[{"tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"department":[{"_id":"JoMa"},{"_id":"GradSch"}],"abstract":[{"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.","lang":"eng"}],"project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"PlanS_conform":"1","month":"02","date_published":"2026-02-01T00:00:00Z","publication_status":"published","_id":"21341","article_type":"original","citation":{"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.","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>.","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>.","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).","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>","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>","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."},"quality_controlled":"1","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"intvolume":"       706","has_accepted_license":"1","publication":"Astronomy & Astrophysics","arxiv":1,"title":"Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy","corr_author":"1","article_number":"A165","oa_version":"Published Version","author":[{"first_name":"Gauri","last_name":"Kotiwale","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","full_name":"Kotiwale, Gauri"},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"first_name":"Daichi","last_name":"Kashino","full_name":"Kashino, Daichi"},{"full_name":"Vijayan, Aswin P.","last_name":"Vijayan","first_name":"Aswin P."},{"last_name":"Torralba Torregrosa","orcid":"0000-0001-5586-6950","first_name":"Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","full_name":"Torralba Torregrosa, Alberto"},{"id":"2d002343-372f-11ef-98ec-a164d20427cb","last_name":"Di Cesare","first_name":"Claudia","full_name":"Di Cesare, Claudia"},{"first_name":"Edoardo","orcid":"0000-0001-8386-3546","last_name":"Iani","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","full_name":"Iani, Edoardo"},{"first_name":"Rongmon","last_name":"Bordoloi","full_name":"Bordoloi, Rongmon"},{"full_name":"Leja, Joel","last_name":"Leja","first_name":"Joel"},{"last_name":"Maseda","first_name":"Michael V.","full_name":"Maseda, Michael V."},{"last_name":"Tacchella","first_name":"Sandro","full_name":"Tacchella, Sandro"},{"first_name":"Irene","last_name":"Shivaei","full_name":"Shivaei, Irene"},{"full_name":"Heintz, Kasper E.","last_name":"Heintz","first_name":"Kasper E."},{"last_name":"Danhaive","first_name":"A. Lola","full_name":"Danhaive, A. Lola"},{"id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","first_name":"Sara","last_name":"Mascia","full_name":"Mascia, Sara"},{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan","orcid":"0000-0001-5346-6048","last_name":"Kramarenko","full_name":"Kramarenko, Ivan"},{"last_name":"Navarrete","first_name":"Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","full_name":"Navarrete, Benjamín"},{"first_name":"Ruari","last_name":"Mackenzie","full_name":"Mackenzie, Ruari"},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"}],"OA_type":"diamond","day":"01","ddc":["520"],"date_updated":"2026-02-24T07:49:42Z","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).","publisher":"EDP Sciences","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","volume":706,"DOAJ_listed":"1","OA_place":"publisher","article_processing_charge":"No","file":[{"checksum":"6f5849d29ad43bee32f90152f6fc0294","access_level":"open_access","date_updated":"2026-02-24T07:46:47Z","content_type":"application/pdf","date_created":"2026-02-24T07:46:47Z","creator":"dernst","file_name":"2026_AstronomyAstrophysics_Kotiwale.pdf","success":1,"file_size":6531719,"relation":"main_file","file_id":"21355"}],"date_created":"2026-02-22T23:01:35Z","file_date_updated":"2026-02-24T07:46:47Z","language":[{"iso":"eng"}],"type":"journal_article","external_id":{"arxiv":["2510.19959"]},"status":"public","oa":1,"year":"2026","scopus_import":"1","doi":"10.1051/0004-6361/202556597"},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"EDP Sciences","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":[{"last_name":"Torralba Torregrosa","orcid":"0000-0001-5586-6950","first_name":"Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","full_name":"Torralba Torregrosa, Alberto"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"full_name":"Pezzulli, Gabriele","last_name":"Pezzulli","first_name":"Gabriele"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"last_name":"Ishikawa","first_name":"Yuzo","full_name":"Ishikawa, Yuzo"},{"last_name":"Brammer","first_name":"Gabriel B.","full_name":"Brammer, Gabriel B."},{"last_name":"Chang","first_name":"Seok Jun","full_name":"Chang, Seok Jun"},{"last_name":"Chisholm","first_name":"John","full_name":"Chisholm, John"},{"full_name":"De Graaff, Anna","first_name":"Anna","last_name":"De Graaff"},{"full_name":"D’Eugenio, Francesco","last_name":"D’Eugenio","first_name":"Francesco"},{"full_name":"Di Cesare, Claudia","first_name":"Claudia","last_name":"Di Cesare","id":"2d002343-372f-11ef-98ec-a164d20427cb"},{"last_name":"Eilers","first_name":"Anna Christina","full_name":"Eilers, Anna Christina"},{"first_name":"Jenny E.","last_name":"Greene","full_name":"Greene, Jenny E."},{"last_name":"Gronke","first_name":"Max","full_name":"Gronke, Max"},{"id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","first_name":"Edoardo","orcid":"0000-0001-8386-3546","last_name":"Iani","full_name":"Iani, Edoardo"},{"full_name":"Kokorev, Vasily","first_name":"Vasily","last_name":"Kokorev"},{"full_name":"Kotiwale, Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","first_name":"Gauri","last_name":"Kotiwale"},{"first_name":"Ivan","orcid":"0000-0001-5346-6048","last_name":"Kramarenko","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","full_name":"Kramarenko, Ivan"},{"full_name":"Ma, Yilun","last_name":"Ma","first_name":"Yilun"},{"full_name":"Mascia, Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","first_name":"Sara","last_name":"Mascia"},{"full_name":"Navarrete, Benjamín","last_name":"Navarrete","first_name":"Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148"},{"first_name":"Erica","last_name":"Nelson","full_name":"Nelson, Erica"},{"full_name":"Oesch, Pascal","last_name":"Oesch","first_name":"Pascal"},{"full_name":"Simcoe, Robert A.","last_name":"Simcoe","first_name":"Robert A."},{"last_name":"Wuyts","first_name":"Stijn","full_name":"Wuyts, Stijn"}],"OA_type":"diamond","day":"01","date_updated":"2026-03-16T10:59:16Z","ddc":["520"],"OA_place":"publisher","file":[{"file_name":"2026_AstronomyAstrophysics_Torralba2.pdf","success":1,"content_type":"application/pdf","date_created":"2026-03-16T10:57:49Z","creator":"dernst","access_level":"open_access","checksum":"fcab9cb3dcf1d68612e1fdc8191643c1","date_updated":"2026-03-16T10:57:49Z","relation":"main_file","file_id":"21460","file_size":2510157}],"article_processing_charge":"No","DOAJ_listed":"1","volume":707,"language":[{"iso":"eng"}],"date_created":"2026-03-15T23:01:36Z","file_date_updated":"2026-03-16T10:57:49Z","oa":1,"year":"2026","status":"public","external_id":{"arxiv":["2510.00103"]},"doi":"10.1051/0004-6361/202557537","scopus_import":"1","type":"journal_article","abstract":[{"lang":"eng","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."}],"department":[{"_id":"JoMa"}],"month":"03","date_published":"2026-03-01T00:00:00Z","project":[{"grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization"}],"PlanS_conform":"1","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_type":"original","_id":"21451","publication_status":"published","quality_controlled":"1","citation":{"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).","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>","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.","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>","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.","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>.","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>."},"intvolume":"       707","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"article_number":"A75","oa_version":"Published Version","publication":"Astronomy & Astrophysics","has_accepted_license":"1","corr_author":"1","title":"The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings","arxiv":1},{"month":"03","date_published":"2026-03-01T00:00:00Z","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"PlanS_conform":"1","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"}],"department":[{"_id":"JoMa"},{"_id":"GradSch"}],"tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_type":"original","_id":"21452","publication_status":"published","intvolume":"       707","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"quality_controlled":"1","citation":{"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>.","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>.","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.","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>","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.","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>","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)."},"oa_version":"Published Version","article_number":"A129","corr_author":"1","arxiv":1,"title":"The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations","publication":"Astronomy & Astrophysics","has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","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).","publisher":"EDP Sciences","date_updated":"2026-03-16T10:52:44Z","day":"01","ddc":["520"],"author":[{"first_name":"Claudia","last_name":"Di Cesare","id":"2d002343-372f-11ef-98ec-a164d20427cb","full_name":"Di Cesare, Claudia"},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"last_name":"Naidu","first_name":"Rohan P.","full_name":"Naidu, Rohan P."},{"first_name":"Alberto","last_name":"Torralba","full_name":"Torralba, Alberto"},{"full_name":"Kotiwale, Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","last_name":"Kotiwale","first_name":"Gauri"},{"orcid":"0000-0001-5346-6048","first_name":"Ivan","last_name":"Kramarenko","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","full_name":"Kramarenko, Ivan"},{"last_name":"Blaizot","first_name":"Jeremy","full_name":"Blaizot, Jeremy"},{"last_name":"Rosdahl","first_name":"Joakim","full_name":"Rosdahl, Joakim"},{"full_name":"Leja, Joel","first_name":"Joel","last_name":"Leja"},{"full_name":"Iani, Edoardo","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","first_name":"Edoardo","orcid":"0000-0001-8386-3546","last_name":"Iani"},{"first_name":"Angela","last_name":"Adamo","full_name":"Adamo, Angela"},{"full_name":"Covelo-Paz, Alba","last_name":"Covelo-Paz","first_name":"Alba"},{"last_name":"Furtak","first_name":"Lukas J.","full_name":"Furtak, Lukas J."},{"first_name":"Kasper E.","last_name":"Heintz","full_name":"Heintz, Kasper E."},{"full_name":"Mascia, Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","first_name":"Sara","last_name":"Mascia"},{"full_name":"Navarrete, Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","first_name":"Benjamín","last_name":"Navarrete"},{"full_name":"Oesch, Pascal A.","first_name":"Pascal A.","last_name":"Oesch"},{"full_name":"Romano, Michael","first_name":"Michael","last_name":"Romano"},{"last_name":"Shivaei","first_name":"Irene","full_name":"Shivaei, Irene"},{"last_name":"Tacchella","first_name":"Sandro","full_name":"Tacchella, Sandro"}],"OA_type":"diamond","file":[{"success":1,"file_name":"2026_AstronomyAstrophysics_DiCesare.pdf","date_updated":"2026-03-16T10:48:07Z","access_level":"open_access","checksum":"c056b00ce7324849754521fde10fb7ca","creator":"dernst","content_type":"application/pdf","date_created":"2026-03-16T10:48:07Z","relation":"main_file","file_id":"21459","file_size":1821411}],"article_processing_charge":"No","OA_place":"publisher","DOAJ_listed":"1","volume":707,"language":[{"iso":"eng"}],"file_date_updated":"2026-03-16T10:48:07Z","date_created":"2026-03-15T23:01:36Z","doi":"10.1051/0004-6361/202557790","scopus_import":"1","oa":1,"year":"2026","external_id":{"arxiv":["2510.19044"]},"status":"public","type":"journal_article"},{"tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"department":[{"_id":"JoMa"}],"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."}],"PlanS_conform":"1","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"date_published":"2026-03-05T00:00:00Z","month":"03","publication_status":"published","_id":"21481","article_type":"original","citation":{"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.","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>","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>","short":"I. Kramarenko, J. Rosdahl, J. Blaizot, J.J. Matthee, H. Katz, C. Di Cesare, Astronomy &#38; Astrophysics 707 (2026).","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>.","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>.","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."},"quality_controlled":"1","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"intvolume":"       707","has_accepted_license":"1","publication":"Astronomy & Astrophysics","arxiv":1,"title":"H α as a tracer of star formation in the SPHINX cosmological simulations","corr_author":"1","article_number":"A184","oa_version":"Published Version","author":[{"full_name":"Kramarenko, Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","last_name":"Kramarenko","orcid":"0000-0001-5346-6048","first_name":"Ivan"},{"full_name":"Rosdahl, J.","last_name":"Rosdahl","first_name":"J."},{"last_name":"Blaizot","first_name":"J.","full_name":"Blaizot, J."},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Katz","first_name":"H.","full_name":"Katz, H."},{"id":"2d002343-372f-11ef-98ec-a164d20427cb","first_name":"Claudia","last_name":"Di Cesare","full_name":"Di Cesare, Claudia"}],"OA_type":"diamond","ddc":["520"],"date_updated":"2026-03-23T15:46:31Z","day":"05","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).","publisher":"EDP Sciences","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","volume":707,"DOAJ_listed":"1","OA_place":"publisher","article_processing_charge":"No","file":[{"relation":"main_file","file_id":"21492","file_size":904565,"success":1,"file_name":"2026_AstronomyAstrophysics_Kramarenko.pdf","creator":"dernst","content_type":"application/pdf","date_created":"2026-03-23T15:44:09Z","date_updated":"2026-03-23T15:44:09Z","checksum":"7429076b381dd498084f40ffd199e714","access_level":"open_access"}],"date_created":"2026-03-23T14:58:03Z","file_date_updated":"2026-03-23T15:44:09Z","language":[{"iso":"eng"}],"type":"journal_article","status":"public","external_id":{"arxiv":["2509.05403"]},"oa":1,"year":"2026","doi":"10.1051/0004-6361/202557114"},{"article_type":"original","_id":"21045","publication_status":"published","abstract":[{"text":"The abundant population of little red dots (LRDs), compact objects with red UV to optical colors and broad Balmer lines at high redshift, is revealing new insights into the properties of early active galactic nuclei (AGN). Perhaps the most surprising features of this population are the presence of Balmer absorption and ubiquitous strong Balmer breaks. Recent models link these features to an active supermassive black hole (SMBH) cocooned in very dense gas (NH ∼ 1024 cm−2). We present a stringent test of such models using VLT/MUSE observations of A2744-45924, the most luminous LRD known to date (LHα ≈ 1044 erg s−1), located behind the Abell-2744 lensing cluster at z = 4.464 (μ = 1.8). We detect a moderately extended Lyα nebula (h ≈ 5.7 pkpc), spatially offset from the point-like Hα seen by JWST by ≈1.6 pkpc. The Lyα emission is narrow (FWHM = 270 ± 15 km s−1), and faint (Lyα = 0.07Hα) compared to Lyα nebulae typically observed around quasars of similar luminosity. We detect compact N IV]λ1486 emission, spatially aligned with Hα, and a spatial shift in the far-UV continuum matching the Lyα offset. We discuss that Hα and Lyα have distinct physical origins: Hα originates from the AGN, while Lyα is powered by star formation. In the environment of A2744-45924, we identified four extended Lyα halos (Δz < 0.02, Δr < 100 pkpc). Their Lyα luminosities match the expectations based on Hα emission, and show no evidence for radiation from A2744-45924 affecting its surroundings. The lack of strong, compact, and broad Lyα and the absence of a luminous extended halo, suggest that the UV AGN light is obscured by dense gas cloaking the SMBH with a covering factor close to unity.","lang":"eng"}],"department":[{"_id":"JoMa"},{"_id":"GradSch"}],"month":"01","date_published":"2026-01-14T00:00:00Z","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224"}],"PlanS_conform":"1","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_number":"A147","oa_version":"Published Version","publication":"Astronomy & Astrophysics","has_accepted_license":"1","corr_author":"1","arxiv":1,"title":"A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth","quality_controlled":"1","citation":{"short":"A. Torralba Torregrosa, J.J. Matthee, G. Pezzulli, T. Urrutia, M. Gronke, S. Mascia, F. D’Eugenio, C. Di Cesare, A.C. Eilers, J.E. Greene, E. Iani, Y. Ishikawa, R. Mackenzie, R.P. Naidu, B. Navarrete, G. Kotiwale, Astronomy &#38; Astrophysics 705 (2026).","ieee":"A. Torralba Torregrosa <i>et al.</i>, “A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth,” <i>Astronomy &#38; Astrophysics</i>, vol. 705. EDP Sciences, 2026.","apa":"Torralba Torregrosa, A., Matthee, J. J., Pezzulli, G., Urrutia, T., Gronke, M., Mascia, S., … Kotiwale, G. (2026). A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202555596\">https://doi.org/10.1051/0004-6361/202555596</a>","ama":"Torralba Torregrosa A, Matthee JJ, Pezzulli G, et al. A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth. <i>Astronomy &#38; Astrophysics</i>. 2026;705. doi:<a href=\"https://doi.org/10.1051/0004-6361/202555596\">10.1051/0004-6361/202555596</a>","ista":"Torralba Torregrosa A, Matthee JJ, Pezzulli G, Urrutia T, Gronke M, Mascia S, D’Eugenio F, Di Cesare C, Eilers AC, Greene JE, Iani E, Ishikawa Y, Mackenzie R, Naidu RP, Navarrete B, Kotiwale G. 2026. A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth. Astronomy &#38; Astrophysics. 705, A147.","chicago":"Torralba Torregrosa, Alberto, Jorryt J Matthee, Gabriele Pezzulli, Tanya Urrutia, Max Gronke, Sara Mascia, Francesco D’Eugenio, et al. “A Weak Ly α Halo for an Extremely Bright Little Red Dot. Indications of Enshrouded Supermassive Black Hole Growth.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202555596\">https://doi.org/10.1051/0004-6361/202555596</a>.","mla":"Torralba Torregrosa, Alberto, et al. “A Weak Ly α Halo for an Extremely Bright Little Red Dot. Indications of Enshrouded Supermassive Black Hole Growth.” <i>Astronomy &#38; Astrophysics</i>, vol. 705, A147, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202555596\">10.1051/0004-6361/202555596</a>."},"intvolume":"       705","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"das_tickbox":"1","OA_place":"publisher","file":[{"file_size":2259914,"file_id":"21224","relation":"main_file","date_created":"2026-02-16T07:35:03Z","content_type":"application/pdf","creator":"dernst","access_level":"open_access","checksum":"3782e03bc0843438aae8487f6af779c5","date_updated":"2026-02-16T07:35:03Z","file_name":"2026_AstronomyAstrophysics_Torralba.pdf","success":1}],"article_processing_charge":"No","volume":705,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We thank the anonymous referee for constructive and useful comments. We thank Sebastiano Cantalupo for comments on the draft. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 114.27M6.001. 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. 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 #3516. MG thanks the Max Planck Society for support through the MPRG. FDE acknowledges support by the Science and Technology Facilities Council (STFC), by the ERC through Advanced Grant 695671 “QUENCH”, and by the UKRI Frontier Research grant RISEandFALL. TU acknowledges funding from the ERC-AdG grant SPECMAP-CGM, GA 101020943. GK acknowledges support from the MERAC foundation.","publisher":"EDP Sciences","OA_type":"diamond","author":[{"last_name":"Torralba Torregrosa","first_name":"Alberto","orcid":"0000-0001-5586-6950","id":"018f0249-0e87-11f0-b167-cbce08fbd541","full_name":"Torralba Torregrosa, Alberto"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"full_name":"Pezzulli, Gabriele","last_name":"Pezzulli","first_name":"Gabriele"},{"full_name":"Urrutia, Tanya","last_name":"Urrutia","first_name":"Tanya"},{"full_name":"Gronke, Max","first_name":"Max","last_name":"Gronke"},{"first_name":"Sara","last_name":"Mascia","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","full_name":"Mascia, Sara"},{"last_name":"D’Eugenio","first_name":"Francesco","full_name":"D’Eugenio, Francesco"},{"first_name":"Claudia","last_name":"Di Cesare","id":"2d002343-372f-11ef-98ec-a164d20427cb","full_name":"Di Cesare, Claudia"},{"full_name":"Eilers, Anna Christina","first_name":"Anna Christina","last_name":"Eilers"},{"full_name":"Greene, Jenny E.","first_name":"Jenny E.","last_name":"Greene"},{"full_name":"Iani, Edoardo","orcid":"0000-0001-8386-3546","first_name":"Edoardo","last_name":"Iani","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a"},{"last_name":"Ishikawa","first_name":"Yuzo","full_name":"Ishikawa, Yuzo"},{"first_name":"Ruari","last_name":"Mackenzie","full_name":"Mackenzie, Ruari"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"full_name":"Navarrete, Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","first_name":"Benjamín","last_name":"Navarrete"},{"full_name":"Kotiwale, Gauri","last_name":"Kotiwale","first_name":"Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875"}],"ddc":["520"],"date_updated":"2026-07-08T06:38:23Z","day":"14","oa":1,"year":"2026","status":"public","external_id":{"arxiv":["2505.09542"]},"doi":"10.1051/0004-6361/202555596","scopus_import":"1","type":"journal_article","language":[{"iso":"eng"}],"date_created":"2026-01-25T23:01:41Z","file_date_updated":"2026-02-16T07:35:03Z"},{"language":[{"iso":"eng"}],"file_date_updated":"2026-02-09T07:28:08Z","date_created":"2026-01-28T15:24:24Z","scopus_import":"1","doi":"10.1051/0004-6361/202553760","status":"public","external_id":{"arxiv":["2501.08268"]},"year":"2025","oa":1,"type":"journal_article","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 programs GTO 1243, ERS 1345, DDT 2750, and GTO 1180, 1181, 3215, 1210, 1286. 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 support from the INAF Large Grant 2022 “Extragalactic Surveys with JWST” (PI Pentericci). We acknowledge support from INAF Mini-grant “Reionization and Fundamental Cosmology with High-Redshift Galaxies” and from PRIN 2022 MUR project 2022CB3PJ3 - First Light And Galaxy aSsembly (FLAGS) funded by the European Union – Next Generation EU. RA acknowledges support of Grant PID2023-147386NB-I00 funded by MICIU/AEI/10.13039/501100011033 and by ERDF/EU, and the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/50110001103. The project that gave rise to these results received the support of a fellowship from the “la Caixa” Foundation (ID 100010434). The fellowship code is LCF/BQ/PR24/12050015. LC acknowledges support from grants PID2022-139567NB-I00 and PIB2021-127718NB-I00 funded by the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/10.13039/501100011033 and by “ERDF A way of making Europe”.","publisher":"EDP Sciences","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","day":"01","date_updated":"2026-02-09T07:33:46Z","ddc":["520"],"author":[{"full_name":"Mascia, Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","last_name":"Mascia","first_name":"Sara"},{"first_name":"L.","last_name":"Pentericci","full_name":"Pentericci, L."},{"full_name":"Llerena, M.","last_name":"Llerena","first_name":"M."},{"full_name":"Calabrò, A.","first_name":"A.","last_name":"Calabrò"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"last_name":"Flury","first_name":"S.","full_name":"Flury, S."},{"first_name":"F.","last_name":"Pacucci","full_name":"Pacucci, F."},{"full_name":"Jaskot, A.","first_name":"A.","last_name":"Jaskot"},{"first_name":"R. O.","last_name":"Amorín","full_name":"Amorín, R. O."},{"first_name":"R.","last_name":"Bhatawdekar","full_name":"Bhatawdekar, R."},{"first_name":"M.","last_name":"Castellano","full_name":"Castellano, M."},{"full_name":"Cleri, N.","last_name":"Cleri","first_name":"N."},{"last_name":"Costantin","first_name":"L.","full_name":"Costantin, L."},{"full_name":"Davis, K.","first_name":"K.","last_name":"Davis"},{"id":"2d002343-372f-11ef-98ec-a164d20427cb","last_name":"Di Cesare","first_name":"Claudia","full_name":"Di Cesare, Claudia"},{"last_name":"Dickinson","first_name":"M.","full_name":"Dickinson, M."},{"full_name":"Fontana, A.","first_name":"A.","last_name":"Fontana"},{"full_name":"Guo, Y.","first_name":"Y.","last_name":"Guo"},{"full_name":"Giavalisco, M.","first_name":"M.","last_name":"Giavalisco"},{"full_name":"Holwerda, B. W.","last_name":"Holwerda","first_name":"B. W."},{"full_name":"Hu, W.","first_name":"W.","last_name":"Hu"},{"last_name":"Huertas-Company","first_name":"M.","full_name":"Huertas-Company, M."},{"full_name":"Jung, Intae","first_name":"Intae","last_name":"Jung"},{"full_name":"Kartaltepe, J.","first_name":"J.","last_name":"Kartaltepe"},{"full_name":"Kashino, D.","last_name":"Kashino","first_name":"D."},{"last_name":"Koekemoer","first_name":"A. M.","full_name":"Koekemoer, A. M."},{"full_name":"Lucas, R. A.","last_name":"Lucas","first_name":"R. A."},{"full_name":"Lotz, J.","last_name":"Lotz","first_name":"J."},{"last_name":"Napolitano","first_name":"L.","full_name":"Napolitano, L."},{"full_name":"Jogee, S.","first_name":"S.","last_name":"Jogee"},{"full_name":"Wilkins, S.","first_name":"S.","last_name":"Wilkins"}],"OA_type":"diamond","article_processing_charge":"No","file":[{"file_name":"2025_AstronomyAstrophysics_Mascia.pdf","success":1,"content_type":"application/pdf","date_created":"2026-02-09T07:28:08Z","creator":"dernst","checksum":"990e384ca19e14b35296712d3b9e2919","access_level":"open_access","date_updated":"2026-02-09T07:28:08Z","relation":"main_file","file_id":"21166","file_size":9994234}],"OA_place":"publisher","volume":701,"DOAJ_listed":"1","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"intvolume":"       701","citation":{"ama":"Mascia S, Pentericci L, Llerena M, et al. Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe. <i>Astronomy &#38; Astrophysics</i>. 2025;701. doi:<a href=\"https://doi.org/10.1051/0004-6361/202553760\">10.1051/0004-6361/202553760</a>","ieee":"S. Mascia <i>et al.</i>, “Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe,” <i>Astronomy &#38; Astrophysics</i>, vol. 701. EDP Sciences, 2025.","apa":"Mascia, S., Pentericci, L., Llerena, M., Calabrò, A., Matthee, J. J., Flury, S., … Wilkins, S. (2025). Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202553760\">https://doi.org/10.1051/0004-6361/202553760</a>","short":"S. Mascia, L. Pentericci, M. Llerena, A. Calabrò, J.J. Matthee, S. Flury, F. Pacucci, A. Jaskot, R.O. Amorín, R. Bhatawdekar, M. Castellano, N. Cleri, L. Costantin, K. Davis, C. Di Cesare, M. Dickinson, A. Fontana, Y. Guo, M. Giavalisco, B.W. Holwerda, W. Hu, M. Huertas-Company, I. Jung, J. Kartaltepe, D. Kashino, A.M. Koekemoer, R.A. Lucas, J. Lotz, L. Napolitano, S. Jogee, S. Wilkins, Astronomy &#38; Astrophysics 701 (2025).","mla":"Mascia, Sara, et al. “Little Impact of Mergers and Galaxy Morphology on the Production and Escape of Ionizing Photons in the Early Universe.” <i>Astronomy &#38; Astrophysics</i>, vol. 701, A122, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202553760\">10.1051/0004-6361/202553760</a>.","chicago":"Mascia, Sara, L. Pentericci, M. Llerena, A. Calabrò, Jorryt J Matthee, S. Flury, F. Pacucci, et al. “Little Impact of Mergers and Galaxy Morphology on the Production and Escape of Ionizing Photons in the Early Universe.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202553760\">https://doi.org/10.1051/0004-6361/202553760</a>.","ista":"Mascia S, Pentericci L, Llerena M, Calabrò A, Matthee JJ, Flury S, Pacucci F, Jaskot A, Amorín RO, Bhatawdekar R, Castellano M, Cleri N, Costantin L, Davis K, Di Cesare C, Dickinson M, Fontana A, Guo Y, Giavalisco M, Holwerda BW, Hu W, Huertas-Company M, Jung I, Kartaltepe J, Kashino D, Koekemoer AM, Lucas RA, Lotz J, Napolitano L, Jogee S, Wilkins S. 2025. Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe. Astronomy &#38; Astrophysics. 701, A122."},"quality_controlled":"1","oa_version":"Published Version","article_number":"A122","arxiv":1,"title":"Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe","corr_author":"1","has_accepted_license":"1","publication":"Astronomy & Astrophysics","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"PlanS_conform":"1","month":"09","date_published":"2025-09-01T00:00:00Z","department":[{"_id":"JoMa"}],"abstract":[{"lang":"eng","text":"Compact, star-forming galaxies with high star formation rate surface densities (ΣSFR) are often efficient Lyman continuum (LyC) emitters at z ≤ 4.5, likely because intense stellar feedback creates low-density channels that allow photons to escape. Irregular or disturbed morphologies, such as those resulting from mergers, can also facilitate LyC escape by creating anisotropic gas distributions. We investigated the influence of galaxy morphology on LyC production and escape at redshifts 5 ≤ z ≤ 7 using observations from various James Webb Space Telescope (JWST) surveys. Our sample consists of 436 sources, which are predominantly low-mass (∼10^8.15 M\f), star-forming galaxies with ionizing photon efficiency (ξion) values consistent with canonical expectations. Since direct measurements of fesc are not possible during the Epoch of  Reionization (EoR), we predicted fesc for high-redshift galaxies by applying survival analysis to a subsample of LyC emitters from the Low-Redshift Lyman Continuum Survey (LzLCS), selected to be direct analogs of reionization-era galaxies. We find that these galaxies exhibit, on average, modest predicted escape fractions (∼0.04). In addition, we evaluated the correlation between morphological features and LyC emission. Our findings indicate that neither ξion nor the predicted fesc values show a significant correlation with the presence of merger signatures. This suggests that in low-mass galaxies at z ≥ 5, strong morphological disturbances are not the primary mechanism driving LyC emission and leakage. Instead, compactness and star formation activity likely play a more pivotal role in regulating LyC escape. "}],"tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"_id":"21060","article_type":"original","publication_status":"published"},{"date_created":"2026-01-28T15:25:42Z","file_date_updated":"2026-02-09T08:20:14Z","language":[{"iso":"eng"}],"type":"journal_article","year":"2025","oa":1,"status":"public","external_id":{"arxiv":["2412.02846"]},"doi":"10.3847/1538-4357/ade886","scopus_import":"1","author":[{"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":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"full_name":"Kotiwale, Gauri","last_name":"Kotiwale","first_name":"Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875"},{"last_name":"Furtak","first_name":"Lukas J.","full_name":"Furtak, Lukas J."},{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","last_name":"Kramarenko","orcid":"0000-0001-5346-6048","first_name":"Ivan","full_name":"Kramarenko, Ivan"},{"first_name":"Ruari","last_name":"Mackenzie","full_name":"Mackenzie, Ruari"},{"full_name":"Greene, Jenny","first_name":"Jenny","last_name":"Greene"},{"full_name":"Adamo, Angela","last_name":"Adamo","first_name":"Angela"},{"full_name":"Bouwens, Rychard J.","last_name":"Bouwens","first_name":"Rychard J."},{"full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","first_name":"Claudia","last_name":"Di Cesare"},{"first_name":"Anna-Christina","last_name":"Eilers","full_name":"Eilers, Anna-Christina"},{"full_name":"de Graaff, Anna","first_name":"Anna","last_name":"de Graaff"},{"full_name":"Heintz, Kasper E.","first_name":"Kasper E.","last_name":"Heintz"},{"last_name":"Kashino","first_name":"Daichi","full_name":"Kashino, Daichi"},{"first_name":"Michael V.","last_name":"Maseda","full_name":"Maseda, Michael V."},{"full_name":"Tacchella, Sandro","first_name":"Sandro","last_name":"Tacchella"},{"id":"018f0249-0e87-11f0-b167-cbce08fbd541","orcid":"0000-0001-5586-6950","first_name":"Alberto","last_name":"Torralba Torregrosa","full_name":"Torralba Torregrosa, Alberto"}],"OA_type":"gold","ddc":["520"],"day":"29","date_updated":"2026-02-09T08:22:01Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","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).","publisher":"IOP Publishing","DOAJ_listed":"1","volume":988,"OA_place":"publisher","file":[{"creator":"dernst","content_type":"application/pdf","date_created":"2026-02-09T08:20:14Z","date_updated":"2026-02-09T08:20:14Z","access_level":"open_access","checksum":"a49fbed72f2ff9c0b13129acb6f44f9d","success":1,"file_name":"2025_AstrophysicalJournal_Matthee.pdf","file_size":6237415,"relation":"main_file","file_id":"21168"}],"article_processing_charge":"Yes","quality_controlled":"1","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>.","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>.","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.","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.","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>","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>","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)."},"intvolume":"       988","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"publication":"The Astrophysical Journal","has_accepted_license":"1","corr_author":"1","arxiv":1,"title":"Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5","article_number":"246","oa_version":"Published Version","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"issue":"2","abstract":[{"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.","lang":"eng"}],"department":[{"_id":"JoMa"}],"month":"07","date_published":"2025-07-29T00:00:00Z","PlanS_conform":"1","project":[{"grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization"}],"publication_status":"published","article_type":"original","_id":"21062"},{"tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"date_published":"2025-02-01T00:00:00Z","month":"02","abstract":[{"lang":"eng","text":"Context. Recent observations suggest a significant and rapid buildup of dust in galaxies at high redshift (z > 4); this presents new challenges to our understanding of galaxy formation in the early Universe. Although our understanding of the physics of dust production and destruction in a galaxy’s interstellar medium (ISM) is improving, investigating the baryonic processes in the early universe remains a complex task owing to the inherent degeneracies in cosmological simulations and chemical evolution models.\r\nAims. In this work we characterized the evolution of 98 z ∼ 5 star-forming galaxies observed as part of the ALMA Large Program ALPINE by constraining the physical processes underpinning the gas and dust production, consumption, and destruction in their ISM.\r\nMethods. We made use of chemical evolution models to simultaneously reproduce the observed dust and gas content of our galaxies, obtained respectively from spectral energy distribution (SED) fitting and ionized carbon measurements. For each galaxy we constrained the initial gas mass, gas inflows and outflows, and efficiencies of dust growth and destruction. We tested these models with both the canonical Chabrier and a top-heavy initial mass function (IMF); the latter allowed rapid dust production on shorter timescales.\r\nResults. We successfully reproduced the gas and dust content in most of the older galaxies (≳600 Myr) regardless of the assumed IMF, predicting dust production primarily through Type II supernovae (SNe) and no dust growth in the ISM, as well as moderate inflow of primordial gas. In the case of intermediate-age galaxies (300−600 Myr), we reproduced the gas and dust content through Type II SNe and dust growth in ISM, though we observed an overprediction of dust mass in older galaxies, potentially indicating an unaccounted dust destruction mechanism and/or an overestimation of the observed dust masses. The number of young galaxies (≲300 Myr) reproduced, increases for models assuming top-heavy IMF but with maximal prescriptions of dust production. Galactic outflows are required (up to a mass-loading factor of 2) to reproduce the observed gas and dust mass, and to recover the decreasing trend of gas and dust over stellar mass with age. Assuming the Chabrier IMF, models are able to reproduce ∼65% of the total sample, while with top-heavy IMF the fraction increases to ∼93%, alleviating the tension between the observations and the models. Observations from the James Webb Space Telescope (JWST) will allow us to remove degeneracies in the diverse intrinsic properties of these galaxies (e.g., star formation histories and metallicity), thereby refining our models."}],"department":[{"_id":"JoMa"}],"publication_status":"published","article_type":"original","_id":"19070","intvolume":"       694","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"quality_controlled":"1","citation":{"ista":"Sawant P, Nanni A, Romano M, Donevski D, Bruzual G, Ysard N, Lemaux BC, Inami H, Calura F, Pozzi F, Małek K, Junais J, Boquien M, Faisst AL, Hamed M, Ginolfi M, Zamorani G, Lorenzon G, Molina J, Bardelli S, Ibar E, Vergani D, Di Cesare C, Béthermin M, Burgarella D, Cassata P, Dessauges-Zavadsky M, D’Onghia E, Dubois Y, Magdis GE, Mendez-Hernandez H. 2025. The ALPINE-ALMA [CII] survey: Unveiling the baryon evolution in the interstellar medium of z ∼ 5 star-forming galaxies. Astronomy &#38; Astrophysics. 694, A82.","chicago":"Sawant, P., A. Nanni, M. Romano, D. Donevski, G. Bruzual, N. Ysard, B. C. Lemaux, et al. “The ALPINE-ALMA [CII] Survey: Unveiling the Baryon Evolution in the Interstellar Medium of z ∼ 5 Star-Forming Galaxies.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202451542\">https://doi.org/10.1051/0004-6361/202451542</a>.","mla":"Sawant, P., et al. “The ALPINE-ALMA [CII] Survey: Unveiling the Baryon Evolution in the Interstellar Medium of z ∼ 5 Star-Forming Galaxies.” <i>Astronomy &#38; Astrophysics</i>, vol. 694, A82, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202451542\">10.1051/0004-6361/202451542</a>.","short":"P. Sawant, A. Nanni, M. Romano, D. Donevski, G. Bruzual, N. Ysard, B.C. Lemaux, H. Inami, F. Calura, F. Pozzi, K. Małek, J. Junais, M. Boquien, A.L. Faisst, M. Hamed, M. Ginolfi, G. Zamorani, G. Lorenzon, J. Molina, S. Bardelli, E. Ibar, D. Vergani, C. Di Cesare, M. Béthermin, D. Burgarella, P. Cassata, M. Dessauges-Zavadsky, E. D’Onghia, Y. Dubois, G.E. Magdis, H. Mendez-Hernandez, Astronomy &#38; Astrophysics 694 (2025).","ama":"Sawant P, Nanni A, Romano M, et al. The ALPINE-ALMA [CII] survey: Unveiling the baryon evolution in the interstellar medium of z ∼ 5 star-forming galaxies. <i>Astronomy &#38; Astrophysics</i>. 2025;694. doi:<a href=\"https://doi.org/10.1051/0004-6361/202451542\">10.1051/0004-6361/202451542</a>","ieee":"P. Sawant <i>et al.</i>, “The ALPINE-ALMA [CII] survey: Unveiling the baryon evolution in the interstellar medium of z ∼ 5 star-forming galaxies,” <i>Astronomy &#38; Astrophysics</i>, vol. 694. EDP Sciences, 2025.","apa":"Sawant, P., Nanni, A., Romano, M., Donevski, D., Bruzual, G., Ysard, N., … Mendez-Hernandez, H. (2025). The ALPINE-ALMA [CII] survey: Unveiling the baryon evolution in the interstellar medium of z ∼ 5 star-forming galaxies. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202451542\">https://doi.org/10.1051/0004-6361/202451542</a>"},"isi":1,"title":"The ALPINE-ALMA [CII] survey: Unveiling the baryon evolution in the interstellar medium of z ∼ 5 star-forming galaxies","publication":"Astronomy & Astrophysics","has_accepted_license":"1","oa_version":"Published Version","article_number":"A82","day":"01","ddc":["520"],"date_updated":"2026-02-16T12:08:24Z","OA_type":"diamond","author":[{"first_name":"P.","last_name":"Sawant","full_name":"Sawant, P."},{"full_name":"Nanni, A.","first_name":"A.","last_name":"Nanni"},{"full_name":"Romano, M.","last_name":"Romano","first_name":"M."},{"full_name":"Donevski, D.","first_name":"D.","last_name":"Donevski"},{"last_name":"Bruzual","first_name":"G.","full_name":"Bruzual, G."},{"full_name":"Ysard, N.","last_name":"Ysard","first_name":"N."},{"first_name":"B. C.","last_name":"Lemaux","full_name":"Lemaux, B. C."},{"last_name":"Inami","first_name":"H.","full_name":"Inami, H."},{"first_name":"F.","last_name":"Calura","full_name":"Calura, F."},{"last_name":"Pozzi","first_name":"F.","full_name":"Pozzi, F."},{"first_name":"K.","last_name":"Małek","full_name":"Małek, K."},{"first_name":"J.","last_name":"Junais","full_name":"Junais, J."},{"full_name":"Boquien, M.","last_name":"Boquien","first_name":"M."},{"first_name":"A. L.","last_name":"Faisst","full_name":"Faisst, A. L."},{"last_name":"Hamed","first_name":"M.","full_name":"Hamed, M."},{"last_name":"Ginolfi","first_name":"M.","full_name":"Ginolfi, M."},{"last_name":"Zamorani","first_name":"G.","full_name":"Zamorani, G."},{"first_name":"G.","last_name":"Lorenzon","full_name":"Lorenzon, G."},{"last_name":"Molina","first_name":"J.","full_name":"Molina, J."},{"full_name":"Bardelli, S.","first_name":"S.","last_name":"Bardelli"},{"full_name":"Ibar, E.","last_name":"Ibar","first_name":"E."},{"full_name":"Vergani, D.","first_name":"D.","last_name":"Vergani"},{"full_name":"Di Cesare, Claudia","last_name":"Di Cesare","first_name":"Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb"},{"first_name":"M.","last_name":"Béthermin","full_name":"Béthermin, M."},{"full_name":"Burgarella, D.","first_name":"D.","last_name":"Burgarella"},{"last_name":"Cassata","first_name":"P.","full_name":"Cassata, P."},{"first_name":"M.","last_name":"Dessauges-Zavadsky","full_name":"Dessauges-Zavadsky, M."},{"last_name":"D'Onghia","first_name":"E.","full_name":"D'Onghia, E."},{"full_name":"Dubois, Y.","last_name":"Dubois","first_name":"Y."},{"full_name":"Magdis, G. E.","last_name":"Magdis","first_name":"G. E."},{"last_name":"Mendez-Hernandez","first_name":"H.","full_name":"Mendez-Hernandez, H."}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We warmly thank the referee for her/his useful comments and suggestions that greatly improved the quality of our paper. P.S., A.N., and M.R. acknowledge support from the Narodowe Centrum Nauki (UMO2020/38/E/ST9/00077). M.R. acknowledges support from the Foundation for Polish Science (FNP) under the program START 063.2023. D.D. acknowledges support from the National Science Center (NCN) grant SONATA (UMO2020/39/D/ST9/00720). J. and K.M. are grateful for the support from the Polish National Science Centre via grant UMO-018/30/E/ST9/00082. J. acknowledges support from the European Union (MSCA EDUCADO, GA 101119830 and WIDERA ExGal-Twin, GA 101158446). M.B. gratefully acknowledges support from the ANID BASAL project FB210003 and from the FONDECYT regular grant 1211000. This work was supported by the French government through the France 2030 investment plan managed by the National Research Agency (ANR), as part of the Initiative of Excellence of Université Côte d’Azur under reference number ANR-15-IDEX-01. M.H. acknowledges support from the Polish National Science Center (UMO-2022/45/N/ST9/01336). E.I. acknowledges funding by ANID FONDECYT Regular 1221846. G.E.M. acknowledges the Villum Fonden research grant 13160 “Gas to stars, stars to dust: tracing star formation across cosmic time”, grant 37440, “The Hidden Cosmos”, and the Cosmic Dawn Center of Excellence funded by the Danish National Research Foundation under the grant No. 140.","publisher":"EDP Sciences","volume":694,"file":[{"file_size":7624067,"file_id":"19086","relation":"main_file","creator":"dernst","content_type":"application/pdf","date_created":"2025-02-25T07:05:19Z","date_updated":"2025-02-25T07:05:19Z","checksum":"792cbcda14148c352dc8c5a26058827d","access_level":"open_access","success":1,"file_name":"2025_AstronomyAstrophysics_Sawant.pdf"}],"article_processing_charge":"Yes","OA_place":"publisher","file_date_updated":"2025-02-25T07:05:19Z","date_created":"2025-02-23T23:01:56Z","language":[{"iso":"eng"}],"type":"journal_article","doi":"10.1051/0004-6361/202451542","scopus_import":"1","year":"2025","oa":1,"external_id":{"isi":["001414753300028"]},"status":"public"},{"language":[{"iso":"eng"}],"date_created":"2024-11-10T23:02:00Z","file_date_updated":"2024-11-11T08:54:11Z","year":"2024","oa":1,"status":"public","external_id":{"isi":["001332213700013"],"arxiv":["2401.03020"]},"doi":"10.1051/0004-6361/202449164","scopus_import":"1","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"EDP Sciences","acknowledgement":"The authors would like to thank the anonymous referee for the useful suggestions which improved this article. This paper is based on data obtained with the ALMA Observatory, under Large Program 2017.1.00428.L. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. CDC would like to thank the GESO group at the European Southern Observatory (ESO) for the useful discussions while preparing this manuscript. The simulated data underlying this article will be shared on reasonable request to the corresponding author. CDC acknowledged support from Sapienza University of Rome program “Bando per la mobilità individuale all’estero” (DR n.1607 del 14 June 2021) during the visiting period (June-November 2022) at ESO Garching, Germany. LG and RS acknowledge support from the PRIN 2022 MUR project 2022CB3PJ3 – First Light And Galaxy aSsembly (FLAGS) funded by the European Union – Next Generation EU, and from the Amaldi Research Center funded by the MIUR program “Dipartimento di Eccellenza” (CUP:B81I18001170001). MR acknowledges support from the Narodowe Centrum Nauki (UMO-2020/38/E/ST9/00077) and support from the Foundation for Polish Science (FNP) under the program START 063.2023. We have benefited from the publicly available software CASA and CARTA and programming language Python, including the numpy (https://numpy.org), matplotlib (https://matplotlib.org), scipy (https://scipy.org) and astropy (http://www.astropy.org) packages. ","author":[{"full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","first_name":"Claudia","last_name":"Di Cesare"},{"full_name":"Ginolfi, M.","first_name":"M.","last_name":"Ginolfi"},{"full_name":"Graziani, L.","last_name":"Graziani","first_name":"L."},{"full_name":"Schneider, R.","first_name":"R.","last_name":"Schneider"},{"last_name":"Romano","first_name":"M.","full_name":"Romano, M."},{"last_name":"Popping","first_name":"G.","full_name":"Popping, G."}],"OA_type":"hybrid","date_updated":"2026-07-08T06:44:39Z","ddc":["520"],"day":"01","OA_place":"publisher","file":[{"creator":"dernst","date_created":"2024-11-11T08:54:11Z","content_type":"application/pdf","date_updated":"2024-11-11T08:54:11Z","checksum":"24c65a64047aba156f39b01425269bdb","access_level":"open_access","success":1,"file_name":"2024_AstronomyAstrophysics_diCesare.pdf","file_size":8033864,"file_id":"18533","relation":"main_file"}],"article_processing_charge":"No","volume":690,"quality_controlled":"1","isi":1,"citation":{"ama":"Di Cesare C, Ginolfi M, Graziani L, Schneider R, Romano M, Popping G. Carbon envelopes around merging galaxies at z ~ 4.5. <i>Astronomy &#38; Astrophysics</i>. 2024;690. doi:<a href=\"https://doi.org/10.1051/0004-6361/202449164\">10.1051/0004-6361/202449164</a>","ieee":"C. Di Cesare, M. Ginolfi, L. Graziani, R. Schneider, M. Romano, and G. Popping, “Carbon envelopes around merging galaxies at z ~ 4.5,” <i>Astronomy &#38; Astrophysics</i>, vol. 690. EDP Sciences, 2024.","apa":"Di Cesare, C., Ginolfi, M., Graziani, L., Schneider, R., Romano, M., &#38; Popping, G. (2024). Carbon envelopes around merging galaxies at z ~ 4.5. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202449164\">https://doi.org/10.1051/0004-6361/202449164</a>","short":"C. Di Cesare, M. Ginolfi, L. Graziani, R. Schneider, M. Romano, G. Popping, Astronomy &#38; Astrophysics 690 (2024).","mla":"Di Cesare, Claudia, et al. “Carbon Envelopes around Merging Galaxies at z ~ 4.5.” <i>Astronomy &#38; Astrophysics</i>, vol. 690, A255, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202449164\">10.1051/0004-6361/202449164</a>.","chicago":"Di Cesare, Claudia, M. Ginolfi, L. Graziani, R. Schneider, M. Romano, and G. Popping. “Carbon Envelopes around Merging Galaxies at z ~ 4.5.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202449164\">https://doi.org/10.1051/0004-6361/202449164</a>.","ista":"Di Cesare C, Ginolfi M, Graziani L, Schneider R, Romano M, Popping G. 2024. Carbon envelopes around merging galaxies at z ~ 4.5. Astronomy &#38; Astrophysics. 690, A255."},"intvolume":"       690","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"das_tickbox":"1","article_number":"A255","oa_version":"Published Version","publication":"Astronomy & Astrophysics","has_accepted_license":"1","corr_author":"1","arxiv":1,"title":"Carbon envelopes around merging galaxies at z ~ 4.5","abstract":[{"text":"Context. Galaxies evolve through a dynamic exchange of material with their immediate surrounding environment, the so-called circumgalactic medium (CGM). Understanding the physics of gas flows and the nature of the CGM is fundamental to studying galaxy evolution, especially at 4 ≤ z ≤ 6 (i.e., after the Epoch of Reionization) when galaxies rapidly assembled their masses and reached their chemical maturity. Galactic outflows are predicted to enrich the CGM with metals, although it has also been suggested that gas stripping in systems undergoing a major merger may play a role.\r\n\r\nAims. In this work, we explore the metal enrichment of the medium around merging galaxies at z ∼ 4.5, observed by the ALMA Large Program to INvestigate [CII] at Early times (ALPINE). To do so, we study the nature of the [CII] 158 μm emission in the CGM around these systems, using simulations to help disentangle the mechanisms contributing to the CGM metal pollution.\r\n\r\nMethods. By adopting an updated classification of major merger systems in the ALPINE survey, we selected and analyzed merging galaxies whose components can be spatially and/or spectrally resolved in a robust way. This makes it possible to distinguish between the [CII] emission coming from the single components of the system and that coming from the system as a whole. We also made use of the dustyGadget cosmological simulation to select synthetic analogs of observed galaxies and guide the interpretation of the observational results.\r\n\r\nResults. We find a large diffuse [CII] envelope (≳20 kpc) embedding all the merging systems, with at least 25% of the total [CII] emission coming from the medium between the galaxies. Using predictions from dustyGadget, we suggest that this emission has a multi-fold nature, with dynamical interactions between galaxies playing a major role in stripping the gas and enriching the medium with heavy elements.","lang":"eng"}],"department":[{"_id":"JoMa"}],"date_published":"2024-10-01T00:00:00Z","month":"10","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_type":"original","_id":"18527","publication_status":"published"}]