[{"publication":"Astronomy & Astrophysics","date_updated":"2026-02-24T07:49:42Z","file_date_updated":"2026-02-24T07:46:47Z","scopus_import":"1","DOAJ_listed":"1","status":"public","PlanS_conform":"1","has_accepted_license":"1","citation":{"ieee":"G. Kotiwale <i>et al.</i>, “Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy,” <i>Astronomy &#38; Astrophysics</i>, vol. 706. EDP Sciences, 2026.","short":"G. Kotiwale, J.J. Matthee, D. Kashino, A.P. Vijayan, A. Torralba Torregrosa, C. Di Cesare, E. Iani, R. Bordoloi, J. Leja, M.V. Maseda, S. Tacchella, I. Shivaei, K.E. Heintz, A.L. Danhaive, S. Mascia, I. Kramarenko, B. Navarrete, R. Mackenzie, R.P. Naidu, D. Sobral, Astronomy &#38; Astrophysics 706 (2026).","mla":"Kotiwale, Gauri, et al. “Rapid, out-of-Equilibrium Metal Enrichment Indicated by a Flat Mass-Metallicity Relation at z ∼ 6 from NIRCam Grism Spectroscopy.” <i>Astronomy &#38; Astrophysics</i>, vol. 706, A165, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202556597\">10.1051/0004-6361/202556597</a>.","apa":"Kotiwale, G., Matthee, J. J., Kashino, D., Vijayan, A. P., Torralba Torregrosa, A., Di Cesare, C., … Sobral, D. (2026). Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202556597\">https://doi.org/10.1051/0004-6361/202556597</a>","ista":"Kotiwale G, Matthee JJ, Kashino D, Vijayan AP, Torralba Torregrosa A, Di Cesare C, Iani E, Bordoloi R, Leja J, Maseda MV, Tacchella S, Shivaei I, Heintz KE, Danhaive AL, Mascia S, Kramarenko I, Navarrete B, Mackenzie R, Naidu RP, Sobral D. 2026. Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy. Astronomy &#38; Astrophysics. 706, A165.","ama":"Kotiwale G, Matthee JJ, Kashino D, et al. Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy. <i>Astronomy &#38; Astrophysics</i>. 2026;706. doi:<a href=\"https://doi.org/10.1051/0004-6361/202556597\">10.1051/0004-6361/202556597</a>","chicago":"Kotiwale, Gauri, Jorryt J Matthee, Daichi Kashino, Aswin P. Vijayan, Alberto Torralba Torregrosa, Claudia Di Cesare, Edoardo Iani, et al. “Rapid, out-of-Equilibrium Metal Enrichment Indicated by a Flat Mass-Metallicity Relation at z ∼ 6 from NIRCam Grism Spectroscopy.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202556597\">https://doi.org/10.1051/0004-6361/202556597</a>."},"day":"01","type":"journal_article","quality_controlled":"1","language":[{"iso":"eng"}],"_id":"21341","abstract":[{"lang":"eng","text":"We aim to characterise the mass-metallicity relation (MZR) and the 3D correlation between the stellar mass, metallicity, and star formation rate (SFR) known as the fundamental metallicity relation (FMR) for galaxies at 5 < z < 7. Using ∼800 [O III] selected galaxies from deep NIRCam grism surveys, we present our stacked measurements of direct-Te metallicities, which we used to test recent strong-line metallicity calibrations. Our measured direct-Te metallicities (0.1–0.2 Z⊙ for M★ ≈ 5 × 107 − 9 M⊙, respectively) match recent JWST/NIRSpec-based results. However, there are significant inconsistencies between observations and hydrodynamical simulations. We observe a flatter MZR slope than the SPHINX20 and FLARES simulations, which cannot be attributed to selection effects. With simple models, we show that the effect of an [O III] flux-limited sample on the observed shape of the MZR is strongly dependent on the FMR. If the FMR is similar to the one in the local Universe, the intrinsic high-redshift MZR should be even flatter than is observed. In turn, a 3D relation where SFR correlates positively with metallicity at fixed mass would imply an intrinsically steeper MZR. Our measurements indicate that metallicity variations at fixed mass show little dependence on the SFR, suggesting a flat intrinsic MZR. This could indicate that the low-mass galaxies at these redshifts are out of equilibrium and that metal enrichment occurs rapidly in low-mass galaxies. However, being limited by our stacking analysis, we are yet to probe the scatter in the MZR and its dependence on SFR. Large carefully selected samples of galaxies with robust metallicity measurements can put tight constraints on the high-redshift FMR and help us to understand the interplay between gas flows, star formation, and feedback in early galaxies."}],"external_id":{"arxiv":["2510.19959"]},"date_published":"2026-02-01T00:00:00Z","OA_place":"publisher","year":"2026","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","ddc":["520"],"intvolume":"       706","article_number":"A165","article_type":"original","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224"}],"month":"02","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"volume":706,"author":[{"id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","first_name":"Gauri","full_name":"Kotiwale, Gauri","last_name":"Kotiwale"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"last_name":"Kashino","full_name":"Kashino, Daichi","first_name":"Daichi"},{"first_name":"Aswin P.","last_name":"Vijayan","full_name":"Vijayan, Aswin P."},{"first_name":"Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","orcid":"0000-0001-5586-6950","last_name":"Torralba Torregrosa","full_name":"Torralba Torregrosa, Alberto"},{"id":"2d002343-372f-11ef-98ec-a164d20427cb","first_name":"Claudia","last_name":"Di Cesare","full_name":"Di Cesare, Claudia"},{"last_name":"Iani","full_name":"Iani, Edoardo","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","first_name":"Edoardo","orcid":"0000-0001-8386-3546"},{"first_name":"Rongmon","last_name":"Bordoloi","full_name":"Bordoloi, Rongmon"},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"first_name":"Michael V.","full_name":"Maseda, Michael V.","last_name":"Maseda"},{"first_name":"Sandro","full_name":"Tacchella, Sandro","last_name":"Tacchella"},{"first_name":"Irene","full_name":"Shivaei, Irene","last_name":"Shivaei"},{"full_name":"Heintz, Kasper E.","last_name":"Heintz","first_name":"Kasper E."},{"last_name":"Danhaive","full_name":"Danhaive, A. Lola","first_name":"A. Lola"},{"first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","full_name":"Mascia, Sara","last_name":"Mascia"},{"last_name":"Kramarenko","full_name":"Kramarenko, Ivan","orcid":"0000-0001-5346-6048","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan"},{"id":"aa14a535-50c9-11ef-b52e-e0c373d10148","first_name":"Benjamín","full_name":"Navarrete, Benjamín","last_name":"Navarrete"},{"full_name":"Mackenzie, Ruari","last_name":"Mackenzie","first_name":"Ruari"},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"}],"acknowledgement":"We thank the anonymous referee for the insightful comments that helped improving this paper. 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 Associations of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations were taken under programmes # 1243, # 1933 and # 3516. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. GK acknowledges support from the Foundation MERAC. APV acknowledge support from the Sussex Astronomy Centre STFC Consolidated Grant (ST/X001040/1).","doi":"10.1051/0004-6361/202556597","oa":1,"publisher":"EDP Sciences","tmp":{"short":"CC BY (4.0)","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)"},"corr_author":"1","article_processing_charge":"No","file":[{"file_name":"2026_AstronomyAstrophysics_Kotiwale.pdf","checksum":"6f5849d29ad43bee32f90152f6fc0294","file_id":"21355","creator":"dernst","date_updated":"2026-02-24T07:46:47Z","relation":"main_file","access_level":"open_access","date_created":"2026-02-24T07:46:47Z","file_size":6531719,"success":1,"content_type":"application/pdf"}],"publication_status":"published","oa_version":"Published Version","OA_type":"diamond","date_created":"2026-02-22T23:01:35Z","title":"Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy","arxiv":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]}},{"doi":"10.1051/0004-6361/202557537","oa":1,"acknowledgement":"We thank the scientific referee for useful and constructive comments. We thank Ylva Götberg and Zoltan Haiman for insightful discussions about the physics of gaseous envelopes and accretion into black holes. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. This work is based in part 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 #5664. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349.","author":[{"orcid":"0000-0001-5586-6950","first_name":"Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","full_name":"Torralba Torregrosa, Alberto","last_name":"Torralba Torregrosa"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"full_name":"Pezzulli, Gabriele","last_name":"Pezzulli","first_name":"Gabriele"},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"first_name":"Yuzo","full_name":"Ishikawa, Yuzo","last_name":"Ishikawa"},{"first_name":"Gabriel B.","full_name":"Brammer, Gabriel B.","last_name":"Brammer"},{"first_name":"Seok Jun","last_name":"Chang","full_name":"Chang, Seok Jun"},{"first_name":"John","full_name":"Chisholm, John","last_name":"Chisholm"},{"first_name":"Anna","last_name":"De Graaff","full_name":"De Graaff, Anna"},{"first_name":"Francesco","full_name":"D’Eugenio, Francesco","last_name":"D’Eugenio"},{"first_name":"Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","last_name":"Di Cesare","full_name":"Di Cesare, Claudia"},{"first_name":"Anna Christina","full_name":"Eilers, Anna Christina","last_name":"Eilers"},{"first_name":"Jenny E.","last_name":"Greene","full_name":"Greene, Jenny E."},{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"full_name":"Iani, Edoardo","last_name":"Iani","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","first_name":"Edoardo","orcid":"0000-0001-8386-3546"},{"last_name":"Kokorev","full_name":"Kokorev, Vasily","first_name":"Vasily"},{"last_name":"Kotiwale","full_name":"Kotiwale, Gauri","first_name":"Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875"},{"last_name":"Kramarenko","full_name":"Kramarenko, Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan","orcid":"0000-0001-5346-6048"},{"first_name":"Yilun","last_name":"Ma","full_name":"Ma, Yilun"},{"full_name":"Mascia, Sara","last_name":"Mascia","first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29"},{"full_name":"Navarrete, Benjamín","last_name":"Navarrete","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","first_name":"Benjamín"},{"full_name":"Nelson, Erica","last_name":"Nelson","first_name":"Erica"},{"first_name":"Pascal","full_name":"Oesch, Pascal","last_name":"Oesch"},{"first_name":"Robert A.","full_name":"Simcoe, Robert A.","last_name":"Simcoe"},{"last_name":"Wuyts","full_name":"Wuyts, Stijn","first_name":"Stijn"}],"volume":707,"department":[{"_id":"JoMa"}],"month":"03","article_type":"original","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"article_processing_charge":"No","corr_author":"1","tmp":{"short":"CC BY (4.0)","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)"},"publisher":"EDP Sciences","publication_status":"published","file":[{"access_level":"open_access","date_created":"2026-03-16T10:57:49Z","file_size":2510157,"success":1,"content_type":"application/pdf","file_name":"2026_AstronomyAstrophysics_Torralba2.pdf","checksum":"fcab9cb3dcf1d68612e1fdc8191643c1","date_updated":"2026-03-16T10:57:49Z","relation":"main_file","file_id":"21460","creator":"dernst"}],"arxiv":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"title":"The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings","date_created":"2026-03-15T23:01:36Z","OA_type":"diamond","oa_version":"Published Version","file_date_updated":"2026-03-16T10:57:49Z","publication":"Astronomy & Astrophysics","date_updated":"2026-03-16T10:59:16Z","PlanS_conform":"1","status":"public","DOAJ_listed":"1","scopus_import":"1","external_id":{"arxiv":["2510.00103"]},"abstract":[{"text":"The population of the little red dots (LRDs) may represent a key phase of supermassive black hole (SMBH) growth. A cocoon of dense excited gas is emerging as a key component to explain the most striking properties of LRDs, such as strong Balmer breaks and Balmer absorption, as well as the weak IR emission. To dissect the structure of LRDs, we analyzed new deep JWST/NIRSpec PRISM and G395H spectra of FRESCO-GN-9771, one of the most luminous known LRDs at z = 5.5. These spectra reveal a strong Balmer break, broad Balmer lines, and very narrow [O III] emission. We revealed a forest of optical [Fe II] lines, which we argue are emerging from a dense (nH = 109 − 10 cm−3) warm layer with electron temperature Te ≈ 7000 K. The broad wings of Hα and Hβ have an exponential profile due to electron scattering in this same layer. The high Hα : Hβ : Hγ flux ratio of ≈10.4 : 1 : 0.14 is an indicator of collisional excitation and resonant scattering dominating the Balmer line emission. A narrow Hγ component, unseen in the other two Balmer lines due to outshining by the broad components, could trace the ISM of a normal host galaxy with a star formation rate of ∼5 M⊙ yr−1. The warm layer is mostly opaque to Balmer transitions, producing a characteristic P Cygni profile in the line centers suggesting outflowing motions. This same layer is responsible for shaping the Balmer break. The broadband spectrum can be reasonably matched by a simple photoionized slab model that dominates the λ > 1500 Å continuum and a low-mass (∼108 M⊙) galaxy that could explain the narrow [O III], with only a subdominant contribution to the UV continuum. Our findings indicate that Balmer lines are not directly tracing the gas kinematics near the SMBH and that the BH mass scale is likely much lower than virial indicators suggest.","lang":"eng"}],"_id":"21451","language":[{"iso":"eng"}],"quality_controlled":"1","type":"journal_article","day":"01","citation":{"apa":"Torralba Torregrosa, A., Matthee, J. J., Pezzulli, G., Naidu, R. P., Ishikawa, Y., Brammer, G. B., … Wuyts, S. (2026). The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202557537\">https://doi.org/10.1051/0004-6361/202557537</a>","mla":"Torralba Torregrosa, Alberto, et al. “The Warm Outer Layer of a Little Red Dot as the Source of [Fe Ii] and Collisional Balmer Lines with Scattering Wings.” <i>Astronomy &#38; Astrophysics</i>, vol. 707, A75, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557537\">10.1051/0004-6361/202557537</a>.","ieee":"A. Torralba Torregrosa <i>et al.</i>, “The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings,” <i>Astronomy &#38; Astrophysics</i>, vol. 707. EDP Sciences, 2026.","short":"A. Torralba Torregrosa, J.J. Matthee, G. Pezzulli, R.P. Naidu, Y. Ishikawa, G.B. Brammer, S.J. Chang, J. Chisholm, A. De Graaff, F. D’Eugenio, C. Di Cesare, A.C. Eilers, J.E. Greene, M. Gronke, E. Iani, V. Kokorev, G. Kotiwale, I. Kramarenko, Y. Ma, S. Mascia, B. Navarrete, E. Nelson, P. Oesch, R.A. Simcoe, S. Wuyts, Astronomy &#38; Astrophysics 707 (2026).","chicago":"Torralba Torregrosa, Alberto, Jorryt J Matthee, Gabriele Pezzulli, Rohan P. Naidu, Yuzo Ishikawa, Gabriel B. Brammer, Seok Jun Chang, et al. “The Warm Outer Layer of a Little Red Dot as the Source of [Fe Ii] and Collisional Balmer Lines with Scattering Wings.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202557537\">https://doi.org/10.1051/0004-6361/202557537</a>.","ama":"Torralba Torregrosa A, Matthee JJ, Pezzulli G, et al. The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings. <i>Astronomy &#38; Astrophysics</i>. 2026;707. doi:<a href=\"https://doi.org/10.1051/0004-6361/202557537\">10.1051/0004-6361/202557537</a>","ista":"Torralba Torregrosa A, Matthee JJ, Pezzulli G, Naidu RP, Ishikawa Y, Brammer GB, Chang SJ, Chisholm J, De Graaff A, D’Eugenio F, Di Cesare C, Eilers AC, Greene JE, Gronke M, Iani E, Kokorev V, Kotiwale G, Kramarenko I, Ma Y, Mascia S, Navarrete B, Nelson E, Oesch P, Simcoe RA, Wuyts S. 2026. The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings. Astronomy &#38; Astrophysics. 707, A75."},"has_accepted_license":"1","article_number":"A75","intvolume":"       707","ddc":["520"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","year":"2026","OA_place":"publisher","date_published":"2026-03-01T00:00:00Z"},{"publisher":"EDP Sciences","tmp":{"short":"CC BY (4.0)","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)"},"corr_author":"1","article_processing_charge":"No","acknowledgement":"We thank the anonymous referee for the insightful comments that helped improving the manuscript. We thank Romain. A. Meyer for valuable discussion, Pierluigi Rinaldi for his help with data handling and Luca Graziani and William McClymont for providing the dustyGadget and\r\nTHESAN-ZOOM data, respectively. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. 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 # 3516. We acknowledge funding from JWST program GO-3516. Software used in developing this work includes: matplotlib (Hunter 2007), numpy (Oliphant 2007), scipy (Virtanen et al. 2020), TOPCAT (Taylor 2005), and Astropy (Astropy Collaboration 2013).","doi":"10.1051/0004-6361/202557790","oa":1,"article_type":"original","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"department":[{"_id":"JoMa"},{"_id":"GradSch"}],"month":"03","author":[{"first_name":"Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","full_name":"Di Cesare, Claudia","last_name":"Di Cesare"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."},{"last_name":"Torralba","full_name":"Torralba, Alberto","first_name":"Alberto"},{"full_name":"Kotiwale, Gauri","last_name":"Kotiwale","first_name":"Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875"},{"orcid":"0000-0001-5346-6048","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan","last_name":"Kramarenko","full_name":"Kramarenko, Ivan"},{"full_name":"Blaizot, Jeremy","last_name":"Blaizot","first_name":"Jeremy"},{"full_name":"Rosdahl, Joakim","last_name":"Rosdahl","first_name":"Joakim"},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"last_name":"Iani","full_name":"Iani, Edoardo","orcid":"0000-0001-8386-3546","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","first_name":"Edoardo"},{"first_name":"Angela","last_name":"Adamo","full_name":"Adamo, Angela"},{"full_name":"Covelo-Paz, Alba","last_name":"Covelo-Paz","first_name":"Alba"},{"first_name":"Lukas J.","full_name":"Furtak, Lukas J.","last_name":"Furtak"},{"full_name":"Heintz, Kasper E.","last_name":"Heintz","first_name":"Kasper E."},{"full_name":"Mascia, Sara","last_name":"Mascia","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","first_name":"Sara"},{"last_name":"Navarrete","full_name":"Navarrete, Benjamín","first_name":"Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148"},{"full_name":"Oesch, Pascal A.","last_name":"Oesch","first_name":"Pascal A."},{"first_name":"Michael","last_name":"Romano","full_name":"Romano, Michael"},{"first_name":"Irene","full_name":"Shivaei, Irene","last_name":"Shivaei"},{"first_name":"Sandro","last_name":"Tacchella","full_name":"Tacchella, Sandro"}],"volume":707,"arxiv":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"oa_version":"Published Version","OA_type":"diamond","title":"The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations","date_created":"2026-03-15T23:01:36Z","publication_status":"published","file":[{"access_level":"open_access","content_type":"application/pdf","success":1,"date_created":"2026-03-16T10:48:07Z","file_size":1821411,"checksum":"c056b00ce7324849754521fde10fb7ca","file_name":"2026_AstronomyAstrophysics_DiCesare.pdf","relation":"main_file","file_id":"21459","date_updated":"2026-03-16T10:48:07Z","creator":"dernst"}],"status":"public","PlanS_conform":"1","scopus_import":"1","DOAJ_listed":"1","file_date_updated":"2026-03-16T10:48:07Z","date_updated":"2026-03-16T10:52:44Z","publication":"Astronomy & Astrophysics","year":"2026","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","ddc":["520"],"article_number":"A129","intvolume":"       707","date_published":"2026-03-01T00:00:00Z","OA_place":"publisher","type":"journal_article","quality_controlled":"1","_id":"21452","abstract":[{"text":"Galaxies exhibit a tight correlation between their star formation rate (SFR) and stellar mass over a wide redshift range known as the star-forming main sequence (SFMS). With JWST, the SFMS can now be investigated at high redshifts down to masses of ∼106 M⊙, using sensitive star formation rate tracers such as the Hα emission, which allow us to probe the variability in the star formation histories. We present inferences of the SFMS based on 316 Hα-selected galaxies at z ∼ 4 − 5 with log(M★/M⊙) = 6.4 − 10.6. These galaxies were identified behind the Abell 2744 lensing cluster with NIRCam grism spectroscopy from the survey All the Little Things (ALT). At face value, our data suggest a shallow slope in the SFMS (SFR ∝ M★α, with α = 0.45). After we corrected this for the Hα-flux limited nature of our survey using a Bayesian framework, the slope steepened to α = 0.59+0.10−0.09, whereas current data on their own are inconclusive on the mass dependence of the scatter. These slopes differ significantly from the slope of ∼1 that is expected from the observed evolution of the galaxy stellar mass function and from simulations. When we fixed the slope to α = 1, we found evidence for a decreasing intrinsic scatter with stellar mass (from ∼0.5 dex at M★ = 108 M⊙ to 0.4 dex at M★ = 1010 M⊙). This difference might be explained by a (combination of) luminosity-dependent SFR(Hα) calibration, a population of (mini)-quenched low-mass galaxies, or underestimated dust attenuation in high-mass galaxies. Future deep observations with different facilities can quantify these processes, which will enable us to achieve better insights into the variability of the star formation histories.","lang":"eng"}],"language":[{"iso":"eng"}],"external_id":{"arxiv":["2510.19044"]},"has_accepted_license":"1","day":"01","citation":{"apa":"Di Cesare, C., Matthee, J. J., Naidu, R. P., Torralba, A., Kotiwale, G., Kramarenko, I., … Tacchella, S. (2026). The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202557790\">https://doi.org/10.1051/0004-6361/202557790</a>","mla":"Di Cesare, Claudia, et al. “The Slope and Scatter of the Star-Forming Main Sequence at z ∼ 5: Reconciling Observations with Simulations.” <i>Astronomy &#38; Astrophysics</i>, vol. 707, A129, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557790\">10.1051/0004-6361/202557790</a>.","ieee":"C. Di Cesare <i>et al.</i>, “The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations,” <i>Astronomy &#38; Astrophysics</i>, vol. 707. EDP Sciences, 2026.","short":"C. Di Cesare, J.J. Matthee, R.P. Naidu, A. Torralba, G. Kotiwale, I. Kramarenko, J. Blaizot, J. Rosdahl, J. Leja, E. Iani, A. Adamo, A. Covelo-Paz, L.J. Furtak, K.E. Heintz, S. Mascia, B. Navarrete, P.A. Oesch, M. Romano, I. Shivaei, S. Tacchella, Astronomy &#38; Astrophysics 707 (2026).","chicago":"Di Cesare, Claudia, Jorryt J Matthee, Rohan P. Naidu, Alberto Torralba, Gauri Kotiwale, Ivan Kramarenko, Jeremy Blaizot, et al. “The Slope and Scatter of the Star-Forming Main Sequence at z ∼ 5: Reconciling Observations with Simulations.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202557790\">https://doi.org/10.1051/0004-6361/202557790</a>.","ama":"Di Cesare C, Matthee JJ, Naidu RP, et al. The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations. <i>Astronomy &#38; Astrophysics</i>. 2026;707. doi:<a href=\"https://doi.org/10.1051/0004-6361/202557790\">10.1051/0004-6361/202557790</a>","ista":"Di Cesare C, Matthee JJ, Naidu RP, Torralba A, Kotiwale G, Kramarenko I, Blaizot J, Rosdahl J, Leja J, Iani E, Adamo A, Covelo-Paz A, Furtak LJ, Heintz KE, Mascia S, Navarrete B, Oesch PA, Romano M, Shivaei I, Tacchella S. 2026. The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations. Astronomy &#38; Astrophysics. 707, A129."}},{"publication":"Astronomy & Astrophysics","date_updated":"2026-03-23T15:46:31Z","file_date_updated":"2026-03-23T15:44:09Z","DOAJ_listed":"1","status":"public","PlanS_conform":"1","has_accepted_license":"1","citation":{"chicago":"Kramarenko, Ivan, J. Rosdahl, J. Blaizot, Jorryt J Matthee, H. Katz, and Claudia Di Cesare. “H α as a Tracer of Star Formation in the SPHINX Cosmological Simulations.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202557114\">https://doi.org/10.1051/0004-6361/202557114</a>.","ama":"Kramarenko I, Rosdahl J, Blaizot J, Matthee JJ, Katz H, Di Cesare C. H α as a tracer of star formation in the SPHINX cosmological simulations. <i>Astronomy &#38; Astrophysics</i>. 2026;707. doi:<a href=\"https://doi.org/10.1051/0004-6361/202557114\">10.1051/0004-6361/202557114</a>","ista":"Kramarenko I, Rosdahl J, Blaizot J, Matthee JJ, Katz H, Di Cesare C. 2026. H α as a tracer of star formation in the SPHINX cosmological simulations. Astronomy &#38; Astrophysics. 707, A184.","apa":"Kramarenko, I., Rosdahl, J., Blaizot, J., Matthee, J. J., Katz, H., &#38; Di Cesare, C. (2026). H α as a tracer of star formation in the SPHINX cosmological simulations. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202557114\">https://doi.org/10.1051/0004-6361/202557114</a>","mla":"Kramarenko, Ivan, et al. “H α as a Tracer of Star Formation in the SPHINX Cosmological Simulations.” <i>Astronomy &#38; Astrophysics</i>, vol. 707, A184, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557114\">10.1051/0004-6361/202557114</a>.","ieee":"I. Kramarenko, J. Rosdahl, J. Blaizot, J. J. Matthee, H. Katz, and C. Di Cesare, “H α as a tracer of star formation in the SPHINX cosmological simulations,” <i>Astronomy &#38; Astrophysics</i>, vol. 707. EDP Sciences, 2026.","short":"I. Kramarenko, J. Rosdahl, J. Blaizot, J.J. Matthee, H. Katz, C. Di Cesare, Astronomy &#38; Astrophysics 707 (2026)."},"day":"05","type":"journal_article","quality_controlled":"1","_id":"21481","abstract":[{"lang":"eng","text":"The Hα emission line in galaxies is a powerful tracer of their recent star formation activity. With the advent of JWST, we are now able to routinely observe Hα in galaxies at high redshift (z ≳ 3) and thus measure their star formation rates (SFRs). However, using classical SFR(Hα) calibrations to derive the SFRs leads to biased results because high-redshift galaxies are commonly characterized by low metallicities and bursty star formation histories, affecting the conversion factor between the Hα luminosity (LHα) and the SFR. We developed a set of new SFR(Hα) calibrations that allowed us to predict the SFRs of Hα-emitters at z ≳ 3 with very little error. We used the SPHINX cosmological simulations to select a sample of star-forming galaxies representative of the Hα-emitter population observed with JWST. We then derived linear corrections to the classical SFR(Hα) calibrations that took variations in the physical properties (e.g., stellar metallicities) among individual galaxies into account. We obtained two new SFR(Hα) calibrations that compared to the classical calibrations reduce the root mean squared error (RMSE) in the predicted SFRs by ΔRMSE ≈ 0.04 dex and ΔRMSE ≈ 0.06 dex, respectively. Using the recent JWST NIRCam/grism observations of Hα-emitters at z ∼ 6, we show that the new calibrations affect the high-redshift galaxy population statistics: (i) the estimated cosmic SFR density decreases by ΔρSFR ≈ 12%, and (ii) the observed slope of the star formation main sequence increases by Δ∂logSFR/∂logM★ = 0.08 ± 0.02."}],"language":[{"iso":"eng"}],"external_id":{"arxiv":["2509.05403"]},"date_published":"2026-03-05T00:00:00Z","OA_place":"publisher","year":"2026","ddc":["520"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"A184","intvolume":"       707","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"article_type":"original","department":[{"_id":"JoMa"}],"month":"03","author":[{"last_name":"Kramarenko","full_name":"Kramarenko, Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan","orcid":"0000-0001-5346-6048"},{"first_name":"J.","last_name":"Rosdahl","full_name":"Rosdahl, J."},{"first_name":"J.","full_name":"Blaizot, J.","last_name":"Blaizot"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"full_name":"Katz, H.","last_name":"Katz","first_name":"H."},{"id":"2d002343-372f-11ef-98ec-a164d20427cb","first_name":"Claudia","last_name":"Di Cesare","full_name":"Di Cesare, Claudia"}],"volume":707,"acknowledgement":"We thank the anonymous referee for the insightful comments that helped improve the manuscript. We also thank Thibault Garel, Pascal Oesch, Irene Shivaei, Charlotte Simmonds, Andrew Hopkins, Daniel Schaerer, and Rashmi Gottumukkala for useful comments and productive discussions. We gratefully acknowledge support from the CBPsmn (PSMN, Pôle Scientifique de Modélisation Numérique) of the ENS de Lyon for the computing resources.\r\nFunded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. This work made extensive use of several open-source software packages, and we gratefully acknowledge the efforts of their authors: numpy (Harris et al. 2020), astropy (Astropy Collaboration 2022), matplotlib (Hunter 2007), ipython (Perez & Granger 2007), and scikit-learn (Pedregosa et al. 2011).","doi":"10.1051/0004-6361/202557114","oa":1,"publisher":"EDP Sciences","corr_author":"1","tmp":{"short":"CC BY (4.0)","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)"},"article_processing_charge":"No","file":[{"success":1,"content_type":"application/pdf","file_size":904565,"date_created":"2026-03-23T15:44:09Z","access_level":"open_access","creator":"dernst","file_id":"21492","date_updated":"2026-03-23T15:44:09Z","relation":"main_file","checksum":"7429076b381dd498084f40ffd199e714","file_name":"2026_AstronomyAstrophysics_Kramarenko.pdf"}],"publication_status":"published","oa_version":"Published Version","OA_type":"diamond","title":"H α as a tracer of star formation in the SPHINX cosmological simulations","date_created":"2026-03-23T14:58:03Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"arxiv":1},{"arxiv":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"date_created":"2025-02-23T23:01:55Z","title":"Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744","oa_version":"Published Version","OA_type":"gold","publication_status":"published","file":[{"creator":"dernst","relation":"main_file","date_updated":"2025-02-25T06:38:43Z","file_id":"19084","file_name":"2025_MonthlyNoticesRAS_Claeyssens.pdf","checksum":"431aef05755e6b5472f5e9b4c326cf84","date_created":"2025-02-25T06:38:43Z","file_size":35099276,"success":1,"content_type":"application/pdf","access_level":"open_access"}],"tmp":{"short":"CC BY (4.0)","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)"},"article_processing_charge":"No","publisher":"Oxford University Press","acknowledgement":"The authors thank the International Space Science Institute for sponsoring the ISSI team: ‘Star Formation within rapidly evolving galaxies’ where many ideas discussed in this article have been brainstormed. AA and AC acknowledge support by the Swedish research council Vetenskapsrådet (2021-05559). MM acknowledges the financial support through grant PRIN-MIUR 2020SKSTHZ. JM and IK acknowledge support by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. RPN acknowledges funding from JWST programme GO-3516. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.","doi":"10.1093/mnras/staf058","oa":1,"author":[{"first_name":"Adélaïde","last_name":"Claeyssens","full_name":"Claeyssens, Adélaïde"},{"full_name":"Adamo, Angela","last_name":"Adamo","first_name":"Angela"},{"first_name":"Matteo","last_name":"Messa","full_name":"Messa, Matteo"},{"first_name":"Miroslava","last_name":"Dessauges-Zavadsky","full_name":"Dessauges-Zavadsky, Miroslava"},{"full_name":"Richard, Johan","last_name":"Richard","first_name":"Johan"},{"full_name":"Kramarenko, Ivan","last_name":"Kramarenko","orcid":"0000-0001-5346-6048","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."}],"volume":537,"project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224"}],"article_type":"original","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"month":"03","intvolume":"       537","year":"2025","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","ddc":["520"],"date_published":"2025-03-01T00:00:00Z","OA_place":"publisher","_id":"19066","language":[{"iso":"eng"}],"abstract":[{"lang":"eng","text":"We present a sample of 1956 individual stellar clumps at redshift 0.7 < z < 10, detected with JWST/NIRCam in 476 galaxies lensed by the galaxy cluster Abell2744. The lensed clumps present magnifications ranging between μ = 1.8 and μ = 300. We perform simultaneous size-photometry estimates in 20 JWST/NIRCam median and broad-band filters from 0.7 to 5 μm.\r\nSpectral energy distribution (SED) fitting analyses enable us to recover the physical properties of the clumps. The majority of the clumps are spatially resolved and have effective radii in the range Reff = 10–700 pc. We restrict this first study to the 1751 post-reionization era clumps with redshift < 5.5. We find a significant evolution of the average clump ages, star formation rates (SFRs), SFR surface densities, and metallicity with increasing redshift, while median stellar mass and stellar mass surface densities are similar in the probed redshift range. We observe a strong correlation between the clump properties and the properties of their host galaxies, with more massive galaxies hosting more massive and older clumps. We find that clumps closer to their host galactic centre are on average more massive, while their ages do not show clear sign of migration. We find that clumps at cosmic noon sample the upper-mass end of the mass function to higher masses than at z > 3, reflecting the rapid increase towards the peak of the cosmic star formation history. We conclude that the results achieved over the studied redshift range are in agreement with expectation of in situ clump formation scenario from large-scale disc fragmentation. "}],"external_id":{"arxiv":["2410.10974"],"isi":["001420026000001"]},"type":"journal_article","quality_controlled":"1","has_accepted_license":"1","day":"01","citation":{"mla":"Claeyssens, Adélaïde, et al. “Tracing Star Formation across Cosmic Time at Tens of Parsec-Scales in the Lensing Cluster Field Abell 2744.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 3, Oxford University Press, 2025, pp. 2535–58, doi:<a href=\"https://doi.org/10.1093/mnras/staf058\">10.1093/mnras/staf058</a>.","short":"A. Claeyssens, A. Adamo, M. Messa, M. Dessauges-Zavadsky, J. Richard, I. Kramarenko, J.J. Matthee, R.P. Naidu, Monthly Notices of the Royal Astronomical Society 537 (2025) 2535–2558.","ieee":"A. Claeyssens <i>et al.</i>, “Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 3. Oxford University Press, pp. 2535–2558, 2025.","apa":"Claeyssens, A., Adamo, A., Messa, M., Dessauges-Zavadsky, M., Richard, J., Kramarenko, I., … Naidu, R. P. (2025). Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf058\">https://doi.org/10.1093/mnras/staf058</a>","ama":"Claeyssens A, Adamo A, Messa M, et al. Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;537(3):2535-2558. doi:<a href=\"https://doi.org/10.1093/mnras/staf058\">10.1093/mnras/staf058</a>","ista":"Claeyssens A, Adamo A, Messa M, Dessauges-Zavadsky M, Richard J, Kramarenko I, Matthee JJ, Naidu RP. 2025. Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744. Monthly Notices of the Royal Astronomical Society. 537(3), 2535–2558.","chicago":"Claeyssens, Adélaïde, Angela Adamo, Matteo Messa, Miroslava Dessauges-Zavadsky, Johan Richard, Ivan Kramarenko, Jorryt J Matthee, and Rohan P. Naidu. “Tracing Star Formation across Cosmic Time at Tens of Parsec-Scales in the Lensing Cluster Field Abell 2744.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf058\">https://doi.org/10.1093/mnras/staf058</a>."},"page":"2535-2558","status":"public","DOAJ_listed":"1","issue":"3","scopus_import":"1","file_date_updated":"2025-02-25T06:38:43Z","publication":"Monthly Notices of the Royal Astronomical Society","date_updated":"2026-02-16T11:51:48Z","isi":1},{"isi":1,"date_updated":"2026-02-16T12:08:59Z","publication":"Astronomy & Astrophysics","file_date_updated":"2025-03-04T09:29:01Z","scopus_import":"1","status":"public","has_accepted_license":"1","citation":{"chicago":"Covelo-Paz, Alba, Emma Giovinazzo, Pascal A. Oesch, Romain A. Meyer, Andrea Weibel, Gabriel Brammer, Yoshinobu Fudamoto, et al. “An Hα View of Galaxy Buildup in the First 2 Gyr: Luminosity Functions at z ∼ 4−6.5 from NIRCam/Grism Spectroscopy.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202452363\">https://doi.org/10.1051/0004-6361/202452363</a>.","ama":"Covelo-Paz A, Giovinazzo E, Oesch PA, et al. An Hα view of galaxy buildup in the first 2 Gyr: Luminosity functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy. <i>Astronomy &#38; Astrophysics</i>. 2025;694. doi:<a href=\"https://doi.org/10.1051/0004-6361/202452363\">10.1051/0004-6361/202452363</a>","ista":"Covelo-Paz A, Giovinazzo E, Oesch PA, Meyer RA, Weibel A, Brammer G, Fudamoto Y, Kerutt J, Lin J, Matharu J, Naidu RP, Velichko A, Bollo V, Bouwens R, Chisholm J, Illingworth GD, Kramarenko I, Magee D, Maseda M, Matthee JJ, Nelson E, Reddy N, Schaerer D, Stefanon M, Xiao M. 2025. An Hα view of galaxy buildup in the first 2 Gyr: Luminosity functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy. Astronomy &#38; Astrophysics. 694, A178.","apa":"Covelo-Paz, A., Giovinazzo, E., Oesch, P. A., Meyer, R. A., Weibel, A., Brammer, G., … Xiao, M. (2025). An Hα view of galaxy buildup in the first 2 Gyr: Luminosity functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202452363\">https://doi.org/10.1051/0004-6361/202452363</a>","mla":"Covelo-Paz, Alba, et al. “An Hα View of Galaxy Buildup in the First 2 Gyr: Luminosity Functions at z ∼ 4−6.5 from NIRCam/Grism Spectroscopy.” <i>Astronomy &#38; Astrophysics</i>, vol. 694, A178, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202452363\">10.1051/0004-6361/202452363</a>.","ieee":"A. Covelo-Paz <i>et al.</i>, “An Hα view of galaxy buildup in the first 2 Gyr: Luminosity functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy,” <i>Astronomy &#38; Astrophysics</i>, vol. 694. EDP Sciences, 2025.","short":"A. Covelo-Paz, E. Giovinazzo, P.A. Oesch, R.A. Meyer, A. Weibel, G. Brammer, Y. Fudamoto, J. Kerutt, J. Lin, J. Matharu, R.P. Naidu, A. Velichko, V. Bollo, R. Bouwens, J. Chisholm, G.D. Illingworth, I. Kramarenko, D. Magee, M. Maseda, J.J. Matthee, E. Nelson, N. Reddy, D. Schaerer, M. Stefanon, M. Xiao, Astronomy &#38; Astrophysics 694 (2025)."},"day":"12","type":"journal_article","quality_controlled":"1","_id":"19284","abstract":[{"text":"The Hα nebular emission line is an optimal tracer for recent star formation in galaxies. With the advent of JWST, this line has recently become observable at z > 3 for the first time. We present a catalog of 1050 Hα emitters at 3.7 < z < 6.7 in the GOODS fields obtained from a blind search in JWST NIRCam/grism data. We made use of the FRESCO survey’s 124 arcmin2 of observations in GOODS-North and GOODS-South with the F444W filter, probing Hα at 4.9 < z < 6.7, and the CONGRESS survey’s 62 arcmin2 of observations in GOODS-North with F356W, probing Hα at 3.8 < z < 5.1. We found an overdensity with 98 sources at z ∼ 4.4 in GOODS-N, and confirmed previously reported overdensities at z ∼ 5.2 in GOODS-N and at z ∼ 5.4 and z ∼ 5.9 in GOODS-S. We computed the observed Hα luminosity functions (LFs) in three bins centered at z ∼ 4.45, 5.30, and 6.15, which are the first such measurements at z > 3 obtained based purely on spectroscopic data, robustly tracing galaxy star formation rates (SFRs) beyond the peak of the cosmic star formation history. We compared our results with theoretical predictions from three different simulations and found good agreement at z ∼ 4 − 6. The UV LFs of this spectroscopically confirmed sample are in good agreement with pre-JWST measurements obtained with photometrically selected objects. Finally, we derived SFR functions and integrated them to compute the evolution of the cosmic SFR densities across z ∼ 4 − 6, finding values in good agreement with recent UV estimates from Lyman-break galaxies, which imply a continuous decrease in SFR density by a factor of three over z ∼ 4 to z ∼ 6. Our work shows the power of NIRCam grism observations to efficiently provide new tests for early galaxy formation models based on emission line statistics.","lang":"eng"}],"language":[{"iso":"eng"}],"external_id":{"arxiv":["2409.17241"],"isi":["001420194600001"]},"date_published":"2025-02-12T00:00:00Z","OA_place":"publisher","year":"2025","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","ddc":["520"],"article_number":"A178","intvolume":"       694","article_type":"original","month":"02","department":[{"_id":"JoMa"}],"author":[{"first_name":"Alba","last_name":"Covelo-Paz","full_name":"Covelo-Paz, Alba"},{"full_name":"Giovinazzo, Emma","last_name":"Giovinazzo","first_name":"Emma"},{"first_name":"Pascal A.","last_name":"Oesch","full_name":"Oesch, Pascal A."},{"first_name":"Romain A.","full_name":"Meyer, Romain A.","last_name":"Meyer"},{"first_name":"Andrea","last_name":"Weibel","full_name":"Weibel, Andrea"},{"first_name":"Gabriel","full_name":"Brammer, Gabriel","last_name":"Brammer"},{"full_name":"Fudamoto, Yoshinobu","last_name":"Fudamoto","first_name":"Yoshinobu"},{"first_name":"Josephine","full_name":"Kerutt, Josephine","last_name":"Kerutt"},{"last_name":"Lin","full_name":"Lin, Jamie","first_name":"Jamie"},{"last_name":"Matharu","full_name":"Matharu, Jasleen","first_name":"Jasleen"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"first_name":"Anna","full_name":"Velichko, Anna","last_name":"Velichko"},{"full_name":"Bollo, Victoria","last_name":"Bollo","first_name":"Victoria"},{"first_name":"Rychard","full_name":"Bouwens, Rychard","last_name":"Bouwens"},{"first_name":"John","full_name":"Chisholm, John","last_name":"Chisholm"},{"first_name":"Garth D.","last_name":"Illingworth","full_name":"Illingworth, Garth D."},{"last_name":"Kramarenko","full_name":"Kramarenko, Ivan","first_name":"Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","orcid":"0000-0001-5346-6048"},{"full_name":"Magee, Daniel","last_name":"Magee","first_name":"Daniel"},{"first_name":"Michael","last_name":"Maseda","full_name":"Maseda, Michael"},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"full_name":"Nelson, Erica","last_name":"Nelson","first_name":"Erica"},{"first_name":"Naveen","full_name":"Reddy, Naveen","last_name":"Reddy"},{"first_name":"Daniel","full_name":"Schaerer, Daniel","last_name":"Schaerer"},{"full_name":"Stefanon, Mauro","last_name":"Stefanon","first_name":"Mauro"},{"last_name":"Xiao","full_name":"Xiao, Mengyuan","first_name":"Mengyuan"}],"volume":694,"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 Nos. 1895 and 3577. The authors sincerely thank the CONGRESS team (PIs: Egami & Sun) for developing their observing program with a zero-exclusive-access period. We thank Aswin Vijayan and Harley Katz for their help in analyzing the simulation data from FLARES and SPHINX. This work has received funding from the Swiss State Secretariat for Education, Research, and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. Support for program #1895 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. Support for this work for RPN was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. MS acknowledges support from the European Research Commission Consolidator Grant 101088789 (SFEER), from the CIDEGENT/2021/059 grant by Generalitat Valenciana, and from project PID2023-149420NB-I00 funded by MICIU/AEI/10.13039/501100011033 and by ERDF/EU.","oa":1,"doi":"10.1051/0004-6361/202452363","related_material":{"link":[{"url":" https://github.com/astroalba/fresco","relation":"software"}]},"publisher":"EDP Sciences","tmp":{"short":"CC BY (4.0)","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)"},"article_processing_charge":"No","file":[{"access_level":"open_access","success":1,"content_type":"application/pdf","file_size":1865856,"date_created":"2025-03-04T09:29:01Z","checksum":"b1e74644a0cd37550e9a553f8675c93f","file_name":"2025_AstronomyAstrophysics_CoveloPaz.pdf","file_id":"19285","date_updated":"2025-03-04T09:29:01Z","creator":"dernst","relation":"main_file"}],"publication_status":"published","oa_version":"Published Version","OA_type":"diamond","title":"An Hα view of galaxy buildup in the first 2 Gyr: Luminosity functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy","date_created":"2025-03-02T23:01:54Z","arxiv":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]}},{"publisher":"IOP Publishing","article_processing_charge":"Yes","corr_author":"1","tmp":{"short":"CC BY (4.0)","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)"},"month":"07","department":[{"_id":"JoMa"}],"project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"article_type":"original","author":[{"last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"first_name":"Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","last_name":"Kotiwale","full_name":"Kotiwale, Gauri"},{"last_name":"Furtak","full_name":"Furtak, Lukas J.","first_name":"Lukas J."},{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan","orcid":"0000-0001-5346-6048","full_name":"Kramarenko, Ivan","last_name":"Kramarenko"},{"last_name":"Mackenzie","full_name":"Mackenzie, Ruari","first_name":"Ruari"},{"last_name":"Greene","full_name":"Greene, Jenny","first_name":"Jenny"},{"first_name":"Angela","full_name":"Adamo, Angela","last_name":"Adamo"},{"full_name":"Bouwens, Rychard J.","last_name":"Bouwens","first_name":"Rychard J."},{"last_name":"Di Cesare","full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","first_name":"Claudia"},{"first_name":"Anna-Christina","full_name":"Eilers, Anna-Christina","last_name":"Eilers"},{"last_name":"de Graaff","full_name":"de Graaff, Anna","first_name":"Anna"},{"last_name":"Heintz","full_name":"Heintz, Kasper E.","first_name":"Kasper E."},{"first_name":"Daichi","full_name":"Kashino, Daichi","last_name":"Kashino"},{"first_name":"Michael V.","full_name":"Maseda, Michael V.","last_name":"Maseda"},{"first_name":"Sandro","last_name":"Tacchella","full_name":"Tacchella, Sandro"},{"full_name":"Torralba Torregrosa, Alberto","last_name":"Torralba Torregrosa","id":"018f0249-0e87-11f0-b167-cbce08fbd541","first_name":"Alberto","orcid":"0000-0001-5586-6950"}],"volume":988,"oa":1,"doi":"10.3847/1538-4357/ade886","acknowledgement":"We thank the referee for their constructive comments that helped to improve the paper. We thank Junyao Li for sharing model output shown in Figure 13, Rob Crain for sharing results from the ONLYAGN EAGLE model shown in Figure 15, and Adi Zitrin for comments. 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 programs # 3516. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. We acknowledge funding from JWST program GO-3516. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS 5-26555. A.A. acknowledges support by the Swedish research council Vetenskapsrådet (2021-05559).","OA_type":"gold","oa_version":"Published Version","date_created":"2026-01-28T15:25:42Z","title":"Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5","arxiv":1,"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"file":[{"success":1,"content_type":"application/pdf","file_size":6237415,"date_created":"2026-02-09T08:20:14Z","access_level":"open_access","file_id":"21168","date_updated":"2026-02-09T08:20:14Z","creator":"dernst","relation":"main_file","checksum":"a49fbed72f2ff9c0b13129acb6f44f9d","file_name":"2025_AstrophysicalJournal_Matthee.pdf"}],"publication_status":"published","scopus_import":"1","DOAJ_listed":"1","issue":"2","status":"public","PlanS_conform":"1","publication":"The Astrophysical Journal","date_updated":"2026-02-09T08:22:01Z","file_date_updated":"2026-02-09T08:20:14Z","OA_place":"publisher","date_published":"2025-07-29T00:00:00Z","ddc":["520"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","year":"2025","intvolume":"       988","article_number":"246","day":"29","citation":{"chicago":"Matthee, Jorryt J, Rohan P. Naidu, Gauri Kotiwale, Lukas J. Furtak, Ivan Kramarenko, Ruari Mackenzie, Jenny Greene, et al. “Environmental Evidence for Overly Massive Black Holes in Low-Mass Galaxies and a Black Hole–Halo Mass Relation at z ∼ 5.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/ade886\">https://doi.org/10.3847/1538-4357/ade886</a>.","ista":"Matthee JJ, Naidu RP, Kotiwale G, Furtak LJ, Kramarenko I, Mackenzie R, Greene J, Adamo A, Bouwens RJ, Di Cesare C, Eilers A-C, de Graaff A, Heintz KE, Kashino D, Maseda MV, Tacchella S, Torralba Torregrosa A. 2025. Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5. The Astrophysical Journal. 988(2), 246.","ama":"Matthee JJ, Naidu RP, Kotiwale G, et al. Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5. <i>The Astrophysical Journal</i>. 2025;988(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ade886\">10.3847/1538-4357/ade886</a>","apa":"Matthee, J. J., Naidu, R. P., Kotiwale, G., Furtak, L. J., Kramarenko, I., Mackenzie, R., … Torralba Torregrosa, A. (2025). Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ade886\">https://doi.org/10.3847/1538-4357/ade886</a>","ieee":"J. J. Matthee <i>et al.</i>, “Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5,” <i>The Astrophysical Journal</i>, vol. 988, no. 2. IOP Publishing, 2025.","short":"J.J. Matthee, R.P. Naidu, G. Kotiwale, L.J. Furtak, I. Kramarenko, R. Mackenzie, J. Greene, A. Adamo, R.J. Bouwens, C. Di Cesare, A.-C. Eilers, A. de Graaff, K.E. Heintz, D. Kashino, M.V. Maseda, S. Tacchella, A. Torralba Torregrosa, The Astrophysical Journal 988 (2025).","mla":"Matthee, Jorryt J., et al. “Environmental Evidence for Overly Massive Black Holes in Low-Mass Galaxies and a Black Hole–Halo Mass Relation at z ∼ 5.” <i>The Astrophysical Journal</i>, vol. 988, no. 2, 246, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/ade886\">10.3847/1538-4357/ade886</a>."},"has_accepted_license":"1","quality_controlled":"1","type":"journal_article","external_id":{"arxiv":["2412.02846"]},"_id":"21062","language":[{"iso":"eng"}],"abstract":[{"lang":"eng","text":"JWST observations have unveiled faint active galactic nuclei (AGNs) at high redshift that provide insights into the formation of supermassive black holes (SMBHs). However, disentangling their stellar from AGN light is challenging. Here, we use an empirical approach to infer the average stellar mass of five faint broad-line (BL) Hα emitters at z = 4–5 with BH masses ≈6 × 10^6 M⊙, with a method independent of their spectral energy distribution (SED). We use the deep JWST/NIRcam grism survey “All the Little Things” to measure the overdensities around BL-Hα emitters and around a spectroscopic reference sample of ∼300 galaxies. In our reference sample, we find that megaparsec-scale overdensity correlates with stellar mass. Their large-scale environments suggest that BL-Hα emitters are hosted by galaxies with stellar masses ≈5 × 10^7 M⊙, ≈40 times lower than those inferred from galaxy-only SED fits. Adding measurements around more luminous z ≈ 6 AGNs, we find tentative correlations between line width, BH mass, and the overdensity, suggestive of a steep BH to halo mass relation. The main implications are (1) when BH masses are taken at face value, we confirm extremely high BH to stellar mass ratios of ≈10%, (2) the galaxies of low stellar mass that host growing SMBHs are in tension with typical hydrodynamical simulations, except those without feedback, (3) a 1% duty cycle implied by the host mass hints at super-Eddington accretion, (4) the masses are at odds with an interpretation of the line broadening in terms of high stellar density, (5) our results imply a luminosity-dependent diversity of galaxy masses, environments, and SEDs among AGN samples."}]},{"type":"journal_article","quality_controlled":"1","abstract":[{"text":"We present the first results on the spatial distribution of star formation in 454 star-forming galaxies just after the epoch of reionisation (4.8 < z < 6.5) using Hα emission-line maps and F444W imaging that traces the stellar continuum from the JWST FRESCO NIRCam Slitless Spectroscopy Survey. The Hα equivalent width profiles of star-forming galaxies across the main sequence at z ∼ 5.3 with stellar masses 6.8≤ log(M*/M⊙) < 11.1 increase with radius, which provides direct evidence for the inside-out growth of star-forming galaxies just after the epoch of reionisation. GALFIT was used to calculate half-light radii, Reff, and central surface densities within 1 kiloparsec, Σ1kpc of Hα and the continuum. At a fixed stellar mass of Log(M*/M⊙) = 9.5, Σ1kpc, Hα is 1.04 ± 0.05 times higher than Σ1kpc, C, Reff, Hα is 1.18 ± 0.03 times larger than Reff, C and both Reff measurements are smaller than 1 kiloparsec. These measurements suggest the rapid build-up of compact bulges via star formation just after the epoch of reionisation. By comparison to analogous work done at lower redshifts with Hubble Space Telescope WFC3 slitless spectroscopy as part of the 3D-HST (z ∼ 1) and CLEAR (z ∼ 0.5) surveys, we find that Reff(z) evolves at the same pace for Hα and the continuum, but Σ1kpc(z) evolves faster for Hα than the stellar continuum. As a function of the Hubble parameter, Reff, Hα/Reff,C = 1.1h(z) and Σ1 kpc, Hα/Σ1 kpc,C = h(z)1.3. These parametrisations suggest that the inside-out growth of the disk starts to dominate the inside-out growth of the bulge towards lower redshifts. This is supported by the redshift evolution in the EW(Hα) profiles from FRESCO, 3D-HST, and CLEAR at fixed stellar mass and when star-forming progenitors are traced, in which in EW(Hα) rapidly increases with radius within the half-light radius at z ∼ 5.3, but EW(Hα) increases only significantly with radius in the outer disk at z ∼ 0.5.","lang":"eng"}],"_id":"18447","language":[{"iso":"eng"}],"external_id":{"isi":["001322237700004"],"arxiv":["2404.17629"]},"has_accepted_license":"1","day":"01","citation":{"chicago":"Matharu, Jasleen, Erica J. Nelson, Gabriel Brammer, Pascal A. Oesch, Natalie Allen, Irene Shivaei, Rohan P. Naidu, et al. “A First Look at Spatially Resolved Star Formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam Slitless Spectroscopy.” <i>Astronomy and Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202450522\">https://doi.org/10.1051/0004-6361/202450522</a>.","ista":"Matharu J, Nelson EJ, Brammer G, Oesch PA, Allen N, Shivaei I, Naidu RP, Chisholm J, Covelo-Paz A, Fudamoto Y, Giovinazzo E, Herard-Demanche T, Kerutt J, Kramarenko I, Marchesini D, Meyer RA, Prieto-Lyon G, Reddy N, Shuntov M, Weibel A, Wuyts S, Xiao M. 2024. A first look at spatially resolved star formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam slitless spectroscopy. Astronomy and Astrophysics. 690, A64.","ama":"Matharu J, Nelson EJ, Brammer G, et al. A first look at spatially resolved star formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam slitless spectroscopy. <i>Astronomy and Astrophysics</i>. 2024;690. doi:<a href=\"https://doi.org/10.1051/0004-6361/202450522\">10.1051/0004-6361/202450522</a>","apa":"Matharu, J., Nelson, E. J., Brammer, G., Oesch, P. A., Allen, N., Shivaei, I., … Xiao, M. (2024). A first look at spatially resolved star formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam slitless spectroscopy. <i>Astronomy and Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202450522\">https://doi.org/10.1051/0004-6361/202450522</a>","ieee":"J. Matharu <i>et al.</i>, “A first look at spatially resolved star formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam slitless spectroscopy,” <i>Astronomy and Astrophysics</i>, vol. 690. EDP Sciences, 2024.","short":"J. Matharu, E.J. Nelson, G. Brammer, P.A. Oesch, N. Allen, I. Shivaei, R.P. Naidu, J. Chisholm, A. Covelo-Paz, Y. Fudamoto, E. Giovinazzo, T. Herard-Demanche, J. Kerutt, I. Kramarenko, D. Marchesini, R.A. Meyer, G. Prieto-Lyon, N. Reddy, M. Shuntov, A. Weibel, S. Wuyts, M. Xiao, Astronomy and Astrophysics 690 (2024).","mla":"Matharu, Jasleen, et al. “A First Look at Spatially Resolved Star Formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam Slitless Spectroscopy.” <i>Astronomy and Astrophysics</i>, vol. 690, A64, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202450522\">10.1051/0004-6361/202450522</a>."},"year":"2024","ddc":["520"],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_number":"A64","intvolume":"       690","date_published":"2024-10-01T00:00:00Z","OA_place":"publisher","file_date_updated":"2024-10-21T11:45:35Z","isi":1,"date_updated":"2025-09-08T14:22:57Z","publication":"Astronomy and Astrophysics","status":"public","scopus_import":"1","publication_status":"published","file":[{"creator":"dernst","file_id":"18457","relation":"main_file","date_updated":"2024-10-21T11:45:35Z","file_name":"2024_AstronomyAstrophysics_Matharu.pdf","checksum":"10ae78291aa9fa9a9e64724c42d91588","date_created":"2024-10-21T11:45:35Z","file_size":825494,"content_type":"application/pdf","success":1,"access_level":"open_access"}],"arxiv":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"oa_version":"Published Version","OA_type":"hybrid","title":"A first look at spatially resolved star formation at 4.8 < z < 6.5 with JWST FRESCO NIRCam slitless spectroscopy","date_created":"2024-10-20T22:02:06Z","acknowledgement":"JM is grateful to the Cosmic Dawn Center for the DAWN Fellowship. JM thanks Adam Muzzin, Viola Gelli and Anne Hutter for useful discussions that led to improvements in the analysis presented in this paper. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The raw data were obtained from the Mikulski Archive for\r\nSpace 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 JWST Cycle 1 GO program #1895. Support for program JWST-GO-1895 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Associations of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. The Cosmic Dawn Center  DAWN) is funded by the Danish National Research Foundation under grant DNRF140.\r\nThis work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. RPN thanks the NASA Hubble Fellowshp Program for the Hubble Fellowship. DM acknowledges funding from JWST-GO-01895.013, provided through a grant from the STScI under NASA contract NAS5-03127.","oa":1,"doi":"10.1051/0004-6361/202450522","article_type":"original","department":[{"_id":"JoMa"}],"month":"10","volume":690,"author":[{"full_name":"Matharu, Jasleen","last_name":"Matharu","first_name":"Jasleen"},{"full_name":"Nelson, Erica J.","last_name":"Nelson","first_name":"Erica J."},{"first_name":"Gabriel","last_name":"Brammer","full_name":"Brammer, Gabriel"},{"first_name":"Pascal A.","last_name":"Oesch","full_name":"Oesch, Pascal A."},{"last_name":"Allen","full_name":"Allen, Natalie","first_name":"Natalie"},{"first_name":"Irene","full_name":"Shivaei, Irene","last_name":"Shivaei"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"last_name":"Chisholm","full_name":"Chisholm, John","first_name":"John"},{"first_name":"Alba","last_name":"Covelo-Paz","full_name":"Covelo-Paz, Alba"},{"first_name":"Yoshinobu","last_name":"Fudamoto","full_name":"Fudamoto, Yoshinobu"},{"first_name":"Emma","last_name":"Giovinazzo","full_name":"Giovinazzo, Emma"},{"first_name":"Thomas","full_name":"Herard-Demanche, Thomas","last_name":"Herard-Demanche"},{"last_name":"Kerutt","full_name":"Kerutt, Josephine","first_name":"Josephine"},{"full_name":"Kramarenko, Ivan","last_name":"Kramarenko","orcid":"0000-0001-5346-6048","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan"},{"first_name":"Danilo","full_name":"Marchesini, Danilo","last_name":"Marchesini"},{"first_name":"Romain A.","last_name":"Meyer","full_name":"Meyer, Romain A."},{"first_name":"Gonzalo","last_name":"Prieto-Lyon","full_name":"Prieto-Lyon, Gonzalo"},{"first_name":"Naveen","full_name":"Reddy, Naveen","last_name":"Reddy"},{"first_name":"Marko","last_name":"Shuntov","full_name":"Shuntov, Marko"},{"last_name":"Weibel","full_name":"Weibel, Andrea","first_name":"Andrea"},{"first_name":"Stijn","last_name":"Wuyts","full_name":"Wuyts, Stijn"},{"first_name":"Mengyuan","last_name":"Xiao","full_name":"Xiao, Mengyuan"}],"publisher":"EDP Sciences","tmp":{"short":"CC BY (4.0)","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)"},"article_processing_charge":"Yes (in subscription journal)"},{"oa_version":"Published Version","OA_type":"hybrid","date_created":"2024-10-20T22:02:06Z","title":"A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with JWST MIRI","arxiv":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"file":[{"file_id":"18458","relation":"main_file","creator":"dernst","date_updated":"2024-10-21T11:52:29Z","checksum":"f399be98968b9ca5611c832a9b1eee2b","file_name":"2024_AstronomyAstrophysics_Shivaei.pdf","success":1,"content_type":"application/pdf","date_created":"2024-10-21T11:52:29Z","file_size":10777358,"access_level":"open_access"}],"publication_status":"published","publisher":"EDP Sciences","tmp":{"short":"CC BY (4.0)","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)"},"article_processing_charge":"Yes (in subscription journal)","article_type":"original","department":[{"_id":"JoMa"}],"month":"10","volume":690,"author":[{"last_name":"Shivaei","full_name":"Shivaei, Irene","first_name":"Irene"},{"last_name":"Alberts","full_name":"Alberts, Stacey","first_name":"Stacey"},{"first_name":"Michael","last_name":"Florian","full_name":"Florian, Michael"},{"first_name":"George","full_name":"Rieke, George","last_name":"Rieke"},{"first_name":"Stijn","full_name":"Wuyts, Stijn","last_name":"Wuyts"},{"last_name":"Bodansky","full_name":"Bodansky, Sarah","first_name":"Sarah"},{"first_name":"Andrew J.","last_name":"Bunker","full_name":"Bunker, Andrew J."},{"last_name":"Cameron","full_name":"Cameron, Alex J.","first_name":"Alex J."},{"first_name":"Mirko","last_name":"Curti","full_name":"Curti, Mirko"},{"first_name":"Francesco","last_name":"Da'Eugenio","full_name":"Da'Eugenio, Francesco"},{"last_name":"Dudzevičiūte","full_name":"Dudzevičiūte, Ugne","first_name":"Ugne"},{"first_name":"Zhiyuan","full_name":"Ji, Zhiyuan","last_name":"Ji"},{"first_name":"Benjamin D.","full_name":"Johnson, Benjamin D.","last_name":"Johnson"},{"orcid":"0000-0001-5346-6048","first_name":"Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","last_name":"Kramarenko","full_name":"Kramarenko, Ivan"},{"first_name":"Jianwei","last_name":"Lyu","full_name":"Lyu, Jianwei"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"full_name":"Morrison, Jane","last_name":"Morrison","first_name":"Jane"},{"first_name":"Rohan","last_name":"Naidu","full_name":"Naidu, Rohan"},{"first_name":"Pablo G.","last_name":"Pérez-González","full_name":"Pérez-González, Pablo G."},{"first_name":"Naveen","last_name":"Reddy","full_name":"Reddy, Naveen"},{"first_name":"Brant","full_name":"Robertson, Brant","last_name":"Robertson"},{"full_name":"Sun, Yang","last_name":"Sun","first_name":"Yang"},{"first_name":"Sandro","full_name":"Tacchella, Sandro","last_name":"Tacchella"},{"full_name":"Whitaker, Katherine","last_name":"Whitaker","first_name":"Katherine"},{"first_name":"Christina C.","last_name":"Williams","full_name":"Williams, Christina C."},{"full_name":"Willmer, Christopher N.A.","last_name":"Willmer","first_name":"Christopher N.A."},{"first_name":"Joris","last_name":"Witstok","full_name":"Witstok, Joris"},{"last_name":"Xiao","full_name":"Xiao, Mengyuan","first_name":"Mengyuan"},{"full_name":"Zhu, Yongda","last_name":"Zhu","first_name":"Yongda"}],"acknowledgement":"IS thanks the members of the JWST/MIRI instrument team for their exceptional efforts and for providing an outstanding experience during the commissioning period of JWST, which fostered numerous fruitful discussions and significantly enhanced the quality of data reduction in this study. IS also thanks Karin Sandstrom and Joel Leja for their insightful discussions during the scientific development of this work. Additionally, IS acknowledges the contribution of Andras Gáspar to the construction of the F560W PSF utilised in this research. This work was supported in part by NASA grant NNX13AD82G. Part of this research has been funded by Atraccíon de Talento Grant No. 2022-T1/TIC-20472 of the Comunidad de Madrid, Spain. AJB and AC acknowledges funding from the ‘FirstGalaxies’ Advanced Grant from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (Grant agreement No. 789056). The work of CCW is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. PGP-G acknowledges support from grant PID2022-139567NB-I00 funded by Spanish Ministerio de Ciencia e Innovación CIN/AEI/10.13039/501100011033, FEDER Una manera de hacer Europa. SA acknowledges support from the JWST Mid-Infrared Instrument (MIRI) Science Team Lead, grant 80NSSC18K0555, from NASA Goddard Space Flight Center to the University of Arizona. 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 PID 1207, 1080, 1081, 1895, 1220, 1286, 1287, 1963. Based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESAC/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA).","doi":"10.1051/0004-6361/202449579","oa":1,"date_published":"2024-10-01T00:00:00Z","OA_place":"publisher","year":"2024","ddc":["520"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","intvolume":"       690","article_number":"A89","has_accepted_license":"1","day":"01","citation":{"apa":"Shivaei, I., Alberts, S., Florian, M., Rieke, G., Wuyts, S., Bodansky, S., … Zhu, Y. (2024). A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with JWST MIRI. <i>Astronomy and Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202449579\">https://doi.org/10.1051/0004-6361/202449579</a>","mla":"Shivaei, Irene, et al. “A New Census of Dust and Polycyclic Aromatic Hydrocarbons at z = 0.7-2 with JWST MIRI.” <i>Astronomy and Astrophysics</i>, vol. 690, A89, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202449579\">10.1051/0004-6361/202449579</a>.","short":"I. Shivaei, S. Alberts, M. Florian, G. Rieke, S. Wuyts, S. Bodansky, A.J. Bunker, A.J. Cameron, M. Curti, F. Da’Eugenio, U. Dudzevičiūte, Z. Ji, B.D. Johnson, I. Kramarenko, J. Lyu, J.J. Matthee, J. Morrison, R. Naidu, P.G. Pérez-González, N. Reddy, B. Robertson, Y. Sun, S. Tacchella, K. Whitaker, C.C. Williams, C.N.A. Willmer, J. Witstok, M. Xiao, Y. Zhu, Astronomy and Astrophysics 690 (2024).","ieee":"I. Shivaei <i>et al.</i>, “A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with JWST MIRI,” <i>Astronomy and Astrophysics</i>, vol. 690. EDP Sciences, 2024.","chicago":"Shivaei, Irene, Stacey Alberts, Michael Florian, George Rieke, Stijn Wuyts, Sarah Bodansky, Andrew J. Bunker, et al. “A New Census of Dust and Polycyclic Aromatic Hydrocarbons at z = 0.7-2 with JWST MIRI.” <i>Astronomy and Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202449579\">https://doi.org/10.1051/0004-6361/202449579</a>.","ama":"Shivaei I, Alberts S, Florian M, et al. A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with JWST MIRI. <i>Astronomy and Astrophysics</i>. 2024;690. doi:<a href=\"https://doi.org/10.1051/0004-6361/202449579\">10.1051/0004-6361/202449579</a>","ista":"Shivaei I, Alberts S, Florian M, Rieke G, Wuyts S, Bodansky S, Bunker AJ, Cameron AJ, Curti M, Da’Eugenio F, Dudzevičiūte U, Ji Z, Johnson BD, Kramarenko I, Lyu J, Matthee JJ, Morrison J, Naidu R, Pérez-González PG, Reddy N, Robertson B, Sun Y, Tacchella S, Whitaker K, Williams CC, Willmer CNA, Witstok J, Xiao M, Zhu Y. 2024. A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with JWST MIRI. Astronomy and Astrophysics. 690, A89."},"type":"journal_article","quality_controlled":"1","_id":"18448","abstract":[{"lang":"eng","text":"Aims. This paper utilises the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) to extend the observational studies of dust and polycyclic aromatic hydrocarbon (PAH) emission to a new mass and star formation rate (SFR) parameter space beyond our local Universe. The combination of fully sampled spectral energy distributions (SEDs) with multiple mid-infrared (mid-IR) bands and the unprecedented sensitivity of MIRI allows us to investigate dust obscuration and PAH behaviour from z = 0.7 up to z = 2 in typical main-sequence galaxies. Our focus is on constraining the evolution of PAH strength and the dust-obscured luminosity fraction before and during cosmic noon, the epoch of peak star formation activity in the Universe.\r\n\r\nMethods. In this study, we utilise MIRI multi-band imaging data from the SMILES survey (5 to 25 μm), complemented with NIRCam photometry from the JADES survey (1 to 5 μm), available HST photometry (0.4 to 0.9 μm), and spectroscopic redshifts from the FRESCO and JADES surveys in GOODS-S for 443 star-forming (without dominant active galactic nucleus (AGN)) galaxies at z = 0.7 − 2.0. This redshift range was chosen to ensure that the MIRI data cover mid-IR dust emission. Our methodology involved employing ultraviolet (UV) to IR energy balance SED fitting to robustly constrain the fraction of dust mass in PAHs and dust-obscured luminosity. Additionally, we inferred dust sizes from MIRI 15 μm imaging data, enhancing our understanding of the physical characteristics of dust within these galaxies.\r\n\r\nResults. We find a strong correlation between the fraction of dust in PAHs (PAH fraction, qPAH) with stellar mass. Moreover, the sub-sample with robust qPAH measurements (N = 216) shows a similar behaviour between qPAH and gas-phase metallicity to that at z ∼ 0, suggesting a universal relation: qPAH is constant (∼3.4%) above a metallicity of Z ∼ 0.5 Z⊙ and decreases to < 1% at metallicities ≲0.3 Z⊙. This indicates that metallicity is a good indicator of the interstellar medium properties that affect the balance between the formation and destruction of PAHs. The lack of a redshift evolution from z ∼ 0 − 2 also implies that above Z ∼ 0.5 Z⊙ the PAH emission effectively traces obscured luminosity and the previous locally calibrated PAH-SFR calibrations remain applicable in this metallicity regime. We observe a strong correlation between the obscured UV luminosity fraction (ratio of obscured to total luminosity) and stellar mass. Above the stellar mass of M* > 5 × 109 M⊙, on average, more than half of the emitted luminosity is obscured, while there exists a non-negligible population of lower-mass galaxies with > 50% obscured fractions. At a fixed mass, the obscured fraction correlates with SFR surface density. This is a result of higher dust covering fractions in galaxies with more compact star-forming regions. Similarly, galaxies with high IRX (IR to UV luminosity) at a given mass or UV continuum slope (β) tend to have higher ΣSFR and shallower attenuation curves, owing to their higher effective dust optical depths and more compact star-forming regions."}],"language":[{"iso":"eng"}],"external_id":{"arxiv":["2402.07989"],"isi":["001381135700006"]},"scopus_import":"1","status":"public","isi":1,"publication":"Astronomy and Astrophysics","date_updated":"2026-03-05T11:19:11Z","file_date_updated":"2024-10-21T11:52:29Z"},{"acknowledgement":"The authors thank the anonymous referee for comments and suggestions which improved this paper. RAM thanks R. Kannan for sharing emission line luminosities from THESAN and H. Katz for similar data from an early version of the SPHINX20 data release (we use the final data release in this paper). The authors thank the CONGRESS team for proposing and designing their program with a zero exclusive access period.\r\nRAM, PA, ACP, and AW acknowledge support from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. PA, AW, EG, and MX acknowledge support from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072. YF acknowledges support by JSPS KAKENHI grant number JP22K21349 and JP23K13149. RPN acknowledges support for this work provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. MS acknowledges support from the European Research Commission Grant 101088789 (SFEER), from the CIDEGENT/2021/059 grant by Generalitat Valenciana, and from project PID2019-109592GB-I00/AEI/10.13039/501100011033 by the Spanish Ministerio de Ciencia e Innovación - Agencia Estatal de Investigación. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant no. 140. Cloud-based data processing and file storage for this work is provided by the AWS Cloud Credits for Research program. RJB and MS acknowledges support from NWO grant TOP1.16.057.\r\nThis work is based on observations made with the NASA/ESA/CSA JWST. The raw 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 JWST Cycle 1 GO program #1895. Support for program JWST-GO-1895 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Associations of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.","oa":1,"doi":"10.1093/mnras/stae2353","author":[{"first_name":"R. A.","full_name":"Meyer, R. A.","last_name":"Meyer"},{"first_name":"P. A.","last_name":"Oesch","full_name":"Oesch, P. A."},{"first_name":"E.","last_name":"Giovinazzo","full_name":"Giovinazzo, E."},{"last_name":"Weibel","full_name":"Weibel, A.","first_name":"A."},{"last_name":"Brammer","full_name":"Brammer, G.","first_name":"G."},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"full_name":"Naidu, R. P.","last_name":"Naidu","first_name":"R. P."},{"first_name":"R. J.","last_name":"Bouwens","full_name":"Bouwens, R. J."},{"last_name":"Chisholm","full_name":"Chisholm, J.","first_name":"J."},{"first_name":"A.","last_name":"Covelo-Paz","full_name":"Covelo-Paz, A."},{"full_name":"Fudamoto, Y.","last_name":"Fudamoto","first_name":"Y."},{"first_name":"M.","full_name":"Maseda, M.","last_name":"Maseda"},{"first_name":"E.","last_name":"Nelson","full_name":"Nelson, E."},{"last_name":"Shivaei","full_name":"Shivaei, I.","first_name":"I."},{"full_name":"Xiao, M.","last_name":"Xiao","first_name":"M."},{"last_name":"Herard-Demanche","full_name":"Herard-Demanche, T.","first_name":"T."},{"first_name":"G. D.","full_name":"Illingworth, G. D.","last_name":"Illingworth"},{"full_name":"Kerutt, J.","last_name":"Kerutt","first_name":"J."},{"last_name":"Kramarenko","full_name":"Kramarenko, Ivan","orcid":"0000-0001-5346-6048","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan"},{"first_name":"I.","full_name":"Labbe, I.","last_name":"Labbe"},{"first_name":"E.","full_name":"Leonova, E.","last_name":"Leonova"},{"first_name":"D.","full_name":"Magee, D.","last_name":"Magee"},{"first_name":"J.","full_name":"Matharu, J.","last_name":"Matharu"},{"first_name":"G.","last_name":"Prieto Lyon","full_name":"Prieto Lyon, G."},{"first_name":"N.","last_name":"Reddy","full_name":"Reddy, N."},{"first_name":"D.","full_name":"Schaerer, D.","last_name":"Schaerer"},{"first_name":"A.","last_name":"Shapley","full_name":"Shapley, A."},{"first_name":"M.","last_name":"Stefanon","full_name":"Stefanon, M."},{"first_name":"M. A.","last_name":"Wozniak","full_name":"Wozniak, M. A."},{"first_name":"S.","last_name":"Wuyts","full_name":"Wuyts, S."}],"volume":535,"article_type":"original","month":"11","department":[{"_id":"JoMa"}],"tmp":{"short":"CC BY (4.0)","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)"},"article_processing_charge":"Yes","publisher":"Oxford University Press","publication_status":"published","file":[{"relation":"main_file","creator":"dernst","date_updated":"2024-12-03T12:52:13Z","file_id":"18613","file_name":"2024_MonthlyNRoyalAstronSoc_Meyer.pdf","checksum":"efe0ce3580e01459f3be78eb111b35a9","file_size":29476699,"date_created":"2024-12-03T12:52:13Z","success":1,"content_type":"application/pdf","access_level":"open_access"}],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"date_created":"2024-11-24T23:01:49Z","title":"JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 < z < 9.0 in the GOODS fields","oa_version":"Published Version","OA_type":"gold","file_date_updated":"2024-12-03T12:52:13Z","date_updated":"2025-09-08T14:47:58Z","publication":"Monthly Notices of the Royal Astronomical Society","isi":1,"page":"1067-1094","status":"public","DOAJ_listed":"1","issue":"1","scopus_import":"1","_id":"18585","language":[{"iso":"eng"}],"abstract":[{"text":"We present the census of Hβ+[OIII] 4960,5008 Åemitters at 6.8<z<9.0 from the JWST FRESCO survey over 124 arcmin2 in the GOODS-North and GOODS-South fields. Our unbiased spectroscopic search results in 137 spectroscopically-confirmed galaxies at 6.8<z<9.0 with observed [OIII] fluxes f[OIII]≳1×10−18 ergs s−1 cm−2. The rest-frame optical line ratios of the median stacked spectrum (median MUV=−19.65+0.59−1.05) indicate negligible dust attenuation, low metallicity (12+log(O/H)=7.2−7.7) and a high ionisation parameter log10U≃−2.5. We find a factor ×1.3 difference in the number density of 6.8<z<9.0 galaxies between GOODS-South and GOODS-North, which is caused by a single overdensity at 7.0<z<7.2 in GOODS-North. The bright end of the UV luminosity function of spectroscopically-confirmed [OIII] emitters is in good agreement with HST dropout-selected samples. Discrepancies between the observed [OIII] LF, [OIII]/UV ratio and [OIII] equivalent widths, and that predicted by theoretical models, suggest burstier star-formation histories and/or more heterogeneous metallicity and ionising conditions in z>7 galaxies. We report a rapid decline of the [OIII] luminosity density at z≳6−7 which cannot be explained by the evolution of the cosmic star-formation rate density. Finally we find that FRESCO detects in only 2h galaxies likely accounting for ∼10−20% of the ionising budget at z=7−8 (assuming an escape fraction of 10%), raising the prospect of directly detecting a significant fraction of the sources of reionisation with JWST.","lang":"eng"}],"external_id":{"isi":["001348009500001"]},"type":"journal_article","quality_controlled":"1","has_accepted_license":"1","citation":{"ama":"Meyer RA, Oesch PA, Giovinazzo E, et al. JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 &#60; z &#60; 9.0 in the GOODS fields. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;535(1):1067-1094. doi:<a href=\"https://doi.org/10.1093/mnras/stae2353\">10.1093/mnras/stae2353</a>","ista":"Meyer RA, Oesch PA, Giovinazzo E, Weibel A, Brammer G, Matthee JJ, Naidu RP, Bouwens RJ, Chisholm J, Covelo-Paz A, Fudamoto Y, Maseda M, Nelson E, Shivaei I, Xiao M, Herard-Demanche T, Illingworth GD, Kerutt J, Kramarenko I, Labbe I, Leonova E, Magee D, Matharu J, Prieto Lyon G, Reddy N, Schaerer D, Shapley A, Stefanon M, Wozniak MA, Wuyts S. 2024. JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 &#60; z &#60; 9.0 in the GOODS fields. Monthly Notices of the Royal Astronomical Society. 535(1), 1067–1094.","chicago":"Meyer, R. A., P. A. Oesch, E. Giovinazzo, A. Weibel, G. Brammer, Jorryt J Matthee, R. P. Naidu, et al. “JWST FRESCO: A Comprehensive Census of H β + [O Iii] Emitters at 6.8 &#60; z &#60; 9.0 in the GOODS Fields.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stae2353\">https://doi.org/10.1093/mnras/stae2353</a>.","mla":"Meyer, R. A., et al. “JWST FRESCO: A Comprehensive Census of H β + [O Iii] Emitters at 6.8 &#60; z &#60; 9.0 in the GOODS Fields.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 535, no. 1, Oxford University Press, 2024, pp. 1067–94, doi:<a href=\"https://doi.org/10.1093/mnras/stae2353\">10.1093/mnras/stae2353</a>.","short":"R.A. Meyer, P.A. Oesch, E. Giovinazzo, A. Weibel, G. Brammer, J.J. Matthee, R.P. Naidu, R.J. Bouwens, J. Chisholm, A. Covelo-Paz, Y. Fudamoto, M. Maseda, E. Nelson, I. Shivaei, M. Xiao, T. Herard-Demanche, G.D. Illingworth, J. Kerutt, I. Kramarenko, I. Labbe, E. Leonova, D. Magee, J. Matharu, G. Prieto Lyon, N. Reddy, D. Schaerer, A. Shapley, M. Stefanon, M.A. Wozniak, S. Wuyts, Monthly Notices of the Royal Astronomical Society 535 (2024) 1067–1094.","ieee":"R. A. Meyer <i>et al.</i>, “JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 &#60; z &#60; 9.0 in the GOODS fields,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 535, no. 1. Oxford University Press, pp. 1067–1094, 2024.","apa":"Meyer, R. A., Oesch, P. A., Giovinazzo, E., Weibel, A., Brammer, G., Matthee, J. J., … Wuyts, S. (2024). JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 &#60; z &#60; 9.0 in the GOODS fields. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stae2353\">https://doi.org/10.1093/mnras/stae2353</a>"},"day":"01","intvolume":"       535","year":"2024","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","ddc":["520"],"date_published":"2024-11-01T00:00:00Z","OA_place":"publisher"},{"publisher":"Oxford University Press","article_processing_charge":"Yes","corr_author":"1","tmp":{"short":"CC BY (4.0)","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)"},"month":"02","department":[{"_id":"GradSch"},{"_id":"JoMa"}],"article_type":"original","author":[{"orcid":"0000-0001-5346-6048","first_name":"Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","last_name":"Kramarenko","full_name":"Kramarenko, Ivan"},{"first_name":"J","last_name":"Kerutt","full_name":"Kerutt, J"},{"last_name":"Verhamme","full_name":"Verhamme, A","first_name":"A"},{"full_name":"Oesch, P A","last_name":"Oesch","first_name":"P A"},{"first_name":"L","last_name":"Barrufet","full_name":"Barrufet, L"},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"H","full_name":"Kusakabe, H","last_name":"Kusakabe"},{"first_name":"I","last_name":"Goovaerts","full_name":"Goovaerts, I"},{"full_name":"Thai, T T","last_name":"Thai","first_name":"T T"}],"volume":527,"oa":1,"doi":"10.1093/mnras/stad3853","acknowledgement":"We thank the anonymous referee for the constructive feedback that helped to improve the manuscript. We thank Michael Maseda, Daniel Schaerer, Charlotte Simmonds, and Rashmi Gottumukkala for useful comments and productive discussions. We also thank the organizers and participants of the 24th MUSE Science Busy Week in Leiden. IGK acknowledges an Excellence Master Fellowship granted by the Faculty of Science of the University of Geneva. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant number 200020_207349 and SNSF Professorship grant number 190079. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant number 140. This paper is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 094.A-0289(B), 095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 094.A-0205, 095.A-0240, 096.A-0090, 097.A-0160, and 098.A-0017. We made extensive use of several open-source software packages and we are thankful to the respective authors for sharing their work: NUMPY (Harris et al. 2020), ASTROPY (Astropy Collaboration 2022), MATPLOTLIB (Hunter 2007), IPYTHON (Perez & Granger 2007), and TOPCAT (Taylor 2005).","oa_version":"Published Version","title":"Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape","date_created":"2024-01-22T08:22:17Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"arxiv":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"file":[{"content_type":"application/pdf","success":1,"date_created":"2024-01-23T12:30:45Z","file_size":4521738,"access_level":"open_access","relation":"main_file","file_id":"14879","date_updated":"2024-01-23T12:30:45Z","creator":"dernst","checksum":"9d02df4035c4951cf63dee0db1e462e9","file_name":"2024_MNAstronomSoc_Kramarenko.pdf"}],"publication_status":"published","scopus_import":"1","issue":"4","DOAJ_listed":"1","page":"9853-9871","status":"public","isi":1,"publication":"Monthly Notices of the Royal Astronomical Society","date_updated":"2025-09-04T11:51:50Z","file_date_updated":"2024-01-23T12:30:45Z","date_published":"2024-02-01T00:00:00Z","ddc":["520"],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","year":"2024","intvolume":"       527","day":"01","citation":{"chicago":"Kramarenko, Ivan, J Kerutt, A Verhamme, P A Oesch, L Barrufet, Jorryt J Matthee, H Kusakabe, I Goovaerts, and T T Thai. “Linking UV Spectral Properties of MUSE Ly α Emitters at <i>z</i> ≳ 3 to Lyman Continuum Escape.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stad3853\">https://doi.org/10.1093/mnras/stad3853</a>.","ama":"Kramarenko I, Kerutt J, Verhamme A, et al. Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;527(4):9853-9871. doi:<a href=\"https://doi.org/10.1093/mnras/stad3853\">10.1093/mnras/stad3853</a>","ista":"Kramarenko I, Kerutt J, Verhamme A, Oesch PA, Barrufet L, Matthee JJ, Kusakabe H, Goovaerts I, Thai TT. 2024. Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape. Monthly Notices of the Royal Astronomical Society. 527(4), 9853–9871.","apa":"Kramarenko, I., Kerutt, J., Verhamme, A., Oesch, P. A., Barrufet, L., Matthee, J. J., … Thai, T. T. (2024). Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stad3853\">https://doi.org/10.1093/mnras/stad3853</a>","mla":"Kramarenko, Ivan, et al. “Linking UV Spectral Properties of MUSE Ly α Emitters at <i>z</i> ≳ 3 to Lyman Continuum Escape.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 527, no. 4, Oxford University Press, 2024, pp. 9853–71, doi:<a href=\"https://doi.org/10.1093/mnras/stad3853\">10.1093/mnras/stad3853</a>.","ieee":"I. Kramarenko <i>et al.</i>, “Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 527, no. 4. Oxford University Press, pp. 9853–9871, 2024.","short":"I. Kramarenko, J. Kerutt, A. Verhamme, P.A. Oesch, L. Barrufet, J.J. Matthee, H. Kusakabe, I. Goovaerts, T.T. Thai, Monthly Notices of the Royal Astronomical Society 527 (2024) 9853–9871."},"has_accepted_license":"1","quality_controlled":"1","type":"journal_article","external_id":{"arxiv":["2305.07044"],"isi":["001133672400004"]},"language":[{"iso":"eng"}],"_id":"14852","abstract":[{"text":"The physical conditions giving rise to high escape fractions of ionizing radiation (LyC fesc) in star-forming galaxies – most likely protagonists of cosmic reionization – are not yet fully understood. Using the VLT/MUSE observations of ∼1400 Ly α emitters at 2.9 &amp;lt; z &amp;lt; 6.7, we compare stacked rest-frame UV spectra of candidates for LyC leakers and non-leakers selected based on their Ly α profiles. We find that the stacks of potential LyC leakers, i.e. galaxies with narrow, symmetric Ly α profiles with small peak separation, generally show (i) strong nebular O iii]λ1666, [Si iii]λ1883, and [C iii]λ1907 +C iii]λ1909 emission, indicating a high-ionization state of the interstellar medium (ISM); (ii) high equivalent widths of He iiλ1640 (∼1 − 3 Å), suggesting the presence of hard ionizing radiation fields; (iii) Si ii*λ1533 emission, revealing substantial amounts of neutral hydrogen off the line of sight; (iv) high C ivλλ1548,1550 to [C iii]λ1907 +C iii]λ1909 ratios (C iv/C iii] ≳0.75) , signalling the presence of low column density channels in the ISM. In contrast, the stacks with broad, asymmetric Ly α profiles with large peak separation show weak nebular emission lines, low He iiλ1640 equivalent widths (≲1 Å), and low C iv/C iii] (≲0.25), implying low-ionization states and high-neutral hydrogen column densities. Our results suggest that C iv/C iii] might be sensitive to the physical conditions that govern LyC photon escape, providing a promising tool for identification of ionizing sources among star-forming galaxies in the epoch of reionization.","lang":"eng"}]}]