---
_id: '11488'
abstract:
- lang: eng
text: Hydrogen Lyα haloes (LAHs) are commonly used as a tracer of the circumgalactic
medium (CGM) at high redshifts. In this work, we aim to explore the existence
of Lyα haloes around individual UV-selected galaxies, rather than around Lyα emitters
(LAEs), at high redshifts. Our sample was continuum-selected with F775W ≤ 27.5,
and spectroscopic redshifts were assigned or constrained for all the sources thanks
to the deepest (100- to 140-h) existing Very Large Telescope (VLT)/Multi-Unit
Spectroscopic Explorer (MUSE) data with adaptive optics. The final sample includes
21 galaxies that are purely F775W-magnitude selected within the redshift range
z ≈ 2.9 − 4.4 and within a UV magnitude range −20 ≤ M1500 ≤ −18, thus avoiding
any bias toward LAEs. We tested whether galaxy’s Lyα emission is significantly
more extended than the MUSE PSF-convolved continuum component. We find 17 LAHs
and four non-LAHs. We report the first individual detections of extended Lyα emission
around non-LAEs. The Lyα halo fraction is thus as high as 81.0−11.2+10.3%, which
is close to that for LAEs at z = 3 − 6 in the literature. This implies that UV-selected
galaxies generally have a large amount of hydrogen in their CGM. We derived the
mean surface brightness (SB) profile for our LAHs with cosmic dimming corrections
and find that Lyα emission extends to 5.4 arcsec (≃40 physical kpc at the midpoint
redshift z = 3.6) above the typical 1σ SB limit. The incidence rate of surrounding
gas detected in Lyα per one-dimensional line of sight per unit redshift, dn/dz,
is estimated to be 0.76−0.09+0.09 for galaxies with M1500 ≤ −18 mag at z ≃ 3.7.
Assuming that Lyα emission and absorption arise in the same gas, this suggests,
based on abundance matching, that LAHs trace the same gas as damped Lyα systems
(DLAs) and sub-DLAs.
acknowledgement: 'We thank the anonymous referee for constructive comments and suggestions.
We would like to express our gratitude to Edmund Christian Herenz, Leindert Boogard,
Miroslava Dessauges, Moupiya Maji, Valentin Mauerhofer, Charlotte Paola Simmonds
Wagemann, Masami Ouchi, Kazuhiro Shimasaku, Akio Inoue, and Rieko Momose for giving
insightful comments and suggestions. H.K. is grateful to Liam McCarney for useful
suggestions on English writing through the UniGE’s Tandems linguistiques. H.K. acknowledges
support from Swiss Government Excellence Scholarships and Japan Society for the
Promotion of Science (JSPS) Overseas Research Fellowship. H.K., F.L., and A.V. are
supported by the SNF grant PP00P2 176808. A.V. and T.G. are supported by the ERC
Starting Grant 757258“TRIPLE”. This work was supported by the Programme National
Cosmology et Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and
CNES. This work is based on observations taken by VLT, which is operated by European
Southern Observatory. This research made use of Astropy, which is a community-developed
core Python package for Astronomy (Astropy Collaboration 2013, 2018), and other
software and packages: MARZ, MPDAF (Piqueras et al. 2019), PHOTUTILS, Numpy (Harris
et al. 2020), Scipy (Virtanen et al. 2020), and matplotlib (Hunter 2007).'
article_number: A44
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- first_name: Anne
full_name: Verhamme, Anne
last_name: Verhamme
- first_name: Jérémy
full_name: Blaizot, Jérémy
last_name: Blaizot
- first_name: Thibault
full_name: Garel, Thibault
last_name: Garel
- first_name: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
- first_name: Floriane
full_name: Leclercq, Floriane
last_name: Leclercq
- first_name: Roland
full_name: Bacon, Roland
last_name: Bacon
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Sofia G.
full_name: Gallego, Sofia G.
last_name: Gallego
- first_name: Josephine
full_name: Kerutt, Josephine
last_name: Kerutt
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Michael
full_name: Maseda, Michael
last_name: Maseda
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
- first_name: Roser
full_name: Pelló, Roser
last_name: Pelló
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Laurence
full_name: Tresse, Laurence
last_name: Tresse
- first_name: Tanya
full_name: Urrutia, Tanya
last_name: Urrutia
- first_name: Eloïse
full_name: Vitte, Eloïse
last_name: Vitte
citation:
ama: 'Kusakabe H, Verhamme A, Blaizot J, et al. The MUSE eXtremely Deep Field: Individual
detections of Lyα haloes around rest-frame UV-selected galaxies at z
≃ 2.9–4.4. Astronomy & Astrophysics. 2022;660. doi:10.1051/0004-6361/202142302'
apa: 'Kusakabe, H., Verhamme, A., Blaizot, J., Garel, T., Wisotzki, L., Leclercq,
F., … Vitte, E. (2022). The MUSE eXtremely Deep Field: Individual detections of
Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4.
Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202142302'
chicago: 'Kusakabe, Haruka, Anne Verhamme, Jérémy Blaizot, Thibault Garel, Lutz
Wisotzki, Floriane Leclercq, Roland Bacon, et al. “The MUSE EXtremely Deep Field:
Individual Detections of Lyα Haloes around Rest-Frame UV-Selected Galaxies
at z ≃ 2.9–4.4.” Astronomy & Astrophysics. EDP Sciences, 2022.
https://doi.org/10.1051/0004-6361/202142302.'
ieee: 'H. Kusakabe et al., “The MUSE eXtremely Deep Field: Individual detections
of Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4,”
Astronomy & Astrophysics, vol. 660. EDP Sciences, 2022.'
ista: 'Kusakabe H, Verhamme A, Blaizot J, Garel T, Wisotzki L, Leclercq F, Bacon
R, Schaye J, Gallego SG, Kerutt J, Matthee JJ, Maseda M, Nanayakkara T, Pelló
R, Richard J, Tresse L, Urrutia T, Vitte E. 2022. The MUSE eXtremely Deep Field:
Individual detections of Lyα haloes around rest-frame UV-selected galaxies
at z ≃ 2.9–4.4. Astronomy & Astrophysics. 660, A44.'
mla: 'Kusakabe, Haruka, et al. “The MUSE EXtremely Deep Field: Individual Detections
of Lyα Haloes around Rest-Frame UV-Selected Galaxies at z ≃ 2.9–4.4.”
Astronomy & Astrophysics, vol. 660, A44, EDP Sciences, 2022, doi:10.1051/0004-6361/202142302.'
short: H. Kusakabe, A. Verhamme, J. Blaizot, T. Garel, L. Wisotzki, F. Leclercq,
R. Bacon, J. Schaye, S.G. Gallego, J. Kerutt, J.J. Matthee, M. Maseda, T. Nanayakkara,
R. Pelló, J. Richard, L. Tresse, T. Urrutia, E. Vitte, Astronomy & Astrophysics
660 (2022).
date_created: 2022-07-05T14:27:26Z
date_published: 2022-04-07T00:00:00Z
date_updated: 2022-07-19T09:33:24Z
day: '07'
doi: 10.1051/0004-6361/202142302
extern: '1'
external_id:
arxiv:
- '2201.07257'
intvolume: ' 660'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology:
observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2201.07257
month: '04'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The MUSE eXtremely Deep Field: Individual detections of Lyα haloes
around rest-frame UV-selected galaxies at z ≃ 2.9–4.4'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 660
year: '2022'
...
---
_id: '11497'
abstract:
- lang: eng
text: "Context. The hydrogen Lyman α line is often the only measurable feature in
optical spectra of high-redshift galaxies. Its shape and strength are influenced
by radiative transfer processes and the properties of the underlying stellar population.
High equivalent widths of several hundred Å are especially hard to explain by
models and could point towards unusual stellar populations, for example with low
metallicities, young stellar ages, and a top-heavy initial mass function. Other
aspects influencing equivalent widths are the morphology of the galaxy and its
gas properties.\r\nAims. The aim of this study is to better understand the connection
between the Lyman α rest-frame equivalent width (EW0) and spectral properties
as well as ultraviolet (UV) continuum morphology by obtaining reliable EW0 histograms
for a statistical sample of galaxies and by assessing the fraction of objects
with large equivalent widths.\r\nMethods. We used integral field spectroscopy
from the Multi Unit Spectroscopic Explorer (MUSE) combined with broad-band data
from the Hubble Space Telescope (HST) to measure EW0. We analysed the emission
lines of 1920 Lyman α emitters (LAEs) detected in the full MUSE-Wide (one hour
exposure time) and MUSE-Deep (ten hour exposure time) surveys and found UV continuum
counterparts in archival HST data. We fitted the UV continuum photometric images
using the Galfit software to gain morphological information on the rest-UV emission
and fitted the spectra obtained from MUSE to determine the double peak fraction,
asymmetry, full-width at half maximum, and flux of the Lyman α line.\r\nResults.
The two surveys show different histograms of Lyman α EW0. In MUSE-Wide, 20% of
objects have EW0 > 240 Å, while this fraction is only 11% in MUSE-Deep and ≈16%
for the full sample. This includes objects without HST continuum counterparts
(one-third of our sample), for which we give lower limits for EW0. The object
with the highest securely measured EW0 has EW0 = 589 ± 193 Å (the highest lower
limit being EW0 = 4464 Å). We investigate the connection between EW0 and Lyman
α spectral or UV continuum morphological properties.\r\nConclusions. The survey
depth has to be taken into account when studying EW0 distributions. We find that
in general, high EW0 objects can have a wide range of spectral and UV morphological
properties, which might reflect that the underlying causes for high EW0 values
are equally varied."
acknowledgement: We thank the referee for thoughtful and constructive comments that
have improved the quality of this manuscript. Based on observations collected at
the European Southern Observatory under ESO programme 1101.A-0127. This work made
use of v2.2.1 of the Binary Population and Spectral Synthesis (BPASS) models as
described in Eldridge et al. (2017) and Stanway & Eldridge (2018). A.F. acknowledges
the support from grant PRIN MIUR2017-20173ML3WW_001. T.N. acknowledges support from
Australian Research Council Laureate Fellowship FL180100060.
article_number: '183'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: J.
full_name: Kerutt, J.
last_name: Kerutt
- first_name: L.
full_name: Wisotzki, L.
last_name: Wisotzki
- first_name: A.
full_name: Verhamme, A.
last_name: Verhamme
- first_name: K. B.
full_name: Schmidt, K. B.
last_name: Schmidt
- first_name: F.
full_name: Leclercq, F.
last_name: Leclercq
- first_name: E. C.
full_name: Herenz, E. C.
last_name: Herenz
- first_name: T.
full_name: Urrutia, T.
last_name: Urrutia
- first_name: T.
full_name: Garel, T.
last_name: Garel
- first_name: T.
full_name: Hashimoto, T.
last_name: Hashimoto
- first_name: M.
full_name: Maseda, M.
last_name: Maseda
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: H.
full_name: Kusakabe, H.
last_name: Kusakabe
- first_name: J.
full_name: Schaye, J.
last_name: Schaye
- first_name: J.
full_name: Richard, J.
last_name: Richard
- first_name: B.
full_name: Guiderdoni, B.
last_name: Guiderdoni
- first_name: V.
full_name: Mauerhofer, V.
last_name: Mauerhofer
- first_name: T.
full_name: Nanayakkara, T.
last_name: Nanayakkara
- first_name: E.
full_name: Vitte, E.
last_name: Vitte
citation:
ama: Kerutt J, Wisotzki L, Verhamme A, et al. Equivalent widths of Lyman α emitters
in MUSE-Wide and MUSE-Deep. Astronomy & Astrophysics. 2022;659. doi:10.1051/0004-6361/202141900
apa: Kerutt, J., Wisotzki, L., Verhamme, A., Schmidt, K. B., Leclercq, F., Herenz,
E. C., … Vitte, E. (2022). Equivalent widths of Lyman α emitters in MUSE-Wide
and MUSE-Deep. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202141900
chicago: Kerutt, J., L. Wisotzki, A. Verhamme, K. B. Schmidt, F. Leclercq, E. C.
Herenz, T. Urrutia, et al. “Equivalent Widths of Lyman α Emitters in MUSE-Wide
and MUSE-Deep.” Astronomy & Astrophysics. EDP Sciences, 2022. https://doi.org/10.1051/0004-6361/202141900.
ieee: J. Kerutt et al., “Equivalent widths of Lyman α emitters in MUSE-Wide
and MUSE-Deep,” Astronomy & Astrophysics, vol. 659. EDP Sciences, 2022.
ista: Kerutt J, Wisotzki L, Verhamme A, Schmidt KB, Leclercq F, Herenz EC, Urrutia
T, Garel T, Hashimoto T, Maseda M, Matthee JJ, Kusakabe H, Schaye J, Richard J,
Guiderdoni B, Mauerhofer V, Nanayakkara T, Vitte E. 2022. Equivalent widths of
Lyman α emitters in MUSE-Wide and MUSE-Deep. Astronomy & Astrophysics. 659,
183.
mla: Kerutt, J., et al. “Equivalent Widths of Lyman α Emitters in MUSE-Wide and
MUSE-Deep.” Astronomy & Astrophysics, vol. 659, 183, EDP Sciences,
2022, doi:10.1051/0004-6361/202141900.
short: J. Kerutt, L. Wisotzki, A. Verhamme, K.B. Schmidt, F. Leclercq, E.C. Herenz,
T. Urrutia, T. Garel, T. Hashimoto, M. Maseda, J.J. Matthee, H. Kusakabe, J. Schaye,
J. Richard, B. Guiderdoni, V. Mauerhofer, T. Nanayakkara, E. Vitte, Astronomy
& Astrophysics 659 (2022).
date_created: 2022-07-06T08:17:27Z
date_published: 2022-03-25T00:00:00Z
date_updated: 2022-07-19T09:47:16Z
day: '25'
doi: 10.1051/0004-6361/202141900
extern: '1'
external_id:
arxiv:
- '2202.06642'
intvolume: ' 659'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology:
observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2202.06642
month: '03'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 659
year: '2022'
...
---
_id: '11585'
abstract:
- lang: eng
text: "Observations show that star-forming galaxies reside on a tight three-dimensional
plane between mass, gas-phase metallicity and star formation rate (SFR), which
can be explained by the interplay between metal-poor gas inflows, SFR and outflows.
However, different metals are released on different time-scales, which may affect
the slope of this relation. Here, we use central, star-forming galaxies with Mstar
= 109.0−10.5 M\f from the EAGLE hydrodynamical simulation to examine three-dimensional
relations between mass, SFR and chemical enrichment using absolute and relative
C, N, O and Fe abundances. We show that the scatter is smaller when gas-phase
α-enhancement is used rather than metallicity. A similar plane also exists for
stellar α-enhancement, implying that present-day specific SFRs are correlated
with long time-scale star formation histories. Between z = 0 and 1, the α-enhancement
plane is even more insensitive to redshift than the plane using metallicity. However,
it evolves at z > 1 due to lagging iron yields. At fixed mass, galaxies with higher
SFRs have star formation histories shifted toward late times, are more α-enhanced
and this α-enhancement increases with redshift as observed. These findings suggest
that relations between physical properties inferred from observations may be affected
by systematic variations in α-enhancements."
acknowledgement: We thank the anonymous referee for their constructive comments. JM
acknowledges the support of a Huygens PhD fellowship from Leiden University. We
thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge
the use of the Topcat software (Taylor 2013) for assisting in rapid exploration
of multi-dimensional datasets and the use of Python and its numpy, matplotlib and
pandas packages.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
citation:
ama: Matthee JJ. Differences in galaxy colours are not just about the mass. Nature
Astronomy. 2021;5:984-985. doi:10.1038/s41550-021-01415-y
apa: Matthee, J. J. (2021). Differences in galaxy colours are not just about the
mass. Nature Astronomy. Springer Nature. https://doi.org/10.1038/s41550-021-01415-y
chicago: Matthee, Jorryt J. “Differences in Galaxy Colours Are Not Just about the
Mass.” Nature Astronomy. Springer Nature, 2021. https://doi.org/10.1038/s41550-021-01415-y.
ieee: J. J. Matthee, “Differences in galaxy colours are not just about the mass,”
Nature Astronomy, vol. 5. Springer Nature, pp. 984–985, 2021.
ista: Matthee JJ. 2021. Differences in galaxy colours are not just about the mass.
Nature Astronomy. 5, 984–985.
mla: Matthee, Jorryt J. “Differences in Galaxy Colours Are Not Just about the Mass.”
Nature Astronomy, vol. 5, Springer Nature, 2021, pp. 984–85, doi:10.1038/s41550-021-01415-y.
short: J.J. Matthee, Nature Astronomy 5 (2021) 984–985.
date_created: 2022-07-14T13:13:39Z
date_published: 2021-07-05T00:00:00Z
date_updated: 2024-10-14T11:38:08Z
day: '05'
doi: 10.1038/s41550-021-01415-y
extern: '1'
external_id:
arxiv:
- '1802.06786'
intvolume: ' 5'
keyword:
- Astronomy and Astrophysics
- galaxies
- formation - galaxies
- evolution - galaxies
- star formation - galaxies
- abundances
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1802.06786
month: '07'
oa: 1
oa_version: Preprint
page: 984-985
publication: Nature Astronomy
publication_identifier:
eissn:
- 2397-3366
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
scopus_import: '1'
status: public
title: Differences in galaxy colours are not just about the mass
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 5
year: '2021'
...
---
_id: '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: '11499'
abstract:
- lang: eng
text: Deep optical spectroscopic surveys of galaxies provide a unique opportunity
to investigate rest-frame ultra-violet (UV) emission line properties of galaxies
at z ∼ 2 − 4.5. Here we combine VLT/MUSE Guaranteed Time Observations of the Hubble
Deep Field South, Ultra Deep Field, COSMOS, and several quasar fields with other
publicly available data from VLT/VIMOS and VLT/FORS2 to construct a catalogue
of He II λ1640 emitters at z ≳ 2. The deepest areas of our MUSE pointings reach
a 3σ line flux limit of 3.1 × 10−19 erg s−1 cm−2. After discarding broad-line
active galactic nuclei, we find 13 He II λ1640 detections from MUSE with a median
MUV = −20.1 and 21 tentative He II λ1640 detections from other public surveys.
Excluding Lyα, all except two galaxies in our sample show at least one other rest-UV
emission line, with C III] λ1907, λ1909 being the most prominent. We use multi-wavelength
data available in the Hubble legacy fields to derive basic galaxy properties of
our sample through spectral energy distribution fitting techniques. Taking advantage
of the high-quality spectra obtained by MUSE (∼10 − 30 h of exposure time per
pointing), we use photo-ionisation models to study the rest-UV emission line diagnostics
of the He II λ1640 emitters. Line ratios of our sample can be reproduced by moderately
sub-solar photo-ionisation models, however, we find that including effects of
binary stars lead to degeneracies in most free parameters. Even after considering
extra ionising photons produced by extreme sub-solar metallicity binary stellar
models, photo-ionisation models are unable to reproduce rest-frame He II λ1640
equivalent widths (∼0.2 − 10 Å), thus additional mechanisms are necessary in models
to match the observed He II λ1640 properties.
acknowledgement: 'The authors wish to thank the referee for constructive comments
that improved the paper substantially. We thank the BPASS team for making the stellar
population models available. We thank Elizabeth Stanway, Claus Leitherer, Daniel
Schaerer, Jorick Vink, and Nell Byler for insightful discussions. We thank the Lorentz
Centre and the scientific organizers of the Characterizing galaxies with spectroscopy
with a view for JWST workshop held at the Lorentz Centre in 2017 October, which
promoted useful discussions in the wider community. TN, JB, and RB acknowledges
the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) top grant TOP1.16.057.
AF acknowledges support from the ERC via an Advanced Grant under grant agreement
no. 339659-MUSICOS. JB acknowledges support by Fundação para a Ciência e a Tecnologia
(FCT) through national funds (UID/FIS/04434/2013) and Investigador FCT contract
IF/01654/2014/CP1215/CT0003, and by FEDER through COMPETE2020 (POCI-01-0145-FEDER-007672).
JR acknowledges support from the ERC Starting grant 336736 (CALENDS). This research
made use of astropy (http://www.astropy.org) a community-developed core Python package
for Astronomy (Astropy Collaboration 2013, 2018) and pandas (McKinney 2010). Figures
were generated using matplotlib (Hunter 2007) and seaborn (https://seaborn.pydata.org).
Facilities: VLT (MUSE).'
article_number: A89
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
- first_name: Jarle
full_name: Brinchmann, Jarle
last_name: Brinchmann
- first_name: Leindert
full_name: Boogaard, Leindert
last_name: Boogaard
- first_name: Rychard
full_name: Bouwens, Rychard
last_name: Bouwens
- first_name: Sebastiano
full_name: Cantalupo, Sebastiano
last_name: Cantalupo
- first_name: Anna
full_name: Feltre, Anna
last_name: Feltre
- first_name: Wolfram
full_name: Kollatschny, Wolfram
last_name: Kollatschny
- first_name: Raffaella Anna
full_name: Marino, Raffaella Anna
last_name: Marino
- first_name: Michael
full_name: Maseda, Michael
last_name: Maseda
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Mieke
full_name: Paalvast, Mieke
last_name: Paalvast
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Anne
full_name: Verhamme, Anne
last_name: Verhamme
citation:
ama: Nanayakkara T, Brinchmann J, Boogaard L, et al. Exploring He II λ1640 emission
line properties at z ∼2−4. Astronomy & Astrophysics. 2019;648. doi:10.1051/0004-6361/201834565
apa: Nanayakkara, T., Brinchmann, J., Boogaard, L., Bouwens, R., Cantalupo, S.,
Feltre, A., … Verhamme, A. (2019). Exploring He II λ1640 emission line properties
at z ∼2−4. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201834565
chicago: Nanayakkara, Themiya, Jarle Brinchmann, Leindert Boogaard, Rychard Bouwens,
Sebastiano Cantalupo, Anna Feltre, Wolfram Kollatschny, et al. “Exploring He II Λ1640
Emission Line Properties at z ∼2−4.” Astronomy & Astrophysics. EDP
Sciences, 2019. https://doi.org/10.1051/0004-6361/201834565.
ieee: T. Nanayakkara et al., “Exploring He II λ1640 emission line properties
at z ∼2−4,” Astronomy & Astrophysics, vol. 648. EDP Sciences, 2019.
ista: Nanayakkara T, Brinchmann J, Boogaard L, Bouwens R, Cantalupo S, Feltre A,
Kollatschny W, Marino RA, Maseda M, Matthee JJ, Paalvast M, Richard J, Verhamme
A. 2019. Exploring He II λ1640 emission line properties at z ∼2−4. Astronomy &
Astrophysics. 648, A89.
mla: Nanayakkara, Themiya, et al. “Exploring He II Λ1640 Emission Line Properties
at z ∼2−4.” Astronomy & Astrophysics, vol. 648, A89, EDP Sciences,
2019, doi:10.1051/0004-6361/201834565.
short: T. Nanayakkara, J. Brinchmann, L. Boogaard, R. Bouwens, S. Cantalupo, A.
Feltre, W. Kollatschny, R.A. Marino, M. Maseda, J.J. Matthee, M. Paalvast, J.
Richard, A. Verhamme, Astronomy & Astrophysics 648 (2019).
date_created: 2022-07-06T09:07:06Z
date_published: 2019-04-16T00:00:00Z
date_updated: 2022-07-19T09:36:08Z
day: '16'
doi: 10.1051/0004-6361/201834565
extern: '1'
external_id:
arxiv:
- '1902.05960'
intvolume: ' 648'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: ISM / galaxies: star formation / galaxies: evolution / galaxies: high-redshift'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1902.05960
month: '04'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
related_material:
link:
- relation: erratum
url: https://doi.org/10.1051/0004-6361/201834565e
scopus_import: '1'
status: public
title: Exploring He II λ1640 emission line properties at z ∼2−4
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 648
year: '2019'
...
---
_id: '11507'
abstract:
- lang: eng
text: 'Lyman-α (Lyα) is intrinsically the brightest line emitted from active galaxies.
While it originates from many physical processes, for star-forming galaxies the
intrinsic Lyα luminosity is a direct tracer of the Lyman-continuum (LyC) radiation
produced by the most massive O- and early-type B-stars (M⋆ ≳ 10 M⊙) with lifetimes
of a few Myrs. As such, Lyα luminosity should be an excellent instantaneous star
formation rate (SFR) indicator. However, its resonant nature and susceptibility
to dust as a rest-frame UV photon makes Lyα very hard to interpret due to the
uncertain Lyα escape fraction, fesc, Lyα. Here we explore results from the CAlibrating
LYMan-α with Hα (CALYMHA) survey at z = 2.2, follow-up of Lyα emitters (LAEs)
at z = 2.2 − 2.6 and a z ∼ 0−0.3 compilation of LAEs to directly measure fesc, Lyα
with Hα. We derive a simple empirical relation that robustly retrieves fesc, Lyα
as a function of Lyα rest-frame EW (EW0): fesc,Lyα = 0.0048 EW0[Å] ± 0.05 and
we show that it constrains a well-defined anti-correlation between ionisation
efficiency (ξion) and dust extinction in LAEs. Observed Lyα luminosities and EW0
are easy measurable quantities at high redshift, thus making our relation a practical
tool to estimate intrinsic Lyα and LyC luminosities under well controlled and
simple assumptions. Our results allow observed Lyα luminosities to be used to
compute SFRs for LAEs at z ∼ 0−2.6 within ±0.2 dex of the Hα dust corrected SFRs.
We apply our empirical SFR(Lyα,EW0) calibration to several sources at z ≥ 2.6
to find that star-forming LAEs have SFRs typically ranging from 0.1 to 20 M⊙ yr−1
and that our calibration might be even applicable for the most luminous LAEs within
the epoch of re-ionisation. Our results imply high ionisation efficiencies (log10[ξion/Hz erg−1]
= 25.4−25.6) and low dust content in LAEs across cosmic time, and will be easily
tested with future observations with JWST which can obtain Hα and Hβ measurements
for high-redshift LAEs.'
acknowledgement: We thank the anonymous referees for multiple comments and suggestions
which have improved the manuscript. JM acknowledges the support of a Huygens PhD
fellowship from Leiden University. We have benefited greatly from the publicly available
programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt et al. 2011;
Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration
2013) packages, and the TOPCAT analysis program (Taylor 2013). The results and samples
of LAEs used for this paper are publicly available (see e.g. Sobral et al. 2017,
2018a) and we also provide the toy model used as a PYTHON script.
article_number: A157
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
citation:
ama: 'Sobral D, Matthee JJ. Predicting Lyα escape fractions with a simple observable:
Lyα in emission as an empirically calibrated star formation rate indicator. 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: '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'
...