---
DOAJ_listed: '1'
OA_place: publisher
OA_type: gold
PlanS_conform: '1'
_id: '22264'
abstract:
- lang: eng
text: 'The correlation between galaxy stellar mass and gas-phase metallicity, known
as the mass–metallicity relation (MZR), gives key insights into the processes
that govern galaxy evolution. However, unquantified observational and selection
biases can result in systematic errors in attempts to recover the intrinsic MZR,
particularly at higher redshifts. We characterize the MZR at z ∼ 3–6 within a
fully Bayesian framework using JWST/NIRSpec spectra of 191 galaxies from the RUBIES
survey. We forward model the observed mass–metallicity surface using prospector-generated
spectra to account for two selection biases: the survey selection function and
the success in observing high signal-to-noise ratio emission lines. We demonstrate
that the RUBIES selection function, based on F444W magnitude and F150W – F444W
color, has a negligible effect on our measured MZR. A correct treatment of the
non-Gaussian metallicity uncertainties from strong-line calibrations lowers the
derived MZR normalization by 0.2 dex and flattens the slope by ∼20%; forward modeling
the effect of emission line observability steepens the slope by ∼15%. Both of
these biases must be taken into account in order to properly measure the intrinsic
MZR. This novel forward-modeling process motivates careful consideration of selection
functions in future surveys, and paves the way for robust, high-redshift chemical
enrichment studies that trace the evolution of the MZR across cosmic time.'
acknowledgement: "This work is based on observations made with the NASA/ESA/CSA James
Webb Space Telescope. The data were obtained from the Mikulski Archive for Space
Telescopes at the Space Telescope Science Institute, which is operated by the Association
of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127
for JWST. These observations are associated with program ID 4233. This material
is based upon work supported by the National Science Foundation Graduate Research
Fellowship under grant No. 2137424 as well as work supported by NASA under Award
No. 2025_3-0, issued through the Wisconsin Space Grant Consortium, and JWST-GO-4233.
Any opinions, findings, and conclusions or recommendations expressed in this material
are those of the author(s) and do not necessarily reflect the views of the National
Aeronautics and Space Administration. Support for program ID 4233 was provided by
NASA through a grant from the Space Telescope Science Institute, which is operated
by the Association of Universities for Research in Astronomy, Inc., under NASA contract
NAS 5-03127. M.V.M. is supported by the National Science Foundation via grant AAG
2205519. A.d.G. acknowledges support from a Clay Fellowship awarded by the Smithsonian
Astrophysical Observatory. T.B.M. was supported by a CIERA Fellowship. Part of the
computations for this research were performed on the Pennsylvania State University’s
Institute for Computational and Data Sciences’ Roar supercomputer. Some/all of the
data presented in this article were obtained from the Mikulski Archive for Space
Telescopes (MAST) at the Space Telescope Science Institute. The specific observations
analyzed can be accessed via doi:10.17909/qk5z-7p30. The scripts used to generate
the data and results in this work can be found in Zenodo at doi:10.5281/zenodo.20513668
and GitHub \r\nhttps://github.com/zachlewis99/rubies_mzr "
article_number: '159'
article_processing_charge: Yes
article_type: original
arxiv: 1
author:
- first_name: Zach
full_name: Lewis, Zach
last_name: Lewis
- first_name: Michael V.
full_name: Maseda, Michael V.
last_name: Maseda
- first_name: Anna
full_name: De Graaff, Anna
last_name: De Graaff
- first_name: Joel
full_name: Leja, Joel
last_name: Leja
- first_name: Bingjie
full_name: Wang, Bingjie
last_name: Wang
- first_name: Hans Walter
full_name: Rix, Hans Walter
last_name: Rix
- first_name: Ian
full_name: Mcconachie, Ian
last_name: Mcconachie
- first_name: Nikko J.
full_name: Cleri, Nikko J.
last_name: Cleri
- first_name: Rachel
full_name: Bezanson, Rachel
last_name: Bezanson
- first_name: Leindert A.
full_name: Boogaard, Leindert A.
last_name: Boogaard
- first_name: Gabriel
full_name: Brammer, Gabriel
last_name: Brammer
- first_name: Jenny E.
full_name: Greene, Jenny E.
last_name: Greene
- first_name: Michaela
full_name: Hirschmann, Michaela
last_name: Hirschmann
- first_name: Harley
full_name: Katz, Harley
last_name: Katz
- first_name: Ivo
full_name: Labbé, Ivo
last_name: Labbé
- 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: Tim B.
full_name: Miller, Tim B.
last_name: Miller
- first_name: Rohan P.
full_name: Naidu, Rohan P.
last_name: Naidu
- first_name: Pascal A.
full_name: Oesch, Pascal A.
last_name: Oesch
- first_name: David J.
full_name: Setton, David J.
last_name: Setton
- first_name: Katherine A.
full_name: Suess, Katherine A.
last_name: Suess
- first_name: Andrea
full_name: Weibel, Andrea
last_name: Weibel
- first_name: Katherine E.
full_name: Whitaker, Katherine E.
last_name: Whitaker
- first_name: Christina C.
full_name: Williams, Christina C.
last_name: Williams
citation:
ama: Lewis Z, Maseda MV, De Graaff A, et al. The mass–metallicity relation and its
observational effects at z ∼ 3–6. The Astrophysical Journal. 2026;1005(2).
doi:10.3847/1538-4357/ae7bfc
apa: Lewis, Z., Maseda, M. V., De Graaff, A., Leja, J., Wang, B., Rix, H. W., …
Williams, C. C. (2026). The mass–metallicity relation and its observational effects
at z ∼ 3–6. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae7bfc
chicago: Lewis, Zach, Michael V. Maseda, Anna De Graaff, Joel Leja, Bingjie Wang,
Hans Walter Rix, Ian Mcconachie, et al. “The Mass–Metallicity Relation and Its
Observational Effects at z ∼ 3–6.” The Astrophysical Journal. IOP Publishing,
2026. https://doi.org/10.3847/1538-4357/ae7bfc.
ieee: Z. Lewis et al., “The mass–metallicity relation and its observational
effects at z ∼ 3–6,” The Astrophysical Journal, vol. 1005, no. 2. IOP Publishing,
2026.
ista: Lewis Z, Maseda MV, De Graaff A, Leja J, Wang B, Rix HW, Mcconachie I, Cleri
NJ, Bezanson R, Boogaard LA, Brammer G, Greene JE, Hirschmann M, Katz H, Labbé
I, Matthee JJ, Miller TB, Naidu RP, Oesch PA, Setton DJ, Suess KA, Weibel A, Whitaker
KE, Williams CC. 2026. The mass–metallicity relation and its observational effects
at z ∼ 3–6. The Astrophysical Journal. 1005(2), 159.
mla: Lewis, Zach, et al. “The Mass–Metallicity Relation and Its Observational Effects
at z ∼ 3–6.” The Astrophysical Journal, vol. 1005, no. 2, 159, IOP Publishing,
2026, doi:10.3847/1538-4357/ae7bfc.
short: Z. Lewis, M.V. Maseda, A. De Graaff, J. Leja, B. Wang, H.W. Rix, I. Mcconachie,
N.J. Cleri, R. Bezanson, L.A. Boogaard, G. Brammer, J.E. Greene, M. Hirschmann,
H. Katz, I. Labbé, J.J. Matthee, T.B. Miller, R.P. Naidu, P.A. Oesch, D.J. Setton,
K.A. Suess, A. Weibel, K.E. Whitaker, C.C. Williams, The Astrophysical Journal
1005 (2026).
das_tickbox: '1'
dataavailabilitystatement: The specific observations analyzed can be accessed via
doi:10.17909/qk5z-7p30. The scripts used to generate the data and results in this
work can be found in Zenodo at doi:10.5281/zenodo.20513668 and GitHub https://github.com/zachlewis99/rubies_mzr
date_created: 2026-07-12T22:02:17Z
date_published: 2026-07-10T00:00:00Z
date_updated: 2026-07-13T07:40:41Z
day: '10'
ddc:
- '520'
department:
- _id: JoMa
doi: 10.3847/1538-4357/ae7bfc
external_id:
arxiv:
- '2512.03134'
file:
- access_level: open_access
checksum: 9b13fbbc5e5e921c04676ebc532d9c42
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creator: dernst
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fulldoi: https://doi.org/10.3847/1538-4357/ae7bfc
has_accepted_license: '1'
intvolume: ' 1005'
issue: '2'
keyword:
- Galaxy evolution
- Chemical enrichment
- Metallicity
- Galaxy abundances
- Scaling relations
language:
- iso: eng
license: https://creativecommons.org/licenses/by/4.0/
month: '07'
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'
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scopus_import: '1'
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supplementarymaterial: no
title: The mass–metallicity relation and its observational effects at z ∼ 3–6
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: 1005
year: '2026'
...
---
_id: '11585'
abstract:
- lang: eng
text: "Observations show that star-forming galaxies reside on a tight three-dimensional
plane between mass, gas-phase metallicity and star formation rate (SFR), which
can be explained by the interplay between metal-poor gas inflows, SFR and outflows.
However, different metals are released on different time-scales, which may affect
the slope of this relation. Here, we use central, star-forming galaxies with Mstar
= 109.0−10.5 M\f from the EAGLE hydrodynamical simulation to examine three-dimensional
relations between mass, SFR and chemical enrichment using absolute and relative
C, N, O and Fe abundances. We show that the scatter is smaller when gas-phase
α-enhancement is used rather than metallicity. A similar plane also exists for
stellar α-enhancement, implying that present-day specific SFRs are correlated
with long time-scale star formation histories. Between z = 0 and 1, the α-enhancement
plane is even more insensitive to redshift than the plane using metallicity. However,
it evolves at z > 1 due to lagging iron yields. At fixed mass, galaxies with higher
SFRs have star formation histories shifted toward late times, are more α-enhanced
and this α-enhancement increases with redshift as observed. These findings suggest
that relations between physical properties inferred from observations may be affected
by systematic variations in α-enhancements."
acknowledgement: We thank the anonymous referee for their constructive comments. JM
acknowledges the support of a Huygens PhD fellowship from Leiden University. We
thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge
the use of the Topcat software (Taylor 2013) for assisting in rapid exploration
of multi-dimensional datasets and the use of Python and its numpy, matplotlib and
pandas packages.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
citation:
ama: Matthee JJ. Differences in galaxy colours are not just about the mass. Nature
Astronomy. 2021;5:984-985. doi:10.1038/s41550-021-01415-y
apa: Matthee, J. J. (2021). Differences in galaxy colours are not just about the
mass. Nature Astronomy. Springer Nature. https://doi.org/10.1038/s41550-021-01415-y
chicago: Matthee, Jorryt J. “Differences in Galaxy Colours Are Not Just about the
Mass.” Nature Astronomy. Springer Nature, 2021. https://doi.org/10.1038/s41550-021-01415-y.
ieee: J. J. Matthee, “Differences in galaxy colours are not just about the mass,”
Nature Astronomy, vol. 5. Springer Nature, pp. 984–985, 2021.
ista: Matthee JJ. 2021. Differences in galaxy colours are not just about the mass.
Nature Astronomy. 5, 984–985.
mla: Matthee, Jorryt J. “Differences in Galaxy Colours Are Not Just about the Mass.”
Nature Astronomy, vol. 5, Springer Nature, 2021, pp. 984–85, doi:10.1038/s41550-021-01415-y.
short: J.J. Matthee, Nature Astronomy 5 (2021) 984–985.
date_created: 2022-07-14T13:13:39Z
date_published: 2021-07-05T00:00:00Z
date_updated: 2024-10-14T11:38:08Z
day: '05'
doi: 10.1038/s41550-021-01415-y
extern: '1'
external_id:
arxiv:
- '1802.06786'
fulldoi: https://doi.org/10.1038/s41550-021-01415-y
intvolume: ' 5'
keyword:
- Astronomy and Astrophysics
- galaxies
- formation - galaxies
- evolution - galaxies
- star formation - galaxies
- abundances
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1802.06786
month: '07'
oa: 1
oa_version: Preprint
page: 984-985
publication: Nature Astronomy
publication_identifier:
eissn:
- 2397-3366
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
scopus_import: '1'
status: public
title: Differences in galaxy colours are not just about the mass
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 5
year: '2021'
...
---
_id: '11584'
abstract:
- lang: eng
text: Observations show that star-forming galaxies reside on a tight 3D plane between
mass, gas-phase metallicity, and star formation rate (SFR), which can be explained
by the interplay between metal-poor gas inflows, SFR and outflows. However, different
metals are released on different time-scales, which may affect the slope of this
relation. Here, we use central, star-forming galaxies with Mstar = 109.0–10.5
M⊙ from the EAGLE hydrodynamical simulation to examine 3D relations between mass,
SFR, and chemical enrichment using absolute and relative C, N, O, and Fe abundances.
We show that the scatter is smaller when gas-phase α-enhancement is used rather
than metallicity. A similar plane also exists for stellar α-enhancement, implying
that present-day specific SFRs are correlated with long time-scale star formation
histories. Between z = 0 and 1, the α-enhancement plane is even more insensitive
to redshift than the plane using metallicity. However, it evolves at z > 1 due
to lagging iron yields. At fixed mass, galaxies with higher SFRs have star formation
histories shifted towards late times, are more α-enhanced, and this α-enhancement
increases with redshift as observed. These findings suggest that relations between
physical properties inferred from observations may be affected by systematic variations
in α-enhancements.
acknowledgement: We thank the anonymous referee for their constructive comments. JM
acknowledges the support of a Huygens PhD fellowship from Leiden University. We
thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge
the use of the TOPCAT software (Taylor 2013) for assisting in rapid exploration
of multidimensional data sets and the use of PYTHON and its NUMPY, MATPLOTLIB, and
PANDAS packages.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: Joop
full_name: Schaye, Joop
last_name: Schaye
citation:
ama: 'Matthee JJ, Schaye J. Star-forming galaxies are predicted to lie on a fundamental
plane of mass, star formation rate, and α-enhancement. Monthly Notices of the
Royal Astronomical Society: Letters. 2018;479(1):L34-L39. doi:10.1093/mnrasl/sly093'
apa: 'Matthee, J. J., & Schaye, J. (2018). Star-forming galaxies are predicted
to lie on a fundamental plane of mass, star formation rate, and α-enhancement.
Monthly Notices of the Royal Astronomical Society: Letters. Oxford University
Press. https://doi.org/10.1093/mnrasl/sly093'
chicago: 'Matthee, Jorryt J, and Joop Schaye. “Star-Forming Galaxies Are Predicted
to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.”
Monthly Notices of the Royal Astronomical Society: Letters. Oxford University
Press, 2018. https://doi.org/10.1093/mnrasl/sly093.'
ieee: 'J. J. Matthee and J. Schaye, “Star-forming galaxies are predicted to lie
on a fundamental plane of mass, star formation rate, and α-enhancement,” Monthly
Notices of the Royal Astronomical Society: Letters, vol. 479, no. 1. Oxford
University Press, pp. L34–L39, 2018.'
ista: 'Matthee JJ, Schaye J. 2018. Star-forming galaxies are predicted to lie on
a fundamental plane of mass, star formation rate, and α-enhancement. Monthly Notices
of the Royal Astronomical Society: Letters. 479(1), L34–L39.'
mla: 'Matthee, Jorryt J., and Joop Schaye. “Star-Forming Galaxies Are Predicted
to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.”
Monthly Notices of the Royal Astronomical Society: Letters, vol. 479, no.
1, Oxford University Press, 2018, pp. L34–39, doi:10.1093/mnrasl/sly093.'
short: 'J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society:
Letters 479 (2018) L34–L39.'
date_created: 2022-07-14T12:49:47Z
date_published: 2018-09-01T00:00:00Z
date_updated: 2024-10-14T11:37:53Z
day: '01'
doi: 10.1093/mnrasl/sly093
extern: '1'
external_id:
arxiv:
- '1802.06786'
fulldoi: https://doi.org/10.1093/mnrasl/sly093
intvolume: ' 479'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: abundances'
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: star formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1802.06786
month: '09'
oa: 1
oa_version: Preprint
page: L34 - L39
publication: 'Monthly Notices of the Royal Astronomical Society: Letters'
publication_identifier:
eissn:
- 1745-3933
issn:
- 1745-3925
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Star-forming galaxies are predicted to lie on a fundamental plane of mass,
star formation rate, and α-enhancement
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 479
year: '2018'
...
---
_id: '11582'
abstract:
- lang: eng
text: We have observed a sample of typical z ∼ 1 star-forming galaxies, selected
from the HiZELS survey, with the new K-band Multi-Object Spectrograph (KMOS) near-infrared,
multi-integral field unit instrument on the Very Large Telescope (VLT), in order
to obtain their dynamics and metallicity gradients. The majority of our galaxies
have a metallicity gradient consistent with being flat or negative (i.e. higher
metallicity cores than outskirts). Intriguingly, we find a trend between metallicity
gradient and specific star formation rate (sSFR), such that galaxies with a high
sSFR tend to have relatively metal poor centres, a result which is strengthened
when combined with data sets from the literature. This result appears to explain
the discrepancies reported between different high-redshift studies and varying
claims for evolution. From a galaxy evolution perspective, the trend we see would
mean that a galaxy's sSFR is governed by the amount of metal-poor gas that can
be funnelled into its core, triggered either by merging or through efficient accretion.
In fact, merging may play a significant role as it is the starburst galaxies at
all epochs, which have the more positive metallicity gradients. Our results may
help to explain the origin of the fundamental metallicity relation, in which galaxies
at a fixed mass are observed to have lower metallicities at higher star formation
rates, especially if the metallicity is measured in an aperture encompassing only
the central regions of the galaxy. Finally, we note that this study demonstrates
the power of KMOS as an efficient instrument for large-scale resolved galaxy surveys.
acknowledgement: First, we acknowledge the referee for their comments, which have
improved the clarity of this paper. JPS and IRS acknowledge support from STFC (ST/I001573/1).
IRS also acknowledges support from the ERC Advanced Investigator programme DUSTYGAL
and a Royal Society/Wolfson Merit Award. DS acknowledges financial support from
NWO through a Veni fellowship and from FCT through the award of an FCT-IF starting
grant. PNB acknowledges STFC for financial support.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: John P.
full_name: Stott, John P.
last_name: Stott
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: A. M.
full_name: Swinbank, A. M.
last_name: Swinbank
- first_name: Ian
full_name: Smail, Ian
last_name: Smail
- first_name: Richard
full_name: Bower, Richard
last_name: Bower
- first_name: Philip N.
full_name: Best, Philip N.
last_name: Best
- first_name: Ray M.
full_name: Sharples, Ray M.
last_name: Sharples
- first_name: James E.
full_name: Geach, James E.
last_name: Geach
- 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: Stott JP, Sobral D, Swinbank AM, et al. A relationship between specific star
formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS.
Monthly Notices of the Royal Astronomical Society. 2014;443(3):2695-2704.
doi:10.1093/mnras/stu1343
apa: Stott, J. P., Sobral, D., Swinbank, A. M., Smail, I., Bower, R., Best, P. N.,
… Matthee, J. J. (2014). A relationship between specific star formation rate and
metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS. Monthly Notices
of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stu1343
chicago: Stott, John P., David Sobral, A. M. Swinbank, Ian Smail, Richard Bower,
Philip N. Best, Ray M. Sharples, James E. Geach, and Jorryt J Matthee. “A Relationship
between Specific Star Formation Rate and Metallicity Gradient within z ∼ 1 Galaxies
from KMOS-HiZELS.” Monthly Notices of the Royal Astronomical Society. Oxford
University Press, 2014. https://doi.org/10.1093/mnras/stu1343.
ieee: J. P. Stott et al., “A relationship between specific star formation
rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS,” Monthly
Notices of the Royal Astronomical Society, vol. 443, no. 3. Oxford University
Press, pp. 2695–2704, 2014.
ista: Stott JP, Sobral D, Swinbank AM, Smail I, Bower R, Best PN, Sharples RM, Geach
JE, Matthee JJ. 2014. A relationship between specific star formation rate and
metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS. Monthly Notices of
the Royal Astronomical Society. 443(3), 2695–2704.
mla: Stott, John P., et al. “A Relationship between Specific Star Formation Rate
and Metallicity Gradient within z ∼ 1 Galaxies from KMOS-HiZELS.” Monthly Notices
of the Royal Astronomical Society, vol. 443, no. 3, Oxford University Press,
2014, pp. 2695–704, doi:10.1093/mnras/stu1343.
short: J.P. Stott, D. Sobral, A.M. Swinbank, I. Smail, R. Bower, P.N. Best, R.M.
Sharples, J.E. Geach, J.J. Matthee, Monthly Notices of the Royal Astronomical
Society 443 (2014) 2695–2704.
date_created: 2022-07-14T12:16:10Z
date_published: 2014-09-21T00:00:00Z
date_updated: 2022-08-19T08:27:25Z
day: '21'
doi: 10.1093/mnras/stu1343
extern: '1'
external_id:
arxiv:
- '1407.1047'
fulldoi: https://doi.org/10.1093/mnras/stu1343
intvolume: ' 443'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: abundances'
- 'galaxies: evolution'
- 'galaxies: kinematics and dynamics'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1407.1047
month: '09'
oa: 1
oa_version: Preprint
page: 2695-2704
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
eissn:
- 1365-2966
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: A relationship between specific star formation rate and metallicity gradient
within z ∼ 1 galaxies from KMOS-HiZELS
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 443
year: '2014'
...