-07-07T10:36:01Z
date_published: 2020-10-01T00:00:00Z
date_updated: 2022-08-18T11:04:05Z
day: '01'
doi: 10.1093/mnras/staa2550
extern: '1'
external_id:
arxiv:
- '2008.01731'
intvolume: ' 498'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- dark ages
- reionization
- first stars
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2008.01731
month: '10'
oa: 1
oa_version: Preprint
page: 3043-3059
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 nature of CR7 revealed with MUSE: A young starburst powering extended
Ly α emission at z = 6.6'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 498
year: '2020'
...
---
_id: '11534'
abstract:
- lang: eng
text: The observed properties of the Lyman-α (Ly α) emission line are a powerful
probe of neutral gas in and around galaxies. We present spatially resolved Ly α
spectroscopy with VLT/MUSE targeting VR7, a UV-luminous galaxy at z = 6.532 with
moderate Ly α equivalent width (EW0 ≈ 38 Å). These data are combined with deep
resolved [CII]158μm spectroscopy obtained with ALMA and UV imaging from HST and
we also detect UV continuum with MUSE. Ly α emission is clearly detected with
S/N ≈ 40 and FWHM of 374 km s−1. Ly α and [C II] are similarly extended beyond
the UV, with effective radius reff = 2.1 ± 0.2 kpc for a single exponential model
or reff,Lyα,halo=3.45+1.08−0.87 kpc when measured jointly with the UV continuum.
The Ly α profile is broader and redshifted with respect to the [C II] line (by
213 km s−1), but there are spatial variations that are qualitatively similar in
both lines and coincide with resolved UV components. This suggests that the emission
originates from two components with plausibly different H I column densities.
We place VR7 in the context of other galaxies at similar and lower redshift. The
Ly α halo scale length is similar at different redshifts and velocity shifts with
respect to the systemic are typically smaller. Overall, we find little indications
of a more neutral vicinity at higher redshift. This means that the local (∼10 kpc)
neutral gas conditions that determine the observed Ly α properties in VR7 resemble
the conditions in post-reionization galaxies.
acknowledgement: 'We thank the referee for their suggestions and constructive comments
that helped to improve the presentation of our results. Based on observations obtained
with the Very Large Telescope, program 99.A-0462. Based on observations made with
the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-26555. These observations are associated with program
#14699. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.01451.S.
ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS
(Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic
of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory
is operated by ESO, AUI/NRAO, and NAOJ. MG acknowledges support from NASA grant
NNX17AK58G. GP and SC gratefully acknowledge support from Swiss National Science
Foundation grant PP00P2 163824. BD acknowledges financial support from the National
Science Foundation, grant number 1716907. We have benefited greatly from the public
available programming language PYTHON, including the NUMPY, MATPLOTLIB, SCIPY (Jones
et al. 2001; Hunter 2007; van der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy
Collaboration 2013) packages, the astronomical imaging tools SEXTRACTOR, SWARP,
and SCAMP (Bertin & Arnouts 1996; Bertin 2006, 2010) and the TOPCAT analysis tool
(Taylor 2013).'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Sebastiano
full_name: Cantalupo, Sebastiano
last_name: Cantalupo
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
- first_name: Behnam
full_name: Darvish, Behnam
last_name: Darvish
- first_name: Sérgio
full_name: Santos, Sérgio
last_name: Santos
citation:
ama: Matthee JJ, Sobral D, Gronke M, et al. Resolved Lyman-α properties of a luminous
Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices
of the Royal Astronomical Society. 2020;492(2):1778-1790. doi:10.1093/mnras/stz3554
apa: Matthee, J. J., Sobral, D., Gronke, M., Pezzulli, G., Cantalupo, S., Röttgering,
H., … Santos, S. (2020). Resolved Lyman-α properties of a luminous Lyman-break
galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal
Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz3554
chicago: Matthee, Jorryt J, David Sobral, Max Gronke, Gabriele Pezzulli, Sebastiano
Cantalupo, Huub Röttgering, Behnam Darvish, and Sérgio Santos. “Resolved Lyman-α
Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53
.” Monthly Notices of the Royal Astronomical Society. Oxford University
Press, 2020. https://doi.org/10.1093/mnras/stz3554.
ieee: J. J. Matthee et al., “Resolved Lyman-α properties of a luminous Lyman-break
galaxy in a large ionized bubble at z = 6.53 ,” Monthly Notices of the Royal
Astronomical Society, vol. 492, no. 2. Oxford University Press, pp. 1778–1790,
2020.
ista: Matthee JJ, Sobral D, Gronke M, Pezzulli G, Cantalupo S, Röttgering H, Darvish
B, Santos S. 2020. Resolved Lyman-α properties of a luminous Lyman-break galaxy
in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical
Society. 492(2), 1778–1790.
mla: Matthee, Jorryt J., et al. “Resolved Lyman-α Properties of a Luminous Lyman-Break
Galaxy in a Large Ionized Bubble at z = 6.53 .” Monthly Notices of the Royal
Astronomical Society, vol. 492, no. 2, Oxford University Press, 2020, pp.
1778–90, doi:10.1093/mnras/stz3554.
short: J.J. Matthee, D. Sobral, M. Gronke, G. Pezzulli, S. Cantalupo, H. Röttgering,
B. Darvish, S. Santos, Monthly Notices of the Royal Astronomical Society 492 (2020)
1778–1790.
date_created: 2022-07-07T12:21:36Z
date_published: 2020-02-01T00:00:00Z
date_updated: 2022-08-18T11:29:53Z
day: '01'
doi: 10.1093/mnras/stz3554
extern: '1'
external_id:
arxiv:
- '1909.06376'
intvolume: ' 492'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- dark ages
- reionization
- first stars
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1909.06376
month: '02'
oa: 1
oa_version: Preprint
page: 1778-1790
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: 'Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized
bubble at z = 6.53 '
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 492
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. Monthly Notices of the Royal Astronomical Society. 2020;493(3):3341-3362.
doi:10.1093/mnras/staa476'
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. Monthly
Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa476'
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.” Monthly Notices of the Royal
Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa476.'
ieee: 'J. Calhau 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,”
Monthly Notices of the Royal Astronomical Society, 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.”
Monthly Notices of the Royal Astronomical Society, vol. 493, no. 3, Oxford
University Press, 2020, pp. 3341–62, doi:10.1093/mnras/staa476.'
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: '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. Monthly
Notices of the Royal Astronomical Society. 2019;489(1):555-573. doi:10.1093/mnras/stz2149'
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. Monthly Notices
of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz2149'
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.” Monthly Notices of the Royal Astronomical Society. Oxford
University Press, 2019. https://doi.org/10.1093/mnras/stz2149.'
ieee: 'A. A. Khostovan et al., “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, 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.” Monthly Notices
of the Royal Astronomical Society, vol. 489, no. 1, Oxford University Press,
2019, pp. 555–73, doi:10.1093/mnras/stz2149.'
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: '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: '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. Monthly Notices of the Royal Astronomical Society. 2018;478(3):2999-3015.
doi:10.1093/mnras/sty925'
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. Monthly Notices
of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty925'
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.” Monthly Notices of the Royal Astronomical Society. Oxford University
Press, 2018. https://doi.org/10.1093/mnras/sty925.'
ieee: 'A. A. Khostovan et al., “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, 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.” Monthly Notices
of the Royal Astronomical Society, vol. 478, no. 3, Oxford University Press,
2018, pp. 2999–3015, doi:10.1093/mnras/sty925.'
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: '11557'
abstract:
- lang: eng
text: Deep narrow-band surveys have revealed a large population of faint Ly α emitters
(LAEs) in the distant Universe, but relatively little is known about the most
luminous sources (LLyα≳1042.7 erg s−1; LLyα≳L∗Lyα). Here we present the spectroscopic
follow-up of 21 luminous LAEs at z ∼ 2–3 found with panoramic narrow-band surveys
over five independent extragalactic fields (≈4 × 106 Mpc3 surveyed at z ∼ 2.2
and z ∼ 3.1). We use WHT/ISIS, Keck/DEIMOS, and VLT/X-SHOOTER to study these sources
using high ionization UV lines. Luminous LAEs at z ∼ 2–3 have blue UV slopes (β=−2.0+0.3−0.1)
and high Ly α escape fractions (50+20−15 per cent) and span five orders of magnitude
in UV luminosity (MUV ≈ −19 to −24). Many (70 per cent) show at least one high
ionization rest-frame UV line such as C IV, N V, C III], He II or O III], typically
blue-shifted by ≈100–200 km s−1 relative to Ly α. Their Ly α profiles reveal a
wide variety of shapes, including significant blue-shifted components and widths
from 200 to 4000 km s−1. Overall, 60 ± 11 per cent appear to be active galactic
nucleus (AGN) dominated, and at LLyα > 1043.3 erg s−1 and/or MUV < −21.5 virtually
all LAEs are AGNs with high ionization parameters (log U = 0.6 ± 0.5) and with
metallicities of ≈0.5 − 1 Z⊙. Those lacking signatures of AGNs (40 ± 11 per cent)
have lower ionization parameters (logU=−3.0+1.6−0.9 and log ξion = 25.4 ± 0.2)
and are apparently metal-poor sources likely powered by young, dust-poor ‘maximal’
starbursts. Our results show that luminous LAEs at z ∼ 2–3 are a diverse population
and that 2×L∗Lyα and 2×M∗UV mark a sharp transition in the nature of LAEs, from
star formation dominated to AGN dominated.
acknowledgement: 'We thank the anonymous reviewer for their timely and constructive
comments that greatly helped us to improve the manuscript. 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. 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, and the National Science
Foundation, grant number 1716907. IRS acknowledges support from the ERC Advanced
Grant DUSTYGAL (321334), STFC (ST/P000541/1), and a Royal Society/Wolfson Merit
Award. PNB is grateful for support from STFC via grant ST/M001229/1. We thank Anne
Verhamme, Kimihiko Nakajima, Ryan Trainor, Sangeeta Malhotra, Max Gronke, James
Rhoads, Fang Xia An, Matthew Hayes, Takashi Kojima, Mark Dijkstra, and Anne Jaskot
for many helpful and engaging discussions, particularly during the SnowCLAW Ly α
workshop. We thank Bruno Ribeiro, Stephane Charlot, and Joseph Caruana for comments
on the manuscript. The authors would also like to thank Ingrid Tengs, Meg Singleton,
Ali Khostovan, and Sara Perez for participating in part of the observations. We
also thank Joao Calhau, Leah Morabito, Sergio Santos, and Aayush Saxena for their
assistance with the narrow-band observations which allowed to select some of the
sour ces. Based on observations obtained with the William Herschel Telescope, program:
W16AN004; the Very Large Telescope, programs: 098.A-0819 & 099.A-0254; and the Keck
II telescope, program: C267D. 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.A-0943, 098.A-0819, 099.A-0254 and 179.A-2005.
The authors acknowledge the award of service time (SW2014b20) on the 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. The authors would also like to thank all the extremely
helpful observatory staff that have greatly contributed towards our observations,
particularly Fiona Riddick, Lilian Dominguez, Florencia Jimenez, and Ian Skillen.
We have benefited greatly from the publicly available programming language PYTHON,
including the NUMPY & SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al.
2001), 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.'
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: Ian
full_name: Smail, Ian
last_name: Smail
- first_name: Philip N
full_name: Best, Philip N
last_name: Best
- first_name: Lara
full_name: Alegre, Lara
last_name: Alegre
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
- first_name: Bahram
full_name: Mobasher, Bahram
last_name: Mobasher
- first_name: Ana
full_name: Paulino-Afonso, Ana
last_name: Paulino-Afonso
- first_name: Andra
full_name: Stroe, Andra
last_name: Stroe
- first_name: Iván
full_name: Oteo, Iván
last_name: Oteo
citation:
ama: 'Sobral D, Matthee JJ, Darvish B, et al. The nature of luminous Ly α emitters
at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly Notices
of the Royal Astronomical Society. 2018;477(2):2817-2840. doi:10.1093/mnras/sty782'
apa: 'Sobral, D., Matthee, J. J., Darvish, B., Smail, I., Best, P. N., Alegre, L.,
… Oteo, I. (2018). The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor
starbursts and highly ionizing AGN. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/sty782'
chicago: 'Sobral, David, Jorryt J Matthee, Behnam Darvish, Ian Smail, Philip N Best,
Lara Alegre, Huub Röttgering, et al. “The Nature of Luminous Ly α Emitters at
z ∼ 2–3: Maximal Dust-Poor Starbursts and Highly Ionizing AGN.” Monthly Notices
of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty782.'
ieee: 'D. Sobral et al., “The nature of luminous Ly α emitters at z ∼ 2–3:
Maximal dust-poor starbursts and highly ionizing AGN,” Monthly Notices of the
Royal Astronomical Society, vol. 477, no. 2. Oxford University Press, pp.
2817–2840, 2018.'
ista: 'Sobral D, Matthee JJ, Darvish B, Smail I, Best PN, Alegre L, Röttgering H,
Mobasher B, Paulino-Afonso A, Stroe A, Oteo I. 2018. The nature of luminous Ly
α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly
Notices of the Royal Astronomical Society. 477(2), 2817–2840.'
mla: 'Sobral, David, et al. “The Nature of Luminous Ly α Emitters at z ∼ 2–3: Maximal
Dust-Poor Starbursts and Highly Ionizing AGN.” Monthly Notices of the Royal
Astronomical Society, vol. 477, no. 2, Oxford University Press, 2018, pp.
2817–40, doi:10.1093/mnras/sty782.'
short: D. Sobral, J.J. Matthee, B. Darvish, I. Smail, P.N. Best, L. Alegre, H. Röttgering,
B. Mobasher, A. Paulino-Afonso, A. Stroe, I. Oteo, Monthly Notices of the Royal
Astronomical Society 477 (2018) 2817–2840.
date_created: 2022-07-12T07:18:02Z
date_published: 2018-06-01T00:00:00Z
date_updated: 2022-08-19T07:01:08Z
day: '01'
doi: 10.1093/mnras/sty782
extern: '1'
external_id:
arxiv:
- '1802.10102'
intvolume: ' 477'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: active'
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: ISM'
- 'galaxies: starburst'
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1802.10102
month: '06'
oa: 1
oa_version: Preprint
page: 2817-2840
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 nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts
and highly ionizing AGN'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 477
year: '2018'
...
---
_id: '11562'
abstract:
- lang: eng
text: We present the CAlibrating LYMan-α with Hα (CALYMHA) pilot survey and new
results on Lyman α (Lyα) selected galaxies at z ∼ 2. We use a custom-built Lyα
narrow-band filter at the Isaac Newton Telescope, designed to provide a matched
volume coverage to the z = 2.23 Hα HiZELS survey. Here, we present the first results
for the COSMOS and UDS fields. Our survey currently reaches a 3σ line flux limit
of ∼4 × 10−17 erg s−1 cm−2, and a Lyα luminosity limit of ∼1042.3 erg s−1. We
find 188 Lyα emitters over 7.3 × 105 Mpc3, but also find significant numbers of
other line-emitting sources corresponding to He II, C III] and C IV emission lines.
These sources are important contaminants, and we carefully remove them, unlike
most previous studies. We find that the Lyα luminosity function at z = 2.23 is
very well described by a Schechter function up to LLy α ≈ 1043 erg s−1 with L∗=1042.59+0.16−0.08
erg s−1, ϕ∗=10−3.09+0.14−0.34 Mpc−3 and α = −1.75 ± 0.25. Above LLy α ≈ 1043 erg
s−1, the Lyα luminosity function becomes power-law like, driven by X-ray AGN.
We find that Lyα-selected emitters have a high escape fraction of 37 ± 7 per cent,
anticorrelated with Lyα luminosity and correlated with Lyα equivalent width. Lyα
emitters have ubiquitous large (≈40 kpc) Lyα haloes, ∼2 times larger than their
Hα extents. By directly comparing our Lyα and Hα luminosity functions, we find
that the global/overall escape fraction of Lyα photons (within a 13 kpc radius)
from the full population of star-forming galaxies is 5.1 ± 0.2 per cent at the
peak of the star formation history. An extra 3.3 ± 0.3 per cent of Lyα photons
likely still escape, but at larger radii.
acknowledgement: 'We thank the reviewer for his/her helpful comments and suggestions
that have greatly improved this work. DS and JM acknowledge financial support from
the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship.
DS also acknowledges funding from FCT through an FCT Investigator Starting Grant
and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from
the UK STFC via grant ST/M001229/1. IRS acknowledges support from STFC (ST/L00075X/1),
the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson
merit award. We thank Matthew Hayes, Ryan Trainor, Kimihiko Nakajima and Anne Verhamme
for many helpful discussions and Ana Sobral, Carolina Duarte and Miguel Domingos
for taking part in observations with the NB392 filter. We also thank Sergio Santos
for helpful comments. This research is based on observations obtained on the Isaac
Newton Telescope (INT), programs: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B
& I15AN008. The authors acknowledge the award of time from programmes: I13AN002,
I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008 on the INT. INT is operated
on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio
del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on
observations made with ESO Telescopes at the La Silla Paranal Observatory under
programme ID 098.A 0819. We have benefited greatly from the publicly available programming
language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages,
the astronomical imaging tools SEXTRACTOR, SWARP (Bertin & Arnouts 1996; Bertin
2010), SCAMP (Bertin 2006) and TOPCAT (Taylor 2005). Dedicated to the memory of
M. L. Nicolau and M. C. Serrano.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Philip
full_name: Best, Philip
last_name: Best
- first_name: Andra
full_name: Stroe, Andra
last_name: Stroe
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
- first_name: Iván
full_name: Oteo, Iván
last_name: Oteo
- first_name: Ian
full_name: Smail, Ian
last_name: Smail
- first_name: Leah
full_name: Morabito, Leah
last_name: Morabito
- first_name: Ana
full_name: Paulino-Afonso, Ana
last_name: Paulino-Afonso
citation:
ama: 'Sobral D, Matthee JJ, Best P, et al. The CALYMHA survey: Lyα luminosity function
and global escape fraction of Lyα photons at z = 2.23. Monthly Notices of the
Royal Astronomical Society. 2017;466(1):1242-1258. doi:10.1093/mnras/stw3090'
apa: 'Sobral, D., Matthee, J. J., Best, P., Stroe, A., Röttgering, H., Oteo, I.,
… Paulino-Afonso, A. (2017). The CALYMHA survey: Lyα luminosity function and global
escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stw3090'
chicago: 'Sobral, David, Jorryt J Matthee, Philip Best, Andra Stroe, Huub Röttgering,
Iván Oteo, Ian Smail, Leah Morabito, and Ana Paulino-Afonso. “The CALYMHA Survey:
Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.”
Monthly Notices of the Royal Astronomical Society. Oxford University Press,
2017. https://doi.org/10.1093/mnras/stw3090.'
ieee: 'D. Sobral et al., “The CALYMHA survey: Lyα luminosity function and
global escape fraction of Lyα photons at z = 2.23,” Monthly Notices of the
Royal Astronomical Society, vol. 466, no. 1. Oxford University Press, pp.
1242–1258, 2017.'
ista: 'Sobral D, Matthee JJ, Best P, Stroe A, Röttgering H, Oteo I, Smail I, Morabito
L, Paulino-Afonso A. 2017. The CALYMHA survey: Lyα luminosity function and global
escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical
Society. 466(1), 1242–1258.'
mla: 'Sobral, David, et al. “The CALYMHA Survey: Lyα Luminosity Function and Global
Escape Fraction of Lyα Photons at z = 2.23.” Monthly Notices of the Royal Astronomical
Society, vol. 466, no. 1, Oxford University Press, 2017, pp. 1242–58, doi:10.1093/mnras/stw3090.'
short: D. Sobral, J.J. Matthee, P. Best, A. Stroe, H. Röttgering, I. Oteo, I. Smail,
L. Morabito, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society
466 (2017) 1242–1258.
date_created: 2022-07-12T12:04:16Z
date_published: 2017-04-01T00:00:00Z
date_updated: 2022-08-19T07:18:20Z
day: '01'
doi: 10.1093/mnras/stw3090
extern: '1'
external_id:
arxiv:
- '1609.05897'
intvolume: ' 466'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: haloes'
- 'galaxies: high-redshift'
- 'galaxies: luminosity function'
- mass function
- 'galaxies: statistics'
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1609.05897
month: '04'
oa: 1
oa_version: Preprint
page: 1242-1258
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The CALYMHA survey: Lyα luminosity function and global escape fraction of
Lyα photons at z = 2.23'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 466
year: '2017'
...
---
_id: '11564'
abstract:
- lang: eng
text: We study the production rate of ionizing photons of a sample of 588 Hα emitters
(HAEs) and 160 Lyman-α emitters (LAEs) at z = 2.2 in the COSMOS field in order
to assess the implied emissivity from galaxies, based on their ultraviolet (UV)
luminosity. By exploring the rest-frame Lyman Continuum (LyC) with GALEX/NUV data,
we find fesc < 2.8 (6.4) per cent through median (mean) stacking. By combining
the Hα luminosity density with intergalactic medium emissivity measurements from
absorption studies, we find a globally averaged 〈fesc〉 of 5.9+14.5−4.2 per cent
at z = 2.2 if we assume HAEs are the only source of ionizing photons. We find
similarly low values of the global 〈fesc〉 at z ≈ 3–5, also ruling out a high 〈fesc〉
at z < 5. These low escape fractions allow us to measure ξion, the number of produced
ionizing photons per unit UV luminosity, and investigate how this depends on galaxy
properties. We find a typical ξion ≈ 1024.77 ± 0.04 Hz erg−1 for HAEs and ξion
≈ 1025.14 ± 0.09 Hz erg−1 for LAEs. LAEs and low-mass HAEs at z = 2.2 show similar
values of ξion as typically assumed in the reionization era, while the typical
HAE is three times less ionizing. Due to an increasing ξion with increasing EW(Hα),
ξion likely increases with redshift. This evolution alone is fully in line with
the observed evolution of ξion between z ≈ 2 and 5, indicating a typical value
of ξion ≈ 1025.4 Hz erg−1 in the reionization era.
acknowledgement: "We thank the referee for the many helpful and constructive comments
which have significantly improved this paper. JM acknowledges the support of a Huygens
PhD fellowship from Leiden University. DS acknowledges financial support from the
Netherlands Organization for Scientific research (NWO) through a Veni fellowship
and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010).
PNB is grateful for support from the UK STFC via grant ST/M001229/1. IO acknowledges
support from the European Research Council in the form of the Advanced Investigator
Programme, 321302, COSMICISM. The authors thank Andreas Faisst, Michael Rutkowski
and Andreas Sandberg for answering questions related to this work and Daniel Schaerer
and Mark Dijkstra for discussions. We acknowledge the work that has been done by
both the COSMOS team in assembling such large, state-of-the-art multi-wavelength
data set, as this has been crucial for the results presented in this paper. We have
benefited greatly from the public available programming language PYTHON, including
the NUMPY, MATPLOTLIB, PYFITS, SCIPY (Jones et al. 2001; Hunter 2007; Van Der Walt,
Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration et al. 2013) packages,
the astronomical imaging tools SEXTRACTOR and SWARP (Bertin & Arnouts 1996;\r\nBertin
2010) and the TOPCAT analysis program (Taylor 2013)."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Philip
full_name: Best, Philip
last_name: Best
- first_name: Ali Ahmad
full_name: Khostovan, Ali Ahmad
last_name: Khostovan
- first_name: Iván
full_name: Oteo, Iván
last_name: Oteo
- first_name: Rychard
full_name: Bouwens, Rychard
last_name: Bouwens
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
citation:
ama: Matthee JJ, Sobral D, Best P, et al. The production and escape of Lyman-Continuum
radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. Monthly
Notices of the Royal Astronomical Society. 2017;465(3):3637-3655. doi:10.1093/mnras/stw2973
apa: Matthee, J. J., Sobral, D., Best, P., Khostovan, A. A., Oteo, I., Bouwens,
R., & Röttgering, H. (2017). The production and escape of Lyman-Continuum
radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. Monthly
Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw2973
chicago: Matthee, Jorryt J, David Sobral, Philip Best, Ali Ahmad Khostovan, Iván
Oteo, Rychard Bouwens, and Huub Röttgering. “The Production and Escape of Lyman-Continuum
Radiation from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” Monthly
Notices of the Royal Astronomical Society. Oxford University Press, 2017.
https://doi.org/10.1093/mnras/stw2973.
ieee: J. J. Matthee et al., “The production and escape of Lyman-Continuum
radiation from star-forming galaxies at z ∼ 2 and their redshift evolution,” Monthly
Notices of the Royal Astronomical Society, vol. 465, no. 3. Oxford University
Press, pp. 3637–3655, 2017.
ista: Matthee JJ, Sobral D, Best P, Khostovan AA, Oteo I, Bouwens R, Röttgering
H. 2017. The production and escape of Lyman-Continuum radiation from star-forming
galaxies at z ∼ 2 and their redshift evolution. Monthly Notices of the Royal Astronomical
Society. 465(3), 3637–3655.
mla: Matthee, Jorryt J., et al. “The Production and Escape of Lyman-Continuum Radiation
from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” Monthly
Notices of the Royal Astronomical Society, vol. 465, no. 3, Oxford University
Press, 2017, pp. 3637–55, doi:10.1093/mnras/stw2973.
short: J.J. Matthee, D. Sobral, P. Best, A.A. Khostovan, I. Oteo, R. Bouwens, H.
Röttgering, Monthly Notices of the Royal Astronomical Society 465 (2017) 3637–3655.
date_created: 2022-07-12T12:12:14Z
date_published: 2017-03-01T00:00:00Z
date_updated: 2022-08-19T07:53:04Z
day: '01'
doi: 10.1093/mnras/stw2973
extern: '1'
external_id:
arxiv:
- '1605.08782'
intvolume: ' 465'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'cosmology: observations'
- dark ages
- reionization
- first stars
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1605.08782
month: '03'
oa: 1
oa_version: Preprint
page: 3637-3655
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The production and escape of Lyman-Continuum radiation from star-forming galaxies
at z ∼ 2 and their redshift evolution
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 465
year: '2017'
...
---
_id: '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 . Monthly Notices of the Royal Astronomical Society. 2017;471(3):2558-2574.
doi:10.1093/mnras/stx1712
apa: Stroe, A., Sobral, D., Matthee, J. J., 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.
Oxford University Press. https://doi.org/10.1093/mnras/stx1712
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 .” Monthly Notices of the Royal Astronomical
Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stx1712.
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 ,” Monthly Notices of the Royal Astronomical Society,
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 .” Monthly Notices
of the Royal Astronomical Society, vol. 471, no. 3, Oxford University Press,
2017, pp. 2558–74, doi:10.1093/mnras/stx1712.
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. Monthly Notices of the Royal Astronomical Society. 2017;471(3):2575-2586.
doi:10.1093/mnras/stx1713
apa: Stroe, A., Sobral, D., Matthee, J. J., 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. Oxford University Press. https://doi.org/10.1093/mnras/stx1713
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.” Monthly Notices of the Royal Astronomical
Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stx1713.
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,” Monthly Notices of the Royal Astronomical Society,
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.” Monthly
Notices of the Royal Astronomical Society, vol. 471, no. 3, Oxford University
Press, 2017, pp. 2575–86, doi:10.1093/mnras/stx1713.
short: A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of
the Royal Astronomical Society 471 (2017) 2575–2586.
date_created: 2022-07-12T12:54:57Z
date_published: 2017-11-01T00:00:00Z
date_updated: 2022-08-19T08:02:04Z
day: '01'
doi: 10.1093/mnras/stx1713
extern: '1'
external_id:
arxiv:
- '1703.10169'
intvolume: ' 471'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: active'
- 'galaxies: high redshift'
- 'galaxies: luminosity function'
- mass function
- 'quasars: emission lines'
- star formation
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1703.10169
month: '11'
oa: 1
oa_version: Preprint
page: 2575-2586
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity
functions and cosmic average line ratios
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...
---
_id: '11572'
abstract:
- lang: eng
text: We present spectroscopic follow-up of candidate luminous Ly α emitters (LAEs)
at z = 5.7–6.6 in the SA22 field with VLT/X-SHOOTER. We confirm two new luminous
LAEs at z = 5.676 (SR6) and z = 6.532 (VR7), and also present HST follow-up of
both sources. These sources have luminosities LLy α ≈ 3 × 1043 erg s−1, very high
rest-frame equivalent widths of EW0 ≳ 200 Å and narrow Ly α lines (200–340 km s−1).
VR7 is the most UV-luminous LAE at z > 6.5, with M1500 = −22.5, even brighter
in the UV than CR7. Besides Ly α, we do not detect any other rest-frame UV lines
in the spectra of SR6 and VR7, and argue that rest-frame UV lines are easier to
observe in bright galaxies with low Ly α equivalent widths. We confirm that Ly α
line widths increase with Ly α luminosity at z = 5.7, while there are indications
that Ly α lines of faint LAEs become broader at z = 6.6, potentially due to reionization.
We find a large spread of up to 3 dex in UV luminosity for >L⋆ LAEs, but find
that the Ly α luminosity of the brightest LAEs is strongly related to UV luminosity
at z = 6.6. Under basic assumptions, we find that several LAEs at z ≈ 6–7 have
Ly α escape fractions ≳ 100 per cent, indicating bursty star formation histories,
alternative Ly α production mechanisms, or dust attenuating Ly α emission differently
than UV emission. Finally, we present a method to compute ξion, the production
efficiency of ionizing photons, and find that LAEs at z ≈ 6–7 have high values
of log10(ξion/Hz erg−1) ≈ 25.51 ± 0.09 that may alleviate the need for high Lyman-Continuum
escape fractions required for reionization.
acknowledgement: 'We thank the referee for a constructive report that has improved
the quality and clarity of this work. The authors thank Grecco Oyarzún for discussions.
JM acknowledges the support of a Huygens PhD fellowship from Leiden University.
DS acknowledges financial support from the Netherlands Organisation for Scientific
research (NWO) through a Veni fellowship and from Lancaster University through an
Early Career Internal Grant A100679. BD acknowledges financial support from NASA
through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G.
We thank Kasper Schmidt for providing measurements. Based on observations with the
W.M. Keck Observatory through programme C267D. The W.M. Keck Observatory is operated
as a scientific partnership amongst the California Institute of Technology, the
University of California and the National Aeronautics and Space Administration.
Based on observations made with ESO Telescopes at the La Silla Paranal Observatory
under programme IDs 097.A-0943, 294.A 5018 and 098.A-0819 and on data products produced
by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.
The authors acknowledge the award of observing time (W16AN004) and of service time
(SW2014b20) on the William Herschel Telescope (WHT). WHT and its service programme
are operated on the island of La Palma by the Isaac Newton Group in the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.
Based on observations made with the NASA/ESA HST, obtained (from the Data Archive)
at the Space Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These
observations are associated with programme #14699. We are grateful for the excellent
data sets from the COSMOS, UltraVISTA, SXDS, UDS and CFHTLS survey teams; without
these legacy surveys, this research would have been impossible. We have benefited
from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB,
PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP
and SCAMP and the TOPCAT analysis tool (Taylor 2013).'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Behnam
full_name: Darvish, Behnam
last_name: Darvish
- first_name: Sérgio
full_name: Santos, Sérgio
last_name: Santos
- first_name: Bahram
full_name: Mobasher, Bahram
last_name: Mobasher
- first_name: Ana
full_name: Paulino-Afonso, Ana
last_name: Paulino-Afonso
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
- first_name: Lara
full_name: Alegre, Lara
last_name: Alegre
citation:
ama: Matthee JJ, Sobral D, Darvish B, et al. Spectroscopic properties of luminous
Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. Monthly
Notices of the Royal Astronomical Society. 2017;472(1):772-787. doi:10.1093/mnras/stx2061
apa: Matthee, J. J., Sobral, D., Darvish, B., Santos, S., Mobasher, B., Paulino-Afonso,
A., … Alegre, L. (2017). Spectroscopic properties of luminous Ly α emitters at
z ≈ 6–7 and comparison to the Lyman-break population. Monthly Notices of the
Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stx2061
chicago: Matthee, Jorryt J, David Sobral, Behnam Darvish, Sérgio Santos, Bahram
Mobasher, Ana Paulino-Afonso, Huub Röttgering, and Lara Alegre. “Spectroscopic
Properties of Luminous Ly α Emitters at z ≈ 6–7 and Comparison to the Lyman-Break
Population.” Monthly Notices of the Royal Astronomical Society. Oxford
University Press, 2017. https://doi.org/10.1093/mnras/stx2061.
ieee: J. J. Matthee et al., “Spectroscopic properties of luminous Ly α emitters
at z ≈ 6–7 and comparison to the Lyman-break population,” Monthly Notices of
the Royal Astronomical Society, vol. 472, no. 1. Oxford University Press,
pp. 772–787, 2017.
ista: Matthee JJ, Sobral D, Darvish B, Santos S, Mobasher B, Paulino-Afonso A, Röttgering
H, Alegre L. 2017. Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7
and comparison to the Lyman-break population. Monthly Notices of the Royal Astronomical
Society. 472(1), 772–787.
mla: Matthee, Jorryt J., et al. “Spectroscopic Properties of Luminous Ly α Emitters
at z ≈ 6–7 and Comparison to the Lyman-Break Population.” Monthly Notices of
the Royal Astronomical Society, vol. 472, no. 1, Oxford University Press,
2017, pp. 772–87, doi:10.1093/mnras/stx2061.
short: J.J. Matthee, D. Sobral, B. Darvish, S. Santos, B. Mobasher, A. Paulino-Afonso,
H. Röttgering, L. Alegre, Monthly Notices of the Royal Astronomical Society 472
(2017) 772–787.
date_created: 2022-07-13T09:47:39Z
date_published: 2017-11-01T00:00:00Z
date_updated: 2022-08-19T08:05:37Z
day: '01'
doi: 10.1093/mnras/stx2061
extern: '1'
external_id:
arxiv:
- '1706.06591'
intvolume: ' 472'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution – galaxies: high-redshift'
- dark ages
- reionization
- first stars
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1706.06591
month: '11'
oa: 1
oa_version: Preprint
page: 772-787
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison
to the Lyman-break population
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 472
year: '2017'
...
---
_id: '11574'
abstract:
- lang: eng
text: We present new results from the widest narrow-band survey search for Lyα emitters
at z = 5.7, just after reionization. We survey a total of 7 deg2 spread over the
COSMOS, UDS and SA22 fields. We find over 11 000 line emitters, out of which 514
are robust Lyα candidates at z = 5.7 within a volume of 6.3 × 106 Mpc3. Our Lyα
emitters span a wide range in Lyα luminosities, from faint to bright (LLyα ∼ 1042.5–44
erg s−1) and rest-frame equivalent widths (EW0 ∼ 25–1000 Å) in a single, homogeneous
data set. By combining all our fields, we find that the faint end slope of the
z = 5.7 Lyα luminosity function is very steep, with α=−2.3+0.4−0.3. We also present
an updated z = 6.6 Lyα luminosity function, based on comparable volumes and obtained
with the same methods, which we directly compare with that at z = 5.7. We find
a significant decline of the number density of faint Lyα emitters from z = 5.7
to 6.6 (by 0.5 ± 0.1 dex), but no evolution at the bright end/no evolution in
L*. Faint Lyα emitters at z = 6.6 show much more extended haloes than those at
z = 5.7, suggesting that neutral Hydrogen plays an important role, increasing
the scattering and leading to observations missing faint Lyα emission within the
epoch of reionization. Altogether, our results suggest that we are observing patchy
reionization which happens first around the brightest Lyα emitters, allowing the
number densities of those sources to remain unaffected by the increase of neutral
Hydrogen fraction from z ∼ 5 to 7.
acknowledgement: 'We thank the anonymous referee for useful and constructive comments
and suggestions which greatly improved the quality and clarity of our work. The
authors acknowledge financial support from the Netherlands Organisation for Scientific
research (NWO) through a Veni fellowship. SS and DS acknowledge funding from FCT
through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010).
SS also acknowledges support from FCT through the research grants UID/FIS/04434/2013
and PTDC/FIS-AST/2194/2012. JM acknowledges a Huygens PhD fellowship from Leiden
University. Based on observations with the Subaru Telescope (Program IDs: S05B-027,
S06A-025, S06B-010, S07A-013, S07B-008, S08B-008, S09A-017, S14A-086). Based on
observations made with ESO Telescopes at the La Silla Paranal Observatory under
programme ID 294.A-5018. Based on observations obtained with MegaPrime/Megacam,
a joint project of CFHT and CEA/IRFU, at the Canada–France–Hawaii Telescope (CFHT)
which is operated by the National Research Council (NRC) of Canada, the Institut
National des Science de l’Univers of the Centre National de la Recherche Scientifique
(CNRS) of France, and the University of Hawaii. This work is based in part on data
products produced at TERAPIX available at the Canadian Astronomy Data Centre as
part of the Canada–France–Hawaii Telescope Legacy Survey, a collaborative project
of NRC and CNRS. Based on data products from observations made with ESO Telescopes
at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data
products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of
the UltraVISTA consortium. We are grateful to the CFHTLS, COSMOS-UltraVISTA, UKIDSS,
SXDF and COSMOS survey teams. Without these legacy surveys, this research would
have been impossible. The authors wish to recognize and acknowledge the very significant
cultural role and reverence that the summit of Mauna Kea has always had within the
indigenous Hawaiian community. We are most fortunate to have the opportunity to
conduct and explore observations from this mountain. Finally, the authors acknowledge
the unique value of the publicly available programming language PYTHON, including
the NUMPY, PYFITS, MATPLOTLIB, SCIPY and ASTROPY (Astropy Collaboration et al.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Sérgio
full_name: Santos, Sérgio
last_name: Santos
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
citation:
ama: 'Santos S, Sobral D, Matthee JJ. The Lyα luminosity function at z= 5.7–6.6
and the steep drop of the faint end: Implications for reionization. Monthly
Notices of the Royal Astronomical Society. 2016;463(2):1678-1691. doi:10.1093/mnras/stw2076'
apa: 'Santos, S., Sobral, D., & Matthee, J. J. (2016). The Lyα luminosity function
at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization.
Monthly Notices of the Royal Astronomical Society. Oxford University Press.
https://doi.org/10.1093/mnras/stw2076'
chicago: 'Santos, Sérgio, David Sobral, and Jorryt J Matthee. “The Lyα Luminosity
Function at Z= 5.7–6.6 and the Steep Drop of the Faint End: Implications for Reionization.”
Monthly Notices of the Royal Astronomical Society. Oxford University Press,
2016. https://doi.org/10.1093/mnras/stw2076.'
ieee: 'S. Santos, D. Sobral, and J. J. Matthee, “The Lyα luminosity function at
z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization,”
Monthly Notices of the Royal Astronomical Society, vol. 463, no. 2. Oxford
University Press, pp. 1678–1691, 2016.'
ista: 'Santos S, Sobral D, Matthee JJ. 2016. The Lyα luminosity function at z= 5.7–6.6
and the steep drop of the faint end: Implications for reionization. Monthly Notices
of the Royal Astronomical Society. 463(2), 1678–1691.'
mla: 'Santos, Sérgio, et al. “The Lyα Luminosity Function at Z= 5.7–6.6 and the
Steep Drop of the Faint End: Implications for Reionization.” Monthly Notices
of the Royal Astronomical Society, vol. 463, no. 2, Oxford University Press,
2016, pp. 1678–91, doi:10.1093/mnras/stw2076.'
short: S. Santos, D. Sobral, J.J. Matthee, Monthly Notices of the Royal Astronomical
Society 463 (2016) 1678–1691.
date_created: 2022-07-13T10:08:20Z
date_published: 2016-12-01T00:00:00Z
date_updated: 2022-08-19T08:09:54Z
day: '01'
doi: 10.1093/mnras/stw2076
extern: '1'
external_id:
arxiv:
- '1606.07435'
intvolume: ' 463'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift'
- 'galaxies: luminosity function'
- mass function
- 'cosmology: observations'
- dark ages
- reionization
- first stars
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1606.07435
month: '12'
oa: 1
oa_version: Preprint
page: 1678-1691
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint
end: Implications for reionization'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 463
year: '2016'
...
---
_id: '11576'
abstract:
- lang: eng
text: We use new near-infrared spectroscopic observations to investigate the nature
and evolution of the most luminous Hα emitters at z ∼ 0.8–2.23, which evolve strongly
in number density over this period, and compare them to more typical Hα emitters.
We study 59 luminous Hα emitters with LHα > L∗Hα, roughly equally split per redshift
slice at z ∼ 0.8, 1.47 and 2.23 from the HiZELS and CF-HiZELS surveys. We find
that, overall, 30 ± 8 per cent are active galactic nuclei [AGNs; 80 ± 30 per cent
of these AGNs are broad-line AGNs, BL-AGNs], and we find little to no evolution
in the AGN fraction with redshift, within the errors. However, the AGN fraction
increases strongly with Hα luminosity and correlates best with LHα/L∗Hα(z). While
LHα ≤ L∗Hα(z) Hα emitters are largely dominated by star-forming galaxies (>80
per cent), the most luminous Hα emitters (LHα>10L∗Hα(z)) at any cosmic time
are essentially all BL-AGN. Using our AGN-decontaminated sample of luminous star-forming
galaxies, and integrating down to a fixed Hα luminosity, we find a factor of ∼1300
evolution in the star formation rate density from z = 0 to 2.23. This is much
stronger than the evolution from typical Hα star-forming galaxies and in line
with the evolution seen for constant luminosity cuts used to select ‘ultraluminous’
infrared galaxies and/or sub-millimetre galaxies. By taking into account the evolution
in the typical Hα luminosity, we show that the most strongly star-forming Hα-selected
galaxies at any epoch (LHα>L∗Hα(z)) contribute the same fractional amount of
≈15 per cent to the total star formation rate density, at least up to z = 2.23.
acknowledgement: "The authors would like to thank the anonymous reviewer for the many
helpful comments and suggestions which greatly improved the clarity and quality
of this work. DS and SAK acknowledge financial support from the Netherlands Organisation
for Scientific research (NWO) through a Veni fellowship. DS also acknowledges funding
from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010)
and from FCT grant PEst-OE/FIS/UI2751/2014. Part of this project was undertaken
during the inaugural Leiden/ESA Astrophysics Program for Summer Students (LEAPS).
IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator
programme DUSTYGAL 321334 and a Royal Society/Wolfson merit award. CH acknowledges
support from STFC. Based on observations made with ESO Telescopes at the La Silla
Paranal Observatory under programme ID 087.A-0337 and ID 089.A-0965. Also based
on data from the Telescopio Nazionale Galileo, with time awarded through OPTICON
programmes 2011A/026 and 2012A020 and the William Herschel Telescope under programme
W12BN007. The William Herschel Telescope is operated on the island of La Palma by
the Isaac Newton Group in the Spanish\r\nObservatorio del Roque de los Muchachos
of the Instituto de Astrofisica de Canarias. The authors wish to thank all the help
given by the telescope staff from all the observatories used in this study: ESO
staff in La Silla, and the TNG and WHT staff in La Palma. This publication makes
use of data products from the Two Micron All-Sky Survey, which is a joint project
of the University of Massachusetts and the Infrared Processing and Analysis Center/California
Institute of Technology, funded by the National Aeronautics and Space Administration
and the National Science Foundation."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Saul A.
full_name: Kohn, Saul A.
last_name: Kohn
- first_name: Philip N.
full_name: Best, Philip N.
last_name: Best
- first_name: Ian
full_name: Smail, Ian
last_name: Smail
- first_name: Chris M.
full_name: Harrison, Chris M.
last_name: Harrison
- first_name: John
full_name: Stott, John
last_name: Stott
- first_name: João
full_name: Calhau, João
last_name: Calhau
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
citation:
ama: 'Sobral D, Kohn SA, Best PN, et al. The most luminous H α emitters at z ∼ 0.8–2.23
from HiZELS: Evolution of AGN and star-forming galaxies. Monthly Notices of
the Royal Astronomical Society. 2016;457(2):1739-1752. doi:10.1093/mnras/stw022'
apa: 'Sobral, D., Kohn, S. A., Best, P. N., Smail, I., Harrison, C. M., Stott, J.,
… Matthee, J. J. (2016). The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS:
Evolution of AGN and star-forming galaxies. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stw022'
chicago: 'Sobral, David, Saul A. Kohn, Philip N. Best, Ian Smail, Chris M. Harrison,
John Stott, João Calhau, and Jorryt J Matthee. “The Most Luminous H α Emitters
at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and Star-Forming Galaxies.” Monthly
Notices of the Royal Astronomical Society. Oxford University Press, 2016.
https://doi.org/10.1093/mnras/stw022.'
ieee: 'D. Sobral et al., “The most luminous H α emitters at z ∼ 0.8–2.23
from HiZELS: Evolution of AGN and star-forming galaxies,” Monthly Notices of
the Royal Astronomical Society, vol. 457, no. 2. Oxford University Press,
pp. 1739–1752, 2016.'
ista: 'Sobral D, Kohn SA, Best PN, Smail I, Harrison CM, Stott J, Calhau J, Matthee
JJ. 2016. The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution
of AGN and star-forming galaxies. Monthly Notices of the Royal Astronomical Society.
457(2), 1739–1752.'
mla: 'Sobral, David, et al. “The Most Luminous H α Emitters at z ∼ 0.8–2.23 from
HiZELS: Evolution of AGN and Star-Forming Galaxies.” Monthly Notices of the
Royal Astronomical Society, vol. 457, no. 2, Oxford University Press, 2016,
pp. 1739–52, doi:10.1093/mnras/stw022.'
short: D. Sobral, S.A. Kohn, P.N. Best, I. Smail, C.M. Harrison, J. Stott, J. Calhau,
J.J. Matthee, Monthly Notices of the Royal Astronomical Society 457 (2016) 1739–1752.
date_created: 2022-07-13T12:50:36Z
date_published: 2016-04-01T00:00:00Z
date_updated: 2022-08-19T08:15:21Z
day: '01'
doi: 10.1093/mnras/stw022
extern: '1'
external_id:
arxiv:
- '1601.02266'
intvolume: ' 457'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1601.02266
month: '04'
oa: 1
oa_version: Preprint
page: 1739-1752
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN
and star-forming galaxies'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 457
year: '2016'
...