---
_id: '14852'
abstract:
- lang: eng
text: The physical conditions giving rise to high escape fractions of ionizing radiation
(LyC fesc) in star-forming galaxies – most likely protagonists of cosmic reionization
– are not yet fully understood. Using the VLT/MUSE observations of ∼1400 Ly α
emitters at 2.9 < z < 6.7, we compare stacked rest-frame UV spectra
of candidates for LyC leakers and non-leakers selected based on their Ly α profiles.
We find that the stacks of potential LyC leakers, i.e. galaxies with narrow, symmetric
Ly α profiles with small peak separation, generally show (i) strong nebular O iii]λ1666,
[Si iii]λ1883, and [C iii]λ1907 +C iii]λ1909 emission, indicating a high-ionization
state of the interstellar medium (ISM); (ii) high equivalent widths of He iiλ1640
(∼1 − 3 Å), suggesting the presence of hard ionizing radiation fields; (iii) Si ii*λ1533
emission, revealing substantial amounts of neutral hydrogen off the line of sight;
(iv) high C ivλλ1548,1550 to [C iii]λ1907 +C iii]λ1909 ratios (C iv/C iii] ≳0.75)
, signalling the presence of low column density channels in the ISM. In contrast,
the stacks with broad, asymmetric Ly α profiles with large peak separation show
weak nebular emission lines, low He iiλ1640 equivalent widths (≲1 Å), and low
C iv/C iii] (≲0.25), implying low-ionization states and high-neutral hydrogen
column densities. Our results suggest that C iv/C iii] might be sensitive to the
physical conditions that govern LyC photon escape, providing a promising tool
for identification of ionizing sources among star-forming galaxies in the epoch
of reionization.
acknowledgement: 'We thank the anonymous referee for the constructive feedback that
helped to improve the manuscript. We thank Michael Maseda, Daniel Schaerer, Charlotte
Simmonds, and Rashmi Gottumukkala for useful comments and productive discussions.
We also thank the organizers and participants of the 24th MUSE Science Busy Week
in Leiden. IGK acknowledges an Excellence Master Fellowship granted by the Faculty
of Science of the University of Geneva. This work has received funding from the
Swiss State Secretariat for Education, Research and Innovation (SERI) under contract
number MB22.00072, as well as from the Swiss National Science Foundation (SNSF)
through project grant number 200020_207349 and SNSF Professorship grant number 190079.
The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation
under grant number 140. This paper is based on observations collected at the European
Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes
094.A-0289(B), 095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 094.A-0205, 095.A-0240,
096.A-0090, 097.A-0160, and 098.A-0017. We made extensive use of several open-source
software packages and we are thankful to the respective authors for sharing their
work: NUMPY (Harris et al. 2020), ASTROPY (Astropy Collaboration 2022), MATPLOTLIB
(Hunter 2007), IPYTHON (Perez & Granger 2007), and TOPCAT (Taylor 2005).'
article_processing_charge: Yes (in subscription journal)
article_type: original
arxiv: 1
author:
- first_name: Ivan
full_name: Kramarenko, Ivan
id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4
last_name: Kramarenko
- first_name: J
full_name: Kerutt, J
last_name: Kerutt
- first_name: A
full_name: Verhamme, A
last_name: Verhamme
- first_name: P A
full_name: Oesch, P A
last_name: Oesch
- first_name: L
full_name: Barrufet, L
last_name: Barrufet
- 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: I
full_name: Goovaerts, I
last_name: Goovaerts
- first_name: T T
full_name: Thai, T T
last_name: Thai
citation:
ama: Kramarenko I, Kerutt J, Verhamme A, et al. Linking UV spectral properties of
MUSE Ly α emitters at z ≳ 3 to Lyman continuum escape. Monthly Notices
of the Royal Astronomical Society. 2024;527(4):9853-9871. doi:10.1093/mnras/stad3853
apa: Kramarenko, I., Kerutt, J., Verhamme, A., Oesch, P. A., Barrufet, L., Matthee,
J. J., … Thai, T. T. (2024). Linking UV spectral properties of MUSE Ly α emitters
at z ≳ 3 to Lyman continuum escape. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stad3853
chicago: Kramarenko, Ivan, J Kerutt, A Verhamme, P A Oesch, L Barrufet, Jorryt J
Matthee, H Kusakabe, I Goovaerts, and T T Thai. “Linking UV Spectral Properties
of MUSE Ly α Emitters at z ≳ 3 to Lyman Continuum Escape.” Monthly Notices
of the Royal Astronomical Society. Oxford University Press, 2024. https://doi.org/10.1093/mnras/stad3853.
ieee: I. Kramarenko et al., “Linking UV spectral properties of MUSE Ly α
emitters at z ≳ 3 to Lyman continuum escape,” Monthly Notices of the
Royal Astronomical Society, vol. 527, no. 4. Oxford University Press, pp.
9853–9871, 2024.
ista: Kramarenko I, Kerutt J, Verhamme A, Oesch PA, Barrufet L, Matthee JJ, Kusakabe
H, Goovaerts I, Thai TT. 2024. Linking UV spectral properties of MUSE Ly α emitters
at z ≳ 3 to Lyman continuum escape. Monthly Notices of the Royal Astronomical
Society. 527(4), 9853–9871.
mla: Kramarenko, Ivan, et al. “Linking UV Spectral Properties of MUSE Ly α Emitters
at z ≳ 3 to Lyman Continuum Escape.” Monthly Notices of the Royal Astronomical
Society, vol. 527, no. 4, Oxford University Press, 2024, pp. 9853–71, doi:10.1093/mnras/stad3853.
short: I. Kramarenko, J. Kerutt, A. Verhamme, P.A. Oesch, L. Barrufet, J.J. Matthee,
H. Kusakabe, I. Goovaerts, T.T. Thai, Monthly Notices of the Royal Astronomical
Society 527 (2024) 9853–9871.
date_created: 2024-01-22T08:22:17Z
date_published: 2024-02-01T00:00:00Z
date_updated: 2024-01-23T12:33:50Z
day: '01'
ddc:
- '520'
department:
- _id: GradSch
- _id: JoMa
doi: 10.1093/mnras/stad3853
external_id:
arxiv:
- '2305.07044'
file:
- access_level: open_access
checksum: 9d02df4035c4951cf63dee0db1e462e9
content_type: application/pdf
creator: dernst
date_created: 2024-01-23T12:30:45Z
date_updated: 2024-01-23T12:30:45Z
file_id: '14879'
file_name: 2024_MNAstronomSoc_Kramarenko.pdf
file_size: 4521738
relation: main_file
success: 1
file_date_updated: 2024-01-23T12:30:45Z
has_accepted_license: '1'
intvolume: ' 527'
issue: '4'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
license: https://creativecommons.org/licenses/by/4.0/
month: '02'
oa: 1
oa_version: Published Version
page: 9853-9871
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'
status: public
title: Linking UV spectral properties of MUSE Ly α emitters at z ≳ 3 to Lyman
continuum escape
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 527
year: '2024'
...
---
_id: '14104'
abstract:
- lang: eng
text: 'Thorne–Żytkow objects (TŻO) are potential end products of the merger of a
neutron star with a non-degenerate star. In this work, we have computed the first
grid of evolutionary models of TŻOs with the MESA stellar evolution code. With
these models, we predict several observational properties of TŻOs, including their
surface temperatures and luminosities, pulsation periods, and nucleosynthetic
products. We expand the range of possible TŻO solutions to cover 3.45≲log(Teff/K)≲3.65
and 4.85≲log(L/L⊙)≲5.5. Due to the much higher densities our TŻOs reach compared
to previous models, if TŻOs form we expect them to be stable over a larger mass
range than previously predicted, without exhibiting a gap in their mass distribution.
Using the GYRE stellar pulsation code we show that TŻOs should have fundamental
pulsation periods of 1000–2000 d, and period ratios of ≈0.2–0.3. Models computed
with a large 399 isotope fully coupled nuclear network show a nucleosynthetic
signal that is different to previously predicted. We propose a new nucleosynthetic
signal to determine a star’s status as a TŻO: the isotopologues 44TiO2 and 44TiO,
which will have a shift in their spectral features as compared to stable titanium-containing
molecules. We find that in the local Universe (∼SMC metallicities and above) TŻOs
show little heavy metal enrichment, potentially explaining the difficulty in finding
TŻOs to-date.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: R
full_name: Farmer, R
last_name: Farmer
- first_name: M
full_name: Renzo, M
last_name: Renzo
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: E
full_name: Bellinger, E
last_name: Bellinger
- first_name: S
full_name: Justham, S
last_name: Justham
- first_name: S E
full_name: de Mink, S E
last_name: de Mink
citation:
ama: Farmer R, Renzo M, Götberg YLL, Bellinger E, Justham S, de Mink SE. Observational
predictions for Thorne–Żytkow objects. Monthly Notices of the Royal Astronomical
Society. 2023;524(2):1692-1709. doi:10.1093/mnras/stad1977
apa: Farmer, R., Renzo, M., Götberg, Y. L. L., Bellinger, E., Justham, S., &
de Mink, S. E. (2023). Observational predictions for Thorne–Żytkow objects. Monthly
Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stad1977
chicago: Farmer, R, M Renzo, Ylva Louise Linsdotter Götberg, E Bellinger, S Justham,
and S E de Mink. “Observational Predictions for Thorne–Żytkow Objects.” Monthly
Notices of the Royal Astronomical Society. Oxford University Press, 2023.
https://doi.org/10.1093/mnras/stad1977.
ieee: R. Farmer, M. Renzo, Y. L. L. Götberg, E. Bellinger, S. Justham, and S. E.
de Mink, “Observational predictions for Thorne–Żytkow objects,” Monthly Notices
of the Royal Astronomical Society, vol. 524, no. 2. Oxford University Press,
pp. 1692–1709, 2023.
ista: Farmer R, Renzo M, Götberg YLL, Bellinger E, Justham S, de Mink SE. 2023.
Observational predictions for Thorne–Żytkow objects. Monthly Notices of the Royal
Astronomical Society. 524(2), 1692–1709.
mla: Farmer, R., et al. “Observational Predictions for Thorne–Żytkow Objects.” Monthly
Notices of the Royal Astronomical Society, vol. 524, no. 2, Oxford University
Press, 2023, pp. 1692–709, doi:10.1093/mnras/stad1977.
short: R. Farmer, M. Renzo, Y.L.L. Götberg, E. Bellinger, S. Justham, S.E. de Mink,
Monthly Notices of the Royal Astronomical Society 524 (2023) 1692–1709.
date_created: 2023-08-21T10:13:56Z
date_published: 2023-09-01T00:00:00Z
date_updated: 2023-08-21T12:12:48Z
day: '01'
doi: 10.1093/mnras/stad1977
extern: '1'
external_id:
arxiv:
- '2305.07337'
intvolume: ' 524'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2305.07337
month: '09'
oa: 1
oa_version: Preprint
page: 1692-1709
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: Observational predictions for Thorne–Żytkow objects
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 524
year: '2023'
...
---
_id: '13452'
abstract:
- lang: eng
text: Magnetic fields can drastically change predictions of evolutionary models
of massive stars via mass-loss quenching, magnetic braking, and efficient angular
momentum transport, which we aim to quantify in this work. We use the MESA software
instrument to compute an extensive main-sequence grid of stellar structure and
evolution models, as well as isochrones, accounting for the effects attributed
to a surface fossil magnetic field. The grid is densely populated in initial mass
(3–60 M⊙), surface equatorial magnetic field strength (0–50 kG), and metallicity
(representative of the Solar neighbourhood and the Magellanic Clouds). We use
two magnetic braking and two chemical mixing schemes and compare the model predictions
for slowly rotating, nitrogen-enriched (‘Group 2’) stars with observations in
the Large Magellanic Cloud. We quantify a range of initial field strengths that
allow for producing Group 2 stars and find that typical values (up to a few kG)
lead to solutions. Between the subgrids, we find notable departures in surface
abundances and evolutionary paths. In our magnetic models, chemical mixing is
always less efficient compared to non-magnetic models due to the rapid spin-down.
We identify that quasi-chemically homogeneous main sequence evolution by efficient
mixing could be prevented by fossil magnetic fields. We recommend comparing this
grid of evolutionary models with spectropolarimetric and spectroscopic observations
with the goals of (i) revisiting the derived stellar parameters of known magnetic
stars, and (ii) observationally constraining the uncertain magnetic braking and
chemical mixing schemes.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Z
full_name: Keszthelyi, Z
last_name: Keszthelyi
- first_name: A
full_name: de Koter, A
last_name: de Koter
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: G
full_name: Meynet, G
last_name: Meynet
- first_name: S A
full_name: Brands, S A
last_name: Brands
- first_name: V
full_name: Petit, V
last_name: Petit
- first_name: M
full_name: Carrington, M
last_name: Carrington
- first_name: A
full_name: David-Uraz, A
last_name: David-Uraz
- first_name: S T
full_name: Geen, S T
last_name: Geen
- first_name: C
full_name: Georgy, C
last_name: Georgy
- first_name: R
full_name: Hirschi, R
last_name: Hirschi
- first_name: J
full_name: Puls, J
last_name: Puls
- first_name: K J
full_name: Ramalatswa, K J
last_name: Ramalatswa
- first_name: M E
full_name: Shultz, M E
last_name: Shultz
- first_name: A
full_name: ud-Doula, A
last_name: ud-Doula
citation:
ama: 'Keszthelyi Z, de Koter A, Götberg YLL, et al. The effects of surface fossil
magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC,
and SMC metallicities. Monthly Notices of the Royal Astronomical Society.
2022;517(2):2028-2055. doi:10.1093/mnras/stac2598'
apa: 'Keszthelyi, Z., de Koter, A., Götberg, Y. L. L., Meynet, G., Brands, S. A.,
Petit, V., … ud-Doula, A. (2022). The effects of surface fossil magnetic fields
on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities.
Monthly Notices of the Royal Astronomical Society. Oxford University Press.
https://doi.org/10.1093/mnras/stac2598'
chicago: 'Keszthelyi, Z, A de Koter, Ylva Louise Linsdotter Götberg, G Meynet, S
A Brands, V Petit, M Carrington, et al. “The Effects of Surface Fossil Magnetic
Fields on Massive Star Evolution: IV. Grids of Models at Solar, LMC, and SMC Metallicities.”
Monthly Notices of the Royal Astronomical Society. Oxford University Press,
2022. https://doi.org/10.1093/mnras/stac2598.'
ieee: 'Z. Keszthelyi et al., “The effects of surface fossil magnetic fields
on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities,”
Monthly Notices of the Royal Astronomical Society, vol. 517, no. 2. Oxford
University Press, pp. 2028–2055, 2022.'
ista: 'Keszthelyi Z, de Koter A, Götberg YLL, Meynet G, Brands SA, Petit V, Carrington
M, David-Uraz A, Geen ST, Georgy C, Hirschi R, Puls J, Ramalatswa KJ, Shultz ME,
ud-Doula A. 2022. The effects of surface fossil magnetic fields on massive star
evolution: IV. Grids of models at Solar, LMC, and SMC metallicities. Monthly Notices
of the Royal Astronomical Society. 517(2), 2028–2055.'
mla: 'Keszthelyi, Z., et al. “The Effects of Surface Fossil Magnetic Fields on Massive
Star Evolution: IV. Grids of Models at Solar, LMC, and SMC Metallicities.” Monthly
Notices of the Royal Astronomical Society, vol. 517, no. 2, Oxford University
Press, 2022, pp. 2028–55, doi:10.1093/mnras/stac2598.'
short: Z. Keszthelyi, A. de Koter, Y.L.L. Götberg, G. Meynet, S.A. Brands, V. Petit,
M. Carrington, A. David-Uraz, S.T. Geen, C. Georgy, R. Hirschi, J. Puls, K.J.
Ramalatswa, M.E. Shultz, A. ud-Doula, Monthly Notices of the Royal Astronomical
Society 517 (2022) 2028–2055.
date_created: 2023-08-03T10:10:37Z
date_published: 2022-12-01T00:00:00Z
date_updated: 2023-08-21T12:02:17Z
day: '01'
doi: 10.1093/mnras/stac2598
extern: '1'
external_id:
arxiv:
- '2209.06350'
intvolume: ' 517'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2209.06350
month: '12'
oa: 1
oa_version: Preprint
page: 2028-2055
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 effects of surface fossil magnetic fields on massive star evolution: IV.
Grids of models at Solar, LMC, and SMC metallicities'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 517
year: '2022'
...
---
_id: '14098'
abstract:
- lang: eng
text: Magnetic fields can drastically change predictions of evolutionary models
of massive stars via mass-loss quenching, magnetic braking, and efficient angular
momentum transport, which we aim to quantify in this work. We use the MESA software
instrument to compute an extensive main-sequence grid of stellar structure and
evolution models, as well as isochrones, accounting for the effects attributed
to a surface fossil magnetic field. The grid is densely populated in initial mass
(3–60 M⊙), surface equatorial magnetic field strength (0–50 kG), and metallicity
(representative of the Solar neighbourhood and the Magellanic Clouds). We use
two magnetic braking and two chemical mixing schemes and compare the model predictions
for slowly rotating, nitrogen-enriched (‘Group 2’) stars with observations in
the Large Magellanic Cloud. We quantify a range of initial field strengths that
allow for producing Group 2 stars and find that typical values (up to a few kG)
lead to solutions. Between the subgrids, we find notable departures in surface
abundances and evolutionary paths. In our magnetic models, chemical mixing is
always less efficient compared to non-magnetic models due to the rapid spin-down.
We identify that quasi-chemically homogeneous main sequence evolution by efficient
mixing could be prevented by fossil magnetic fields. We recommend comparing this
grid of evolutionary models with spectropolarimetric and spectroscopic observations
with the goals of (i) revisiting the derived stellar parameters of known magnetic
stars, and (ii) observationally constraining the uncertain magnetic braking and
chemical mixing schemes.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Z.
full_name: Keszthelyi, Z.
last_name: Keszthelyi
- first_name: A. de
full_name: Koter, A. de
last_name: Koter
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: G.
full_name: Meynet, G.
last_name: Meynet
- first_name: S. A.
full_name: Brands, S. A.
last_name: Brands
- first_name: V.
full_name: Petit, V.
last_name: Petit
- first_name: M.
full_name: Carrington, M.
last_name: Carrington
- first_name: A. David-Uraz
full_name: A. David-Uraz, A. David-Uraz
last_name: A. David-Uraz
- first_name: S. T.
full_name: Geen, S. T.
last_name: Geen
- first_name: C.
full_name: Georgy, C.
last_name: Georgy
- first_name: R.
full_name: Hirschi, R.
last_name: Hirschi
- first_name: J.
full_name: Puls, J.
last_name: Puls
- first_name: K. J.
full_name: Ramalatswa, K. J.
last_name: Ramalatswa
- first_name: M. E.
full_name: Shultz, M. E.
last_name: Shultz
- first_name: A. ud-Doula
full_name: A. ud-Doula, A. ud-Doula
last_name: A. ud-Doula
citation:
ama: 'Keszthelyi Z, Koter A de, Götberg YLL, et al. The effects of surface fossil
magnetic fields on massive star evolution: IV. Grids of models at solar, LMC,
and SMC metallicities. Monthly Notices of the Royal Astronomical Society.
2022;517(2):2028-2055. doi:10.1093/mnras/stac2598'
apa: 'Keszthelyi, Z., Koter, A. de, Götberg, Y. L. L., Meynet, G., Brands, S. A.,
Petit, V., … A. ud-Doula, A. ud-Doula. (2022). The effects of surface fossil magnetic
fields on massive star evolution: IV. Grids of models at solar, LMC, and SMC metallicities.
Monthly Notices of the Royal Astronomical Society. Oxford Academic. https://doi.org/10.1093/mnras/stac2598'
chicago: 'Keszthelyi, Z., A. de Koter, Ylva Louise Linsdotter Götberg, G. Meynet,
S. A. Brands, V. Petit, M. Carrington, et al. “The Effects of Surface Fossil Magnetic
Fields on Massive Star Evolution: IV. Grids of Models at Solar, LMC, and SMC Metallicities.”
Monthly Notices of the Royal Astronomical Society. Oxford Academic, 2022.
https://doi.org/10.1093/mnras/stac2598.'
ieee: 'Z. Keszthelyi et al., “The effects of surface fossil magnetic fields
on massive star evolution: IV. Grids of models at solar, LMC, and SMC metallicities,”
Monthly Notices of the Royal Astronomical Society, vol. 517, no. 2. Oxford
Academic, pp. 2028–2055, 2022.'
ista: 'Keszthelyi Z, Koter A de, Götberg YLL, Meynet G, Brands SA, Petit V, Carrington
M, A. David-Uraz AD-U, Geen ST, Georgy C, Hirschi R, Puls J, Ramalatswa KJ, Shultz
ME, A. ud-Doula A ud-Doula. 2022. The effects of surface fossil magnetic fields
on massive star evolution: IV. Grids of models at solar, LMC, and SMC metallicities.
Monthly Notices of the Royal Astronomical Society. 517(2), 2028–2055.'
mla: 'Keszthelyi, Z., et al. “The Effects of Surface Fossil Magnetic Fields on Massive
Star Evolution: IV. Grids of Models at Solar, LMC, and SMC Metallicities.” Monthly
Notices of the Royal Astronomical Society, vol. 517, no. 2, Oxford Academic,
2022, pp. 2028–55, doi:10.1093/mnras/stac2598.'
short: Z. Keszthelyi, A. de Koter, Y.L.L. Götberg, G. Meynet, S.A. Brands, V. Petit,
M. Carrington, A.D.-U. A. David-Uraz, S.T. Geen, C. Georgy, R. Hirschi, J. Puls,
K.J. Ramalatswa, M.E. Shultz, A. ud-Doula A. ud-Doula, Monthly Notices of the
Royal Astronomical Society 517 (2022) 2028–2055.
date_created: 2023-08-21T10:11:21Z
date_published: 2022-12-01T00:00:00Z
date_updated: 2023-08-22T13:18:34Z
day: '01'
doi: 10.1093/mnras/stac2598
extern: '1'
external_id:
arxiv:
- '2209.06350'
intvolume: ' 517'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/stac2598
month: '12'
oa: 1
oa_version: Published Version
page: 2028-2055
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford Academic
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The effects of surface fossil magnetic fields on massive star evolution: IV.
Grids of models at solar, LMC, and SMC metallicities'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 517
year: '2022'
...
---
_id: '11521'
abstract:
- lang: eng
text: 'The cosmic ionizing emissivity from star-forming galaxies has long been anchored
to UV luminosity functions. Here, we introduce an emissivity framework based on
Lyα emitters (LAEs), which naturally hones in on the subset of galaxies responsible
for the ionizing background due to the intimate connection between production
and escape of Lyα and LyC photons. Using constraints on the escape fractions of
bright LAEs (LLyα > 0.2L*) at z ≈ 2 obtained from resolved Lyα profiles, and arguing
for their redshift-invariance, we show that: (i) quasars and LAEs together reproduce
the relatively flat emissivity at z ≈ 2–6, which is non-trivial given the strong
evolution in both the star formation density and quasar number density at these
epochs and (ii) LAEs produce late and rapid reionization between z ≈ 6−9 under
plausible assumptions. Within this framework, the >10 × rise in the UV population-averaged
fesc between z ≈ 3–7 naturally arises due to the same phenomena that drive the
growing LAE fraction with redshift. Generally, a LAE dominated emissivity yields
a peak in the distribution of the ionizing budget with UV luminosity as reported
in latest simulations. Using our adopted parameters (fesc=50 per cent, ξion
= 1025.9 Hz erg−1 for half the bright LAEs), a highly ionizing minority of galaxies
with MUV < −17 accounts for the entire ionizing budget from star-forming galaxies.
Rapid flashes of LyC from such rare galaxies produce a ‘disco’ ionizing background.
We conclude proposing tests to further develop our suggested Lyα-anchored formalism.'
acknowledgement: We thank an anonymous referee for an encouraging and constructive
report that helped improving the quality of this work. We acknowledge illuminating
conversations with Xiaohan Wu, Chris Cain, Anna-Christina Eilers, Simon Lilly and
Ruari Mackenzie. RPN gratefully acknowledges an Ashford Fellowship granted by Harvard
University. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409.
PO acknowledges support from the Swiss National Science Foundation through the SNSF
Professorship grant 190079. GP acknowledges support from the Netherlands Research
School for Astronomy (NOVA). MH is fellow of the Knut and Alice Wallenberg Foundation.
DE is supported by the US National Science Foundation (NSF) through Astronomy &
Astrophysics grant AST-1909198. The Cosmic Dawn Center (DAWN) is funded by the Danish
National Research Foundation under grant No. 140. RA acknowledges support from Fondecyt
Regular Grant 1202007. ST is supported by the 2021 Research Fund 1.210134.01 of
UNIST (Ulsan National Institute of Science & Technology). MLl acknowledges support
from the ANID/Scholarship Program/Doctorado Nacional/2019-21191036. JC acknowledges
support from the Spanish Ministry of Science and Innovation, project PID2019-107408GB-C43
(ESTALLIDOS) and from Gobierno de Canarias through EU FEDER funding, project PID2020010050.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: Matthew
full_name: Hayes, Matthew
last_name: Hayes
- first_name: Dawn
full_name: Erb, Dawn
last_name: Erb
- first_name: Daniel
full_name: Schaerer, Daniel
last_name: Schaerer
- first_name: Ricardo
full_name: Amorín, Ricardo
last_name: Amorín
- first_name: Sandro
full_name: Tacchella, Sandro
last_name: Tacchella
- first_name: Ana Paulino-Afonso
full_name: Ana Paulino-Afonso, Ana Paulino-Afonso
last_name: Ana Paulino-Afonso
- first_name: Mario
full_name: Llerena, Mario
last_name: Llerena
- first_name: João
full_name: Calhau, João
last_name: Calhau
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
citation:
ama: 'Matthee JJ, Naidu RP, Pezzulli G, et al. (Re)Solving reionization with Lyα:
How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background.
Monthly Notices of the Royal Astronomical Society. 2022;512(4):5960-5977.
doi:10.1093/mnras/stac801'
apa: 'Matthee, J. J., Naidu, R. P., Pezzulli, G., Gronke, M., Sobral, D., Oesch,
P. A., … Röttgering, H. (2022). (Re)Solving reionization with Lyα: How bright
Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly
Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stac801'
chicago: 'Matthee, Jorryt J, Rohan P. Naidu, Gabriele Pezzulli, Max Gronke, David
Sobral, Pascal A. Oesch, Matthew Hayes, et al. “(Re)Solving Reionization with
Lyα: How Bright Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.”
Monthly Notices of the Royal Astronomical Society. Oxford University Press,
2022. https://doi.org/10.1093/mnras/stac801.'
ieee: 'J. J. Matthee et al., “(Re)Solving reionization with Lyα: How bright
Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background,” Monthly
Notices of the Royal Astronomical Society, vol. 512, no. 4. Oxford University
Press, pp. 5960–5977, 2022.'
ista: 'Matthee JJ, Naidu RP, Pezzulli G, Gronke M, Sobral D, Oesch PA, Hayes M,
Erb D, Schaerer D, Amorín R, Tacchella S, Ana Paulino-Afonso AP-A, Llerena M,
Calhau J, Röttgering H. 2022. (Re)Solving reionization with Lyα: How bright Lyα
emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly Notices
of the Royal Astronomical Society. 512(4), 5960–5977.'
mla: 'Matthee, Jorryt J., et al. “(Re)Solving Reionization with Lyα: How Bright
Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.” Monthly
Notices of the Royal Astronomical Society, vol. 512, no. 4, Oxford University
Press, 2022, pp. 5960–77, doi:10.1093/mnras/stac801.'
short: J.J. Matthee, R.P. Naidu, G. Pezzulli, M. Gronke, D. Sobral, P.A. Oesch,
M. Hayes, D. Erb, D. Schaerer, R. Amorín, S. Tacchella, A.P.-A. Ana Paulino-Afonso,
M. Llerena, J. Calhau, H. Röttgering, Monthly Notices of the Royal Astronomical
Society 512 (2022) 5960–5977.
date_created: 2022-07-07T09:21:30Z
date_published: 2022-06-01T00:00:00Z
date_updated: 2022-08-18T10:42:47Z
day: '01'
doi: 10.1093/mnras/stac801
extern: '1'
external_id:
arxiv:
- '2110.11967'
intvolume: ' 512'
issue: '4'
keyword:
- 'galaxies: high-redshift'
- intergalactic medium
- 'cosmology: observations'
- dark ages
- reionization
- first stars
- 'ultraviolet: galaxies'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2110.11967
month: '06'
oa: 1
oa_version: Preprint
page: 5960-5977
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: '(Re)Solving reionization with Lyα: How bright Lyα emitters account for the
z ≈ 2 − 8 cosmic ionizing background'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 512
year: '2022'
...
---
_id: '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: 2022-08-18T10:49:00Z
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: '11524'
abstract:
- lang: eng
text: We measure the evolution of the rest-frame UV luminosity function (LF) and
the stellar mass function (SMF) of Lyman-α (Ly α) emitters (LAEs) from z ∼ 2 to
z ∼ 6 by exploring ∼4000 LAEs from the SC4K sample. We find a correlation between
Ly α luminosity (LLy α) and rest-frame UV (MUV), with best fit MUV=−1.6+0.2−0.3log10(LLyα/ergs−1)+47+12−11
and a shallower relation between LLy α and stellar mass (M⋆), with best fit log10(M⋆/M⊙)=0.9+0.1−0.1log10(LLyα/ergs−1)−28+4.0−3.8.
An increasing LLy α cut predominantly lowers the number density of faint MUV and
low M⋆ LAEs. We estimate a proxy for the full UV LFs and SMFs of LAEs with simple
assumptions of the faint end slope. For the UV LF, we find a brightening of the
characteristic UV luminosity (M∗UV) with increasing redshift and a decrease of
the characteristic number density (Φ*). For the SMF, we measure a characteristic
stellar mass (M∗⋆/M⊙) increase with increasing redshift, and a Φ* decline. However,
if we apply a uniform luminosity cut of log10(LLyα/ergs−1)≥43.0, we find much
milder to no evolution in the UV and SMF of LAEs. The UV luminosity density (ρUV)
of the full sample of LAEs shows moderate evolution and the stellar mass density
(ρM) decreases, with both being always lower than the total ρUV and ρM of more
typical galaxies but slowly approaching them with increasing redshift. Overall,
our results indicate that both ρUV and ρM of LAEs slowly approach the measurements
of continuum-selected galaxies at z > 6, which suggests a key role of LAEs in
the epoch of reionization.
acknowledgement: This research made use of Astropy, a community developed core Python
package for Astronomy (Astropy Collaboration et al. 2013). topcat, a graphical tool
for manipulating tabular data, was also utilized in this analysis (Taylor 2005).
SG would like to thank Nastasha Wijers for the discussion on the column density
distribution in EAGLE. SC gratefully acknowledges support from Swiss National Science
Foundation grants PP00P2 163824 and PP00P2 190092, and from the European Research
Council (ERC) under the European Union’s Horizon 2020 research and innovation programme
grant agreement No 864361. GP acknowledges support from the Swiss National Science
Foundation (SNF) and from the Netherlands Research School for Astronomy (NOVA).
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: J
full_name: Butterworth, J
last_name: Butterworth
- first_name: A
full_name: Paulino-Afonso, A
last_name: Paulino-Afonso
- first_name: B
full_name: Ribeiro, B
last_name: Ribeiro
- first_name: E
full_name: da Cunha, E
last_name: da Cunha
- first_name: J
full_name: Calhau, J
last_name: Calhau
- first_name: A A
full_name: Khostovan, A A
last_name: Khostovan
- 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
full_name: Arrabal Haro, P
last_name: Arrabal Haro
citation:
ama: Santos S, Sobral D, Butterworth J, et al. The evolution of the UV luminosity
and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. Monthly
Notices of the Royal Astronomical Society. 2021;505(1):1117-1134. doi:10.1093/mnras/stab1218
apa: Santos, S., Sobral, D., Butterworth, J., Paulino-Afonso, A., Ribeiro, B., da Cunha,
E., … Arrabal Haro, P. (2021). The evolution of the UV luminosity and stellar
mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. Monthly Notices of
the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stab1218
chicago: Santos, S, D Sobral, J Butterworth, A Paulino-Afonso, B Ribeiro, E da Cunha,
J Calhau, A A Khostovan, Jorryt J Matthee, and P Arrabal Haro. “The Evolution
of the UV Luminosity and Stellar Mass Functions of Lyman-α Emitters from z ∼ 2
to z ∼ 6.” Monthly Notices of the Royal Astronomical Society. Oxford University
Press, 2021. https://doi.org/10.1093/mnras/stab1218.
ieee: S. Santos et al., “The evolution of the UV luminosity and stellar mass
functions of Lyman-α emitters from z ∼ 2 to z ∼ 6,” Monthly Notices of the
Royal Astronomical Society, vol. 505, no. 1. Oxford University Press, pp.
1117–1134, 2021.
ista: Santos S, Sobral D, Butterworth J, Paulino-Afonso A, Ribeiro B, da Cunha E,
Calhau J, Khostovan AA, Matthee JJ, Arrabal Haro P. 2021. The evolution of the
UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼
6. Monthly Notices of the Royal Astronomical Society. 505(1), 1117–1134.
mla: Santos, S., et al. “The Evolution of the UV Luminosity and Stellar Mass Functions
of Lyman-α Emitters from z ∼ 2 to z ∼ 6.” Monthly Notices of the Royal Astronomical
Society, vol. 505, no. 1, Oxford University Press, 2021, pp. 1117–34, doi:10.1093/mnras/stab1218.
short: S. Santos, D. Sobral, J. Butterworth, A. Paulino-Afonso, B. Ribeiro, E. da Cunha,
J. Calhau, A.A. Khostovan, J.J. Matthee, P. Arrabal Haro, Monthly Notices of the
Royal Astronomical Society 505 (2021) 1117–1134.
date_created: 2022-07-07T10:02:59Z
date_published: 2021-07-01T00:00:00Z
date_updated: 2022-08-18T10:51:47Z
day: '01'
doi: 10.1093/mnras/stab1218
extern: '1'
external_id:
arxiv:
- '2105.00007'
intvolume: ' 505'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: luminosity function'
- mass function
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2105.00007
month: '07'
oa: 1
oa_version: Preprint
page: 1117-1134
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 the UV luminosity and stellar mass functions of Lyman-α emitters
from z ∼ 2 to z ∼ 6
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 505
year: '2021'
...
---
_id: '11525'
abstract:
- lang: eng
text: The intensity of the Cosmic UV background (UVB), coming from all sources of
ionizing photons such as star-forming galaxies and quasars, determines the thermal
evolution and ionization state of the intergalactic medium (IGM) and is, therefore,
a critical ingredient for models of cosmic structure formation. Most of the previous
estimates are based on the comparison between observed and simulated Lyman-α forest.
We present the results of an independent method to constrain the product of the
UVB photoionization rate and the covering fraction of Lyman limit systems (LLSs)
by searching for the fluorescent Lyman-α emission produced by self-shielded clouds.
Because the expected surface brightness is well below current sensitivity limits
for direct imaging, we developed a new method based on 3D stacking of the IGM
around Lyman-α emitting galaxies (LAEs) between 2.9 < z < 6.6 using deep MUSE
observations. Combining our results with covering fractions of LLSs obtained from
mock cubes extracted from the EAGLE simulation, we obtain new and independent
constraints on the UVB at z > 3 that are consistent with previous measurements,
with a preference for relatively low UVB intensities at z = 3, and which suggest
a non-monotonic decrease of ΓH I with increasing redshift between 3 < z < 5. This
could suggest a possible tension between some UVB models and current observations
which however require deeper and wider observations in Lyman-α emission and absorption
to be confirmed. Assuming instead a value of UVB from current models, our results
constrain the covering fraction of LLSs at 3 < z < 4.5 to be less than 25 per cent
within 150 kpc from LAEs.
acknowledgement: This research made use of Astropy, a community developed core Python
package for Astronomy (Astropy Collaboration et al. 2013). topcat, a graphical tool
for manipulating tabular data, was also utilized in this analysis (Taylor 2005).
SG would like to thank Nastasha Wijers for the discussion on the column density
distribution in EAGLE. SC gratefully acknowledges support from Swiss National Science
Foundation grants PP00P2 163824 and PP00P2 190092, and from the European Research
Council (ERC) under the European Union’s Horizon 2020 research and innovation programme
grant agreement No 864361. GP acknowledges support from the Swiss National Science
Foundation (SNF) and from the Netherlands Research School for Astronomy (NOVA).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Sofia G
full_name: Gallego, Sofia G
last_name: Gallego
- first_name: Sebastiano
full_name: Cantalupo, Sebastiano
last_name: Cantalupo
- first_name: Saeed
full_name: Sarpas, Saeed
last_name: Sarpas
- first_name: Bastien
full_name: Duboeuf, Bastien
last_name: Duboeuf
- first_name: Simon
full_name: Lilly, Simon
last_name: Lilly
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Raffaella Anna
full_name: Marino, Raffaella Anna
last_name: Marino
- 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: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- first_name: Valentin
full_name: Mauerhofer, Valentin
last_name: Mauerhofer
citation:
ama: Gallego SG, Cantalupo S, Sarpas S, et al. Constraining the cosmic UV background
at z > 3 with MUSE Lyman-α emission observations. Monthly Notices of the
Royal Astronomical Society. 2021;504(1):16-32. doi:10.1093/mnras/stab796
apa: Gallego, S. G., Cantalupo, S., Sarpas, S., Duboeuf, B., Lilly, S., Pezzulli,
G., … Mauerhofer, V. (2021). Constraining the cosmic UV background at z >
3 with MUSE Lyman-α emission observations. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stab796
chicago: Gallego, Sofia G, Sebastiano Cantalupo, Saeed Sarpas, Bastien Duboeuf,
Simon Lilly, Gabriele Pezzulli, Raffaella Anna Marino, et al. “Constraining the
Cosmic UV Background at z > 3 with MUSE Lyman-α Emission Observations.” Monthly
Notices of the Royal Astronomical Society. Oxford University Press, 2021.
https://doi.org/10.1093/mnras/stab796.
ieee: S. G. Gallego et al., “Constraining the cosmic UV background at z >
3 with MUSE Lyman-α emission observations,” Monthly Notices of the Royal Astronomical
Society, vol. 504, no. 1. Oxford University Press, pp. 16–32, 2021.
ista: Gallego SG, Cantalupo S, Sarpas S, Duboeuf B, Lilly S, Pezzulli G, Marino
RA, Matthee JJ, Wisotzki L, Schaye J, Richard J, Kusakabe H, Mauerhofer V. 2021.
Constraining the cosmic UV background at z > 3 with MUSE Lyman-α emission
observations. Monthly Notices of the Royal Astronomical Society. 504(1), 16–32.
mla: Gallego, Sofia G., et al. “Constraining the Cosmic UV Background at z >
3 with MUSE Lyman-α Emission Observations.” Monthly Notices of the Royal Astronomical
Society, vol. 504, no. 1, Oxford University Press, 2021, pp. 16–32, doi:10.1093/mnras/stab796.
short: S.G. Gallego, S. Cantalupo, S. Sarpas, B. Duboeuf, S. Lilly, G. Pezzulli,
R.A. Marino, J.J. Matthee, L. Wisotzki, J. Schaye, J. Richard, H. Kusakabe, V.
Mauerhofer, Monthly Notices of the Royal Astronomical Society 504 (2021) 16–32.
date_created: 2022-07-07T10:07:11Z
date_published: 2021-06-01T00:00:00Z
date_updated: 2022-08-18T10:54:19Z
day: '01'
doi: 10.1093/mnras/stab796
extern: '1'
external_id:
arxiv:
- '2103.09250'
intvolume: ' 504'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2103.09250
month: '06'
oa: 1
oa_version: Preprint
page: 16-32
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: Constraining the cosmic UV background at z > 3 with MUSE Lyman-α emission observations
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 504
year: '2021'
...
---
_id: '11526'
abstract:
- lang: eng
text: We present the results from a MUSE survey of twelve z ≃ 3.15 quasars, which
were selected to be much fainter (20 < iSDSS < 23) than in previous studies of
giant Ly α nebulae around the brightest quasars (16.6 < iAB < 18.7). We detect
H I Ly α nebulae around 100 per cent of our target quasars, with emission extending
to scales of at least 60 physical kpc, and up to 190 pkpc. We explore correlations
between properties of the nebulae and their host quasars, with the goal of connecting
variations in the properties of the illuminating QSO to the response in nebular
emission. We show that the surface brightness profiles of the nebulae are similar
to those of nebulae around bright quasars, but with a lower normalization. Our
targeted quasars are on average 3.7 mag (≃30 times) fainter in UV continuum than
our bright reference sample, and yet the nebulae around them are only 4.3 times
fainter in mean Ly α surface brightness, measured between 20 and 50 pkpc. We find
significant correlations between the surface brightness of the nebula and the
luminosity of the quasar in both UV continuum and Ly α. The latter can be interpreted
as evidence for a substantial contribution from unresolved inner parts of the
nebulae to the narrow components seen in the Ly α lines of some of our faint quasars,
possibly from the inner circumgalactic medium or from the host galaxy’s interstellar
medium.
acknowledgement: The authors thank Daichi Kashino, for providing access to unpublished
zCOSMOS Deep data, and Jakob S. den Brok for sharing code used in den Brok et al.
(2020). GP and SC acknowledge the support of the Swiss National Science Foundation
[grant PP00P2163824]. SM is supported by the Experienced Researchers Fellowship,
Alexander von Humboldt-Stiftung, Germany. This work is based on observations collected
at the European Organisation for Astronomical Research in the Southern Hemisphere
under the MUSE GTO programme. The major analysis and production of figures in this
work was conducted in Python, using standard libraries which include NumPy (Harris
et al. 2020), SciPy (Virtanen et al. 2020), Matplotlib (Hunter 2007) and the interactive
command shell IPython (Pérez & Granger 2007). This research also made use of Astropy,
a community-developed core Python package for Astronomy (Astropy Collaboration et
al. 2013), and Photutils, an Astropy package for detection and photometry of astronomica
sources (Bradley et al. 2019). The python interface dustmaps (Green 2018) was used
to query galactic extinction maps. topcat, a graphical tool for manipulating tabular
data, was also utilized in this analysis (Taylor 2005). This research has made use
of the "Aladin sky atlas" developed at CDS, Strasbourg Observatory, France (Bonnarel
et al. 2000).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Ruari
full_name: Mackenzie, Ruari
last_name: Mackenzie
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Sebastiano
full_name: Cantalupo, Sebastiano
last_name: Cantalupo
- first_name: Raffaella A
full_name: Marino, Raffaella A
last_name: Marino
- first_name: Simon
full_name: Lilly, Simon
last_name: Lilly
- first_name: Sowgat
full_name: Muzahid, Sowgat
last_name: Muzahid
- 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: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
citation:
ama: Mackenzie R, Pezzulli G, Cantalupo S, et al. Revealing the impact of quasar
luminosity on giant Lyα nebulae. Monthly Notices of the Royal Astronomical
Society. 2021;502(1):494-509. doi:10.1093/mnras/staa3277
apa: Mackenzie, R., Pezzulli, G., Cantalupo, S., Marino, R. A., Lilly, S., Muzahid,
S., … Wisotzki, L. (2021). Revealing the impact of quasar luminosity on giant
Lyα nebulae. Monthly Notices of the Royal Astronomical Society. Oxford
University Press. https://doi.org/10.1093/mnras/staa3277
chicago: Mackenzie, Ruari, Gabriele Pezzulli, Sebastiano Cantalupo, Raffaella A
Marino, Simon Lilly, Sowgat Muzahid, Jorryt J Matthee, Joop Schaye, and Lutz Wisotzki.
“Revealing the Impact of Quasar Luminosity on Giant Lyα Nebulae.” Monthly Notices
of the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/staa3277.
ieee: R. Mackenzie et al., “Revealing the impact of quasar luminosity on
giant Lyα nebulae,” Monthly Notices of the Royal Astronomical Society,
vol. 502, no. 1. Oxford University Press, pp. 494–509, 2021.
ista: Mackenzie R, Pezzulli G, Cantalupo S, Marino RA, Lilly S, Muzahid S, Matthee
JJ, Schaye J, Wisotzki L. 2021. Revealing the impact of quasar luminosity on giant
Lyα nebulae. Monthly Notices of the Royal Astronomical Society. 502(1), 494–509.
mla: Mackenzie, Ruari, et al. “Revealing the Impact of Quasar Luminosity on Giant
Lyα Nebulae.” Monthly Notices of the Royal Astronomical Society, vol. 502,
no. 1, Oxford University Press, 2021, pp. 494–509, doi:10.1093/mnras/staa3277.
short: R. Mackenzie, G. Pezzulli, S. Cantalupo, R.A. Marino, S. Lilly, S. Muzahid,
J.J. Matthee, J. Schaye, L. Wisotzki, Monthly Notices of the Royal Astronomical
Society 502 (2021) 494–509.
date_created: 2022-07-07T10:11:15Z
date_published: 2021-03-01T00:00:00Z
date_updated: 2022-08-18T10:56:28Z
day: '01'
doi: 10.1093/mnras/staa3277
extern: '1'
external_id:
arxiv:
- '2010.12589'
intvolume: ' 502'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'techniques: imaging spectroscopy'
- intergalactic medium
- 'quasars: emission lines'
- 'quasars: general'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2010.12589
month: '03'
oa: 1
oa_version: Preprint
page: 494-509
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: Revealing the impact of quasar luminosity on giant Lyα nebulae
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 502
year: '2021'
...
---
_id: '13465'
abstract:
- lang: eng
text: "Gravitational-wave detections are now probing the black hole (BH) mass distribution,
including the predicted pair-instability mass gap. These data require robust quantitative
predictions, which are challenging to obtain. The most massive BH progenitors
experience episodic mass ejections on time-scales shorter than the convective
turnover time-scale. This invalidates the steady-state assumption on which the
classic mixing length theory relies. We compare the final BH masses computed with
two different versions of the stellar evolutionary code MESA\r\n: (i) using the
default implementation of Paxton et al. (2018) and (ii) solving an additional
equation accounting for the time-scale for convective deceleration. In the second
grid, where stronger convection develops during the pulses and carries part of
the energy, we find weaker pulses. This leads to lower amounts of mass being ejected
and thus higher final BH masses of up to ∼5M⊙\r\n. The differences are much smaller
for the progenitors that determine the maximum mass of BHs below the gap. This
prediction is robust at MBH,max≃48M⊙\r\n, at least within the idealized context
of this study. This is an encouraging indication that current models are robust
enough for comparison with the present-day gravitational-wave detections. However,
the large differences between individual models emphasize the importance of improving
the treatment of convection in stellar models, especially in the light of the
data anticipated from the third generation of gravitational-wave detectors."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: M
full_name: Renzo, M
last_name: Renzo
- first_name: R J
full_name: Farmer, R J
last_name: Farmer
- first_name: S
full_name: Justham, S
last_name: Justham
- first_name: S E
full_name: de Mink, S E
last_name: de Mink
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: P
full_name: Marchant, P
last_name: Marchant
citation:
ama: Renzo M, Farmer RJ, Justham S, de Mink SE, Götberg YLL, Marchant P. Sensitivity
of the lower edge of the pair-instability black hole mass gap to the treatment
of time-dependent convection. Monthly Notices of the Royal Astronomical Society.
2020;493(3):4333-4341. doi:10.1093/mnras/staa549
apa: Renzo, M., Farmer, R. J., Justham, S., de Mink, S. E., Götberg, Y. L. L., &
Marchant, P. (2020). Sensitivity of the lower edge of the pair-instability black
hole mass gap to the treatment of time-dependent convection. Monthly Notices
of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa549
chicago: Renzo, M, R J Farmer, S Justham, S E de Mink, Ylva Louise Linsdotter Götberg,
and P Marchant. “Sensitivity of the Lower Edge of the Pair-Instability Black Hole
Mass Gap to the Treatment of Time-Dependent Convection.” Monthly Notices of
the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa549.
ieee: M. Renzo, R. J. Farmer, S. Justham, S. E. de Mink, Y. L. L. Götberg, and P.
Marchant, “Sensitivity of the lower edge of the pair-instability black hole mass
gap to the treatment of time-dependent convection,” Monthly Notices of the
Royal Astronomical Society, vol. 493, no. 3. Oxford University Press, pp.
4333–4341, 2020.
ista: Renzo M, Farmer RJ, Justham S, de Mink SE, Götberg YLL, Marchant P. 2020.
Sensitivity of the lower edge of the pair-instability black hole mass gap to the
treatment of time-dependent convection. Monthly Notices of the Royal Astronomical
Society. 493(3), 4333–4341.
mla: Renzo, M., et al. “Sensitivity of the Lower Edge of the Pair-Instability Black
Hole Mass Gap to the Treatment of Time-Dependent Convection.” Monthly Notices
of the Royal Astronomical Society, vol. 493, no. 3, Oxford University Press,
2020, pp. 4333–41, doi:10.1093/mnras/staa549.
short: M. Renzo, R.J. Farmer, S. Justham, S.E. de Mink, Y.L.L. Götberg, P. Marchant,
Monthly Notices of the Royal Astronomical Society 493 (2020) 4333–4341.
date_created: 2023-08-03T10:13:20Z
date_published: 2020-04-04T00:00:00Z
date_updated: 2023-08-09T12:53:37Z
day: '04'
doi: 10.1093/mnras/staa549
extern: '1'
external_id:
arxiv:
- '2002.08200'
intvolume: ' 493'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/staa549
month: '04'
oa: 1
oa_version: Published Version
page: 4333-4341
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: Sensitivity of the lower edge of the pair-instability black hole mass gap to
the treatment of time-dependent convection
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 493
year: '2020'
...
---
_id: '11528'
abstract:
- lang: eng
text: Ly α emission lines are typically found to be redshifted with respect to the
systemic redshifts of galaxies, likely due to resonant scattering of Ly α photons.
Here, we measure the average velocity offset for a sample of 96 z ≈ 3.3 Ly α emitters
(LAEs) with a median Ly α flux (luminosity) of ≈10−17 erg cm−2 s−1 (≈1042 erg
s−1) and a median star formation rate (SFR) of ≈1.3 M⊙ yr−1 (not corrected for
possible dust extinction), detected by the Multi-Unit Spectroscopic Explorer as
part of our MUSEQuBES circumgalactic medium (CGM) survey. By postulating that
the stacked CGM absorption profiles of these LAEs, probed by eight background
quasars, must be centred on the systemic redshift, we measure an average velocity
offset, Voffset = 171\pm 8 km s−1, between the Ly α emission peak and the systemic
redshift. The observed Voffset is lower by factors of ≈1.4 and ≈2.6 compared to
the velocity offsets measured for narrow-band-selected LAEs and Lyman break galaxies,
respectively, which probe galaxies with higher masses and SFRs. Consistent with
earlier studies based on direct measurements for individual objects, we find that
the Voffset is correlated with the full width at half-maximum of the red peak
of the Ly α line, and anticorrelated with the rest-frame equivalent width. Moreover,
we find that Voffset is correlated with SFR with a sub-linear scaling relation,
Voffset∝SFR0.16±0.03. Adopting the mass scaling for main-sequence galaxies, such
a relation suggests that Voffset scales with the circular velocity of the dark
matter haloes hosting the LAEs.
acknowledgement: 'We thank the anonymous referee for useful suggestions. This study
is based on observations collected at the European Organisation for Astronomical
Research in the Southern Hemisphere under ESO programme(s): 094.A-0131(B), 095.A
0200(A), 096.A0222(A), 097.A-0089(A), and 099.A-0159(A). SM acknowledges support
from the Alexander von Humboldt Foundation, Germany. SM thanks Christian Herenz
for useful discussion. SC gratefully acknowledges support from Swiss National Science
Foundation grant PP00P2 163824. JB acknowledges support by FCT/MCTES through national
funds by grant UID/FIS/04434/2019 and through Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003.
NB and JZ acknowledge support from ANR grant ANR-17-CE31- 0017 (3DGasFlows). AC
and JR acknowledge support from the ERC starting grant 336736-CALENDS. MA acknowledges
support from European Union’s H2020 Marie Skłodowska-Curie Actions grant 721463
to the SUNDIAL ITN, and from the Spanish Ministry of Economy and Competitiveness
(MINECO) under grant number AYA2016-76219-P. MA also acknowledges support from the
Fundacion BBVA under its 2017 programme of assistance to ´scientific research groups,
for the project ‘Using machine-learning techniques to drag galaxies from the noise
in deep imaging’. FL and AV acknowledge support from the ERC starting grant ERC757258-TRIPLE.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Sowgat
full_name: Muzahid, Sowgat
last_name: Muzahid
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Raffaella Anna
full_name: Marino, Raffaella Anna
last_name: Marino
- first_name: Sebastiano
full_name: Cantalupo, Sebastiano
last_name: Cantalupo
- first_name: Jarle
full_name: Brinchmann, Jarle
last_name: Brinchmann
- first_name: Thierry
full_name: Contini, Thierry
last_name: Contini
- first_name: Martin
full_name: Wendt, Martin
last_name: Wendt
- first_name: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
- first_name: Johannes
full_name: Zabl, Johannes
last_name: Zabl
- first_name: Nicolas
full_name: Bouché, Nicolas
last_name: Bouché
- first_name: Mohammad
full_name: Akhlaghi, Mohammad
last_name: Akhlaghi
- first_name: Hsiao-Wen
full_name: Chen, Hsiao-Wen
last_name: Chen
- first_name: Adélaîde
full_name: Claeyssens, Adélaîde
last_name: Claeyssens
- first_name: Sean
full_name: Johnson, Sean
last_name: Johnson
- first_name: Floriane
full_name: Leclercq, Floriane
last_name: Leclercq
- 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: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Tanya
full_name: Urrutia, Tanya
last_name: Urrutia
- first_name: Anne
full_name: Verhamme, Anne
last_name: Verhamme
citation:
ama: 'Muzahid S, Schaye J, Marino RA, et al. MUSEQuBES: Calibrating the redshifts
of Lyα emitters using stacked circumgalactic medium absorption profiles. Monthly
Notices of the Royal Astronomical Society. 2020;496(2):1013-1022. doi:10.1093/mnras/staa1347'
apa: 'Muzahid, S., Schaye, J., Marino, R. A., Cantalupo, S., Brinchmann, J., Contini,
T., … Verhamme, A. (2020). MUSEQuBES: Calibrating the redshifts of Lyα emitters
using stacked circumgalactic medium absorption profiles. Monthly Notices of
the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa1347'
chicago: 'Muzahid, Sowgat, Joop Schaye, Raffaella Anna Marino, Sebastiano Cantalupo,
Jarle Brinchmann, Thierry Contini, Martin Wendt, et al. “MUSEQuBES: Calibrating
the Redshifts of Lyα Emitters Using Stacked Circumgalactic Medium Absorption Profiles.”
Monthly Notices of the Royal Astronomical Society. Oxford University Press,
2020. https://doi.org/10.1093/mnras/staa1347.'
ieee: 'S. Muzahid et al., “MUSEQuBES: Calibrating the redshifts of Lyα emitters
using stacked circumgalactic medium absorption profiles,” Monthly Notices of
the Royal Astronomical Society, vol. 496, no. 2. Oxford University Press,
pp. 1013–1022, 2020.'
ista: 'Muzahid S, Schaye J, Marino RA, Cantalupo S, Brinchmann J, Contini T, Wendt
M, Wisotzki L, Zabl J, Bouché N, Akhlaghi M, Chen H-W, Claeyssens A, Johnson S,
Leclercq F, Maseda M, Matthee JJ, Richard J, Urrutia T, Verhamme A. 2020. MUSEQuBES:
Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium
absorption profiles. Monthly Notices of the Royal Astronomical Society. 496(2),
1013–1022.'
mla: 'Muzahid, Sowgat, et al. “MUSEQuBES: Calibrating the Redshifts of Lyα Emitters
Using Stacked Circumgalactic Medium Absorption Profiles.” Monthly Notices of
the Royal Astronomical Society, vol. 496, no. 2, Oxford University Press,
2020, pp. 1013–22, doi:10.1093/mnras/staa1347.'
short: S. Muzahid, J. Schaye, R.A. Marino, S. Cantalupo, J. Brinchmann, T. Contini,
M. Wendt, L. Wisotzki, J. Zabl, N. Bouché, M. Akhlaghi, H.-W. Chen, A. Claeyssens,
S. Johnson, F. Leclercq, M. Maseda, J.J. Matthee, J. Richard, T. Urrutia, A. Verhamme,
Monthly Notices of the Royal Astronomical Society 496 (2020) 1013–1022.
date_created: 2022-07-07T10:20:11Z
date_published: 2020-08-01T00:00:00Z
date_updated: 2022-08-18T11:00:24Z
day: '01'
doi: 10.1093/mnras/staa1347
extern: '1'
external_id:
arxiv:
- '1910.03593'
intvolume: ' 496'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: haloes'
- 'galaxies: high-redshift'
- 'quasars: absorption lines'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1910.03593
month: '08'
oa: 1
oa_version: Preprint
page: 1013-1022
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'
related_material:
link:
- relation: erratum
url: https://doi.org/10.1093/mnras/staa2668
scopus_import: '1'
status: public
title: 'MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic
medium absorption profiles'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 496
year: '2020'
...
---
_id: '11529'
abstract:
- lang: eng
text: CR7 is among the most luminous Ly α emitters (LAEs) known at z = 6.6 and consists
of at least three UV components that are surrounded by Ly α emission. Previous
studies have suggested that it may host an extreme ionizing source. Here, we present
deep integral field spectroscopy of CR7 with VLT/Multi Unit Spectroscopic Explorer
(MUSE). We measure extended emission with a similar halo scale length as typical
LAEs at z ≈ 5. CR7’s Ly α halo is clearly elongated along the direction connecting
the multiple components, likely tracing the underlying gas distribution. The Ly α
emission originates almost exclusively from the brightest UV component, but we
also identify a faint kinematically distinct Ly α emitting region nearby a fainter
component. Combined with new near-infrared data, the MUSE data show that the rest-frame
Ly α equivalent width (EW) is ≈100 Å. This is a factor 4 higher than the EW measured
in low-redshift analogues with carefully matched Ly α profiles (and thus arguably
H I column density), but this EW can plausibly be explained by star formation.
Alternative scenarios requiring active galactic nucleus (AGN) powering are also
disfavoured by the narrower and steeper Ly α spectrum and much smaller IR to UV
ratio compared to obscured AGN in other Ly α blobs. CR7’s Ly α emission, while
extremely luminous, resembles the emission in more common LAEs at lower redshifts
very well and is likely powered by a young metal-poor starburst.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Ruari
full_name: Mackenzie, Ruari
last_name: Mackenzie
- first_name: Sebastiano
full_name: Cantalupo, Sebastiano
last_name: Cantalupo
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- first_name: Floriane
full_name: Leclercq, Floriane
last_name: Leclercq
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
- first_name: Simon
full_name: Lilly, Simon
last_name: Lilly
- first_name: Leindert
full_name: Boogaard, Leindert
last_name: Boogaard
- first_name: Raffaella
full_name: Marino, Raffaella
last_name: Marino
- first_name: Michael
full_name: Maseda, Michael
last_name: Maseda
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
citation:
ama: 'Matthee JJ, Pezzulli G, Mackenzie R, et al. The nature of CR7 revealed with
MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly
Notices of the Royal Astronomical Society. 2020;498(2):3043-3059. doi:10.1093/mnras/staa2550'
apa: 'Matthee, J. J., Pezzulli, G., Mackenzie, R., Cantalupo, S., Kusakabe, H.,
Leclercq, F., … Nanayakkara, T. (2020). The nature of CR7 revealed with MUSE:
A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices
of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa2550'
chicago: 'Matthee, Jorryt J, Gabriele Pezzulli, Ruari Mackenzie, Sebastiano Cantalupo,
Haruka Kusakabe, Floriane Leclercq, David Sobral, et al. “The Nature of CR7 Revealed
with MUSE: A Young Starburst Powering Extended Ly α Emission at z = 6.6.” Monthly
Notices of the Royal Astronomical Society. Oxford University Press, 2020.
https://doi.org/10.1093/mnras/staa2550.'
ieee: 'J. J. Matthee et al., “The nature of CR7 revealed with MUSE: A young
starburst powering extended Ly α emission at z = 6.6,” Monthly Notices of the
Royal Astronomical Society, vol. 498, no. 2. Oxford University Press, pp.
3043–3059, 2020.'
ista: 'Matthee JJ, Pezzulli G, Mackenzie R, Cantalupo S, Kusakabe H, Leclercq F,
Sobral D, Richard J, Wisotzki L, Lilly S, Boogaard L, Marino R, Maseda M, Nanayakkara
T. 2020. The nature of CR7 revealed with MUSE: A young starburst powering extended
Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. 498(2),
3043–3059.'
mla: 'Matthee, Jorryt J., et al. “The Nature of CR7 Revealed with MUSE: A Young
Starburst Powering Extended Ly α Emission at z = 6.6.” Monthly Notices of the
Royal Astronomical Society, vol. 498, no. 2, Oxford University Press, 2020,
pp. 3043–59, doi:10.1093/mnras/staa2550.'
short: J.J. Matthee, G. Pezzulli, R. Mackenzie, S. Cantalupo, H. Kusakabe, F. Leclercq,
D. Sobral, J. Richard, L. Wisotzki, S. Lilly, L. Boogaard, R. Marino, M. Maseda,
T. Nanayakkara, Monthly Notices of the Royal Astronomical Society 498 (2020) 3043–3059.
date_created: 2022-07-07T10:36:01Z
date_published: 2020-10-01T00:00:00Z
date_updated: 2022-08-18T11:04:05Z
day: '01'
doi: 10.1093/mnras/staa2550
extern: '1'
external_id:
arxiv:
- '2008.01731'
intvolume: ' 498'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- dark ages
- reionization
- first stars
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2008.01731
month: '10'
oa: 1
oa_version: Preprint
page: 3043-3059
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The nature of CR7 revealed with MUSE: A young starburst powering extended
Ly α emission at z = 6.6'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 498
year: '2020'
...
---
_id: '11530'
abstract:
- lang: eng
text: A prediction of the classic active galactic nucleus (AGN) unification model
is the presence of ionization cones with different orientations depending on the
AGN type. Confirmations of this model exist for present times, but it is less
clear in the early Universe. Here, we use the morphology of giant Ly α nebulae
around AGNs at redshift z ∼ 3 to probe AGN emission and therefore the validity
of the AGN unification model at this redshift. We compare the spatial morphology
of 19 nebulae previously found around type I AGNs with a new sample of four Ly α
nebulae detected around type II AGNs. Using two independent techniques, we find
that nebulae around type II AGNs are more asymmetric than around type I, at least
at radial distances r > 30 physical kpc (pkpc) from the ionizing source. We conclude
that the type I and type II AGNs in our sample show evidence of different surrounding
ionizing geometries. This suggests that the classical AGN unification model is
also valid for high-redshift sources. Finally, we discuss how the lack of asymmetry
in the inner parts (r ≲ 30 pkpc) and the associated high values of the He II to
Ly α ratios in these regions could indicate additional sources of (hard) ionizing
radiation originating within or in proximity of the AGN host galaxies. This work
demonstrates that the morphologies of giant Ly α nebulae can be used to understand
and study the geometry of high-redshift AGNs on circumnuclear scales and it lays
the foundation for future studies using much larger statistical samples.
acknowledgement: SC and GP gratefully acknowledge support from Swiss National Science
Foundation grant PP00P2 163824. MK acknowledges support by DLR500R1904.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: J S
full_name: den Brok, J S
last_name: den Brok
- first_name: S
full_name: Cantalupo, S
last_name: Cantalupo
- first_name: R
full_name: Mackenzie, R
last_name: Mackenzie
- first_name: R A
full_name: Marino, R A
last_name: Marino
- first_name: G
full_name: Pezzulli, G
last_name: Pezzulli
- 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: S D
full_name: Johnson, S D
last_name: Johnson
- first_name: M
full_name: Krumpe, M
last_name: Krumpe
- first_name: T
full_name: Urrutia, T
last_name: Urrutia
- first_name: W
full_name: Kollatschny, W
last_name: Kollatschny
citation:
ama: den Brok JS, Cantalupo S, Mackenzie R, et al. Probing the AGN unification model
at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae. Monthly Notices
of the Royal Astronomical Society. 2020;495(2):1874-1887. doi:10.1093/mnras/staa1269
apa: den Brok, J. S., Cantalupo, S., Mackenzie, R., Marino, R. A., Pezzulli, G.,
Matthee, J. J., … Kollatschny, W. (2020). Probing the AGN unification model at
redshift z ∼ 3 with MUSE observations of giant Lyα nebulae. Monthly Notices
of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa1269
chicago: den Brok, J S, S Cantalupo, R Mackenzie, R A Marino, G Pezzulli, Jorryt
J Matthee, S D Johnson, M Krumpe, T Urrutia, and W Kollatschny. “Probing the AGN
Unification Model at Redshift z ∼ 3 with MUSE Observations of Giant Lyα Nebulae.”
Monthly Notices of the Royal Astronomical Society. Oxford University Press,
2020. https://doi.org/10.1093/mnras/staa1269.
ieee: J. S. den Brok et al., “Probing the AGN unification model at redshift
z ∼ 3 with MUSE observations of giant Lyα nebulae,” Monthly Notices of the
Royal Astronomical Society, vol. 495, no. 2. Oxford University Press, pp.
1874–1887, 2020.
ista: den Brok JS, Cantalupo S, Mackenzie R, Marino RA, Pezzulli G, Matthee JJ,
Johnson SD, Krumpe M, Urrutia T, Kollatschny W. 2020. Probing the AGN unification
model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae. Monthly Notices
of the Royal Astronomical Society. 495(2), 1874–1887.
mla: den Brok, J. S., et al. “Probing the AGN Unification Model at Redshift z ∼
3 with MUSE Observations of Giant Lyα Nebulae.” Monthly Notices of the Royal
Astronomical Society, vol. 495, no. 2, Oxford University Press, 2020, pp.
1874–87, doi:10.1093/mnras/staa1269.
short: J.S. den Brok, S. Cantalupo, R. Mackenzie, R.A. Marino, G. Pezzulli, J.J.
Matthee, S.D. Johnson, M. Krumpe, T. Urrutia, W. Kollatschny, Monthly Notices
of the Royal Astronomical Society 495 (2020) 1874–1887.
date_created: 2022-07-07T10:40:17Z
date_published: 2020-06-01T00:00:00Z
date_updated: 2022-08-18T11:17:47Z
day: '01'
doi: 10.1093/mnras/staa1269
extern: '1'
external_id:
arxiv:
- '2005.01732'
intvolume: ' 495'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: active'
- 'galaxies: high-redshift'
- intergalactic medium
- 'quasars: emission lines'
- 'quasars: general'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2005.01732
month: '06'
oa: 1
oa_version: Preprint
page: 1874-1887
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: Probing the AGN unification model at redshift z ∼ 3 with MUSE observations
of giant Lyα nebulae
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 495
year: '2020'
...
---
_id: '11531'
abstract:
- lang: eng
text: While low-luminosity galaxies dominate number counts at all redshifts, their
contribution to cosmic reionization is poorly understood due to a lack of knowledge
of their physical properties. We isolate a sample of 35 z ≈ 4–5 continuum-faint
Lyman-α emitters from deep VLT/MUSE spectroscopy and directly measure their H α
emission using stacked Spitzer/IRAC Ch. 1 photometry. Based on Hubble Space Telescope
imaging, we determine that the average UV continuum magnitude is fainter than
−16 (≈ 0.01 L⋆), implying a median Lyman-α equivalent width of 259 Å. By combining
the H α measurement with the UV magnitude, we determine the ionizing photon production
efficiency, ξion, a first for such faint galaxies. The measurement of log10 (ξion
[Hz erg−1]) = 26.28 (+0.28−0.40) is in excess of literature measurements of
both continuum- and emission line-selected samples, implying a more efficient
production of ionizing photons in these lower luminosity, Lyman-α-selected systems.
We conclude that this elevated efficiency can be explained by stellar populations
with metallicities between 4 × 10−4 and 0.008, with light-weighted ages less than
3 Myr.
acknowledgement: 'We would like to thank the anonymous referee for a thoughtful report
and suggestions that have improved this manuscript. We are also grateful to everyone
involved in the Spitzer Space Telescope mission and everyone at the Spitzer Science
Center: we are truly fortunate to have been able to use data from this facility.
J. B. acknowledges support by FCT/MCTES through national funds by this grant UID/FIS/04434/2019
and through the Investigador FCT contract no. IF/01654/2014/CP1215/CT0003. S. C.
gratefully acknowledges support from Swiss National Science Foundation grant PP00P2
163824. We would also like to thank Mauro Stefanon for his assistance with de-blending
the IRAC photometry, Pieter van Dokkum for a number of useful suggestions, and Daniel
Schaerer for information regarding the stellar population models. This study is
based on observations made with ESO telescopes at the La Silla Paranal Observatory
under programs IDs 094.A-2089(B), 095.A0010(A), 096.A-0045(A), and 096.A-0045(B).'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Michael V
full_name: Maseda, Michael V
last_name: Maseda
- first_name: Roland
full_name: Bacon, Roland
last_name: Bacon
- first_name: Daniel
full_name: Lam, Daniel
last_name: Lam
- 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: Jarle
full_name: Brinchmann, Jarle
last_name: Brinchmann
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Ivo
full_name: Labbe, Ivo
last_name: Labbe
- first_name: Kasper B
full_name: Schmidt, Kasper B
last_name: Schmidt
- 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: Marijn
full_name: Franx, Marijn
last_name: Franx
- first_name: Takuya
full_name: Hashimoto, Takuya
last_name: Hashimoto
- first_name: Hanae
full_name: Inami, Hanae
last_name: Inami
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- first_name: Guillaume
full_name: Mahler, Guillaume
last_name: Mahler
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
- first_name: Johan
full_name: Richard, Johan
last_name: Richard
- first_name: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
citation:
ama: Maseda MV, Bacon R, Lam D, et al. Elevated ionizing photon production efficiency
in faint high-equivalent-width Lyman-α emitters. Monthly Notices of the Royal
Astronomical Society. 2020;493(4):5120-5130. doi:10.1093/mnras/staa622
apa: Maseda, M. V., Bacon, R., Lam, D., Matthee, J. J., Brinchmann, J., Schaye,
J., … Wisotzki, L. (2020). Elevated ionizing photon production efficiency in faint
high-equivalent-width Lyman-α emitters. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/staa622
chicago: Maseda, Michael V, Roland Bacon, Daniel Lam, Jorryt J Matthee, Jarle Brinchmann,
Joop Schaye, Ivo Labbe, et al. “Elevated Ionizing Photon Production Efficiency
in Faint High-Equivalent-Width Lyman-α Emitters.” Monthly Notices of the Royal
Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa622.
ieee: M. V. Maseda et al., “Elevated ionizing photon production efficiency
in faint high-equivalent-width Lyman-α emitters,” Monthly Notices of the Royal
Astronomical Society, vol. 493, no. 4. Oxford University Press, pp. 5120–5130,
2020.
ista: Maseda MV, Bacon R, Lam D, Matthee JJ, Brinchmann J, Schaye J, Labbe I, Schmidt
KB, Boogaard L, Bouwens R, Cantalupo S, Franx M, Hashimoto T, Inami H, Kusakabe
H, Mahler G, Nanayakkara T, Richard J, Wisotzki L. 2020. Elevated ionizing photon
production efficiency in faint high-equivalent-width Lyman-α emitters. Monthly
Notices of the Royal Astronomical Society. 493(4), 5120–5130.
mla: Maseda, Michael V., et al. “Elevated Ionizing Photon Production Efficiency
in Faint High-Equivalent-Width Lyman-α Emitters.” Monthly Notices of the Royal
Astronomical Society, vol. 493, no. 4, Oxford University Press, 2020, pp.
5120–30, doi:10.1093/mnras/staa622.
short: M.V. Maseda, R. Bacon, D. Lam, J.J. Matthee, J. Brinchmann, J. Schaye, I.
Labbe, K.B. Schmidt, L. Boogaard, R. Bouwens, S. Cantalupo, M. Franx, T. Hashimoto,
H. Inami, H. Kusakabe, G. Mahler, T. Nanayakkara, J. Richard, L. Wisotzki, Monthly
Notices of the Royal Astronomical Society 493 (2020) 5120–5130.
date_created: 2022-07-07T10:46:41Z
date_published: 2020-04-01T00:00:00Z
date_updated: 2022-08-18T11:23:27Z
day: '01'
doi: 10.1093/mnras/staa622
extern: '1'
external_id:
arxiv:
- '2002.11117'
intvolume: ' 493'
issue: '4'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'Galaxies: evolution'
- 'Galaxies: high-redshift'
- 'Galaxies: ISM'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/staa622
month: '04'
oa: 1
oa_version: Published Version
page: 5120-5130
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: Elevated ionizing photon production efficiency in faint high-equivalent-width
Lyman-α emitters
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 493
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: '11534'
abstract:
- lang: eng
text: The observed properties of the Lyman-α (Ly α) emission line are a powerful
probe of neutral gas in and around galaxies. We present spatially resolved Ly α
spectroscopy with VLT/MUSE targeting VR7, a UV-luminous galaxy at z = 6.532 with
moderate Ly α equivalent width (EW0 ≈ 38 Å). These data are combined with deep
resolved [CII]158μm spectroscopy obtained with ALMA and UV imaging from HST and
we also detect UV continuum with MUSE. Ly α emission is clearly detected with
S/N ≈ 40 and FWHM of 374 km s−1. Ly α and [C II] are similarly extended beyond
the UV, with effective radius reff = 2.1 ± 0.2 kpc for a single exponential model
or reff,Lyα,halo=3.45+1.08−0.87 kpc when measured jointly with the UV continuum.
The Ly α profile is broader and redshifted with respect to the [C II] line (by
213 km s−1), but there are spatial variations that are qualitatively similar in
both lines and coincide with resolved UV components. This suggests that the emission
originates from two components with plausibly different H I column densities.
We place VR7 in the context of other galaxies at similar and lower redshift. The
Ly α halo scale length is similar at different redshifts and velocity shifts with
respect to the systemic are typically smaller. Overall, we find little indications
of a more neutral vicinity at higher redshift. This means that the local (∼10 kpc)
neutral gas conditions that determine the observed Ly α properties in VR7 resemble
the conditions in post-reionization galaxies.
acknowledgement: 'We thank the referee for their suggestions and constructive comments
that helped to improve the presentation of our results. Based on observations obtained
with the Very Large Telescope, program 99.A-0462. Based on observations made with
the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-26555. These observations are associated with program
#14699. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.01451.S.
ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS
(Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic
of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory
is operated by ESO, AUI/NRAO, and NAOJ. MG acknowledges support from NASA grant
NNX17AK58G. GP and SC gratefully acknowledge support from Swiss National Science
Foundation grant PP00P2 163824. BD acknowledges financial support from the National
Science Foundation, grant number 1716907. We have benefited greatly from the public
available programming language PYTHON, including the NUMPY, MATPLOTLIB, SCIPY (Jones
et al. 2001; Hunter 2007; van der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy
Collaboration 2013) packages, the astronomical imaging tools SEXTRACTOR, SWARP,
and SCAMP (Bertin & Arnouts 1996; Bertin 2006, 2010) and the TOPCAT analysis tool
(Taylor 2013).'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Sebastiano
full_name: Cantalupo, Sebastiano
last_name: Cantalupo
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
- first_name: Behnam
full_name: Darvish, Behnam
last_name: Darvish
- first_name: Sérgio
full_name: Santos, Sérgio
last_name: Santos
citation:
ama: Matthee JJ, Sobral D, Gronke M, et al. Resolved Lyman-α properties of a luminous
Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices
of the Royal Astronomical Society. 2020;492(2):1778-1790. doi:10.1093/mnras/stz3554
apa: Matthee, J. J., Sobral, D., Gronke, M., Pezzulli, G., Cantalupo, S., Röttgering,
H., … Santos, S. (2020). Resolved Lyman-α properties of a luminous Lyman-break
galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal
Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz3554
chicago: Matthee, Jorryt J, David Sobral, Max Gronke, Gabriele Pezzulli, Sebastiano
Cantalupo, Huub Röttgering, Behnam Darvish, and Sérgio Santos. “Resolved Lyman-α
Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53
.” Monthly Notices of the Royal Astronomical Society. Oxford University
Press, 2020. https://doi.org/10.1093/mnras/stz3554.
ieee: J. J. Matthee et al., “Resolved Lyman-α properties of a luminous Lyman-break
galaxy in a large ionized bubble at z = 6.53 ,” Monthly Notices of the Royal
Astronomical Society, vol. 492, no. 2. Oxford University Press, pp. 1778–1790,
2020.
ista: Matthee JJ, Sobral D, Gronke M, Pezzulli G, Cantalupo S, Röttgering H, Darvish
B, Santos S. 2020. Resolved Lyman-α properties of a luminous Lyman-break galaxy
in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical
Society. 492(2), 1778–1790.
mla: Matthee, Jorryt J., et al. “Resolved Lyman-α Properties of a Luminous Lyman-Break
Galaxy in a Large Ionized Bubble at z = 6.53 .” Monthly Notices of the Royal
Astronomical Society, vol. 492, no. 2, Oxford University Press, 2020, pp.
1778–90, doi:10.1093/mnras/stz3554.
short: J.J. Matthee, D. Sobral, M. Gronke, G. Pezzulli, S. Cantalupo, H. Röttgering,
B. Darvish, S. Santos, Monthly Notices of the Royal Astronomical Society 492 (2020)
1778–1790.
date_created: 2022-07-07T12:21:36Z
date_published: 2020-02-01T00:00:00Z
date_updated: 2022-08-18T11:29:53Z
day: '01'
doi: 10.1093/mnras/stz3554
extern: '1'
external_id:
arxiv:
- '1909.06376'
intvolume: ' 492'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- dark ages
- reionization
- first stars
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1909.06376
month: '02'
oa: 1
oa_version: Preprint
page: 1778-1790
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized
bubble at z = 6.53 '
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 492
year: '2020'
...
---
_id: '11539'
abstract:
- lang: eng
text: 'Despite recent progress in understanding Ly α emitters (LAEs), relatively
little is known regarding their typical black hole activity across cosmic time.
Here, we study the X-ray and radio properties of ∼4000 LAEs at 2.2 < z < 6 from
the SC4K survey in the COSMOS field. We detect 254 (6.8per cent±0.4per cent)
LAEs individually in the X-rays (S/N > 3) with an average luminosity of 1044.31±0.01ergs−1
and average black hole accretion rate (BHAR) of 0.72±0.01 M⊙ yr−1, consistent
with moderate to high accreting active galactic neuclei (AGNs). We detect 120
sources in deep radio data (radio AGN fraction of 3.2per cent±0.3per cent). The
global AGN fraction (8.6per cent±0.4per cent) rises with Ly α luminosity and
declines with increasing redshift. For X-ray-detected LAEs, Ly α luminosities
correlate with the BHARs, suggesting that Ly α luminosity becomes a BHAR indicator.
Most LAEs (93.1per cent±0.6per cent) at 2 < z < 6 have no detectable X-ray emission
(BHARs < 0.017 M⊙ yr−1). The median star formation rate (SFR) of star-forming
LAEs from Ly α and radio luminosities is 7.6+6.6−2.8 M⊙ yr−1. The black hole to
galaxy growth ratio (BHAR/SFR) for LAEs is <0.0022, consistent with typical star-forming
galaxies and the local BHAR/SFR relation. We conclude that LAEs at 2 < z < 6 include
two different populations: an AGN population, where Ly α luminosity traces BHAR,
and another with low SFRs which remain undetected in even the deepest X-ray stacks
but is detected in the radio stacks.'
acknowledgement: JM acknowledges the support of a Huygens PhD fellowship from Leiden
University. We thank Camila Correa for help analysing snipshot merger trees. We
thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann,
Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and
suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade
of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and
ideas. We have benefited from the public available programming language PYTHON,
including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT
analysis tool (Taylor 2013).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: João
full_name: Calhau, João
last_name: Calhau
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Sérgio
full_name: Santos, Sérgio
last_name: Santos
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Ana
full_name: Paulino-Afonso, Ana
last_name: Paulino-Afonso
- first_name: Andra
full_name: Stroe, Andra
last_name: Stroe
- first_name: Brooke
full_name: Simmons, Brooke
last_name: Simmons
- first_name: Cassandra
full_name: Barlow-Hall, Cassandra
last_name: Barlow-Hall
- first_name: Benjamin
full_name: Adams, Benjamin
last_name: Adams
citation:
ama: 'Calhau J, Sobral D, Santos S, et al. The X-ray and radio activity of typical
and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving
population. Monthly Notices of the Royal Astronomical Society. 2020;493(3):3341-3362.
doi:10.1093/mnras/staa476'
apa: 'Calhau, J., Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Stroe,
A., … Adams, B. (2020). The X-ray and radio activity of typical and luminous Ly α
emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. Monthly
Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa476'
chicago: 'Calhau, João, David Sobral, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso,
Andra Stroe, Brooke Simmons, Cassandra Barlow-Hall, and Benjamin Adams. “The X-Ray
and Radio Activity of Typical and Luminous Ly α Emitters from z ∼ 2 to z ∼ 6:
Evidence for a Diverse, Evolving Population.” Monthly Notices of the Royal
Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa476.'
ieee: 'J. Calhau et al., “The X-ray and radio activity of typical and luminous
Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population,”
Monthly Notices of the Royal Astronomical Society, vol. 493, no. 3. Oxford
University Press, pp. 3341–3362, 2020.'
ista: 'Calhau J, Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Stroe A, Simmons
B, Barlow-Hall C, Adams B. 2020. The X-ray and radio activity of typical and luminous
Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population.
Monthly Notices of the Royal Astronomical Society. 493(3), 3341–3362.'
mla: 'Calhau, João, et al. “The X-Ray and Radio Activity of Typical and Luminous
Ly α Emitters from z ∼ 2 to z ∼ 6: Evidence for a Diverse, Evolving Population.”
Monthly Notices of the Royal Astronomical Society, vol. 493, no. 3, Oxford
University Press, 2020, pp. 3341–62, doi:10.1093/mnras/staa476.'
short: J. Calhau, D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, A. Stroe,
B. Simmons, C. Barlow-Hall, B. Adams, Monthly Notices of the Royal Astronomical
Society 493 (2020) 3341–3362.
date_created: 2022-07-08T07:34:10Z
date_published: 2020-04-01T00:00:00Z
date_updated: 2022-08-18T11:25:31Z
day: '01'
doi: 10.1093/mnras/staa476
extern: '1'
external_id:
arxiv:
- '1909.11672'
intvolume: ' 493'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: active'
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'quasars: supermassive black holes'
- 'galaxies: star formation'
- 'cosmology: observations'
- 'X-rays: galaxies'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1909.11672
month: '04'
oa: 1
oa_version: Preprint
page: 3341-3362
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The X-ray and radio activity of typical and luminous Ly α emitters from z
∼ 2 to z ∼ 6: Evidence for a diverse, evolving population'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 493
year: '2020'
...
---
_id: '11535'
abstract:
- lang: eng
text: We investigate the clustering and halo properties of ∼5000 Ly α-selected emission-line
galaxies (LAEs) from the Slicing COSMOS 4K (SC4K) and from archival NB497 imaging
of SA22 split in 15 discrete redshift slices between z ∼ 2.5 and 6. We measure
clustering lengths of r0 ∼ 3–6 h−1 Mpc and typical halo masses of ∼1011 M⊙ for
our narrowband-selected LAEs with typical LLy α ∼ 1042–43 erg s−1. The intermediate-band-selected
LAEs are observed to have r0 ∼ 3.5–15 h−1 Mpc with typical halo masses of ∼1011–12
M⊙ and typical LLy α ∼ 1043–43.6 erg s−1. We find a strong, redshift-independent
correlation between halo mass and Ly α luminosity normalized by the characteristic
Ly α luminosity, L⋆(z). The faintest LAEs (L ∼ 0.1 L⋆(z)) typically identified
by deep narrowband surveys are found in 1010 M⊙ haloes and the brightest LAEs
(L ∼ 7 L⋆(z)) are found in ∼5 × 1012 M⊙ haloes. A dependency on the rest-frame
1500 Å UV luminosity, MUV, is also observed where the halo masses increase from
1011 to 1013 M⊙ for MUV ∼ −19 to −23.5 mag. Halo mass is also observed to increase
from 109.8 to 1012 M⊙ for dust-corrected UV star formation rates from ∼0.6 to
10 M⊙ yr−1 and continues to increase up to 1013 M⊙ in halo mass, where the majority
of those sources are active galactic nuclei. All the trends we observe are found
to be redshift independent. Our results reveal that LAEs are the likely progenitors
of a wide range of galaxies depending on their luminosity, from dwarf-like, to
Milky Way-type, to bright cluster galaxies. LAEs therefore provide unique insight
into the early formation and evolution of the galaxies we observe in the local
Universe.
acknowledgement: We thank the anonymous referee for their useful comments and suggestions
that helped improve this study. AAK acknowledges that this work was supported by
NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant
NNX16AO92H. JM acknowledges support from the ETH Zwicky fellowship. RKC acknowledges
funding from STFC via a studentship. APA acknowledges support from the Fundac¸ao
para a Ci ˜ encia e a Tecnologia FCT through the fellowship PD/BD/52706/2014 and
the research grant UID/FIS/04434/2013. JC and SS both acknowledge their support
from the Lancaster University PhD Fellowship. We have benefited greatly from the
publicly available programming language PYTHON, including the NUMPY, SCIPY, MATPLOTLIB,
SCIKIT-LEARN, and ASTROPY packages, as well as the TOPCAT analysis program. The
SC4K samples used in this paper are all publicly available for use by the community
(Sobral et al. 2018a). The catalogue is also available on the COSMOS IPAC website
(https://irsa.ipac.caltech.edu/data/COSMOS/overview.html).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: A A
full_name: Khostovan, A A
last_name: Khostovan
- first_name: D
full_name: Sobral, D
last_name: Sobral
- first_name: B
full_name: Mobasher, B
last_name: Mobasher
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: R K
full_name: Cochrane, R K
last_name: Cochrane
- first_name: N
full_name: Chartab, N
last_name: Chartab
- first_name: M
full_name: Jafariyazani, M
last_name: Jafariyazani
- first_name: A
full_name: Paulino-Afonso, A
last_name: Paulino-Afonso
- first_name: S
full_name: Santos, S
last_name: Santos
- first_name: J
full_name: Calhau, J
last_name: Calhau
citation:
ama: 'Khostovan AA, Sobral D, Mobasher B, et al. The clustering of typical Ly α emitters
from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly
Notices of the Royal Astronomical Society. 2019;489(1):555-573. doi:10.1093/mnras/stz2149'
apa: 'Khostovan, A. A., Sobral, D., Mobasher, B., Matthee, J. J., Cochrane, R. K.,
Chartab, N., … Calhau, J. (2019). The clustering of typical Ly α emitters from
z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices
of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz2149'
chicago: 'Khostovan, A A, D Sobral, B Mobasher, Jorryt J Matthee, R K Cochrane,
N Chartab, M Jafariyazani, A Paulino-Afonso, S Santos, and J Calhau. “The Clustering
of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV
Luminosities.” Monthly Notices of the Royal Astronomical Society. Oxford
University Press, 2019. https://doi.org/10.1093/mnras/stz2149.'
ieee: 'A. A. Khostovan et al., “The clustering of typical Ly α emitters from
z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities,” Monthly Notices
of the Royal Astronomical Society, vol. 489, no. 1. Oxford University Press,
pp. 555–573, 2019.'
ista: 'Khostovan AA, Sobral D, Mobasher B, Matthee JJ, Cochrane RK, Chartab N, Jafariyazani
M, Paulino-Afonso A, Santos S, Calhau J. 2019. The clustering of typical Ly α emitters
from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices
of the Royal Astronomical Society. 489(1), 555–573.'
mla: 'Khostovan, A. A., et al. “The Clustering of Typical Ly α Emitters from z ∼
2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” Monthly Notices
of the Royal Astronomical Society, vol. 489, no. 1, Oxford University Press,
2019, pp. 555–73, doi:10.1093/mnras/stz2149.'
short: A.A. Khostovan, D. Sobral, B. Mobasher, J.J. Matthee, R.K. Cochrane, N. Chartab,
M. Jafariyazani, A. Paulino-Afonso, S. Santos, J. Calhau, Monthly Notices of the
Royal Astronomical Society 489 (2019) 555–573.
date_created: 2022-07-07T13:01:03Z
date_published: 2019-10-01T00:00:00Z
date_updated: 2022-08-19T06:38:42Z
day: '01'
doi: 10.1093/mnras/stz2149
extern: '1'
external_id:
arxiv:
- '1811.00556'
intvolume: ' 489'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: haloes'
- 'galaxies: high-redshift'
- 'galaxies: star formation'
- 'cosmology: observations'
- large-scale structure of Universe
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1811.00556
month: '10'
oa: 1
oa_version: Preprint
page: 555-573
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend
on Ly α and UV luminosities'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 489
year: '2019'
...
---
_id: '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: 2022-08-19T06:42:43Z
day: '01'
doi: 10.1093/mnras/stz030
extern: '1'
external_id:
arxiv:
- '1805.05956'
intvolume: ' 484'
issue: '1'
keyword:
- Space and Planetary Science
- 'Astronomy and Astrophysics : galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: star formation'
- 'cosmology: theory'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1805.05956
month: '03'
oa: 1
oa_version: Preprint
page: 915-932
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The origin of scatter in the star formation rate–stellar mass relation
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 484
year: '2019'
...