---
_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: '11490'
abstract:
- lang: eng
text: Directly characterising the first generations of stars in distant galaxies
is a key quest of observational cosmology. We present a case study of ID53 at
z = 4.77, the UV-brightest (but L⋆) star-forming galaxy at z > 3 in the MUSE eXtremely
Deep Field with a mass of ≈109 M⊙. In addition to very strong Lyman-α (Lyα) emission,
we clearly detect the (stellar) continuum and an N V P Cygni feature, interstellar
absorption, fine-structure emission and nebular C IV emission lines in the 140
h spectrum. Continuum emission from two spatially resolved components in Hubble
Space Telescope data are blended in the MUSE data, but we show that the nebular
C IV emission originates from a subcomponent of the galaxy. The UV spectrum can
be fit with recent BPASS stellar population models combined with single-burst
or continuous star formation histories (SFHs), a standard initial mass function,
and an attenuation law. Models with a young age and low metallicity (log10(age/yr)
= 6.5–7.6 and [Z/H] = −2.15 to −1.15) are preferred, but the details depend on
the assumed SFH. The intrinsic Hα luminosity of the best-fit models is an order
of magnitude higher than the Hα luminosity inferred from Spitzer/IRAC data, which
either suggests a high escape fraction of ionising photons, a high relative attenuation
of nebular to stellar dust, or a complex SFH. The metallicity appears lower than
the metallicity in more massive galaxies at z = 3 − 5, consistent with the scenario
according to which younger galaxies have lower metallicities. This chemical immaturity
likely facilitates Lyα escape, explaining why the Lyα equivalent width is anti-correlated
with stellar metallicity. Finally, we stress that uncertainties in SFHs impose
a challenge for future inferences of the stellar metallicity of young galaxies.
This highlights the need for joint (spatially resolved) analyses of stellar spectra
and photo-ionisation models.
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: A10
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: Anna
full_name: Feltre, Anna
last_name: Feltre
- first_name: Michael
full_name: Maseda, Michael
last_name: Maseda
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
- first_name: Leindert
full_name: Boogaard, Leindert
last_name: Boogaard
- first_name: Roland
full_name: Bacon, Roland
last_name: Bacon
- first_name: Anne
full_name: Verhamme, Anne
last_name: Verhamme
- first_name: Floriane
full_name: Leclercq, Floriane
last_name: Leclercq
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- first_name: Tanya
full_name: Urrutia, Tanya
last_name: Urrutia
- first_name: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
citation:
ama: 'Matthee JJ, Feltre A, Maseda M, et al. Deciphering stellar metallicities in
the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely
Deep Field. Astronomy & Astrophysics. 2022;660. doi:10.1051/0004-6361/202142187'
apa: 'Matthee, J. J., Feltre, A., Maseda, M., Nanayakkara, T., Boogaard, L., Bacon,
R., … Wisotzki, L. (2022). Deciphering stellar metallicities in the early universe:
Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field. Astronomy
& Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202142187'
chicago: 'Matthee, Jorryt J, Anna Feltre, Michael Maseda, Themiya Nanayakkara, Leindert
Boogaard, Roland Bacon, Anne Verhamme, et al. “Deciphering Stellar Metallicities
in the Early Universe: Case Study of a Young Galaxy at z = 4.77 in the MUSE EXtremely
Deep Field.” Astronomy & Astrophysics. EDP Sciences, 2022. https://doi.org/10.1051/0004-6361/202142187.'
ieee: 'J. J. Matthee et al., “Deciphering stellar metallicities in the early
universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep
Field,” Astronomy & Astrophysics, vol. 660. EDP Sciences, 2022.'
ista: 'Matthee JJ, Feltre A, Maseda M, Nanayakkara T, Boogaard L, Bacon R, Verhamme
A, Leclercq F, Kusakabe H, Urrutia T, Wisotzki L. 2022. Deciphering stellar metallicities
in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely
Deep Field. Astronomy & Astrophysics. 660, A10.'
mla: 'Matthee, Jorryt J., et al. “Deciphering Stellar Metallicities in the Early
Universe: Case Study of a Young Galaxy at z = 4.77 in the MUSE EXtremely Deep
Field.” Astronomy & Astrophysics, vol. 660, A10, EDP Sciences, 2022,
doi:10.1051/0004-6361/202142187.'
short: J.J. Matthee, A. Feltre, M. Maseda, T. Nanayakkara, L. Boogaard, R. Bacon,
A. Verhamme, F. Leclercq, H. Kusakabe, T. Urrutia, L. Wisotzki, Astronomy &
Astrophysics 660 (2022).
date_created: 2022-07-05T15:25:35Z
date_published: 2022-03-30T00:00:00Z
date_updated: 2024-10-14T11:31:22Z
day: '30'
doi: 10.1051/0004-6361/202142187
extern: '1'
external_id:
arxiv:
- '2111.14855'
intvolume: ' 660'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / techniques: spectroscopic / galaxies: stellar content
/ galaxies: formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2111.14855
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: 'Deciphering stellar metallicities in the early universe: Case study of a young
galaxy at z = 4.77 in the MUSE eXtremely Deep Field'
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: '11522'
abstract:
- lang: eng
text: The decline in abundance of Lyman-α (Lyα) emitting galaxies at z ≳ 6 is a
powerful and commonly used probe to constrain the progress of cosmic reionization.
We use the CODAII simulation, which is a radiation hydrodynamic simulation featuring
a box of ∼94 comoving Mpc side length, to compute the Lyα transmission properties
of the intergalactic medium (IGM) at z ∼ 5.8 to 7. Our results mainly confirm
previous studies, i.e. we find a declining Lyα transmission with redshift and
a large sightline-to-sightline variation. However, motivated by the recent discovery
of blue Lyα peaks at high redshift, we also analyse the IGM transmission on the
blue side, which shows a rapid decline at z ≳ 6 of the blue transmission. This
low transmission can be attributed not only to the presence of neutral regions
but also to the residual neutral hydrogen within ionized regions, for which a
density even as low as nHI∼10−9cm−3 (sometimes combined with kinematic effects)
leads to a significantly reduced visibility. Still, we find that ∼1 per cent of
sightlines towards M1600AB ∼ −21 galaxies at z ∼ 7 are transparent enough to allow
a transmission of a blue Lyα peak. We discuss our results in the context of the
interpretation of observations.
acknowledgement: The authors thank the referee for constructive feedback that improved
the outcome of this study. We are grateful to Antoinette Songaila Cowie for sharing
the ‘NEPLA4’ spectrum with us. This research has made use of NASA’s Astrophysics
Data System, and many open source projects such as trident (Hummels et al. 2017),
IPython (Pérez & Granger 2007), SciPy (Virtanen et al. 2019), NumPy (Walt et al.
2011), matplotlib (Hunter 2007), pandas (McKinney 2010), and the yt-project (Turk
et al. 2011). MG was supported by NASA through the NASA Hubble Fellowship grant
HST-HF2-51409 awarded by the Space Telescope Science Institute, which is operated
by the Association of Universities for Research in Astronomy, Inc., for NASA, under
contract NAS5-26555. MG acknowledges support from NASA grants HST-GO-15643.017,
and HST-AR15797.001 as well as XSEDE grant TG-AST180036. CAM acknowledges support
by NASA Headquarters through the NASA Hubble Fellowship grant HST-HF2-51413.001-A.
PRS was supported in part by U.S. NSF grant AST-1009799, NASA grant NNX11AE09G,
and supercomputer resources from NSF XSEDE grant TG AST090005 and the Texas Advanced
Computing Center (TACC) at The University of Texas at Austin. JM acknowledges a
Zwicky Prize Fellowship from ETH Zurich. GY acknowledges financial support by MICIU/FEDER
under project grant PGC2018-094975-C21. SEIB acknowledges funding from the European
Research Council (ERC) under the European Union’s Horizon 2020 research and innovation
programme (grant agreement No. 669253). ITI was supported by the Science and Technology
Facilities Council [grants ST/I000976/1, ST/F002858/1, ST/P000525/1, and ST/T000473/1];
and The Southeast Physics Network (SEPNet). KA was supported by NRF2016R1D1A1B04935414
and NRF-2016R1A5A1013277. KA also appreciates APCTP for its hospitality during completion
of this work. PO acknowledges support from the French ANR funded project ORAGE (ANR-14-CE33-0016).
ND and DA acknowledge funding from the French ANR for project ANR-12-JS05- 0001
(EMMA). The CoDa II simulation was performed at Oak Ridge National Laboratory/Oak
Ridge Leadership Computing Facility on the Titan supercomputer (INCITE 2016 award
AST031). Processing was performed on the Eos and Rhea clusters. Resolution study
simulations were performed on Piz Daint at the Swiss National Supercomputing Center
(PRACE Tier 0 award, project id pr37). The authors would like to acknowledge the
High Performance Computing center of the University of Strasbourg for supporting
this work by providing scientific support and access to computing resources. Part
of the computing resources were funded by the Equipex EquipMeso project (Programme
Investissements d’Avenir) and the CPER Alsacalcul/Big Data.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: Pierre
full_name: Ocvirk, Pierre
last_name: Ocvirk
- first_name: Charlotte
full_name: Mason, Charlotte
last_name: Mason
- 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: Sarah E I
full_name: Bosman, Sarah E I
last_name: Bosman
- first_name: Jenny G
full_name: Sorce, Jenny G
last_name: Sorce
- first_name: Joseph
full_name: Lewis, Joseph
last_name: Lewis
- first_name: Kyungjin
full_name: Ahn, Kyungjin
last_name: Ahn
- first_name: Dominique
full_name: Aubert, Dominique
last_name: Aubert
- first_name: Taha
full_name: Dawoodbhoy, Taha
last_name: Dawoodbhoy
- first_name: Ilian T
full_name: Iliev, Ilian T
last_name: Iliev
- first_name: Paul R
full_name: Shapiro, Paul R
last_name: Shapiro
- first_name: Gustavo
full_name: Yepes, Gustavo
last_name: Yepes
citation:
ama: Gronke M, Ocvirk P, Mason C, et al. Lyman-α transmission properties of the
intergalactic medium in the CoDaII simulation. Monthly Notices of the Royal
Astronomical Society. 2021;508(3):3697-3709. doi:10.1093/mnras/stab2762
apa: Gronke, M., Ocvirk, P., Mason, C., Matthee, J. J., Bosman, S. E. I., Sorce,
J. G., … Yepes, G. (2021). Lyman-α transmission properties of the intergalactic
medium in the CoDaII simulation. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stab2762
chicago: Gronke, Max, Pierre Ocvirk, Charlotte Mason, Jorryt J Matthee, Sarah E
I Bosman, Jenny G Sorce, Joseph Lewis, et al. “Lyman-α Transmission Properties
of the Intergalactic Medium in the CoDaII Simulation.” Monthly Notices of the
Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab2762.
ieee: M. Gronke et al., “Lyman-α transmission properties of the intergalactic
medium in the CoDaII simulation,” Monthly Notices of the Royal Astronomical
Society, vol. 508, no. 3. Oxford University Press, pp. 3697–3709, 2021.
ista: Gronke M, Ocvirk P, Mason C, Matthee JJ, Bosman SEI, Sorce JG, Lewis J, Ahn
K, Aubert D, Dawoodbhoy T, Iliev IT, Shapiro PR, Yepes G. 2021. Lyman-α transmission
properties of the intergalactic medium in the CoDaII simulation. Monthly Notices
of the Royal Astronomical Society. 508(3), 3697–3709.
mla: Gronke, Max, et al. “Lyman-α Transmission Properties of the Intergalactic Medium
in the CoDaII Simulation.” Monthly Notices of the Royal Astronomical Society,
vol. 508, no. 3, Oxford University Press, 2021, pp. 3697–709, doi:10.1093/mnras/stab2762.
short: M. Gronke, P. Ocvirk, C. Mason, J.J. Matthee, S.E.I. Bosman, J.G. Sorce,
J. Lewis, K. Ahn, D. Aubert, T. Dawoodbhoy, I.T. Iliev, P.R. Shapiro, G. Yepes,
Monthly Notices of the Royal Astronomical Society 508 (2021) 3697–3709.
date_created: 2022-07-07T09:30:21Z
date_published: 2021-12-01T00:00:00Z
date_updated: 2022-08-18T10:45:56Z
day: '01'
doi: 10.1093/mnras/stab2762
extern: '1'
external_id:
arxiv:
- '2004.14496'
intvolume: ' 508'
issue: '3'
keyword:
- dark ages
- reionization
- first stars
- intergalactic medium
- 'galaxies: formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2004.14496
month: '12'
oa: 1
oa_version: Preprint
page: 3697-3709
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: Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 508
year: '2021'
...
---
_id: '11523'
abstract:
- lang: eng
text: We present the first results from the X-SHOOTER Lyman α survey at z = 2 (XLS-z2).
XLS-z2 is a deep spectroscopic survey of 35 Lyman α emitters (LAEs) utilizing
≈90 h of exposure time with Very Large Telescope/X-SHOOTER and covers rest-frame
Ly α to H α emission with R ≈ 4000. We present the sample selection, the observations,
and the data reduction. Systemic redshifts are measured from rest-frame optical
lines for 33/35 sources. In the stacked spectrum, our LAEs are characterized by
an interstellar medium with little dust, a low metallicity, and a high ionization
state. The ionizing sources are young hot stars that power strong emission lines
in the optical and high-ionization lines in the ultraviolet (UV). The LAEs exhibit
clumpy UV morphologies and have outflowing kinematics with blueshifted Si II absorption,
a broad [O III] component, and a red-skewed Ly α line. Typically, 30 per cent
of the Ly α photons escape, of which one quarter on the blue side of the systemic
velocity. A fraction of Ly α photons escape directly at the systemic suggesting
clear channels enabling an ≈10 per cent escape of ionizing photons, consistent
with an inference based on Mg II. A combination of a low effective H I column
density, a low dust content, and young starburst determines whether a star-forming
galaxy is observed as an LAE. The first is possibly related to outflows and/or
a fortunate viewing angle, while we find that the latter two in LAEs are typical
for their stellar mass of 109 M⊙.
acknowledgement: "We thank the referee for constructive comments and suggestions.
We thank Dawn Erb, Ruari Mackenzie, Ivan Oteo, Ryan Sanders, and Johannes Zabl for
useful discussions and suggestions. It is a pleasure to thank the ESO User Support,
in particular Giacomo Beccari, Carlo Manara, John Pritchard, Marina Rejkuba, and
Lowell Tacconi-Garman for assistance in the preparation and execution of the observations.
Based on observations obtained with the VLT, programs 084.A-0303, 088.A-0672, 091.A-0413,
091.A-0546, 092.A0774, 097.A-0153, 098.A-0819, 099.A-0758, 099.A-0254, 101.B0779,
and 102.A-0652. Based on data products from observations made with ESO Telescopes
at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data
products produced by CALET and the Cambridge Astronomy Survey Unit on behalf of
the UltraVISTA consortium. Based on observations made with the NASA/ESA HST through
programs 9133, 9367, 11694, and 12471, and obtained from the Hubble Legacy Archive,
which is a collaboration between the Space Telescope Science Institute (STScI/NASA),
the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian
Astronomy Data Centre (CADC/NRC/CSA). This work is based on observations taken by
the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated
by the Association of Universities for Research in Astronomy, Inc., under NASA contract
NAS5-26555. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409
and acknowledges support from HST grants\r\nHST-GO-15643.017-A, HST-AR-15039.003-A,
and XSEDE grant TG-AST180036. GP acknowledges support from the Netherlands Research
School for Astronomy (NOVA). RA acknowledges the support of ANID FONDECYT Regular
Grant 1202007. We gratefully acknowledge the PYTHON programming language, its NUMPY,
MATPLOTLIB, SCIPY, LMFIT (Jones et al. 2001; Hunter 2007; van der Walt, Colbert
& Varoquaux 2011), PANDAS (McKinney 2010), and ASTROPY (Astropy Collaboration 2013)
packages, and the TOPCAT analysis tool (Taylor 2013). Dedicated to the memory of
A. C. J.Matthee (1953–2020)."
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: Matthew
full_name: Hayes, Matthew
last_name: Hayes
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: Daniel
full_name: Schaerer, Daniel
last_name: Schaerer
- first_name: Rohan P
full_name: Naidu, Rohan P
last_name: Naidu
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
- first_name: João
full_name: Calhau, João
last_name: Calhau
- first_name: Ana
full_name: Paulino-Afonso, Ana
last_name: Paulino-Afonso
- first_name: Sérgio
full_name: Santos, Sérgio
last_name: Santos
- first_name: Ricardo
full_name: Amorín, Ricardo
last_name: Amorín
citation:
ama: 'Matthee JJ, Sobral D, Hayes M, et al. The X-SHOOTER Lyman α survey at z =
2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? Monthly Notices of the
Royal Astronomical Society. 2021;505(1):1382-1412. doi:10.1093/mnras/stab1304'
apa: 'Matthee, J. J., Sobral, D., Hayes, M., Pezzulli, G., Gronke, M., Schaerer,
D., … Amorín, R. (2021). The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What
makes a galaxy a Lyman α emitter? Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stab1304'
chicago: 'Matthee, Jorryt J, David Sobral, Matthew Hayes, Gabriele Pezzulli, Max
Gronke, Daniel Schaerer, Rohan P Naidu, et al. “The X-SHOOTER Lyman α Survey at
z = 2 (XLS-Z2) I: What Makes a Galaxy a Lyman α Emitter?” Monthly Notices of
the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab1304.'
ieee: 'J. J. Matthee et al., “The X-SHOOTER Lyman α survey at z = 2 (XLS-z2)
I: What makes a galaxy a Lyman α emitter?,” Monthly Notices of the Royal Astronomical
Society, vol. 505, no. 1. Oxford University Press, pp. 1382–1412, 2021.'
ista: 'Matthee JJ, Sobral D, Hayes M, Pezzulli G, Gronke M, Schaerer D, Naidu RP,
Röttgering H, Calhau J, Paulino-Afonso A, Santos S, Amorín R. 2021. The X-SHOOTER
Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? Monthly
Notices of the Royal Astronomical Society. 505(1), 1382–1412.'
mla: 'Matthee, Jorryt J., et al. “The X-SHOOTER Lyman α Survey at z = 2 (XLS-Z2)
I: What Makes a Galaxy a Lyman α Emitter?” Monthly Notices of the Royal Astronomical
Society, vol. 505, no. 1, Oxford University Press, 2021, pp. 1382–412, doi:10.1093/mnras/stab1304.'
short: J.J. Matthee, D. Sobral, M. Hayes, G. Pezzulli, M. Gronke, D. Schaerer, R.P.
Naidu, H. Röttgering, J. Calhau, A. Paulino-Afonso, S. Santos, R. Amorín, Monthly
Notices of the Royal Astronomical Society 505 (2021) 1382–1412.
date_created: 2022-07-07T09:33:39Z
date_published: 2021-07-01T00:00:00Z
date_updated: 2024-10-14T11:32:39Z
day: '01'
doi: 10.1093/mnras/stab1304
extern: '1'
external_id:
arxiv:
- '2102.07779'
intvolume: ' 505'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: formation'
- 'galaxies: ISM'
- 'galaxies: starburst'
- dark ages
- reionization
- first stars
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2102.07779
month: '07'
oa: 1
oa_version: Preprint
page: 1382-1412
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-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman
α emitter?'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 505
year: '2021'
...
---
_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: '11533'
abstract:
- lang: eng
text: We explore deep rest-frame UV to FIR data in the COSMOS field to measure the
individual spectral energy distributions (SED) of the ∼4000 SC4K (Sobral et al.)
Lyman α (Ly α) emitters (LAEs) at z ∼ 2–6. We find typical stellar masses of 109.3
± 0.6 M⊙ and star formation rates (SFR) of SFRSED=4.4+10.5−2.4 M⊙ yr−1 and SFRLyα=5.9+6.3−2.6 M⊙ yr−1,
combined with very blue UV slopes of β=−2.1+0.5−0.4, but with significant variations
within the population. MUV and β are correlated in a similar way to UV-selected
sources, but LAEs are consistently bluer. This suggests that LAEs are the youngest
and/or most dust-poor subset of the UV-selected population. We also study the
Ly α rest-frame equivalent width (EW0) and find 45 ‘extreme’ LAEs with EW0 > 240 Å
(3σ), implying a low number density of (7 ± 1) × 10−7 Mpc−3. Overall, we measure
little to no evolution of the Ly α EW0 and scale length parameter (w0), which
are consistently high (EW0=140+280−70 Å, w0=129+11−11 Å) from z ∼ 6 to z ∼ 2 and
below. However, w0 is anticorrelated with MUV and stellar mass. Our results imply
that sources selected as LAEs have a high Ly α escape fraction (fesc,Ly α) irrespective
of cosmic time, but fesc,Ly α is still higher for UV-fainter and lower mass LAEs.
The least massive LAEs (<109.5 M⊙) are typically located above the star formation
‘main sequence’ (MS), but the offset from the MS decreases towards z ∼ 6 and towards
1010 M⊙. Our results imply a lack of evolution in the properties of LAEs across
time and reveals the increasing overlap in properties of LAEs and UV-continuum
selected galaxies as typical star-forming galaxies at high redshift effectively
become LAEs.
acknowledgement: We thank the anonymous referee for the valuable feedback that significantly
improved the quality and clarity of this paper. SS and JC acknowledge studentships
from Lancaster University. APA acknowledges support from Fundação para a Ciência
e a Tecnologia through the project PTDC/FISAST/31546/2017. The authors would like
to thank Ali Khostovan, Sara Perez Sanchez, Alex Bennett and Tom Rose for contributions
and discussions in the early stages of this work. Based on data products from observations
made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme
ID 179.A-2005 and on data products produced by CALET and the Cambridge Astronomy
Survey Unit on behalf of the UltraVISTA consortium. Finally, the authors acknowledge
the unique value of the publicly available analysis software TOPCAT (Taylor 2005)
and publicly available programming language Python, including the numpy, pyfits,
matplotlib, scipy and astropy (Astropy Collaboration et al. 2013) packages. This
work is based on the public SC4K sample of LAEs (Sobral et al. 2018a) and we release
the full catalogue with all the photometry and properties derived in this paper,
in electronic format, along with the relevant tables.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: S
full_name: Santos, S
last_name: Santos
- first_name: D
full_name: Sobral, D
last_name: Sobral
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: J
full_name: Calhau, J
last_name: Calhau
- first_name: E
full_name: da Cunha, E
last_name: da Cunha
- first_name: B
full_name: Ribeiro, B
last_name: Ribeiro
- first_name: A
full_name: Paulino-Afonso, A
last_name: Paulino-Afonso
- first_name: P
full_name: Arrabal Haro, P
last_name: Arrabal Haro
- first_name: J
full_name: Butterworth, J
last_name: Butterworth
citation:
ama: Santos S, Sobral D, Matthee JJ, et al. The evolution of rest-frame UV properties,
Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. Monthly
Notices of the Royal Astronomical Society. 2020;493(1):141-160. doi:10.1093/mnras/staa093
apa: Santos, S., Sobral, D., Matthee, J. J., Calhau, J., da Cunha, E., Ribeiro,
B., … Butterworth, J. (2020). The evolution of rest-frame UV properties, Ly α
EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. Monthly Notices
of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa093
chicago: Santos, S, D Sobral, Jorryt J Matthee, J Calhau, E da Cunha, B Ribeiro,
A Paulino-Afonso, P Arrabal Haro, and J Butterworth. “The Evolution of Rest-Frame
UV Properties, Ly α EWs, and the SFR–Stellar Mass Relation at z ∼ 2–6 for SC4K
LAEs.” Monthly Notices of the Royal Astronomical Society. Oxford University
Press, 2020. https://doi.org/10.1093/mnras/staa093.
ieee: S. Santos et al., “The evolution of rest-frame UV properties, Ly α
EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs,” Monthly Notices
of the Royal Astronomical Society, vol. 493, no. 1. Oxford University Press,
pp. 141–160, 2020.
ista: Santos S, Sobral D, Matthee JJ, Calhau J, da Cunha E, Ribeiro B, Paulino-Afonso
A, Arrabal Haro P, Butterworth J. 2020. The evolution of rest-frame UV properties,
Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. Monthly
Notices of the Royal Astronomical Society. 493(1), 141–160.
mla: Santos, S., et al. “The Evolution of Rest-Frame UV Properties, Ly α EWs, and
the SFR–Stellar Mass Relation at z ∼ 2–6 for SC4K LAEs.” Monthly Notices of
the Royal Astronomical Society, vol. 493, no. 1, Oxford University Press,
2020, pp. 141–60, doi:10.1093/mnras/staa093.
short: S. Santos, D. Sobral, J.J. Matthee, J. Calhau, E. da Cunha, B. Ribeiro, A.
Paulino-Afonso, P. Arrabal Haro, J. Butterworth, Monthly Notices of the Royal
Astronomical Society 493 (2020) 141–160.
date_created: 2022-07-07T12:05:23Z
date_published: 2020-03-01T00:00:00Z
date_updated: 2022-08-18T11:27:43Z
day: '01'
doi: 10.1093/mnras/staa093
extern: '1'
external_id:
arxiv:
- '1910.02959'
intvolume: ' 493'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: high-redshift'
- 'galaxies: star formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1910.02959
month: '03'
oa: 1
oa_version: Preprint
page: 141-160
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass
relation at z ∼ 2–6 for SC4K LAEs
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 493
year: '2020'
...
---
_id: '11586'
abstract:
- lang: eng
text: Distant luminous Lyman-α emitters are excellent targets for detailed observations
of galaxies in the epoch of reionisation. Spatially resolved observations of these
galaxies allow us to simultaneously probe the emission from young stars, partially
ionised gas in the interstellar medium and to constrain the properties of the
surrounding hydrogen in the circumgalactic medium. We review recent results from
(spectroscopic) follow-up studies of the rest-frame UV, Lyman-α and [CII] emission
in luminous galaxies observed ∼500 Myr after the Big Bang with ALMA, HST/WFC3
and VLT/X-SHOOTER. These galaxies likely reside in early ionised bubbles and are
complex systems, consisting of multiple well separated and resolved components
where traces of metals are already present.
article_processing_charge: No
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
citation:
ama: 'Matthee JJ, Sobral D. Unveiling the most luminous Lyman-α emitters in the
epoch of reionisation. In: Proceedings of the International Astronomical Union.
Vol 15. Cambridge University Press; 2020:21-25. doi:10.1017/s1743921319009451'
apa: Matthee, J. J., & Sobral, D. (2020). Unveiling the most luminous Lyman-α
emitters in the epoch of reionisation. In Proceedings of the International
Astronomical Union (Vol. 15, pp. 21–25). Cambridge University Press. https://doi.org/10.1017/s1743921319009451
chicago: Matthee, Jorryt J, and David Sobral. “Unveiling the Most Luminous Lyman-α
Emitters in the Epoch of Reionisation.” In Proceedings of the International
Astronomical Union, 15:21–25. Cambridge University Press, 2020. https://doi.org/10.1017/s1743921319009451.
ieee: J. J. Matthee and D. Sobral, “Unveiling the most luminous Lyman-α emitters
in the epoch of reionisation,” in Proceedings of the International Astronomical
Union, 2020, vol. 15, no. S352, pp. 21–25.
ista: Matthee JJ, Sobral D. 2020. Unveiling the most luminous Lyman-α emitters in
the epoch of reionisation. Proceedings of the International Astronomical Union.
vol. 15, 21–25.
mla: Matthee, Jorryt J., and David Sobral. “Unveiling the Most Luminous Lyman-α
Emitters in the Epoch of Reionisation.” Proceedings of the International Astronomical
Union, vol. 15, no. S352, Cambridge University Press, 2020, pp. 21–25, doi:10.1017/s1743921319009451.
short: J.J. Matthee, D. Sobral, in:, Proceedings of the International Astronomical
Union, Cambridge University Press, 2020, pp. 21–25.
date_created: 2022-07-14T14:08:41Z
date_published: 2020-06-04T00:00:00Z
date_updated: 2024-10-14T11:38:21Z
day: '04'
doi: 10.1017/s1743921319009451
extern: '1'
external_id:
arxiv:
- '1911.04774'
intvolume: ' 15'
issue: S352
keyword:
- Astronomy and Astrophysics
- Space and Planetary Science
- 'galaxies: formation'
- 'galaxies: evolution'
- 'galaxies: high-redshift'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1911.04774
month: '06'
oa: 1
oa_version: Preprint
page: 21-25
publication: Proceedings of the International Astronomical Union
publication_identifier:
eissn:
- 1743-9221
issn:
- 1743-9213
publication_status: published
publisher: Cambridge University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Unveiling the most luminous Lyman-α emitters in the epoch of reionisation
type: conference
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 15
year: '2020'
...
---
_id: '11507'
abstract:
- lang: eng
text: 'Lyman-α (Lyα) is intrinsically the brightest line emitted from active galaxies.
While it originates from many physical processes, for star-forming galaxies the
intrinsic Lyα luminosity is a direct tracer of the Lyman-continuum (LyC) radiation
produced by the most massive O- and early-type B-stars (M⋆ ≳ 10 M⊙) with lifetimes
of a few Myrs. As such, Lyα luminosity should be an excellent instantaneous star
formation rate (SFR) indicator. However, its resonant nature and susceptibility
to dust as a rest-frame UV photon makes Lyα very hard to interpret due to the
uncertain Lyα escape fraction, fesc, Lyα. Here we explore results from the CAlibrating
LYMan-α with Hα (CALYMHA) survey at z = 2.2, follow-up of Lyα emitters (LAEs)
at z = 2.2 − 2.6 and a z ∼ 0−0.3 compilation of LAEs to directly measure fesc, Lyα
with Hα. We derive a simple empirical relation that robustly retrieves fesc, Lyα
as a function of Lyα rest-frame EW (EW0): fesc,Lyα = 0.0048 EW0[Å] ± 0.05 and
we show that it constrains a well-defined anti-correlation between ionisation
efficiency (ξion) and dust extinction in LAEs. Observed Lyα luminosities and EW0
are easy measurable quantities at high redshift, thus making our relation a practical
tool to estimate intrinsic Lyα and LyC luminosities under well controlled and
simple assumptions. Our results allow observed Lyα luminosities to be used to
compute SFRs for LAEs at z ∼ 0−2.6 within ±0.2 dex of the Hα dust corrected SFRs.
We apply our empirical SFR(Lyα,EW0) calibration to several sources at z ≥ 2.6
to find that star-forming LAEs have SFRs typically ranging from 0.1 to 20 M⊙ yr−1
and that our calibration might be even applicable for the most luminous LAEs within
the epoch of re-ionisation. Our results imply high ionisation efficiencies (log10[ξion/Hz erg−1]
= 25.4−25.6) and low dust content in LAEs across cosmic time, and will be easily
tested with future observations with JWST which can obtain Hα and Hβ measurements
for high-redshift LAEs.'
acknowledgement: We thank the anonymous referees for multiple comments and suggestions
which have improved the manuscript. JM acknowledges the support of a Huygens PhD
fellowship from Leiden University. We have benefited greatly from the publicly available
programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt et al. 2011;
Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration
2013) packages, and the TOPCAT analysis program (Taylor 2013). The results and samples
of LAEs used for this paper are publicly available (see e.g. Sobral et al. 2017,
2018a) and we also provide the toy model used as a PYTHON script.
article_number: A157
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
citation:
ama: 'Sobral D, Matthee JJ. Predicting Lyα escape fractions with a simple observable:
Lyα in emission as an empirically calibrated star formation rate indicator. Astronomy
& Astrophysics. 2019;623. doi:10.1051/0004-6361/201833075'
apa: 'Sobral, D., & Matthee, J. J. (2019). Predicting Lyα escape fractions with
a simple observable: Lyα in emission as an empirically calibrated star formation
rate indicator. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201833075'
chicago: 'Sobral, David, and Jorryt J Matthee. “Predicting Lyα Escape Fractions
with a Simple Observable: Lyα in Emission as an Empirically Calibrated Star Formation
Rate Indicator.” Astronomy & Astrophysics. EDP Sciences, 2019. https://doi.org/10.1051/0004-6361/201833075.'
ieee: 'D. Sobral and J. J. Matthee, “Predicting Lyα escape fractions with a simple
observable: Lyα in emission as an empirically calibrated star formation rate indicator,”
Astronomy & Astrophysics, vol. 623. EDP Sciences, 2019.'
ista: 'Sobral D, Matthee JJ. 2019. Predicting Lyα escape fractions with a simple
observable: Lyα in emission as an empirically calibrated star formation rate indicator.
Astronomy & Astrophysics. 623, A157.'
mla: 'Sobral, David, and Jorryt J. Matthee. “Predicting Lyα Escape Fractions with
a Simple Observable: Lyα in Emission as an Empirically Calibrated Star Formation
Rate Indicator.” Astronomy & Astrophysics, vol. 623, A157, EDP Sciences,
2019, doi:10.1051/0004-6361/201833075.'
short: D. Sobral, J.J. Matthee, Astronomy & Astrophysics 623 (2019).
date_created: 2022-07-06T11:08:16Z
date_published: 2019-03-26T00:00:00Z
date_updated: 2022-07-19T09:37:20Z
day: '26'
doi: 10.1051/0004-6361/201833075
extern: '1'
external_id:
arxiv:
- '1803.08923'
intvolume: ' 623'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / galaxies: star formation / galaxies: statistics / galaxies:
evolution / galaxies: formation / galaxies: ISM'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1803.08923
month: '03'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Predicting Lyα escape fractions with a simple observable: Lyα in emission
as an empirically calibrated star formation rate indicator'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 623
year: '2019'
...
---
_id: '11540'
abstract:
- lang: eng
text: Observations have revealed that the star formation rate (SFR) and stellar
mass (Mstar) of star-forming galaxies follow a tight relation known as the galaxy
main sequence. However, what physical information is encoded in this relation
is under debate. Here, we use the EAGLE cosmological hydrodynamical simulation
to study the mass dependence, evolution, and origin of scatter in the SFR–Mstar
relation. At z = 0, we find that the scatter decreases slightly with stellar mass
from 0.35 dex at Mstar ≈ 109 M⊙ to 0.30 dex at Mstar ≳ 1010.5 M⊙. The scatter
decreases from z = 0 to z = 5 by 0.05 dex at Mstar ≳ 1010 M⊙ and by 0.15 dex for
lower masses. We show that the scatter at z = 0.1 originates from a combination
of fluctuations on short time-scales (ranging from 0.2–2 Gyr) that are presumably
associated with self-regulation from cooling, star formation, and outflows, but
is dominated by long time-scale (∼10 Gyr) variations related to differences in
halo formation times. Shorter time-scale fluctuations are relatively more important
for lower mass galaxies. At high masses, differences in black hole formation efficiency
cause additional scatter, but also diminish the scatter caused by different halo
formation times. While individual galaxies cross the main sequence multiple times
during their evolution, they fluctuate around tracks associated with their halo
properties, i.e. galaxies above/below the main sequence at z = 0.1 tend to have
been above/below the main sequence for ≫1 Gyr.
acknowledgement: JM acknowledges the support of a Huygens PhD fellowship from Leiden
University. We thank Camila Correa for help analysing snipshot merger trees. We
thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann,
Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and
suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade
of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and
ideas. We have benefited from the public available programming language PYTHON,
including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT
analysis tool (Taylor 2013).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
citation:
ama: Matthee JJ, Schaye J. The origin of scatter in the star formation rate–stellar
mass relation. Monthly Notices of the Royal Astronomical Society. 2019;484(1):915-932.
doi:10.1093/mnras/stz030
apa: Matthee, J. J., & Schaye, J. (2019). The origin of scatter in the star
formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stz030
chicago: Matthee, Jorryt J, and Joop Schaye. “The Origin of Scatter in the Star
Formation Rate–Stellar Mass Relation.” Monthly Notices of the Royal Astronomical
Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz030.
ieee: J. J. Matthee and J. Schaye, “The origin of scatter in the star formation
rate–stellar mass relation,” Monthly Notices of the Royal Astronomical Society,
vol. 484, no. 1. Oxford University Press, pp. 915–932, 2019.
ista: Matthee JJ, Schaye J. 2019. The origin of scatter in the star formation rate–stellar
mass relation. Monthly Notices of the Royal Astronomical Society. 484(1), 915–932.
mla: Matthee, Jorryt J., and Joop Schaye. “The Origin of Scatter in the Star Formation
Rate–Stellar Mass Relation.” Monthly Notices of the Royal Astronomical Society,
vol. 484, no. 1, Oxford University Press, 2019, pp. 915–32, doi:10.1093/mnras/stz030.
short: J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society
484 (2019) 915–932.
date_created: 2022-07-08T07:48:31Z
date_published: 2019-03-01T00:00:00Z
date_updated: 2024-10-14T11:33:52Z
day: '01'
doi: 10.1093/mnras/stz030
extern: '1'
external_id:
arxiv:
- '1805.05956'
intvolume: ' 484'
issue: '1'
keyword:
- Space and Planetary Science
- 'Astronomy and Astrophysics : galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: star formation'
- 'cosmology: theory'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1805.05956
month: '03'
oa: 1
oa_version: Preprint
page: 915-932
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The origin of scatter in the star formation rate–stellar mass relation
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 484
year: '2019'
...
---
_id: '11508'
abstract:
- lang: eng
text: Distant luminous Lyman-α emitters (LAEs) are excellent targets for spectroscopic
observations of galaxies in the epoch of reionisation (EoR). We present deep high-resolution
(R = 5000) VLT/X-shooter observations, along with an extensive collection of photometric
data of COLA1, a proposed double peaked LAE at z = 6.6. We rule out the possibility
that COLA1’s emission line is an [OII] doublet at z = 1.475 on the basis of i)
the asymmetric red line-profile and flux ratio of the peaks (blue/red=0.31 ± 0.03)
and ii) an unphysical [OII]/Hα ratio ([OII]/Hα > 22). We show that COLA1’s observed
B-band flux is explained by a faint extended foreground LAE, for which we detect
Lyα and [OIII] at z = 2.142. We thus conclude that COLA1 is a real double-peaked
LAE at z = 6.593, the first discovered at z > 6. COLA1 is UV luminous (M1500 = −21.6 ± 0.3),
has a high equivalent width (EW0,Lyα = 120−40+50 Å) and very compact Lyα emission
(r50,Lyα = 0.33−0.04+0.07 kpc). Relatively weak inferred Hβ+[OIII] line-emission
from Spitzer/IRAC indicates an extremely low metallicity of Z < 1/20 Z⊙ or reduced
strength of nebular lines due to high escape of ionising photons. The small Lyα
peak separation of 220 ± 20 km s−1 implies a low HI column density and an ionising
photon escape fraction of ≈15 − 30%, providing the first direct evidence that
such galaxies contribute actively to the reionisation of the Universe at z > 6.
Based on simple estimates, we find that COLA1 could have provided just enough
photons to reionise its own ≈0.3 pMpc (2.3 cMpc) bubble, allowing the blue Lyα
line to be observed. However, we also discuss alternative scenarios explaining
the detected double peaked nature of COLA1. Our results show that future high-resolution
observations of statistical samples of double peaked LAEs at z > 5 are a promising
probe of the occurrence of ionised regions around galaxies in the EoR.
acknowledgement: JM acknowledges the award of a Huygens PhD fellowship from Leiden
University. MG acknowledges support from NASA grant NNX17AK58G. APA, PhD::SPACE
fellow, acknowledges support from the FCT through the fellowship PD/BD/52706/2014.
Based on observations made with ESO Telescopes at the La Silla Paranal Observatory
under programme IDs 294.A-5018, 098.A-0819, 099.A-0254 and 0100.A-0213. We are grateful
for the excellent data-sets from the COSMOS and UltraVISTA survey teams. This research
was supported by the Munich Institute for Astro- and Particle Physics (MIAPP) of
the DFG cluster of excellence “Origin and Structure of the Universe”. We thank the
referee for their comments that improved the paper. We also thank Christoph Behrens,
Len Cowie, Koki Kakiichi, Peter Laursen, Charlotte Mason, Eros Vanzella, Lewis Weinberger
and Johannes Zabl for discussions. We have benefited from the public available programming
language Python, including the numpy, matplotlib, scipy and astropy packages (Hunter
2007; Astropy Collaboration 2013), the astronomical imaging tools Swarp (Bertin
2010) and ds9 and the Topcat analysis tool (Taylor 2013).
article_number: A136
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: Ana
full_name: Paulino-Afonso, Ana
last_name: Paulino-Afonso
- first_name: Mauro
full_name: Stefanon, Mauro
last_name: Stefanon
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
citation:
ama: 'Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H.
Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly
contributing to the reionisation of the universe. Astronomy & Astrophysics.
2018;619. doi:10.1051/0004-6361/201833528'
apa: 'Matthee, J. J., Sobral, D., Gronke, M., Paulino-Afonso, A., Stefanon, M.,
& Röttgering, H. (2018). Confirmation of double peaked Lyα emission at z =
6.593: Witnessing a galaxy directly contributing to the reionisation of the universe.
Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201833528'
chicago: 'Matthee, Jorryt J, David Sobral, Max Gronke, Ana Paulino-Afonso, Mauro
Stefanon, and Huub Röttgering. “Confirmation of Double Peaked Lyα Emission at
z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the
Universe.” Astronomy & Astrophysics. EDP Sciences, 2018. https://doi.org/10.1051/0004-6361/201833528.'
ieee: 'J. J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, and
H. Röttgering, “Confirmation of double peaked Lyα emission at z = 6.593: Witnessing
a galaxy directly contributing to the reionisation of the universe,” Astronomy
& Astrophysics, vol. 619. EDP Sciences, 2018.'
ista: 'Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering
H. 2018. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a
galaxy directly contributing to the reionisation of the universe. Astronomy &
Astrophysics. 619, A136.'
mla: 'Matthee, Jorryt J., et al. “Confirmation of Double Peaked Lyα Emission at
z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the
Universe.” Astronomy & Astrophysics, vol. 619, A136, EDP Sciences,
2018, doi:10.1051/0004-6361/201833528.'
short: J.J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, H. Röttgering,
Astronomy & Astrophysics 619 (2018).
date_created: 2022-07-06T11:14:23Z
date_published: 2018-11-19T00:00:00Z
date_updated: 2024-10-14T11:31:36Z
day: '19'
doi: 10.1051/0004-6361/201833528
extern: '1'
external_id:
arxiv:
- '1805.11621'
intvolume: ' 619'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / galaxies: formation / dark ages / reionization / first
stars / techniques: spectroscopic / intergalactic medium'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1805.11621
month: '11'
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: 'Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy
directly contributing to the reionisation of the universe'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 619
year: '2018'
...
---
_id: '11555'
abstract:
- lang: eng
text: We investigate the morphology of the [C II] emission in a sample of ‘normal’
star-forming galaxies at 5 < z < 7.2 in relation to their UV (rest-frame) counterpart.
We use new Atacama Large Millimetre/submillimetre Array (ALMA) observations of
galaxies at z ∼ 6–7, as well as a careful re-analysis of archival ALMA data. In
total 29 galaxies were analysed, 21 of which are detected in [C II]. For several
of the latter the [C II] emission breaks into multiple components. Only a fraction
of these [C II] components, if any, is associated with the primary UV systems,
while the bulk of the [C II] emission is associated either with fainter UV components,
or not associated with any UV counterpart at the current limits. By taking into
account the presence of all these components, we find that the L[CII]–SFR (star
formation rate) relation at early epochs is fully consistent with the local relation,
but it has a dispersion of 0.48 ± 0.07 dex, which is about two times larger than
observed locally. We also find that the deviation from the local L[CII]–SFR relation
has a weak anticorrelation with the EW(Ly α). The morphological analysis also
reveals that [C II] emission is generally much more extended than the UV emission.
As a consequence, these primordial galaxies are characterized by a [C II] surface
brightness generally much lower than expected from the local Σ[CII]−ΣSFR relation.
These properties are likely a consequence of a combination of different effects,
namely gas metallicity, [C II] emission from obscured star-forming regions, strong
variations of the ionization parameter, and circumgalactic gas in accretion or
ejected by these primeval galaxies.
acknowledgement: "This paper makes use of the following ALMA data:\r\nADS/JAO.ALMA#2012.1.00719.S,
ADS/JAO.ALMA#2012.A.00040.S,\r\nADS/JAO.ALMA#2013.A.00433.S, ADS/JAO.ALMA#2011.0.00115.S,\r\nADS/JAO.ALMA#2012.1.00033.S,
ADS/JAO.ALMA#2012.1.00523.S,\r\nADS/JAO.ALMA#2013.1.00815.S, ADS/JAO.ALMA#2015.1.00834.S.,\r\nADS/JAO.ALMA#2015.1.01105.S,
AND ADS/JAO.ALMA#2016.1.01240.S\r\nwhich can be retrieved from the ALMA data archive:\r\nhttps://almascience.eso.org/
alma-data/archive. ALMA is a partnership of ESO (representing its member states),
NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan),
in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated
by ESO, AUI/NRAO, and NAOJ. We are grateful to G. Jones to for providing his [C
II] flux maps. RM and SC acknowledge support by the Science and Technology Facilities
Council (STFC). RM acknowledges ERC Advanced Grant 695671 ‘QUENCH’. AF acknowledges
support from the ERC Advanced Grant INTERSTELLAR H2020/740120."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: S
full_name: Carniani, S
last_name: Carniani
- first_name: R
full_name: Maiolino, R
last_name: Maiolino
- first_name: R
full_name: Amorin, R
last_name: Amorin
- first_name: L
full_name: Pentericci, L
last_name: Pentericci
- first_name: A
full_name: Pallottini, A
last_name: Pallottini
- first_name: A
full_name: Ferrara, A
last_name: Ferrara
- first_name: C J
full_name: Willott, C J
last_name: Willott
- first_name: R
full_name: Smit, R
last_name: Smit
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: D
full_name: Sobral, D
last_name: Sobral
- first_name: P
full_name: Santini, P
last_name: Santini
- first_name: M
full_name: Castellano, M
last_name: Castellano
- first_name: S
full_name: De Barros, S
last_name: De Barros
- first_name: A
full_name: Fontana, A
last_name: Fontana
- first_name: A
full_name: Grazian, A
last_name: Grazian
- first_name: L
full_name: Guaita, L
last_name: Guaita
citation:
ama: Carniani S, Maiolino R, Amorin R, et al. Kiloparsec-scale gaseous clumps and
star formation at z = 5–7. Monthly Notices of the Royal Astronomical Society.
2018;478(1):1170-1184. doi:10.1093/mnras/sty1088
apa: Carniani, S., Maiolino, R., Amorin, R., Pentericci, L., Pallottini, A., Ferrara,
A., … Guaita, L. (2018). Kiloparsec-scale gaseous clumps and star formation at
z = 5–7. Monthly Notices of the Royal Astronomical Society. Oxford University
Press. https://doi.org/10.1093/mnras/sty1088
chicago: Carniani, S, R Maiolino, R Amorin, L Pentericci, A Pallottini, A Ferrara,
C J Willott, et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at z = 5–7.”
Monthly Notices of the Royal Astronomical Society. Oxford University Press,
2018. https://doi.org/10.1093/mnras/sty1088.
ieee: S. Carniani et al., “Kiloparsec-scale gaseous clumps and star formation
at z = 5–7,” Monthly Notices of the Royal Astronomical Society, vol. 478,
no. 1. Oxford University Press, pp. 1170–1184, 2018.
ista: Carniani S, Maiolino R, Amorin R, Pentericci L, Pallottini A, Ferrara A, Willott
CJ, Smit R, Matthee JJ, Sobral D, Santini P, Castellano M, De Barros S, Fontana
A, Grazian A, Guaita L. 2018. Kiloparsec-scale gaseous clumps and star formation
at z = 5–7. Monthly Notices of the Royal Astronomical Society. 478(1), 1170–1184.
mla: Carniani, S., et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at
z = 5–7.” Monthly Notices of the Royal Astronomical Society, vol. 478,
no. 1, Oxford University Press, 2018, pp. 1170–84, doi:10.1093/mnras/sty1088.
short: S. Carniani, R. Maiolino, R. Amorin, L. Pentericci, A. Pallottini, A. Ferrara,
C.J. Willott, R. Smit, J.J. Matthee, D. Sobral, P. Santini, M. Castellano, S.
De Barros, A. Fontana, A. Grazian, L. Guaita, Monthly Notices of the Royal Astronomical
Society 478 (2018) 1170–1184.
date_created: 2022-07-11T08:05:42Z
date_published: 2018-07-01T00:00:00Z
date_updated: 2022-08-19T06:58:06Z
day: '01'
doi: 10.1093/mnras/sty1088
extern: '1'
external_id:
arxiv:
- '1712.03985'
intvolume: ' 478'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: ISM'
- 'galaxies: formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1712.03985
month: '07'
oa: 1
oa_version: Preprint
page: 1170-1184
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: Kiloparsec-scale gaseous clumps and star formation at z = 5–7
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 478
year: '2018'
...
---
_id: '11558'
abstract:
- lang: eng
text: We present and explore deep narrow- and medium-band data obtained with the
Subaru and the Isaac Newton Telescopes in the ∼2 deg2 COSMOS field. We use these
data as an extremely wide, low-resolution (R ∼ 20–80) Integral Field Unit survey
to slice through the COSMOS field and obtain a large sample of ∼4000 Ly α emitters
(LAEs) from z ∼ 2 to 6 in 16 redshift slices (SC4K). We present new Ly α luminosity
functions (LFs) covering a comoving volume of ∼108 Mpc3. SC4K extensively complements
ultradeep surveys, jointly covering over 4 dex in Ly α luminosity and revealing
a global (2.5 < z < 6) synergy LF with α=−1.93+0.12−0.12, log10Φ∗Lyα=−3.45+0.22−0.29 Mpc−3,
and log10L∗Lyα=42.93+0.15−0.11 erg s−1. The Schechter component of the Ly α LF
reveals a factor ∼5 rise in L∗Lyα and a ∼7 × decline in Φ∗Lyα from z ∼ 2 to 6.
The data reveal an extra power-law (or Schechter) component above LLy α ≈ 1043.3 erg s−1
at z ∼ 2.2–3.5 and we show that it is partially driven by X-ray and radio active
galactic nucleus (AGN), as their Ly α LF resembles the excess. The power-law component
vanishes and/or is below our detection limits above z > 3.5, likely linked with
the evolution of the AGN population. The Ly α luminosity density rises by a factor
∼2 from z ∼ 2 to 3 but is then found to be roughly constant (1.1+0.2−0.2×1040 erg s−1 Mpc−3)
to z ∼ 6, despite the ∼0.7 dex drop in ultraviolet (UV) luminosity density. The
Ly α/UV luminosity density ratio rises from 4 ± 1 per cent to 30 ± 6 per cent
from z ∼ 2.2 to 6. Our results imply a rise of a factor of ≈2 in the global ionization
efficiency (ξion) and a factor ≈4 ± 1 in the Ly α escape fraction from z ∼ 2 to
6, hinting for evolution in both the typical burstiness/stellar populations and
even more so in the typical interstellar medium conditions allowing Ly α photons
to escape.
acknowledgement: "We thank the anonymous referee for their constructive comments that
helped us improve the manuscript. DS acknowledges the hospitality of the IAC and
a Severo Ochoa visiting grant. SS and JC acknowledge studentships from the Lancaster
University. JM acknowledges a Huygens PhD fellowship from Leiden University. APA
acknowledges financial support from the Science and Technology Foundation (FCT,
Portugal) through research grants UID/FIS/04434/2013 and fellowship PD/BD/52706/2014.
The authors thank Alyssa Drake, Kimihiko Nakajima, Yuichi Harikane, Max Gronke,
Irene Shivaei, Helmut Dannerbauer, Huub Rottgering, ¨ Marius Eide, and Masami Ouchi
for many engaging and stimulating discussions. We also thank Sara Perez, Alex Bennett,
and Tom Rose for their involvement in the early stages of this project. Based on
data products from observations made with European Southern Observatory (ESO) Telescopes
at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 097.A 0943,\r\n098.A-0819,
099.A-0254, and 179.A-2005 and on data products produced by TERAPIX and the Cambridge
Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations
using the WFC on the 2.5 m INT, as part of programmes 2013AN002, 2013BN008, 2014AC88,
2014AN002, 2014BN006, 2014BC118, and 2016AN001. The 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. 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 (CFHTLS), a collaborative
project of NRC and CNRS.\r\nWe are grateful to the CFHTLS, COSMOS-UltraVISTA, and
COSMOS survey teams. We are also unmeasurably thankful to the pioneering and continuous
work from previous Ly α surveys’ teams. Without these previous Ly α and the wider
reach legacy surveys, this research would have been impossible. We also thank the
VUDS team for making available spectroscopic redshifts from data obtained with VIMOS
at the European Southern Observatory Very Large Telescope, Paranal, Chile, under
Large Programme 185.A-0791. Finally, the authors acknowledge the unique value of
the publicly available programming language PYTHON, including the NUMPY and 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 2005). We publicly release a catalogue with all LAEs used in this paper
(SC4K), so it can be freely explored by the community (see five example entries
in Table A1)."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- 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: Bruno
full_name: Ribeiro, Bruno
last_name: Ribeiro
- first_name: João
full_name: Calhau, João
last_name: Calhau
- first_name: Ali A
full_name: Khostovan, Ali A
last_name: Khostovan
citation:
ama: 'Sobral D, Santos S, Matthee JJ, et al. Slicing COSMOS with SC4K: The evolution
of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly
Notices of the Royal Astronomical Society. 2018;476(4):4725-4752. doi:10.1093/mnras/sty378'
apa: 'Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Ribeiro, B., Calhau,
J., & Khostovan, A. A. (2018). Slicing COSMOS with SC4K: The evolution of
typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly
Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty378'
chicago: 'Sobral, David, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso, Bruno
Ribeiro, João Calhau, and Ali A Khostovan. “Slicing COSMOS with SC4K: The Evolution
of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” Monthly
Notices of the Royal Astronomical Society. Oxford University Press, 2018.
https://doi.org/10.1093/mnras/sty378.'
ieee: 'D. Sobral et al., “Slicing COSMOS with SC4K: The evolution of typical
Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6,” Monthly Notices
of the Royal Astronomical Society, vol. 476, no. 4. Oxford University Press,
pp. 4725–4752, 2018.'
ista: 'Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Ribeiro B, Calhau J, Khostovan
AA. 2018. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and
the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical
Society. 476(4), 4725–4752.'
mla: 'Sobral, David, et al. “Slicing COSMOS with SC4K: The Evolution of Typical
Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” Monthly Notices
of the Royal Astronomical Society, vol. 476, no. 4, Oxford University Press,
2018, pp. 4725–52, doi:10.1093/mnras/sty378.'
short: D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, B. Ribeiro, J. Calhau,
A.A. Khostovan, Monthly Notices of the Royal Astronomical Society 476 (2018) 4725–4752.
date_created: 2022-07-12T10:41:08Z
date_published: 2018-06-01T00:00:00Z
date_updated: 2022-08-19T07:04:45Z
day: '01'
doi: 10.1093/mnras/sty378
extern: '1'
external_id:
arxiv:
- '1712.04451'
intvolume: ' 476'
issue: '4'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: high-redshift'
- 'galaxies: luminosity function'
- mass function
- 'galaxies: statistics'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1712.04451
month: '06'
oa: 1
oa_version: Preprint
page: 4725-4752
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: 'Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α
escape fraction from z ∼ 2 to 6'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 476
year: '2018'
...
---
_id: '11584'
abstract:
- lang: eng
text: Observations show that star-forming galaxies reside on a tight 3D plane between
mass, gas-phase metallicity, and star formation rate (SFR), which can be explained
by the interplay between metal-poor gas inflows, SFR and outflows. However, different
metals are released on different time-scales, which may affect the slope of this
relation. Here, we use central, star-forming galaxies with Mstar = 109.0–10.5
M⊙ from the EAGLE hydrodynamical simulation to examine 3D relations between mass,
SFR, and chemical enrichment using absolute and relative C, N, O, and Fe abundances.
We show that the scatter is smaller when gas-phase α-enhancement is used rather
than metallicity. A similar plane also exists for stellar α-enhancement, implying
that present-day specific SFRs are correlated with long time-scale star formation
histories. Between z = 0 and 1, the α-enhancement plane is even more insensitive
to redshift than the plane using metallicity. However, it evolves at z > 1 due
to lagging iron yields. At fixed mass, galaxies with higher SFRs have star formation
histories shifted towards late times, are more α-enhanced, and this α-enhancement
increases with redshift as observed. These findings suggest that relations between
physical properties inferred from observations may be affected by systematic variations
in α-enhancements.
acknowledgement: We thank the anonymous referee for their constructive comments. JM
acknowledges the support of a Huygens PhD fellowship from Leiden University. We
thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge
the use of the TOPCAT software (Taylor 2013) for assisting in rapid exploration
of multidimensional data sets and the use of PYTHON and its NUMPY, MATPLOTLIB, and
PANDAS packages.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
citation:
ama: 'Matthee JJ, Schaye J. Star-forming galaxies are predicted to lie on a fundamental
plane of mass, star formation rate, and α-enhancement. Monthly Notices of the
Royal Astronomical Society: Letters. 2018;479(1):L34-L39. doi:10.1093/mnrasl/sly093'
apa: 'Matthee, J. J., & Schaye, J. (2018). Star-forming galaxies are predicted
to lie on a fundamental plane of mass, star formation rate, and α-enhancement.
Monthly Notices of the Royal Astronomical Society: Letters. Oxford University
Press. https://doi.org/10.1093/mnrasl/sly093'
chicago: 'Matthee, Jorryt J, and Joop Schaye. “Star-Forming Galaxies Are Predicted
to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.”
Monthly Notices of the Royal Astronomical Society: Letters. Oxford University
Press, 2018. https://doi.org/10.1093/mnrasl/sly093.'
ieee: 'J. J. Matthee and J. Schaye, “Star-forming galaxies are predicted to lie
on a fundamental plane of mass, star formation rate, and α-enhancement,” Monthly
Notices of the Royal Astronomical Society: Letters, vol. 479, no. 1. Oxford
University Press, pp. L34–L39, 2018.'
ista: 'Matthee JJ, Schaye J. 2018. Star-forming galaxies are predicted to lie on
a fundamental plane of mass, star formation rate, and α-enhancement. Monthly Notices
of the Royal Astronomical Society: Letters. 479(1), L34–L39.'
mla: 'Matthee, Jorryt J., and Joop Schaye. “Star-Forming Galaxies Are Predicted
to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.”
Monthly Notices of the Royal Astronomical Society: Letters, vol. 479, no.
1, Oxford University Press, 2018, pp. L34–39, doi:10.1093/mnrasl/sly093.'
short: 'J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society:
Letters 479 (2018) L34–L39.'
date_created: 2022-07-14T12:49:47Z
date_published: 2018-09-01T00:00:00Z
date_updated: 2024-10-14T11:37:53Z
day: '01'
doi: 10.1093/mnrasl/sly093
extern: '1'
external_id:
arxiv:
- '1802.06786'
intvolume: ' 479'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: abundances'
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: star formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1802.06786
month: '09'
oa: 1
oa_version: Preprint
page: L34 - L39
publication: 'Monthly Notices of the Royal Astronomical Society: Letters'
publication_identifier:
eissn:
- 1745-3933
issn:
- 1745-3925
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Star-forming galaxies are predicted to lie on a fundamental plane of mass,
star formation rate, and α-enhancement
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 479
year: '2018'
...
---
_id: '11518'
abstract:
- lang: eng
text: "We present spectroscopic follow-up observations of CR7 with ALMA, targeted
at constraining the infrared (IR) continuum and [C II]158 mm line-emission at
high spatial resolution matched to the HST/WFC3 imaging. CR7 is a luminous Lyα
emitting galaxy at z = 6.6 that consists of three separated UV-continuum components.
Our observations reveal several well-separated components of [C II] emission.
The two most luminous components in [C II] coincide with the brightest UV components
(A and B), blueshifted by »150 km s−1 with respect to the\r\npeak of Lyα emission.
Other [C II] components are observed close to UV clumps B and C and are blueshifted
by »300 and ≈80 km s−1 with respect to the systemic redshift. We do not detect
FIR continuum emission due to dust with a 3σ limiting luminosity LIR T L d 35
K 3.1 10 = <´ 10 ( ) . This allows us to mitigate uncertainties in the dust-corrected
SFR and derive SFRs for the three UV clumps A, B, and C of 28, 5, and 7 M yr−1.
All clumps have [C II] luminosities consistent within the scatter observed in
the local relation between SFR and L[ ] C II , implying that strong Lyα emission
does not necessarily anti-correlate with [C II] luminosity. Combining\r\nour measurements
with the literature, we show that galaxies with blue UV slopes have weaker [C
II] emission at fixed SFR, potentially due to their lower metallicities and/or
higher photoionization. Comparison with hydrodynamical simulations suggests that
CR7ʼs clumps have metallicities of 0.1 Z Z 0.2 < < . The observed ISM structure
of CR7 indicates that we are likely witnessing the build up of a central galaxy
in the early universe through complex accretion of satellites."
acknowledgement: 'We thank the referee for their constructive comments, which have
helped improve the quality and clarity of this work. We thank Raffaella Schneider
for comments on an earlier version of this paper. We thank Leindert Boogaard, Steven
Bos, Rychard Bouwens, and Renske Smit for discussions. J.M. acknowledges the support
of a Huygens PhD fellowship from Leiden University. D.S. acknowledges financial
support from the Netherlands Organisation for Scientific research (NWO) through
a Veni fellowship and from Lancaster University through an Early Career Internal
Grant A100679. A.F. acknowledges support from the ERC Advanced Grant INTERSTELLAR
H2020/740120. B.D. acknowledges financial support from NASA through the Astrophysics
Data Analysis Program (ADAP), grant number NNX12AE20G. Based on observations made
with ESO Telescopes at the La Silla Paranal Observatory under programme ID 294.A-5018.
This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00122.S. ALMA
is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan),
together with NRC (Canada) and NSC and ASIAA (Taiwan), and KASI (Republic of Korea),
in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated
by ESO, AUI/NRAO, and NAOJ.'
article_number: '145'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: D.
full_name: Sobral, D.
last_name: Sobral
- first_name: F.
full_name: Boone, F.
last_name: Boone
- first_name: H.
full_name: Röttgering, H.
last_name: Röttgering
- first_name: D.
full_name: Schaerer, D.
last_name: Schaerer
- first_name: M.
full_name: Girard, M.
last_name: Girard
- first_name: A.
full_name: Pallottini, A.
last_name: Pallottini
- first_name: L.
full_name: Vallini, L.
last_name: Vallini
- first_name: A.
full_name: Ferrara, A.
last_name: Ferrara
- first_name: B.
full_name: Darvish, B.
last_name: Darvish
- first_name: B.
full_name: Mobasher, B.
last_name: Mobasher
citation:
ama: Matthee JJ, Sobral D, Boone F, et al. ALMA reveals metals yet no dust within
multiple components in CR7. The Astrophysical Journal. 2017;851(2). doi:10.3847/1538-4357/aa9931
apa: Matthee, J. J., Sobral, D., Boone, F., Röttgering, H., Schaerer, D., Girard,
M., … Mobasher, B. (2017). ALMA reveals metals yet no dust within multiple components
in CR7. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/aa9931
chicago: Matthee, Jorryt J, D. Sobral, F. Boone, H. Röttgering, D. Schaerer, M.
Girard, A. Pallottini, et al. “ALMA Reveals Metals yet No Dust within Multiple
Components in CR7.” The Astrophysical Journal. IOP Publishing, 2017. https://doi.org/10.3847/1538-4357/aa9931.
ieee: J. J. Matthee et al., “ALMA reveals metals yet no dust within multiple
components in CR7,” The Astrophysical Journal, vol. 851, no. 2. IOP Publishing,
2017.
ista: Matthee JJ, Sobral D, Boone F, Röttgering H, Schaerer D, Girard M, Pallottini
A, Vallini L, Ferrara A, Darvish B, Mobasher B. 2017. ALMA reveals metals yet
no dust within multiple components in CR7. The Astrophysical Journal. 851(2),
145.
mla: Matthee, Jorryt J., et al. “ALMA Reveals Metals yet No Dust within Multiple
Components in CR7.” The Astrophysical Journal, vol. 851, no. 2, 145, IOP
Publishing, 2017, doi:10.3847/1538-4357/aa9931.
short: J.J. Matthee, D. Sobral, F. Boone, H. Röttgering, D. Schaerer, M. Girard,
A. Pallottini, L. Vallini, A. Ferrara, B. Darvish, B. Mobasher, The Astrophysical
Journal 851 (2017).
date_created: 2022-07-07T08:48:04Z
date_published: 2017-12-21T00:00:00Z
date_updated: 2024-10-14T11:32:14Z
day: '21'
doi: 10.3847/1538-4357/aa9931
extern: '1'
external_id:
arxiv:
- '1709.06569'
intvolume: ' 851'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- dark ages
- reionization
- 'first stars – galaxies: formation – galaxies: high-redshift – galaxies: ISM – galaxies:
kinematics and dynamics'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1709.06569
month: '12'
oa: 1
oa_version: Preprint
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: ALMA reveals metals yet no dust within multiple components in CR7
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 851
year: '2017'
...
---
_id: '11565'
abstract:
- lang: eng
text: We use the hydrodynamical EAGLE simulation to study the magnitude and origin
of the scatter in the stellar mass–halo mass relation for central galaxies. We
separate cause and effect by correlating stellar masses in the baryonic simulation
with halo properties in a matched dark matter only (DMO) simulation. The scatter
in stellar mass increases with redshift and decreases with halo mass. At z = 0.1,
it declines from 0.25 dex at M200, DMO ≈ 1011 M⊙ to 0.12 dex at M200, DMO ≈ 1013
M⊙, but the trend is weak above 1012 M⊙. For M200, DMO < 1012.5 M⊙ up to 0.04
dex of the scatter is due to scatter in the halo concentration. At fixed halo
mass, a larger stellar mass corresponds to a more concentrated halo. This is likely
because higher concentrations imply earlier formation times and hence more time
for accretion and star formation, and/or because feedback is less efficient in
haloes with higher binding energies. The maximum circular velocity, Vmax, DMO,
and binding energy are therefore more fundamental properties than halo mass, meaning
that they are more accurate predictors of stellar mass, and we provide fitting
formulae for their relations with stellar mass. However, concentration alone cannot
explain the total scatter in the Mstar−M200,DMO relation, and it does not explain
the scatter in Mstar–Vmax, DMO. Halo spin, sphericity, triaxiality, substructure
and environment are also not responsible for the remaining scatter, which thus
could be due to more complex halo properties or non-linear/stochastic baryonic
effects.
acknowledgement: We thank the anonymous referee for their comments. JM acknowledges
the support of a Huygens PhD fellowship from Leiden University. JM thanks David
Sobral for useful discussions and help with fitting routines and Jonas Chavez Montero
and Ying Zu for providing data. We thank PRACE for the access to the Curie facility
in France. We have used the DiRAC system which is a part of National E-Infrastructure
at Durham University, operated by the Institute for Computational Cosmology on behalf
of the STFC DiRAC HPC Facility (www.dirac.ac.uk); the equipment was funded by BIS
National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1,
STFC DiRAC Operations grant ST/K003267/1 and Durham University. The study was sponsored
by the Dutch National Computing Facilities Foundation (NCF) for the use of supercomputer
facilities, with financial support from the Netherlands Organisation for Scientific
Research (NWO), through VICI grant 639.043.409, and the European Research Council
under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC Grant
agreement 278594- GasAroundGalaxies, and from the Belgian Science Policy Office
([AP P7/08 CHARM]). We have benefited greatly from the public available programming
language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY, H5PY and RPY2 packages,
and the TOPCAT analysis program (Taylor 2005).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Robert A.
full_name: Crain, Robert A.
last_name: Crain
- first_name: Matthieu
full_name: Schaller, Matthieu
last_name: Schaller
- first_name: Richard
full_name: Bower, Richard
last_name: Bower
- first_name: Tom
full_name: Theuns, Tom
last_name: Theuns
citation:
ama: Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. The origin of
scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE
simulation. Monthly Notices of the Royal Astronomical Society. 2017;465(2):2381-2396.
doi:10.1093/mnras/stw2884
apa: Matthee, J. J., Schaye, J., Crain, R. A., Schaller, M., Bower, R., & Theuns,
T. (2017). The origin of scatter in the stellar mass–halo mass relation of central
galaxies in the EAGLE simulation. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stw2884
chicago: Matthee, Jorryt J, Joop Schaye, Robert A. Crain, Matthieu Schaller, Richard
Bower, and Tom Theuns. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation
of Central Galaxies in the EAGLE Simulation.” Monthly Notices of the Royal
Astronomical Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stw2884.
ieee: J. J. Matthee, J. Schaye, R. A. Crain, M. Schaller, R. Bower, and T. Theuns,
“The origin of scatter in the stellar mass–halo mass relation of central galaxies
in the EAGLE simulation,” Monthly Notices of the Royal Astronomical Society,
vol. 465, no. 2. Oxford University Press, pp. 2381–2396, 2017.
ista: Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. 2017. The origin
of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE
simulation. Monthly Notices of the Royal Astronomical Society. 465(2), 2381–2396.
mla: Matthee, Jorryt J., et al. “The Origin of Scatter in the Stellar Mass–Halo
Mass Relation of Central Galaxies in the EAGLE Simulation.” Monthly Notices
of the Royal Astronomical Society, vol. 465, no. 2, Oxford University Press,
2017, pp. 2381–96, doi:10.1093/mnras/stw2884.
short: J.J. Matthee, J. Schaye, R.A. Crain, M. Schaller, R. Bower, T. Theuns, Monthly
Notices of the Royal Astronomical Society 465 (2017) 2381–2396.
date_created: 2022-07-12T12:25:08Z
date_published: 2017-02-01T00:00:00Z
date_updated: 2024-10-14T11:36:05Z
day: '01'
doi: 10.1093/mnras/stw2884
extern: '1'
external_id:
arxiv:
- '1608.08218'
intvolume: ' 465'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: haloes'
- 'cosmology: theory'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1608.08218
month: '02'
oa: 1
oa_version: Preprint
page: 2381-2396
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The origin of scatter in the stellar mass–halo mass relation of central galaxies
in the EAGLE simulation
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 465
year: '2017'
...
---
_id: '11575'
abstract:
- lang: eng
text: We investigate correlations between different physical properties of star-forming
galaxies in the ‘Evolution and Assembly of GaLaxies and their Environments’ (EAGLE)
cosmological hydrodynamical simulation suite over the redshift range 0 ≤ z ≤ 4.5.
A principal component analysis reveals that neutral gas fraction (fgas,neutral),
stellar mass (Mstellar) and star formation rate (SFR) account for most of the
variance seen in the population, with galaxies tracing a two-dimensional, nearly
flat, surface in the three-dimensional space of fgas, neutral–Mstellar–SFR with
little scatter. The location of this plane varies little with redshift, whereas
galaxies themselves move along the plane as their fgas, neutral and SFR drop with
redshift. The positions of galaxies along the plane are highly correlated with
gas metallicity. The metallicity can therefore be robustly predicted from fgas,
neutral, or from the Mstellar and SFR. We argue that the appearance of this ‘Fundamental
Plane of star formation’ is a consequence of self-regulation, with the plane's
curvature set by the dependence of the SFR on gas density and metallicity. We
analyse a large compilation of observations spanning the redshift range 0 ≲ z
≲ 3, and find that such a plane is also present in the data. The properties of
the observed Fundamental Plane of star formation are in good agreement with EAGLE's
predictions.
acknowledgement: We thank Luca Cortese, Matt Bothwell, Paola Santini and Tim Davis
for providing observational data sets, and Aaron Robotham, Luca Cortese and Barbara
Catinella for useful discussions. CdPL is funded by a Discovery Early Career Researcher
Award (DE150100618). CdPL also thanks the MERAC Foundation for a Postdoctoral Research
Award. This work used the DiRAC Data Centric system at Durham University, operated
by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility
(www.dirac.ac.uk). This equipment was funded by BIS National E-infrastructure capital
grant ST/K00042X/1, STFC capital grant ST/H008519/1, and STFC DiRAC Operations grant
ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure.
Support was also received via the Interuniversity Attraction Poles Programme initiated
by the Belgian Science Policy Office ([AP P7/08 CHARM]), the National Science Foundation
under grant no. NSF PHY11-25915, and the UK Science and Technology Facilities Council
(grant numbers ST/F001166/1 and ST/I000976/1) via rolling and consolidating grants
awarded to the ICC. The research was supported in part by the European Research
Council under the European Union‘s Seventh Framework Programme (FP7/2007-2013)/ERC
grant agreement 278594-GasAroundGalaxies.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Claudia del P.
full_name: Lagos, Claudia del P.
last_name: Lagos
- first_name: Tom
full_name: Theuns, Tom
last_name: Theuns
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Michelle
full_name: Furlong, Michelle
last_name: Furlong
- first_name: Richard G.
full_name: Bower, Richard G.
last_name: Bower
- first_name: Matthieu
full_name: Schaller, Matthieu
last_name: Schaller
- first_name: Robert A.
full_name: Crain, Robert A.
last_name: Crain
- first_name: James W.
full_name: Trayford, James W.
last_name: Trayford
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
citation:
ama: Lagos C del P, Theuns T, Schaye J, et al. The Fundamental Plane of star formation
in galaxies revealed by the EAGLE hydrodynamical simulations. Monthly Notices
of the Royal Astronomical Society. 2016;459(3):2632-2650. doi:10.1093/mnras/stw717
apa: Lagos, C. del P., Theuns, T., Schaye, J., Furlong, M., Bower, R. G., Schaller,
M., … Matthee, J. J. (2016). The Fundamental Plane of star formation in galaxies
revealed by the EAGLE hydrodynamical simulations. Monthly Notices of the Royal
Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw717
chicago: Lagos, Claudia del P., Tom Theuns, Joop Schaye, Michelle Furlong, Richard
G. Bower, Matthieu Schaller, Robert A. Crain, James W. Trayford, and Jorryt J
Matthee. “The Fundamental Plane of Star Formation in Galaxies Revealed by the
EAGLE Hydrodynamical Simulations.” Monthly Notices of the Royal Astronomical
Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw717.
ieee: C. del P. Lagos et al., “The Fundamental Plane of star formation in
galaxies revealed by the EAGLE hydrodynamical simulations,” Monthly Notices
of the Royal Astronomical Society, vol. 459, no. 3. Oxford University Press,
pp. 2632–2650, 2016.
ista: Lagos C del P, Theuns T, Schaye J, Furlong M, Bower RG, Schaller M, Crain
RA, Trayford JW, Matthee JJ. 2016. The Fundamental Plane of star formation in
galaxies revealed by the EAGLE hydrodynamical simulations. Monthly Notices of
the Royal Astronomical Society. 459(3), 2632–2650.
mla: Lagos, Claudia del P., et al. “The Fundamental Plane of Star Formation in Galaxies
Revealed by the EAGLE Hydrodynamical Simulations.” Monthly Notices of the Royal
Astronomical Society, vol. 459, no. 3, Oxford University Press, 2016, pp.
2632–50, doi:10.1093/mnras/stw717.
short: C. del P. Lagos, T. Theuns, J. Schaye, M. Furlong, R.G. Bower, M. Schaller,
R.A. Crain, J.W. Trayford, J.J. Matthee, Monthly Notices of the Royal Astronomical
Society 459 (2016) 2632–2650.
date_created: 2022-07-13T10:21:24Z
date_published: 2016-07-01T00:00:00Z
date_updated: 2022-08-19T08:12:07Z
day: '01'
doi: 10.1093/mnras/stw717
extern: '1'
external_id:
arxiv:
- '1510.08067'
intvolume: ' 459'
issue: '3'
keyword:
- Space and Planetary Science
- 'Astronomy and Astrophysics stars: formation'
- 'ISM: evolution'
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: ISM'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1510.08067
month: '07'
oa: 1
oa_version: Preprint
page: 2632-2650
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical
simulations
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 459
year: '2016'
...
---
_id: '11580'
abstract:
- lang: eng
text: 'We present results from the largest contiguous narrow-band survey in the
near-infrared. We have used the wide-field infrared camera/Canada–France–Hawaii
Telescope and the lowOH2 filter (1.187 ± 0.005 μm) to survey ≈10 deg2 of contiguous
extragalactic sky in the SA22 field. A total of ∼6000 candidate emission-line
galaxies are found. We use deep ugrizJK data to obtain robust photometric redshifts.
We combine our data with the High-redshift(Z) Emission Line Survey (HiZELS), explore
spectroscopic surveys (VVDS, VIPERS) and obtain our own spectroscopic follow-up
with KMOS, FMOS and MOSFIRE to derive large samples of high-redshift emission-line
selected galaxies: 3471 Hα emitters at z = 0.8, 1343 [O III] + Hβ emitters at
z = 1.4 and 572 [O II] emitters at z = 2.2. We probe comoving volumes of >106
Mpc3 and find significant overdensities, including an 8.5σ (spectroscopically
confirmed) overdensity of Hα emitters at z = 0.81. We derive Hα, [O III] + Hβ
and [O II] luminosity functions at z = 0.8, 1.4, 2.2, respectively, and present
implications for future surveys such as Euclid. Our uniquely large volumes/areas
allow us to subdivide the samples in thousands of randomized combinations of areas
and provide a robust empirical measurement of sample/cosmic variance. We show
that surveys for star-forming/emission-line galaxies at a depth similar to ours
can only overcome cosmic-variance (errors <10 per cent) if they are based on volumes
>5 × 105 Mpc3; errors on L* and ϕ* due to sample (cosmic) variance on surveys
probing ∼104 and ∼105 Mpc3 are typically very high: ∼300 and ∼40–60 per cent,
respectively.'
acknowledgement: The authors wish to thank the anonymous reviewer for many helpful
comments and suggestions which greatly improved the clarity and quality of this
work. DS acknowledges financial support from the Netherlands Organization for Scientific
research (NWO) through a Veni fellowship, from FCT through an FCT Investigator Starting
Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010), from FCT grant PEst-OE/FIS/UI2751/2014,
and from LSF and LKBF. JM acknowledges the award of a Huygens PhD fellowship. PNB
is grateful for support from STFC. IRS acknowledges support from STFC, a Leverhulme
Fellowship, the ERC Advanced Investigator programme DUSTYGAL and a Royal Society/Wolfson
Merit Award. BMJ acknowledges support from the ERC-StG grant EGGS-278202. The Dark
Cosmology Centre is funded by the DNRF. The Dark Cosmology Centre is funded by the
DNRF. JWK acknowledges support from the National Research Foundation of Korea (NRF)
grant, no. 2008-0060544, funded by the Korea government (MSIP). JPS acknowledges
support from STFC (ST/I001573/1). JC acknowledges support from the FCT-IF grant
IF/01154/2012/CP0189/CT0010. The work was only possible due to OPTICON/FP7 and the
invaluable access that it granted to the CFHT telescope. We would also like to acknowledge
the excellent work done by CFHT staff in conducting the observations in service
mode, and on delivering truly excellent data. We are also tremendously thankful
to Kentaro Aoki for the incredible support while observing at Subaru with FMOS,
and also to the Keck staff for the help with the observations with MOSFIRE. This
work is based on observations obtained with WIRCam on the CFHT, OPTICON programme
2011B/029, 2012A019 and 2012B/016. Based on observations made with ESO telescopes
at the La Silla Paranal Observatory under programmes IDs 60.A-9460 (data can be
accessed through the ESO data archive), 087.A 0337 and 089.A-0965. Based on observations
done with FMOS on Subaru under programme S14A-084, and on MOSFIRE/Keck observations
under programme U066M. Part of the data on which this analysis is based are available
from Sobral et al. (2013a). Dedicated to the memory of C. M. Sobral (1953-2014).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: D.
full_name: Sobral, D.
last_name: Sobral
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: P. N.
full_name: Best, P. N.
last_name: Best
- first_name: I.
full_name: Smail, I.
last_name: Smail
- first_name: A. A.
full_name: Khostovan, A. A.
last_name: Khostovan
- first_name: B.
full_name: Milvang-Jensen, B.
last_name: Milvang-Jensen
- first_name: J.-W.
full_name: Kim, J.-W.
last_name: Kim
- first_name: J.
full_name: Stott, J.
last_name: Stott
- first_name: J.
full_name: Calhau, J.
last_name: Calhau
- first_name: H.
full_name: Nayyeri, H.
last_name: Nayyeri
- first_name: B.
full_name: Mobasher, B.
last_name: Mobasher
citation:
ama: 'Sobral D, Matthee JJ, Best PN, et al. CF-HiZELS, an ∼10 deg2 emission-line
survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions
at z = 0.8, 1.4 and 2.2 . Monthly Notices of the Royal Astronomical Society.
2015;451(3):2303-2323. doi:10.1093/mnras/stv1076'
apa: 'Sobral, D., Matthee, J. J., Best, P. N., Smail, I., Khostovan, A. A., Milvang-Jensen,
B., … Mobasher, B. (2015). CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic
follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and
2.2 . Monthly Notices of the Royal Astronomical Society. Oxford University
Press. https://doi.org/10.1093/mnras/stv1076'
chicago: 'Sobral, D., Jorryt J Matthee, P. N. Best, I. Smail, A. A. Khostovan, B.
Milvang-Jensen, J.-W. Kim, et al. “CF-HiZELS, an ∼10 Deg2 Emission-Line Survey
with Spectroscopic Follow-up: Hα, [O III] + Hβ and [O II] Luminosity Functions
at z = 0.8, 1.4 and 2.2 .” Monthly Notices of the Royal Astronomical Society.
Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv1076.'
ieee: 'D. Sobral et al., “CF-HiZELS, an ∼10 deg2 emission-line survey with
spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z
= 0.8, 1.4 and 2.2 ,” Monthly Notices of the Royal Astronomical Society,
vol. 451, no. 3. Oxford University Press, pp. 2303–2323, 2015.'
ista: 'Sobral D, Matthee JJ, Best PN, Smail I, Khostovan AA, Milvang-Jensen B, Kim
J-W, Stott J, Calhau J, Nayyeri H, Mobasher B. 2015. CF-HiZELS, an ∼10 deg2 emission-line
survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions
at z = 0.8, 1.4 and 2.2 . Monthly Notices of the Royal Astronomical Society. 451(3),
2303–2323.'
mla: 'Sobral, D., et al. “CF-HiZELS, an ∼10 Deg2 Emission-Line Survey with Spectroscopic
Follow-up: Hα, [O III] + Hβ and [O II] Luminosity Functions at z = 0.8, 1.4 and
2.2 .” Monthly Notices of the Royal Astronomical Society, vol. 451, no.
3, Oxford University Press, 2015, pp. 2303–23, doi:10.1093/mnras/stv1076.'
short: D. Sobral, J.J. Matthee, P.N. Best, I. Smail, A.A. Khostovan, B. Milvang-Jensen,
J.-W. Kim, J. Stott, J. Calhau, H. Nayyeri, B. Mobasher, Monthly Notices of the
Royal Astronomical Society 451 (2015) 2303–2323.
date_created: 2022-07-14T09:02:22Z
date_published: 2015-08-11T00:00:00Z
date_updated: 2024-10-14T11:36:57Z
day: '11'
doi: 10.1093/mnras/stv1076
extern: '1'
external_id:
arxiv:
- '1502.06602'
intvolume: ' 451'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: luminosity function'
- mass function
- 'cosmology: observations'
- early Universe
- large-scale structure of Universe
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1502.06602
month: '08'
oa: 1
oa_version: Preprint
page: 2303-2323
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up:
Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 '
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 451
year: '2015'
...