---
_id: '11514'
abstract:
- lang: eng
text: We discuss the nature and physical properties of gas-mass selected galaxies
in the ALMA spectroscopic survey (ASPECS) of the Hubble Ultra Deep Field (HUDF).
We capitalize on the deep optical integral-field spectroscopy from the Multi Unit
Spectroscopic Explorer (MUSE) HUDF Survey and multiwavelength data to uniquely
associate all 16 line emitters, detected in the ALMA data without preselection,
with rotational transitions of carbon monoxide (CO). We identify 10 as CO(2–1)
at 1 < z < 2, 5 as CO(3–2) at 2 < z < 3, and 1 as CO(4–3) at z = 3.6. Using the
MUSE data as a prior, we identify two additional CO(2–1) emitters, increasing
the total sample size to 18. We infer metallicities consistent with (super-)solar
for the CO-detected galaxies at z ≤ 1.5, motivating our choice of a Galactic conversion
factor between CO luminosity and molecular gas mass for these galaxies. Using
deep Chandra imaging of the HUDF, we determine an X-ray AGN fraction of 20% and
60% among the CO emitters at z ∼ 1.4 and z ∼ 2.6, respectively. Being a CO-flux-limited
survey, ASPECS-LP detects molecular gas in galaxies on, above, and below the main
sequence (MS) at z ∼ 1.4. For stellar masses ≥1010 (1010.5) ${M}_{\odot }$, we
detect about 40% (50%) of all galaxies in the HUDF at 1 < z < 2 (2 < z < 3). The
combination of ALMA and MUSE integral-field spectroscopy thus enables an unprecedented
view of MS galaxies during the peak of galaxy formation.
acknowledgement: "We are grateful to the referee for providing a constructive report.
L.A.B. wants to thank Madusha L.P. Gunawardhana for her help with platefit. Based
on observations collected at the European Southern Observatory under ESO programme(s):
094.A-2089(B), 095.A-0010(A), 096.A-0045(A), and 096.A-0045(B). This paper makes
use of the following ALMA data: ADS/JAO.ALMA#2016.1.00324.L. ALMA is a partnership
of ESO (representing its member states), NSF (USA) and NINS (Japan), together with
NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation
with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO,
and NAOJ. The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated Universities,
Inc.\r\n\r\n\"Este trabajo contó con el apoyo de CONICYT+Programa de Astronomía+
Fondo CHINA-CONICYT\" J.G-L. acknowledges partial support from ALMA-CONICYT project
31160033. F.E.B. acknowledges support from CONICYT grant Basal AFB-170002 (FEB),
and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative
through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS
(FEB). J.B. acknowledges support by Fundação para a Ciência e a Tecnologia (FCT)
through national funds (UID/FIS/04434/2013) and Investigador FCT contract IF/01654/2014/CP1215/CT0003.,
and by FEDER through COMPETE2020 (POCI-01-0145-FEDER-007672). T.D-S. acknowledges
support from ALMA-CONYCIT project 31130005 and FONDECYT project 1151239. J.H. acknowledges
support of the VIDI research programme with project number 639.042.611, which is
(partly) financed by the Netherlands Organization for Scientific Research (NWO).
D.R. acknowledges support from the National Science Foundation under grant No. AST-1614213.
I.R.S. acknowledges support from the ERC Advanced Grant DUSTYGAL (321334) and STFC
(ST/P000541/1)\r\n\r\nWork on Gnuastro has been funded by the Japanese MEXT scholarship
and its Grant-in-Aid for Scientific Research (21244012, 24253003), the ERC advanced
grant 339659-MUSICOS, European Union's Horizon 2020 research and innovation programme
under Marie Sklodowska-Curie grant agreement No. 721463 to the SUNDIAL ITN, and
from the Spanish MINECO under grant No. AYA2016-76219-P."
article_number: '140'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Leindert A.
full_name: Boogaard, Leindert A.
last_name: Boogaard
- first_name: Roberto
full_name: Decarli, Roberto
last_name: Decarli
- first_name: Jorge
full_name: González-López, Jorge
last_name: González-López
- first_name: Paul
full_name: van der Werf, Paul
last_name: van der Werf
- first_name: Fabian
full_name: Walter, Fabian
last_name: Walter
- first_name: Rychard
full_name: Bouwens, Rychard
last_name: Bouwens
- first_name: Manuel
full_name: Aravena, Manuel
last_name: Aravena
- first_name: Chris
full_name: Carilli, Chris
last_name: Carilli
- first_name: Franz Erik
full_name: Bauer, Franz Erik
last_name: Bauer
- first_name: Jarle
full_name: Brinchmann, Jarle
last_name: Brinchmann
- first_name: Thierry
full_name: Contini, Thierry
last_name: Contini
- first_name: Pierre
full_name: Cox, Pierre
last_name: Cox
- first_name: Elisabete
full_name: da Cunha, Elisabete
last_name: da Cunha
- first_name: Emanuele
full_name: Daddi, Emanuele
last_name: Daddi
- first_name: Tanio
full_name: Díaz-Santos, Tanio
last_name: Díaz-Santos
- first_name: Jacqueline
full_name: Hodge, Jacqueline
last_name: Hodge
- first_name: Hanae
full_name: Inami, Hanae
last_name: Inami
- first_name: Rob
full_name: Ivison, Rob
last_name: Ivison
- first_name: Michael
full_name: Maseda, Michael
last_name: Maseda
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Pascal
full_name: Oesch, Pascal
last_name: Oesch
- first_name: Gergö
full_name: Popping, Gergö
last_name: Popping
- first_name: Dominik
full_name: Riechers, Dominik
last_name: Riechers
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
- first_name: Sander
full_name: Schouws, Sander
last_name: Schouws
- first_name: Ian
full_name: Smail, Ian
last_name: Smail
- first_name: Axel
full_name: Weiss, Axel
last_name: Weiss
- first_name: Lutz
full_name: Wisotzki, Lutz
last_name: Wisotzki
- first_name: Roland
full_name: Bacon, Roland
last_name: Bacon
- first_name: Paulo C.
full_name: Cortes, Paulo C.
last_name: Cortes
- first_name: Hans-Walter
full_name: Rix, Hans-Walter
last_name: Rix
- first_name: Rachel S.
full_name: Somerville, Rachel S.
last_name: Somerville
- first_name: Mark
full_name: Swinbank, Mark
last_name: Swinbank
- first_name: Jeff
full_name: Wagg, Jeff
last_name: Wagg
citation:
ama: 'Boogaard LA, Decarli R, González-López J, et al. The ALMA spectroscopic survey
in the HUDF: Nature and physical properties of gas-mass selected galaxies using
MUSE spectroscopy. The Astrophysical Journal. 2019;882(2). doi:10.3847/1538-4357/ab3102'
apa: 'Boogaard, L. A., Decarli, R., González-López, J., van der Werf, P., Walter,
F., Bouwens, R., … Wagg, J. (2019). The ALMA spectroscopic survey in the HUDF:
Nature and physical properties of gas-mass selected galaxies using MUSE spectroscopy.
The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ab3102'
chicago: 'Boogaard, Leindert A., Roberto Decarli, Jorge González-López, Paul van
der Werf, Fabian Walter, Rychard Bouwens, Manuel Aravena, et al. “The ALMA Spectroscopic
Survey in the HUDF: Nature and Physical Properties of Gas-Mass Selected Galaxies
Using MUSE Spectroscopy.” The Astrophysical Journal. IOP Publishing, 2019.
https://doi.org/10.3847/1538-4357/ab3102.'
ieee: 'L. A. Boogaard et al., “The ALMA spectroscopic survey in the HUDF:
Nature and physical properties of gas-mass selected galaxies using MUSE spectroscopy,”
The Astrophysical Journal, vol. 882, no. 2. IOP Publishing, 2019.'
ista: 'Boogaard LA, Decarli R, González-López J, van der Werf P, Walter F, Bouwens
R, Aravena M, Carilli C, Bauer FE, Brinchmann J, Contini T, Cox P, da Cunha E,
Daddi E, Díaz-Santos T, Hodge J, Inami H, Ivison R, Maseda M, Matthee JJ, Oesch
P, Popping G, Riechers D, Schaye J, Schouws S, Smail I, Weiss A, Wisotzki L, Bacon
R, Cortes PC, Rix H-W, Somerville RS, Swinbank M, Wagg J. 2019. The ALMA spectroscopic
survey in the HUDF: Nature and physical properties of gas-mass selected galaxies
using MUSE spectroscopy. The Astrophysical Journal. 882(2), 140.'
mla: 'Boogaard, Leindert A., et al. “The ALMA Spectroscopic Survey in the HUDF:
Nature and Physical Properties of Gas-Mass Selected Galaxies Using MUSE Spectroscopy.”
The Astrophysical Journal, vol. 882, no. 2, 140, IOP Publishing, 2019,
doi:10.3847/1538-4357/ab3102.'
short: L.A. Boogaard, R. Decarli, J. González-López, P. van der Werf, F. Walter,
R. Bouwens, M. Aravena, C. Carilli, F.E. Bauer, J. Brinchmann, T. Contini, P.
Cox, E. da Cunha, E. Daddi, T. Díaz-Santos, J. Hodge, H. Inami, R. Ivison, M.
Maseda, J.J. Matthee, P. Oesch, G. Popping, D. Riechers, J. Schaye, S. Schouws,
I. Smail, A. Weiss, L. Wisotzki, R. Bacon, P.C. Cortes, H.-W. Rix, R.S. Somerville,
M. Swinbank, J. Wagg, The Astrophysical Journal 882 (2019).
date_created: 2022-07-06T13:31:35Z
date_published: 2019-09-11T00:00:00Z
date_updated: 2022-07-19T09:50:55Z
day: '11'
doi: 10.3847/1538-4357/ab3102
extern: '1'
external_id:
arxiv:
- '1903.09167'
intvolume: ' 882'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1903.09167
month: '09'
oa: 1
oa_version: Preprint
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The ALMA spectroscopic survey in the HUDF: Nature and physical properties
of gas-mass selected galaxies using MUSE spectroscopy'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 882
year: '2019'
...
---
_id: '11515'
abstract:
- lang: eng
text: We present new deep ALMA and Hubble Space Telescope (HST)/WFC3 observations
of MASOSA and VR7, two luminous Lyα emitters (LAEs) at z = 6.5, for which the
UV continuum levels differ by a factor of four. No IR dust continuum emission
is detected in either, indicating little amounts of obscured star formation and/or
high dust temperatures. MASOSA, with a UV luminosity M1500 = −20.9, compact size,
and very high Lyα ${\mathrm{EW}}_{0}\approx 145\,\mathring{\rm A} $, is undetected
in [C ii] to a limit of L[C ii] < 2.2 × 107 L⊙, implying a metallicity Z ≲ 0.07
Z⊙. Intriguingly, our HST data indicate a red UV slope β = −1.1 ± 0.7, at odds
with the low dust content. VR7, which is a bright (M1500 = −22.4) galaxy with
moderate color (β = −1.4 ± 0.3) and Lyα EW0 = 34 Å, is clearly detected in [C
ii] emission (S/N = 15). VR7's rest-frame UV morphology can be described by two
components separated by ≈1.5 kpc and is globally more compact than the [C ii]
emission. The global [C ii]/UV ratio indicates Z ≈ 0.2 Z⊙, but there are large
variations in the UV/[C ii] ratio on kiloparsec scales. We also identify diffuse,
possibly outflowing, [C ii]-emitting gas at ≈100 km s−1 with respect to the peak.
VR7 appears to be assembling its components at a slightly more evolved stage than
other luminous LAEs, with outflows already shaping its direct environment at z
∼ 7. Our results further indicate that the global [C ii]−UV relation steepens
at SFR < 30 M⊙ yr−1, naturally explaining why the [C ii]/UV ratio is anticorrelated
with Lyα EW in many, but not all, observed LAEs.
acknowledgement: 'We thank the anonymous referee for constructive comments and suggestions.
We thank Max Gronke for comments on an earlier version of this paper. L.V. acknowledges
funding from the European Union’s Horizon 2020 research and innovation program under
the Marie Skłodowska-Curie grant agreement No. 746119. This paper makes use of the
following ALMA data: ADS/JAO.ALMA#2017.1.01451.S. ALMA is a partnership of ESO (representing
its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC
and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic
of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. Based
on observations obtained with the Very Large Telescope, programs 294.A-5018, 097.A-0943,
and 99.A-0462. Based on observations made with the NASA/ESA Hubble Space Telescope,
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 program
No. 14699.'
article_number: '124'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: D.
full_name: Sobral, D.
last_name: Sobral
- first_name: L. A.
full_name: Boogaard, L. A.
last_name: Boogaard
- first_name: H.
full_name: Röttgering, H.
last_name: Röttgering
- first_name: L.
full_name: Vallini, L.
last_name: Vallini
- first_name: A.
full_name: Ferrara, A.
last_name: Ferrara
- first_name: A.
full_name: Paulino-Afonso, A.
last_name: Paulino-Afonso
- first_name: F.
full_name: Boone, F.
last_name: Boone
- first_name: D.
full_name: Schaerer, D.
last_name: Schaerer
- first_name: B.
full_name: Mobasher, B.
last_name: Mobasher
citation:
ama: Matthee JJ, Sobral D, Boogaard LA, et al. Resolved UV and [C ii] structures
of luminous galaxies within the epoch of reionization. The Astrophysical Journal.
2019;881(2). doi:10.3847/1538-4357/ab2f81
apa: Matthee, J. J., Sobral, D., Boogaard, L. A., Röttgering, H., Vallini, L., Ferrara,
A., … Mobasher, B. (2019). Resolved UV and [C ii] structures of luminous galaxies
within the epoch of reionization. The Astrophysical Journal. IOP Publishing.
https://doi.org/10.3847/1538-4357/ab2f81
chicago: Matthee, Jorryt J, D. Sobral, L. A. Boogaard, H. Röttgering, L. Vallini,
A. Ferrara, A. Paulino-Afonso, F. Boone, D. Schaerer, and B. Mobasher. “Resolved
UV and [C Ii] Structures of Luminous Galaxies within the Epoch of Reionization.”
The Astrophysical Journal. IOP Publishing, 2019. https://doi.org/10.3847/1538-4357/ab2f81.
ieee: J. J. Matthee et al., “Resolved UV and [C ii] structures of luminous
galaxies within the epoch of reionization,” The Astrophysical Journal,
vol. 881, no. 2. IOP Publishing, 2019.
ista: Matthee JJ, Sobral D, Boogaard LA, Röttgering H, Vallini L, Ferrara A, Paulino-Afonso
A, Boone F, Schaerer D, Mobasher B. 2019. Resolved UV and [C ii] structures of
luminous galaxies within the epoch of reionization. The Astrophysical Journal.
881(2), 124.
mla: Matthee, Jorryt J., et al. “Resolved UV and [C Ii] Structures of Luminous Galaxies
within the Epoch of Reionization.” The Astrophysical Journal, vol. 881,
no. 2, 124, IOP Publishing, 2019, doi:10.3847/1538-4357/ab2f81.
short: J.J. Matthee, D. Sobral, L.A. Boogaard, H. Röttgering, L. Vallini, A. Ferrara,
A. Paulino-Afonso, F. Boone, D. Schaerer, B. Mobasher, The Astrophysical Journal
881 (2019).
date_created: 2022-07-06T13:38:15Z
date_published: 2019-08-21T00:00:00Z
date_updated: 2022-08-18T10:19:48Z
day: '21'
doi: 10.3847/1538-4357/ab2f81
extern: '1'
external_id:
arxiv:
- '1903.08171'
intvolume: ' 881'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1903.08171
month: '08'
oa: 1
oa_version: Preprint
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Resolved UV and [C ii] structures of luminous galaxies within the epoch of
reionization
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 881
year: '2019'
...
---
_id: '11516'
abstract:
- lang: eng
text: The well-known quasar SDSS J095253.83+011421.9 (J0952+0114) at z = 3.02 has
one of the most peculiar spectra discovered so far, showing the presence of narrow
Lyα and broad metal emission lines. Although recent studies have suggested that
a proximate damped Lyα absorption (PDLA) system causes this peculiar spectrum,
the origin of the gas associated with the PDLA is unknown. Here we report the
results of observations with the Multi Unit Spectroscopic Explorer (MUSE) that
reveal a new giant (≈100 physical kpc) Lyα nebula. The detailed analysis of the
Lyα velocity, velocity dispersion, and surface brightness profiles suggests that
the J0952+0114 Lyα nebula shares similar properties with other QSO nebulae previously
detected with MUSE, implying that the PDLA in J0952+0144 is covering only a small
fraction of the solid angle of the QSO emission. We also detected bright and spectrally
narrow C iv λ1550 and He ii λ1640 extended emission around J0952+0114 with velocity
centroids similar to the peak of the extended and central narrow Lyα emission.
The presence of a peculiarly bright, unresolved, and relatively broad He ii λ1640
emission in the central region at exactly the same PDLA redshift hints at the
possibility that the PDLA originates in a clumpy outflow with a bulk velocity
of about 500 km s−1. The smaller velocity dispersion of the large-scale Lyα emission
suggests that the high-speed outflow is confined to the central region. Lastly,
the derived spatially resolved He ii/Lyα and C iv/Lyα maps show a positive gradient
with the distance to the QSO, hinting at a non-homogeneous distribution of the
ionization parameter.
acknowledgement: We thank Lutz Wisotzki for stimulating discussions. This work is
based on observations taken at ESO/VLT in Paranal and we would like to thank the
ESO staff for their assistance and support during the MUSE GTO campaigns. This work
was supported by the Swiss National Science Foundation. This research made use of
Astropy, a community-developed core PYTHON package for astronomy (Astropy Collaboration
et al. 2013), NumPy and SciPy (Oliphant 2007), Matplotlib (Hunter 2007), IPython
(Perez & Granger 2007), and of the NASA Astrophysics Data System Bibliographic Services.
S.C. and G.P. gratefully acknowledge support from Swiss National Science Foundation
grant PP00P2−163824. A.F. acknowledges support from the ERC via Advanced Grant under
grants agreement no. 339659-MUSICOS. J.B. acknowledges support by FCT/MCTES through
national funds by grant UID/FIS/04434/2019 and through Investigador FCT Contract
No. IF/01654/2014/CP1215/CT0003. S.D.J. is supported by a NASA Hubble Fellowship
(HST-HF2-51375.001-A). T.N. acknowledges the Nederlandse Organisatie voor Wetenschappelijk
Onderzoek (NWO) top grant TOP1.16.057.
article_number: '47'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Raffaella Anna
full_name: Marino, Raffaella Anna
last_name: Marino
- first_name: Sebastiano
full_name: Cantalupo, Sebastiano
last_name: Cantalupo
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Simon J.
full_name: Lilly, Simon J.
last_name: Lilly
- first_name: Sofia
full_name: Gallego, Sofia
last_name: Gallego
- first_name: Ruari
full_name: Mackenzie, Ruari
last_name: Mackenzie
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Jarle
full_name: Brinchmann, Jarle
last_name: Brinchmann
- first_name: Nicolas
full_name: Bouché, Nicolas
last_name: Bouché
- first_name: Anna
full_name: Feltre, Anna
last_name: Feltre
- first_name: Sowgat
full_name: Muzahid, Sowgat
last_name: Muzahid
- first_name: Ilane
full_name: Schroetter, Ilane
last_name: Schroetter
- first_name: Sean D.
full_name: Johnson, Sean D.
last_name: Johnson
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
citation:
ama: Marino RA, Cantalupo S, Pezzulli G, et al. A giant Lyα nebula and a small-scale
clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE.
The Astrophysical Journal. 2019;880(1). doi:10.3847/1538-4357/ab2881
apa: Marino, R. A., Cantalupo, S., Pezzulli, G., Lilly, S. J., Gallego, S., Mackenzie,
R., … Nanayakkara, T. (2019). A giant Lyα nebula and a small-scale clumpy outflow
in the system of the exotic quasar J0952+0114 unveiled by MUSE. The Astrophysical
Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ab2881
chicago: Marino, Raffaella Anna, Sebastiano Cantalupo, Gabriele Pezzulli, Simon
J. Lilly, Sofia Gallego, Ruari Mackenzie, Jorryt J Matthee, et al. “A Giant Lyα
Nebula and a Small-Scale Clumpy Outflow in the System of the Exotic Quasar J0952+0114
Unveiled by MUSE.” The Astrophysical Journal. IOP Publishing, 2019. https://doi.org/10.3847/1538-4357/ab2881.
ieee: R. A. Marino et al., “A giant Lyα nebula and a small-scale clumpy outflow
in the system of the exotic quasar J0952+0114 unveiled by MUSE,” The Astrophysical
Journal, vol. 880, no. 1. IOP Publishing, 2019.
ista: Marino RA, Cantalupo S, Pezzulli G, Lilly SJ, Gallego S, Mackenzie R, Matthee
JJ, Brinchmann J, Bouché N, Feltre A, Muzahid S, Schroetter I, Johnson SD, Nanayakkara
T. 2019. A giant Lyα nebula and a small-scale clumpy outflow in the system of
the exotic quasar J0952+0114 unveiled by MUSE. The Astrophysical Journal. 880(1),
47.
mla: Marino, Raffaella Anna, et al. “A Giant Lyα Nebula and a Small-Scale Clumpy
Outflow in the System of the Exotic Quasar J0952+0114 Unveiled by MUSE.” The
Astrophysical Journal, vol. 880, no. 1, 47, IOP Publishing, 2019, doi:10.3847/1538-4357/ab2881.
short: R.A. Marino, S. Cantalupo, G. Pezzulli, S.J. Lilly, S. Gallego, R. Mackenzie,
J.J. Matthee, J. Brinchmann, N. Bouché, A. Feltre, S. Muzahid, I. Schroetter,
S.D. Johnson, T. Nanayakkara, The Astrophysical Journal 880 (2019).
date_created: 2022-07-06T13:50:33Z
date_published: 2019-07-24T00:00:00Z
date_updated: 2022-08-18T10:20:18Z
day: '24'
doi: 10.3847/1538-4357/ab2881
extern: '1'
external_id:
arxiv:
- '1906.06347'
intvolume: ' 880'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1906.06347
month: '07'
oa: 1
oa_version: Preprint
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic
quasar J0952+0114 unveiled by MUSE
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 880
year: '2019'
...
---
_id: '11517'
abstract:
- lang: eng
text: To understand star formation in galaxies, we investigate the star formation
rate (SFR) surface density (ΣSFR) profiles for galaxies, based on a well-defined
sample of 976 star-forming MaNGA galaxies. We find that the typical ΣSFR profiles
within 1.5Re of normal SF galaxies can be well described by an exponential function
for different stellar mass intervals, while the sSFR profile shows positive gradients,
especially for more massive SF galaxies. This is due to the more pronounced central
cores or bulges rather than the onset of a `quenching' process. While galaxies
that lie significantly above (or below) the star formation main sequence (SFMS)
show overall an elevation (or suppression) of ΣSFR at all radii, this central
elevation (or suppression) is more pronounced in more massive galaxies. The degree
of central enhancement and suppression is quite symmetric, suggesting that both
the elevation and suppression of star formation are following the same physical
processes. Furthermore, we find that the dispersion in ΣSFR within and across
the population is found to be tightly correlated with the inferred gas depletion
time, whether based on the stellar surface mass density or the orbital dynamical
time. This suggests that we are seeing the response of a simple gas-regulator
system to variations in the accretion rate. This is explored using a heuristic
model that can quantitatively explain the dependence of σ(ΣSFR) on gas depletion
timescale. Variations in accretion rate are progressively more damped out in regions
of low star-formation efficiency leading to a reduced amplitude of variations
in star-formation.
acknowledgement: "We are grateful to the anonymous referee for their thoughtful and
constructive review of the paper and their several suggestions (including the analysis
of Section 3.4), which have improved the paper. This research has been supported
by the Swiss National Science Foundation.\r\n\r\nFunding for the Sloan Digital Sky
Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department
of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges
support and resources from the Center for High-Performance Computing at the University
of Utah. The SDSS website is www.sdss.org.\r\n\r\nSDSS-IV is managed by the Astrophysical
Research Consortium for the Participating Institutions of the SDSS Collaboration,
including the Brazilian Participation Group, the Carnegie Institution for Science,
Carnegie Mellon University, the Chilean Participation Group, the French Participation
Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofísica de
Canarias, the Johns Hopkins University, Kavli Institute for the Physics and Mathematics
of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory,
Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie
(MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut
für Extraterrestrische Physik (MPE), National Astronomical Observatory of China,
New Mexico State University, New York University, University of Notre Dame, Observatário
Nacional/MCTI, the Ohio State University, Pennsylvania State University, Shanghai
Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional
Autónoma de México, University of Arizona, University of Colorado Boulder, University
of Oxford, University of Portsmouth, University of Utah, University of Virginia,
University of Washington, University of Wisconsin, Vanderbilt University, and Yale
University"
article_number: '132'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Enci
full_name: Wang, Enci
last_name: Wang
- first_name: Simon J.
full_name: Lilly, Simon J.
last_name: Lilly
- first_name: Gabriele
full_name: Pezzulli, Gabriele
last_name: Pezzulli
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
citation:
ama: Wang E, Lilly SJ, Pezzulli G, Matthee JJ. On the elevation and suppression
of star formation within galaxies. The Astrophysical Journal. 2019;877(2).
doi:10.3847/1538-4357/ab1c5b
apa: Wang, E., Lilly, S. J., Pezzulli, G., & Matthee, J. J. (2019). On the elevation
and suppression of star formation within galaxies. The Astrophysical Journal.
IOP Publishing. https://doi.org/10.3847/1538-4357/ab1c5b
chicago: Wang, Enci, Simon J. Lilly, Gabriele Pezzulli, and Jorryt J Matthee. “On
the Elevation and Suppression of Star Formation within Galaxies.” The Astrophysical
Journal. IOP Publishing, 2019. https://doi.org/10.3847/1538-4357/ab1c5b.
ieee: E. Wang, S. J. Lilly, G. Pezzulli, and J. J. Matthee, “On the elevation and
suppression of star formation within galaxies,” The Astrophysical Journal,
vol. 877, no. 2. IOP Publishing, 2019.
ista: Wang E, Lilly SJ, Pezzulli G, Matthee JJ. 2019. On the elevation and suppression
of star formation within galaxies. The Astrophysical Journal. 877(2), 132.
mla: Wang, Enci, et al. “On the Elevation and Suppression of Star Formation within
Galaxies.” The Astrophysical Journal, vol. 877, no. 2, 132, IOP Publishing,
2019, doi:10.3847/1538-4357/ab1c5b.
short: E. Wang, S.J. Lilly, G. Pezzulli, J.J. Matthee, The Astrophysical Journal
877 (2019).
date_created: 2022-07-07T08:38:24Z
date_published: 2019-06-04T00:00:00Z
date_updated: 2022-08-18T10:19:08Z
day: '04'
doi: 10.3847/1538-4357/ab1c5b
extern: '1'
external_id:
arxiv:
- '1901.10276'
intvolume: ' 877'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1901.10276
month: '06'
oa: 1
oa_version: Preprint
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: On the elevation and suppression of star formation within galaxies
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 877
year: '2019'
...
---
_id: '11535'
abstract:
- lang: eng
text: We investigate the clustering and halo properties of ∼5000 Ly α-selected emission-line
galaxies (LAEs) from the Slicing COSMOS 4K (SC4K) and from archival NB497 imaging
of SA22 split in 15 discrete redshift slices between z ∼ 2.5 and 6. We measure
clustering lengths of r0 ∼ 3–6 h−1 Mpc and typical halo masses of ∼1011 M⊙ for
our narrowband-selected LAEs with typical LLy α ∼ 1042–43 erg s−1. The intermediate-band-selected
LAEs are observed to have r0 ∼ 3.5–15 h−1 Mpc with typical halo masses of ∼1011–12
M⊙ and typical LLy α ∼ 1043–43.6 erg s−1. We find a strong, redshift-independent
correlation between halo mass and Ly α luminosity normalized by the characteristic
Ly α luminosity, L⋆(z). The faintest LAEs (L ∼ 0.1 L⋆(z)) typically identified
by deep narrowband surveys are found in 1010 M⊙ haloes and the brightest LAEs
(L ∼ 7 L⋆(z)) are found in ∼5 × 1012 M⊙ haloes. A dependency on the rest-frame
1500 Å UV luminosity, MUV, is also observed where the halo masses increase from
1011 to 1013 M⊙ for MUV ∼ −19 to −23.5 mag. Halo mass is also observed to increase
from 109.8 to 1012 M⊙ for dust-corrected UV star formation rates from ∼0.6 to
10 M⊙ yr−1 and continues to increase up to 1013 M⊙ in halo mass, where the majority
of those sources are active galactic nuclei. All the trends we observe are found
to be redshift independent. Our results reveal that LAEs are the likely progenitors
of a wide range of galaxies depending on their luminosity, from dwarf-like, to
Milky Way-type, to bright cluster galaxies. LAEs therefore provide unique insight
into the early formation and evolution of the galaxies we observe in the local
Universe.
acknowledgement: We thank the anonymous referee for their useful comments and suggestions
that helped improve this study. AAK acknowledges that this work was supported by
NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant
NNX16AO92H. JM acknowledges support from the ETH Zwicky fellowship. RKC acknowledges
funding from STFC via a studentship. APA acknowledges support from the Fundac¸ao
para a Ci ˜ encia e a Tecnologia FCT through the fellowship PD/BD/52706/2014 and
the research grant UID/FIS/04434/2013. JC and SS both acknowledge their support
from the Lancaster University PhD Fellowship. We have benefited greatly from the
publicly available programming language PYTHON, including the NUMPY, SCIPY, MATPLOTLIB,
SCIKIT-LEARN, and ASTROPY packages, as well as the TOPCAT analysis program. The
SC4K samples used in this paper are all publicly available for use by the community
(Sobral et al. 2018a). The catalogue is also available on the COSMOS IPAC website
(https://irsa.ipac.caltech.edu/data/COSMOS/overview.html).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: A A
full_name: Khostovan, A A
last_name: Khostovan
- first_name: D
full_name: Sobral, D
last_name: Sobral
- first_name: B
full_name: Mobasher, B
last_name: Mobasher
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: R K
full_name: Cochrane, R K
last_name: Cochrane
- first_name: N
full_name: Chartab, N
last_name: Chartab
- first_name: M
full_name: Jafariyazani, M
last_name: Jafariyazani
- first_name: A
full_name: Paulino-Afonso, A
last_name: Paulino-Afonso
- first_name: S
full_name: Santos, S
last_name: Santos
- first_name: J
full_name: Calhau, J
last_name: Calhau
citation:
ama: 'Khostovan AA, Sobral D, Mobasher B, et al. The clustering of typical Ly α emitters
from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly
Notices of the Royal Astronomical Society. 2019;489(1):555-573. doi:10.1093/mnras/stz2149'
apa: 'Khostovan, A. A., Sobral, D., Mobasher, B., Matthee, J. J., Cochrane, R. K.,
Chartab, N., … Calhau, J. (2019). The clustering of typical Ly α emitters from
z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices
of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz2149'
chicago: 'Khostovan, A A, D Sobral, B Mobasher, Jorryt J Matthee, R K Cochrane,
N Chartab, M Jafariyazani, A Paulino-Afonso, S Santos, and J Calhau. “The Clustering
of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV
Luminosities.” Monthly Notices of the Royal Astronomical Society. Oxford
University Press, 2019. https://doi.org/10.1093/mnras/stz2149.'
ieee: 'A. A. Khostovan et al., “The clustering of typical Ly α emitters from
z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities,” Monthly Notices
of the Royal Astronomical Society, vol. 489, no. 1. Oxford University Press,
pp. 555–573, 2019.'
ista: 'Khostovan AA, Sobral D, Mobasher B, Matthee JJ, Cochrane RK, Chartab N, Jafariyazani
M, Paulino-Afonso A, Santos S, Calhau J. 2019. The clustering of typical Ly α emitters
from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices
of the Royal Astronomical Society. 489(1), 555–573.'
mla: 'Khostovan, A. A., et al. “The Clustering of Typical Ly α Emitters from z ∼
2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” Monthly Notices
of the Royal Astronomical Society, vol. 489, no. 1, Oxford University Press,
2019, pp. 555–73, doi:10.1093/mnras/stz2149.'
short: A.A. Khostovan, D. Sobral, B. Mobasher, J.J. Matthee, R.K. Cochrane, N. Chartab,
M. Jafariyazani, A. Paulino-Afonso, S. Santos, J. Calhau, Monthly Notices of the
Royal Astronomical Society 489 (2019) 555–573.
date_created: 2022-07-07T13:01:03Z
date_published: 2019-10-01T00:00:00Z
date_updated: 2022-08-19T06:38:42Z
day: '01'
doi: 10.1093/mnras/stz2149
extern: '1'
external_id:
arxiv:
- '1811.00556'
intvolume: ' 489'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: haloes'
- 'galaxies: high-redshift'
- 'galaxies: star formation'
- 'cosmology: observations'
- large-scale structure of Universe
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1811.00556
month: '10'
oa: 1
oa_version: Preprint
page: 555-573
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend
on Ly α and UV luminosities'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 489
year: '2019'
...
---
_id: '11540'
abstract:
- lang: eng
text: Observations have revealed that the star formation rate (SFR) and stellar
mass (Mstar) of star-forming galaxies follow a tight relation known as the galaxy
main sequence. However, what physical information is encoded in this relation
is under debate. Here, we use the EAGLE cosmological hydrodynamical simulation
to study the mass dependence, evolution, and origin of scatter in the SFR–Mstar
relation. At z = 0, we find that the scatter decreases slightly with stellar mass
from 0.35 dex at Mstar ≈ 109 M⊙ to 0.30 dex at Mstar ≳ 1010.5 M⊙. The scatter
decreases from z = 0 to z = 5 by 0.05 dex at Mstar ≳ 1010 M⊙ and by 0.15 dex for
lower masses. We show that the scatter at z = 0.1 originates from a combination
of fluctuations on short time-scales (ranging from 0.2–2 Gyr) that are presumably
associated with self-regulation from cooling, star formation, and outflows, but
is dominated by long time-scale (∼10 Gyr) variations related to differences in
halo formation times. Shorter time-scale fluctuations are relatively more important
for lower mass galaxies. At high masses, differences in black hole formation efficiency
cause additional scatter, but also diminish the scatter caused by different halo
formation times. While individual galaxies cross the main sequence multiple times
during their evolution, they fluctuate around tracks associated with their halo
properties, i.e. galaxies above/below the main sequence at z = 0.1 tend to have
been above/below the main sequence for ≫1 Gyr.
acknowledgement: JM acknowledges the support of a Huygens PhD fellowship from Leiden
University. We thank Camila Correa for help analysing snipshot merger trees. We
thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann,
Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and
suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade
of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and
ideas. We have benefited from the public available programming language PYTHON,
including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT
analysis tool (Taylor 2013).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
citation:
ama: Matthee JJ, Schaye J. The origin of scatter in the star formation rate–stellar
mass relation. Monthly Notices of the Royal Astronomical Society. 2019;484(1):915-932.
doi:10.1093/mnras/stz030
apa: Matthee, J. J., & Schaye, J. (2019). The origin of scatter in the star
formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stz030
chicago: Matthee, Jorryt J, and Joop Schaye. “The Origin of Scatter in the Star
Formation Rate–Stellar Mass Relation.” Monthly Notices of the Royal Astronomical
Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz030.
ieee: J. J. Matthee and J. Schaye, “The origin of scatter in the star formation
rate–stellar mass relation,” Monthly Notices of the Royal Astronomical Society,
vol. 484, no. 1. Oxford University Press, pp. 915–932, 2019.
ista: Matthee JJ, Schaye J. 2019. The origin of scatter in the star formation rate–stellar
mass relation. Monthly Notices of the Royal Astronomical Society. 484(1), 915–932.
mla: Matthee, Jorryt J., and Joop Schaye. “The Origin of Scatter in the Star Formation
Rate–Stellar Mass Relation.” Monthly Notices of the Royal Astronomical Society,
vol. 484, no. 1, Oxford University Press, 2019, pp. 915–32, doi:10.1093/mnras/stz030.
short: J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society
484 (2019) 915–932.
date_created: 2022-07-08T07:48:31Z
date_published: 2019-03-01T00:00:00Z
date_updated: 2022-08-19T06:42:43Z
day: '01'
doi: 10.1093/mnras/stz030
extern: '1'
external_id:
arxiv:
- '1805.05956'
intvolume: ' 484'
issue: '1'
keyword:
- Space and Planetary Science
- 'Astronomy and Astrophysics : galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: star formation'
- 'cosmology: theory'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1805.05956
month: '03'
oa: 1
oa_version: Preprint
page: 915-932
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The origin of scatter in the star formation rate–stellar mass relation
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 484
year: '2019'
...
---
_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: '11613'
abstract:
- lang: eng
text: Over 2,000 stars were observed for 1 month with a high enough cadence in order
to look for acoustic modes during the survey phase of the Kepler mission. Solar-like
oscillations have been detected in about 540 stars. The question of why no oscillations
were detected in the remaining stars is still open. Previous works explained the
non-detection of modes with the high level of magnetic activity of the stars.
However, the sample of stars studied contained some classical pulsators and red
giants that could have biased the results. In this work, we revisit this analysis
on a cleaner sample of main-sequence solar-like stars that consists of 1,014 stars.
First we compute the predicted amplitude of the modes of that sample and for the
stars with detected oscillation and compare it to the noise at high frequency
in the power spectrum. We find that the stars with detected modes have an amplitude
to noise ratio larger than 0.94. We measure reliable rotation periods and the
associated photometric magnetic index for 684 stars out of the full sample and
in particular for 323 stars where the amplitude of the modes is predicted to be
high enough to be detected. We find that among these 323 stars 32% of them have
a level of magnetic activity larger than the Sun during its maximum activity,
explaining the non-detection of acoustic modes. Interestingly, magnetic activity
cannot be the primary reason responsible for the absence of detectable modes in
the remaining 68% of the stars without acoustic modes detected and with reliable
rotation periods. Thus, we investigate metallicity, inclination angle of the rotation
axis, and binarity as possible causes of low mode amplitudes. Using spectroscopic
observations for a subsample, we find that a low metallicity could be the reason
for suppressed modes. No clear correlation with binarity nor inclination is found.
We also derive the lower limit for our photometric activity index (of 20–30 ppm)
below which rotation and magnetic activity are not detected. Finally, with our
analysis we conclude that stars with a photometric activity index larger than
2,000 ppm have 98.3% probability of not having oscillations detected.
acknowledgement: This paper includes data collected by the Kepler mission. Funding
for the Kepler mission is provided by the NASA Science Mission directorate. Some
of the data presented in this paper were obtained from the Mikulski Archive for
Space Telescopes (MAST). STScI is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS5-26555. Partly Based on observations
obtained with the HERMES spectrograph on the Mercator Telescope, which was supported
by the Research Foundation—Flanders (FWO), Belgium, the Research Council of KU Leuven,
Belgium, the Fonds National de la Recherche Scientifique (F.R.S.-FNRS), Belgium,
the Royal Observatory of Belgium, the Observatoire de Genève, Switzerland, and the
Thüringer Landessternwarte Tautenburg, Germany. SM acknowledges support by the National
Aeronautics and Space Administration under Grant NNX15AF13G, by the National Science
Foundation grant AST-1411685, and the Ramon y Cajal fellowship number RYC-2015-17697.
RG acknowledges the support from PLATO and GOLF CNES grants. ÂS acknowledges the
support from National Aeronautics and Space Administration under Grant NNX17AF27G.
PB acknowledges the support of the MINECO under the fellowship program Juan de la
Cierva Incorporacion (IJCI-2015-26034).
article_number: '46'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Savita
full_name: Mathur, Savita
last_name: Mathur
- first_name: Rafael A.
full_name: García, Rafael A.
last_name: García
- 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: Ângela R.G.
full_name: Santos, Ângela R.G.
last_name: Santos
- first_name: Netsha
full_name: Santiago, Netsha
last_name: Santiago
- first_name: Paul G.
full_name: Beck, Paul G.
last_name: Beck
citation:
ama: Mathur S, García RA, Bugnet LA, Santos ÂRG, Santiago N, Beck PG. Revisiting
the impact of stellar magnetic activity on the detectability of solar-like oscillations
by Kepler. Frontiers in Astronomy and Space Sciences. 2019;6. doi:10.3389/fspas.2019.00046
apa: Mathur, S., García, R. A., Bugnet, L. A., Santos, Â. R. G., Santiago, N., &
Beck, P. G. (2019). Revisiting the impact of stellar magnetic activity on the
detectability of solar-like oscillations by Kepler. Frontiers in Astronomy
and Space Sciences. Frontiers Media. https://doi.org/10.3389/fspas.2019.00046
chicago: Mathur, Savita, Rafael A. García, Lisa Annabelle Bugnet, Ângela R.G. Santos,
Netsha Santiago, and Paul G. Beck. “Revisiting the Impact of Stellar Magnetic
Activity on the Detectability of Solar-like Oscillations by Kepler.” Frontiers
in Astronomy and Space Sciences. Frontiers Media, 2019. https://doi.org/10.3389/fspas.2019.00046.
ieee: S. Mathur, R. A. García, L. A. Bugnet, Â. R. G. Santos, N. Santiago, and P.
G. Beck, “Revisiting the impact of stellar magnetic activity on the detectability
of solar-like oscillations by Kepler,” Frontiers in Astronomy and Space Sciences,
vol. 6. Frontiers Media, 2019.
ista: Mathur S, García RA, Bugnet LA, Santos ÂRG, Santiago N, Beck PG. 2019. Revisiting
the impact of stellar magnetic activity on the detectability of solar-like oscillations
by Kepler. Frontiers in Astronomy and Space Sciences. 6, 46.
mla: Mathur, Savita, et al. “Revisiting the Impact of Stellar Magnetic Activity
on the Detectability of Solar-like Oscillations by Kepler.” Frontiers in Astronomy
and Space Sciences, vol. 6, 46, Frontiers Media, 2019, doi:10.3389/fspas.2019.00046.
short: S. Mathur, R.A. García, L.A. Bugnet, Â.R.G. Santos, N. Santiago, P.G. Beck,
Frontiers in Astronomy and Space Sciences 6 (2019).
date_created: 2022-07-18T14:00:36Z
date_published: 2019-07-10T00:00:00Z
date_updated: 2022-08-22T07:29:55Z
day: '10'
doi: 10.3389/fspas.2019.00046
extern: '1'
external_id:
arxiv:
- '1907.01415'
intvolume: ' 6'
keyword:
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1907.01415
month: '07'
oa: 1
oa_version: Preprint
publication: Frontiers in Astronomy and Space Sciences
publication_identifier:
eissn:
- 2296-987X
publication_status: published
publisher: Frontiers Media
quality_controlled: '1'
scopus_import: '1'
status: public
title: Revisiting the impact of stellar magnetic activity on the detectability of
solar-like oscillations by Kepler
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 6
year: '2019'
...
---
_id: '11614'
abstract:
- lang: eng
text: The NASA Transiting Exoplanet Survey Satellite (TESS) is about to provide
full-frame images of almost the entire sky. The amount of stellar data to be analysed
represents hundreds of millions stars, which is several orders of magnitude more
than the number of stars observed by the Convection, Rotation and planetary Transits
satellite (CoRoT), and NASA Kepler and K2 missions. We aim at automatically classifying
the newly observed stars with near real-time algorithms to better guide the subsequent
detailed studies. In this paper, we present a classification algorithm built to
recognise solar-like pulsators among classical pulsators. This algorithm relies
on the global amount of power contained in the power spectral density (PSD), also
known as the flicker in spectral power density (FliPer). Because each type of
pulsating star has a characteristic background or pulsation pattern, the shape
of the PSD at different frequencies can be used to characterise the type of pulsating
star. The FliPer classifier (FliPerClass) uses different FliPer parameters along
with the effective temperature as input parameters to feed a ML algorithm in order
to automatically classify the pulsating stars observed by TESS. Using noisy TESS-simulated
data from the TESS Asteroseismic Science Consortium (TASC), we classify pulsators
with a 98% accuracy. Among them, solar-like pulsating stars are recognised with
a 99% accuracy, which is of great interest for a further seismic analysis of these
stars, which are like our Sun. Similar results are obtained when we trained our
classifier and applied it to 27-day subsets of real Kepler data. FliPerClass is
part of the large TASC classification pipeline developed by the TESS Data for
Asteroseismology (T’DA) classification working group.
acknowledgement: We thank the enitre T’DA team for useful comments and discussions,
in particular Andrew Tkachenko. We also acknowledge Marc Hon, Keaton Bell, and James
Kuszlewicz for useful comments on the manuscript. L.B. and R.A.G. acknowledge the
support from PLATO and GOLF CNES grants. S.M. acknowledges support by the Ramon
y Cajal fellowship number RYC-2015-17697. O.J.H. and B.M.R. acknowledge the support
of the UK Science and Technology Facilities Council (STFC). M.N.L. acknowledges
the support of the ESA PRODEX programme (PEA 4000119301). Funding for the Stellar
Astrophysics Centre is provided by the Danish National Research Foundation (Grant
DNRF106).
article_number: A79
article_processing_charge: No
article_type: original
arxiv: 1
author:
- 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: R. A.
full_name: García, R. A.
last_name: García
- first_name: S.
full_name: Mathur, S.
last_name: Mathur
- first_name: G. R.
full_name: Davies, G. R.
last_name: Davies
- first_name: O. J.
full_name: Hall, O. J.
last_name: Hall
- first_name: M. N.
full_name: Lund, M. N.
last_name: Lund
- first_name: B. M.
full_name: Rendle, B. M.
last_name: Rendle
citation:
ama: 'Bugnet LA, García RA, Mathur S, et al. FliPerClass: In search of solar-like
pulsators among TESS targets. Astronomy & Astrophysics. 2019;624. doi:10.1051/0004-6361/201834780'
apa: 'Bugnet, L. A., García, R. A., Mathur, S., Davies, G. R., Hall, O. J., Lund,
M. N., & Rendle, B. M. (2019). FliPerClass: In search of solar-like pulsators
among TESS targets. Astronomy & Astrophysics. EDP Science. https://doi.org/10.1051/0004-6361/201834780'
chicago: 'Bugnet, Lisa Annabelle, R. A. García, S. Mathur, G. R. Davies, O. J. Hall,
M. N. Lund, and B. M. Rendle. “FliPerClass: In Search of Solar-like Pulsators
among TESS Targets.” Astronomy & Astrophysics. EDP Science, 2019. https://doi.org/10.1051/0004-6361/201834780.'
ieee: 'L. A. Bugnet et al., “FliPerClass: In search of solar-like pulsators
among TESS targets,” Astronomy & Astrophysics, vol. 624. EDP Science,
2019.'
ista: 'Bugnet LA, García RA, Mathur S, Davies GR, Hall OJ, Lund MN, Rendle BM. 2019.
FliPerClass: In search of solar-like pulsators among TESS targets. Astronomy &
Astrophysics. 624, A79.'
mla: 'Bugnet, Lisa Annabelle, et al. “FliPerClass: In Search of Solar-like Pulsators
among TESS Targets.” Astronomy & Astrophysics, vol. 624, A79, EDP Science,
2019, doi:10.1051/0004-6361/201834780.'
short: L.A. Bugnet, R.A. García, S. Mathur, G.R. Davies, O.J. Hall, M.N. Lund, B.M.
Rendle, Astronomy & Astrophysics 624 (2019).
date_created: 2022-07-18T14:13:34Z
date_published: 2019-04-19T00:00:00Z
date_updated: 2022-08-22T07:32:51Z
day: '19'
doi: 10.1051/0004-6361/201834780
extern: '1'
external_id:
arxiv:
- '1902.09854'
intvolume: ' 624'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1902.09854
month: '04'
oa: 1
oa_version: Preprint
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Science
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'FliPerClass: In search of solar-like pulsators among TESS targets'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 624
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: '11616'
abstract:
- lang: eng
text: We present the discovery of HD 221416 b, the first transiting planet identified
by the Transiting Exoplanet Survey Satellite (TESS) for which asteroseismology
of the host star is possible. HD 221416 b (HIP 116158, TOI-197) is a bright (V
= 8.2 mag), spectroscopically classified subgiant that oscillates with an average
frequency of about 430 μHz and displays a clear signature of mixed modes. The
oscillation amplitude confirms that the redder TESS bandpass compared to Kepler
has a small effect on the oscillations, supporting the expected yield of thousands
of solar-like oscillators with TESS 2 minute cadence observations. Asteroseismic
modeling yields a robust determination of the host star radius (R⋆ = 2.943 ± 0.064
R⊙), mass (M⋆ = 1.212 ± 0.074 M⊙), and age (4.9 ± 1.1 Gyr), and demonstrates that
it has just started ascending the red-giant branch. Combining asteroseismology
with transit modeling and radial-velocity observations, we show that the planet
is a "hot Saturn" (Rp = 9.17 ± 0.33 R⊕) with an orbital period of ∼14.3 days,
irradiance of F = 343 ± 24 F⊕, and moderate mass (Mp = 60.5 ± 5.7 M⊕) and density
(ρp = 0.431 ± 0.062 g cm−3). The properties of HD 221416 b show that the host-star
metallicity–planet mass correlation found in sub-Saturns (4–8 R⊕) does not extend
to larger radii, indicating that planets in the transition between sub-Saturns
and Jupiters follow a relatively narrow range of densities. With a density measured
to ∼15%, HD 221416 b is one of the best characterized Saturn-size planets to date,
augmenting the small number of known transiting planets around evolved stars and
demonstrating the power of TESS to characterize exoplanets and their host stars
using asteroseismology.
acknowledgement: "The authors wish to recognize and acknowledge the very significant
cultural role and reverence that the summit of Maunakea has always had within the
indigenous Hawai'ian community. We are most fortunate to have the opportunity to
conduct observations from this mountain. We thank Andrei Tokovinin for helpful information
on the Speckle observations obtained with SOAR. D.H. acknowledges support by the
National Aeronautics and Space Administration through the TESS Guest Investigator
Program (80NSSC18K1585) and by the National Science Foundation (AST-1717000). A.C.
acknowledges support by the National Science Foundation under the Graduate Research
Fellowship Program. W.J.C., W.H.B., A.M., O.J.H., and G.R.D. acknowledge support
from the Science and Technology Facilities Council and UK Space Agency. H.K. and
F.G. acknowledge support from the European Social Fund via the Lithuanian Science
Council grant No. 09.3.3-LMT-K-712-01-0103. Funding for the Stellar Astrophysics
Centre is provided by The Danish National Research Foundation (grant DNRF106). A.J.
acknowledges support from FONDECYT project 1171208, CONICYT project BASAL AFB-170002,
and by the Ministry for the Economy, Development, and Tourism's Programa Iniciativa
Científica Milenio through grant IC 120009, awarded to the Millennium Institute
of Astrophysics (MAS). R.B. acknowledges support from FONDECYT Post-doctoral Fellowship
Project 3180246, and from the Millennium Institute of Astrophysics (MAS). A.M.S.
is supported by grants ESP2017-82674-R (MINECO) and SGR2017-1131 (AGAUR). R.A.G.
and L.B. acknowledge the support of the PLATO grant from the CNES. The research
leading to the presented results has received funding from the European Research
Council under the European Community's Seventh Framework Programme (FP72007-2013)ERC
grant agreement No. 338251 (StellarAges). S.M. acknowledges support from the European
Research Council through the SPIRE grant 647383. This work was also supported by
FCT (Portugal) through national funds and by FEDER through COMPETE2020 by these
grants: UID/FIS/04434/2013 and POCI-01-0145-FEDER-007672, PTDC/FIS-AST/30389/2017,
and POCI-01-0145-FEDER-030389. T.L.C. acknowledges support from the European Union's
Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie
grant agreement No. 792848 (PULSATION). E.C. is funded by the European Union's Horizon
2020 research and innovation program under the Marie Sklodowska-Curie grant agreement
No. 664931. V.S.A. acknowledges support from the Independent Research Fund Denmark
(Research grant 7027-00096B). D.S. acknowledges support from the Australian Research
Council. S.B. acknowledges NASA grant NNX16AI09G and NSF grant AST-1514676. T.R.W.
acknowledges support from the Australian Research Council through grant DP150100250.
A.M. acknowledges support from the ERC Consolidator Grant funding scheme (project
ASTEROCHRONOMETRY, G.A. n. 772293). S.M. acknowledges support from the Ramon y Cajal
fellowship number RYC-2015-17697. M.S.L. is supported by the Carlsberg Foundation
(grant agreement No. CF17-0760). A.M. and P.R. acknowledge support from the HBCSE-NIUS
programme. J.K.T. and J.T. acknowledge that support for this work was provided by
NASA through Hubble Fellowship grants HST-HF2-51399.001 and HST-HF2-51424.001 awarded
by the Space Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555.
T.S.R. acknowledges financial support from Premiale 2015 MITiC (PI B. Garilli).
This project has been supported by the NKFIH K-115709 grant and the Lendület Program
of the Hungarian Academy of Sciences, project No. LP2018-7/2018.\r\n\r\nBased on
observations made with the Hertzsprung SONG telescope operated on the Spanish Observatorio
del Teide on the island of Tenerife by the Aarhus and Copenhagen Universities and
by the Instituto de Astrofísica de Canarias. Funding for the TESS mission is provided
by NASA's Science Mission directorate. We acknowledge the use of public TESS Alert
data from pipelines at the TESS Science Office and at the TESS Science Processing
Operations Center. This research has made use of the Exoplanet Follow-up Observation
Program website, which is operated by the California Institute of Technology, under
contract with the National Aeronautics and Space Administration under the Exoplanet
Exploration Program. This paper includes data collected by the TESS mission, which
are publicly available from the Mikulski Archive for Space Telescopes (MAST).\r\n\r\nSoftware:
Astropy (Astropy Collaboration et al. 2018), Matplotlib (Hunter 2007), DIAMONDS
(Corsaro & De Ridder 2014), isoclassify (Huber et al. 2017), EXOFASTv2 (Eastman
2017), ktransit (Barclay 2018)."
article_number: '245'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Daniel
full_name: Huber, Daniel
last_name: Huber
- first_name: William J.
full_name: Chaplin, William J.
last_name: Chaplin
- first_name: Ashley
full_name: Chontos, Ashley
last_name: Chontos
- first_name: Hans
full_name: Kjeldsen, Hans
last_name: Kjeldsen
- first_name: Jørgen
full_name: Christensen-Dalsgaard, Jørgen
last_name: Christensen-Dalsgaard
- first_name: Timothy R.
full_name: Bedding, Timothy R.
last_name: Bedding
- first_name: Warrick
full_name: Ball, Warrick
last_name: Ball
- first_name: Rafael
full_name: Brahm, Rafael
last_name: Brahm
- first_name: Nestor
full_name: Espinoza, Nestor
last_name: Espinoza
- first_name: Thomas
full_name: Henning, Thomas
last_name: Henning
- first_name: Andrés
full_name: Jordán, Andrés
last_name: Jordán
- first_name: Paula
full_name: Sarkis, Paula
last_name: Sarkis
- first_name: Emil
full_name: Knudstrup, Emil
last_name: Knudstrup
- first_name: Simon
full_name: Albrecht, Simon
last_name: Albrecht
- first_name: Frank
full_name: Grundahl, Frank
last_name: Grundahl
- first_name: Mads Fredslund
full_name: Andersen, Mads Fredslund
last_name: Andersen
- first_name: Pere L.
full_name: Pallé, Pere L.
last_name: Pallé
- first_name: Ian
full_name: Crossfield, Ian
last_name: Crossfield
- first_name: Benjamin
full_name: Fulton, Benjamin
last_name: Fulton
- first_name: Andrew W.
full_name: Howard, Andrew W.
last_name: Howard
- first_name: Howard T.
full_name: Isaacson, Howard T.
last_name: Isaacson
- first_name: Lauren M.
full_name: Weiss, Lauren M.
last_name: Weiss
- first_name: Rasmus
full_name: Handberg, Rasmus
last_name: Handberg
- first_name: Mikkel N.
full_name: Lund, Mikkel N.
last_name: Lund
- first_name: Aldo M.
full_name: Serenelli, Aldo M.
last_name: Serenelli
- first_name: Jakob
full_name: Rørsted Mosumgaard, Jakob
last_name: Rørsted Mosumgaard
- first_name: Amalie
full_name: Stokholm, Amalie
last_name: Stokholm
- first_name: Allyson
full_name: Bieryla, Allyson
last_name: Bieryla
- first_name: Lars A.
full_name: Buchhave, Lars A.
last_name: Buchhave
- first_name: David W.
full_name: Latham, David W.
last_name: Latham
- first_name: Samuel N.
full_name: Quinn, Samuel N.
last_name: Quinn
- first_name: Eric
full_name: Gaidos, Eric
last_name: Gaidos
- first_name: Teruyuki
full_name: Hirano, Teruyuki
last_name: Hirano
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full_name: Ricker, George R.
last_name: Ricker
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full_name: Vanderspek, Roland K.
last_name: Vanderspek
- first_name: Sara
full_name: Seager, Sara
last_name: Seager
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full_name: Jenkins, Jon M.
last_name: Jenkins
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full_name: Winn, Joshua N.
last_name: Winn
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full_name: Antia, H. M.
last_name: Antia
- first_name: Thierry
full_name: Appourchaux, Thierry
last_name: Appourchaux
- first_name: Sarbani
full_name: Basu, Sarbani
last_name: Basu
- first_name: Keaton J.
full_name: Bell, Keaton J.
last_name: Bell
- first_name: Othman
full_name: Benomar, Othman
last_name: Benomar
- first_name: Alfio
full_name: Bonanno, Alfio
last_name: Bonanno
- first_name: Derek L.
full_name: Buzasi, Derek L.
last_name: Buzasi
- first_name: Tiago L.
full_name: Campante, Tiago L.
last_name: Campante
- first_name: Z.
full_name: Çelik Orhan, Z.
last_name: Çelik Orhan
- first_name: Enrico
full_name: Corsaro, Enrico
last_name: Corsaro
- first_name: Margarida S.
full_name: Cunha, Margarida S.
last_name: Cunha
- first_name: Guy R.
full_name: Davies, Guy R.
last_name: Davies
- first_name: Sebastien
full_name: Deheuvels, Sebastien
last_name: Deheuvels
- first_name: Samuel K.
full_name: Grunblatt, Samuel K.
last_name: Grunblatt
- first_name: Amir
full_name: Hasanzadeh, Amir
last_name: Hasanzadeh
- first_name: Maria Pia
full_name: Di Mauro, Maria Pia
last_name: Di Mauro
- first_name: Rafael
full_name: A. García, Rafael
last_name: A. García
- first_name: Patrick
full_name: Gaulme, Patrick
last_name: Gaulme
- first_name: Léo
full_name: Girardi, Léo
last_name: Girardi
- first_name: Joyce A.
full_name: Guzik, Joyce A.
last_name: Guzik
- first_name: Marc
full_name: Hon, Marc
last_name: Hon
- first_name: Chen
full_name: Jiang, Chen
last_name: Jiang
- first_name: Thomas
full_name: Kallinger, Thomas
last_name: Kallinger
- first_name: Steven D.
full_name: Kawaler, Steven D.
last_name: Kawaler
- first_name: James S.
full_name: Kuszlewicz, James S.
last_name: Kuszlewicz
- first_name: Yveline
full_name: Lebreton, Yveline
last_name: Lebreton
- first_name: Tanda
full_name: Li, Tanda
last_name: Li
- first_name: Miles
full_name: Lucas, Miles
last_name: Lucas
- first_name: Mia S.
full_name: Lundkvist, Mia S.
last_name: Lundkvist
- first_name: Andrew W.
full_name: Mann, Andrew W.
last_name: Mann
- first_name: Stéphane
full_name: Mathis, Stéphane
last_name: Mathis
- first_name: Savita
full_name: Mathur, Savita
last_name: Mathur
- first_name: Anwesh
full_name: Mazumdar, Anwesh
last_name: Mazumdar
- first_name: Travis S.
full_name: Metcalfe, Travis S.
last_name: Metcalfe
- first_name: Andrea
full_name: Miglio, Andrea
last_name: Miglio
- first_name: Mário J. P.
full_name: F. G. Monteiro, Mário J. P.
last_name: F. G. Monteiro
- first_name: Benoit
full_name: Mosser, Benoit
last_name: Mosser
- first_name: Anthony
full_name: Noll, Anthony
last_name: Noll
- first_name: Benard
full_name: Nsamba, Benard
last_name: Nsamba
- first_name: Jia Mian
full_name: Joel Ong, Jia Mian
last_name: Joel Ong
- first_name: S.
full_name: Örtel, S.
last_name: Örtel
- first_name: Filipe
full_name: Pereira, Filipe
last_name: Pereira
- first_name: Pritesh
full_name: Ranadive, Pritesh
last_name: Ranadive
- first_name: Clara
full_name: Régulo, Clara
last_name: Régulo
- first_name: Thaíse S.
full_name: Rodrigues, Thaíse S.
last_name: Rodrigues
- first_name: Ian W.
full_name: Roxburgh, Ian W.
last_name: Roxburgh
- first_name: Victor Silva
full_name: Aguirre, Victor Silva
last_name: Aguirre
- first_name: Barry
full_name: Smalley, Barry
last_name: Smalley
- first_name: Mathew
full_name: Schofield, Mathew
last_name: Schofield
- first_name: Sérgio G.
full_name: Sousa, Sérgio G.
last_name: Sousa
- first_name: Keivan G.
full_name: Stassun, Keivan G.
last_name: Stassun
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last_name: Stello
- first_name: Jamie
full_name: Tayar, Jamie
last_name: Tayar
- first_name: Timothy R.
full_name: White, Timothy R.
last_name: White
- first_name: Kuldeep
full_name: Verma, Kuldeep
last_name: Verma
- first_name: Mathieu
full_name: Vrard, Mathieu
last_name: Vrard
- first_name: M.
full_name: Yıldız, M.
last_name: Yıldız
- first_name: David
full_name: Baker, David
last_name: Baker
- first_name: Michaël
full_name: Bazot, Michaël
last_name: Bazot
- first_name: Charles
full_name: Beichmann, Charles
last_name: Beichmann
- first_name: Christoph
full_name: Bergmann, Christoph
last_name: Bergmann
- 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: Bryson
full_name: Cale, Bryson
last_name: Cale
- first_name: Roberto
full_name: Carlino, Roberto
last_name: Carlino
- first_name: Scott M.
full_name: Cartwright, Scott M.
last_name: Cartwright
- first_name: Jessie L.
full_name: Christiansen, Jessie L.
last_name: Christiansen
- first_name: David R.
full_name: Ciardi, David R.
last_name: Ciardi
- first_name: Orlagh
full_name: Creevey, Orlagh
last_name: Creevey
- first_name: Jason A.
full_name: Dittmann, Jason A.
last_name: Dittmann
- first_name: Jose-Dias Do
full_name: Nascimento, Jose-Dias Do
last_name: Nascimento
- first_name: Vincent Van
full_name: Eylen, Vincent Van
last_name: Eylen
- first_name: Gabor
full_name: Fürész, Gabor
last_name: Fürész
- first_name: Jonathan
full_name: Gagné, Jonathan
last_name: Gagné
- first_name: Peter
full_name: Gao, Peter
last_name: Gao
- first_name: Kosmas
full_name: Gazeas, Kosmas
last_name: Gazeas
- first_name: Frank
full_name: Giddens, Frank
last_name: Giddens
- first_name: Oliver J.
full_name: Hall, Oliver J.
last_name: Hall
- first_name: Saskia
full_name: Hekker, Saskia
last_name: Hekker
- first_name: Michael J.
full_name: Ireland, Michael J.
last_name: Ireland
- first_name: Natasha
full_name: Latouf, Natasha
last_name: Latouf
- first_name: Danny
full_name: LeBrun, Danny
last_name: LeBrun
- first_name: Alan M.
full_name: Levine, Alan M.
last_name: Levine
- first_name: William
full_name: Matzko, William
last_name: Matzko
- first_name: Eva
full_name: Natinsky, Eva
last_name: Natinsky
- first_name: Emma
full_name: Page, Emma
last_name: Page
- first_name: Peter
full_name: Plavchan, Peter
last_name: Plavchan
- first_name: Masoud
full_name: Mansouri-Samani, Masoud
last_name: Mansouri-Samani
- first_name: Sean
full_name: McCauliff, Sean
last_name: McCauliff
- first_name: Susan E.
full_name: Mullally, Susan E.
last_name: Mullally
- first_name: Brendan
full_name: Orenstein, Brendan
last_name: Orenstein
- first_name: Aylin Garcia
full_name: Soto, Aylin Garcia
last_name: Soto
- first_name: Martin
full_name: Paegert, Martin
last_name: Paegert
- first_name: Jennifer L.
full_name: van Saders, Jennifer L.
last_name: van Saders
- first_name: Chloe
full_name: Schnaible, Chloe
last_name: Schnaible
- first_name: David R.
full_name: Soderblom, David R.
last_name: Soderblom
- first_name: Róbert
full_name: Szabó, Róbert
last_name: Szabó
- first_name: Angelle
full_name: Tanner, Angelle
last_name: Tanner
- first_name: C. G.
full_name: Tinney, C. G.
last_name: Tinney
- first_name: Johanna
full_name: Teske, Johanna
last_name: Teske
- first_name: Alexandra
full_name: Thomas, Alexandra
last_name: Thomas
- first_name: Regner
full_name: Trampedach, Regner
last_name: Trampedach
- first_name: Duncan
full_name: Wright, Duncan
last_name: Wright
- first_name: Thomas T.
full_name: Yuan, Thomas T.
last_name: Yuan
- first_name: Farzaneh
full_name: Zohrabi, Farzaneh
last_name: Zohrabi
citation:
ama: Huber D, Chaplin WJ, Chontos A, et al. A hot Saturn orbiting an oscillating
late subgiant discovered by TESS. The Astronomical Journal. 2019;157(6).
doi:10.3847/1538-3881/ab1488
apa: Huber, D., Chaplin, W. J., Chontos, A., Kjeldsen, H., Christensen-Dalsgaard,
J., Bedding, T. R., … Zohrabi, F. (2019). A hot Saturn orbiting an oscillating
late subgiant discovered by TESS. The Astronomical Journal. IOP Publishing.
https://doi.org/10.3847/1538-3881/ab1488
chicago: Huber, Daniel, William J. Chaplin, Ashley Chontos, Hans Kjeldsen, Jørgen
Christensen-Dalsgaard, Timothy R. Bedding, Warrick Ball, et al. “A Hot Saturn
Orbiting an Oscillating Late Subgiant Discovered by TESS.” The Astronomical
Journal. IOP Publishing, 2019. https://doi.org/10.3847/1538-3881/ab1488.
ieee: D. Huber et al., “A hot Saturn orbiting an oscillating late subgiant
discovered by TESS,” The Astronomical Journal, vol. 157, no. 6. IOP Publishing,
2019.
ista: Huber D et al. 2019. A hot Saturn orbiting an oscillating late subgiant discovered
by TESS. The Astronomical Journal. 157(6), 245.
mla: Huber, Daniel, et al. “A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered
by TESS.” The Astronomical Journal, vol. 157, no. 6, 245, IOP Publishing,
2019, doi:10.3847/1538-3881/ab1488.
short: D. Huber, W.J. Chaplin, A. Chontos, H. Kjeldsen, J. Christensen-Dalsgaard,
T.R. Bedding, W. Ball, R. Brahm, N. Espinoza, T. Henning, A. Jordán, P. Sarkis,
E. Knudstrup, S. Albrecht, F. Grundahl, M.F. Andersen, P.L. Pallé, I. Crossfield,
B. Fulton, A.W. Howard, H.T. Isaacson, L.M. Weiss, R. Handberg, M.N. Lund, A.M.
Serenelli, J. Rørsted Mosumgaard, A. Stokholm, A. Bieryla, L.A. Buchhave, D.W.
Latham, S.N. Quinn, E. Gaidos, T. Hirano, G.R. Ricker, R.K. Vanderspek, S. Seager,
J.M. Jenkins, J.N. Winn, H.M. Antia, T. Appourchaux, S. Basu, K.J. Bell, O. Benomar,
A. Bonanno, D.L. Buzasi, T.L. Campante, Z. Çelik Orhan, E. Corsaro, M.S. Cunha,
G.R. Davies, S. Deheuvels, S.K. Grunblatt, A. Hasanzadeh, M.P. Di Mauro, R. A.
García, P. Gaulme, L. Girardi, J.A. Guzik, M. Hon, C. Jiang, T. Kallinger, S.D.
Kawaler, J.S. Kuszlewicz, Y. Lebreton, T. Li, M. Lucas, M.S. Lundkvist, A.W. Mann,
S. Mathis, S. Mathur, A. Mazumdar, T.S. Metcalfe, A. Miglio, M.J.P. F. G. Monteiro,
B. Mosser, A. Noll, B. Nsamba, J.M. Joel Ong, S. Örtel, F. Pereira, P. Ranadive,
C. Régulo, T.S. Rodrigues, I.W. Roxburgh, V.S. Aguirre, B. Smalley, M. Schofield,
S.G. Sousa, K.G. Stassun, D. Stello, J. Tayar, T.R. White, K. Verma, M. Vrard,
M. Yıldız, D. Baker, M. Bazot, C. Beichmann, C. Bergmann, L.A. Bugnet, B. Cale,
R. Carlino, S.M. Cartwright, J.L. Christiansen, D.R. Ciardi, O. Creevey, J.A.
Dittmann, J.-D.D. Nascimento, V.V. Eylen, G. Fürész, J. Gagné, P. Gao, K. Gazeas,
F. Giddens, O.J. Hall, S. Hekker, M.J. Ireland, N. Latouf, D. LeBrun, A.M. Levine,
W. Matzko, E. Natinsky, E. Page, P. Plavchan, M. Mansouri-Samani, S. McCauliff,
S.E. Mullally, B. Orenstein, A.G. Soto, M. Paegert, J.L. van Saders, C. Schnaible,
D.R. Soderblom, R. Szabó, A. Tanner, C.G. Tinney, J. Teske, A. Thomas, R. Trampedach,
D. Wright, T.T. Yuan, F. Zohrabi, The Astronomical Journal 157 (2019).
date_created: 2022-07-18T14:29:07Z
date_published: 2019-05-30T00:00:00Z
date_updated: 2022-08-22T07:38:34Z
day: '30'
doi: 10.3847/1538-3881/ab1488
extern: '1'
external_id:
arxiv:
- '1901.01643'
intvolume: ' 157'
issue: '6'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1901.01643
month: '05'
oa: 1
oa_version: Preprint
publication: The Astronomical Journal
publication_identifier:
issn:
- 0004-6256
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: A hot Saturn orbiting an oscillating late subgiant discovered by TESS
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 157
year: '2019'
...
---
_id: '11623'
abstract:
- lang: eng
text: Brightness variations due to dark spots on the stellar surface encode information
about stellar surface rotation and magnetic activity. In this work, we analyze
the Kepler long-cadence data of 26,521 main-sequence stars of spectral types M
and K in order to measure their surface rotation and photometric activity level.
Rotation-period estimates are obtained by the combination of a wavelet analysis
and autocorrelation function of the light curves. Reliable rotation estimates
are determined by comparing the results from the different rotation diagnostics
and four data sets. We also measure the photometric activity proxy Sph using the
amplitude of the flux variations on an appropriate timescale. We report rotation
periods and photometric activity proxies for about 60% of the sample, including
4431 targets for which McQuillan et al. did not report a rotation period. For
the common targets with rotation estimates in this study and in McQuillan et al.,
our rotation periods agree within 99%. In this work, we also identify potential
polluters, such as misclassified red giants and classical pulsator candidates.
Within the parameter range we study, there is a mild tendency for hotter stars
to have shorter rotation periods. The photometric activity proxy spans a wider
range of values with increasing effective temperature. The rotation period and
photometric activity proxy are also related, with Sph being larger for fast rotators.
Similar to McQuillan et al., we find a bimodal distribution of rotation periods.
acknowledgement: "The authors thank Róbert Szabó Paul G. Beck, Katrien Kolenberg,
and Isabel L. Colman for helping on the classification of stars. This paper includes
data collected by the Kepler mission and obtained from the MAST data archive at
the Space Telescope Science Institute (STScI). Funding for the Kepler mission is
provided by the National Aeronautics and Space Administration (NASA) Science Mission
Directorate. STScI is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS 5–26555. A.R.G.S. acknowledges the support
from NASA under grant NNX17AF27G. R.A.G. and L.B. acknowledge the support from PLATO
and GOLF CNES grants. S.M. acknowledges the support from the Ramon y Cajal fellowship
number RYC-2015-17697. T.S.M. acknowledges support from a Visiting Fellowship at
the Max Planck Institute for Solar System Research. This research has made use of
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.\r\n\r\nSoftware: KADACS (García et al. 2011), NumPy
(van der Walt et al. 2011), SciPy (Jones et al. 2001), Matplotlib (Hunter 2007).\r\n\r\nFacilities:
MAST - , Kepler Eclipsing Binary Catalog - , Exoplanet Archive. -"
article_number: '21'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: A. R. G.
full_name: Santos, A. R. G.
last_name: Santos
- first_name: R. A.
full_name: García, R. A.
last_name: García
- first_name: S.
full_name: Mathur, S.
last_name: Mathur
- 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: J. L.
full_name: van Saders, J. L.
last_name: van Saders
- first_name: T. S.
full_name: Metcalfe, T. S.
last_name: Metcalfe
- first_name: G. V. A.
full_name: Simonian, G. V. A.
last_name: Simonian
- first_name: M. H.
full_name: Pinsonneault, M. H.
last_name: Pinsonneault
citation:
ama: Santos ARG, García RA, Mathur S, et al. Surface rotation and photometric activity
for Kepler targets. I. M and K main-sequence stars. The Astrophysical Journal
Supplement Series. 2019;244(1). doi:10.3847/1538-4365/ab3b56
apa: Santos, A. R. G., García, R. A., Mathur, S., Bugnet, L. A., van Saders, J.
L., Metcalfe, T. S., … Pinsonneault, M. H. (2019). Surface rotation and photometric
activity for Kepler targets. I. M and K main-sequence stars. The Astrophysical
Journal Supplement Series. IOP Publishing. https://doi.org/10.3847/1538-4365/ab3b56
chicago: Santos, A. R. G., R. A. García, S. Mathur, Lisa Annabelle Bugnet, J. L.
van Saders, T. S. Metcalfe, G. V. A. Simonian, and M. H. Pinsonneault. “Surface
Rotation and Photometric Activity for Kepler Targets. I. M and K Main-Sequence
Stars.” The Astrophysical Journal Supplement Series. IOP Publishing, 2019.
https://doi.org/10.3847/1538-4365/ab3b56.
ieee: A. R. G. Santos et al., “Surface rotation and photometric activity
for Kepler targets. I. M and K main-sequence stars,” The Astrophysical Journal
Supplement Series, vol. 244, no. 1. IOP Publishing, 2019.
ista: Santos ARG, García RA, Mathur S, Bugnet LA, van Saders JL, Metcalfe TS, Simonian
GVA, Pinsonneault MH. 2019. Surface rotation and photometric activity for Kepler
targets. I. M and K main-sequence stars. The Astrophysical Journal Supplement
Series. 244(1), 21.
mla: Santos, A. R. G., et al. “Surface Rotation and Photometric Activity for Kepler
Targets. I. M and K Main-Sequence Stars.” The Astrophysical Journal Supplement
Series, vol. 244, no. 1, 21, IOP Publishing, 2019, doi:10.3847/1538-4365/ab3b56.
short: A.R.G. Santos, R.A. García, S. Mathur, L.A. Bugnet, J.L. van Saders, T.S.
Metcalfe, G.V.A. Simonian, M.H. Pinsonneault, The Astrophysical Journal Supplement
Series 244 (2019).
date_created: 2022-07-19T09:21:58Z
date_published: 2019-09-19T00:00:00Z
date_updated: 2022-08-22T08:10:38Z
day: '19'
doi: 10.3847/1538-4365/ab3b56
extern: '1'
external_id:
arxiv:
- '1908.05222'
intvolume: ' 244'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'methods: data analysis'
- 'stars: activity'
- 'stars: low-mass'
- 'stars: rotation'
- starspots
- 'techniques: photometric'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1908.05222
month: '09'
oa: 1
oa_version: Preprint
publication: The Astrophysical Journal Supplement Series
publication_identifier:
issn:
- 0067-0049
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence
stars
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 244
year: '2019'
...
---
_id: '11627'
abstract:
- lang: eng
text: 'For a solar-like star, the surface rotation evolves with time, allowing in
principle to estimate the age of a star from its surface rotation period. Here
we are interested in measuring surface rotation periods of solar-like stars observed
by the NASA mission Kepler. Different methods have been developed to track rotation
signals in Kepler photometric light curves: time-frequency analysis based on wavelet
techniques, autocorrelation and composite spectrum. We use the learning abilities
of random forest classifiers to take decisions during two crucial steps of the
analysis. First, given some input parameters, we discriminate the considered Kepler
targets between rotating MS stars, non-rotating MS stars, red giants, binaries
and pulsators. We then use a second classifier only on the MS rotating targets
to decide the best data analysis treatment.'
article_number: '1906.09609'
article_processing_charge: No
arxiv: 1
author:
- first_name: S. N.
full_name: Breton, S. N.
last_name: Breton
- 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: A. R. G.
full_name: Santos, A. R. G.
last_name: Santos
- first_name: A. Le
full_name: Saux, A. Le
last_name: Saux
- first_name: S.
full_name: Mathur, S.
last_name: Mathur
- first_name: P. L.
full_name: Palle, P. L.
last_name: Palle
- first_name: R. A.
full_name: Garcia, R. A.
last_name: Garcia
citation:
ama: Breton SN, Bugnet LA, Santos ARG, et al. Determining surface rotation periods
of solar-like stars observed by the Kepler mission using machine learning techniques.
arXiv. doi:10.48550/arXiv.1906.09609
apa: Breton, S. N., Bugnet, L. A., Santos, A. R. G., Saux, A. L., Mathur, S., Palle,
P. L., & Garcia, R. A. (n.d.). Determining surface rotation periods of solar-like
stars observed by the Kepler mission using machine learning techniques. arXiv.
https://doi.org/10.48550/arXiv.1906.09609
chicago: Breton, S. N., Lisa Annabelle Bugnet, A. R. G. Santos, A. Le Saux, S. Mathur,
P. L. Palle, and R. A. Garcia. “Determining Surface Rotation Periods of Solar-like
Stars Observed by the Kepler Mission Using Machine Learning Techniques.” ArXiv,
n.d. https://doi.org/10.48550/arXiv.1906.09609.
ieee: S. N. Breton et al., “Determining surface rotation periods of solar-like
stars observed by the Kepler mission using machine learning techniques,” arXiv.
.
ista: Breton SN, Bugnet LA, Santos ARG, Saux AL, Mathur S, Palle PL, Garcia RA.
Determining surface rotation periods of solar-like stars observed by the Kepler
mission using machine learning techniques. arXiv, 1906.09609.
mla: Breton, S. N., et al. “Determining Surface Rotation Periods of Solar-like Stars
Observed by the Kepler Mission Using Machine Learning Techniques.” ArXiv,
1906.09609, doi:10.48550/arXiv.1906.09609.
short: S.N. Breton, L.A. Bugnet, A.R.G. Santos, A.L. Saux, S. Mathur, P.L. Palle,
R.A. Garcia, ArXiv (n.d.).
date_created: 2022-07-20T11:18:53Z
date_published: 2019-06-23T00:00:00Z
date_updated: 2022-08-22T08:16:53Z
day: '23'
doi: 10.48550/arXiv.1906.09609
extern: '1'
external_id:
arxiv:
- '1906.09609'
keyword:
- asteroseismology
- rotation
- solar-like stars
- kepler
- machine learning
- random forest
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1906.09609
month: '06'
oa: 1
oa_version: Preprint
publication: arXiv
publication_status: submitted
status: public
title: Determining surface rotation periods of solar-like stars observed by the Kepler
mission using machine learning techniques
type: preprint
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2019'
...
---
_id: '11630'
abstract:
- lang: eng
text: 'The second mission of NASA’s Kepler satellite, K2, has collected hundreds
of thousands of lightcurves for stars close to the ecliptic plane. This new sample
could increase the number of known pulsating stars and then improve our understanding
of those stars. For the moment only a few stars have been properly classified
and published. In this work, we present a method to automaticly classify K2 pulsating
stars using a Machine Learning technique called Random Forest. The objective is
to sort out the stars in four classes: red giant (RG), main-sequence Solar-like
stars (SL), classical pulsators (PULS) and Other. To do this we use the effective
temperatures and the luminosities of the stars as well as the FliPer features,
that measures the amount of power contained in the power spectral density. The
classifier now retrieves the right classification for more than 80% of the stars.'
article_number: '1906.09611'
article_processing_charge: No
arxiv: 1
author:
- first_name: A. Le
full_name: Saux, A. Le
last_name: Saux
- 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: S.
full_name: Mathur, S.
last_name: Mathur
- first_name: S. N.
full_name: Breton, S. N.
last_name: Breton
- first_name: R. A.
full_name: Garcia, R. A.
last_name: Garcia
citation:
ama: Saux AL, Bugnet LA, Mathur S, Breton SN, Garcia RA. Automatic classification
of K2 pulsating stars using machine learning techniques. arXiv. doi:10.48550/arXiv.1906.09611
apa: Saux, A. L., Bugnet, L. A., Mathur, S., Breton, S. N., & Garcia, R. A.
(n.d.). Automatic classification of K2 pulsating stars using machine learning
techniques. arXiv. https://doi.org/10.48550/arXiv.1906.09611
chicago: Saux, A. Le, Lisa Annabelle Bugnet, S. Mathur, S. N. Breton, and R. A.
Garcia. “Automatic Classification of K2 Pulsating Stars Using Machine Learning
Techniques.” ArXiv, n.d. https://doi.org/10.48550/arXiv.1906.09611.
ieee: A. L. Saux, L. A. Bugnet, S. Mathur, S. N. Breton, and R. A. Garcia, “Automatic
classification of K2 pulsating stars using machine learning techniques,” arXiv.
.
ista: Saux AL, Bugnet LA, Mathur S, Breton SN, Garcia RA. Automatic classification
of K2 pulsating stars using machine learning techniques. arXiv, 1906.09611.
mla: Saux, A. Le, et al. “Automatic Classification of K2 Pulsating Stars Using Machine
Learning Techniques.” ArXiv, 1906.09611, doi:10.48550/arXiv.1906.09611.
short: A.L. Saux, L.A. Bugnet, S. Mathur, S.N. Breton, R.A. Garcia, ArXiv (n.d.).
date_created: 2022-07-21T06:57:10Z
date_published: 2019-06-23T00:00:00Z
date_updated: 2022-08-22T08:20:29Z
day: '23'
doi: 10.48550/arXiv.1906.09611
extern: '1'
external_id:
arxiv:
- '1906.09611'
keyword:
- asteroseismology - methods
- data analysis - thecniques
- machine learning - stars
- oscillations
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.48550/arXiv.1906.09611
month: '06'
oa: 1
oa_version: Preprint
publication: arXiv
publication_status: submitted
status: public
title: Automatic classification of K2 pulsating stars using machine learning techniques
type: preprint
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2019'
...
---
_id: '7782'
abstract:
- lang: eng
text: As genome-wide association studies (GWAS) increased in size, numerous gene-environment
interactions (GxE) have been discovered, many of which however explore only one
environment at a time and may suffer from statistical artefacts leading to biased
interaction estimates. Here we propose a maximum likelihood method to estimate
the contribution of GxE to complex traits taking into account all interacting
environmental variables at the same time, without the need to measure any. This
is possible because GxE induces fluctuations in the conditional trait variance,
the extent of which depends on the strength of GxE. The approach can be applied
to continuous outcomes and for single SNPs or genetic risk scores (GRS). Extensive
simulations demonstrated that our method yields unbiased interaction estimates
and excellent confidence interval coverage. We also offer a strategy to distinguish
specific GxE from general heteroscedasticity (scale effects). Applying our method
to 32 complex traits in the UK Biobank reveals that for body mass index (BMI)
the GRSxE explains an additional 1.9% variance on top of the 5.2% GRS contribution.
However, this interaction is not specific to the GRS and holds for any variable
similarly correlated with BMI. On the contrary, the GRSxE interaction effect for
leg impedance Embedded Image is significantly (P < 10−56) larger than it would
be expected for a similarly correlated variable Embedded Image. We showed that
our method could robustly detect the global contribution of GxE to complex traits,
which turned out to be substantial for certain obesity measures.
article_processing_charge: No
author:
- first_name: Jonathan
full_name: Sulc, Jonathan
last_name: Sulc
- first_name: Ninon
full_name: Mounier, Ninon
last_name: Mounier
- first_name: Felix
full_name: Günther, Felix
last_name: Günther
- first_name: Thomas
full_name: Winkler, Thomas
last_name: Winkler
- first_name: Andrew R.
full_name: Wood, Andrew R.
last_name: Wood
- first_name: Timothy M.
full_name: Frayling, Timothy M.
last_name: Frayling
- first_name: Iris M.
full_name: Heid, Iris M.
last_name: Heid
- first_name: Matthew Richard
full_name: Robinson, Matthew Richard
id: E5D42276-F5DA-11E9-8E24-6303E6697425
last_name: Robinson
orcid: 0000-0001-8982-8813
- first_name: Zoltán
full_name: Kutalik, Zoltán
last_name: Kutalik
citation:
ama: 'Sulc J, Mounier N, Günther F, et al. Maximum likelihood method quantifies
the overall contribution of gene-environment interaction to continuous traits:
An application to complex traits in the UK Biobank. bioRxiv. 2019.'
apa: 'Sulc, J., Mounier, N., Günther, F., Winkler, T., Wood, A. R., Frayling, T.
M., … Kutalik, Z. (2019). Maximum likelihood method quantifies the overall contribution
of gene-environment interaction to continuous traits: An application to complex
traits in the UK Biobank. bioRxiv. Cold Spring Harbor Laboratory.'
chicago: 'Sulc, Jonathan, Ninon Mounier, Felix Günther, Thomas Winkler, Andrew R.
Wood, Timothy M. Frayling, Iris M. Heid, Matthew Richard Robinson, and Zoltán
Kutalik. “Maximum Likelihood Method Quantifies the Overall Contribution of Gene-Environment
Interaction to Continuous Traits: An Application to Complex Traits in the UK Biobank.”
BioRxiv. Cold Spring Harbor Laboratory, 2019.'
ieee: 'J. Sulc et al., “Maximum likelihood method quantifies the overall
contribution of gene-environment interaction to continuous traits: An application
to complex traits in the UK Biobank,” bioRxiv. Cold Spring Harbor Laboratory,
2019.'
ista: 'Sulc J, Mounier N, Günther F, Winkler T, Wood AR, Frayling TM, Heid IM, Robinson
MR, Kutalik Z. 2019. Maximum likelihood method quantifies the overall contribution
of gene-environment interaction to continuous traits: An application to complex
traits in the UK Biobank. bioRxiv, .'
mla: 'Sulc, Jonathan, et al. “Maximum Likelihood Method Quantifies the Overall Contribution
of Gene-Environment Interaction to Continuous Traits: An Application to Complex
Traits in the UK Biobank.” BioRxiv, Cold Spring Harbor Laboratory, 2019.'
short: J. Sulc, N. Mounier, F. Günther, T. Winkler, A.R. Wood, T.M. Frayling, I.M.
Heid, M.R. Robinson, Z. Kutalik, BioRxiv (2019).
date_created: 2020-04-30T13:04:26Z
date_published: 2019-06-14T00:00:00Z
date_updated: 2021-01-12T08:15:30Z
day: '14'
extern: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: 'https://doi.org/10.1101/632380 '
month: '06'
oa: 1
oa_version: Preprint
page: '20'
publication: bioRxiv
publication_status: published
publisher: Cold Spring Harbor Laboratory
status: public
title: 'Maximum likelihood method quantifies the overall contribution of gene-environment
interaction to continuous traits: An application to complex traits in the UK Biobank'
type: preprint
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2019'
...
---
_id: '7950'
abstract:
- lang: eng
text: "The input to the token swapping problem is a graph with vertices v1, v2,
. . . , vn, and n tokens with labels 1,2, . . . , n, one on each vertex. The
goal is to get token i to vertex vi for all i= 1, . . . , n using a minimum number
of swaps, where a swap exchanges the tokens on the endpoints of an edge.Token
swapping on a tree, also known as “sorting with a transposition tree,” is not
known to be in P nor NP-complete. We present some partial results:\r\n1. An
optimum swap sequence may need to perform a swap on a leaf vertex that has the
correct token (a “happy leaf”), disproving a conjecture of Vaughan.\r\n2. Any
algorithm that fixes happy leaves—as all known approximation algorithms for the
problem do—has approximation factor at least 4/3. Furthermore, the two best-known
2-approximation algorithms have approximation factor exactly 2.\r\n3. A generalized
problem—weighted coloured token swapping—is NP-complete on trees, but solvable
in polynomial time on paths and stars. In this version, tokens and vertices
\ have colours, and colours have weights. The goal is to get every
token to a vertex of the same colour, and the cost of a swap is the sum of the
weights of the two tokens involved."
article_number: '1903.06981'
article_processing_charge: No
arxiv: 1
author:
- first_name: Ahmad
full_name: Biniaz, Ahmad
last_name: Biniaz
- first_name: Kshitij
full_name: Jain, Kshitij
last_name: Jain
- first_name: Anna
full_name: Lubiw, Anna
last_name: Lubiw
- first_name: Zuzana
full_name: Masárová, Zuzana
id: 45CFE238-F248-11E8-B48F-1D18A9856A87
last_name: Masárová
orcid: 0000-0002-6660-1322
- first_name: Tillmann
full_name: Miltzow, Tillmann
last_name: Miltzow
- first_name: Debajyoti
full_name: Mondal, Debajyoti
last_name: Mondal
- first_name: Anurag Murty
full_name: Naredla, Anurag Murty
last_name: Naredla
- first_name: Josef
full_name: Tkadlec, Josef
id: 3F24CCC8-F248-11E8-B48F-1D18A9856A87
last_name: Tkadlec
orcid: 0000-0002-1097-9684
- first_name: Alexi
full_name: Turcotte, Alexi
last_name: Turcotte
citation:
ama: Biniaz A, Jain K, Lubiw A, et al. Token swapping on trees. arXiv.
apa: Biniaz, A., Jain, K., Lubiw, A., Masárová, Z., Miltzow, T., Mondal, D., … Turcotte,
A. (n.d.). Token swapping on trees. arXiv.
chicago: Biniaz, Ahmad, Kshitij Jain, Anna Lubiw, Zuzana Masárová, Tillmann Miltzow,
Debajyoti Mondal, Anurag Murty Naredla, Josef Tkadlec, and Alexi Turcotte. “Token
Swapping on Trees.” ArXiv, n.d.
ieee: A. Biniaz et al., “Token swapping on trees,” arXiv. .
ista: Biniaz A, Jain K, Lubiw A, Masárová Z, Miltzow T, Mondal D, Naredla AM, Tkadlec
J, Turcotte A. Token swapping on trees. arXiv, 1903.06981.
mla: Biniaz, Ahmad, et al. “Token Swapping on Trees.” ArXiv, 1903.06981.
short: A. Biniaz, K. Jain, A. Lubiw, Z. Masárová, T. Miltzow, D. Mondal, A.M. Naredla,
J. Tkadlec, A. Turcotte, ArXiv (n.d.).
date_created: 2020-06-08T12:25:25Z
date_published: 2019-03-16T00:00:00Z
date_updated: 2024-01-04T12:42:08Z
day: '16'
department:
- _id: HeEd
- _id: UlWa
- _id: KrCh
external_id:
arxiv:
- '1903.06981'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1903.06981
month: '03'
oa: 1
oa_version: Preprint
publication: arXiv
publication_status: submitted
related_material:
record:
- id: '7944'
relation: dissertation_contains
status: public
- id: '12833'
relation: later_version
status: public
status: public
title: Token swapping on trees
type: preprint
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
year: '2019'
...
---
_id: '8'
abstract:
- lang: eng
text: Despite their different origins, Drosophila glia and hemocytes are related
cell populations that provide an immune function. Drosophila hemocytes patrol
the body cavity and act as macrophages outside the nervous system whereas glia
originate from the neuroepithelium and provide the scavenger population of the
nervous system. Drosophila glia are hence the functional orthologs of vertebrate
microglia, even though the latter are cells of immune origin that subsequently
move into the brain during development. Interestingly, the Drosophila immune cells
within (glia) and outside the nervous system (hemocytes) require the same transcription
factor Glide/Gcm for their development. This raises the issue of how do glia specifically
differentiate in the nervous system and hemocytes in the procephalic mesoderm.
The Repo homeodomain transcription factor and pan-glial direct target of Glide/Gcm
is known to ensure glial terminal differentiation. Here we show that Repo also
takes center stage in the process that discriminates between glia and hemocytes.
First, Repo expression is repressed in the hemocyte anlagen by mesoderm-specific
factors. Second, Repo ectopic activation in the procephalic mesoderm is sufficient
to repress the expression of hemocyte-specific genes. Third, the lack of Repo
triggers the expression of hemocyte markers in glia. Thus, a complex network of
tissue-specific cues biases the potential of Glide/Gcm. These data allow us to
revise the concept of fate determinants and help us understand the bases of cell
specification. Both sexes were analyzed.SIGNIFICANCE STATEMENTDistinct cell types
often require the same pioneer transcription factor, raising the issue of how
does one factor trigger different fates. In Drosophila, glia and hemocytes provide
a scavenger activity within and outside the nervous system, respectively. While
they both require the Glide/Gcm transcription factor, glia originate from the
ectoderm, hemocytes from the mesoderm. Here we show that tissue-specific factors
inhibit the gliogenic potential of Glide/Gcm in the mesoderm by repressing the
expression of the homeodomain protein Repo, a major glial-specific target of Glide/Gcm.
Repo expression in turn inhibits the expression of hemocyte-specific genes in
the nervous system. These cell-specific networks secure the establishment of the
glial fate only in the nervous system and allow cell diversification.
acknowledgement: This work was supported by INSERM, CNRS, UDS, Ligue Régionale contre
le Cancer, Hôpital de Strasbourg, Association pour la Recherche sur le Cancer (ARC)
and Agence Nationale de la Recherche (ANR) grants. P.B.C. was funded by the ANR
and by the ARSEP (Fondation pour l'Aide à la Recherche sur la Sclérose en Plaques),
and G.T. by governmental and ARC fellowships. This work was also supported by grants
from the Ataxia UK (2491) and the NC3R (NC/L000199/1) awarded to M.F. The Institut
de Génétique et de Biologie Moléculaire et Cellulaire was also supported by a French
state fund through the ANR labex. D.E.S. was funded by Marie Curie Grant CIG 334077/IRTIM.
We thank B. Altenhein, K. Brückner, M. Crozatier, L. Waltzer, M. Logan, E. Kurant,
R. Reuter, E. Kurucz, J.L Dimarcq, J. Hoffmann, C. Goodman, the DHSB, and the BDSC
for reagents and flies. We also thank all of the laboratory members for comments
on the manuscript; C. Diebold, C. Delaporte, M. Pezze, the fly, and imaging and
antibody facilities for technical assistance; and D. Dembele for help with statistics.
In addition, we thank Alison Brewer for help with Luciferase assays.
article_processing_charge: No
article_type: original
author:
- first_name: Guillaume
full_name: Trébuchet, Guillaume
last_name: Trébuchet
- first_name: Pierre B
full_name: Cattenoz, Pierre B
last_name: Cattenoz
- first_name: János
full_name: Zsámboki, János
last_name: Zsámboki
- first_name: David
full_name: Mazaud, David
last_name: Mazaud
- first_name: Daria E
full_name: Siekhaus, Daria E
id: 3D224B9E-F248-11E8-B48F-1D18A9856A87
last_name: Siekhaus
orcid: 0000-0001-8323-8353
- first_name: Manolis
full_name: Fanto, Manolis
last_name: Fanto
- first_name: Angela
full_name: Giangrande, Angela
last_name: Giangrande
citation:
ama: Trébuchet G, Cattenoz PB, Zsámboki J, et al. The Repo homeodomain transcription
factor suppresses hematopoiesis in Drosophila and preserves the glial fate. Journal
of Neuroscience. 2019;39(2):238-255. doi:10.1523/JNEUROSCI.1059-18.2018
apa: Trébuchet, G., Cattenoz, P. B., Zsámboki, J., Mazaud, D., Siekhaus, D. E.,
Fanto, M., & Giangrande, A. (2019). The Repo homeodomain transcription factor
suppresses hematopoiesis in Drosophila and preserves the glial fate. Journal
of Neuroscience. Society for Neuroscience. https://doi.org/10.1523/JNEUROSCI.1059-18.2018
chicago: Trébuchet, Guillaume, Pierre B Cattenoz, János Zsámboki, David Mazaud,
Daria E Siekhaus, Manolis Fanto, and Angela Giangrande. “The Repo Homeodomain
Transcription Factor Suppresses Hematopoiesis in Drosophila and Preserves the
Glial Fate.” Journal of Neuroscience. Society for Neuroscience, 2019. https://doi.org/10.1523/JNEUROSCI.1059-18.2018.
ieee: G. Trébuchet et al., “The Repo homeodomain transcription factor suppresses
hematopoiesis in Drosophila and preserves the glial fate,” Journal of Neuroscience,
vol. 39, no. 2. Society for Neuroscience, pp. 238–255, 2019.
ista: Trébuchet G, Cattenoz PB, Zsámboki J, Mazaud D, Siekhaus DE, Fanto M, Giangrande
A. 2019. The Repo homeodomain transcription factor suppresses hematopoiesis in
Drosophila and preserves the glial fate. Journal of Neuroscience. 39(2), 238–255.
mla: Trébuchet, Guillaume, et al. “The Repo Homeodomain Transcription Factor Suppresses
Hematopoiesis in Drosophila and Preserves the Glial Fate.” Journal of Neuroscience,
vol. 39, no. 2, Society for Neuroscience, 2019, pp. 238–55, doi:10.1523/JNEUROSCI.1059-18.2018.
short: G. Trébuchet, P.B. Cattenoz, J. Zsámboki, D. Mazaud, D.E. Siekhaus, M. Fanto,
A. Giangrande, Journal of Neuroscience 39 (2019) 238–255.
date_created: 2018-12-11T11:44:07Z
date_published: 2019-01-09T00:00:00Z
date_updated: 2023-09-19T10:10:55Z
day: '09'
ddc:
- '570'
department:
- _id: DaSi
doi: 10.1523/JNEUROSCI.1059-18.2018
ec_funded: 1
external_id:
isi:
- '000455189900006'
pmid:
- '30504274'
file:
- access_level: open_access
checksum: 8f6925eb4cd1e8747d8ea25929c68de6
content_type: application/pdf
creator: dernst
date_created: 2020-10-02T09:33:28Z
date_updated: 2020-10-02T09:33:28Z
file_id: '8596'
file_name: 2019_JournNeuroscience_Trebuchet.pdf
file_size: 9455414
relation: main_file
success: 1
file_date_updated: 2020-10-02T09:33:28Z
has_accepted_license: '1'
intvolume: ' 39'
isi: 1
issue: '2'
language:
- iso: eng
month: '01'
oa: 1
oa_version: Published Version
page: 238-255
pmid: 1
project:
- _id: 2536F660-B435-11E9-9278-68D0E5697425
call_identifier: FP7
grant_number: '334077'
name: Investigating the role of transporters in invasive migration through junctions
publication: Journal of Neuroscience
publication_status: published
publisher: Society for Neuroscience
publist_id: '8048'
quality_controlled: '1'
scopus_import: '1'
status: public
title: The Repo homeodomain transcription factor suppresses hematopoiesis in Drosophila
and preserves the glial fate
type: journal_article
user_id: c635000d-4b10-11ee-a964-aac5a93f6ac1
volume: 39
year: '2019'
...
---
_id: '80'
abstract:
- lang: eng
text: 'We consider an interacting, dilute Bose gas trapped in a harmonic potential
at a positive temperature. The system is analyzed in a combination of a thermodynamic
and a Gross–Pitaevskii (GP) limit where the trap frequency ω, the temperature
T, and the particle number N are related by N∼ (T/ ω) 3→ ∞ while the scattering
length is so small that the interaction energy per particle around the center
of the trap is of the same order of magnitude as the spectral gap in the trap.
We prove that the difference between the canonical free energy of the interacting
gas and the one of the noninteracting system can be obtained by minimizing the
GP energy functional. We also prove Bose–Einstein condensation in the following
sense: The one-particle density matrix of any approximate minimizer of the canonical
free energy functional is to leading order given by that of the noninteracting
gas but with the free condensate wavefunction replaced by the GP minimizer.'
article_processing_charge: Yes (via OA deal)
article_type: original
author:
- first_name: Andreas
full_name: Deuchert, Andreas
id: 4DA65CD0-F248-11E8-B48F-1D18A9856A87
last_name: Deuchert
orcid: 0000-0003-3146-6746
- first_name: Robert
full_name: Seiringer, Robert
id: 4AFD0470-F248-11E8-B48F-1D18A9856A87
last_name: Seiringer
orcid: 0000-0002-6781-0521
- first_name: Jakob
full_name: Yngvason, Jakob
last_name: Yngvason
citation:
ama: Deuchert A, Seiringer R, Yngvason J. Bose–Einstein condensation in a dilute,
trapped gas at positive temperature. Communications in Mathematical Physics.
2019;368(2):723-776. doi:10.1007/s00220-018-3239-0
apa: Deuchert, A., Seiringer, R., & Yngvason, J. (2019). Bose–Einstein condensation
in a dilute, trapped gas at positive temperature. Communications in Mathematical
Physics. Springer. https://doi.org/10.1007/s00220-018-3239-0
chicago: Deuchert, Andreas, Robert Seiringer, and Jakob Yngvason. “Bose–Einstein
Condensation in a Dilute, Trapped Gas at Positive Temperature.” Communications
in Mathematical Physics. Springer, 2019. https://doi.org/10.1007/s00220-018-3239-0.
ieee: A. Deuchert, R. Seiringer, and J. Yngvason, “Bose–Einstein condensation in
a dilute, trapped gas at positive temperature,” Communications in Mathematical
Physics, vol. 368, no. 2. Springer, pp. 723–776, 2019.
ista: Deuchert A, Seiringer R, Yngvason J. 2019. Bose–Einstein condensation in a
dilute, trapped gas at positive temperature. Communications in Mathematical Physics.
368(2), 723–776.
mla: Deuchert, Andreas, et al. “Bose–Einstein Condensation in a Dilute, Trapped
Gas at Positive Temperature.” Communications in Mathematical Physics, vol.
368, no. 2, Springer, 2019, pp. 723–76, doi:10.1007/s00220-018-3239-0.
short: A. Deuchert, R. Seiringer, J. Yngvason, Communications in Mathematical Physics
368 (2019) 723–776.
date_created: 2018-12-11T11:44:31Z
date_published: 2019-06-01T00:00:00Z
date_updated: 2023-08-24T14:27:51Z
day: '01'
ddc:
- '530'
department:
- _id: RoSe
doi: 10.1007/s00220-018-3239-0
ec_funded: 1
external_id:
isi:
- '000467796800007'
file:
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checksum: c7e9880b43ac726712c1365e9f2f73a6
content_type: application/pdf
creator: dernst
date_created: 2018-12-17T10:34:06Z
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oa: 1
oa_version: Published Version
page: 723-776
project:
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call_identifier: H2020
grant_number: '694227'
name: Analysis of quantum many-body systems
- _id: 25C878CE-B435-11E9-9278-68D0E5697425
call_identifier: FWF
grant_number: P27533_N27
name: Structure of the Excitation Spectrum for Many-Body Quantum Systems
publication: Communications in Mathematical Physics
publication_status: published
publisher: Springer
publist_id: '7974'
quality_controlled: '1'
scopus_import: '1'
status: public
title: Bose–Einstein condensation in a dilute, trapped gas at positive temperature
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 4359f0d1-fa6c-11eb-b949-802e58b17ae8
volume: 368
year: '2019'
...
---
_id: '8013'
article_number: e1007049
article_processing_charge: No
article_type: original
author:
- first_name: Christopher B.
full_name: Currin, Christopher B.
last_name: Currin
- first_name: Phumlani N.
full_name: Khoza, Phumlani N.
last_name: Khoza
- first_name: Alexander D.
full_name: Antrobus, Alexander D.
last_name: Antrobus
- first_name: Peter E.
full_name: Latham, Peter E.
last_name: Latham
- first_name: Tim P
full_name: Vogels, Tim P
id: CB6FF8D2-008F-11EA-8E08-2637E6697425
last_name: Vogels
orcid: 0000-0003-3295-6181
- first_name: Joseph V.
full_name: Raimondo, Joseph V.
last_name: Raimondo
citation:
ama: 'Currin CB, Khoza PN, Antrobus AD, Latham PE, Vogels TP, Raimondo JV. Think:
Theory for Africa. PLOS Computational Biology. 2019;15(7). doi:10.1371/journal.pcbi.1007049'
apa: 'Currin, C. B., Khoza, P. N., Antrobus, A. D., Latham, P. E., Vogels, T. P.,
& Raimondo, J. V. (2019). Think: Theory for Africa. PLOS Computational
Biology. Public Library of Science. https://doi.org/10.1371/journal.pcbi.1007049'
chicago: 'Currin, Christopher B., Phumlani N. Khoza, Alexander D. Antrobus, Peter
E. Latham, Tim P Vogels, and Joseph V. Raimondo. “Think: Theory for Africa.” PLOS
Computational Biology. Public Library of Science, 2019. https://doi.org/10.1371/journal.pcbi.1007049.'
ieee: 'C. B. Currin, P. N. Khoza, A. D. Antrobus, P. E. Latham, T. P. Vogels, and
J. V. Raimondo, “Think: Theory for Africa,” PLOS Computational Biology,
vol. 15, no. 7. Public Library of Science, 2019.'
ista: 'Currin CB, Khoza PN, Antrobus AD, Latham PE, Vogels TP, Raimondo JV. 2019.
Think: Theory for Africa. PLOS Computational Biology. 15(7), e1007049.'
mla: 'Currin, Christopher B., et al. “Think: Theory for Africa.” PLOS Computational
Biology, vol. 15, no. 7, e1007049, Public Library of Science, 2019, doi:10.1371/journal.pcbi.1007049.'
short: C.B. Currin, P.N. Khoza, A.D. Antrobus, P.E. Latham, T.P. Vogels, J.V. Raimondo,
PLOS Computational Biology 15 (2019).
date_created: 2020-06-25T12:50:39Z
date_published: 2019-07-11T00:00:00Z
date_updated: 2021-01-12T08:16:31Z
day: '11'
ddc:
- '570'
doi: 10.1371/journal.pcbi.1007049
extern: '1'
external_id:
pmid:
- '31295253'
file:
- access_level: open_access
checksum: 723bdfb6ee5c747cbbb32baf01d17fad
content_type: application/pdf
creator: cziletti
date_created: 2020-07-02T12:22:57Z
date_updated: 2020-07-14T12:48:08Z
file_id: '8079'
file_name: 2019_PlosCompBio_Currin.pdf
file_size: 773969
relation: main_file
file_date_updated: 2020-07-14T12:48:08Z
has_accepted_license: '1'
intvolume: ' 15'
issue: '7'
language:
- iso: eng
month: '07'
oa: 1
oa_version: Published Version
pmid: 1
publication: PLOS Computational Biology
publication_identifier:
issn:
- 1553-7358
publication_status: published
publisher: Public Library of Science
quality_controlled: '1'
status: public
title: 'Think: Theory for Africa'
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: D865714E-FA4E-11E9-B85B-F5C5E5697425
volume: 15
year: '2019'
...
---
_id: '8014'
abstract:
- lang: eng
text: 'Working memory, the ability to keep recently accessed information available
for immediate manipulation, has been proposed to rely on two mechanisms that appear
difficult to reconcile: self-sustained neural firing, or the opposite—activity-silent
synaptic traces. Here we review and contrast models of these two mechanisms, and
then show that both phenomena can co-exist within a unified system in which neurons
hold information in both activity and synapses. Rapid plasticity in flexibly-coding
neurons allows features to be bound together into objects, with an important emergent
property being the focus of attention. One memory item is held by persistent activity
in an attended or “focused” state, and is thus remembered better than other items.
Other, previously attended items can remain in memory but in the background, encoded
in activity-silent synaptic traces. This dual functional architecture provides
a unified common mechanism accounting for a diversity of perplexing attention
and memory effects that have been hitherto difficult to explain in a single theoretical
framework.'
article_processing_charge: No
article_type: original
author:
- first_name: Sanjay G.
full_name: Manohar, Sanjay G.
last_name: Manohar
- first_name: Nahid
full_name: Zokaei, Nahid
last_name: Zokaei
- first_name: Sean J.
full_name: Fallon, Sean J.
last_name: Fallon
- first_name: Tim P
full_name: Vogels, Tim P
id: CB6FF8D2-008F-11EA-8E08-2637E6697425
last_name: Vogels
orcid: 0000-0003-3295-6181
- first_name: Masud
full_name: Husain, Masud
last_name: Husain
citation:
ama: Manohar SG, Zokaei N, Fallon SJ, Vogels TP, Husain M. Neural mechanisms of
attending to items in working memory. Neuroscience and Biobehavioral Reviews.
2019;101:1-12. doi:10.1016/j.neubiorev.2019.03.017
apa: Manohar, S. G., Zokaei, N., Fallon, S. J., Vogels, T. P., & Husain, M.
(2019). Neural mechanisms of attending to items in working memory. Neuroscience
and Biobehavioral Reviews. Elsevier . https://doi.org/10.1016/j.neubiorev.2019.03.017
chicago: Manohar, Sanjay G., Nahid Zokaei, Sean J. Fallon, Tim P Vogels, and Masud
Husain. “Neural Mechanisms of Attending to Items in Working Memory.” Neuroscience
and Biobehavioral Reviews. Elsevier , 2019. https://doi.org/10.1016/j.neubiorev.2019.03.017.
ieee: S. G. Manohar, N. Zokaei, S. J. Fallon, T. P. Vogels, and M. Husain, “Neural
mechanisms of attending to items in working memory,” Neuroscience and Biobehavioral
Reviews, vol. 101. Elsevier , pp. 1–12, 2019.
ista: Manohar SG, Zokaei N, Fallon SJ, Vogels TP, Husain M. 2019. Neural mechanisms
of attending to items in working memory. Neuroscience and Biobehavioral Reviews.
101, 1–12.
mla: Manohar, Sanjay G., et al. “Neural Mechanisms of Attending to Items in Working
Memory.” Neuroscience and Biobehavioral Reviews, vol. 101, Elsevier , 2019,
pp. 1–12, doi:10.1016/j.neubiorev.2019.03.017.
short: S.G. Manohar, N. Zokaei, S.J. Fallon, T.P. Vogels, M. Husain, Neuroscience
and Biobehavioral Reviews 101 (2019) 1–12.
date_created: 2020-06-25T12:52:13Z
date_published: 2019-06-01T00:00:00Z
date_updated: 2021-01-12T08:16:31Z
day: '01'
ddc:
- '570'
doi: 10.1016/j.neubiorev.2019.03.017
extern: '1'
external_id:
pmid:
- '30922977'
file:
- access_level: open_access
checksum: 7b972e3d6f7bb3122c8c5648f44e60ca
content_type: application/pdf
creator: cziletti
date_created: 2020-07-02T13:17:52Z
date_updated: 2020-07-14T12:48:08Z
file_id: '8080'
file_name: 2019_NeurosBiobehavRev_Manohar.pdf
file_size: 1754418
relation: main_file
file_date_updated: 2020-07-14T12:48:08Z
has_accepted_license: '1'
intvolume: ' 101'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: 'https://doi.org/10.1101/233007 '
month: '06'
oa: 1
oa_version: Published Version
page: 1-12
pmid: 1
publication: Neuroscience and Biobehavioral Reviews
publication_identifier:
issn:
- 0149-7634
publication_status: published
publisher: 'Elsevier '
quality_controlled: '1'
status: public
title: Neural mechanisms of attending to items in working memory
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: D865714E-FA4E-11E9-B85B-F5C5E5697425
volume: 101
year: '2019'
...