---
_id: '13443'
abstract:
- lang: eng
text: 'The ages of solar-like stars have been at the center of many studies such
as exoplanet characterization or Galactic-archeology. While ages are usually computed
from stellar evolution models, relations linking ages to other stellar properties,
such as rotation and magnetic activity, have been investigated. With the large
catalog of 55,232 rotation periods, Prot, and photometric magnetic activity index,
Sph from Kepler data, we have the opportunity to look for such magneto-gyro-chronology
relations. Stellar ages are obtained with two stellar evolution codes that include
treatment of angular momentum evolution, hence using Prot as input in addition
to classical atmospheric parameters. We explore two different ways of predicting
stellar ages on three subsamples with spectroscopic observations: solar analogs,
late-F and G dwarfs, and K dwarfs. We first perform a Bayesian analysis to derive
relations between Sph and ages between 1 and 5 Gyr, and other stellar properties.
For late-F and G dwarfs, and K dwarfs, the multivariate regression favors the
model with Prot and Sph with median differences of 0.1% and 0.2%, respectively.
We also apply Machine Learning techniques with a Random Forest algorithm to predict
ages up to 14 Gyr with the same set of input parameters. For late-F, G and K dwarfs
together, predicted ages are on average within 5.3% of the model ages and improve
to 3.1% when including Prot. These are very promising results for a quick age
estimation for solar-like stars with photometric observations, especially with
current and future space missions.'
acknowledgement: '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 NASA Science Mission Directorate. STScI
is operated by the Association of Universities for Research in Astronomy, Inc.,
under NASA contract NAS 5–26555. We acknowledge that this research was supported
in part by the National Science Foundation under grant No. NSF PHY-1748958. S.M.
acknowledges support from the Spanish Ministry of Science and Innovation (MICINN)
with the Ramón y Cajal fellowship No. RYC-2015-17697, the grant No. PID2019-107061GB-C66,
and through AEI under the Severo Ochoa Centres of Excellence Programme 2020–2023
(CEX2019-000920-S). S.M. and D.G.R. acknowledge support from the Spanish Ministry
of Science and Innovation (MICINN) with the grant No. PID2019-107187GB-I00. Z.R.C.
acknowledges support from National Aeronautics and Space Administration via the
TESS Guest Investigator Program (grant No. 80NSSC18K18584). The work presented here
was partially supported by the NASA grant NNX17AF27G. A.R.G.S. acknowledges the
support by FCT through national funds and by FEDER through COMPETE2020 by the following
grants: UIDB/04434/2020 and UIDP/04434/2020. A.R.G.S. is supported by FCT through
the work contract No. 2020.02480.CEECIND/CP1631/CT0001. R.A.G., L.A., and S.N.B.
acknowledge the support from PLATO and GOLF CNES grants. S.N.B. acknowledges support
from PLATO ASI-INAF agreement No. 2015-019-R.1-2018.'
article_number: '131'
article_processing_charge: Yes
article_type: original
author:
- first_name: Savita
full_name: Mathur, Savita
last_name: Mathur
- first_name: Zachary R.
full_name: Claytor, Zachary R.
last_name: Claytor
- first_name: Ângela R. G.
full_name: Santos, Ângela R. G.
last_name: Santos
- first_name: Rafael A.
full_name: García, Rafael A.
last_name: García
- first_name: Louis
full_name: Amard, Louis
last_name: Amard
- 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: Enrico
full_name: Corsaro, Enrico
last_name: Corsaro
- first_name: Alfio
full_name: Bonanno, Alfio
last_name: Bonanno
- first_name: Sylvain N.
full_name: Breton, Sylvain N.
last_name: Breton
- first_name: Diego
full_name: Godoy-Rivera, Diego
last_name: Godoy-Rivera
- first_name: Marc H.
full_name: Pinsonneault, Marc H.
last_name: Pinsonneault
- first_name: Jennifer
full_name: van Saders, Jennifer
last_name: van Saders
citation:
ama: Mathur S, Claytor ZR, Santos ÂRG, et al. Magnetic activity evolution of solar-like
stars. I. Sph–age relation derived from Kepler observations. The Astrophysical
Journal. 2023;952(2). doi:10.3847/1538-4357/acd118
apa: Mathur, S., Claytor, Z. R., Santos, Â. R. G., García, R. A., Amard, L., Bugnet,
L. A., … van Saders, J. (2023). Magnetic activity evolution of solar-like stars.
I. Sph–age relation derived from Kepler observations. The Astrophysical Journal.
American Astronomical Society. https://doi.org/10.3847/1538-4357/acd118
chicago: Mathur, Savita, Zachary R. Claytor, Ângela R. G. Santos, Rafael A. García,
Louis Amard, Lisa Annabelle Bugnet, Enrico Corsaro, et al. “Magnetic Activity
Evolution of Solar-like Stars. I. Sph–Age Relation Derived from Kepler Observations.”
The Astrophysical Journal. American Astronomical Society, 2023. https://doi.org/10.3847/1538-4357/acd118.
ieee: S. Mathur et al., “Magnetic activity evolution of solar-like stars.
I. Sph–age relation derived from Kepler observations,” The Astrophysical Journal,
vol. 952, no. 2. American Astronomical Society, 2023.
ista: Mathur S, Claytor ZR, Santos ÂRG, García RA, Amard L, Bugnet LA, Corsaro E,
Bonanno A, Breton SN, Godoy-Rivera D, Pinsonneault MH, van Saders J. 2023. Magnetic
activity evolution of solar-like stars. I. Sph–age relation derived from Kepler
observations. The Astrophysical Journal. 952(2), 131.
mla: Mathur, Savita, et al. “Magnetic Activity Evolution of Solar-like Stars. I.
Sph–Age Relation Derived from Kepler Observations.” The Astrophysical Journal,
vol. 952, no. 2, 131, American Astronomical Society, 2023, doi:10.3847/1538-4357/acd118.
short: S. Mathur, Z.R. Claytor, Â.R.G. Santos, R.A. García, L. Amard, L.A. Bugnet,
E. Corsaro, A. Bonanno, S.N. Breton, D. Godoy-Rivera, M.H. Pinsonneault, J. van
Saders, The Astrophysical Journal 952 (2023).
date_created: 2023-08-01T14:19:16Z
date_published: 2023-08-01T00:00:00Z
date_updated: 2023-12-13T12:00:15Z
day: '01'
ddc:
- '520'
department:
- _id: LiBu
doi: 10.3847/1538-4357/acd118
external_id:
isi:
- '001034185700001'
file:
- access_level: open_access
checksum: f12452834d7ed6748dbf5ace18af4723
content_type: application/pdf
creator: dernst
date_created: 2023-08-02T07:42:26Z
date_updated: 2023-08-02T07:42:26Z
file_id: '13448'
file_name: 2023_AstrophysicalJour_Mathur.pdf
file_size: 4192386
relation: main_file
success: 1
file_date_updated: 2023-08-02T07:42:26Z
has_accepted_license: '1'
intvolume: ' 952'
isi: 1
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
license: https://creativecommons.org/licenses/by/4.0/
month: '08'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
status: public
title: Magnetic activity evolution of solar-like stars. I. Sph–age relation derived
from Kepler observations
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 952
year: '2023'
...
---
_id: '13450'
abstract:
- lang: eng
text: In previous work, we identified a population of 38 cool and luminous variable
stars in the Magellanic Clouds and examined 11 in detail in order to classify
them as either Thorne–Żytkow objects (TŻOs; red supergiants with a neutron star
cores) or super-asymptotic giant branch (sAGB) stars (the most massive stars that
will not undergo core collapse). This population includes HV 2112, a peculiar
star previously considered in other works to be either a TŻO or high-mass asymptotic
giant branch (AGB) star. Here we continue this investigation, using the kinematic
and radio environments and local star formation history of these stars to place
constraints on the age of the progenitor systems and the presence of past supernovae.
These stars are not associated with regions of recent star formation, and we find
no evidence of past supernovae at their locations. Finally, we also assess the
presence of heavy elements and lithium in their spectra compared to red supergiants.
We find strong absorption in Li and s-process elements compared to RSGs in most
of the sample, consistent with sAGB nucleosynthesis, while HV 2112 shows additional
strong lines associated with TŻO nucleosynthesis. Coupled with our previous mass
estimates, the results are consistent with the stars being massive (∼4–6.5 M⊙)
or sAGB (∼6.5–12 M⊙) stars in the thermally pulsing phase, providing crucial observations
of the transition between low- and high-mass stellar populations. HV 2112 is more
ambiguous; it could either be a maximally massive sAGB star, or a TŻO if the minimum
mass for stability extends down to ≲13 M⊙.
article_number: '18'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Anna J. G.
full_name: O‘Grady, Anna J. G.
last_name: O‘Grady
- first_name: Maria R.
full_name: Drout, Maria R.
last_name: Drout
- first_name: B. M.
full_name: Gaensler, B. M.
last_name: Gaensler
- first_name: C. S.
full_name: Kochanek, C. S.
last_name: Kochanek
- first_name: Kathryn F.
full_name: Neugent, Kathryn F.
last_name: Neugent
- first_name: Carolyn L.
full_name: Doherty, Carolyn L.
last_name: Doherty
- first_name: Joshua S.
full_name: Speagle, Joshua S.
last_name: Speagle
- first_name: B. J.
full_name: Shappee, B. J.
last_name: Shappee
- first_name: Michael
full_name: Rauch, Michael
last_name: Rauch
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: Bethany
full_name: Ludwig, Bethany
last_name: Ludwig
- first_name: Todd A.
full_name: Thompson, Todd A.
last_name: Thompson
citation:
ama: O‘Grady AJG, Drout MR, Gaensler BM, et al. Cool, luminous, and highly variable
stars in the Magellanic Clouds. II. Spectroscopic and environmental analysis of
Thorne–Żytkow object and super-AGB star candidates. The Astrophysical Journal.
2023;943(1). doi:10.3847/1538-4357/aca655
apa: O‘Grady, A. J. G., Drout, M. R., Gaensler, B. M., Kochanek, C. S., Neugent,
K. F., Doherty, C. L., … Thompson, T. A. (2023). Cool, luminous, and highly variable
stars in the Magellanic Clouds. II. Spectroscopic and environmental analysis of
Thorne–Żytkow object and super-AGB star candidates. The Astrophysical Journal.
American Astronomical Society. https://doi.org/10.3847/1538-4357/aca655
chicago: O‘Grady, Anna J. G., Maria R. Drout, B. M. Gaensler, C. S. Kochanek, Kathryn
F. Neugent, Carolyn L. Doherty, Joshua S. Speagle, et al. “Cool, Luminous, and
Highly Variable Stars in the Magellanic Clouds. II. Spectroscopic and Environmental
Analysis of Thorne–Żytkow Object and Super-AGB Star Candidates.” The Astrophysical
Journal. American Astronomical Society, 2023. https://doi.org/10.3847/1538-4357/aca655.
ieee: A. J. G. O‘Grady et al., “Cool, luminous, and highly variable stars
in the Magellanic Clouds. II. Spectroscopic and environmental analysis of Thorne–Żytkow
object and super-AGB star candidates,” The Astrophysical Journal, vol.
943, no. 1. American Astronomical Society, 2023.
ista: O‘Grady AJG, Drout MR, Gaensler BM, Kochanek CS, Neugent KF, Doherty CL, Speagle
JS, Shappee BJ, Rauch M, Götberg YLL, Ludwig B, Thompson TA. 2023. Cool, luminous,
and highly variable stars in the Magellanic Clouds. II. Spectroscopic and environmental
analysis of Thorne–Żytkow object and super-AGB star candidates. The Astrophysical
Journal. 943(1), 18.
mla: O‘Grady, Anna J. G., et al. “Cool, Luminous, and Highly Variable Stars in the
Magellanic Clouds. II. Spectroscopic and Environmental Analysis of Thorne–Żytkow
Object and Super-AGB Star Candidates.” The Astrophysical Journal, vol.
943, no. 1, 18, American Astronomical Society, 2023, doi:10.3847/1538-4357/aca655.
short: A.J.G. O‘Grady, M.R. Drout, B.M. Gaensler, C.S. Kochanek, K.F. Neugent, C.L.
Doherty, J.S. Speagle, B.J. Shappee, M. Rauch, Y.L.L. Götberg, B. Ludwig, T.A.
Thompson, The Astrophysical Journal 943 (2023).
date_created: 2023-08-03T10:10:12Z
date_published: 2023-01-20T00:00:00Z
date_updated: 2023-08-21T12:07:05Z
day: '20'
doi: 10.3847/1538-4357/aca655
extern: '1'
external_id:
arxiv:
- '2211.12438'
intvolume: ' 943'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/aca655
month: '01'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Cool, luminous, and highly variable stars in the Magellanic Clouds. II. Spectroscopic
and environmental analysis of Thorne–Żytkow object and super-AGB star candidates
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 943
year: '2023'
...
---
_id: '11509'
abstract:
- lang: eng
text: We present Keck/LRIS follow-up spectroscopy for 13 photometric candidates
of extremely metal-poor galaxies (EMPGs) selected by a machine-learning technique
applied to the deep (∼26 AB mag) optical and wide-area (∼500 deg2) Subaru imaging
data in the EMPRESS survey. Nine out of the 13 candidates are EMPGs with an oxygen
abundance (O/H) less than ∼10% solar value (O/H)⊙, and four sources are contaminants
of moderately metal-rich galaxies or no emission-line objects. Notably, two out
of the nine EMPGs have extremely low stellar masses and oxygen abundances of 5
× 10⁴x–7 × -10⁵ M⊙ and 2%–3% (O/H)⊙, respectively. With a sample of five EMPGs
with (Fe/O) measurements, two (three) of which are taken from this study (the
literature), we confirm that two EMPGs with the lowest (O/H) ratios of ∼2% (O/H)⊙
show high (Fe/O) ratios of ∼0.1, close to the solar abundance ratio. Comparing
galaxy chemical enrichment models, we find that the two EMPGs cannot be explained
by a scenario of metal-poor gas accretion/episodic star formation history due
to their low (N/O) ratios. We conclude that the two EMPGs can be reproduced by
the inclusion of bright hypernovae and/or hypothetical pair-instability supernovae
(SNe) preferentially produced in a metal-poor environment. This conclusion implies
that primordial galaxies at z ∼ 10 could have a high abundance of Fe that did
not originate from Type Ia SNe with delays and that Fe may not serve as a cosmic
clock for primordial galaxies.
acknowledgement: We thank the referee for the valuable comments. We are also grateful
to Koh Takahashi, Nozomu Tominaga, Chiaki Kobayashi, Yutaka Hirai, and Daichi Kashino
for having useful discussions. This paper includes data gathered with the 10 m Keck
Telescope located at W. M. Keck Observatory, Hawaii. We thank the staff of Keck
Observatory for their help with the observations. The Hyper Suprime-Cam (HSC) collaboration
includes the astronomical communities of Japan and Taiwan, and Princeton University.
The HSC instrumentation and software were developed by the National Astronomical
Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics
of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator
Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics
in Taiwan (ASIAA), and Princeton University. Based on data collected at the Subaru
Telescope and retrieved from the HSC data archive system, which is operated by the
Subaru Telescope and Astronomy Data Center at NAOJ. This work was supported by the
joint research program of the Institute for Cosmic Ray Research (ICRR), University
of Tokyo. The Cosmic Dawn Center is funded by the Danish National Research Foundation
under grant No. 140. S.F. acknowledges support from the European Research Council
(ERC) Consolidator Grant funding scheme (project ConTExt, grant No. 648179). This
project has received funding from the European Union’s Horizon 2020 research and
innovation program under the Marie Sklodowska-Curie grant agreement No. 847523 “INTERACTIONS.”
This work is supported by World Premier International Research Center Initiative
(WPI Initiative), MEXT, Japan, as well as the KAKENHI Grant-in-Aid for Scientific
Research (A; 15H02064, 17H01110, 17H01114, 20H00180, and 21H04467) through the Japan
Society for the Promotion of Science (JSPS). This work has been supported in part
by JSPS KAKENHI grant Nos. JP17K05382, JP20K04024, and JP21H04499 (K.N.). Yuki Isobe,
Kimihiko Nakajima, Yuichi Harikane, Takashi Kojima, and Masato Onodera are supported
by JSPS KAKENHI grant Nos. 21J20785, 20K22373,19J01222, 18J12840, and 17K14257,
respectively.
article_number: '111'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Yuki
full_name: Isobe, Yuki
last_name: Isobe
- first_name: Masami
full_name: Ouchi, Masami
last_name: Ouchi
- first_name: Akihiro
full_name: Suzuki, Akihiro
last_name: Suzuki
- first_name: Takashi J.
full_name: Moriya, Takashi J.
last_name: Moriya
- first_name: Kimihiko
full_name: Nakajima, Kimihiko
last_name: Nakajima
- first_name: Ken’ichi
full_name: Nomoto, Ken’ichi
last_name: Nomoto
- first_name: Michael
full_name: Rauch, Michael
last_name: Rauch
- first_name: Yuichi
full_name: Harikane, Yuichi
last_name: Harikane
- first_name: Takashi
full_name: Kojima, Takashi
last_name: Kojima
- first_name: Yoshiaki
full_name: Ono, Yoshiaki
last_name: Ono
- first_name: Seiji
full_name: Fujimoto, Seiji
last_name: Fujimoto
- first_name: Akio K.
full_name: Inoue, Akio K.
last_name: Inoue
- first_name: Ji Hoon
full_name: Kim, Ji Hoon
last_name: Kim
- first_name: Yutaka
full_name: Komiyama, Yutaka
last_name: Komiyama
- first_name: Haruka
full_name: Kusakabe, Haruka
last_name: Kusakabe
- first_name: Chien-Hsiu
full_name: Lee, Chien-Hsiu
last_name: Lee
- 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: Leo
full_name: Michel-Dansac, Leo
last_name: Michel-Dansac
- first_name: Tohru
full_name: Nagao, Tohru
last_name: Nagao
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
- first_name: Moka
full_name: Nishigaki, Moka
last_name: Nishigaki
- first_name: Masato
full_name: Onodera, Masato
last_name: Onodera
- first_name: Yuma
full_name: Sugahara, Yuma
last_name: Sugahara
- first_name: Yi
full_name: Xu, Yi
last_name: Xu
citation:
ama: 'Isobe Y, Ouchi M, Suzuki A, et al. EMPRESS. IV. Extremely metal-poor galaxies
including very low-mass primordial systems with M∗= 104-105⊙
and 2%–3% (O/H): High (Fe/O) suggestive of metal enrichment by hypernovae/pair-instability
supernovae. The Astrophysical Journal. 2022;925(2). doi:10.3847/1538-4357/ac3509'
apa: 'Isobe, Y., Ouchi, M., Suzuki, A., Moriya, T. J., Nakajima, K., Nomoto, K.,
… Xu, Y. (2022). EMPRESS. IV. Extremely metal-poor galaxies including very low-mass
primordial systems with M∗= 104-105⊙ and 2%–3% (O/H): High
(Fe/O) suggestive of metal enrichment by hypernovae/pair-instability supernovae.
The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ac3509'
chicago: 'Isobe, Yuki, Masami Ouchi, Akihiro Suzuki, Takashi J. Moriya, Kimihiko
Nakajima, Ken’ichi Nomoto, Michael Rauch, et al. “EMPRESS. IV. Extremely Metal-Poor
Galaxies Including Very Low-Mass Primordial Systems with M∗= 104-105⊙
and 2%–3% (O/H): High (Fe/O) Suggestive of Metal Enrichment by Hypernovae/Pair-Instability
Supernovae.” The Astrophysical Journal. IOP Publishing, 2022. https://doi.org/10.3847/1538-4357/ac3509.'
ieee: 'Y. Isobe et al., “EMPRESS. IV. Extremely metal-poor galaxies including
very low-mass primordial systems with M∗= 104-105⊙ and 2%–3%
(O/H): High (Fe/O) suggestive of metal enrichment by hypernovae/pair-instability
supernovae,” The Astrophysical Journal, vol. 925, no. 2. IOP Publishing,
2022.'
ista: 'Isobe Y, Ouchi M, Suzuki A, Moriya TJ, Nakajima K, Nomoto K, Rauch M, Harikane
Y, Kojima T, Ono Y, Fujimoto S, Inoue AK, Kim JH, Komiyama Y, Kusakabe H, Lee
C-H, Maseda M, Matthee JJ, Michel-Dansac L, Nagao T, Nanayakkara T, Nishigaki
M, Onodera M, Sugahara Y, Xu Y. 2022. EMPRESS. IV. Extremely metal-poor galaxies
including very low-mass primordial systems with M∗= 104-105⊙
and 2%–3% (O/H): High (Fe/O) suggestive of metal enrichment by hypernovae/pair-instability
supernovae. The Astrophysical Journal. 925(2), 111.'
mla: 'Isobe, Yuki, et al. “EMPRESS. IV. Extremely Metal-Poor Galaxies Including
Very Low-Mass Primordial Systems with M∗= 104-105⊙ and 2%–3%
(O/H): High (Fe/O) Suggestive of Metal Enrichment by Hypernovae/Pair-Instability
Supernovae.” The Astrophysical Journal, vol. 925, no. 2, 111, IOP Publishing,
2022, doi:10.3847/1538-4357/ac3509.'
short: Y. Isobe, M. Ouchi, A. Suzuki, T.J. Moriya, K. Nakajima, K. Nomoto, M. Rauch,
Y. Harikane, T. Kojima, Y. Ono, S. Fujimoto, A.K. Inoue, J.H. Kim, Y. Komiyama,
H. Kusakabe, C.-H. Lee, M. Maseda, J.J. Matthee, L. Michel-Dansac, T. Nagao, T.
Nanayakkara, M. Nishigaki, M. Onodera, Y. Sugahara, Y. Xu, The Astrophysical Journal
925 (2022).
date_created: 2022-07-06T12:01:48Z
date_published: 2022-01-31T00:00:00Z
date_updated: 2022-07-21T05:51:25Z
day: '31'
doi: 10.3847/1538-4357/ac3509
extern: '1'
external_id:
arxiv:
- '2108.03850'
intvolume: ' 925'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2108.03850
month: '01'
oa: 1
oa_version: Published Version
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: 'EMPRESS. IV. Extremely metal-poor galaxies including very low-mass primordial
systems with M∗= 10⁴-10⁵⊙ and 2%–3% (O/H): High (Fe/O) suggestive of metal enrichment
by hypernovae/pair-instability supernovae'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 925
year: '2022'
...
---
_id: '11510'
abstract:
- lang: eng
text: Galaxy evolution is driven by a variety of physical processes that are predicted
to proceed at different rates for different dark matter haloes and environments
across cosmic times. A record of this evolution is preserved in galaxy stellar
populations, which we can access using absorption-line spectroscopy. Here we explore
the large LEGA-C survey (DR3) to investigate the role of the environment and stellar
mass on stellar populations at z ∼ 0.6–1 in the COSMOS field. Leveraging the statistical
power and depth of LEGA-C, we reveal significant gradients in Dn4000 and Hδ equivalent
widths (EWs) distributions over the stellar mass versus environment 2D spaces
for the massive galaxy population (M > 1010 M⊙) at z ∼ 0.6–1.0. Dn4000 and Hδ
EWs primarily depend on stellar mass, but they also depend on environment at fixed
stellar mass. By splitting the sample into centrals and satellites, and in terms
of star-forming galaxies and quiescent galaxies, we reveal that the significant
environmental trends of Dn4000 and Hδ EW, when controlling for stellar mass, are
driven by quiescent galaxies. Regardless of being centrals or satellites, star-forming
galaxies reveal Dn4000 and Hδ EWs, which depend strongly on their stellar mass
and are completely independent of the environment at 0.6 < z < 1.0. The environmental
trends seen for satellite galaxies are fully driven by the trends that hold only
for quiescent galaxies, combined with the strong environmental dependency of the
quiescent fraction at fixed stellar mass. Our results are consistent with recent
predictions from simulations that point toward massive galaxies forming first
in overdensities or the most compact dark matter haloes.
acknowledgement: We thank the reviewer for several valuable comments that improved
the clarity of the manuscript. P.F.W. acknowledges the support of the fellowship
by the East Asian Core Observatories Association. This work is based on observations
made with ESO VLT Telescopes at the La Silla Paranal Observatory under programmes
ID 194-A.2005 and 1100.A-0949 (The LEGA-C Public Spectroscopy Survey). This project
has received funding from the European Research Council (ERC) under the European
Union—Horizon 2020 research and innovation program (grant agreement No. 683184).
article_number: '117'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Arjen
full_name: van der Wel, Arjen
last_name: van der Wel
- first_name: Rachel
full_name: Bezanson, Rachel
last_name: Bezanson
- first_name: Eric
full_name: Bell, Eric
last_name: Bell
- first_name: Adam
full_name: Muzzin, Adam
last_name: Muzzin
- first_name: Francesco
full_name: D’Eugenio, Francesco
last_name: D’Eugenio
- first_name: Behnam
full_name: Darvish, Behnam
last_name: Darvish
- first_name: Anna
full_name: Gallazzi, Anna
last_name: Gallazzi
- first_name: Po-Feng
full_name: Wu, Po-Feng
last_name: Wu
- 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: Ana
full_name: Paulino-Afonso, Ana
last_name: Paulino-Afonso
- first_name: Caroline
full_name: Straatman, Caroline
last_name: Straatman
- first_name: Pieter G.
full_name: van Dokkum, Pieter G.
last_name: van Dokkum
citation:
ama: 'Sobral D, van der Wel A, Bezanson R, et al. The LEGA-C of nature and nurture
in stellar populations at z ∼ 0.6–1.0: Dn4000 and Hδ reveal different assembly
histories for quiescent galaxies in different environments. The Astrophysical
Journal. 2022;926(2). doi:10.3847/1538-4357/ac4419'
apa: 'Sobral, D., van der Wel, A., Bezanson, R., Bell, E., Muzzin, A., D’Eugenio,
F., … van Dokkum, P. G. (2022). The LEGA-C of nature and nurture in stellar populations
at z ∼ 0.6–1.0: Dn4000 and Hδ reveal different assembly histories for quiescent
galaxies in different environments. The Astrophysical Journal. IOP Publishing.
https://doi.org/10.3847/1538-4357/ac4419'
chicago: 'Sobral, David, Arjen van der Wel, Rachel Bezanson, Eric Bell, Adam Muzzin,
Francesco D’Eugenio, Behnam Darvish, et al. “The LEGA-C of Nature and Nurture
in Stellar Populations at z ∼ 0.6–1.0: Dn4000 and Hδ Reveal Different Assembly
Histories for Quiescent Galaxies in Different Environments.” The Astrophysical
Journal. IOP Publishing, 2022. https://doi.org/10.3847/1538-4357/ac4419.'
ieee: 'D. Sobral et al., “The LEGA-C of nature and nurture in stellar populations
at z ∼ 0.6–1.0: Dn4000 and Hδ reveal different assembly histories for quiescent
galaxies in different environments,” The Astrophysical Journal, vol. 926,
no. 2. IOP Publishing, 2022.'
ista: 'Sobral D, van der Wel A, Bezanson R, Bell E, Muzzin A, D’Eugenio F, Darvish
B, Gallazzi A, Wu P-F, Maseda M, Matthee JJ, Paulino-Afonso A, Straatman C, van
Dokkum PG. 2022. The LEGA-C of nature and nurture in stellar populations at z
∼ 0.6–1.0: Dn4000 and Hδ reveal different assembly histories for quiescent galaxies
in different environments. The Astrophysical Journal. 926(2), 117.'
mla: 'Sobral, David, et al. “The LEGA-C of Nature and Nurture in Stellar Populations
at z ∼ 0.6–1.0: Dn4000 and Hδ Reveal Different Assembly Histories for Quiescent
Galaxies in Different Environments.” The Astrophysical Journal, vol. 926,
no. 2, 117, IOP Publishing, 2022, doi:10.3847/1538-4357/ac4419.'
short: D. Sobral, A. van der Wel, R. Bezanson, E. Bell, A. Muzzin, F. D’Eugenio,
B. Darvish, A. Gallazzi, P.-F. Wu, M. Maseda, J.J. Matthee, A. Paulino-Afonso,
C. Straatman, P.G. van Dokkum, The Astrophysical Journal 926 (2022).
date_created: 2022-07-06T12:38:42Z
date_published: 2022-02-17T00:00:00Z
date_updated: 2022-07-19T09:37:42Z
day: '17'
doi: 10.3847/1538-4357/ac4419
extern: '1'
external_id:
arxiv:
- '2112.08372'
intvolume: ' 926'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2112.08372
month: '02'
oa: 1
oa_version: Published Version
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 LEGA-C of nature and nurture in stellar populations at z ∼ 0.6–1.0: Dn4000
and Hδ reveal different assembly histories for quiescent galaxies in different environments'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 926
year: '2022'
...
---
_id: '11511'
abstract:
- lang: eng
text: The ratio of α-elements to iron in galaxies holds valuable information about
the star formation history (SFH) since their enrichment occurs on different timescales.
The fossil record of stars in galaxies has mostly been excavated for passive galaxies,
since the light of star-forming galaxies is dominated by young stars, which have
much weaker atmospheric absorption features. Here we use the largest reference
cosmological simulation of the EAGLE project to investigate the origin of variations
in stellar α-enhancement among star-forming galaxies at z = 0, and their impact
on integrated spectra. The definition of α-enhancement in a composite stellar
population is ambiguous. We elucidate two definitions—termed “mean” and “galactic”
α-enhancement—in more detail. While a star-forming galaxy has a high “mean” α-enhancement
when its stars formed rapidly, a galaxy with a large “galactic” α-enhancement
generally had a delayed SFH. We find that absorption-line strengths of Mg and
Fe correlate with variations in α-enhancement. These correlations are strongest
for the “galactic” α-enhancement. However, we show that these are mostly caused
by other effects that are cross-correlated with α-enhancement, such as variations
in the light-weighted age. This severely complicates the retrieval of α-enhancements
in star-forming galaxies. The ambiguity is not severe for passive galaxies, and
we confirm that spectral variations in these galaxies are caused by measurable
variations in α-enhancements. We suggest that this more complex coupling between
α-enhancement and SFHs can guide the interpretation of new observations of star-forming
galaxies.
acknowledgement: "We thank our anonymous referee for the constructive feedback. We
extend our gratitude to Maarten Baes, Simon Lilly, Rafael Ottersberg, Gabriele Pezzulli,
Alvio Renzini, and Andrea Weibel for insightful discussions. A.G. gratefully acknowledges
financial support from the Fund for Scientific Research Flanders (FWO-Vlaanderen,
project G.0G04.16N). This work used the DiRAC Data Centric system at Durham University,
operated by the ICC on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk).
This equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1,
STFC capital grant ST/H008519/1, and STFC DiRAC Operations grant ST/K003267/1 and
Durham University. DiRAC is part of the National E-Infrastructure.\r\n\r\nWe have
benefited from the data analysis tool Topcat (Taylor 2013) and the programming language
Python, including the numpy (van der Walt et al. 2011), matplotlib (Hunter 2007),
and scipy (Virtanen et al. 2020) packages."
article_number: '73'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Andrea
full_name: Gebek, Andrea
last_name: Gebek
- 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: Gebek A, Matthee JJ. On the variation in stellar α-enhancements of star-forming
galaxies in the EAGLE simulation. The Astrophysical Journal. 2022;924(2).
doi:10.3847/1538-4357/ac350b
apa: Gebek, A., & Matthee, J. J. (2022). On the variation in stellar α-enhancements
of star-forming galaxies in the EAGLE simulation. The Astrophysical Journal.
IOP Publishing. https://doi.org/10.3847/1538-4357/ac350b
chicago: Gebek, Andrea, and Jorryt J Matthee. “On the Variation in Stellar α-Enhancements
of Star-Forming Galaxies in the EAGLE Simulation.” The Astrophysical Journal.
IOP Publishing, 2022. https://doi.org/10.3847/1538-4357/ac350b.
ieee: A. Gebek and J. J. Matthee, “On the variation in stellar α-enhancements of
star-forming galaxies in the EAGLE simulation,” The Astrophysical Journal,
vol. 924, no. 2. IOP Publishing, 2022.
ista: Gebek A, Matthee JJ. 2022. On the variation in stellar α-enhancements of star-forming
galaxies in the EAGLE simulation. The Astrophysical Journal. 924(2), 73.
mla: Gebek, Andrea, and Jorryt J. Matthee. “On the Variation in Stellar α-Enhancements
of Star-Forming Galaxies in the EAGLE Simulation.” The Astrophysical Journal,
vol. 924, no. 2, 73, IOP Publishing, 2022, doi:10.3847/1538-4357/ac350b.
short: A. Gebek, J.J. Matthee, The Astrophysical Journal 924 (2022).
date_created: 2022-07-06T12:48:32Z
date_published: 2022-01-13T00:00:00Z
date_updated: 2022-07-19T09:38:03Z
day: '13'
doi: 10.3847/1538-4357/ac350b
extern: '1'
external_id:
arxiv:
- '2102.04561'
intvolume: ' 924'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2102.04561
month: '01'
oa: 1
oa_version: Published Version
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 variation in stellar α-enhancements of star-forming galaxies in the
EAGLE simulation
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 924
year: '2022'
...
---
_id: '11601'
abstract:
- lang: eng
text: We present the third and final data release of the K2 Galactic Archaeology
Program (K2 GAP) for Campaigns C1–C8 and C10–C18. We provide asteroseismic radius
and mass coefficients, κR and κM, for ∼19,000 red giant stars, which translate
directly to radius and mass given a temperature. As such, K2 GAP DR3 represents
the largest asteroseismic sample in the literature to date. K2 GAP DR3 stellar
parameters are calibrated to be on an absolute parallactic scale based on Gaia
DR2, with red giant branch and red clump evolutionary state classifications provided
via a machine-learning approach. Combining these stellar parameters with GALAH
DR3 spectroscopy, we determine asteroseismic ages with precisions of ∼20%–30%
and compare age-abundance relations to Galactic chemical evolution models among
both low- and high-α populations for α, light, iron-peak, and neutron-capture
elements. We confirm recent indications in the literature of both increased Ba
production at late Galactic times as well as significant contributions to r-process
enrichment from prompt sources associated with, e.g., core-collapse supernovae.
With an eye toward other Galactic archeology applications, we characterize K2
GAP DR3 uncertainties and completeness using injection tests, suggesting that
K2 GAP DR3 is largely unbiased in mass/age, with uncertainties of 2.9% (stat.)
± 0.1% (syst.) and 6.7% (stat.) ± 0.3% (syst.) in κR and κM for red giant branch
stars and 4.7% (stat.) ± 0.3% (syst.) and 11% (stat.) ± 0.9% (syst.) for red clump
stars. We also identify percent-level asteroseismic systematics, which are likely
related to the time baseline of the underlying data, and which therefore should
be considered in TESS asteroseismic analysis.
acknowledgement: "We would like to thank the anonymous referee whose comments significantly
improved the manuscript. J.C.Z. is supported by an NSF Astronomy and Astrophysics
Postdoctoral Fellowship under award AST-2001869. J.C.Z. and M.H.P. acknowledge support
from NASA grants 80NSSC18K0391 and NNX17AJ40G. Y.E. and C.J. acknowledge the support
of the UK Science and Technology Facilities Council (STFC). S.M. acknowledges support
from the Spanish Ministry of Science and Innovation with the Ramon y Cajal fellowship
number RYC-2015-17697 and the grant number PID2019-107187GB-I00. R.A.G. acknowledges
funding received from the PLATO CNES grant. C.K. acknowledges funding from the UK
Science and Technology Facilities Council (STFC) through grants ST/M000958/1, ST/R000905/1,
and ST/V000632/1.\r\n\r\nFunding for the Stellar Astrophysics Centre (SAC) is provided
by the Danish National Research Foundation (grant agreement No. DNRF106).\r\n\r\nThe
K2 Galactic Archaeology Program is supported by the National Aeronautics and Space
Administration under grant NNX16AJ17G issued through the K2 Guest Observer Program.
This publication makes use of data products from the Two Micron All Sky Survey,
which is a joint project of the University of Massachusetts and the Infrared Processing
and Analysis Center/California Institute of Technology, funded by the National Aeronautics
and Space Administration and the National Science Foundation.\r\n\r\nThis paper
includes data collected by the Kepler mission. Funding for the Kepler mission is
provided by the NASA Science Mission directorate.\r\n\r\nParts of this research
were supported by the Australian Research Council Centre of Excellence for All Sky
Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013.\r\n\r\nThis
research was partially conducted during the Exostar19 program at the Kavli Institute
for Theoretical Physics at UC Santa Barbara, which was supported in part by the
National Science Foundation under grant No. NSF PHY-1748958.\r\n\r\nBased in part
on data obtained at Siding Spring Observatory via GALAH. We acknowledge the traditional
owners of the land on which the AAT stands, the Gamilaraay people, and pay our respects
to elders past and present.\r\n\r\nThis work has made use of data from the European
Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by
the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).
Funding for DPAC has been provided by national institutions, in particular the institutions
participating in the Gaia Multilateral Agreement.\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 (www.sdss.org).\r\n\r\nSoftware: asfgrid (Sharma & Stello 2016), corner
(Foreman-Mackey 2016), emcee (Foreman-Mackey et al. 2013), NumPy (Walt 2011), pandas
(McKinney 2010), Matplotlib (Hunter 2007), IPython (Pérez & Granger 2007), SciPy
(Virtanen et al.2020)."
article_number: '191'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Joel C.
full_name: Zinn, Joel C.
last_name: Zinn
- first_name: Dennis
full_name: Stello, Dennis
last_name: Stello
- first_name: Yvonne
full_name: Elsworth, Yvonne
last_name: Elsworth
- first_name: Rafael A.
full_name: García, Rafael A.
last_name: García
- first_name: Thomas
full_name: Kallinger, Thomas
last_name: Kallinger
- first_name: Savita
full_name: Mathur, Savita
last_name: Mathur
- first_name: Benoît
full_name: Mosser, Benoît
last_name: Mosser
- first_name: Marc
full_name: Hon, Marc
last_name: Hon
- 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: Caitlin
full_name: Jones, Caitlin
last_name: Jones
- first_name: Claudia
full_name: Reyes, Claudia
last_name: Reyes
- first_name: Sanjib
full_name: Sharma, Sanjib
last_name: Sharma
- first_name: Ralph
full_name: Schönrich, Ralph
last_name: Schönrich
- first_name: Jack T.
full_name: Warfield, Jack T.
last_name: Warfield
- first_name: Rodrigo
full_name: Luger, Rodrigo
last_name: Luger
- first_name: Andrew
full_name: Vanderburg, Andrew
last_name: Vanderburg
- first_name: Chiaki
full_name: Kobayashi, Chiaki
last_name: Kobayashi
- first_name: Marc H.
full_name: Pinsonneault, Marc H.
last_name: Pinsonneault
- first_name: Jennifer A.
full_name: Johnson, Jennifer A.
last_name: Johnson
- first_name: Daniel
full_name: Huber, Daniel
last_name: Huber
- first_name: Sven
full_name: Buder, Sven
last_name: Buder
- first_name: Meridith
full_name: Joyce, Meridith
last_name: Joyce
- first_name: Joss
full_name: Bland-Hawthorn, Joss
last_name: Bland-Hawthorn
- first_name: Luca
full_name: Casagrande, Luca
last_name: Casagrande
- first_name: Geraint F.
full_name: Lewis, Geraint F.
last_name: Lewis
- first_name: Andrea
full_name: Miglio, Andrea
last_name: Miglio
- first_name: Thomas
full_name: Nordlander, Thomas
last_name: Nordlander
- first_name: Guy R.
full_name: Davies, Guy R.
last_name: Davies
- first_name: Gayandhi De
full_name: Silva, Gayandhi De
last_name: Silva
- first_name: William J.
full_name: Chaplin, William J.
last_name: Chaplin
- first_name: Victor
full_name: Silva Aguirre, Victor
last_name: Silva Aguirre
citation:
ama: 'Zinn JC, Stello D, Elsworth Y, et al. The K2 Galactic Archaeology Program
data release 3: Age-abundance patterns in C1–C8 and C10–C18. The Astrophysical
Journal. 2022;926(2). doi:10.3847/1538-4357/ac2c83'
apa: 'Zinn, J. C., Stello, D., Elsworth, Y., García, R. A., Kallinger, T., Mathur,
S., … Silva Aguirre, V. (2022). The K2 Galactic Archaeology Program data release
3: Age-abundance patterns in C1–C8 and C10–C18. The Astrophysical Journal.
IOP Publishing. https://doi.org/10.3847/1538-4357/ac2c83'
chicago: 'Zinn, Joel C., Dennis Stello, Yvonne Elsworth, Rafael A. García, Thomas
Kallinger, Savita Mathur, Benoît Mosser, et al. “The K2 Galactic Archaeology Program
Data Release 3: Age-Abundance Patterns in C1–C8 and C10–C18.” The Astrophysical
Journal. IOP Publishing, 2022. https://doi.org/10.3847/1538-4357/ac2c83.'
ieee: 'J. C. Zinn et al., “The K2 Galactic Archaeology Program data release
3: Age-abundance patterns in C1–C8 and C10–C18,” The Astrophysical Journal,
vol. 926, no. 2. IOP Publishing, 2022.'
ista: 'Zinn JC, Stello D, Elsworth Y, García RA, Kallinger T, Mathur S, Mosser B,
Hon M, Bugnet LA, Jones C, Reyes C, Sharma S, Schönrich R, Warfield JT, Luger
R, Vanderburg A, Kobayashi C, Pinsonneault MH, Johnson JA, Huber D, Buder S, Joyce
M, Bland-Hawthorn J, Casagrande L, Lewis GF, Miglio A, Nordlander T, Davies GR,
Silva GD, Chaplin WJ, Silva Aguirre V. 2022. The K2 Galactic Archaeology Program
data release 3: Age-abundance patterns in C1–C8 and C10–C18. The Astrophysical
Journal. 926(2), 191.'
mla: 'Zinn, Joel C., et al. “The K2 Galactic Archaeology Program Data Release 3:
Age-Abundance Patterns in C1–C8 and C10–C18.” The Astrophysical Journal,
vol. 926, no. 2, 191, IOP Publishing, 2022, doi:10.3847/1538-4357/ac2c83.'
short: J.C. Zinn, D. Stello, Y. Elsworth, R.A. García, T. Kallinger, S. Mathur,
B. Mosser, M. Hon, L.A. Bugnet, C. Jones, C. Reyes, S. Sharma, R. Schönrich, J.T.
Warfield, R. Luger, A. Vanderburg, C. Kobayashi, M.H. Pinsonneault, J.A. Johnson,
D. Huber, S. Buder, M. Joyce, J. Bland-Hawthorn, L. Casagrande, G.F. Lewis, A.
Miglio, T. Nordlander, G.R. Davies, G.D. Silva, W.J. Chaplin, V. Silva Aguirre,
The Astrophysical Journal 926 (2022).
date_created: 2022-07-18T10:57:30Z
date_published: 2022-02-24T00:00:00Z
date_updated: 2022-08-19T09:52:08Z
day: '24'
doi: 10.3847/1538-4357/ac2c83
extern: '1'
external_id:
arxiv:
- '2108.05455'
intvolume: ' 926'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2108.05455
month: '02'
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 K2 Galactic Archaeology Program data release 3: Age-abundance patterns
in C1–C8 and C10–C18'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 926
year: '2022'
...
---
_id: '13445'
abstract:
- lang: eng
text: Rotation is typically assumed to induce strictly symmetric rotational splitting
into the rotational multiplets of pure p- and g-modes. However, for evolved stars
exhibiting mixed modes, avoided crossings between different multiplet components
are known to yield asymmetric rotational splitting, in particular for near-degenerate
mixed-mode pairs, where notional pure p-modes are fortuitously in resonance with
pure g-modes. These near-degeneracy effects have been described in subgiants,
but their consequences for the characterization of internal rotation in red giants
have not previously been investigated in detail, in part owing to theoretical
intractability. We employ new developments in the analytic theory of mixed-mode
coupling to study these near-resonance phenomena. In the vicinity of the most
p-dominated mixed modes, the near-degenerate intrinsic asymmetry from pure rotational
splitting increases dramatically over the course of stellar evolution, and it
depends strongly on the mode-mixing fraction ζ. We also find that a linear treatment
of rotation remains viable for describing the underlying p- and g-modes, even
when it does not for the resulting mixed modes undergoing these avoided crossings.
We explore observational consequences for potential measurements of asymmetric
mixed-mode splitting, which has been proposed as a magnetic-field diagnostic.
Finally, we propose improved measurement techniques for rotational characterization,
exploiting the linearity of rotational effects on the underlying p/g-modes, while
still accounting for these mixed-mode coupling effects.
article_number: '18'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: J. M. Joel
full_name: Ong, J. M. Joel
last_name: Ong
- 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: Sarbani
full_name: Basu, Sarbani
last_name: Basu
citation:
ama: Ong JMJ, Bugnet LA, Basu S. Mode mixing and rotational splittings. I. Near-degeneracy
effects revisited. The Astrophysical Journal. 2022;940(1). doi:10.3847/1538-4357/ac97e7
apa: Ong, J. M. J., Bugnet, L. A., & Basu, S. (2022). Mode mixing and rotational
splittings. I. Near-degeneracy effects revisited. The Astrophysical Journal.
American Astronomical Society. https://doi.org/10.3847/1538-4357/ac97e7
chicago: Ong, J. M. Joel, Lisa Annabelle Bugnet, and Sarbani Basu. “Mode Mixing
and Rotational Splittings. I. Near-Degeneracy Effects Revisited.” The Astrophysical
Journal. American Astronomical Society, 2022. https://doi.org/10.3847/1538-4357/ac97e7.
ieee: J. M. J. Ong, L. A. Bugnet, and S. Basu, “Mode mixing and rotational splittings.
I. Near-degeneracy effects revisited,” The Astrophysical Journal, vol.
940, no. 1. American Astronomical Society, 2022.
ista: Ong JMJ, Bugnet LA, Basu S. 2022. Mode mixing and rotational splittings. I.
Near-degeneracy effects revisited. The Astrophysical Journal. 940(1), 18.
mla: Ong, J. M. Joel, et al. “Mode Mixing and Rotational Splittings. I. Near-Degeneracy
Effects Revisited.” The Astrophysical Journal, vol. 940, no. 1, 18, American
Astronomical Society, 2022, doi:10.3847/1538-4357/ac97e7.
short: J.M.J. Ong, L.A. Bugnet, S. Basu, The Astrophysical Journal 940 (2022).
date_created: 2023-08-01T14:20:41Z
date_published: 2022-11-16T00:00:00Z
date_updated: 2023-09-06T07:27:45Z
day: '16'
doi: 10.3847/1538-4357/ac97e7
extern: '1'
external_id:
arxiv:
- '2210.01928'
intvolume: ' 940'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2210.01928
month: '11'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Mode mixing and rotational splittings. I. Near-degeneracy effects revisited
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 940
year: '2022'
...
---
_id: '13451'
abstract:
- lang: eng
text: 'We characterize massive stars (M > 8 M⊙) in the nearby (D ∼ 0.8 Mpc) extremely
metal-poor (Z ∼ 5% Z⊙) galaxy Leo A using Hubble Space Telescope ultraviolet (UV),
optical, and near-infrared (NIR) imaging along with Keck/Low-Resolution Imaging
Spectrograph and MMT/Binospec optical spectroscopy for 18 main-sequence OB stars.
We find that: (a) 12 of our 18 stars show emission lines, despite not being associated
with an H ii region, suggestive of stellar activity (e.g., mass loss, accretion,
binary star interaction), which is consistent with previous predictions of enhanced
activity at low metallicity; (b) six are Be stars, which are the first to be spectroscopically
studied at such low metallicity—these Be stars have unusual panchromatic SEDs;
(c) for stars well fit by the TLUSTY nonlocal thermodynamic equilibrium models,
the photometric and spectroscopic values of $\mathrm{log}({T}_{\mathrm{eff}})$
and $\mathrm{log}(g)$ agree to within ∼0.01 dex and ∼0.18 dex, respectively, indicating
that near-UV/optical/NIR imaging can be used to reliably characterize massive
(M ∼ 8–30 M⊙) main-sequence star properties relative to optical spectroscopy;
(d) the properties of the most-massive stars in H II regions are consistent with
constraints from previous nebular emission line studies; and (e) 13 stars with
M > 8M⊙ are >40 pc from a known star cluster or H II region. Our sample comprises
∼50% of all known massive stars at Z ≲ 10% Z⊙with derived stellar parameters,
high-quality optical spectra, and panchromatic photometry.'
article_number: '206'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Maude
full_name: Gull, Maude
last_name: Gull
- first_name: Daniel R.
full_name: Weisz, Daniel R.
last_name: Weisz
- first_name: Peter
full_name: Senchyna, Peter
last_name: Senchyna
- first_name: Nathan R.
full_name: Sandford, Nathan R.
last_name: Sandford
- first_name: Yumi
full_name: Choi, Yumi
last_name: Choi
- first_name: Anna F.
full_name: McLeod, Anna F.
last_name: McLeod
- first_name: Kareem
full_name: El-Badry, Kareem
last_name: El-Badry
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: Karoline M.
full_name: Gilbert, Karoline M.
last_name: Gilbert
- first_name: Martha
full_name: Boyer, Martha
last_name: Boyer
- first_name: Julianne J.
full_name: Dalcanton, Julianne J.
last_name: Dalcanton
- first_name: Puragra
full_name: GuhaThakurta, Puragra
last_name: GuhaThakurta
- first_name: Steven
full_name: Goldman, Steven
last_name: Goldman
- first_name: Paola
full_name: Marigo, Paola
last_name: Marigo
- first_name: Kristen B. W.
full_name: McQuinn, Kristen B. W.
last_name: McQuinn
- first_name: Giada
full_name: Pastorelli, Giada
last_name: Pastorelli
- first_name: Daniel P.
full_name: Stark, Daniel P.
last_name: Stark
- first_name: Evan
full_name: Skillman, Evan
last_name: Skillman
- first_name: Yuan-sen
full_name: Ting, Yuan-sen
last_name: Ting
- first_name: Benjamin F.
full_name: Williams, Benjamin F.
last_name: Williams
citation:
ama: Gull M, Weisz DR, Senchyna P, et al. A panchromatic study of massive stars
in the extremely metal-poor local group dwarf galaxy Leo A. The Astrophysical
Journal. 2022;941(2). doi:10.3847/1538-4357/aca295
apa: Gull, M., Weisz, D. R., Senchyna, P., Sandford, N. R., Choi, Y., McLeod, A.
F., … Williams, B. F. (2022). A panchromatic study of massive stars in the extremely
metal-poor local group dwarf galaxy Leo A. The Astrophysical Journal. American
Astronomical Society. https://doi.org/10.3847/1538-4357/aca295
chicago: Gull, Maude, Daniel R. Weisz, Peter Senchyna, Nathan R. Sandford, Yumi
Choi, Anna F. McLeod, Kareem El-Badry, et al. “A Panchromatic Study of Massive
Stars in the Extremely Metal-Poor Local Group Dwarf Galaxy Leo A.” The Astrophysical
Journal. American Astronomical Society, 2022. https://doi.org/10.3847/1538-4357/aca295.
ieee: M. Gull et al., “A panchromatic study of massive stars in the extremely
metal-poor local group dwarf galaxy Leo A,” The Astrophysical Journal,
vol. 941, no. 2. American Astronomical Society, 2022.
ista: Gull M, Weisz DR, Senchyna P, Sandford NR, Choi Y, McLeod AF, El-Badry K,
Götberg YLL, Gilbert KM, Boyer M, Dalcanton JJ, GuhaThakurta P, Goldman S, Marigo
P, McQuinn KBW, Pastorelli G, Stark DP, Skillman E, Ting Y, Williams BF. 2022.
A panchromatic study of massive stars in the extremely metal-poor local group
dwarf galaxy Leo A. The Astrophysical Journal. 941(2), 206.
mla: Gull, Maude, et al. “A Panchromatic Study of Massive Stars in the Extremely
Metal-Poor Local Group Dwarf Galaxy Leo A.” The Astrophysical Journal,
vol. 941, no. 2, 206, American Astronomical Society, 2022, doi:10.3847/1538-4357/aca295.
short: M. Gull, D.R. Weisz, P. Senchyna, N.R. Sandford, Y. Choi, A.F. McLeod, K.
El-Badry, Y.L.L. Götberg, K.M. Gilbert, M. Boyer, J.J. Dalcanton, P. GuhaThakurta,
S. Goldman, P. Marigo, K.B.W. McQuinn, G. Pastorelli, D.P. Stark, E. Skillman,
Y. Ting, B.F. Williams, The Astrophysical Journal 941 (2022).
date_created: 2023-08-03T10:10:25Z
date_published: 2022-12-27T00:00:00Z
date_updated: 2023-08-21T12:04:58Z
day: '27'
doi: 10.3847/1538-4357/aca295
extern: '1'
external_id:
arxiv:
- '2211.14349'
intvolume: ' 941'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/aca295
month: '12'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: A panchromatic study of massive stars in the extremely metal-poor local group
dwarf galaxy Leo A
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 941
year: '2022'
...
---
_id: '11512'
abstract:
- lang: eng
text: We study the molecular gas content of 24 star-forming galaxies at z = 3–4,
with a median stellar mass of 109.1 M⊙, from the MUSE Hubble Ultra Deep Field
(HUDF) Survey. Selected by their Lyα λ1216 emission and HF160W-band magnitude,
the galaxies show an average $\langle {\mathrm{EW}}_{\mathrm{Ly}\alpha }^{0}\rangle
\approx 20$ Å, below the typical selection threshold for Lyα emitters (${\mathrm{EW}}_{\mathrm{Ly}\alpha
}^{0}\gt 25$ Å), and a rest-frame UV spectrum similar to Lyman-break galaxies.
We use rest-frame optical spectroscopy from KMOS and MOSFIRE, and the UV features
observed with MUSE, to determine the systemic redshifts, which are offset from
Lyα by 〈Δv(Lyα)〉 = 346 km s−1, with a 100 to 600 km s−1 range. Stacking 12CO J
= 4 → 3 and [C i]3P1 → 3P0 (and higher-J CO lines) from the ALMA Spectroscopic
Survey of the HUDF, we determine 3σ upper limits on the line luminosities of 4.0
× 108 K km s−1pc2 and 5.6 × 108 K km s−1pc2, respectively (for a 300 km s−1 line
width). Stacking the 1.2 mm and 3 mm dust-continuum flux densities, we find a
3σ upper limits of 9 μJy and 1.2 μJy, respectively. The inferred gas fractions,
under the assumption of a "Galactic" CO-to-H2 conversion factor and gas-to-dust
ratio, are in tension with previously determined scaling relations. This implies
a substantially higher αCO ≥ 10 and δGDR ≥ 1200, consistent with the subsolar
metallicity estimated for these galaxies ($12+\mathrm{log}({\rm{O}}/{\rm{H}})\approx
7.8\pm 0.2$). The low metallicity of z ≥ 3 star-forming galaxies may thus make
it very challenging to unveil their cold gas through CO or dust emission, warranting
further exploration of alternative tracers, such as [C ii].
acknowledgement: 'We would like to thank the referee for a constructive and helpful
report. L.A.B. is grateful to Corentin Schreiber for assisting with the near-infrared
spectroscopy during the early stages of this work. L.A.B. acknowledges support from
the Leids Kerkhoven-Bosscha Fonds under subsidy numbers 18.2.074 and 19.1.147. D.R.
acknowledges support from the National Science Foundation under grant numbers AST-1614213
and AST-1910107. D.R. also acknowledges support from the Alexander von Humboldt
Foundation through a Humboldt Research Fellowship for Experienced Researchers. A.F.
acknowledges the support from grant PRIN MIUR 201720173ML3WW_001. J.B. acknowledges
support by Fundação para a Ciência e a Tecnologia (FCT) through the research grants
UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020. H.I. acknowledges support
from JSPS KAKENHI grant No. JP19K23462. This work is based on observations collected
at the European Southern Observatory under ESO programs 094.A-2089(B), 095.A-0010(A),
096.A-0045(A), 096.A-0045(B), 099.A-0858(A), and 0101.A-0725(A). 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. This work was supported by a NASA Keck PI Data Award, administered by the NASA
Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck
Observatory from telescope time allocated to the National Aeronautics and Space
Administration through the agency''s scientific partnership with the California
Institute of Technology and the University of California. The Observatory was made
possible by the generous financial support of the W. M. Keck Foundation. 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 Hawaiian community.
We are most fortunate to have the opportunity to conduct observations from this
mountain.'
article_number: '12'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Leindert A.
full_name: Boogaard, Leindert A.
last_name: Boogaard
- first_name: Rychard J.
full_name: Bouwens, Rychard J.
last_name: Bouwens
- first_name: Dominik
full_name: Riechers, Dominik
last_name: Riechers
- first_name: Paul
full_name: van der Werf, Paul
last_name: van der Werf
- first_name: Roland
full_name: Bacon, Roland
last_name: Bacon
- 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: Mauro
full_name: Stefanon, Mauro
last_name: Stefanon
- first_name: Anna
full_name: Feltre, Anna
last_name: Feltre
- first_name: Michael
full_name: Maseda, Michael
last_name: Maseda
- first_name: Hanae
full_name: Inami, Hanae
last_name: Inami
- first_name: Manuel
full_name: Aravena, Manuel
last_name: Aravena
- first_name: Jarle
full_name: Brinchmann, Jarle
last_name: Brinchmann
- first_name: Chris
full_name: Carilli, Chris
last_name: Carilli
- first_name: Thierry
full_name: Contini, Thierry
last_name: Contini
- first_name: Roberto
full_name: Decarli, Roberto
last_name: Decarli
- first_name: Jorge
full_name: González-López, Jorge
last_name: González-López
- first_name: Themiya
full_name: Nanayakkara, Themiya
last_name: Nanayakkara
- first_name: Fabian
full_name: Walter, Fabian
last_name: Walter
citation:
ama: Boogaard LA, Bouwens RJ, Riechers D, et al. Measuring the average molecular
gas content of star-forming galaxies at z = 3–4. The Astrophysical Journal.
2021;916(1). doi:10.3847/1538-4357/ac01d7
apa: Boogaard, L. A., Bouwens, R. J., Riechers, D., van der Werf, P., Bacon, R.,
Matthee, J. J., … Walter, F. (2021). Measuring the average molecular gas content
of star-forming galaxies at z = 3–4. The Astrophysical Journal. IOP Publishing.
https://doi.org/10.3847/1538-4357/ac01d7
chicago: Boogaard, Leindert A., Rychard J. Bouwens, Dominik Riechers, Paul van der
Werf, Roland Bacon, Jorryt J Matthee, Mauro Stefanon, et al. “Measuring the Average
Molecular Gas Content of Star-Forming Galaxies at z = 3–4.” The Astrophysical
Journal. IOP Publishing, 2021. https://doi.org/10.3847/1538-4357/ac01d7.
ieee: L. A. Boogaard et al., “Measuring the average molecular gas content
of star-forming galaxies at z = 3–4,” The Astrophysical Journal, vol. 916,
no. 1. IOP Publishing, 2021.
ista: Boogaard LA, Bouwens RJ, Riechers D, van der Werf P, Bacon R, Matthee JJ,
Stefanon M, Feltre A, Maseda M, Inami H, Aravena M, Brinchmann J, Carilli C, Contini
T, Decarli R, González-López J, Nanayakkara T, Walter F. 2021. Measuring the average
molecular gas content of star-forming galaxies at z = 3–4. The Astrophysical Journal.
916(1), 12.
mla: Boogaard, Leindert A., et al. “Measuring the Average Molecular Gas Content
of Star-Forming Galaxies at z = 3–4.” The Astrophysical Journal, vol. 916,
no. 1, 12, IOP Publishing, 2021, doi:10.3847/1538-4357/ac01d7.
short: L.A. Boogaard, R.J. Bouwens, D. Riechers, P. van der Werf, R. Bacon, J.J.
Matthee, M. Stefanon, A. Feltre, M. Maseda, H. Inami, M. Aravena, J. Brinchmann,
C. Carilli, T. Contini, R. Decarli, J. González-López, T. Nanayakkara, F. Walter,
The Astrophysical Journal 916 (2021).
date_created: 2022-07-06T13:05:50Z
date_published: 2021-07-20T00:00:00Z
date_updated: 2022-07-19T09:32:48Z
day: '20'
doi: 10.3847/1538-4357/ac01d7
extern: '1'
external_id:
arxiv:
- '2105.12489'
intvolume: ' 916'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2105.12489
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: Measuring the average molecular gas content of star-forming galaxies at z =
3–4
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 916
year: '2021'
...
---
_id: '13453'
abstract:
- lang: eng
text: Most massive stars are born in binaries close enough for mass transfer episodes.
These modify the appearance, structure, and future evolution of both stars. We
compute the evolution of a 100-day-period binary, consisting initially of a 25
M⊙ star and a 17 M⊙ star, which experiences stable mass transfer. We focus on
the impact of mass accretion on the surface composition, internal rotation, and
structure of the accretor. To anchor our models, we show that our accretor broadly
reproduces the properties of ζ Ophiuchi, which has long been proposed to have
accreted mass before being ejected as a runaway star when the companion exploded.
We compare our accretor to models of single rotating stars and find that the later
and stronger spin-up provided by mass accretion produces significant differences.
Specifically, the core of the accretor retains higher spin at the end of the main
sequence, and a convective layer develops that changes its density profile. Moreover,
the surface of the accretor star is polluted by CNO-processed material donated
by the companion. Our models show effects of mass accretion in binaries that are
not captured in single rotating stellar models. This possibly impacts the further
evolution (either in a binary or as single stars), the final collapse, and the
resulting spin of the compact object.
article_number: '277'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: M.
full_name: Renzo, M.
last_name: Renzo
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
citation:
ama: 'Renzo M, Götberg YLL. Evolution of accretor stars in massive binaries: Broader
implications from modeling ζ Ophiuchi. The Astrophysical Journal. 2021;923(2).
doi:10.3847/1538-4357/ac29c5'
apa: 'Renzo, M., & Götberg, Y. L. L. (2021). Evolution of accretor stars in
massive binaries: Broader implications from modeling ζ Ophiuchi. The Astrophysical
Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/ac29c5'
chicago: 'Renzo, M., and Ylva Louise Linsdotter Götberg. “Evolution of Accretor
Stars in Massive Binaries: Broader Implications from Modeling ζ Ophiuchi.” The
Astrophysical Journal. American Astronomical Society, 2021. https://doi.org/10.3847/1538-4357/ac29c5.'
ieee: 'M. Renzo and Y. L. L. Götberg, “Evolution of accretor stars in massive binaries:
Broader implications from modeling ζ Ophiuchi,” The Astrophysical Journal,
vol. 923, no. 2. American Astronomical Society, 2021.'
ista: 'Renzo M, Götberg YLL. 2021. Evolution of accretor stars in massive binaries:
Broader implications from modeling ζ Ophiuchi. The Astrophysical Journal. 923(2),
277.'
mla: 'Renzo, M., and Ylva Louise Linsdotter Götberg. “Evolution of Accretor Stars
in Massive Binaries: Broader Implications from Modeling ζ Ophiuchi.” The Astrophysical
Journal, vol. 923, no. 2, 277, American Astronomical Society, 2021, doi:10.3847/1538-4357/ac29c5.'
short: M. Renzo, Y.L.L. Götberg, The Astrophysical Journal 923 (2021).
date_created: 2023-08-03T10:10:48Z
date_published: 2021-12-29T00:00:00Z
date_updated: 2023-08-21T11:59:34Z
day: '29'
doi: 10.3847/1538-4357/ac29c5
extern: '1'
external_id:
arxiv:
- '2107.10933'
intvolume: ' 923'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2107.10933
month: '12'
oa: 1
oa_version: Preprint
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Evolution of accretor stars in massive binaries: Broader implications from
modeling ζ Ophiuchi'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 923
year: '2021'
...
---
_id: '13454'
abstract:
- lang: eng
text: Helium star–carbon-oxygen white dwarf (CO WD) binaries are potential single-degenerate
progenitor systems of thermonuclear supernovae. Revisiting a set of binary evolution
calculations using the stellar evolution code MESA, we refine our previous predictions
about which systems can lead to a thermonuclear supernova and then characterize
the properties of the helium star donor at the time of explosion. We convert these
model properties to near-UV/optical magnitudes assuming a blackbody spectrum and
support this approach using a matched stellar atmosphere model. These models will
be valuable to compare with pre-explosion imaging for future supernovae, though
we emphasize the observational difficulty of detecting extremely blue companions.
The pre-explosion source detected in association with SN 2012Z has been interpreted
as a helium star binary containing an initially ultra-massive WD in a multiday
orbit. However, extending our binary models to initial CO WD masses of up to 1.2
M⊙, we find that these systems undergo off-center carbon ignitions and thus are
not expected to produce thermonuclear supernovae. This tension suggests that,
if SN 2012Z is associated with a helium star–WD binary, then the pre-explosion
optical light from the system must be significantly modified by the binary environment
and/or the WD does not have a carbon-rich interior composition.
article_number: '241'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Tin Long Sunny
full_name: Wong, Tin Long Sunny
last_name: Wong
- first_name: Josiah
full_name: Schwab, Josiah
last_name: Schwab
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
citation:
ama: Wong TLS, Schwab J, Götberg YLL. Pre-explosion properties of Helium star donors
to thermonuclear supernovae. The Astrophysical Journal. 2021;922(2). doi:10.3847/1538-4357/ac27ae
apa: Wong, T. L. S., Schwab, J., & Götberg, Y. L. L. (2021). Pre-explosion properties
of Helium star donors to thermonuclear supernovae. The Astrophysical Journal.
American Astronomical Society. https://doi.org/10.3847/1538-4357/ac27ae
chicago: Wong, Tin Long Sunny, Josiah Schwab, and Ylva Louise Linsdotter Götberg.
“Pre-Explosion Properties of Helium Star Donors to Thermonuclear Supernovae.”
The Astrophysical Journal. American Astronomical Society, 2021. https://doi.org/10.3847/1538-4357/ac27ae.
ieee: T. L. S. Wong, J. Schwab, and Y. L. L. Götberg, “Pre-explosion properties
of Helium star donors to thermonuclear supernovae,” The Astrophysical Journal,
vol. 922, no. 2. American Astronomical Society, 2021.
ista: Wong TLS, Schwab J, Götberg YLL. 2021. Pre-explosion properties of Helium
star donors to thermonuclear supernovae. The Astrophysical Journal. 922(2), 241.
mla: Wong, Tin Long Sunny, et al. “Pre-Explosion Properties of Helium Star Donors
to Thermonuclear Supernovae.” The Astrophysical Journal, vol. 922, no.
2, 241, American Astronomical Society, 2021, doi:10.3847/1538-4357/ac27ae.
short: T.L.S. Wong, J. Schwab, Y.L.L. Götberg, The Astrophysical Journal 922 (2021).
date_created: 2023-08-03T10:10:58Z
date_published: 2021-12-03T00:00:00Z
date_updated: 2023-08-21T11:52:05Z
day: '03'
doi: 10.3847/1538-4357/ac27ae
extern: '1'
external_id:
arxiv:
- '2109.14817'
intvolume: ' 922'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2109.14817
month: '12'
oa: 1
oa_version: Preprint
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Pre-explosion properties of Helium star donors to thermonuclear supernovae
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 922
year: '2021'
...
---
_id: '13456'
abstract:
- lang: eng
text: While most simulations of the epoch of reionization have focused on single-stellar
populations in star-forming dwarf galaxies, products of binary evolution are expected
to significantly contribute to emissions of hydrogen-ionizing photons. Among these
products are stripped stars (or helium stars), which have their envelopes stripped
from interactions with binary companions, leaving an exposed helium core. Previous
work has suggested these stripped stars can dominate the Lyman Continuum (LyC)
photon output of high-redshift, low-luminosity galaxies post-starburst. Other
sources of hard radiation in the early universe include zero-metallicity Population
iii stars, which may have similar spectral energy distribution (SED) properties
to galaxies with radiation dominated by stripped-star emissions. Here, we use
four metrics (the power-law exponent over wavelength intervals 240–500 Å, 600–900
Å, and 1200–2000 Å, and the ratio of total luminosity in FUV wavelengths to LyC
wavelengths) to compare the SEDs of simulated galaxies with only single-stellar
evolution, galaxies containing stripped stars, and galaxies containing Population
iii stars, with four different initial mass functions (IMFs). We find that stripped
stars significantly alter SEDs in the LyC range of galaxies at the epoch of reionization.
SEDs in galaxies with stripped stars have lower power-law indices in the LyC range
and lower FUV to LyC luminosity ratios. These differences in SEDs are present
at all considered luminosities (${M}_{\mathrm{UV}}\gt -15$, AB system), and are
most pronounced for lower-luminosity galaxies. Intrinsic SEDs as well as those
with interstellar medium absorption of galaxies with stripped stars and Population
iii stars are found to be distinct for all tested Population iii IMFs.
article_number: '5'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Elizabeth
full_name: Berzin, Elizabeth
last_name: Berzin
- first_name: Amy
full_name: Secunda, Amy
last_name: Secunda
- first_name: Renyue
full_name: Cen, Renyue
last_name: Cen
- first_name: Alexander
full_name: Menegas, Alexander
last_name: Menegas
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
citation:
ama: Berzin E, Secunda A, Cen R, Menegas A, Götberg YLL. Spectral signatures of
population III and envelope-stripped stars in galaxies at the epoch of reionization.
The Astrophysical Journal. 2021;918(1). doi:10.3847/1538-4357/ac0af6
apa: Berzin, E., Secunda, A., Cen, R., Menegas, A., & Götberg, Y. L. L. (2021).
Spectral signatures of population III and envelope-stripped stars in galaxies
at the epoch of reionization. The Astrophysical Journal. American Astronomical
Society. https://doi.org/10.3847/1538-4357/ac0af6
chicago: Berzin, Elizabeth, Amy Secunda, Renyue Cen, Alexander Menegas, and Ylva
Louise Linsdotter Götberg. “Spectral Signatures of Population III and Envelope-Stripped
Stars in Galaxies at the Epoch of Reionization.” The Astrophysical Journal.
American Astronomical Society, 2021. https://doi.org/10.3847/1538-4357/ac0af6.
ieee: E. Berzin, A. Secunda, R. Cen, A. Menegas, and Y. L. L. Götberg, “Spectral
signatures of population III and envelope-stripped stars in galaxies at the epoch
of reionization,” The Astrophysical Journal, vol. 918, no. 1. American
Astronomical Society, 2021.
ista: Berzin E, Secunda A, Cen R, Menegas A, Götberg YLL. 2021. Spectral signatures
of population III and envelope-stripped stars in galaxies at the epoch of reionization.
The Astrophysical Journal. 918(1), 5.
mla: Berzin, Elizabeth, et al. “Spectral Signatures of Population III and Envelope-Stripped
Stars in Galaxies at the Epoch of Reionization.” The Astrophysical Journal,
vol. 918, no. 1, 5, American Astronomical Society, 2021, doi:10.3847/1538-4357/ac0af6.
short: E. Berzin, A. Secunda, R. Cen, A. Menegas, Y.L.L. Götberg, The Astrophysical
Journal 918 (2021).
date_created: 2023-08-03T10:11:24Z
date_published: 2021-08-27T00:00:00Z
date_updated: 2023-08-21T11:44:50Z
day: '27'
doi: 10.3847/1538-4357/ac0af6
extern: '1'
external_id:
arxiv:
- '2102.08408'
intvolume: ' 918'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/ac0af6
month: '08'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Spectral signatures of population III and envelope-stripped stars in galaxies
at the epoch of reionization
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 918
year: '2021'
...
---
_id: '11513'
abstract:
- lang: eng
text: We report the spectroscopic confirmation of a new protocluster in the COSMOS
field at z ∼ 2.2, COSMOS Cluster 2.2 (CC2.2), originally identified as an overdensity
of narrowband selected Hα emitting candidates. With only two masks of Keck/MOSFIRE
near-IR spectroscopy in both H (∼1.47–1.81 μm) and K (∼1.92–2.40 μm) bands (∼1.5
hr each), we confirm 35 unique protocluster members with at least two emission
lines detected with S/N > 3. Combined with 12 extra members from the zCOSMOS-deep
spectroscopic survey (47 in total), we estimate a mean redshift and a line-of-sight
velocity dispersion of zmean = 2.23224 ± 0.00101 and σlos = 645 ± 69 km s−1 for
this protocluster, respectively. Assuming virialization and spherical symmetry
for the system, we estimate a total mass of Mvir ∼ (1–2) ×1014M⊙ for the structure.
We evaluate a number density enhancement of δg ∼ 7 for this system and we argue
that the structure is likely not fully virialized at z ∼ 2.2. However, in a spherical
collapse model, δg is expected to grow to a linear matter enhancement of ∼1.9
by z = 0, exceeding the collapse threshold of 1.69, and leading to a fully collapsed
and virialized Coma-type structure with a total mass of Mdyn(z = 0) ∼ 9.2 × 1014M⊙
by now. This observationally efficient confirmation suggests that large narrowband
emission-line galaxy surveys, when combined with ancillary photometric data, can
be used to effectively trace the large-scale structure and protoclusters at a
time when they are mostly dominated by star-forming galaxies.
acknowledgement: We are thankful to the anonymous referee for useful comments and
suggestions that improved the quality of this paper. B.D. acknowledges financial
support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number
NNX12AE20G, and the National Science Foundation, grant number 1716907. B.D. is thankful
to Andreas Faisst, Laura Danly, and Matthew Burlando for their companionship during
the observing run. B.D. is grateful to the COSMOS team for their useful comments
during the team meeting in New York City 2019 May 14–17. A.R. research was made
possible by Friends of W. M. Keck Observatory who philanthropically support the
Keck Science Collaborative (KSC) fund. The observations presented herein were obtained
at the W. M. Keck Observatory (program C236, PI Scoville), which is operated as
a scientific partnership among the California Institute of Technology, the University
of California, and the National Aeronautics and Space Administration. The Observatory
was made possible by the generous financial support of the W. M. Keck Foundation.
The authors would like to recognize and acknowledge the very prominent cultural
role and reverence that the summit of Maunakea has always had within the indigenous
Hawaiian community. We are fortunate to have the opportunity to perform observations
from this mountain.
article_number: '8'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Behnam
full_name: Darvish, Behnam
last_name: Darvish
- first_name: Nick Z.
full_name: Scoville, Nick Z.
last_name: Scoville
- first_name: Christopher
full_name: Martin, Christopher
last_name: Martin
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Bahram
full_name: Mobasher, Bahram
last_name: Mobasher
- first_name: Alessandro
full_name: Rettura, Alessandro
last_name: Rettura
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Peter
full_name: Capak, Peter
last_name: Capak
- first_name: Nima
full_name: Chartab, Nima
last_name: Chartab
- first_name: Shoubaneh
full_name: Hemmati, Shoubaneh
last_name: Hemmati
- first_name: Daniel
full_name: Masters, Daniel
last_name: Masters
- first_name: Hooshang
full_name: Nayyeri, Hooshang
last_name: Nayyeri
- first_name: Donal
full_name: O’Sullivan, Donal
last_name: O’Sullivan
- first_name: Ana
full_name: Paulino-Afonso, Ana
last_name: Paulino-Afonso
- first_name: Zahra
full_name: Sattari, Zahra
last_name: Sattari
- first_name: Abtin
full_name: Shahidi, Abtin
last_name: Shahidi
- first_name: Mara
full_name: Salvato, Mara
last_name: Salvato
- first_name: Brian C.
full_name: Lemaux, Brian C.
last_name: Lemaux
- first_name: Olivier Le
full_name: Fèvre, Olivier Le
last_name: Fèvre
- first_name: Olga
full_name: Cucciati, Olga
last_name: Cucciati
citation:
ama: Darvish B, Scoville NZ, Martin C, et al. Spectroscopic confirmation of a coma
cluster progenitor at z ∼ 2.2. The Astrophysical Journal. 2020;892(1).
doi:10.3847/1538-4357/ab75c3
apa: Darvish, B., Scoville, N. Z., Martin, C., Sobral, D., Mobasher, B., Rettura,
A., … Cucciati, O. (2020). Spectroscopic confirmation of a coma cluster progenitor
at z ∼ 2.2. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ab75c3
chicago: Darvish, Behnam, Nick Z. Scoville, Christopher Martin, David Sobral, Bahram
Mobasher, Alessandro Rettura, Jorryt J Matthee, et al. “Spectroscopic Confirmation
of a Coma Cluster Progenitor at z ∼ 2.2.” The Astrophysical Journal. IOP
Publishing, 2020. https://doi.org/10.3847/1538-4357/ab75c3.
ieee: B. Darvish et al., “Spectroscopic confirmation of a coma cluster progenitor
at z ∼ 2.2,” The Astrophysical Journal, vol. 892, no. 1. IOP Publishing,
2020.
ista: Darvish B, Scoville NZ, Martin C, Sobral D, Mobasher B, Rettura A, Matthee
JJ, Capak P, Chartab N, Hemmati S, Masters D, Nayyeri H, O’Sullivan D, Paulino-Afonso
A, Sattari Z, Shahidi A, Salvato M, Lemaux BC, Fèvre OL, Cucciati O. 2020. Spectroscopic
confirmation of a coma cluster progenitor at z ∼ 2.2. The Astrophysical Journal.
892(1), 8.
mla: Darvish, Behnam, et al. “Spectroscopic Confirmation of a Coma Cluster Progenitor
at z ∼ 2.2.” The Astrophysical Journal, vol. 892, no. 1, 8, IOP Publishing,
2020, doi:10.3847/1538-4357/ab75c3.
short: B. Darvish, N.Z. Scoville, C. Martin, D. Sobral, B. Mobasher, A. Rettura,
J.J. Matthee, P. Capak, N. Chartab, S. Hemmati, D. Masters, H. Nayyeri, D. O’Sullivan,
A. Paulino-Afonso, Z. Sattari, A. Shahidi, M. Salvato, B.C. Lemaux, O.L. Fèvre,
O. Cucciati, The Astrophysical Journal 892 (2020).
date_created: 2022-07-06T13:10:51Z
date_published: 2020-03-19T00:00:00Z
date_updated: 2022-07-19T09:31:35Z
day: '19'
doi: 10.3847/1538-4357/ab75c3
extern: '1'
external_id:
arxiv:
- '2002.06207'
intvolume: ' 892'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/2002.06207
month: '03'
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: Spectroscopic confirmation of a coma cluster progenitor at z ∼ 2.2
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 892
year: '2020'
...
---
_id: '11612'
abstract:
- lang: eng
text: Since the onset of the "space revolution" of high-precision high-cadence photometry,
asteroseismology has been demonstrated as a powerful tool for informing Galactic
archeology investigations. The launch of the NASA Transiting Exoplanet Survey
Satellite (TESS) mission has enabled seismic-based inferences to go full sky—providing
a clear advantage for large ensemble studies of the different Milky Way components.
Here we demonstrate its potential for investigating the Galaxy by carrying out
the first asteroseismic ensemble study of red giant stars observed by TESS. We
use a sample of 25 stars for which we measure their global asteroseimic observables
and estimate their fundamental stellar properties, such as radius, mass, and age.
Significant improvements are seen in the uncertainties of our estimates when combining
seismic observables from TESS with astrometric measurements from the Gaia mission
compared to when the seismology and astrometry are applied separately. Specifically,
when combined we show that stellar radii can be determined to a precision of a
few percent, masses to 5%–10%, and ages to the 20% level. This is comparable to
the precision typically obtained using end-of-mission Kepler data.
acknowledgement: 'This Letter includes data collected by the TESS mission, which are
publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding
for the TESS mission is provided by NASA''s Science Mission directorate. Funding
for the TESS Asteroseismic Science Operations Centre is provided by the Danish National
Research Foundation (grant agreement No. DNRF106), ESA PRODEX (PEA 4000119301),
and Stellar Astrophysics Centre (SAC) at Aarhus University. V.S.A. acknowledges
support from the Independent Research Fund Denmark (Research grant 7027-00096B).
D.B. is supported in the form of work contract FCT/MCTES through national funds
and by FEDER through COMPETE2020 in connection to these grants: UID/FIS/04434/2019;
PTDC/FIS-AST/30389/2017 & POCI-01-0145-FEDER-030389. L.B., R.A.G., and B.M. acknowledge
the support from the CNES/PLATO grant. D.B. acknowledges NASA grant NNX16AB76G.
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). This work was supported by FCT/MCTES through national funds (UID/FIS/04434/2019).
E.C. is funded by the European Union''s Horizon 2020 research and innovation program
under the Marie Skłodowska-Curie grant agreement No. 664931. R.H. and M.N.L. acknowledge
the support of the ESA PRODEX programme. T.S.R. acknowledges financial support from
Premiale 2015 MITiC (PI B. Garilli). K.J.B. is supported by the National Science
Foundation under Award AST-1903828. M.S.L. is supported by the Carlsberg Foundation
(grant agreement No. CF17-0760). M.C. is funded by FCT//MCTES through national funds
and by FEDER through COMPETE2020 through these grants: UID/FIS/04434/2019, PTDC/FIS-AST/30389/2017
& POCI-01-0145-FEDER-030389, CEECIND/02619/2017. The research leading to the presented
results has received funding from the European Research Council under the European
Community''s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no
338251 (StellarAges). A.M. acknowledges support from the European Research Council
Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, grant agreement No.
772293, http://www.asterochronometry.eu). A.M.S. is partially supported by MINECO
grant ESP2017-82674-R. J.C.S. acknowledges funding support from Spanish public funds
for research under projects ESP2017-87676-2-2, and from project RYC-2012-09913 under
the ''Ramón y Cajal'' program of the Spanish Ministry of Science and Education.
Resources supporting this work were provided by the NASA High-End Computing (HEC)
Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research
Center for the production of the SPOC data products.'
article_number: L34
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Víctor Silva
full_name: Aguirre, Víctor Silva
last_name: Aguirre
- first_name: Dennis
full_name: Stello, Dennis
last_name: Stello
- first_name: Amalie
full_name: Stokholm, Amalie
last_name: Stokholm
- first_name: Jakob R.
full_name: Mosumgaard, Jakob R.
last_name: Mosumgaard
- first_name: Warrick H.
full_name: Ball, Warrick H.
last_name: Ball
- first_name: Sarbani
full_name: Basu, Sarbani
last_name: Basu
- first_name: Diego
full_name: Bossini, Diego
last_name: Bossini
- 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: Derek
full_name: Buzasi, Derek
last_name: Buzasi
- first_name: Tiago L.
full_name: Campante, Tiago L.
last_name: Campante
- first_name: Lindsey
full_name: Carboneau, Lindsey
last_name: Carboneau
- first_name: William J.
full_name: Chaplin, William J.
last_name: Chaplin
- first_name: Enrico
full_name: Corsaro, Enrico
last_name: Corsaro
- first_name: Guy R.
full_name: Davies, Guy R.
last_name: Davies
- first_name: Yvonne
full_name: Elsworth, Yvonne
last_name: Elsworth
- first_name: Rafael A.
full_name: García, Rafael A.
last_name: García
- first_name: Patrick
full_name: Gaulme, Patrick
last_name: Gaulme
- first_name: Oliver J.
full_name: Hall, Oliver J.
last_name: Hall
- first_name: Rasmus
full_name: Handberg, Rasmus
last_name: Handberg
- first_name: Marc
full_name: Hon, Marc
last_name: Hon
- first_name: Thomas
full_name: Kallinger, Thomas
last_name: Kallinger
- first_name: Liu
full_name: Kang, Liu
last_name: Kang
- first_name: Mikkel N.
full_name: Lund, Mikkel N.
last_name: Lund
- first_name: Savita
full_name: Mathur, Savita
last_name: Mathur
- first_name: Alexey
full_name: Mints, Alexey
last_name: Mints
- first_name: Benoit
full_name: Mosser, Benoit
last_name: Mosser
- first_name: Zeynep
full_name: Çelik Orhan, Zeynep
last_name: Çelik Orhan
- first_name: Thaíse S.
full_name: Rodrigues, Thaíse S.
last_name: Rodrigues
- first_name: Mathieu
full_name: Vrard, Mathieu
last_name: Vrard
- first_name: Mutlu
full_name: Yıldız, Mutlu
last_name: Yıldız
- first_name: Joel C.
full_name: Zinn, Joel C.
last_name: Zinn
- first_name: Sibel
full_name: Örtel, Sibel
last_name: Örtel
- first_name: Paul G.
full_name: Beck, Paul G.
last_name: Beck
- first_name: Keaton J.
full_name: Bell, Keaton J.
last_name: Bell
- first_name: Zhao
full_name: Guo, Zhao
last_name: Guo
- first_name: Chen
full_name: Jiang, Chen
last_name: Jiang
- first_name: James S.
full_name: Kuszlewicz, James S.
last_name: Kuszlewicz
- first_name: Charles A.
full_name: Kuehn, Charles A.
last_name: Kuehn
- first_name: Tanda
full_name: Li, Tanda
last_name: Li
- first_name: Mia S.
full_name: Lundkvist, Mia S.
last_name: Lundkvist
- first_name: Marc
full_name: Pinsonneault, Marc
last_name: Pinsonneault
- first_name: Jamie
full_name: Tayar, Jamie
last_name: Tayar
- first_name: Margarida S.
full_name: Cunha, Margarida S.
last_name: Cunha
- first_name: Saskia
full_name: Hekker, Saskia
last_name: Hekker
- first_name: Daniel
full_name: Huber, Daniel
last_name: Huber
- first_name: Andrea
full_name: Miglio, Andrea
last_name: Miglio
- first_name: Mario J. P.
full_name: F. G. Monteiro, Mario J. P.
last_name: F. G. Monteiro
- first_name: Ditte
full_name: Slumstrup, Ditte
last_name: Slumstrup
- first_name: Mark L.
full_name: Winther, Mark L.
last_name: Winther
- first_name: George
full_name: Angelou, George
last_name: Angelou
- first_name: Othman
full_name: Benomar, Othman
last_name: Benomar
- first_name: Attila
full_name: Bódi, Attila
last_name: Bódi
- first_name: Bruno L.
full_name: De Moura, Bruno L.
last_name: De Moura
- first_name: Sébastien
full_name: Deheuvels, Sébastien
last_name: Deheuvels
- first_name: Aliz
full_name: Derekas, Aliz
last_name: Derekas
- first_name: Maria Pia
full_name: Di Mauro, Maria Pia
last_name: Di Mauro
- first_name: Marc-Antoine
full_name: Dupret, Marc-Antoine
last_name: Dupret
- first_name: Antonio
full_name: Jiménez, Antonio
last_name: Jiménez
- first_name: Yveline
full_name: Lebreton, Yveline
last_name: Lebreton
- first_name: Jaymie
full_name: Matthews, Jaymie
last_name: Matthews
- first_name: Nicolas
full_name: Nardetto, Nicolas
last_name: Nardetto
- first_name: Jose D.
full_name: do Nascimento, Jose D.
last_name: do Nascimento
- first_name: Filipe
full_name: Pereira, Filipe
last_name: Pereira
- first_name: Luisa F.
full_name: Rodríguez Díaz, Luisa F.
last_name: Rodríguez Díaz
- first_name: Aldo M.
full_name: Serenelli, Aldo M.
last_name: Serenelli
- first_name: Emanuele
full_name: Spitoni, Emanuele
last_name: Spitoni
- first_name: Edita
full_name: Stonkutė, Edita
last_name: Stonkutė
- first_name: Juan Carlos
full_name: Suárez, Juan Carlos
last_name: Suárez
- first_name: Robert
full_name: Szabó, Robert
last_name: Szabó
- first_name: Vincent
full_name: Van Eylen, Vincent
last_name: Van Eylen
- first_name: Rita
full_name: Ventura, Rita
last_name: Ventura
- first_name: Kuldeep
full_name: Verma, Kuldeep
last_name: Verma
- first_name: Achim
full_name: Weiss, Achim
last_name: Weiss
- first_name: Tao
full_name: Wu, Tao
last_name: Wu
- first_name: Thomas
full_name: Barclay, Thomas
last_name: Barclay
- first_name: Jørgen
full_name: Christensen-Dalsgaard, Jørgen
last_name: Christensen-Dalsgaard
- first_name: Jon M.
full_name: Jenkins, Jon M.
last_name: Jenkins
- first_name: Hans
full_name: Kjeldsen, Hans
last_name: Kjeldsen
- first_name: George R.
full_name: Ricker, George R.
last_name: Ricker
- first_name: Sara
full_name: Seager, Sara
last_name: Seager
- first_name: Roland
full_name: Vanderspek, Roland
last_name: Vanderspek
citation:
ama: 'Aguirre VS, Stello D, Stokholm A, et al. Detection and characterization of
oscillating red giants: First results from the TESS satellite. The Astrophysical
Journal Letters. 2020;889(2). doi:10.3847/2041-8213/ab6443'
apa: 'Aguirre, V. S., Stello, D., Stokholm, A., Mosumgaard, J. R., Ball, W. H.,
Basu, S., … Vanderspek, R. (2020). Detection and characterization of oscillating
red giants: First results from the TESS satellite. The Astrophysical Journal
Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ab6443'
chicago: 'Aguirre, Víctor Silva, Dennis Stello, Amalie Stokholm, Jakob R. Mosumgaard,
Warrick H. Ball, Sarbani Basu, Diego Bossini, et al. “Detection and Characterization
of Oscillating Red Giants: First Results from the TESS Satellite.” The Astrophysical
Journal Letters. IOP Publishing, 2020. https://doi.org/10.3847/2041-8213/ab6443.'
ieee: 'V. S. Aguirre et al., “Detection and characterization of oscillating
red giants: First results from the TESS satellite,” The Astrophysical Journal
Letters, vol. 889, no. 2. IOP Publishing, 2020.'
ista: 'Aguirre VS, Stello D, Stokholm A, Mosumgaard JR, Ball WH, Basu S, Bossini
D, Bugnet LA, Buzasi D, Campante TL, Carboneau L, Chaplin WJ, Corsaro E, Davies
GR, Elsworth Y, García RA, Gaulme P, Hall OJ, Handberg R, Hon M, Kallinger T,
Kang L, Lund MN, Mathur S, Mints A, Mosser B, Çelik Orhan Z, Rodrigues TS, Vrard
M, Yıldız M, Zinn JC, Örtel S, Beck PG, Bell KJ, Guo Z, Jiang C, Kuszlewicz JS,
Kuehn CA, Li T, Lundkvist MS, Pinsonneault M, Tayar J, Cunha MS, Hekker S, Huber
D, Miglio A, F. G. Monteiro MJP, Slumstrup D, Winther ML, Angelou G, Benomar O,
Bódi A, De Moura BL, Deheuvels S, Derekas A, Di Mauro MP, Dupret M-A, Jiménez
A, Lebreton Y, Matthews J, Nardetto N, do Nascimento JD, Pereira F, Rodríguez
Díaz LF, Serenelli AM, Spitoni E, Stonkutė E, Suárez JC, Szabó R, Van Eylen V,
Ventura R, Verma K, Weiss A, Wu T, Barclay T, Christensen-Dalsgaard J, Jenkins
JM, Kjeldsen H, Ricker GR, Seager S, Vanderspek R. 2020. Detection and characterization
of oscillating red giants: First results from the TESS satellite. The Astrophysical
Journal Letters. 889(2), L34.'
mla: 'Aguirre, Víctor Silva, et al. “Detection and Characterization of Oscillating
Red Giants: First Results from the TESS Satellite.” The Astrophysical Journal
Letters, vol. 889, no. 2, L34, IOP Publishing, 2020, doi:10.3847/2041-8213/ab6443.'
short: V.S. Aguirre, D. Stello, A. Stokholm, J.R. Mosumgaard, W.H. Ball, S. Basu,
D. Bossini, L.A. Bugnet, D. Buzasi, T.L. Campante, L. Carboneau, W.J. Chaplin,
E. Corsaro, G.R. Davies, Y. Elsworth, R.A. García, P. Gaulme, O.J. Hall, R. Handberg,
M. Hon, T. Kallinger, L. Kang, M.N. Lund, S. Mathur, A. Mints, B. Mosser, Z. Çelik
Orhan, T.S. Rodrigues, M. Vrard, M. Yıldız, J.C. Zinn, S. Örtel, P.G. Beck, K.J.
Bell, Z. Guo, C. Jiang, J.S. Kuszlewicz, C.A. Kuehn, T. Li, M.S. Lundkvist, M.
Pinsonneault, J. Tayar, M.S. Cunha, S. Hekker, D. Huber, A. Miglio, M.J.P. F.
G. Monteiro, D. Slumstrup, M.L. Winther, G. Angelou, O. Benomar, A. Bódi, B.L.
De Moura, S. Deheuvels, A. Derekas, M.P. Di Mauro, M.-A. Dupret, A. Jiménez, Y.
Lebreton, J. Matthews, N. Nardetto, J.D. do Nascimento, F. Pereira, L.F. Rodríguez
Díaz, A.M. Serenelli, E. Spitoni, E. Stonkutė, J.C. Suárez, R. Szabó, V. Van Eylen,
R. Ventura, K. Verma, A. Weiss, T. Wu, T. Barclay, J. Christensen-Dalsgaard, J.M.
Jenkins, H. Kjeldsen, G.R. Ricker, S. Seager, R. Vanderspek, The Astrophysical
Journal Letters 889 (2020).
date_created: 2022-07-18T13:52:54Z
date_published: 2020-02-01T00:00:00Z
date_updated: 2022-08-22T07:25:51Z
day: '01'
doi: 10.3847/2041-8213/ab6443
extern: '1'
external_id:
arxiv:
- '1912.07604'
intvolume: ' 889'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1912.07604
month: '02'
oa: 1
oa_version: Preprint
publication: The Astrophysical Journal Letters
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: IOP Publishing
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Detection and characterization of oscillating red giants: First results from
the TESS satellite'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 889
year: '2020'
...
---
_id: '13460'
abstract:
- lang: eng
text: Binary interaction can cause stellar envelopes to be stripped, which significantly
reduces the radius of the star. The orbit of a binary composed of a stripped star
and a compact object can therefore be so tight that the gravitational radiation
the system produces reaches frequencies accessible to the Laser Interferometer
Space Antenna (LISA). Two such stripped stars in tight orbits with white dwarfs
are known so far (ZTF J2130+4420 and CD−30°11223), but many more are expected
to exist. These binaries provide important constraints for binary evolution models
and may be used as LISA verification sources. We develop a Monte Carlo code that
uses detailed evolutionary models to simulate the Galactic population of stripped
stars in tight orbits with either neutron star or white dwarf companions. We predict
0–100 stripped star + white dwarf binaries and 0–4 stripped star + neutron star
binaries with a signal-to-noise ratio >5 after 10 yr of observations with LISA.
More than 90% of these binaries are expected to show large radial velocity shifts
of ≳200 $\,\mathrm{km}\,{{\rm{s}}}^{-1}$, which are spectroscopically detectable.
Photometric variability due to tidal deformation of the stripped star is also
expected and has been observed in ZTF J2130+4420 and CD−30°11223. In addition,
the stripped star + neutron star binaries are expected to be X-ray bright with
LX ≳ 1033–1036 $\,\mathrm{erg}\,{{\rm{s}}}^{-1}$. Our results show that stripped
star binaries are promising multimessenger sources for the upcoming electromagnetic
and gravitational wave facilities.
article_number: '56'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: V.
full_name: Korol, V.
last_name: Korol
- first_name: A.
full_name: Lamberts, A.
last_name: Lamberts
- first_name: T.
full_name: Kupfer, T.
last_name: Kupfer
- first_name: K.
full_name: Breivik, K.
last_name: Breivik
- first_name: B.
full_name: Ludwig, B.
last_name: Ludwig
- first_name: M. R.
full_name: Drout, M. R.
last_name: Drout
citation:
ama: 'Götberg YLL, Korol V, Lamberts A, et al. Stars stripped in binaries: The living
gravitational-wave sources. The Astrophysical Journal. 2020;904(1). doi:10.3847/1538-4357/abbda5'
apa: 'Götberg, Y. L. L., Korol, V., Lamberts, A., Kupfer, T., Breivik, K., Ludwig,
B., & Drout, M. R. (2020). Stars stripped in binaries: The living gravitational-wave
sources. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/abbda5'
chicago: 'Götberg, Ylva Louise Linsdotter, V. Korol, A. Lamberts, T. Kupfer, K.
Breivik, B. Ludwig, and M. R. Drout. “Stars Stripped in Binaries: The Living Gravitational-Wave
Sources.” The Astrophysical Journal. American Astronomical Society, 2020.
https://doi.org/10.3847/1538-4357/abbda5.'
ieee: 'Y. L. L. Götberg et al., “Stars stripped in binaries: The living gravitational-wave
sources,” The Astrophysical Journal, vol. 904, no. 1. American Astronomical
Society, 2020.'
ista: 'Götberg YLL, Korol V, Lamberts A, Kupfer T, Breivik K, Ludwig B, Drout MR.
2020. Stars stripped in binaries: The living gravitational-wave sources. The Astrophysical
Journal. 904(1), 56.'
mla: 'Götberg, Ylva Louise Linsdotter, et al. “Stars Stripped in Binaries: The Living
Gravitational-Wave Sources.” The Astrophysical Journal, vol. 904, no. 1,
56, American Astronomical Society, 2020, doi:10.3847/1538-4357/abbda5.'
short: Y.L.L. Götberg, V. Korol, A. Lamberts, T. Kupfer, K. Breivik, B. Ludwig,
M.R. Drout, The Astrophysical Journal 904 (2020).
date_created: 2023-08-03T10:12:07Z
date_published: 2020-11-20T00:00:00Z
date_updated: 2023-08-21T11:32:40Z
day: '20'
doi: 10.3847/1538-4357/abbda5
extern: '1'
external_id:
arxiv:
- '2006.07382'
intvolume: ' 904'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.48550/arXiv.2006.07382
month: '11'
oa: 1
oa_version: Preprint
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Stars stripped in binaries: The living gravitational-wave sources'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 904
year: '2020'
...
---
_id: '13461'
abstract:
- lang: eng
text: High-resolution numerical simulations including feedback and aimed at calculating
the escape fraction (fesc) of hydrogen-ionizing photons often assume stellar radiation
based on single-stellar population synthesis models. However, strong evidence
suggests the binary fraction of massive stars is ≳70%. Moreover, simulations so
far have yielded values of fesc falling only on the lower end of the ∼10%–20%
range, the amount presumed necessary to reionize the universe. Analyzing a high-resolution
(4 pc) cosmological radiation-hydrodynamic simulation, we study how fesc changes
when we include two different products of binary stellar evolution—stars stripped
of their hydrogen envelopes and massive blue stragglers. Both produce significant
amounts of ionizing photons 10–200 Myr after each starburst. We find the relative
importance of these photons to be amplified with respect to escaped ionizing photons,
because peaks in star formation rates (SFRs) and fesc are often out of phase by
this 10–200 Myr. Additionally, low-mass, bursty galaxies emit Lyman continuum
radiation primarily from binary products when SFRs are low. Observations of these
galaxies by the James Webb Space Telescope could provide crucial information on
the evolution of binary stars as a function of redshift. Overall, including stripped
stars and massive blue stragglers increases our photon-weighted mean escape fraction
($\langle {f}_{\mathrm{esc}}\rangle $) by ∼13% and ∼10%, respectively, resulting
in $\langle {f}_{\mathrm{esc}}\rangle =17 \% $. Our results emphasize that using
updated stellar population synthesis models with binary stellar evolution provides
a more sound physical basis for stellar reionization.
article_number: '72'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Amy
full_name: Secunda, Amy
last_name: Secunda
- first_name: Renyue
full_name: Cen, Renyue
last_name: Cen
- first_name: Taysun
full_name: Kimm, Taysun
last_name: Kimm
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: Selma E.
full_name: de Mink, Selma E.
last_name: de Mink
citation:
ama: Secunda A, Cen R, Kimm T, Götberg YLL, de Mink SE. Delayed photons from binary
evolution help reionize the universe. The Astrophysical Journal. 2020;901(1).
doi:10.3847/1538-4357/abaefa
apa: Secunda, A., Cen, R., Kimm, T., Götberg, Y. L. L., & de Mink, S. E. (2020).
Delayed photons from binary evolution help reionize the universe. The Astrophysical
Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/abaefa
chicago: Secunda, Amy, Renyue Cen, Taysun Kimm, Ylva Louise Linsdotter Götberg,
and Selma E. de Mink. “Delayed Photons from Binary Evolution Help Reionize the
Universe.” The Astrophysical Journal. American Astronomical Society, 2020.
https://doi.org/10.3847/1538-4357/abaefa.
ieee: A. Secunda, R. Cen, T. Kimm, Y. L. L. Götberg, and S. E. de Mink, “Delayed
photons from binary evolution help reionize the universe,” The Astrophysical
Journal, vol. 901, no. 1. American Astronomical Society, 2020.
ista: Secunda A, Cen R, Kimm T, Götberg YLL, de Mink SE. 2020. Delayed photons from
binary evolution help reionize the universe. The Astrophysical Journal. 901(1),
72.
mla: Secunda, Amy, et al. “Delayed Photons from Binary Evolution Help Reionize the
Universe.” The Astrophysical Journal, vol. 901, no. 1, 72, American Astronomical
Society, 2020, doi:10.3847/1538-4357/abaefa.
short: A. Secunda, R. Cen, T. Kimm, Y.L.L. Götberg, S.E. de Mink, The Astrophysical
Journal 901 (2020).
date_created: 2023-08-03T10:12:16Z
date_published: 2020-09-23T00:00:00Z
date_updated: 2023-08-09T13:01:45Z
day: '23'
doi: 10.3847/1538-4357/abaefa
extern: '1'
external_id:
arxiv:
- '2007.15012'
intvolume: ' 901'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/abaefa
month: '09'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
eissn:
- 1538-4357
issn:
- 0004-637X
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Delayed photons from binary evolution help reionize the universe
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 901
year: '2020'
...
---
_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'
...