[{"year":"2026","article_number":"159","day":"10","date_created":"2026-07-12T22:02:17Z","volume":1005,"author":[{"last_name":"Lewis","first_name":"Zach","full_name":"Lewis, Zach"},{"first_name":"Michael V.","last_name":"Maseda","full_name":"Maseda, Michael V."},{"last_name":"De Graaff","first_name":"Anna","full_name":"De Graaff, Anna"},{"last_name":"Leja","first_name":"Joel","full_name":"Leja, Joel"},{"full_name":"Wang, Bingjie","last_name":"Wang","first_name":"Bingjie"},{"last_name":"Rix","first_name":"Hans Walter","full_name":"Rix, Hans Walter"},{"full_name":"Mcconachie, Ian","first_name":"Ian","last_name":"Mcconachie"},{"full_name":"Cleri, Nikko J.","first_name":"Nikko J.","last_name":"Cleri"},{"full_name":"Bezanson, Rachel","last_name":"Bezanson","first_name":"Rachel"},{"full_name":"Boogaard, Leindert A.","last_name":"Boogaard","first_name":"Leindert A."},{"full_name":"Brammer, Gabriel","last_name":"Brammer","first_name":"Gabriel"},{"first_name":"Jenny E.","last_name":"Greene","full_name":"Greene, Jenny E."},{"full_name":"Hirschmann, Michaela","last_name":"Hirschmann","first_name":"Michaela"},{"full_name":"Katz, Harley","first_name":"Harley","last_name":"Katz"},{"last_name":"Labbé","first_name":"Ivo","full_name":"Labbé, Ivo"},{"last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"last_name":"Miller","first_name":"Tim B.","full_name":"Miller, Tim B."},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."},{"last_name":"Oesch","first_name":"Pascal A.","full_name":"Oesch, Pascal A."},{"full_name":"Setton, David J.","last_name":"Setton","first_name":"David J."},{"full_name":"Suess, Katherine A.","first_name":"Katherine A.","last_name":"Suess"},{"full_name":"Weibel, Andrea","first_name":"Andrea","last_name":"Weibel"},{"first_name":"Katherine E.","last_name":"Whitaker","full_name":"Whitaker, Katherine E."},{"full_name":"Williams, Christina C.","last_name":"Williams","first_name":"Christina C."}],"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","quality_controlled":"1","month":"07","oa":1,"publication":"The Astrophysical Journal","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."}],"citation":{"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.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae7bfc\">https://doi.org/10.3847/1538-4357/ae7bfc</a>.","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).","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. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae7bfc\">https://doi.org/10.3847/1538-4357/ae7bfc</a>","ieee":"Z. Lewis <i>et al.</i>, “The mass–metallicity relation and its observational effects at z ∼ 3–6,” <i>The Astrophysical Journal</i>, 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.","ama":"Lewis Z, Maseda MV, De Graaff A, et al. The mass–metallicity relation and its observational effects at z ∼ 3–6. <i>The Astrophysical Journal</i>. 2026;1005(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae7bfc\">10.3847/1538-4357/ae7bfc</a>","mla":"Lewis, Zach, et al. “The Mass–Metallicity Relation and Its Observational Effects at z ∼ 3–6.” <i>The Astrophysical Journal</i>, vol. 1005, no. 2, 159, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae7bfc\">10.3847/1538-4357/ae7bfc</a>."},"tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"publisher":"IOP Publishing","das_tickbox":"1","has_accepted_license":"1","supplementarymaterial":"no","OA_place":"publisher","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"file_date_updated":"2026-07-13T07:35:16Z","external_id":{"arxiv":["2512.03134"]},"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 ","date_published":"2026-07-10T00:00:00Z","article_type":"original","keyword":["Galaxy evolution","Chemical enrichment","Metallicity","Galaxy abundances","Scaling relations"],"PlanS_conform":"1","oa_version":"Published Version","type":"journal_article","department":[{"_id":"JoMa"}],"title":"The mass–metallicity relation and its observational effects at z ∼ 3–6","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"DOAJ_listed":"1","researchdata_availability":"yes","scopus_import":"1","doi":"10.3847/1538-4357/ae7bfc","intvolume":"      1005","date_updated":"2026-07-13T07:40:41Z","issue":"2","publication_status":"published","status":"public","_id":"22264","file":[{"content_type":"application/pdf","date_created":"2026-07-13T07:35:16Z","success":1,"file_name":"2026_AstrophysicalJour_Lewis.pdf","checksum":"9b13fbbc5e5e921c04676ebc532d9c42","access_level":"open_access","date_updated":"2026-07-13T07:35:16Z","relation":"main_file","file_size":1854628,"creator":"dernst","file_id":"22273"}],"ddc":["520"],"OA_type":"gold","language":[{"iso":"eng"}],"article_processing_charge":"Yes"},{"page":"984-985","arxiv":1,"extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"Differences in galaxy colours are not just about the mass","article_type":"original","keyword":["Astronomy and Astrophysics","galaxies","formation - galaxies","evolution - galaxies","star formation - galaxies","abundances"],"type":"journal_article","oa_version":"Preprint","_id":"11585","article_processing_charge":"No","language":[{"iso":"eng"}],"date_updated":"2024-10-14T11:38:08Z","status":"public","publication_status":"published","doi":"10.1038/s41550-021-01415-y","scopus_import":"1","intvolume":"         5","oa":1,"quality_controlled":"1","author":[{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"month":"07","volume":5,"day":"05","year":"2021","date_created":"2022-07-14T13:13:39Z","date_published":"2021-07-05T00:00:00Z","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.","external_id":{"arxiv":["1802.06786"]},"publication_identifier":{"eissn":["2397-3366"]},"publisher":"Springer Nature","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."}],"citation":{"mla":"Matthee, Jorryt J. “Differences in Galaxy Colours Are Not Just about the Mass.” <i>Nature Astronomy</i>, vol. 5, Springer Nature, 2021, pp. 984–85, doi:<a href=\"https://doi.org/10.1038/s41550-021-01415-y\">10.1038/s41550-021-01415-y</a>.","ama":"Matthee JJ. Differences in galaxy colours are not just about the mass. <i>Nature Astronomy</i>. 2021;5:984-985. doi:<a href=\"https://doi.org/10.1038/s41550-021-01415-y\">10.1038/s41550-021-01415-y</a>","ista":"Matthee JJ. 2021. Differences in galaxy colours are not just about the mass. Nature Astronomy. 5, 984–985.","ieee":"J. J. Matthee, “Differences in galaxy colours are not just about the mass,” <i>Nature Astronomy</i>, vol. 5. Springer Nature, pp. 984–985, 2021.","apa":"Matthee, J. J. (2021). Differences in galaxy colours are not just about the mass. <i>Nature Astronomy</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41550-021-01415-y\">https://doi.org/10.1038/s41550-021-01415-y</a>","chicago":"Matthee, Jorryt J. “Differences in Galaxy Colours Are Not Just about the Mass.” <i>Nature Astronomy</i>. Springer Nature, 2021. <a href=\"https://doi.org/10.1038/s41550-021-01415-y\">https://doi.org/10.1038/s41550-021-01415-y</a>.","short":"J.J. Matthee, Nature Astronomy 5 (2021) 984–985."},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1802.06786"}],"publication":"Nature Astronomy"},{"oa":1,"month":"09","quality_controlled":"1","author":[{"full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"last_name":"Schaye","first_name":"Joop","full_name":"Schaye, Joop"}],"volume":479,"date_created":"2022-07-14T12:49:47Z","day":"01","year":"2018","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.","date_published":"2018-09-01T00:00:00Z","external_id":{"arxiv":["1802.06786"]},"publication_identifier":{"eissn":["1745-3933"],"issn":["1745-3925"]},"publisher":"Oxford University Press","citation":{"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.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnrasl/sly093\">https://doi.org/10.1093/mnrasl/sly093</a>.","short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society: Letters 479 (2018) L34–L39.","apa":"Matthee, J. J., &#38; Schaye, J. (2018). Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnrasl/sly093\">https://doi.org/10.1093/mnrasl/sly093</a>","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,” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, 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.","ama":"Matthee JJ, Schaye J. Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. 2018;479(1):L34-L39. doi:<a href=\"https://doi.org/10.1093/mnrasl/sly093\">10.1093/mnrasl/sly093</a>","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.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 479, no. 1, Oxford University Press, 2018, pp. L34–39, doi:<a href=\"https://doi.org/10.1093/mnrasl/sly093\">10.1093/mnrasl/sly093</a>."},"abstract":[{"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.","lang":"eng"}],"main_file_link":[{"url":"https://arxiv.org/abs/1802.06786","open_access":"1"}],"publication":"Monthly Notices of the Royal Astronomical Society: Letters","arxiv":1,"extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","page":"L34 - L39","title":"Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement","type":"journal_article","oa_version":"Preprint","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: abundances","galaxies: evolution","galaxies: formation","galaxies: star formation"],"article_type":"original","article_processing_charge":"No","language":[{"iso":"eng"}],"_id":"11584","status":"public","issue":"1","publication_status":"published","date_updated":"2024-10-14T11:37:53Z","intvolume":"       479","doi":"10.1093/mnrasl/sly093","scopus_import":"1"},{"volume":443,"day":"21","year":"2014","date_created":"2022-07-14T12:16:10Z","oa":1,"quality_controlled":"1","author":[{"full_name":"Stott, John P.","last_name":"Stott","first_name":"John P."},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"last_name":"Swinbank","first_name":"A. M.","full_name":"Swinbank, A. M."},{"last_name":"Smail","first_name":"Ian","full_name":"Smail, Ian"},{"first_name":"Richard","last_name":"Bower","full_name":"Bower, Richard"},{"full_name":"Best, Philip N.","last_name":"Best","first_name":"Philip N."},{"full_name":"Sharples, Ray M.","last_name":"Sharples","first_name":"Ray M."},{"full_name":"Geach, James E.","first_name":"James E.","last_name":"Geach"},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"}],"month":"09","abstract":[{"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.","lang":"eng"}],"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. <i>Monthly Notices of the Royal Astronomical Society</i>. 2014;443(3):2695-2704. doi:<a href=\"https://doi.org/10.1093/mnras/stu1343\">10.1093/mnras/stu1343</a>","mla":"Stott, John P., et al. “A Relationship between Specific Star Formation Rate and Metallicity Gradient within z ∼ 1 Galaxies from KMOS-HiZELS.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 443, no. 3, Oxford University Press, 2014, pp. 2695–704, doi:<a href=\"https://doi.org/10.1093/mnras/stu1343\">10.1093/mnras/stu1343</a>.","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.","ieee":"J. P. Stott <i>et al.</i>, “A relationship between specific star formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 443, no. 3. Oxford University Press, pp. 2695–2704, 2014.","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.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2014. <a href=\"https://doi.org/10.1093/mnras/stu1343\">https://doi.org/10.1093/mnras/stu1343</a>.","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.","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. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stu1343\">https://doi.org/10.1093/mnras/stu1343</a>"},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1407.1047"}],"publication":"Monthly Notices of the Royal Astronomical Society","external_id":{"arxiv":["1407.1047"]},"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.","date_published":"2014-09-21T00:00:00Z","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publisher":"Oxford University Press","title":"A relationship between specific star formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: abundances","galaxies: evolution","galaxies: kinematics and dynamics"],"article_type":"original","type":"journal_article","oa_version":"Preprint","page":"2695-2704","arxiv":1,"extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-19T08:27:25Z","status":"public","publication_status":"published","issue":"3","scopus_import":"1","doi":"10.1093/mnras/stu1343","intvolume":"       443","_id":"11582","article_processing_charge":"No","language":[{"iso":"eng"}]}]