---
_id: '11541'
abstract:
- lang: eng
text: We present new Hubble Space Telescope (HST)/WFC3 observations and re-analyse
VLT data to unveil the continuum, variability, and rest-frame ultraviolet (UV)
lines of the multiple UV clumps of the most luminous Lyα emitter at z = 6.6, CR7
(COSMOS Redshift 7). Our re-reduced, flux-calibrated X-SHOOTER spectra of CR7
reveal an He II emission line in observations obtained along the major axis of
Lyα emission with the best seeing conditions. He II is spatially offset by ≈+0.8
arcsec from the peak of Lyα emission, and it is found towards clump B. Our WFC3
grism spectra detects the UV continuum of CR7’s clump A, yielding a power law
with β=−2.5+0.6−0.7 and MUV=−21.87+0.25−0.20. No significant variability is found
for any of the UV clumps on their own, but there is tentative (≈2.2 σ) brightening
of CR7 in F110W as a whole from 2012 to 2017. HST grism data fail to robustly
detect rest-frame UV lines in any of the clumps, implying fluxes ≲2×10−17 erg s−1 cm−2
(3σ). We perform CLOUDY modelling to constrain the metallicity and the ionizing
nature of CR7. CR7 seems to be actively forming stars without any clear active
galactic nucleus activity in clump A, consistent with a metallicity of ∼0.05–0.2 Z⊙.
Component C or an interclump component between B and C may host a high ionization
source. Our results highlight the need for spatially resolved information to study
the formation and assembly of early galaxies.
acknowledgement: We thank the anonymous reviewer for the numerous detailed comments
that led us to greatly improve the quality, extent, and statistical robustness of
this work. DS acknowledges financial support from the Netherlands Organisation for
Scientific research through a Veni fellowship. JM acknowledges the support of a
Huygens PhD fellowship from Leiden University. AF acknowledges support from the
ERC Advanced Grant INTERSTELLAR H2020/740120. BD acknowledges financial support
from NASA through the Astrophysics Data Analysis Program, grant number NNX12AE20G
and the National Science Foundation, grant number 1716907. We are thankful for several
discussions and constructive comments from Johannes Zabl, Eros Vanzella, Bo Milvang-Jensen,
Henry McCracken, Max Gronke, Mark Dijkstra, Richard Ellis, and Nicolas Laporte.
We also thank Umar Burhanudin and Izzy Garland for taking part in the XGAL internship
in Lancaster and for exploring the HST grism data independently. Based on observations
obtained with HST/WFC3 programs 12578, 14495, and 14596. Based on observations of
the National Japanese Observatory with the Suprime-Cam on the Subaru telescope (S14A-086)
on the big island of Hawaii. This work is based in part on data products produced
at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France–Hawaii
Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on data
products from observations made with ESO Telescopes at the La Silla Paranal Observatory
under ESO programme IDs 294.A-5018, 294.A-5039, 092.A 0786, 093.A-0561, 097.A0043,
097.A-0943, 098.A-0819, 298.A-5012, and 179.A-2005, and on data products produced
by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.
The authors acknowledge the award of service time (SW2014b20) on the William Herschel
Telescope (WHT). WHT and its service programme are operated on the island of La
Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos
of the Instituto de Astrofisica de Canarias. This research was supported by the
Munich Institute for Astro- and Particle Physics of the DFG cluster of excellence
‘Origin and Structure of the Universe’. We have benefitted immensely from the public
available programming language PYTHON, including NUMPY and SCIPY (Jones et al. 2001;
Van Der Walt, Colbert & Varoquaux 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy
Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This
research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France.
All data used for this paper are publicly available, and we make all reduced data
available with the refereed paper.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Gabriel
full_name: Brammer, Gabriel
last_name: Brammer
- first_name: Andrea
full_name: Ferrara, Andrea
last_name: Ferrara
- first_name: Lara
full_name: Alegre, Lara
last_name: Alegre
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
- first_name: Daniel
full_name: Schaerer, Daniel
last_name: Schaerer
- first_name: Bahram
full_name: Mobasher, Bahram
last_name: Mobasher
- first_name: Behnam
full_name: Darvish, Behnam
last_name: Darvish
citation:
ama: Sobral D, Matthee JJ, Brammer G, et al. On the nature and physical conditions
of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly
Notices of the Royal Astronomical Society. 2019;482(2):2422-2441. doi:10.1093/mnras/sty2779
apa: Sobral, D., Matthee, J. J., Brammer, G., Ferrara, A., Alegre, L., Röttgering,
H., … Darvish, B. (2019). On the nature and physical conditions of the luminous
Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal
Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty2779
chicago: Sobral, David, Jorryt J Matthee, Gabriel Brammer, Andrea Ferrara, Lara
Alegre, Huub Röttgering, Daniel Schaerer, Bahram Mobasher, and Behnam Darvish.
“On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its
Rest-Frame UV Components.” Monthly Notices of the Royal Astronomical Society.
Oxford University Press, 2019. https://doi.org/10.1093/mnras/sty2779.
ieee: D. Sobral et al., “On the nature and physical conditions of the luminous
Ly α emitter CR7 and its rest-frame UV components,” Monthly Notices of the
Royal Astronomical Society, vol. 482, no. 2. Oxford University Press, pp.
2422–2441, 2019.
ista: Sobral D, Matthee JJ, Brammer G, Ferrara A, Alegre L, Röttgering H, Schaerer
D, Mobasher B, Darvish B. 2019. On the nature and physical conditions of the luminous
Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal
Astronomical Society. 482(2), 2422–2441.
mla: Sobral, David, et al. “On the Nature and Physical Conditions of the Luminous
Ly α Emitter CR7 and Its Rest-Frame UV Components.” Monthly Notices of the
Royal Astronomical Society, vol. 482, no. 2, Oxford University Press, 2019,
pp. 2422–41, doi:10.1093/mnras/sty2779.
short: D. Sobral, J.J. Matthee, G. Brammer, A. Ferrara, L. Alegre, H. Röttgering,
D. Schaerer, B. Mobasher, B. Darvish, Monthly Notices of the Royal Astronomical
Society 482 (2019) 2422–2441.
date_created: 2022-07-08T10:40:05Z
date_published: 2019-01-01T00:00:00Z
date_updated: 2022-08-19T06:49:36Z
day: '01'
doi: 10.1093/mnras/sty2779
extern: '1'
external_id:
arxiv:
- '1710.08422'
intvolume: ' 482'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: ISM'
- 'cosmology: observations'
- dark ages
- reionization
- first stars
- early Universe
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1710.08422
month: '01'
oa: 1
oa_version: Preprint
page: 2422-2441
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: On the nature and physical conditions of the luminous Ly α emitter CR7 and
its rest-frame UV components
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 482
year: '2019'
...
---
_id: '11615'
abstract:
- lang: eng
text: The recently published Kepler mission Data Release 25 (DR25) reported on ∼197 000
targets observed during the mission. Despite this, no wide search for red giants
showing solar-like oscillations have been made across all stars observed in Kepler’s
long-cadence mode. In this work, we perform this task using custom apertures on
the Kepler pixel files and detect oscillations in 21 914 stars, representing the
largest sample of solar-like oscillating stars to date. We measure their frequency
at maximum power, νmax, down to νmax≃4μHz and obtain log (g) estimates with a
typical uncertainty below 0.05 dex, which is superior to typical measurements
from spectroscopy. Additionally, the νmax distribution of our detections show
good agreement with results from a simulated model of the Milky Way, with a ratio
of observed to predicted stars of 0.992 for stars with 10<νmax<270μHz. Among our
red giant detections, we find 909 to be dwarf/subgiant stars whose flux signal
is polluted by a neighbouring giant as a result of using larger photometric apertures
than those used by the NASA Kepler science processing pipeline. We further find
that only 293 of the polluting giants are known Kepler targets. The remainder
comprises over 600 newly identified oscillating red giants, with many expected
to belong to the Galactic halo, serendipitously falling within the Kepler pixel
files of targeted stars.
acknowledgement: Funding for this Discovery mission is provided by NASA’s Science
mission Directorate. We thank the entire Kepler team without whom this investigation
would not be possible. DS is the recipient of an Australian Research Council Future
Fellowship (project number FT1400147). RAG acknowledges the support from CNES. SM
acknowledges support from NASA grant NNX15AF13G, NSF grant AST-1411685, and the
Ramon y Cajal fellowship number RYC-2015-17697. ILC acknowledges scholarship support
from the University of Sydney. We would like to thank Nicholas Barbara and Timothy
Bedding for providing us with a list of variable stars that helped to validate a
number of detections in this study. We also thank the group at the University of
Sydney for fruitful discussions. Finally, we gratefully acknowledge the support
of NVIDIA Corporation with the donation of the Titan Xp GPU used for this research.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Marc
full_name: Hon, Marc
last_name: Hon
- first_name: Dennis
full_name: Stello, Dennis
last_name: Stello
- first_name: Rafael A
full_name: García, Rafael A
last_name: García
- first_name: Savita
full_name: Mathur, Savita
last_name: Mathur
- first_name: Sanjib
full_name: Sharma, Sanjib
last_name: Sharma
- first_name: Isabel L
full_name: Colman, Isabel L
last_name: Colman
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
citation:
ama: Hon M, Stello D, García RA, et al. A search for red giant solar-like oscillations
in all Kepler data. Monthly Notices of the Royal Astronomical Society.
2019;485(4):5616-5630. doi:10.1093/mnras/stz622
apa: Hon, M., Stello, D., García, R. A., Mathur, S., Sharma, S., Colman, I. L.,
& Bugnet, L. A. (2019). A search for red giant solar-like oscillations in
all Kepler data. Monthly Notices of the Royal Astronomical Society. Oxford
University Press. https://doi.org/10.1093/mnras/stz622
chicago: Hon, Marc, Dennis Stello, Rafael A García, Savita Mathur, Sanjib Sharma,
Isabel L Colman, and Lisa Annabelle Bugnet. “A Search for Red Giant Solar-like
Oscillations in All Kepler Data.” Monthly Notices of the Royal Astronomical
Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz622.
ieee: M. Hon et al., “A search for red giant solar-like oscillations in all
Kepler data,” Monthly Notices of the Royal Astronomical Society, vol. 485,
no. 4. Oxford University Press, pp. 5616–5630, 2019.
ista: Hon M, Stello D, García RA, Mathur S, Sharma S, Colman IL, Bugnet LA. 2019.
A search for red giant solar-like oscillations in all Kepler data. Monthly Notices
of the Royal Astronomical Society. 485(4), 5616–5630.
mla: Hon, Marc, et al. “A Search for Red Giant Solar-like Oscillations in All Kepler
Data.” Monthly Notices of the Royal Astronomical Society, vol. 485, no.
4, Oxford University Press, 2019, pp. 5616–30, doi:10.1093/mnras/stz622.
short: M. Hon, D. Stello, R.A. García, S. Mathur, S. Sharma, I.L. Colman, L.A. Bugnet,
Monthly Notices of the Royal Astronomical Society 485 (2019) 5616–5630.
date_created: 2022-07-18T14:26:03Z
date_published: 2019-06-01T00:00:00Z
date_updated: 2022-08-22T07:35:19Z
day: '01'
doi: 10.1093/mnras/stz622
extern: '1'
external_id:
arxiv:
- '1903.00115'
intvolume: ' 485'
issue: '4'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- asteroseismology
- 'methods: data analysis'
- 'techniques: image processing'
- 'stars: oscillations'
- 'stars: statistics'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1903.00115
month: '06'
oa: 1
oa_version: Preprint
page: 5616-5630
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: A search for red giant solar-like oscillations in all Kepler data
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 485
year: '2019'
...
---
_id: '13474'
abstract:
- lang: eng
text: Recent surveys of the Magellanic Clouds have revealed a subtype of Wolf–Rayet
(WR) star with peculiar properties. WN3/O3 spectra exhibit both WR-like emission
and O3 V-like absorption – but at lower luminosity than O3 V or WN stars. We examine
the projected spatial distribution of WN3/O3 stars in the Large Magellanic Cloud
as compared to O-type stars. Surprisingly, WN3/O3 stars are among the most isolated
of all classes of massive stars; they have a distribution similar to red supergiants
dominated by initial masses of 10–15 M⊙, and are far more dispersed than classical
WR stars or luminous blue variables. Their lack of association with clusters of
O-type stars suggests strongly that WN3/O3 stars are not the descendants of single
massive stars (30 M⊙ or above). Instead, they are likely products of interacting
binaries at lower initial mass (10–18 M⊙). Comparison with binary models suggests
a probable origin with primaries in this mass range that were stripped of their
H envelopes through non-conservative mass transfer by a low-mass secondary. We
show that model spectra and positions on the Hertzsprung–Russell diagram for binary-stripped
stars are consistent with WN3/O3 stars. Monitoring radial velocities with high-resolution
spectra can test for low-mass companions or runaway velocities. With lower initial
mass and environments that avoid very massive stars, the WN3/O3 stars fit expectations
for progenitors of Type Ib and possibly Type Ibn supernovae.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Nathan
full_name: Smith, Nathan
last_name: Smith
- 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: Selma E
full_name: de Mink, Selma E
last_name: de Mink
citation:
ama: Smith N, Götberg YLL, de Mink SE. Extreme isolation of WN3/O3 stars and implications
for their evolutionary origin as the elusive stripped binaries. Monthly Notices
of the Royal Astronomical Society. 2018;475(1):772-782. doi:10.1093/mnras/stx3181
apa: Smith, N., Götberg, Y. L. L., & de Mink, S. E. (2018). Extreme isolation
of WN3/O3 stars and implications for their evolutionary origin as the elusive
stripped binaries. Monthly Notices of the Royal Astronomical Society. Oxford
University Press. https://doi.org/10.1093/mnras/stx3181
chicago: Smith, Nathan, Ylva Louise Linsdotter Götberg, and Selma E de Mink. “Extreme
Isolation of WN3/O3 Stars and Implications for Their Evolutionary Origin as the
Elusive Stripped Binaries.” Monthly Notices of the Royal Astronomical Society.
Oxford University Press, 2018. https://doi.org/10.1093/mnras/stx3181.
ieee: N. Smith, Y. L. L. Götberg, and S. E. de Mink, “Extreme isolation of WN3/O3
stars and implications for their evolutionary origin as the elusive stripped binaries,”
Monthly Notices of the Royal Astronomical Society, vol. 475, no. 1. Oxford
University Press, pp. 772–782, 2018.
ista: Smith N, Götberg YLL, de Mink SE. 2018. Extreme isolation of WN3/O3 stars
and implications for their evolutionary origin as the elusive stripped binaries.
Monthly Notices of the Royal Astronomical Society. 475(1), 772–782.
mla: Smith, Nathan, et al. “Extreme Isolation of WN3/O3 Stars and Implications for
Their Evolutionary Origin as the Elusive Stripped Binaries.” Monthly Notices
of the Royal Astronomical Society, vol. 475, no. 1, Oxford University Press,
2018, pp. 772–82, doi:10.1093/mnras/stx3181.
short: N. Smith, Y.L.L. Götberg, S.E. de Mink, Monthly Notices of the Royal Astronomical
Society 475 (2018) 772–782.
date_created: 2023-08-03T10:14:47Z
date_published: 2018-03-01T00:00:00Z
date_updated: 2023-08-09T12:17:34Z
day: '01'
doi: 10.1093/mnras/stx3181
extern: '1'
external_id:
arxiv:
- '1704.03516'
intvolume: ' 475'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/stx3181
month: '03'
oa: 1
oa_version: Published Version
page: 772-782
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: Extreme isolation of WN3/O3 stars and implications for their evolutionary origin
as the elusive stripped binaries
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 475
year: '2018'
...
---
_id: '11549'
abstract:
- lang: eng
text: We investigate the clustering properties of ∼7000 H β + [O III] and [O II]
narrowband-selected emitters at z ∼ 0.8–4.7 from the High-z Emission Line Survey.
We find clustering lengths, r0, of 1.5–4.0 h−1 Mpc and minimum dark matter halo
masses of 1010.7–12.1 M⊙ for our z = 0.8–3.2 H β + [O III] emitters and r0 ∼ 2.0–8.3
h−1 Mpc and halo masses of 1011.5–12.6 M⊙ for our z = 1.5–4.7 [O II] emitters.
We find r0 to strongly increase both with increasing line luminosity and redshift.
By taking into account the evolution of the characteristic line luminosity, L⋆(z),
and using our model predictions of halo mass given r0, we find a strong, redshift-independent
increasing trend between L/L⋆(z) and minimum halo mass. The faintest H β + [O III]
emitters are found to reside in 109.5 M⊙ haloes and the brightest emitters in
1013.0 M⊙ haloes. For [O II] emitters, the faintest emitters are found in 1010.5
M⊙ haloes and the brightest emitters in 1012.6 M⊙ haloes. A redshift-independent
stellar mass dependency is also observed where the halo mass increases from 1011
to 1012.5 M⊙ for stellar masses of 108.5 to 1011.5 M⊙, respectively. We investigate
the interdependencies of these trends by repeating our analysis in a Lline−Mstar
grid space for our most populated samples (H β + [O III] z = 0.84 and [O II] z
= 1.47) and find that the line luminosity dependency is stronger than the stellar
mass dependency on halo mass. For L > L⋆ emitters at all epochs, we find a relatively
flat trend with halo masses of 1012.5–13 M⊙, which may be due to quenching mechanisms
in massive haloes that is consistent with a transitional halo mass predicted by
models.
acknowledgement: We thank the anonymous referee for their useful comments and suggestions
that improved this study. AAK thanks Anahita Alavi and Irene Shivaei for useful
discussion in the making of this paper. AAK acknowledges that this work was supported
by NASA Headquarters under the NASA Earth and Space Science Fellowship Program –
Grant NNX16AO92H. DS acknowledges financial support from the Netherlands Organization
for Scientific Research (NWO) through a Veni fellowship and from Lancaster University
through an Early Career Internal Grant A100679. PNB is grateful for support from
STFC via grant STM001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the
ERC Advanced Grant DUSTYGAL (321334), and a Royal Society/Wolfson Merit award. JM
acknowledges the support of a Huygens PhD fellowship from Leiden University. BD
acknowledges financial support from NASA through the Astrophysics Data Analysis
Program (ADAP), grant number NNX12AE20G.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: A A
full_name: Khostovan, A A
last_name: Khostovan
- first_name: D
full_name: Sobral, D
last_name: Sobral
- first_name: B
full_name: Mobasher, B
last_name: Mobasher
- first_name: P N
full_name: Best, P N
last_name: Best
- first_name: I
full_name: Smail, I
last_name: Smail
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: B
full_name: Darvish, B
last_name: Darvish
- first_name: H
full_name: Nayyeri, H
last_name: Nayyeri
- first_name: S
full_name: Hemmati, S
last_name: Hemmati
- first_name: J P
full_name: Stott, J P
last_name: Stott
citation:
ama: 'Khostovan AA, Sobral D, Mobasher B, et al. The clustering of H β + [O III]
and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar
mass. Monthly Notices of the Royal Astronomical Society. 2018;478(3):2999-3015.
doi:10.1093/mnras/sty925'
apa: 'Khostovan, A. A., Sobral, D., Mobasher, B., Best, P. N., Smail, I., Matthee,
J. J., … Stott, J. P. (2018). The clustering of H β + [O III] and [O II] emitters
since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly Notices
of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty925'
chicago: 'Khostovan, A A, D Sobral, B Mobasher, P N Best, I Smail, Jorryt J Matthee,
B Darvish, H Nayyeri, S Hemmati, and J P Stott. “The Clustering of H β + [O III]
and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar
Mass.” Monthly Notices of the Royal Astronomical Society. Oxford University
Press, 2018. https://doi.org/10.1093/mnras/sty925.'
ieee: 'A. A. Khostovan et al., “The clustering of H β + [O III] and [O II]
emitters since z ∼ 5: Dependencies with line luminosity and stellar mass,” Monthly
Notices of the Royal Astronomical Society, vol. 478, no. 3. Oxford University
Press, pp. 2999–3015, 2018.'
ista: 'Khostovan AA, Sobral D, Mobasher B, Best PN, Smail I, Matthee JJ, Darvish
B, Nayyeri H, Hemmati S, Stott JP. 2018. The clustering of H β + [O III] and [O II]
emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly
Notices of the Royal Astronomical Society. 478(3), 2999–3015.'
mla: 'Khostovan, A. A., et al. “The Clustering of H β + [O III] and [O II] Emitters
since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” Monthly Notices
of the Royal Astronomical Society, vol. 478, no. 3, Oxford University Press,
2018, pp. 2999–3015, doi:10.1093/mnras/sty925.'
short: A.A. Khostovan, D. Sobral, B. Mobasher, P.N. Best, I. Smail, J.J. Matthee,
B. Darvish, H. Nayyeri, S. Hemmati, J.P. Stott, Monthly Notices of the Royal Astronomical
Society 478 (2018) 2999–3015.
date_created: 2022-07-08T11:48:48Z
date_published: 2018-08-01T00:00:00Z
date_updated: 2022-08-19T06:53:39Z
day: '01'
doi: 10.1093/mnras/sty925
extern: '1'
external_id:
arxiv:
- '1705.01101'
intvolume: ' 478'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: haloes'
- 'galaxies: high-redshift'
- 'galaxies: star formation'
- 'cosmology: observations'
- large-scale structure of Universe
language:
- iso: eng
main_file_link:
- url: https://arxiv.org/abs/1705.01101
month: '08'
oa_version: Published Version
page: 2999-3015
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies
with line luminosity and stellar mass'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 478
year: '2018'
...
---
_id: '11555'
abstract:
- lang: eng
text: We investigate the morphology of the [C II] emission in a sample of ‘normal’
star-forming galaxies at 5 < z < 7.2 in relation to their UV (rest-frame) counterpart.
We use new Atacama Large Millimetre/submillimetre Array (ALMA) observations of
galaxies at z ∼ 6–7, as well as a careful re-analysis of archival ALMA data. In
total 29 galaxies were analysed, 21 of which are detected in [C II]. For several
of the latter the [C II] emission breaks into multiple components. Only a fraction
of these [C II] components, if any, is associated with the primary UV systems,
while the bulk of the [C II] emission is associated either with fainter UV components,
or not associated with any UV counterpart at the current limits. By taking into
account the presence of all these components, we find that the L[CII]–SFR (star
formation rate) relation at early epochs is fully consistent with the local relation,
but it has a dispersion of 0.48 ± 0.07 dex, which is about two times larger than
observed locally. We also find that the deviation from the local L[CII]–SFR relation
has a weak anticorrelation with the EW(Ly α). The morphological analysis also
reveals that [C II] emission is generally much more extended than the UV emission.
As a consequence, these primordial galaxies are characterized by a [C II] surface
brightness generally much lower than expected from the local Σ[CII]−ΣSFR relation.
These properties are likely a consequence of a combination of different effects,
namely gas metallicity, [C II] emission from obscured star-forming regions, strong
variations of the ionization parameter, and circumgalactic gas in accretion or
ejected by these primeval galaxies.
acknowledgement: "This paper makes use of the following ALMA data:\r\nADS/JAO.ALMA#2012.1.00719.S,
ADS/JAO.ALMA#2012.A.00040.S,\r\nADS/JAO.ALMA#2013.A.00433.S, ADS/JAO.ALMA#2011.0.00115.S,\r\nADS/JAO.ALMA#2012.1.00033.S,
ADS/JAO.ALMA#2012.1.00523.S,\r\nADS/JAO.ALMA#2013.1.00815.S, ADS/JAO.ALMA#2015.1.00834.S.,\r\nADS/JAO.ALMA#2015.1.01105.S,
AND ADS/JAO.ALMA#2016.1.01240.S\r\nwhich can be retrieved from the ALMA data archive:\r\nhttps://almascience.eso.org/
alma-data/archive. ALMA is a partnership of ESO (representing its member states),
NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan),
in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated
by ESO, AUI/NRAO, and NAOJ. We are grateful to G. Jones to for providing his [C
II] flux maps. RM and SC acknowledge support by the Science and Technology Facilities
Council (STFC). RM acknowledges ERC Advanced Grant 695671 ‘QUENCH’. AF acknowledges
support from the ERC Advanced Grant INTERSTELLAR H2020/740120."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: S
full_name: Carniani, S
last_name: Carniani
- first_name: R
full_name: Maiolino, R
last_name: Maiolino
- first_name: R
full_name: Amorin, R
last_name: Amorin
- first_name: L
full_name: Pentericci, L
last_name: Pentericci
- first_name: A
full_name: Pallottini, A
last_name: Pallottini
- first_name: A
full_name: Ferrara, A
last_name: Ferrara
- first_name: C J
full_name: Willott, C J
last_name: Willott
- first_name: R
full_name: Smit, R
last_name: Smit
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: D
full_name: Sobral, D
last_name: Sobral
- first_name: P
full_name: Santini, P
last_name: Santini
- first_name: M
full_name: Castellano, M
last_name: Castellano
- first_name: S
full_name: De Barros, S
last_name: De Barros
- first_name: A
full_name: Fontana, A
last_name: Fontana
- first_name: A
full_name: Grazian, A
last_name: Grazian
- first_name: L
full_name: Guaita, L
last_name: Guaita
citation:
ama: Carniani S, Maiolino R, Amorin R, et al. Kiloparsec-scale gaseous clumps and
star formation at z = 5–7. Monthly Notices of the Royal Astronomical Society.
2018;478(1):1170-1184. doi:10.1093/mnras/sty1088
apa: Carniani, S., Maiolino, R., Amorin, R., Pentericci, L., Pallottini, A., Ferrara,
A., … Guaita, L. (2018). Kiloparsec-scale gaseous clumps and star formation at
z = 5–7. Monthly Notices of the Royal Astronomical Society. Oxford University
Press. https://doi.org/10.1093/mnras/sty1088
chicago: Carniani, S, R Maiolino, R Amorin, L Pentericci, A Pallottini, A Ferrara,
C J Willott, et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at z = 5–7.”
Monthly Notices of the Royal Astronomical Society. Oxford University Press,
2018. https://doi.org/10.1093/mnras/sty1088.
ieee: S. Carniani et al., “Kiloparsec-scale gaseous clumps and star formation
at z = 5–7,” Monthly Notices of the Royal Astronomical Society, vol. 478,
no. 1. Oxford University Press, pp. 1170–1184, 2018.
ista: Carniani S, Maiolino R, Amorin R, Pentericci L, Pallottini A, Ferrara A, Willott
CJ, Smit R, Matthee JJ, Sobral D, Santini P, Castellano M, De Barros S, Fontana
A, Grazian A, Guaita L. 2018. Kiloparsec-scale gaseous clumps and star formation
at z = 5–7. Monthly Notices of the Royal Astronomical Society. 478(1), 1170–1184.
mla: Carniani, S., et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at
z = 5–7.” Monthly Notices of the Royal Astronomical Society, vol. 478,
no. 1, Oxford University Press, 2018, pp. 1170–84, doi:10.1093/mnras/sty1088.
short: S. Carniani, R. Maiolino, R. Amorin, L. Pentericci, A. Pallottini, A. Ferrara,
C.J. Willott, R. Smit, J.J. Matthee, D. Sobral, P. Santini, M. Castellano, S.
De Barros, A. Fontana, A. Grazian, L. Guaita, Monthly Notices of the Royal Astronomical
Society 478 (2018) 1170–1184.
date_created: 2022-07-11T08:05:42Z
date_published: 2018-07-01T00:00:00Z
date_updated: 2022-08-19T06:58:06Z
day: '01'
doi: 10.1093/mnras/sty1088
extern: '1'
external_id:
arxiv:
- '1712.03985'
intvolume: ' 478'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: ISM'
- 'galaxies: formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1712.03985
month: '07'
oa: 1
oa_version: Preprint
page: 1170-1184
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Kiloparsec-scale gaseous clumps and star formation at z = 5–7
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 478
year: '2018'
...
---
_id: '11557'
abstract:
- lang: eng
text: Deep narrow-band surveys have revealed a large population of faint Ly α emitters
(LAEs) in the distant Universe, but relatively little is known about the most
luminous sources (LLyα≳1042.7 erg s−1; LLyα≳L∗Lyα). Here we present the spectroscopic
follow-up of 21 luminous LAEs at z ∼ 2–3 found with panoramic narrow-band surveys
over five independent extragalactic fields (≈4 × 106 Mpc3 surveyed at z ∼ 2.2
and z ∼ 3.1). We use WHT/ISIS, Keck/DEIMOS, and VLT/X-SHOOTER to study these sources
using high ionization UV lines. Luminous LAEs at z ∼ 2–3 have blue UV slopes (β=−2.0+0.3−0.1)
and high Ly α escape fractions (50+20−15 per cent) and span five orders of magnitude
in UV luminosity (MUV ≈ −19 to −24). Many (70 per cent) show at least one high
ionization rest-frame UV line such as C IV, N V, C III], He II or O III], typically
blue-shifted by ≈100–200 km s−1 relative to Ly α. Their Ly α profiles reveal a
wide variety of shapes, including significant blue-shifted components and widths
from 200 to 4000 km s−1. Overall, 60 ± 11 per cent appear to be active galactic
nucleus (AGN) dominated, and at LLyα > 1043.3 erg s−1 and/or MUV < −21.5 virtually
all LAEs are AGNs with high ionization parameters (log U = 0.6 ± 0.5) and with
metallicities of ≈0.5 − 1 Z⊙. Those lacking signatures of AGNs (40 ± 11 per cent)
have lower ionization parameters (logU=−3.0+1.6−0.9 and log ξion = 25.4 ± 0.2)
and are apparently metal-poor sources likely powered by young, dust-poor ‘maximal’
starbursts. Our results show that luminous LAEs at z ∼ 2–3 are a diverse population
and that 2×L∗Lyα and 2×M∗UV mark a sharp transition in the nature of LAEs, from
star formation dominated to AGN dominated.
acknowledgement: 'We thank the anonymous reviewer for their timely and constructive
comments that greatly helped us to improve the manuscript. DS acknowledges financial
support from the Netherlands Organization for Scientific research (NWO) through
a Veni fellowship and from Lancaster University through an Early Career Internal
Grant A100679. JM acknowledges the support of a Huygens PhD fellowship from Leiden
University. BD acknowledges financial support from NASA through the Astrophysics
Data Analysis Program (ADAP), grant number NNX12AE20G, and the National Science
Foundation, grant number 1716907. IRS acknowledges support from the ERC Advanced
Grant DUSTYGAL (321334), STFC (ST/P000541/1), and a Royal Society/Wolfson Merit
Award. PNB is grateful for support from STFC via grant ST/M001229/1. We thank Anne
Verhamme, Kimihiko Nakajima, Ryan Trainor, Sangeeta Malhotra, Max Gronke, James
Rhoads, Fang Xia An, Matthew Hayes, Takashi Kojima, Mark Dijkstra, and Anne Jaskot
for many helpful and engaging discussions, particularly during the SnowCLAW Ly α
workshop. We thank Bruno Ribeiro, Stephane Charlot, and Joseph Caruana for comments
on the manuscript. The authors would also like to thank Ingrid Tengs, Meg Singleton,
Ali Khostovan, and Sara Perez for participating in part of the observations. We
also thank Joao Calhau, Leah Morabito, Sergio Santos, and Aayush Saxena for their
assistance with the narrow-band observations which allowed to select some of the
sour ces. Based on observations obtained with the William Herschel Telescope, program:
W16AN004; the Very Large Telescope, programs: 098.A-0819 & 099.A-0254; and the Keck
II telescope, program: C267D. Based on data products from observations made with
ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018,
294.A-5039, 092.A-0786, 093.A-0561, 097.A-0943, 098.A-0819, 099.A-0254 and 179.A-2005.
The authors acknowledge the award of service time (SW2014b20) on the WHT. WHT and
its service programme are operated on the island of La Palma by the Isaac Newton
Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de
Astrofisica de Canarias. The authors would also like to thank all the extremely
helpful observatory staff that have greatly contributed towards our observations,
particularly Fiona Riddick, Lilian Dominguez, Florencia Jimenez, and Ian Skillen.
We have benefited greatly from the publicly available programming language PYTHON,
including the NUMPY & SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al.
2001), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and
the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR
catalogue access tool, CDS, Strasbourg, France.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Behnam
full_name: Darvish, Behnam
last_name: Darvish
- first_name: Ian
full_name: Smail, Ian
last_name: Smail
- first_name: Philip N
full_name: Best, Philip N
last_name: Best
- first_name: Lara
full_name: Alegre, Lara
last_name: Alegre
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
- first_name: Bahram
full_name: Mobasher, Bahram
last_name: Mobasher
- first_name: Ana
full_name: Paulino-Afonso, Ana
last_name: Paulino-Afonso
- first_name: Andra
full_name: Stroe, Andra
last_name: Stroe
- first_name: Iván
full_name: Oteo, Iván
last_name: Oteo
citation:
ama: 'Sobral D, Matthee JJ, Darvish B, et al. The nature of luminous Ly α emitters
at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly Notices
of the Royal Astronomical Society. 2018;477(2):2817-2840. doi:10.1093/mnras/sty782'
apa: 'Sobral, D., Matthee, J. J., Darvish, B., Smail, I., Best, P. N., Alegre, L.,
… Oteo, I. (2018). The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor
starbursts and highly ionizing AGN. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/sty782'
chicago: 'Sobral, David, Jorryt J Matthee, Behnam Darvish, Ian Smail, Philip N Best,
Lara Alegre, Huub Röttgering, et al. “The Nature of Luminous Ly α Emitters at
z ∼ 2–3: Maximal Dust-Poor Starbursts and Highly Ionizing AGN.” Monthly Notices
of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty782.'
ieee: 'D. Sobral et al., “The nature of luminous Ly α emitters at z ∼ 2–3:
Maximal dust-poor starbursts and highly ionizing AGN,” Monthly Notices of the
Royal Astronomical Society, vol. 477, no. 2. Oxford University Press, pp.
2817–2840, 2018.'
ista: 'Sobral D, Matthee JJ, Darvish B, Smail I, Best PN, Alegre L, Röttgering H,
Mobasher B, Paulino-Afonso A, Stroe A, Oteo I. 2018. The nature of luminous Ly
α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly
Notices of the Royal Astronomical Society. 477(2), 2817–2840.'
mla: 'Sobral, David, et al. “The Nature of Luminous Ly α Emitters at z ∼ 2–3: Maximal
Dust-Poor Starbursts and Highly Ionizing AGN.” Monthly Notices of the Royal
Astronomical Society, vol. 477, no. 2, Oxford University Press, 2018, pp.
2817–40, doi:10.1093/mnras/sty782.'
short: D. Sobral, J.J. Matthee, B. Darvish, I. Smail, P.N. Best, L. Alegre, H. Röttgering,
B. Mobasher, A. Paulino-Afonso, A. Stroe, I. Oteo, Monthly Notices of the Royal
Astronomical Society 477 (2018) 2817–2840.
date_created: 2022-07-12T07:18:02Z
date_published: 2018-06-01T00:00:00Z
date_updated: 2022-08-19T07:01:08Z
day: '01'
doi: 10.1093/mnras/sty782
extern: '1'
external_id:
arxiv:
- '1802.10102'
intvolume: ' 477'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: active'
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: ISM'
- 'galaxies: starburst'
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1802.10102
month: '06'
oa: 1
oa_version: Preprint
page: 2817-2840
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts
and highly ionizing AGN'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 477
year: '2018'
...
---
_id: '11558'
abstract:
- lang: eng
text: We present and explore deep narrow- and medium-band data obtained with the
Subaru and the Isaac Newton Telescopes in the ∼2 deg2 COSMOS field. We use these
data as an extremely wide, low-resolution (R ∼ 20–80) Integral Field Unit survey
to slice through the COSMOS field and obtain a large sample of ∼4000 Ly α emitters
(LAEs) from z ∼ 2 to 6 in 16 redshift slices (SC4K). We present new Ly α luminosity
functions (LFs) covering a comoving volume of ∼108 Mpc3. SC4K extensively complements
ultradeep surveys, jointly covering over 4 dex in Ly α luminosity and revealing
a global (2.5 < z < 6) synergy LF with α=−1.93+0.12−0.12, log10Φ∗Lyα=−3.45+0.22−0.29 Mpc−3,
and log10L∗Lyα=42.93+0.15−0.11 erg s−1. The Schechter component of the Ly α LF
reveals a factor ∼5 rise in L∗Lyα and a ∼7 × decline in Φ∗Lyα from z ∼ 2 to 6.
The data reveal an extra power-law (or Schechter) component above LLy α ≈ 1043.3 erg s−1
at z ∼ 2.2–3.5 and we show that it is partially driven by X-ray and radio active
galactic nucleus (AGN), as their Ly α LF resembles the excess. The power-law component
vanishes and/or is below our detection limits above z > 3.5, likely linked with
the evolution of the AGN population. The Ly α luminosity density rises by a factor
∼2 from z ∼ 2 to 3 but is then found to be roughly constant (1.1+0.2−0.2×1040 erg s−1 Mpc−3)
to z ∼ 6, despite the ∼0.7 dex drop in ultraviolet (UV) luminosity density. The
Ly α/UV luminosity density ratio rises from 4 ± 1 per cent to 30 ± 6 per cent
from z ∼ 2.2 to 6. Our results imply a rise of a factor of ≈2 in the global ionization
efficiency (ξion) and a factor ≈4 ± 1 in the Ly α escape fraction from z ∼ 2 to
6, hinting for evolution in both the typical burstiness/stellar populations and
even more so in the typical interstellar medium conditions allowing Ly α photons
to escape.
acknowledgement: "We thank the anonymous referee for their constructive comments that
helped us improve the manuscript. DS acknowledges the hospitality of the IAC and
a Severo Ochoa visiting grant. SS and JC acknowledge studentships from the Lancaster
University. JM acknowledges a Huygens PhD fellowship from Leiden University. APA
acknowledges financial support from the Science and Technology Foundation (FCT,
Portugal) through research grants UID/FIS/04434/2013 and fellowship PD/BD/52706/2014.
The authors thank Alyssa Drake, Kimihiko Nakajima, Yuichi Harikane, Max Gronke,
Irene Shivaei, Helmut Dannerbauer, Huub Rottgering, ¨ Marius Eide, and Masami Ouchi
for many engaging and stimulating discussions. We also thank Sara Perez, Alex Bennett,
and Tom Rose for their involvement in the early stages of this project. Based on
data products from observations made with European Southern Observatory (ESO) Telescopes
at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 097.A 0943,\r\n098.A-0819,
099.A-0254, and 179.A-2005 and on data products produced by TERAPIX and the Cambridge
Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations
using the WFC on the 2.5 m INT, as part of programmes 2013AN002, 2013BN008, 2014AC88,
2014AN002, 2014BN006, 2014BC118, and 2016AN001. The INT is operated on the island
of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los
Muchachos of the Instituto de Astrofisica de Canarias. This work is based in part
on data products produced at TERAPIX available at the Canadian Astronomy Data Centre
as part of the Canada–France– Hawaii Telescope Legacy Survey (CFHTLS), a collaborative
project of NRC and CNRS.\r\nWe are grateful to the CFHTLS, COSMOS-UltraVISTA, and
COSMOS survey teams. We are also unmeasurably thankful to the pioneering and continuous
work from previous Ly α surveys’ teams. Without these previous Ly α and the wider
reach legacy surveys, this research would have been impossible. We also thank the
VUDS team for making available spectroscopic redshifts from data obtained with VIMOS
at the European Southern Observatory Very Large Telescope, Paranal, Chile, under
Large Programme 185.A-0791. Finally, the authors acknowledge the unique value of
the publicly available programming language PYTHON, including the NUMPY and SCIPY
(Van Der Walt, Colbert & Varoquaux 2011; Jones et al. 2001), MATPLOTLIB (Hunter
2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program
(Taylor 2005). We publicly release a catalogue with all LAEs used in this paper
(SC4K), so it can be freely explored by the community (see five example entries
in Table A1)."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Sérgio
full_name: Santos, Sérgio
last_name: Santos
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Ana
full_name: Paulino-Afonso, Ana
last_name: Paulino-Afonso
- first_name: Bruno
full_name: Ribeiro, Bruno
last_name: Ribeiro
- first_name: João
full_name: Calhau, João
last_name: Calhau
- first_name: Ali A
full_name: Khostovan, Ali A
last_name: Khostovan
citation:
ama: 'Sobral D, Santos S, Matthee JJ, et al. Slicing COSMOS with SC4K: The evolution
of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly
Notices of the Royal Astronomical Society. 2018;476(4):4725-4752. doi:10.1093/mnras/sty378'
apa: 'Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Ribeiro, B., Calhau,
J., & Khostovan, A. A. (2018). Slicing COSMOS with SC4K: The evolution of
typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly
Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty378'
chicago: 'Sobral, David, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso, Bruno
Ribeiro, João Calhau, and Ali A Khostovan. “Slicing COSMOS with SC4K: The Evolution
of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” Monthly
Notices of the Royal Astronomical Society. Oxford University Press, 2018.
https://doi.org/10.1093/mnras/sty378.'
ieee: 'D. Sobral et al., “Slicing COSMOS with SC4K: The evolution of typical
Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6,” Monthly Notices
of the Royal Astronomical Society, vol. 476, no. 4. Oxford University Press,
pp. 4725–4752, 2018.'
ista: 'Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Ribeiro B, Calhau J, Khostovan
AA. 2018. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and
the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical
Society. 476(4), 4725–4752.'
mla: 'Sobral, David, et al. “Slicing COSMOS with SC4K: The Evolution of Typical
Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” Monthly Notices
of the Royal Astronomical Society, vol. 476, no. 4, Oxford University Press,
2018, pp. 4725–52, doi:10.1093/mnras/sty378.'
short: D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, B. Ribeiro, J. Calhau,
A.A. Khostovan, Monthly Notices of the Royal Astronomical Society 476 (2018) 4725–4752.
date_created: 2022-07-12T10:41:08Z
date_published: 2018-06-01T00:00:00Z
date_updated: 2022-08-19T07:04:45Z
day: '01'
doi: 10.1093/mnras/sty378
extern: '1'
external_id:
arxiv:
- '1712.04451'
intvolume: ' 476'
issue: '4'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: high-redshift'
- 'galaxies: luminosity function'
- mass function
- 'galaxies: statistics'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1712.04451
month: '06'
oa: 1
oa_version: Preprint
page: 4725-4752
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α
escape fraction from z ∼ 2 to 6'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 476
year: '2018'
...
---
_id: '11620'
abstract:
- lang: eng
text: We report the discovery and characterization of HD 89345b (K2-234b; EPIC 248777106b),
a Saturn-sized planet orbiting a slightly evolved star. HD 89345 is a bright star
(V = 9.3 mag) observed by the K2 mission with 1 min time sampling. It exhibits
solar-like oscillations. We conducted asteroseismology to determine the parameters
of the star, finding the mass and radius to be 1.12+0.04−0.01M⊙ and 1.657+0.020−0.004R⊙,
respectively. The star appears to have recently left the main sequence, based
on the inferred age, 9.4+0.4−1.3Gyr, and the non-detection of mixed modes. The
star hosts a ‘warm Saturn’ (P = 11.8 d, Rp = 6.86 ± 0.14 R⊕). Radial-velocity
follow-up observations performed with the FIbre-fed Echelle Spectrograph, HARPS,
and HARPS-N spectrographs show that the planet has a mass of 35.7 ± 3.3 M⊕. The
data also show that the planet’s orbit is eccentric (e ≈ 0.2). An investigation
of the rotational splitting of the oscillation frequencies of the star yields
no conclusive evidence on the stellar inclination angle. We further obtained Rossiter–McLaughlin
observations, which result in a broad posterior of the stellar obliquity. The
planet seems to confirm to the same patterns that have been observed for other
sub-Saturns regarding planet mass and multiplicity, orbital eccentricity, and
stellar metallicity.
acknowledgement: 'We gratefully acknowledge many helpful suggestions by the anonymous
referee. Based on observations made with a) the Nordic Optical Telescope, operated
by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque
de los Muchachos; b) the ESO-3.6m telescope at La Silla Observatory under programme
ID 0100.C-0808; c) the Italian Telescopio Nazionale Galileo operated on the island
of La Palma by the Fundación Galileo Galilei of the Istituto Nazionale di Astrofisica.
NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research
Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott,
Elliott P. Horch, and Emmett Quigley. This project has received funding from the
European Union’s Horizon 2020 research and innovation programme under grant agreement
No 730890. This material reflects only the authors views and the Commission is not
liable for any use that may be made of the information contained therein. DG gratefully
acknowledges the financial support of the Programma Giovani Ricercatori – Rita Levi
Montalcini – Rientro dei Cervelli (2012) awarded by the Italian Ministry of Education,
Universities and Research (MIUR). SaM would like to acknowledge support from the
Ramon y Cajal fellowship number RYC-2015-17697. AJ, MH, and SA acknowledge support
by the Danish Council for Independent Research, through a DFF Sapere Aude Starting
Grant nr. 4181-00487B. SzCs, APH, MP, and HR acknowledge the support of the DFG
priority program SPP 1992Exploring the Diversity of Extrasolar Planets (grants HA
3279/12-1, PA 525/18-1, PA5 25/19-1 and PA525/20-1, RA 714/14-1) HD, CR, and FPH
acknowledge the financial support from MINECO under grants ESP2015-65712-C5-4-R
and AYA2016-76378-P. This paper has made use of the IAC Supercomputing facility
HTCondor (http://research.cs.wisc.edu/htcondor/), partly financed by the Ministry
of Economy and Competitiveness with FEDER funds, code IACA13-3E-2493. MF and CMP
gratefully acknowledge the support of the Swedish National Space Board. RAG and
StM thanks the support of the CNES PLATO grant. PGB is a postdoctoral fellow in
the MINECO-programme ’Juan de la Cierva Incorporacion’ (IJCI-2015-26034). StM acknowledges
support from ERC through SPIRE grant (647383) and from ISSI through the ENCELADE
2.0 team. VSA acknowledges support from VILLUM FONDEN (research grant 10118). MNL
acknowledges support from the ESA-PRODEX programme. Funding for the Stellar Astrophysics
Centre is provided by The Danish National Research Foundation (Grant agreement no.:
DNRF106) This work has made use of data from the European Space Agency (ESA) mission
Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and
Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).
Funding for the DPAC has been provided by national institutions, in particular the
institutions participating in the Gaia Multilateral Agreement. This research was
made with the use of NASA’s Astrophysics Data System and the NASA Exoplanet Archive,
which is operated by the California Institute of Technology, under contract with
the National Aeronautics and Space Administration under the Exoplanet Exploration
Program.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: V
full_name: Van Eylen, V
last_name: Van Eylen
- first_name: F
full_name: Dai, F
last_name: Dai
- first_name: S
full_name: Mathur, S
last_name: Mathur
- first_name: D
full_name: Gandolfi, D
last_name: Gandolfi
- first_name: S
full_name: Albrecht, S
last_name: Albrecht
- first_name: M
full_name: Fridlund, M
last_name: Fridlund
- first_name: R A
full_name: García, R A
last_name: García
- first_name: E
full_name: Guenther, E
last_name: Guenther
- first_name: M
full_name: Hjorth, M
last_name: Hjorth
- first_name: A B
full_name: Justesen, A B
last_name: Justesen
- first_name: J
full_name: Livingston, J
last_name: Livingston
- first_name: M N
full_name: Lund, M N
last_name: Lund
- first_name: F
full_name: Pérez Hernández, F
last_name: Pérez Hernández
- first_name: J
full_name: Prieto-Arranz, J
last_name: Prieto-Arranz
- first_name: C
full_name: Regulo, C
last_name: Regulo
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
- first_name: M E
full_name: Everett, M E
last_name: Everett
- first_name: T
full_name: Hirano, T
last_name: Hirano
- first_name: D
full_name: Nespral, D
last_name: Nespral
- first_name: G
full_name: Nowak, G
last_name: Nowak
- first_name: E
full_name: Palle, E
last_name: Palle
- first_name: V
full_name: Silva Aguirre, V
last_name: Silva Aguirre
- first_name: T
full_name: Trifonov, T
last_name: Trifonov
- first_name: J N
full_name: Winn, J N
last_name: Winn
- first_name: O
full_name: Barragán, O
last_name: Barragán
- first_name: P G
full_name: Beck, P G
last_name: Beck
- first_name: W J
full_name: Chaplin, W J
last_name: Chaplin
- first_name: W D
full_name: Cochran, W D
last_name: Cochran
- first_name: S
full_name: Csizmadia, S
last_name: Csizmadia
- first_name: H
full_name: Deeg, H
last_name: Deeg
- first_name: M
full_name: Endl, M
last_name: Endl
- first_name: P
full_name: Heeren, P
last_name: Heeren
- first_name: S
full_name: Grziwa, S
last_name: Grziwa
- first_name: A P
full_name: Hatzes, A P
last_name: Hatzes
- first_name: D
full_name: Hidalgo, D
last_name: Hidalgo
- first_name: J
full_name: Korth, J
last_name: Korth
- first_name: S
full_name: Mathis, S
last_name: Mathis
- first_name: P
full_name: Montañes Rodriguez, P
last_name: Montañes Rodriguez
- first_name: N
full_name: Narita, N
last_name: Narita
- first_name: M
full_name: Patzold, M
last_name: Patzold
- first_name: C M
full_name: Persson, C M
last_name: Persson
- first_name: F
full_name: Rodler, F
last_name: Rodler
- first_name: A M S
full_name: Smith, A M S
last_name: Smith
citation:
ama: 'Van Eylen V, Dai F, Mathur S, et al. HD 89345: A bright oscillating star hosting
a transiting warm Saturn-sized planet observed by K2. Monthly Notices of the
Royal Astronomical Society. 2018;478(4):4866-4880. doi:10.1093/mnras/sty1390'
apa: 'Van Eylen, V., Dai, F., Mathur, S., Gandolfi, D., Albrecht, S., Fridlund,
M., … Smith, A. M. S. (2018). HD 89345: A bright oscillating star hosting a transiting
warm Saturn-sized planet observed by K2. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/sty1390'
chicago: 'Van Eylen, V, F Dai, S Mathur, D Gandolfi, S Albrecht, M Fridlund, R A
García, et al. “HD 89345: A Bright Oscillating Star Hosting a Transiting Warm
Saturn-Sized Planet Observed by K2.” Monthly Notices of the Royal Astronomical
Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty1390.'
ieee: 'V. Van Eylen et al., “HD 89345: A bright oscillating star hosting
a transiting warm Saturn-sized planet observed by K2,” Monthly Notices of the
Royal Astronomical Society, vol. 478, no. 4. Oxford University Press, pp.
4866–4880, 2018.'
ista: 'Van Eylen V, Dai F, Mathur S, Gandolfi D, Albrecht S, Fridlund M, García
RA, Guenther E, Hjorth M, Justesen AB, Livingston J, Lund MN, Pérez Hernández
F, Prieto-Arranz J, Regulo C, Bugnet LA, Everett ME, Hirano T, Nespral D, Nowak
G, Palle E, Silva Aguirre V, Trifonov T, Winn JN, Barragán O, Beck PG, Chaplin
WJ, Cochran WD, Csizmadia S, Deeg H, Endl M, Heeren P, Grziwa S, Hatzes AP, Hidalgo
D, Korth J, Mathis S, Montañes Rodriguez P, Narita N, Patzold M, Persson CM, Rodler
F, Smith AMS. 2018. HD 89345: A bright oscillating star hosting a transiting warm
Saturn-sized planet observed by K2. Monthly Notices of the Royal Astronomical
Society. 478(4), 4866–4880.'
mla: 'Van Eylen, V., et al. “HD 89345: A Bright Oscillating Star Hosting a Transiting
Warm Saturn-Sized Planet Observed by K2.” Monthly Notices of the Royal Astronomical
Society, vol. 478, no. 4, Oxford University Press, 2018, pp. 4866–80, doi:10.1093/mnras/sty1390.'
short: V. Van Eylen, F. Dai, S. Mathur, D. Gandolfi, S. Albrecht, M. Fridlund, R.A.
García, E. Guenther, M. Hjorth, A.B. Justesen, J. Livingston, M.N. Lund, F. Pérez Hernández,
J. Prieto-Arranz, C. Regulo, L.A. Bugnet, M.E. Everett, T. Hirano, D. Nespral,
G. Nowak, E. Palle, V. Silva Aguirre, T. Trifonov, J.N. Winn, O. Barragán, P.G.
Beck, W.J. Chaplin, W.D. Cochran, S. Csizmadia, H. Deeg, M. Endl, P. Heeren, S.
Grziwa, A.P. Hatzes, D. Hidalgo, J. Korth, S. Mathis, P. Montañes Rodriguez, N.
Narita, M. Patzold, C.M. Persson, F. Rodler, A.M.S. Smith, Monthly Notices of
the Royal Astronomical Society 478 (2018) 4866–4880.
date_created: 2022-07-18T14:43:17Z
date_published: 2018-08-01T00:00:00Z
date_updated: 2022-08-22T07:45:38Z
day: '01'
doi: 10.1093/mnras/sty1390
extern: '1'
external_id:
arxiv:
- '1805.01860'
intvolume: ' 478'
issue: '4'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- asteroseismology
- 'planets and satellites: composition'
- 'planets and satellites: formation'
- 'planets and satellites: fundamental parameters'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1805.01860
month: '08'
oa: 1
oa_version: Preprint
page: 4866-4880
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: 'HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized
planet observed by K2'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 478
year: '2018'
...
---
_id: '11562'
abstract:
- lang: eng
text: We present the CAlibrating LYMan-α with Hα (CALYMHA) pilot survey and new
results on Lyman α (Lyα) selected galaxies at z ∼ 2. We use a custom-built Lyα
narrow-band filter at the Isaac Newton Telescope, designed to provide a matched
volume coverage to the z = 2.23 Hα HiZELS survey. Here, we present the first results
for the COSMOS and UDS fields. Our survey currently reaches a 3σ line flux limit
of ∼4 × 10−17 erg s−1 cm−2, and a Lyα luminosity limit of ∼1042.3 erg s−1. We
find 188 Lyα emitters over 7.3 × 105 Mpc3, but also find significant numbers of
other line-emitting sources corresponding to He II, C III] and C IV emission lines.
These sources are important contaminants, and we carefully remove them, unlike
most previous studies. We find that the Lyα luminosity function at z = 2.23 is
very well described by a Schechter function up to LLy α ≈ 1043 erg s−1 with L∗=1042.59+0.16−0.08
erg s−1, ϕ∗=10−3.09+0.14−0.34 Mpc−3 and α = −1.75 ± 0.25. Above LLy α ≈ 1043 erg
s−1, the Lyα luminosity function becomes power-law like, driven by X-ray AGN.
We find that Lyα-selected emitters have a high escape fraction of 37 ± 7 per cent,
anticorrelated with Lyα luminosity and correlated with Lyα equivalent width. Lyα
emitters have ubiquitous large (≈40 kpc) Lyα haloes, ∼2 times larger than their
Hα extents. By directly comparing our Lyα and Hα luminosity functions, we find
that the global/overall escape fraction of Lyα photons (within a 13 kpc radius)
from the full population of star-forming galaxies is 5.1 ± 0.2 per cent at the
peak of the star formation history. An extra 3.3 ± 0.3 per cent of Lyα photons
likely still escape, but at larger radii.
acknowledgement: 'We thank the reviewer for his/her helpful comments and suggestions
that have greatly improved this work. DS and JM acknowledge financial support from
the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship.
DS also acknowledges funding from FCT through an FCT Investigator Starting Grant
and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from
the UK STFC via grant ST/M001229/1. IRS acknowledges support from STFC (ST/L00075X/1),
the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson
merit award. We thank Matthew Hayes, Ryan Trainor, Kimihiko Nakajima and Anne Verhamme
for many helpful discussions and Ana Sobral, Carolina Duarte and Miguel Domingos
for taking part in observations with the NB392 filter. We also thank Sergio Santos
for helpful comments. This research is based on observations obtained on the Isaac
Newton Telescope (INT), programs: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B
& I15AN008. The authors acknowledge the award of time from programmes: I13AN002,
I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008 on the INT. INT is operated
on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio
del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on
observations made with ESO Telescopes at the La Silla Paranal Observatory under
programme ID 098.A 0819. We have benefited greatly from the publicly available programming
language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages,
the astronomical imaging tools SEXTRACTOR, SWARP (Bertin & Arnouts 1996; Bertin
2010), SCAMP (Bertin 2006) and TOPCAT (Taylor 2005). Dedicated to the memory of
M. L. Nicolau and M. C. Serrano.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Philip
full_name: Best, Philip
last_name: Best
- first_name: Andra
full_name: Stroe, Andra
last_name: Stroe
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
- first_name: Iván
full_name: Oteo, Iván
last_name: Oteo
- first_name: Ian
full_name: Smail, Ian
last_name: Smail
- first_name: Leah
full_name: Morabito, Leah
last_name: Morabito
- first_name: Ana
full_name: Paulino-Afonso, Ana
last_name: Paulino-Afonso
citation:
ama: 'Sobral D, Matthee JJ, Best P, et al. The CALYMHA survey: Lyα luminosity function
and global escape fraction of Lyα photons at z = 2.23. Monthly Notices of the
Royal Astronomical Society. 2017;466(1):1242-1258. doi:10.1093/mnras/stw3090'
apa: 'Sobral, D., Matthee, J. J., Best, P., Stroe, A., Röttgering, H., Oteo, I.,
… Paulino-Afonso, A. (2017). The CALYMHA survey: Lyα luminosity function and global
escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stw3090'
chicago: 'Sobral, David, Jorryt J Matthee, Philip Best, Andra Stroe, Huub Röttgering,
Iván Oteo, Ian Smail, Leah Morabito, and Ana Paulino-Afonso. “The CALYMHA Survey:
Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.”
Monthly Notices of the Royal Astronomical Society. Oxford University Press,
2017. https://doi.org/10.1093/mnras/stw3090.'
ieee: 'D. Sobral et al., “The CALYMHA survey: Lyα luminosity function and
global escape fraction of Lyα photons at z = 2.23,” Monthly Notices of the
Royal Astronomical Society, vol. 466, no. 1. Oxford University Press, pp.
1242–1258, 2017.'
ista: 'Sobral D, Matthee JJ, Best P, Stroe A, Röttgering H, Oteo I, Smail I, Morabito
L, Paulino-Afonso A. 2017. The CALYMHA survey: Lyα luminosity function and global
escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical
Society. 466(1), 1242–1258.'
mla: 'Sobral, David, et al. “The CALYMHA Survey: Lyα Luminosity Function and Global
Escape Fraction of Lyα Photons at z = 2.23.” Monthly Notices of the Royal Astronomical
Society, vol. 466, no. 1, Oxford University Press, 2017, pp. 1242–58, doi:10.1093/mnras/stw3090.'
short: D. Sobral, J.J. Matthee, P. Best, A. Stroe, H. Röttgering, I. Oteo, I. Smail,
L. Morabito, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society
466 (2017) 1242–1258.
date_created: 2022-07-12T12:04:16Z
date_published: 2017-04-01T00:00:00Z
date_updated: 2022-08-19T07:18:20Z
day: '01'
doi: 10.1093/mnras/stw3090
extern: '1'
external_id:
arxiv:
- '1609.05897'
intvolume: ' 466'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: haloes'
- 'galaxies: high-redshift'
- 'galaxies: luminosity function'
- mass function
- 'galaxies: statistics'
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1609.05897
month: '04'
oa: 1
oa_version: Preprint
page: 1242-1258
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The CALYMHA survey: Lyα luminosity function and global escape fraction of
Lyα photons at z = 2.23'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 466
year: '2017'
...
---
_id: '11564'
abstract:
- lang: eng
text: We study the production rate of ionizing photons of a sample of 588 Hα emitters
(HAEs) and 160 Lyman-α emitters (LAEs) at z = 2.2 in the COSMOS field in order
to assess the implied emissivity from galaxies, based on their ultraviolet (UV)
luminosity. By exploring the rest-frame Lyman Continuum (LyC) with GALEX/NUV data,
we find fesc < 2.8 (6.4) per cent through median (mean) stacking. By combining
the Hα luminosity density with intergalactic medium emissivity measurements from
absorption studies, we find a globally averaged 〈fesc〉 of 5.9+14.5−4.2 per cent
at z = 2.2 if we assume HAEs are the only source of ionizing photons. We find
similarly low values of the global 〈fesc〉 at z ≈ 3–5, also ruling out a high 〈fesc〉
at z < 5. These low escape fractions allow us to measure ξion, the number of produced
ionizing photons per unit UV luminosity, and investigate how this depends on galaxy
properties. We find a typical ξion ≈ 1024.77 ± 0.04 Hz erg−1 for HAEs and ξion
≈ 1025.14 ± 0.09 Hz erg−1 for LAEs. LAEs and low-mass HAEs at z = 2.2 show similar
values of ξion as typically assumed in the reionization era, while the typical
HAE is three times less ionizing. Due to an increasing ξion with increasing EW(Hα),
ξion likely increases with redshift. This evolution alone is fully in line with
the observed evolution of ξion between z ≈ 2 and 5, indicating a typical value
of ξion ≈ 1025.4 Hz erg−1 in the reionization era.
acknowledgement: "We thank the referee for the many helpful and constructive comments
which have significantly improved this paper. JM acknowledges the support of a Huygens
PhD fellowship from Leiden University. DS acknowledges financial support from the
Netherlands Organization for Scientific research (NWO) through a Veni fellowship
and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010).
PNB is grateful for support from the UK STFC via grant ST/M001229/1. IO acknowledges
support from the European Research Council in the form of the Advanced Investigator
Programme, 321302, COSMICISM. The authors thank Andreas Faisst, Michael Rutkowski
and Andreas Sandberg for answering questions related to this work and Daniel Schaerer
and Mark Dijkstra for discussions. We acknowledge the work that has been done by
both the COSMOS team in assembling such large, state-of-the-art multi-wavelength
data set, as this has been crucial for the results presented in this paper. We have
benefited greatly from the public available programming language PYTHON, including
the NUMPY, MATPLOTLIB, PYFITS, SCIPY (Jones et al. 2001; Hunter 2007; Van Der Walt,
Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration et al. 2013) packages,
the astronomical imaging tools SEXTRACTOR and SWARP (Bertin & Arnouts 1996;\r\nBertin
2010) and the TOPCAT analysis program (Taylor 2013)."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Philip
full_name: Best, Philip
last_name: Best
- first_name: Ali Ahmad
full_name: Khostovan, Ali Ahmad
last_name: Khostovan
- first_name: Iván
full_name: Oteo, Iván
last_name: Oteo
- first_name: Rychard
full_name: Bouwens, Rychard
last_name: Bouwens
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
citation:
ama: Matthee JJ, Sobral D, Best P, et al. The production and escape of Lyman-Continuum
radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. Monthly
Notices of the Royal Astronomical Society. 2017;465(3):3637-3655. doi:10.1093/mnras/stw2973
apa: Matthee, J. J., Sobral, D., Best, P., Khostovan, A. A., Oteo, I., Bouwens,
R., & Röttgering, H. (2017). The production and escape of Lyman-Continuum
radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. Monthly
Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw2973
chicago: Matthee, Jorryt J, David Sobral, Philip Best, Ali Ahmad Khostovan, Iván
Oteo, Rychard Bouwens, and Huub Röttgering. “The Production and Escape of Lyman-Continuum
Radiation from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” Monthly
Notices of the Royal Astronomical Society. Oxford University Press, 2017.
https://doi.org/10.1093/mnras/stw2973.
ieee: J. J. Matthee et al., “The production and escape of Lyman-Continuum
radiation from star-forming galaxies at z ∼ 2 and their redshift evolution,” Monthly
Notices of the Royal Astronomical Society, vol. 465, no. 3. Oxford University
Press, pp. 3637–3655, 2017.
ista: Matthee JJ, Sobral D, Best P, Khostovan AA, Oteo I, Bouwens R, Röttgering
H. 2017. The production and escape of Lyman-Continuum radiation from star-forming
galaxies at z ∼ 2 and their redshift evolution. Monthly Notices of the Royal Astronomical
Society. 465(3), 3637–3655.
mla: Matthee, Jorryt J., et al. “The Production and Escape of Lyman-Continuum Radiation
from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” Monthly
Notices of the Royal Astronomical Society, vol. 465, no. 3, Oxford University
Press, 2017, pp. 3637–55, doi:10.1093/mnras/stw2973.
short: J.J. Matthee, D. Sobral, P. Best, A.A. Khostovan, I. Oteo, R. Bouwens, H.
Röttgering, Monthly Notices of the Royal Astronomical Society 465 (2017) 3637–3655.
date_created: 2022-07-12T12:12:14Z
date_published: 2017-03-01T00:00:00Z
date_updated: 2022-08-19T07:53:04Z
day: '01'
doi: 10.1093/mnras/stw2973
extern: '1'
external_id:
arxiv:
- '1605.08782'
intvolume: ' 465'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'cosmology: observations'
- dark ages
- reionization
- first stars
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1605.08782
month: '03'
oa: 1
oa_version: Preprint
page: 3637-3655
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The production and escape of Lyman-Continuum radiation from star-forming galaxies
at z ∼ 2 and their redshift evolution
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 465
year: '2017'
...
---
_id: '11565'
abstract:
- lang: eng
text: We use the hydrodynamical EAGLE simulation to study the magnitude and origin
of the scatter in the stellar mass–halo mass relation for central galaxies. We
separate cause and effect by correlating stellar masses in the baryonic simulation
with halo properties in a matched dark matter only (DMO) simulation. The scatter
in stellar mass increases with redshift and decreases with halo mass. At z = 0.1,
it declines from 0.25 dex at M200, DMO ≈ 1011 M⊙ to 0.12 dex at M200, DMO ≈ 1013
M⊙, but the trend is weak above 1012 M⊙. For M200, DMO < 1012.5 M⊙ up to 0.04
dex of the scatter is due to scatter in the halo concentration. At fixed halo
mass, a larger stellar mass corresponds to a more concentrated halo. This is likely
because higher concentrations imply earlier formation times and hence more time
for accretion and star formation, and/or because feedback is less efficient in
haloes with higher binding energies. The maximum circular velocity, Vmax, DMO,
and binding energy are therefore more fundamental properties than halo mass, meaning
that they are more accurate predictors of stellar mass, and we provide fitting
formulae for their relations with stellar mass. However, concentration alone cannot
explain the total scatter in the Mstar−M200,DMO relation, and it does not explain
the scatter in Mstar–Vmax, DMO. Halo spin, sphericity, triaxiality, substructure
and environment are also not responsible for the remaining scatter, which thus
could be due to more complex halo properties or non-linear/stochastic baryonic
effects.
acknowledgement: We thank the anonymous referee for their comments. JM acknowledges
the support of a Huygens PhD fellowship from Leiden University. JM thanks David
Sobral for useful discussions and help with fitting routines and Jonas Chavez Montero
and Ying Zu for providing data. We thank PRACE for the access to the Curie facility
in France. We have used the DiRAC system which is a part of National E-Infrastructure
at Durham University, operated by the Institute for Computational Cosmology on behalf
of the STFC DiRAC HPC Facility (www.dirac.ac.uk); the equipment was funded by BIS
National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1,
STFC DiRAC Operations grant ST/K003267/1 and Durham University. The study was sponsored
by the Dutch National Computing Facilities Foundation (NCF) for the use of supercomputer
facilities, with financial support from the Netherlands Organisation for Scientific
Research (NWO), through VICI grant 639.043.409, and the European Research Council
under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC Grant
agreement 278594- GasAroundGalaxies, and from the Belgian Science Policy Office
([AP P7/08 CHARM]). We have benefited greatly from the public available programming
language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY, H5PY and RPY2 packages,
and the TOPCAT analysis program (Taylor 2005).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Robert A.
full_name: Crain, Robert A.
last_name: Crain
- first_name: Matthieu
full_name: Schaller, Matthieu
last_name: Schaller
- first_name: Richard
full_name: Bower, Richard
last_name: Bower
- first_name: Tom
full_name: Theuns, Tom
last_name: Theuns
citation:
ama: Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. The origin of
scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE
simulation. Monthly Notices of the Royal Astronomical Society. 2017;465(2):2381-2396.
doi:10.1093/mnras/stw2884
apa: Matthee, J. J., Schaye, J., Crain, R. A., Schaller, M., Bower, R., & Theuns,
T. (2017). The origin of scatter in the stellar mass–halo mass relation of central
galaxies in the EAGLE simulation. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stw2884
chicago: Matthee, Jorryt J, Joop Schaye, Robert A. Crain, Matthieu Schaller, Richard
Bower, and Tom Theuns. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation
of Central Galaxies in the EAGLE Simulation.” Monthly Notices of the Royal
Astronomical Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stw2884.
ieee: J. J. Matthee, J. Schaye, R. A. Crain, M. Schaller, R. Bower, and T. Theuns,
“The origin of scatter in the stellar mass–halo mass relation of central galaxies
in the EAGLE simulation,” Monthly Notices of the Royal Astronomical Society,
vol. 465, no. 2. Oxford University Press, pp. 2381–2396, 2017.
ista: Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. 2017. The origin
of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE
simulation. Monthly Notices of the Royal Astronomical Society. 465(2), 2381–2396.
mla: Matthee, Jorryt J., et al. “The Origin of Scatter in the Stellar Mass–Halo
Mass Relation of Central Galaxies in the EAGLE Simulation.” Monthly Notices
of the Royal Astronomical Society, vol. 465, no. 2, Oxford University Press,
2017, pp. 2381–96, doi:10.1093/mnras/stw2884.
short: J.J. Matthee, J. Schaye, R.A. Crain, M. Schaller, R. Bower, T. Theuns, Monthly
Notices of the Royal Astronomical Society 465 (2017) 2381–2396.
date_created: 2022-07-12T12:25:08Z
date_published: 2017-02-01T00:00:00Z
date_updated: 2022-08-19T07:56:07Z
day: '01'
doi: 10.1093/mnras/stw2884
extern: '1'
external_id:
arxiv:
- '1608.08218'
intvolume: ' 465'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: haloes'
- 'cosmology: theory'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1608.08218
month: '02'
oa: 1
oa_version: Preprint
page: 2381-2396
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The origin of scatter in the stellar mass–halo mass relation of central galaxies
in the EAGLE simulation
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 465
year: '2017'
...
---
_id: '11566'
abstract:
- lang: eng
text: While traditionally associated with active galactic nuclei (AGN), the properties
of the C II] (λ = 2326 Å), C III] (λ, λ = 1907, 1909 Å) and C IV (λ, λ = 1549,
1551 Å) emission lines are still uncertain as large, unbiased samples of sources
are scarce. We present the first blind, statistical study of C II], C III] and
C IV emitters at z ∼ 0.68, 1.05, 1.53, respectively, uniformly selected down to
a flux limit of ∼4 × 10−17 erg s−1 cm−1 through a narrow-band survey covering
an area of ∼1.4 deg2 over COSMOS and UDS. We detect 16 C II], 35 C III] and 17
C IV emitters, whose nature we investigate using optical colours as well as Hubble
Space Telescope (HST), X-ray, radio and far-infrared data. We find that z ∼ 0.7
C II] emitters are consistent with a mixture of blue (UV slope β = −2.0 ± 0.4)
star-forming (SF) galaxies with discy HST structure and AGN with Seyfert-like
morphologies. Bright C II] emitters have individual X-ray detections as well as
high average black hole accretion rates (BHARs) of ∼0.1 M⊙ yr−1. C III] emitters
at z ∼ 1.05 trace a general population of SF galaxies, with β = −0.8 ± 1.1, a
variety of optical morphologies, including isolated and interacting galaxies and
low BHAR (<0.02 M⊙ yr−1). Our C IV emitters at z ∼ 1.5 are consistent with young,
blue quasars (β ∼ −1.9) with point-like optical morphologies, bright X-ray counterparts
and large BHAR (0.8 M⊙ yr−1). We also find some surprising C II], C III] and
C IV emitters with rest-frame equivalent widths (EWs) that could be as large as
50–100 Å. AGN or spatial offsets between the UV continuum stellar disc and the
line-emitting regions may explain the large EW. These bright C II], C III] and
C IV emitters are ideal candidates for spectroscopic follow-up to fully unveil
their nature.
acknowledgement: 'We would like to thank the anonymous referee for her/his valuable
input that helped improve the clarity and interpretation of our results. DS acknowledges
financial support from the Netherlands Organisation for Scientific research (NWO),
through a Veni fellowship. IO acknowledges support from the European Research Council
in the form of the Advanced Investigator Programme, 321302, COSMICISM. CALYMHA data
are based on observations made with the Isaac Newton Telescope (proposals 13AN002,
I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008) operated on the island
of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los
Muchachos of the Instituto de Astrofísica de Canarias. Also based on data products
from observations made with ESO Telescopes at the La Silla Paranal Observatory under
ESO programme IDs 098.A-0819 and 179.A-2005. We are grateful to E. L. Wright and
J. Schombert for their cosmology calculator. We would like to thank the authors
of NUMPY (van der Walt et al. 2011), SCIPY (Jones et al. 2001), MATPLOTLIB (Hunter
2007) and ASTROPY (Astropy Collaboration et al. 2013) for making these packages
publicly available. This research has made use of the NASA/IPAC Extragalactic Database
(NED), which is '
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Andra
full_name: Stroe, Andra
last_name: Stroe
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: João
full_name: Calhau, João
last_name: Calhau
- first_name: Ivan
full_name: Oteo, Ivan
last_name: Oteo
citation:
ama: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for
C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent
widths . Monthly Notices of the Royal Astronomical Society. 2017;471(3):2558-2574.
doi:10.1093/mnras/stx1712
apa: Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., & Oteo, I. (2017). A
1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies
and equivalent widths . Monthly Notices of the Royal Astronomical Society.
Oxford University Press. https://doi.org/10.1093/mnras/stx1712
chicago: Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo.
“A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature,
Morphologies and Equivalent Widths .” Monthly Notices of the Royal Astronomical
Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stx1712.
ieee: A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind
survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and
equivalent widths ,” Monthly Notices of the Royal Astronomical Society,
vol. 471, no. 3. Oxford University Press, pp. 2558–2574, 2017.
ista: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey
for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent
widths . Monthly Notices of the Royal Astronomical Society. 471(3), 2558–2574.
mla: Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at
z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” Monthly Notices
of the Royal Astronomical Society, vol. 471, no. 3, Oxford University Press,
2017, pp. 2558–74, doi:10.1093/mnras/stx1712.
short: A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of
the Royal Astronomical Society 471 (2017) 2558–2574.
date_created: 2022-07-12T12:33:16Z
date_published: 2017-11-01T00:00:00Z
date_updated: 2022-08-19T07:59:57Z
day: '01'
doi: 10.1093/mnras/stx1712
extern: '1'
external_id:
arxiv:
- '1703.10169'
intvolume: ' 471'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: active'
- 'galaxies: high-redshift'
- 'quasars: emission lines'
- 'galaxies: star formation'
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1703.10169
month: '11'
oa: 1
oa_version: Preprint
page: 2558-2574
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature,
morphologies and equivalent widths '
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...
---
_id: '11567'
abstract:
- lang: eng
text: Recently, the C III] and C IV emission lines have been observed in galaxies
in the early Universe (z > 5), providing new ways to measure their redshift and
study their stellar populations and active galactic nuclei (AGN). We explore the
first blind C II], C III] and C IV survey (z ∼ 0.68, 1.05, 1.53, respectively)
presented in Stroe et al. (2017). We derive luminosity functions (LF) and study
properties of C II], C III] and C IV line emitters through comparisons to the
LFs of H α and Ly α emitters, UV selected star-forming (SF) galaxies and quasars
at similar redshifts. The C II] LF at z ∼ 0.68 is equally well described by a
Schechter or a power-law LF, characteristic of a mixture of SF and AGN activity.
The C III] LF (z ∼ 1.05) is consistent to a scaled down version of the Schechter
H α and Ly α LF at their redshift, indicating a SF origin. In stark contrast,
the C IV LF at z ∼ 1.53 is well fit by a power-law, quasar-like LF. We find that
the brightest UV sources (MUV < −22) will universally have C III] and C IV emission.
However, on average, C III] and C IV are not as abundant as H α or Ly α emitters
at the same redshift, with cosmic average ratios of ∼0.02–0.06 to H α and ∼0.01–0.1
to intrinsic Ly α. We predict that the C III] and C IV lines can only be truly
competitive in confirming high-redshift candidates when the hosts are intrinsically
bright and the effective Ly α escape fraction is below 1 per cent. While C III]
and C IV were proposed as good tracers of young, relatively low-metallicity galaxies
typical of the early Universe, we find that, at least at z ∼ 1.5, C IV is exclusively
hosted by AGN/quasars, especially at large line equivalent widths.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Andra
full_name: Stroe, Andra
last_name: Stroe
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: João
full_name: Calhau, João
last_name: Calhau
- first_name: Ivan
full_name: Oteo, Ivan
last_name: Oteo
citation:
ama: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for
C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average
line ratios. Monthly Notices of the Royal Astronomical Society. 2017;471(3):2575-2586.
doi:10.1093/mnras/stx1713
apa: Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., & Oteo, I. (2017). A
1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity
functions and cosmic average line ratios. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stx1713
chicago: Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo.
“A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity
Functions and Cosmic Average Line Ratios.” Monthly Notices of the Royal Astronomical
Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stx1713.
ieee: A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind
survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and
cosmic average line ratios,” Monthly Notices of the Royal Astronomical Society,
vol. 471, no. 3. Oxford University Press, pp. 2575–2586, 2017.
ista: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey
for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic
average line ratios. Monthly Notices of the Royal Astronomical Society. 471(3),
2575–2586.
mla: Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at
z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” Monthly
Notices of the Royal Astronomical Society, vol. 471, no. 3, Oxford University
Press, 2017, pp. 2575–86, doi:10.1093/mnras/stx1713.
short: A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of
the Royal Astronomical Society 471 (2017) 2575–2586.
date_created: 2022-07-12T12:54:57Z
date_published: 2017-11-01T00:00:00Z
date_updated: 2022-08-19T08:02:04Z
day: '01'
doi: 10.1093/mnras/stx1713
extern: '1'
external_id:
arxiv:
- '1703.10169'
intvolume: ' 471'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: active'
- 'galaxies: high redshift'
- 'galaxies: luminosity function'
- mass function
- 'quasars: emission lines'
- star formation
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1703.10169
month: '11'
oa: 1
oa_version: Preprint
page: 2575-2586
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity
functions and cosmic average line ratios
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...
---
_id: '11572'
abstract:
- lang: eng
text: We present spectroscopic follow-up of candidate luminous Ly α emitters (LAEs)
at z = 5.7–6.6 in the SA22 field with VLT/X-SHOOTER. We confirm two new luminous
LAEs at z = 5.676 (SR6) and z = 6.532 (VR7), and also present HST follow-up of
both sources. These sources have luminosities LLy α ≈ 3 × 1043 erg s−1, very high
rest-frame equivalent widths of EW0 ≳ 200 Å and narrow Ly α lines (200–340 km s−1).
VR7 is the most UV-luminous LAE at z > 6.5, with M1500 = −22.5, even brighter
in the UV than CR7. Besides Ly α, we do not detect any other rest-frame UV lines
in the spectra of SR6 and VR7, and argue that rest-frame UV lines are easier to
observe in bright galaxies with low Ly α equivalent widths. We confirm that Ly α
line widths increase with Ly α luminosity at z = 5.7, while there are indications
that Ly α lines of faint LAEs become broader at z = 6.6, potentially due to reionization.
We find a large spread of up to 3 dex in UV luminosity for >L⋆ LAEs, but find
that the Ly α luminosity of the brightest LAEs is strongly related to UV luminosity
at z = 6.6. Under basic assumptions, we find that several LAEs at z ≈ 6–7 have
Ly α escape fractions ≳ 100 per cent, indicating bursty star formation histories,
alternative Ly α production mechanisms, or dust attenuating Ly α emission differently
than UV emission. Finally, we present a method to compute ξion, the production
efficiency of ionizing photons, and find that LAEs at z ≈ 6–7 have high values
of log10(ξion/Hz erg−1) ≈ 25.51 ± 0.09 that may alleviate the need for high Lyman-Continuum
escape fractions required for reionization.
acknowledgement: 'We thank the referee for a constructive report that has improved
the quality and clarity of this work. The authors thank Grecco Oyarzún for discussions.
JM acknowledges the support of a Huygens PhD fellowship from Leiden University.
DS acknowledges financial support from the Netherlands Organisation for Scientific
research (NWO) through a Veni fellowship and from Lancaster University through an
Early Career Internal Grant A100679. BD acknowledges financial support from NASA
through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G.
We thank Kasper Schmidt for providing measurements. Based on observations with the
W.M. Keck Observatory through programme C267D. The W.M. Keck Observatory is operated
as a scientific partnership amongst the California Institute of Technology, the
University of California and the National Aeronautics and Space Administration.
Based on observations made with ESO Telescopes at the La Silla Paranal Observatory
under programme IDs 097.A-0943, 294.A 5018 and 098.A-0819 and on data products produced
by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.
The authors acknowledge the award of observing time (W16AN004) and of service time
(SW2014b20) on the William Herschel Telescope (WHT). WHT and its service programme
are operated on the island of La Palma by the Isaac Newton Group in the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.
Based on observations made with the NASA/ESA HST, obtained (from the Data Archive)
at the Space Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These
observations are associated with programme #14699. We are grateful for the excellent
data sets from the COSMOS, UltraVISTA, SXDS, UDS and CFHTLS survey teams; without
these legacy surveys, this research would have been impossible. We have benefited
from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB,
PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP
and SCAMP and the TOPCAT analysis tool (Taylor 2013).'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Behnam
full_name: Darvish, Behnam
last_name: Darvish
- first_name: Sérgio
full_name: Santos, Sérgio
last_name: Santos
- first_name: Bahram
full_name: Mobasher, Bahram
last_name: Mobasher
- first_name: Ana
full_name: Paulino-Afonso, Ana
last_name: Paulino-Afonso
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
- first_name: Lara
full_name: Alegre, Lara
last_name: Alegre
citation:
ama: Matthee JJ, Sobral D, Darvish B, et al. Spectroscopic properties of luminous
Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. Monthly
Notices of the Royal Astronomical Society. 2017;472(1):772-787. doi:10.1093/mnras/stx2061
apa: Matthee, J. J., Sobral, D., Darvish, B., Santos, S., Mobasher, B., Paulino-Afonso,
A., … Alegre, L. (2017). Spectroscopic properties of luminous Ly α emitters at
z ≈ 6–7 and comparison to the Lyman-break population. Monthly Notices of the
Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stx2061
chicago: Matthee, Jorryt J, David Sobral, Behnam Darvish, Sérgio Santos, Bahram
Mobasher, Ana Paulino-Afonso, Huub Röttgering, and Lara Alegre. “Spectroscopic
Properties of Luminous Ly α Emitters at z ≈ 6–7 and Comparison to the Lyman-Break
Population.” Monthly Notices of the Royal Astronomical Society. Oxford
University Press, 2017. https://doi.org/10.1093/mnras/stx2061.
ieee: J. J. Matthee et al., “Spectroscopic properties of luminous Ly α emitters
at z ≈ 6–7 and comparison to the Lyman-break population,” Monthly Notices of
the Royal Astronomical Society, vol. 472, no. 1. Oxford University Press,
pp. 772–787, 2017.
ista: Matthee JJ, Sobral D, Darvish B, Santos S, Mobasher B, Paulino-Afonso A, Röttgering
H, Alegre L. 2017. Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7
and comparison to the Lyman-break population. Monthly Notices of the Royal Astronomical
Society. 472(1), 772–787.
mla: Matthee, Jorryt J., et al. “Spectroscopic Properties of Luminous Ly α Emitters
at z ≈ 6–7 and Comparison to the Lyman-Break Population.” Monthly Notices of
the Royal Astronomical Society, vol. 472, no. 1, Oxford University Press,
2017, pp. 772–87, doi:10.1093/mnras/stx2061.
short: J.J. Matthee, D. Sobral, B. Darvish, S. Santos, B. Mobasher, A. Paulino-Afonso,
H. Röttgering, L. Alegre, Monthly Notices of the Royal Astronomical Society 472
(2017) 772–787.
date_created: 2022-07-13T09:47:39Z
date_published: 2017-11-01T00:00:00Z
date_updated: 2022-08-19T08:05:37Z
day: '01'
doi: 10.1093/mnras/stx2061
extern: '1'
external_id:
arxiv:
- '1706.06591'
intvolume: ' 472'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution – galaxies: high-redshift'
- dark ages
- reionization
- first stars
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1706.06591
month: '11'
oa: 1
oa_version: Preprint
page: 772-787
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison
to the Lyman-break population
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 472
year: '2017'
...
---
_id: '11573'
abstract:
- lang: eng
text: We present dynamical measurements from the KMOS (K-band multi-object spectrograph)
Deep Survey (KDS), which comprises 77 typical star-forming galaxies at z ≃ 3.5
in the mass range 9.0 < log (M⋆/M⊙) < 10.5. These measurements constrain the internal
dynamics, the intrinsic velocity dispersions (σint) and rotation velocities (VC)
of galaxies in the high-redshift Universe. The mean velocity dispersion of the
galaxies in our sample is σint=70.8+3.3−3.1kms−1, revealing that the increasing
average σint with increasing redshift, reported for z ≲ 2, continues out to z
≃ 3.5. Only 36 ± 8 per cent of our galaxies are rotation-dominated (VC/σint >
1), with the sample average VC/σint value much smaller than at lower redshift.
After carefully selecting comparable star-forming samples at multiple epochs,
we find that the rotation-dominated fraction evolves with redshift with a z−0.2
dependence. The rotation-dominated KDS galaxies show no clear offset from the
local rotation velocity–stellar mass (i.e. VC–M⋆) relation, although a smaller
fraction of the galaxies are on the relation due to the increase in the dispersion-dominated
fraction. These observations are consistent with a simple equilibrium model picture,
in which random motions are boosted in high-redshift galaxies by a combination
of the increasing gas fractions, accretion efficiency, specific star formation
rate and stellar feedback and which may provide significant pressure support against
gravity on the galactic disc scale.
acknowledgement: 'We wish to thank the anonymous referee for their comments, which
have improved the quality and clarity of this work. OJT acknowledges the financial
support of the Science and Technology Facilities Council through a studentship award.
MC and OJT acknowledge the KMOS team and all the personnel of the European Southern
Observatory Very Large Telescope for outstanding support during the KMOS GTO observations.
CMH, AMS and RMS acknowledge the Science and Technology Facilities Council through
grant code ST/L00075X/1. RJM acknowledges the support of the European Research Council
via the award of a Consolidator Grant (PI: McLure). JSD acknowledges the support
of the European Research Council via the award of an Advanced Grant (PI J. Dunlop),
and the contribution of the EC FP7 SPACE project ASTRODEEP (Ref.No: 312725). AMS
acknowledges the Leverhulme Foundation. JM acknowledges the support of a Huygens
PhD fellowship from Leiden University. DS acknowledges financial support from the
Netherlands Organization for Scientific research (NWO) through a Veni fellowship
and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010).
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. This work is based
on observations taken by the 3D HST Treasury Program (GO 12177 and 12328) with the
NASA/ESA HST, which is operated by the Association of Universities for Research
in Astronomy, Inc., under NASA contract NAS5-26555. Based on data obtained with
the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large
Program 185.A-0791, and made available by the VUDS team at the CESAM data centre,
Laboratoire d’Astrophysique de Marseille, France. Based on observations obtained
at the Very Large Telescope of the European Southern Observatory. Programme IDs:
092.A 0399(A), 093.A-0122(A,B), 094.A-0214(A,B),095.A0680(A,B),096.A-0315(A,B,C).'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: O. J.
full_name: Turner, O. J.
last_name: Turner
- first_name: M.
full_name: Cirasuolo, M.
last_name: Cirasuolo
- first_name: C. M.
full_name: Harrison, C. M.
last_name: Harrison
- first_name: R. J.
full_name: McLure, R. J.
last_name: McLure
- first_name: J. S.
full_name: Dunlop, J. S.
last_name: Dunlop
- first_name: A. M.
full_name: Swinbank, A. M.
last_name: Swinbank
- first_name: H. L.
full_name: Johnson, H. L.
last_name: Johnson
- 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: R. M.
full_name: Sharples, R. M.
last_name: Sharples
citation:
ama: Turner OJ, Cirasuolo M, Harrison CM, et al. The KMOS Deep Survey (KDS) – I.
Dynamical measurements of typical star-forming galaxies at z ≃ 3.5. Monthly
Notices of the Royal Astronomical Society. 2017;471(2):1280-1320. doi:10.1093/mnras/stx1366
apa: Turner, O. J., Cirasuolo, M., Harrison, C. M., McLure, R. J., Dunlop, J. S.,
Swinbank, A. M., … Sharples, R. M. (2017). The KMOS Deep Survey (KDS) – I. Dynamical
measurements of typical star-forming galaxies at z ≃ 3.5. Monthly Notices of
the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stx1366
chicago: Turner, O. J., M. Cirasuolo, C. M. Harrison, R. J. McLure, J. S. Dunlop,
A. M. Swinbank, H. L. Johnson, D. Sobral, Jorryt J Matthee, and R. M. Sharples.
“The KMOS Deep Survey (KDS) – I. Dynamical Measurements of Typical Star-Forming
Galaxies at z ≃ 3.5.” Monthly Notices of the Royal Astronomical Society.
Oxford University Press, 2017. https://doi.org/10.1093/mnras/stx1366.
ieee: O. J. Turner et al., “The KMOS Deep Survey (KDS) – I. Dynamical measurements
of typical star-forming galaxies at z ≃ 3.5,” Monthly Notices of the Royal
Astronomical Society, vol. 471, no. 2. Oxford University Press, pp. 1280–1320,
2017.
ista: Turner OJ, Cirasuolo M, Harrison CM, McLure RJ, Dunlop JS, Swinbank AM, Johnson
HL, Sobral D, Matthee JJ, Sharples RM. 2017. The KMOS Deep Survey (KDS) – I. Dynamical
measurements of typical star-forming galaxies at z ≃ 3.5. Monthly Notices of the
Royal Astronomical Society. 471(2), 1280–1320.
mla: Turner, O. J., et al. “The KMOS Deep Survey (KDS) – I. Dynamical Measurements
of Typical Star-Forming Galaxies at z ≃ 3.5.” Monthly Notices of the Royal
Astronomical Society, vol. 471, no. 2, Oxford University Press, 2017, pp.
1280–320, doi:10.1093/mnras/stx1366.
short: O.J. Turner, M. Cirasuolo, C.M. Harrison, R.J. McLure, J.S. Dunlop, A.M.
Swinbank, H.L. Johnson, D. Sobral, J.J. Matthee, R.M. Sharples, Monthly Notices
of the Royal Astronomical Society 471 (2017) 1280–1320.
date_created: 2022-07-13T10:03:01Z
date_published: 2017-10-01T00:00:00Z
date_updated: 2022-08-19T08:07:31Z
day: '01'
doi: 10.1093/mnras/stx1366
extern: '1'
external_id:
arxiv:
- '1704.06263'
intvolume: ' 471'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: kinematics and dynamics'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1704.06263
month: '10'
oa: 1
oa_version: Preprint
page: 1280-1320
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 KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming
galaxies at z ≃ 3.5
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...
---
_id: '11574'
abstract:
- lang: eng
text: We present new results from the widest narrow-band survey search for Lyα emitters
at z = 5.7, just after reionization. We survey a total of 7 deg2 spread over the
COSMOS, UDS and SA22 fields. We find over 11 000 line emitters, out of which 514
are robust Lyα candidates at z = 5.7 within a volume of 6.3 × 106 Mpc3. Our Lyα
emitters span a wide range in Lyα luminosities, from faint to bright (LLyα ∼ 1042.5–44
erg s−1) and rest-frame equivalent widths (EW0 ∼ 25–1000 Å) in a single, homogeneous
data set. By combining all our fields, we find that the faint end slope of the
z = 5.7 Lyα luminosity function is very steep, with α=−2.3+0.4−0.3. We also present
an updated z = 6.6 Lyα luminosity function, based on comparable volumes and obtained
with the same methods, which we directly compare with that at z = 5.7. We find
a significant decline of the number density of faint Lyα emitters from z = 5.7
to 6.6 (by 0.5 ± 0.1 dex), but no evolution at the bright end/no evolution in
L*. Faint Lyα emitters at z = 6.6 show much more extended haloes than those at
z = 5.7, suggesting that neutral Hydrogen plays an important role, increasing
the scattering and leading to observations missing faint Lyα emission within the
epoch of reionization. Altogether, our results suggest that we are observing patchy
reionization which happens first around the brightest Lyα emitters, allowing the
number densities of those sources to remain unaffected by the increase of neutral
Hydrogen fraction from z ∼ 5 to 7.
acknowledgement: 'We thank the anonymous referee for useful and constructive comments
and suggestions which greatly improved the quality and clarity of our work. The
authors acknowledge financial support from the Netherlands Organisation for Scientific
research (NWO) through a Veni fellowship. SS and DS acknowledge funding from FCT
through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010).
SS also acknowledges support from FCT through the research grants UID/FIS/04434/2013
and PTDC/FIS-AST/2194/2012. JM acknowledges a Huygens PhD fellowship from Leiden
University. Based on observations with the Subaru Telescope (Program IDs: S05B-027,
S06A-025, S06B-010, S07A-013, S07B-008, S08B-008, S09A-017, S14A-086). Based on
observations made with ESO Telescopes at the La Silla Paranal Observatory under
programme ID 294.A-5018. Based on observations obtained with MegaPrime/Megacam,
a joint project of CFHT and CEA/IRFU, at the Canada–France–Hawaii Telescope (CFHT)
which is operated by the National Research Council (NRC) of Canada, the Institut
National des Science de l’Univers of the Centre National de la Recherche Scientifique
(CNRS) of France, and the University of Hawaii. This work is based in part on data
products produced at TERAPIX available at the Canadian Astronomy Data Centre as
part of the Canada–France–Hawaii Telescope Legacy Survey, a collaborative project
of NRC and CNRS. Based on data products from observations made with ESO Telescopes
at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data
products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of
the UltraVISTA consortium. We are grateful to the CFHTLS, COSMOS-UltraVISTA, UKIDSS,
SXDF and COSMOS survey teams. Without these legacy surveys, this research would
have been impossible. The authors wish to recognize and acknowledge the very significant
cultural role and reverence that the summit of Mauna Kea has always had within the
indigenous Hawaiian community. We are most fortunate to have the opportunity to
conduct and explore observations from this mountain. Finally, the authors acknowledge
the unique value of the publicly available programming language PYTHON, including
the NUMPY, PYFITS, MATPLOTLIB, SCIPY and ASTROPY (Astropy Collaboration et al.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Sérgio
full_name: Santos, Sérgio
last_name: Santos
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
citation:
ama: 'Santos S, Sobral D, Matthee JJ. The Lyα luminosity function at z= 5.7–6.6
and the steep drop of the faint end: Implications for reionization. Monthly
Notices of the Royal Astronomical Society. 2016;463(2):1678-1691. doi:10.1093/mnras/stw2076'
apa: 'Santos, S., Sobral, D., & Matthee, J. J. (2016). The Lyα luminosity function
at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization.
Monthly Notices of the Royal Astronomical Society. Oxford University Press.
https://doi.org/10.1093/mnras/stw2076'
chicago: 'Santos, Sérgio, David Sobral, and Jorryt J Matthee. “The Lyα Luminosity
Function at Z= 5.7–6.6 and the Steep Drop of the Faint End: Implications for Reionization.”
Monthly Notices of the Royal Astronomical Society. Oxford University Press,
2016. https://doi.org/10.1093/mnras/stw2076.'
ieee: 'S. Santos, D. Sobral, and J. J. Matthee, “The Lyα luminosity function at
z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization,”
Monthly Notices of the Royal Astronomical Society, vol. 463, no. 2. Oxford
University Press, pp. 1678–1691, 2016.'
ista: 'Santos S, Sobral D, Matthee JJ. 2016. The Lyα luminosity function at z= 5.7–6.6
and the steep drop of the faint end: Implications for reionization. Monthly Notices
of the Royal Astronomical Society. 463(2), 1678–1691.'
mla: 'Santos, Sérgio, et al. “The Lyα Luminosity Function at Z= 5.7–6.6 and the
Steep Drop of the Faint End: Implications for Reionization.” Monthly Notices
of the Royal Astronomical Society, vol. 463, no. 2, Oxford University Press,
2016, pp. 1678–91, doi:10.1093/mnras/stw2076.'
short: S. Santos, D. Sobral, J.J. Matthee, Monthly Notices of the Royal Astronomical
Society 463 (2016) 1678–1691.
date_created: 2022-07-13T10:08:20Z
date_published: 2016-12-01T00:00:00Z
date_updated: 2022-08-19T08:09:54Z
day: '01'
doi: 10.1093/mnras/stw2076
extern: '1'
external_id:
arxiv:
- '1606.07435'
intvolume: ' 463'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift'
- 'galaxies: luminosity function'
- mass function
- 'cosmology: observations'
- dark ages
- reionization
- first stars
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1606.07435
month: '12'
oa: 1
oa_version: Preprint
page: 1678-1691
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint
end: Implications for reionization'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 463
year: '2016'
...
---
_id: '11575'
abstract:
- lang: eng
text: We investigate correlations between different physical properties of star-forming
galaxies in the ‘Evolution and Assembly of GaLaxies and their Environments’ (EAGLE)
cosmological hydrodynamical simulation suite over the redshift range 0 ≤ z ≤ 4.5.
A principal component analysis reveals that neutral gas fraction (fgas,neutral),
stellar mass (Mstellar) and star formation rate (SFR) account for most of the
variance seen in the population, with galaxies tracing a two-dimensional, nearly
flat, surface in the three-dimensional space of fgas, neutral–Mstellar–SFR with
little scatter. The location of this plane varies little with redshift, whereas
galaxies themselves move along the plane as their fgas, neutral and SFR drop with
redshift. The positions of galaxies along the plane are highly correlated with
gas metallicity. The metallicity can therefore be robustly predicted from fgas,
neutral, or from the Mstellar and SFR. We argue that the appearance of this ‘Fundamental
Plane of star formation’ is a consequence of self-regulation, with the plane's
curvature set by the dependence of the SFR on gas density and metallicity. We
analyse a large compilation of observations spanning the redshift range 0 ≲ z
≲ 3, and find that such a plane is also present in the data. The properties of
the observed Fundamental Plane of star formation are in good agreement with EAGLE's
predictions.
acknowledgement: We thank Luca Cortese, Matt Bothwell, Paola Santini and Tim Davis
for providing observational data sets, and Aaron Robotham, Luca Cortese and Barbara
Catinella for useful discussions. CdPL is funded by a Discovery Early Career Researcher
Award (DE150100618). CdPL also thanks the MERAC Foundation for a Postdoctoral Research
Award. This work used the DiRAC Data Centric system at Durham University, operated
by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility
(www.dirac.ac.uk). This equipment was funded by BIS National E-infrastructure capital
grant ST/K00042X/1, STFC capital grant ST/H008519/1, and STFC DiRAC Operations grant
ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure.
Support was also received via the Interuniversity Attraction Poles Programme initiated
by the Belgian Science Policy Office ([AP P7/08 CHARM]), the National Science Foundation
under grant no. NSF PHY11-25915, and the UK Science and Technology Facilities Council
(grant numbers ST/F001166/1 and ST/I000976/1) via rolling and consolidating grants
awarded to the ICC. The research was supported in part by the European Research
Council under the European Union‘s Seventh Framework Programme (FP7/2007-2013)/ERC
grant agreement 278594-GasAroundGalaxies.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Claudia del P.
full_name: Lagos, Claudia del P.
last_name: Lagos
- first_name: Tom
full_name: Theuns, Tom
last_name: Theuns
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Michelle
full_name: Furlong, Michelle
last_name: Furlong
- first_name: Richard G.
full_name: Bower, Richard G.
last_name: Bower
- first_name: Matthieu
full_name: Schaller, Matthieu
last_name: Schaller
- first_name: Robert A.
full_name: Crain, Robert A.
last_name: Crain
- first_name: James W.
full_name: Trayford, James W.
last_name: Trayford
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
citation:
ama: Lagos C del P, Theuns T, Schaye J, et al. The Fundamental Plane of star formation
in galaxies revealed by the EAGLE hydrodynamical simulations. Monthly Notices
of the Royal Astronomical Society. 2016;459(3):2632-2650. doi:10.1093/mnras/stw717
apa: Lagos, C. del P., Theuns, T., Schaye, J., Furlong, M., Bower, R. G., Schaller,
M., … Matthee, J. J. (2016). The Fundamental Plane of star formation in galaxies
revealed by the EAGLE hydrodynamical simulations. Monthly Notices of the Royal
Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw717
chicago: Lagos, Claudia del P., Tom Theuns, Joop Schaye, Michelle Furlong, Richard
G. Bower, Matthieu Schaller, Robert A. Crain, James W. Trayford, and Jorryt J
Matthee. “The Fundamental Plane of Star Formation in Galaxies Revealed by the
EAGLE Hydrodynamical Simulations.” Monthly Notices of the Royal Astronomical
Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw717.
ieee: C. del P. Lagos et al., “The Fundamental Plane of star formation in
galaxies revealed by the EAGLE hydrodynamical simulations,” Monthly Notices
of the Royal Astronomical Society, vol. 459, no. 3. Oxford University Press,
pp. 2632–2650, 2016.
ista: Lagos C del P, Theuns T, Schaye J, Furlong M, Bower RG, Schaller M, Crain
RA, Trayford JW, Matthee JJ. 2016. The Fundamental Plane of star formation in
galaxies revealed by the EAGLE hydrodynamical simulations. Monthly Notices of
the Royal Astronomical Society. 459(3), 2632–2650.
mla: Lagos, Claudia del P., et al. “The Fundamental Plane of Star Formation in Galaxies
Revealed by the EAGLE Hydrodynamical Simulations.” Monthly Notices of the Royal
Astronomical Society, vol. 459, no. 3, Oxford University Press, 2016, pp.
2632–50, doi:10.1093/mnras/stw717.
short: C. del P. Lagos, T. Theuns, J. Schaye, M. Furlong, R.G. Bower, M. Schaller,
R.A. Crain, J.W. Trayford, J.J. Matthee, Monthly Notices of the Royal Astronomical
Society 459 (2016) 2632–2650.
date_created: 2022-07-13T10:21:24Z
date_published: 2016-07-01T00:00:00Z
date_updated: 2022-08-19T08:12:07Z
day: '01'
doi: 10.1093/mnras/stw717
extern: '1'
external_id:
arxiv:
- '1510.08067'
intvolume: ' 459'
issue: '3'
keyword:
- Space and Planetary Science
- 'Astronomy and Astrophysics stars: formation'
- 'ISM: evolution'
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: ISM'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1510.08067
month: '07'
oa: 1
oa_version: Preprint
page: 2632-2650
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical
simulations
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 459
year: '2016'
...
---
_id: '11576'
abstract:
- lang: eng
text: We use new near-infrared spectroscopic observations to investigate the nature
and evolution of the most luminous Hα emitters at z ∼ 0.8–2.23, which evolve strongly
in number density over this period, and compare them to more typical Hα emitters.
We study 59 luminous Hα emitters with LHα > L∗Hα, roughly equally split per redshift
slice at z ∼ 0.8, 1.47 and 2.23 from the HiZELS and CF-HiZELS surveys. We find
that, overall, 30 ± 8 per cent are active galactic nuclei [AGNs; 80 ± 30 per cent
of these AGNs are broad-line AGNs, BL-AGNs], and we find little to no evolution
in the AGN fraction with redshift, within the errors. However, the AGN fraction
increases strongly with Hα luminosity and correlates best with LHα/L∗Hα(z). While
LHα ≤ L∗Hα(z) Hα emitters are largely dominated by star-forming galaxies (>80
per cent), the most luminous Hα emitters (LHα>10L∗Hα(z)) at any cosmic time
are essentially all BL-AGN. Using our AGN-decontaminated sample of luminous star-forming
galaxies, and integrating down to a fixed Hα luminosity, we find a factor of ∼1300
evolution in the star formation rate density from z = 0 to 2.23. This is much
stronger than the evolution from typical Hα star-forming galaxies and in line
with the evolution seen for constant luminosity cuts used to select ‘ultraluminous’
infrared galaxies and/or sub-millimetre galaxies. By taking into account the evolution
in the typical Hα luminosity, we show that the most strongly star-forming Hα-selected
galaxies at any epoch (LHα>L∗Hα(z)) contribute the same fractional amount of
≈15 per cent to the total star formation rate density, at least up to z = 2.23.
acknowledgement: "The authors would like to thank the anonymous reviewer for the many
helpful comments and suggestions which greatly improved the clarity and quality
of this work. DS and SAK acknowledge financial support from the Netherlands Organisation
for Scientific research (NWO) through a Veni fellowship. DS also acknowledges funding
from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010)
and from FCT grant PEst-OE/FIS/UI2751/2014. Part of this project was undertaken
during the inaugural Leiden/ESA Astrophysics Program for Summer Students (LEAPS).
IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator
programme DUSTYGAL 321334 and a Royal Society/Wolfson merit award. CH acknowledges
support from STFC. Based on observations made with ESO Telescopes at the La Silla
Paranal Observatory under programme ID 087.A-0337 and ID 089.A-0965. Also based
on data from the Telescopio Nazionale Galileo, with time awarded through OPTICON
programmes 2011A/026 and 2012A020 and the William Herschel Telescope under programme
W12BN007. The William Herschel Telescope is operated on the island of La Palma by
the Isaac Newton Group in the Spanish\r\nObservatorio del Roque de los Muchachos
of the Instituto de Astrofisica de Canarias. The authors wish to thank all the help
given by the telescope staff from all the observatories used in this study: ESO
staff in La Silla, and the TNG and WHT staff in La Palma. This publication makes
use of data products from the Two Micron All-Sky Survey, which is a joint project
of the University of Massachusetts and the Infrared Processing and Analysis Center/California
Institute of Technology, funded by the National Aeronautics and Space Administration
and the National Science Foundation."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Saul A.
full_name: Kohn, Saul A.
last_name: Kohn
- first_name: Philip N.
full_name: Best, Philip N.
last_name: Best
- first_name: Ian
full_name: Smail, Ian
last_name: Smail
- first_name: Chris M.
full_name: Harrison, Chris M.
last_name: Harrison
- first_name: John
full_name: Stott, John
last_name: Stott
- first_name: João
full_name: Calhau, João
last_name: Calhau
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
citation:
ama: 'Sobral D, Kohn SA, Best PN, et al. The most luminous H α emitters at z ∼ 0.8–2.23
from HiZELS: Evolution of AGN and star-forming galaxies. Monthly Notices of
the Royal Astronomical Society. 2016;457(2):1739-1752. doi:10.1093/mnras/stw022'
apa: 'Sobral, D., Kohn, S. A., Best, P. N., Smail, I., Harrison, C. M., Stott, J.,
… Matthee, J. J. (2016). The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS:
Evolution of AGN and star-forming galaxies. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stw022'
chicago: 'Sobral, David, Saul A. Kohn, Philip N. Best, Ian Smail, Chris M. Harrison,
John Stott, João Calhau, and Jorryt J Matthee. “The Most Luminous H α Emitters
at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and Star-Forming Galaxies.” Monthly
Notices of the Royal Astronomical Society. Oxford University Press, 2016.
https://doi.org/10.1093/mnras/stw022.'
ieee: 'D. Sobral et al., “The most luminous H α emitters at z ∼ 0.8–2.23
from HiZELS: Evolution of AGN and star-forming galaxies,” Monthly Notices of
the Royal Astronomical Society, vol. 457, no. 2. Oxford University Press,
pp. 1739–1752, 2016.'
ista: 'Sobral D, Kohn SA, Best PN, Smail I, Harrison CM, Stott J, Calhau J, Matthee
JJ. 2016. The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution
of AGN and star-forming galaxies. Monthly Notices of the Royal Astronomical Society.
457(2), 1739–1752.'
mla: 'Sobral, David, et al. “The Most Luminous H α Emitters at z ∼ 0.8–2.23 from
HiZELS: Evolution of AGN and Star-Forming Galaxies.” Monthly Notices of the
Royal Astronomical Society, vol. 457, no. 2, Oxford University Press, 2016,
pp. 1739–52, doi:10.1093/mnras/stw022.'
short: D. Sobral, S.A. Kohn, P.N. Best, I. Smail, C.M. Harrison, J. Stott, J. Calhau,
J.J. Matthee, Monthly Notices of the Royal Astronomical Society 457 (2016) 1739–1752.
date_created: 2022-07-13T12:50:36Z
date_published: 2016-04-01T00:00:00Z
date_updated: 2022-08-19T08:15:21Z
day: '01'
doi: 10.1093/mnras/stw022
extern: '1'
external_id:
arxiv:
- '1601.02266'
intvolume: ' 457'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1601.02266
month: '04'
oa: 1
oa_version: Preprint
page: 1739-1752
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN
and star-forming galaxies'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 457
year: '2016'
...
---
_id: '11578'
abstract:
- lang: eng
text: We present the first results from our CAlibrating LYMan α with Hα (CALYMHA)
pilot survey at the Isaac Newton Telescope. We measure Lyα emission for 488 Hα
selected galaxies at z = 2.23 from High-z Emission Line Survey in the COSMOS and
UDS fields with a specially designed narrow-band filter (λc = 3918 Å, Δλ = 52
Å). We find 17 dual Hα-Lyα emitters [fLyα > 5 × 10−17 erg s−1 cm−2, of which five
are X-ray active galactic nuclei (AGN)]. For star-forming galaxies, we find a
range of Lyα escape fractions (fesc, measured with 3 arcsec apertures) from 2
to 30 per cent. These galaxies have masses from 3 × 108 M⊙ to 1011 M⊙ and dust
attenuations E(B − V) = 0–0.5. Using stacking, we measure a median escape fraction
of 1.6 ± 0.5 per cent (4.0 ± 1.0 per cent without correcting Hα for dust), but
show that this depends on galaxy properties. The stacked fesc tends to decrease
with increasing star formation rate and dust attenuation. However, at the highest
masses and dust attenuations, we detect individual galaxies with fesc much higher
than the typical values from stacking, indicating significant scatter in the values
of fesc. Relations between fesc and UV slope are bimodal, with high fesc for either
the bluest or reddest galaxies. We speculate that this bimodality and large scatter
in the values of fesc is due to additional physical mechanisms such as outflows
facilitating fesc for dusty/massive systems. Lyα is significantly more extended
than Hα and the UV. fesc continues to increase up to at least 20 kpc (3σ, 40 kpc
[2σ]) for typical star-forming galaxies and thus the aperture is the most important
predictor of fesc.
acknowledgement: "We thank the anonymous referee for constructive comments and suggestions
which have improved the quality of this work. JM acknowledges the support of a Huygens
PhD fellowship from Leiden University. DS and JM acknowledge financial support from
the Netherlands Organization for Scientific research (NWO) through a Veni fellowship,
and DS from FCT through a FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010)
and from FCT grant PEst-OE/FIS/UI2751/2014. IO acknowledges support from the European
Research Council (ERC) in the form of Advanced Investigator Programme, COSMICISM,
321302. HR acknowledges support from the ERC Advanced Investigator programme NewClusters
321271. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator
programme DUSTYGAL 321334 and a Royal Society/Wolfson Merit Award. APA acknowledges
support from the Fundac¸ao para a Ciencia e para a Tecnologia (FCT) through the
Fellowship SFRH/BD/52706/2014.\r\nBased on observations made with the Isaac Newton
Telescope (proposals 2013AN002, 2013BN008, 2014AC88, 2014AN002, 2014BN006, 2014BC118)
operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio
del Roque de los Muchachos of the Instituto de Astrof´ısica de Canarias. We acknowledge
the tremendous work that has been done by both COSMOS and UKIDSS UDS/SXDF teams
in assembling such large, state-ofthe-art multi-wavelength data sets over such wide
areas, as those have been crucial for the results presented in this paper. The sample
of HAEs is publicly available from Sobral et al. (2013).\r\nWe have benefited greatly
from the publically available programming language PYTHON, including the NUMPY,
MATPLOTLIB, PYFITS, SCIPY (Jones et al. 2001; Hunter 2007; Van Der Walt, Colbert
& Varoquaux 2011) and ASTROPY (Astropy Collaboration et al. 2013) packages, the
imaging tools SEXTRACTOR, SWARP and SCAMP (Bertin & Arnouts 1996; Bertin 2006, 2010)
and the TOPCAT analysis program (Taylor 2005)."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Iván
full_name: Oteo, Iván
last_name: Oteo
- first_name: Philip
full_name: Best, Philip
last_name: Best
- first_name: Ian
full_name: Smail, Ian
last_name: Smail
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
- first_name: Ana
full_name: Paulino-Afonso, Ana
last_name: Paulino-Afonso
citation:
ama: 'Matthee JJ, Sobral D, Oteo I, et al. The CALYMHA survey: Lyα escape fraction
and its dependence on galaxy properties at z = 2.23. Monthly Notices of the
Royal Astronomical Society. 2016;458(1):449-467. doi:10.1093/mnras/stw322'
apa: 'Matthee, J. J., Sobral, D., Oteo, I., Best, P., Smail, I., Röttgering, H.,
& Paulino-Afonso, A. (2016). The CALYMHA survey: Lyα escape fraction and its
dependence on galaxy properties at z = 2.23. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stw322'
chicago: 'Matthee, Jorryt J, David Sobral, Iván Oteo, Philip Best, Ian Smail, Huub
Röttgering, and Ana Paulino-Afonso. “The CALYMHA Survey: Lyα Escape Fraction and
Its Dependence on Galaxy Properties at z = 2.23.” Monthly Notices of the Royal
Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw322.'
ieee: 'J. J. Matthee et al., “The CALYMHA survey: Lyα escape fraction and
its dependence on galaxy properties at z = 2.23,” Monthly Notices of the Royal
Astronomical Society, vol. 458, no. 1. Oxford University Press, pp. 449–467,
2016.'
ista: 'Matthee JJ, Sobral D, Oteo I, Best P, Smail I, Röttgering H, Paulino-Afonso
A. 2016. The CALYMHA survey: Lyα escape fraction and its dependence on galaxy
properties at z = 2.23. Monthly Notices of the Royal Astronomical Society. 458(1),
449–467.'
mla: 'Matthee, Jorryt J., et al. “The CALYMHA Survey: Lyα Escape Fraction and Its
Dependence on Galaxy Properties at z = 2.23.” Monthly Notices of the Royal
Astronomical Society, vol. 458, no. 1, Oxford University Press, 2016, pp.
449–67, doi:10.1093/mnras/stw322.'
short: J.J. Matthee, D. Sobral, I. Oteo, P. Best, I. Smail, H. Röttgering, A. Paulino-Afonso,
Monthly Notices of the Royal Astronomical Society 458 (2016) 449–467.
date_created: 2022-07-14T08:51:37Z
date_published: 2016-05-01T00:00:00Z
date_updated: 2022-08-19T08:17:19Z
day: '01'
doi: 10.1093/mnras/stw322
extern: '1'
external_id:
arxiv:
- '1602.02756'
intvolume: ' 458'
issue: '1'
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://arxiv.org/abs/1602.02756
month: '05'
oa: 1
oa_version: Preprint
page: 449-467
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties
at z = 2.23'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 458
year: '2016'
...
---
_id: '11579'
abstract:
- lang: eng
text: CR7 is the brightest z = 6.6 Ly α emitter (LAE) known to date, and spectroscopic
follow-up by Sobral et al. suggests that CR7 might host Population (Pop) III stars.
We examine this interpretation using cosmological hydrodynamical simulations.
Several simulated galaxies show the same ‘Pop III wave’ pattern observed in CR7.
However, to reproduce the extreme CR7 Ly α/He II1640 line luminosities (Lα/HeII)
a top-heavy initial mass function and a massive ( ≳ 107 M⊙) Pop III burst with
age ≲ 2 Myr are required. Assuming that the observed properties of Ly α and He II
emission are typical for Pop III, we predict that in the COSMOS/UDS/SA22 fields,
14 out of the 30 LAEs at z = 6.6 with Lα > 1043.3 erg s−1 should also host Pop
III stars producing an observable LHeII≳1042.7ergs−1. As an alternate explanation,
we explore the possibility that CR7 is instead powered by accretion on to a direct
collapse black hole. Our model predicts Lα, LHeII, and X-ray luminosities that
are in agreement with the observations. In any case, the observed properties of
CR7 indicate that this galaxy is most likely powered by sources formed from pristine
gas. We propose that further X-ray observations can distinguish between the two
above scenarios.
acknowledgement: SS acknowledges support from the Netherlands Organization for Scientific
research (NWO), VENI grant 639.041.233. RS acknowledges support from the European
Research Council under the European Union (FP/2007-2013)/ERC grant agreement no.
306476. DS acknowledges (i) financial support from the NWO through a Veni fellowship
and (ii) funding from FCT through a FCT Investigator Starting Grant and Start-up
Grant (IF/01154/2012/CP0189/CT0010) and from FCT grant PEstOE/FIS/UI2751/2014.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: A.
full_name: Pallottini, A.
last_name: Pallottini
- first_name: A.
full_name: Ferrara, A.
last_name: Ferrara
- first_name: F.
full_name: Pacucci, F.
last_name: Pacucci
- first_name: S.
full_name: Gallerani, S.
last_name: Gallerani
- first_name: S.
full_name: Salvadori, S.
last_name: Salvadori
- first_name: R.
full_name: Schneider, R.
last_name: Schneider
- first_name: D.
full_name: Schaerer, D.
last_name: Schaerer
- 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
citation:
ama: 'Pallottini A, Ferrara A, Pacucci F, et al. The brightest Lyα emitter: Pop
III or black hole? Monthly Notices of the Royal Astronomical Society. 2015;453(3):2465-2470.
doi:10.1093/mnras/stv1795'
apa: 'Pallottini, A., Ferrara, A., Pacucci, F., Gallerani, S., Salvadori, S., Schneider,
R., … Matthee, J. J. (2015). The brightest Lyα emitter: Pop III or black hole?
Monthly Notices of the Royal Astronomical Society. Oxford University Press.
https://doi.org/10.1093/mnras/stv1795'
chicago: 'Pallottini, A., A. Ferrara, F. Pacucci, S. Gallerani, S. Salvadori, R.
Schneider, D. Schaerer, D. Sobral, and Jorryt J Matthee. “The Brightest Lyα Emitter:
Pop III or Black Hole?” Monthly Notices of the Royal Astronomical Society.
Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv1795.'
ieee: 'A. Pallottini et al., “The brightest Lyα emitter: Pop III or black
hole?,” Monthly Notices of the Royal Astronomical Society, vol. 453, no.
3. Oxford University Press, pp. 2465–2470, 2015.'
ista: 'Pallottini A, Ferrara A, Pacucci F, Gallerani S, Salvadori S, Schneider R,
Schaerer D, Sobral D, Matthee JJ. 2015. The brightest Lyα emitter: Pop III or
black hole? Monthly Notices of the Royal Astronomical Society. 453(3), 2465–2470.'
mla: 'Pallottini, A., et al. “The Brightest Lyα Emitter: Pop III or Black Hole?”
Monthly Notices of the Royal Astronomical Society, vol. 453, no. 3, Oxford
University Press, 2015, pp. 2465–70, doi:10.1093/mnras/stv1795.'
short: A. Pallottini, A. Ferrara, F. Pacucci, S. Gallerani, S. Salvadori, R. Schneider,
D. Schaerer, D. Sobral, J.J. Matthee, Monthly Notices of the Royal Astronomical
Society 453 (2015) 2465–2470.
date_created: 2022-07-14T08:58:36Z
date_published: 2015-11-01T00:00:00Z
date_updated: 2022-08-19T08:19:23Z
day: '01'
doi: 10.1093/mnras/stv1795
extern: '1'
external_id:
arxiv:
- '1506.07173'
intvolume: ' 453'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- black hole physics
- 'stars: Population III'
- 'galaxies: high-redshift'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1506.07173
month: '11'
oa: 1
oa_version: Preprint
page: 2465-2470
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 brightest Lyα emitter: Pop III or black hole?'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 453
year: '2015'
...