[{"article_type":"original","_id":"21341","publication_status":"published","date_published":"2026-02-01T00:00:00Z","month":"02","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"PlanS_conform":"1","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"}],"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)"},"oa_version":"Published Version","article_number":"A165","corr_author":"1","title":"Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy","arxiv":1,"publication":"Astronomy & Astrophysics","has_accepted_license":"1","intvolume":"       706","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"quality_controlled":"1","citation":{"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).","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.","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>","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>","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>."},"file":[{"file_name":"2026_AstronomyAstrophysics_Kotiwale.pdf","success":1,"date_created":"2026-02-24T07:46:47Z","content_type":"application/pdf","creator":"dernst","access_level":"open_access","checksum":"6f5849d29ad43bee32f90152f6fc0294","date_updated":"2026-02-24T07:46:47Z","file_id":"21355","relation":"main_file","file_size":6531719}],"article_processing_charge":"No","OA_place":"publisher","DOAJ_listed":"1","volume":706,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"EDP Sciences","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).","date_updated":"2026-02-24T07:49:42Z","day":"01","ddc":["520"],"author":[{"full_name":"Kotiwale, Gauri","last_name":"Kotiwale","first_name":"Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Daichi","last_name":"Kashino","full_name":"Kashino, Daichi"},{"last_name":"Vijayan","first_name":"Aswin P.","full_name":"Vijayan, Aswin P."},{"last_name":"Torralba Torregrosa","first_name":"Alberto","orcid":"0000-0001-5586-6950","id":"018f0249-0e87-11f0-b167-cbce08fbd541","full_name":"Torralba Torregrosa, Alberto"},{"full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","first_name":"Claudia","last_name":"Di Cesare"},{"id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","last_name":"Iani","first_name":"Edoardo","orcid":"0000-0001-8386-3546","full_name":"Iani, Edoardo"},{"last_name":"Bordoloi","first_name":"Rongmon","full_name":"Bordoloi, Rongmon"},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"full_name":"Maseda, Michael V.","first_name":"Michael V.","last_name":"Maseda"},{"last_name":"Tacchella","first_name":"Sandro","full_name":"Tacchella, Sandro"},{"full_name":"Shivaei, Irene","first_name":"Irene","last_name":"Shivaei"},{"full_name":"Heintz, Kasper E.","last_name":"Heintz","first_name":"Kasper E."},{"full_name":"Danhaive, A. Lola","first_name":"A. Lola","last_name":"Danhaive"},{"full_name":"Mascia, Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","first_name":"Sara","last_name":"Mascia"},{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","last_name":"Kramarenko","first_name":"Ivan","orcid":"0000-0001-5346-6048","full_name":"Kramarenko, Ivan"},{"full_name":"Navarrete, Benjamín","last_name":"Navarrete","first_name":"Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148"},{"first_name":"Ruari","last_name":"Mackenzie","full_name":"Mackenzie, Ruari"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"}],"OA_type":"diamond","doi":"10.1051/0004-6361/202556597","scopus_import":"1","year":"2026","oa":1,"status":"public","external_id":{"arxiv":["2510.19959"]},"type":"journal_article","language":[{"iso":"eng"}],"file_date_updated":"2026-02-24T07:46:47Z","date_created":"2026-02-22T23:01:35Z"},{"date_updated":"2026-03-16T10:59:16Z","day":"01","ddc":["520"],"OA_type":"diamond","author":[{"full_name":"Torralba Torregrosa, Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","last_name":"Torralba Torregrosa","orcid":"0000-0001-5586-6950","first_name":"Alberto"},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"full_name":"Pezzulli, Gabriele","first_name":"Gabriele","last_name":"Pezzulli"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"full_name":"Ishikawa, Yuzo","last_name":"Ishikawa","first_name":"Yuzo"},{"full_name":"Brammer, Gabriel B.","first_name":"Gabriel B.","last_name":"Brammer"},{"full_name":"Chang, Seok Jun","last_name":"Chang","first_name":"Seok Jun"},{"first_name":"John","last_name":"Chisholm","full_name":"Chisholm, John"},{"first_name":"Anna","last_name":"De Graaff","full_name":"De Graaff, Anna"},{"full_name":"D’Eugenio, Francesco","first_name":"Francesco","last_name":"D’Eugenio"},{"id":"2d002343-372f-11ef-98ec-a164d20427cb","first_name":"Claudia","last_name":"Di Cesare","full_name":"Di Cesare, Claudia"},{"full_name":"Eilers, Anna Christina","first_name":"Anna Christina","last_name":"Eilers"},{"full_name":"Greene, Jenny E.","last_name":"Greene","first_name":"Jenny E."},{"full_name":"Gronke, Max","first_name":"Max","last_name":"Gronke"},{"last_name":"Iani","first_name":"Edoardo","orcid":"0000-0001-8386-3546","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","full_name":"Iani, Edoardo"},{"full_name":"Kokorev, Vasily","last_name":"Kokorev","first_name":"Vasily"},{"full_name":"Kotiwale, Gauri","first_name":"Gauri","last_name":"Kotiwale","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875"},{"full_name":"Kramarenko, Ivan","first_name":"Ivan","orcid":"0000-0001-5346-6048","last_name":"Kramarenko","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4"},{"full_name":"Ma, Yilun","last_name":"Ma","first_name":"Yilun"},{"last_name":"Mascia","first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","full_name":"Mascia, Sara"},{"full_name":"Navarrete, Benjamín","last_name":"Navarrete","first_name":"Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148"},{"full_name":"Nelson, Erica","last_name":"Nelson","first_name":"Erica"},{"first_name":"Pascal","last_name":"Oesch","full_name":"Oesch, Pascal"},{"full_name":"Simcoe, Robert A.","last_name":"Simcoe","first_name":"Robert A."},{"full_name":"Wuyts, Stijn","first_name":"Stijn","last_name":"Wuyts"}],"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.","publisher":"EDP Sciences","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","volume":707,"DOAJ_listed":"1","article_processing_charge":"No","file":[{"file_name":"2026_AstronomyAstrophysics_Torralba2.pdf","success":1,"content_type":"application/pdf","date_created":"2026-03-16T10:57:49Z","creator":"dernst","checksum":"fcab9cb3dcf1d68612e1fdc8191643c1","access_level":"open_access","date_updated":"2026-03-16T10:57:49Z","file_id":"21460","relation":"main_file","file_size":2510157}],"OA_place":"publisher","file_date_updated":"2026-03-16T10:57:49Z","date_created":"2026-03-15T23:01:36Z","language":[{"iso":"eng"}],"type":"journal_article","scopus_import":"1","doi":"10.1051/0004-6361/202557537","external_id":{"arxiv":["2510.00103"]},"status":"public","year":"2026","oa":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)"},"PlanS_conform":"1","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"month":"03","date_published":"2026-03-01T00:00:00Z","department":[{"_id":"JoMa"}],"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."}],"publication_status":"published","_id":"21451","article_type":"original","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"intvolume":"       707","citation":{"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>.","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>.","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.","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>","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)."},"quality_controlled":"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,"corr_author":"1","has_accepted_license":"1","publication":"Astronomy & Astrophysics","oa_version":"Published Version","article_number":"A75"},{"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)"},"abstract":[{"lang":"eng","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."}],"department":[{"_id":"JoMa"},{"_id":"GradSch"}],"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","publication_status":"published","article_type":"original","_id":"21452","quality_controlled":"1","citation":{"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).","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>","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.","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>.","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>."},"intvolume":"       707","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"publication":"Astronomy & Astrophysics","has_accepted_license":"1","corr_author":"1","arxiv":1,"title":"The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations","article_number":"A129","oa_version":"Published Version","author":[{"id":"2d002343-372f-11ef-98ec-a164d20427cb","last_name":"Di Cesare","first_name":"Claudia","full_name":"Di Cesare, Claudia"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"last_name":"Naidu","first_name":"Rohan P.","full_name":"Naidu, Rohan P."},{"full_name":"Torralba, Alberto","last_name":"Torralba","first_name":"Alberto"},{"id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","first_name":"Gauri","last_name":"Kotiwale","full_name":"Kotiwale, Gauri"},{"full_name":"Kramarenko, Ivan","first_name":"Ivan","orcid":"0000-0001-5346-6048","last_name":"Kramarenko","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4"},{"last_name":"Blaizot","first_name":"Jeremy","full_name":"Blaizot, Jeremy"},{"full_name":"Rosdahl, Joakim","first_name":"Joakim","last_name":"Rosdahl"},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","last_name":"Iani","first_name":"Edoardo","orcid":"0000-0001-8386-3546","full_name":"Iani, Edoardo"},{"first_name":"Angela","last_name":"Adamo","full_name":"Adamo, Angela"},{"full_name":"Covelo-Paz, Alba","first_name":"Alba","last_name":"Covelo-Paz"},{"first_name":"Lukas J.","last_name":"Furtak","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"},{"id":"aa14a535-50c9-11ef-b52e-e0c373d10148","last_name":"Navarrete","first_name":"Benjamín","full_name":"Navarrete, Benjamín"},{"full_name":"Oesch, Pascal A.","last_name":"Oesch","first_name":"Pascal A."},{"full_name":"Romano, Michael","last_name":"Romano","first_name":"Michael"},{"full_name":"Shivaei, Irene","last_name":"Shivaei","first_name":"Irene"},{"full_name":"Tacchella, Sandro","last_name":"Tacchella","first_name":"Sandro"}],"OA_type":"diamond","date_updated":"2026-03-16T10:52:44Z","ddc":["520"],"day":"01","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"EDP Sciences","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).","DOAJ_listed":"1","volume":707,"OA_place":"publisher","file":[{"relation":"main_file","file_id":"21459","file_size":1821411,"file_name":"2026_AstronomyAstrophysics_DiCesare.pdf","success":1,"date_created":"2026-03-16T10:48:07Z","content_type":"application/pdf","creator":"dernst","checksum":"c056b00ce7324849754521fde10fb7ca","access_level":"open_access","date_updated":"2026-03-16T10:48:07Z"}],"article_processing_charge":"No","date_created":"2026-03-15T23:01:36Z","file_date_updated":"2026-03-16T10:48:07Z","language":[{"iso":"eng"}],"type":"journal_article","year":"2026","oa":1,"status":"public","external_id":{"arxiv":["2510.19044"]},"doi":"10.1051/0004-6361/202557790","scopus_import":"1"},{"language":[{"iso":"eng"}],"date_created":"2026-01-25T23:01:41Z","file_date_updated":"2026-02-16T07:35:03Z","oa":1,"year":"2026","status":"public","external_id":{"arxiv":["2505.09542"]},"doi":"10.1051/0004-6361/202555596","scopus_import":"1","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"EDP Sciences","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.","author":[{"full_name":"Torralba Torregrosa, Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","first_name":"Alberto","orcid":"0000-0001-5586-6950","last_name":"Torralba Torregrosa"},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee"},{"full_name":"Pezzulli, Gabriele","last_name":"Pezzulli","first_name":"Gabriele"},{"full_name":"Urrutia, Tanya","first_name":"Tanya","last_name":"Urrutia"},{"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"},{"full_name":"D’Eugenio, Francesco","last_name":"D’Eugenio","first_name":"Francesco"},{"last_name":"Di Cesare","first_name":"Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","full_name":"Di Cesare, Claudia"},{"first_name":"Anna Christina","last_name":"Eilers","full_name":"Eilers, Anna Christina"},{"full_name":"Greene, Jenny E.","last_name":"Greene","first_name":"Jenny E."},{"id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","orcid":"0000-0001-8386-3546","first_name":"Edoardo","last_name":"Iani","full_name":"Iani, Edoardo"},{"last_name":"Ishikawa","first_name":"Yuzo","full_name":"Ishikawa, Yuzo"},{"last_name":"Mackenzie","first_name":"Ruari","full_name":"Mackenzie, Ruari"},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."},{"full_name":"Navarrete, Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","first_name":"Benjamín","last_name":"Navarrete"},{"full_name":"Kotiwale, Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","last_name":"Kotiwale","first_name":"Gauri"}],"OA_type":"diamond","ddc":["520"],"date_updated":"2026-07-08T06:38:23Z","day":"14","OA_place":"publisher","file":[{"relation":"main_file","file_id":"21224","file_size":2259914,"success":1,"file_name":"2026_AstronomyAstrophysics_Torralba.pdf","date_updated":"2026-02-16T07:35:03Z","checksum":"3782e03bc0843438aae8487f6af779c5","access_level":"open_access","creator":"dernst","content_type":"application/pdf","date_created":"2026-02-16T07:35:03Z"}],"article_processing_charge":"No","volume":705,"quality_controlled":"1","citation":{"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>","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>","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.","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).","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>.","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."},"intvolume":"       705","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"das_tickbox":"1","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","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"}],"date_published":"2026-01-14T00:00:00Z","month":"01","PlanS_conform":"1","project":[{"grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization"}],"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":"21045","publication_status":"published"},{"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"intvolume":"       994","citation":{"short":"P. Rinaldi, P.G. Pérez-González, G.H. Rieke, J. Lyu, F. D’Eugenio, Z. Wu, S. Carniani, T.J. Looser, I. Shivaei, L.A. Boogaard, T. Diaz-Santos, L. Colina, G. Östlin, S. Alberts, J. Álvarez-Márquez, M. Annuziatella, M. Aravena, R. Bhatawdekar, A.J. Bunker, K.I. Caputi, S. Charlot, A. Crespo Gómez, M. Curti, A. Eckart, S. Gillman, K. Hainline, N. Kumari, J. Hjorth, E. Iani, H. Inami, Z. Ji, B.D. Johnson, G.C. Jones, Á. Labiano, R. Maiolino, J. Melinder, T. Moutard, F. Peissker, M. Rieke, B. Robertson, J. Scholtz, S. Tacchella, P.P. Van Der Werf, F. Walter, C.C. Williams, C. Willott, J. Witstok, H. Übler, Y. Zhu, The Astrophysical Journal 994 (2025).","ama":"Rinaldi P, Pérez-González PG, Rieke GH, et al. Deciphering the nature of Virgil: An obscured active galactic nucleus lurking within an apparently normal Lyα emitter during cosmic reionization. <i>The Astrophysical Journal</i>. 2025;994(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae089c\">10.3847/1538-4357/ae089c</a>","apa":"Rinaldi, P., Pérez-González, P. G., Rieke, G. H., Lyu, J., D’Eugenio, F., Wu, Z., … Zhu, Y. (2025). Deciphering the nature of Virgil: An obscured active galactic nucleus lurking within an apparently normal Lyα emitter during cosmic reionization. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae089c\">https://doi.org/10.3847/1538-4357/ae089c</a>","ieee":"P. Rinaldi <i>et al.</i>, “Deciphering the nature of Virgil: An obscured active galactic nucleus lurking within an apparently normal Lyα emitter during cosmic reionization,” <i>The Astrophysical Journal</i>, vol. 994, no. 1. IOP Publishing, 2025.","ista":"Rinaldi P, Pérez-González PG, Rieke GH, Lyu J, D’Eugenio F, Wu Z, Carniani S, Looser TJ, Shivaei I, Boogaard LA, Diaz-Santos T, Colina L, Östlin G, Alberts S, Álvarez-Márquez J, Annuziatella M, Aravena M, Bhatawdekar R, Bunker AJ, Caputi KI, Charlot S, Crespo Gómez A, Curti M, Eckart A, Gillman S, Hainline K, Kumari N, Hjorth J, Iani E, Inami H, Ji Z, Johnson BD, Jones GC, Labiano Á, Maiolino R, Melinder J, Moutard T, Peissker F, Rieke M, Robertson B, Scholtz J, Tacchella S, Van Der Werf PP, Walter F, Williams CC, Willott C, Witstok J, Übler H, Zhu Y. 2025. Deciphering the nature of Virgil: An obscured active galactic nucleus lurking within an apparently normal Lyα emitter during cosmic reionization. The Astrophysical Journal. 994(1), 86.","chicago":"Rinaldi, Pierluigi, Pablo G. Pérez-González, George H. Rieke, Jianwei Lyu, Francesco D’Eugenio, Zihao Wu, Stefano Carniani, et al. “Deciphering the Nature of Virgil: An Obscured Active Galactic Nucleus Lurking within an Apparently Normal Lyα Emitter during Cosmic Reionization.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/ae089c\">https://doi.org/10.3847/1538-4357/ae089c</a>.","mla":"Rinaldi, Pierluigi, et al. “Deciphering the Nature of Virgil: An Obscured Active Galactic Nucleus Lurking within an Apparently Normal Lyα Emitter during Cosmic Reionization.” <i>The Astrophysical Journal</i>, vol. 994, no. 1, 86, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae089c\">10.3847/1538-4357/ae089c</a>."},"quality_controlled":"1","oa_version":"Published Version","article_number":"86","title":"Deciphering the nature of Virgil: An obscured active galactic nucleus lurking within an apparently normal Lyα emitter during cosmic reionization","has_accepted_license":"1","publication":"The Astrophysical Journal","PlanS_conform":"1","month":"11","date_published":"2025-11-20T00:00:00Z","department":[{"_id":"JoMa"}],"abstract":[{"lang":"eng","text":"We present a comprehensive analysis of the MIRI Extremely Red Object Virgil, a Lyα emitter at zspec = 6.6379 ± 0.0035 with the photometric properties of a Little Red Dot. Leveraging new JWST/MIRI imaging from the MIDIS and PAHSPECS programs, we confirm Virgil’s extraordinary nature among galaxies in JADES/GOODS-South, exhibiting a strikingly red NIRCam-to-MIRI color (F444W–F1500W = 2.84 ± 0.04 mag). Deep NIRSpec/PRISM spectroscopy from the OASIS program offers key insights into the host galaxy, revealing properties of an average star-forming galaxy during Cosmic Reionization, such as a subsolar metallicity, low-to-moderate dust content, and a relatively high ionization parameter and electron temperature. By estimating the star formation rate of Virgil from UV and Hα, we find evidence that the galaxy is either entering or fading out of a bursty episode. Although line-ratio diagnostics employed at high z would classify Virgil as an active galactic nucleus (AGN), this classification becomes ambiguous once redshift evolution is considered. Nonetheless, Virgil occupies the same parameter space as recently confirmed AGNs at similar redshifts. The new deep MIRI data at 15 μm reinforce the AGN nature of Virgil, as inferred from multiple spectral energy distribution (SED) fitting codes. Virgil’s rising infrared SED and UV excess resemble those of Dust-Obscured Galaxies (DOGs) studied with Spitzer at Cosmic Noon, particularly blue-excess HotDOGs. Our results highlight the need for a multiwavelength approach incorporating MIRI to uncover such extreme sources at z ≳ 6 and to shed light on the interplay between galaxy evolution and early black hole growth during Cosmic Reionization."}],"issue":"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)"},"_id":"21727","article_type":"original","publication_status":"published","language":[{"iso":"eng"}],"file_date_updated":"2026-04-13T07:53:00Z","date_created":"2026-04-12T22:01:53Z","scopus_import":"1","doi":"10.3847/1538-4357/ae089c","status":"public","oa":1,"year":"2025","type":"journal_article","publisher":"IOP Publishing","acknowledgement":"The authors are deeply grateful to Antonello Calabrò for valuable insights on CLOUDY and pyCloudy, and for publicly sharing their SFG and AGN models, which were used as a reference to verify the consistency of our photoionization models. The authors also thank Adam Carnall for insightful input on bagpipes and for assistance with the implementation of the two-population model adopted in this work. Finally, they also thank Camilla Pacifici, Vasily Kokorev, and Cristian Vignali for their insightful discussions.\r\n\r\nThis work is based on observations made with the NASA/ESA/CSA JWST. The data were obtained from the Mikulski Archive for Space Telescopes (MAST) 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 programs GTO #1180, GO #1210, GTO#1283, GO #1963, GO #1895, GO# 3215, and GO#6511.\r\n\r\nThe authors acknowledge the FRESCO, JEMS, and #3215 teams led by co-PIs P. Oesch, C. C. Williams, M. Maseda, D. Eisenstein, and R. Maiolino for developing their observing program with a zero-exclusive-access period. Processing for the JADES NIRCam data release was performed on the lux cluster at the University of California, Santa Cruz, funded by NSF MRI grant AST 1828315. Also based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 526555. The data presented in this article were obtained from MAST at the Space Telescope Science Institute. The specific observations analyzed can be accessed via doi: 10.17909/1rq3-8048 P. Oesch & D. Magee (2023), C. Williams et al. (2023), G. Illingworth (2015), and M. Rieke et al. (2023).\r\n\r\nA.J.B. 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).\r\n\r\nP.G.P.-G. acknowledges support from grant PID2022-139567NB-I00 funded by the Spanish Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033, FEDER, UE.\r\n\r\nB.E.R. acknowledges support from the NIRCam Science Team contract to the University of Arizona, NAS5-02015, and JWST Program 3215.\r\n\r\nS.T. acknowledges support by the Royal Society Research Grant G125142.\r\n\r\nThe research of C.C.W. 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.\r\n\r\nJ.W. gratefully acknowledges support from the Cosmic Dawn Center through the DAWN Fellowship. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140.\r\n\r\nY.Z., Z.J., and P.L. gratefully acknowledge the JWST/NIRCam contract to the University of Arizona NAS5-02015.\r\n\r\nThe work of G.H.R. and P.L. was also supported by grant 80NSSC18K0555, from the NASA Goddard Space Flight Center to the University of Arizona.\r\n\r\nH.Ü. acknowledges funding by the European Union (ERC APEX, 101164796). Views and opinions expressed are however those of the authors only and do not necessarily reflect those of the European Union or the European Research Council Executive Agency. Neither the European Union nor the granting authority can be held responsible for them.\r\n\r\nG.C.J. acknowledges support by the Science and Technology Facilities Council (STFC), ERC Advanced grant 695671 “QUENCH.”\r\n\r\nA.C.G. acknowledges support by JWST contract B0215/JWST-GO-02926.\r\n\r\nG.O. acknowledges support from the Swedish National Space Agency (SNSA).\r\n\r\nH.I. acknowledges support from JSPS KAKENHI grant No. JP21H01129.\r\n\r\nM.A. gratefully acknowledges support from ANID Basal Project FB210003 and ANID MILENIO NCN2024_112.\r\n\r\nT.D.S. acknowledges the research project was supported by the Hellenic Foundation for Research and Innovation (HFRI) under the “2nd Call for HFRI Research Projects to Support Faculty Members and Researchers” (project No.: 03382).\r\n\r\nR.M. 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. R.M. also acknowledges funding from a research professorship from the Royal Society.\r\n\r\nI.S. acknowledges funding from the Atraccíon de Talento grant No. 2022-T1/TIC-20472 of the Comunidad de Madrid, Spain, and the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant No. 101117541, DistantDust).\r\n\r\nK.I.C. acknowledges funding from the Dutch Research Council (NWO) through the award of the Vici grant VI.C.212.036.\r\n\r\nFacilities: HST - Hubble Space Telescope satellite, JWST. -\r\n\r\nSoftware: Astropy (Astropy Collaboration et al. 2022), Bagpipes (A. C. Carnall et al. 2019), MSAEXP (G. Brammer 2023) NumPy (C. R. Harris et al. 2020), pandas (The pandas development team 2024) Photutils (L. Bradley et al. 2016), TOPCAT (M. Taylor 2022).","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","day":"20","ddc":["520"],"date_updated":"2026-04-13T07:54:11Z","author":[{"full_name":"Rinaldi, Pierluigi","last_name":"Rinaldi","first_name":"Pierluigi"},{"full_name":"Pérez-González, Pablo G.","first_name":"Pablo G.","last_name":"Pérez-González"},{"full_name":"Rieke, George H.","first_name":"George H.","last_name":"Rieke"},{"full_name":"Lyu, Jianwei","first_name":"Jianwei","last_name":"Lyu"},{"first_name":"Francesco","last_name":"D’Eugenio","full_name":"D’Eugenio, Francesco"},{"full_name":"Wu, Zihao","last_name":"Wu","first_name":"Zihao"},{"last_name":"Carniani","first_name":"Stefano","full_name":"Carniani, Stefano"},{"first_name":"Tobias J.","last_name":"Looser","full_name":"Looser, Tobias J."},{"full_name":"Shivaei, Irene","first_name":"Irene","last_name":"Shivaei"},{"full_name":"Boogaard, Leindert A.","last_name":"Boogaard","first_name":"Leindert A."},{"last_name":"Diaz-Santos","first_name":"Tanio","full_name":"Diaz-Santos, Tanio"},{"last_name":"Colina","first_name":"Luis","full_name":"Colina, Luis"},{"first_name":"Göran","last_name":"Östlin","full_name":"Östlin, Göran"},{"first_name":"Stacey","last_name":"Alberts","full_name":"Alberts, Stacey"},{"full_name":"Álvarez-Márquez, Javier","first_name":"Javier","last_name":"Álvarez-Márquez"},{"last_name":"Annuziatella","first_name":"Marianna","full_name":"Annuziatella, Marianna"},{"last_name":"Aravena","first_name":"Manuel","full_name":"Aravena, Manuel"},{"full_name":"Bhatawdekar, Rachana","first_name":"Rachana","last_name":"Bhatawdekar"},{"last_name":"Bunker","first_name":"Andrew J.","full_name":"Bunker, Andrew J."},{"full_name":"Caputi, Karina I.","last_name":"Caputi","first_name":"Karina I."},{"full_name":"Charlot, Stéphane","first_name":"Stéphane","last_name":"Charlot"},{"full_name":"Crespo Gómez, Alejandro","first_name":"Alejandro","last_name":"Crespo Gómez"},{"full_name":"Curti, Mirko","last_name":"Curti","first_name":"Mirko"},{"last_name":"Eckart","first_name":"Andreas","full_name":"Eckart, Andreas"},{"first_name":"Steven","last_name":"Gillman","full_name":"Gillman, Steven"},{"full_name":"Hainline, Kevin","last_name":"Hainline","first_name":"Kevin"},{"full_name":"Kumari, Nimisha","first_name":"Nimisha","last_name":"Kumari"},{"last_name":"Hjorth","first_name":"Jens","full_name":"Hjorth, Jens"},{"full_name":"Iani, Edoardo","last_name":"Iani","first_name":"Edoardo","orcid":"0000-0001-8386-3546","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a"},{"full_name":"Inami, Hanae","last_name":"Inami","first_name":"Hanae"},{"full_name":"Ji, Zhiyuan","last_name":"Ji","first_name":"Zhiyuan"},{"full_name":"Johnson, Benjamin D.","last_name":"Johnson","first_name":"Benjamin D."},{"first_name":"Gareth C.","last_name":"Jones","full_name":"Jones, Gareth C."},{"full_name":"Labiano, Álvaro","last_name":"Labiano","first_name":"Álvaro"},{"first_name":"Roberto","last_name":"Maiolino","full_name":"Maiolino, Roberto"},{"full_name":"Melinder, Jens","last_name":"Melinder","first_name":"Jens"},{"full_name":"Moutard, Thibaud","first_name":"Thibaud","last_name":"Moutard"},{"full_name":"Peissker, Florian","last_name":"Peissker","first_name":"Florian"},{"full_name":"Rieke, Marcia","last_name":"Rieke","first_name":"Marcia"},{"first_name":"Brant","last_name":"Robertson","full_name":"Robertson, Brant"},{"last_name":"Scholtz","first_name":"Jan","full_name":"Scholtz, Jan"},{"last_name":"Tacchella","first_name":"Sandro","full_name":"Tacchella, Sandro"},{"full_name":"Van Der Werf, Paul P.","last_name":"Van Der Werf","first_name":"Paul P."},{"full_name":"Walter, Fabian","first_name":"Fabian","last_name":"Walter"},{"full_name":"Williams, Christina C.","last_name":"Williams","first_name":"Christina C."},{"full_name":"Willott, Chris","last_name":"Willott","first_name":"Chris"},{"full_name":"Witstok, Joris","first_name":"Joris","last_name":"Witstok"},{"first_name":"Hannah","last_name":"Übler","full_name":"Übler, Hannah"},{"last_name":"Zhu","first_name":"Yongda","full_name":"Zhu, Yongda"}],"OA_type":"gold","article_processing_charge":"Yes","file":[{"creator":"dernst","date_created":"2026-04-13T07:53:00Z","content_type":"application/pdf","date_updated":"2026-04-13T07:53:00Z","checksum":"5d13b0ad3e9f56cbe29c5de0ba5757c8","access_level":"open_access","success":1,"file_name":"2025_AstrophysicalJournal_Rinaldi.pdf","file_size":10298729,"file_id":"21731","relation":"main_file"}],"OA_place":"publisher","volume":994,"DOAJ_listed":"1"},{"article_type":"original","_id":"19845","publication_status":"published","abstract":[{"text":"Context. The recently launched James Webb Space Telescope (JWST) is opening new observing windows on the distant Universe. Among JWST’s instruments, the Mid Infrared Instrument (MIRI) offers the unique capability of imaging observations at wavelengths of λ > 5 μm. This enables unique access to the rest frame near-infrared (NIR, λ ≥ 1 μm) emission from galaxies at redshifts of z > 4 and the visual (λ ≳ 5000 Å) rest frame for z > 9. We report here on the guaranteed time observations (GTO), from the MIRI European Consortium, of the Hubble Ultra Deep Field (HUDF), forming the MIRI Deep Imaging Survey (MIDIS), consisting of an on source integration time of ∼41 hours in the MIRI/F560W (5.6 μm) filter. The F560W filter was selected since it would produce the deepest data in terms of AB magnitudes in a given time. To our knowledge, this constitutes the longest single filter exposure obtained with JWST of an extragalactic field as of yet.\r\nAims. The HUDF is one of the most observed extragalactic fields, with extensive multi-wavelength coverage, where (before JWST) galaxies up to z ∼ 7 have been confirmed, and at z > 10 suggested, from HST photometry. We aim to characterise the galaxy population in HUDF at 5.6 μm, enabling studies such as: the rest frame NIR morphologies for galaxies at z ≲ 4.6, probing mature stellar populations and emission lines in z > 6 sources, intrinsically red and dusty galaxies, and active galactic nuclei (AGNs) and their host galaxies at intermediate redshifts.\r\n\r\nMethods. We reduced the MIRI data using the official JWST pipeline, augmented by in-house custom scripts. We measured the noise characteristics of the resulting image. Galaxy photometry was obtained, and photometric redshifts were estimated for sources with available multi-wavelength photometry (and compared to spectroscopic redshifts when available).\r\n\r\nResults. Over the deepest part of our image, the 5σ point source limit is 28.65 mag AB (12.6 nJy), ∼0.35 mag better than predicted by the JWST exposure time calculator. We find ∼2500 sources, the overwhelming majority of which are distant galaxies, but we note that spurious sources likely remain at faint magnitudes due to imperfect cosmic ray rejection in the JWST pipeline. More than 500 galaxies with available spectroscopic redshifts, up to z ≈ 11, have been identified, the majority of which are at z < 6. More than 1000 galaxies have reliable photometric redshift estimates, of which ∼25 are at 6 < z < 12. The point spread function in the F560W filter has a full width at half maximum (FWHM) of ≈0.2″ (corresponding to 1.4 kpc at z = 4), allowing the NIR rest frame morphologies and stellar mass distributions to be resolved for z < 4.5. Moreover, > 100 objects with very red NIRCam vs MIRI (3.6–5.6 μm > 1 mag) colours have been found, suggestive of dusty or old stellar populations at high redshifts.\r\n\r\nConclusions. We conclude that MIDIS surpasses preflight expectations and that deep MIRI imaging has great potential to characterise the galaxy population from cosmic noon to dawn.","lang":"eng"}],"department":[{"_id":"JoMa"}],"month":"04","date_published":"2025-04-01T00:00:00Z","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":"A57","oa_version":"Published Version","publication":"Astronomy & Astrophysics","has_accepted_license":"1","arxiv":1,"title":"MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey description and early results for the galaxy population detected at 5.6 µm","quality_controlled":"1","isi":1,"citation":{"mla":"Östlin, Göran, et al. “MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey Description and Early Results for the Galaxy Population Detected at 5.6 Μm.” <i>Astronomy &#38; Astrophysics</i>, vol. 696, A57, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202451723\">10.1051/0004-6361/202451723</a>.","chicago":"Östlin, Göran, Pablo G. Pérez-González, Jens Melinder, Steven Gillman, Edoardo Iani, Luca Costantin, Leindert A. Boogaard, et al. “MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey Description and Early Results for the Galaxy Population Detected at 5.6 Μm.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202451723\">https://doi.org/10.1051/0004-6361/202451723</a>.","ista":"Östlin G, Pérez-González PG, Melinder J, Gillman S, Iani E, Costantin L, Boogaard LA, Rinaldi P, Colina L, Nørgaard-Nielsen HU, Dicken D, Greve TR, Wright G, Alonso-Herrero A, Álvarez-Márquez J, Annunziatella M, Bik A, Bosman SEI, Caputi KI, Gomez AC, Eckart A, Garcia-Marin M, Hjorth J, Ilbert O, Jermann I, Kendrew S, Labiano A, Langeroodi D, Le Fevre O, Libralato M, Meyer RA, Moutard T, Peissker F, Pye JP, Tikkanen TV, Topinka M, Walter F, Ward M, Van Der Werf P, Van Dishoeck EF, Güdel M, Henning T, Lagage PO, Ray TP, Vandenbussche B. 2025. MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey description and early results for the galaxy population detected at 5.6 µm. Astronomy &#38; Astrophysics. 696, A57.","apa":"Östlin, G., Pérez-González, P. G., Melinder, J., Gillman, S., Iani, E., Costantin, L., … Vandenbussche, B. (2025). MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey description and early results for the galaxy population detected at 5.6 µm. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202451723\">https://doi.org/10.1051/0004-6361/202451723</a>","ieee":"G. Östlin <i>et al.</i>, “MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey description and early results for the galaxy population detected at 5.6 µm,” <i>Astronomy &#38; Astrophysics</i>, vol. 696. EDP Sciences, 2025.","ama":"Östlin G, Pérez-González PG, Melinder J, et al. MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey description and early results for the galaxy population detected at 5.6 µm. <i>Astronomy &#38; Astrophysics</i>. 2025;696. doi:<a href=\"https://doi.org/10.1051/0004-6361/202451723\">10.1051/0004-6361/202451723</a>","short":"G. Östlin, P.G. Pérez-González, J. Melinder, S. Gillman, E. Iani, L. Costantin, L.A. Boogaard, P. Rinaldi, L. Colina, H.U. Nørgaard-Nielsen, D. Dicken, T.R. Greve, G. Wright, A. Alonso-Herrero, J. Álvarez-Márquez, M. Annunziatella, A. Bik, S.E.I. Bosman, K.I. Caputi, A.C. Gomez, A. Eckart, M. Garcia-Marin, J. Hjorth, O. Ilbert, I. Jermann, S. Kendrew, A. Labiano, D. Langeroodi, O. Le Fevre, M. Libralato, R.A. Meyer, T. Moutard, F. Peissker, J.P. Pye, T.V. Tikkanen, M. Topinka, F. Walter, M. Ward, P. Van Der Werf, E.F. Van Dishoeck, M. Güdel, T. Henning, P.O. Lagage, T.P. Ray, B. Vandenbussche, Astronomy &#38; Astrophysics 696 (2025)."},"intvolume":"       696","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"OA_place":"publisher","file":[{"success":1,"file_name":"2025_AstronomyAstrophysics_Oestlin.pdf","creator":"dernst","date_created":"2025-06-23T07:46:01Z","content_type":"application/pdf","date_updated":"2025-06-23T07:46:01Z","checksum":"67600eba8bda24987a130ac334f10456","access_level":"open_access","file_id":"19865","relation":"main_file","file_size":15858045}],"article_processing_charge":"Yes","volume":696,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"EDP Sciences","acknowledgement":"We dedicate this paper to the memory of our deceased and much valued MIRI-EC team members Hans Ulrik Nørgaard-Nielsen and Olivier Le Fèvre, both of whom played a central role in defining the MIDIS project. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The work presented is the effort of the entire MIRI team and the enthusiasm within the MIRI partnership is a significant factor in its success. The following National and International Funding Agencies funded and supported the MIRI development: NASA; ESA; Belgian Science Policy Office (BELSPO); Centre Nationale d’Etudes Spatiales (CNES); Danish National Space Centre; Deutsches Zentrum fur Luftund Raumfahrt (DLR); Enterprise Ireland; Ministerio De Economia y Competividad; Netherlands Research School for Astronomy (NOVA); Netherlands Organisation for Scientific Research (NWO); Science and Technology Facilities Council; Swiss Space Office; Swedish National Space Agency (SNSA); and UK Space Agency. MIRI drew on the scientific and technical expertise of the following organizations: Ames Research Center, USA; Airbus Defence and Space, UK; CEAIrfu, Saclay, France; Centre Spatial de Liège, Belgium; Consejo Superior de Investigaciones Cientficas, Spain; Carl Zeiss Optronics, Germany; Chalmers University of Technology, Sweden; Danish Space Research Institute, Denmark; Dublin Institute for Advanced Studies, Ireland; European Space Agency, Netherlands; ETCA, Belgium; ETH Zurich, Switzerland; Goddard Space Flight Center, USA; Institute d’Astrophysique Spatiale, France; Instituto Nacional de Técnica Aeroespacial,Spain; Institute for Astronomy, Edinburgh, UK; Jet Propulsion Laboratory, USA; Laboratoire d’Astrophysique de Marseille (LAM), France; Leiden University, Netherlands; Lockheed Advanced Technology Center (USA); NOVA Opt-IR group at Dwingeloo, Netherlands; Northrop Grumman, USA; Max Planck Institut f ür Astronomie (MPIA), Heidelberg, Germany; Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique (LESIA), France; Paul Scherrer Institut, Switzerland; Raytheon Vision Systems, USA; RUAG Aerospace, Switzerland; Rutherford Appleton Laboratory (RAL Space), UK; Space Telescope Science Institute, USA; Stockholm University, Sweden; Toegepast- Natuurwetenschappelijk Onderzoek (TNOTPD), Netherlands; UK Astronomy Technology Centre, UK; University College London, UK; University of Amsterdam, Netherlands; University of Arizona, USA; University of Cardiff, UK; University of Cologne, Germany; University of Ghent; University of Groningen, Netherlands; University of Leicester, UK; University of Leuven, Belgium; Utah State University, USA. Additional acknowledgements related to specific grants: G.Ö., J.M. and A.B. acknowledges funding from the Swedish National Space Administration (SNSA). P.G.P.-G. acknowledges support from grant PID2022-139567NB-I00 funded by Spanish Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033, FEDER Una manera de hacer Europa. This work was supported by research grants (VIL16599,VIL54489) from VILLUM FONDEN. L.C. and J.A.-M. acknowledge support by grant PIB2021-127718NB-100 from the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/10.13039/501100011033 and by “ERDF A way of making Europe”. M.A. acknowledges financial support from Comunidad de Madrid under Atracción de Talento grant 2020-T2/TIC-19971. J.P.P. and T.V.T. acknowledge financial support from the UK Science and Technology Facilities Council, and the UK Space Agency. A.A.-H. acknowledges financial support from grant PID2021-124665NB-I00 funded by MCIN/AEI/10.13039/501100011033 and by “ERDF A way of making Europe”. E.I. and K.I.C. acknowledge funding from the Netherlands Research School for Astronomy (NOVA). K.I.C. acknowledges funding from the Dutch Research Council (NWO) through the award of the Vici Grant VI.C.212.036. RAM acknowledges support from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. The paper uses JWST data from programme #1283, obtained from the Barbara Mikulski Archive for Space Telescopes at the Space Telescope Science Institute (STScI). For the purpose of open access, the authors have applied a Creative Commons Attribution (CC BY) licence to the Author Accepted Manuscript version arising from this submission.","OA_type":"diamond","author":[{"full_name":"Östlin, Göran","last_name":"Östlin","first_name":"Göran"},{"first_name":"Pablo G.","last_name":"Pérez-González","full_name":"Pérez-González, Pablo G."},{"last_name":"Melinder","first_name":"Jens","full_name":"Melinder, Jens"},{"full_name":"Gillman, Steven","last_name":"Gillman","first_name":"Steven"},{"full_name":"Iani, Edoardo","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","last_name":"Iani","first_name":"Edoardo","orcid":"0000-0001-8386-3546"},{"full_name":"Costantin, Luca","first_name":"Luca","last_name":"Costantin"},{"full_name":"Boogaard, Leindert A.","last_name":"Boogaard","first_name":"Leindert A."},{"full_name":"Rinaldi, Pierluigi","first_name":"Pierluigi","last_name":"Rinaldi"},{"first_name":"Luis","last_name":"Colina","full_name":"Colina, Luis"},{"full_name":"Nørgaard-Nielsen, Hans Ulrik","first_name":"Hans Ulrik","last_name":"Nørgaard-Nielsen"},{"full_name":"Dicken, Daniel","first_name":"Daniel","last_name":"Dicken"},{"first_name":"Thomas R.","last_name":"Greve","full_name":"Greve, Thomas R."},{"full_name":"Wright, Gillian","first_name":"Gillian","last_name":"Wright"},{"full_name":"Alonso-Herrero, Almudena","last_name":"Alonso-Herrero","first_name":"Almudena"},{"full_name":"Álvarez-Márquez, Javier","first_name":"Javier","last_name":"Álvarez-Márquez"},{"full_name":"Annunziatella, Marianna","last_name":"Annunziatella","first_name":"Marianna"},{"last_name":"Bik","first_name":"Arjan","full_name":"Bik, Arjan"},{"full_name":"Bosman, Sarah E.I.","first_name":"Sarah E.I.","last_name":"Bosman"},{"full_name":"Caputi, Karina I.","first_name":"Karina I.","last_name":"Caputi"},{"first_name":"Alejandro Crespo","last_name":"Gomez","full_name":"Gomez, Alejandro Crespo"},{"last_name":"Eckart","first_name":"Andreas","full_name":"Eckart, Andreas"},{"first_name":"Macarena","last_name":"Garcia-Marin","full_name":"Garcia-Marin, Macarena"},{"last_name":"Hjorth","first_name":"Jens","full_name":"Hjorth, Jens"},{"full_name":"Ilbert, Olivier","first_name":"Olivier","last_name":"Ilbert"},{"full_name":"Jermann, Iris","last_name":"Jermann","first_name":"Iris"},{"last_name":"Kendrew","first_name":"Sarah","full_name":"Kendrew, Sarah"},{"last_name":"Labiano","first_name":"Alvaro","full_name":"Labiano, Alvaro"},{"full_name":"Langeroodi, Danial","first_name":"Danial","last_name":"Langeroodi"},{"full_name":"Le Fevre, Olivier","last_name":"Le Fevre","first_name":"Olivier"},{"full_name":"Libralato, Mattia","first_name":"Mattia","last_name":"Libralato"},{"first_name":"Romain A.","last_name":"Meyer","full_name":"Meyer, Romain A."},{"first_name":"Thibaud","last_name":"Moutard","full_name":"Moutard, Thibaud"},{"full_name":"Peissker, Florian","first_name":"Florian","last_name":"Peissker"},{"first_name":"John P.","last_name":"Pye","full_name":"Pye, John P."},{"full_name":"Tikkanen, Tuomo V.","last_name":"Tikkanen","first_name":"Tuomo V."},{"full_name":"Topinka, Martin","last_name":"Topinka","first_name":"Martin"},{"full_name":"Walter, Fabian","first_name":"Fabian","last_name":"Walter"},{"last_name":"Ward","first_name":"Martin","full_name":"Ward, Martin"},{"first_name":"Paul","last_name":"Van Der Werf","full_name":"Van Der Werf, Paul"},{"last_name":"Van Dishoeck","first_name":"Ewine F.","full_name":"Van Dishoeck, Ewine F."},{"last_name":"Güdel","first_name":"Manuel","full_name":"Güdel, Manuel"},{"full_name":"Henning, Thomas","first_name":"Thomas","last_name":"Henning"},{"full_name":"Lagage, Pierre Olivier","first_name":"Pierre Olivier","last_name":"Lagage"},{"last_name":"Ray","first_name":"Tom P.","full_name":"Ray, Tom P."},{"first_name":"Bart","last_name":"Vandenbussche","full_name":"Vandenbussche, Bart"}],"date_updated":"2026-02-16T12:10:36Z","day":"01","ddc":["520"],"year":"2025","oa":1,"external_id":{"isi":["001459780300005"],"arxiv":["2411.19686 "]},"status":"public","doi":"10.1051/0004-6361/202451723","scopus_import":"1","type":"journal_article","language":[{"iso":"eng"}],"date_created":"2025-06-15T22:01:30Z","file_date_updated":"2025-06-23T07:46:01Z"},{"oa_version":"Published Version","article_number":"160","arxiv":1,"title":"MIDIS: MIRI uncovers Virgil, the first Little Red Dot with clear detection of its host galaxy at z ≃ 6.6","publication":"The Astrophysical Journal","has_accepted_license":"1","intvolume":"       989","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"quality_controlled":"1","citation":{"short":"E. Iani, P. Rinaldi, K.I. Caputi, M. Annunziatella, D. Langeroodi, J. Melinder, P.G. Pérez-González, J. Álvarez-Márquez, L.A. Boogaard, S.E.I. Bosman, L. Costantin, T. Moutard, L. Colina, G. Östlin, T.R. Greve, G. Wright, A. Alonso-Herrero, A. Bik, S. Gillman, A. Crespo Gómez, J. Hjorth, S. Kendrew, A. Labiano, J.P. Pye, T.V. Tikkanen, F. Walter, M. Güdel, T. Henning, P.P. Van Der Werf, The Astrophysical Journal 989 (2025).","ama":"Iani E, Rinaldi P, Caputi KI, et al. MIDIS: MIRI uncovers Virgil, the first Little Red Dot with clear detection of its host galaxy at z ≃ 6.6. <i>The Astrophysical Journal</i>. 2025;989(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ade5a6\">10.3847/1538-4357/ade5a6</a>","apa":"Iani, E., Rinaldi, P., Caputi, K. I., Annunziatella, M., Langeroodi, D., Melinder, J., … Van Der Werf, P. P. (2025). MIDIS: MIRI uncovers Virgil, the first Little Red Dot with clear detection of its host galaxy at z ≃ 6.6. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ade5a6\">https://doi.org/10.3847/1538-4357/ade5a6</a>","ieee":"E. Iani <i>et al.</i>, “MIDIS: MIRI uncovers Virgil, the first Little Red Dot with clear detection of its host galaxy at z ≃ 6.6,” <i>The Astrophysical Journal</i>, vol. 989, no. 2. IOP Publishing, 2025.","ista":"Iani E, Rinaldi P, Caputi KI, Annunziatella M, Langeroodi D, Melinder J, Pérez-González PG, Álvarez-Márquez J, Boogaard LA, Bosman SEI, Costantin L, Moutard T, Colina L, Östlin G, Greve TR, Wright G, Alonso-Herrero A, Bik A, Gillman S, Crespo Gómez A, Hjorth J, Kendrew S, Labiano A, Pye JP, Tikkanen TV, Walter F, Güdel M, Henning T, Van Der Werf PP. 2025. MIDIS: MIRI uncovers Virgil, the first Little Red Dot with clear detection of its host galaxy at z ≃ 6.6. The Astrophysical Journal. 989(2), 160.","mla":"Iani, Edoardo, et al. “MIDIS: MIRI Uncovers Virgil, the First Little Red Dot with Clear Detection of Its Host Galaxy at z ≃ 6.6.” <i>The Astrophysical Journal</i>, vol. 989, no. 2, 160, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/ade5a6\">10.3847/1538-4357/ade5a6</a>.","chicago":"Iani, Edoardo, Pierluigi Rinaldi, Karina I. Caputi, Marianna Annunziatella, Danial Langeroodi, Jens Melinder, Pablo G. Pérez-González, et al. “MIDIS: MIRI Uncovers Virgil, the First Little Red Dot with Clear Detection of Its Host Galaxy at z ≃ 6.6.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/ade5a6\">https://doi.org/10.3847/1538-4357/ade5a6</a>."},"isi":1,"article_type":"original","_id":"20217","publication_status":"published","month":"08","date_published":"2025-08-20T00:00:00Z","PlanS_conform":"1","abstract":[{"lang":"eng","text":"We present Virgil, a Mid-Infrared Instrument (MIRI) extremely red object detected with the F1000W filter as part of the MIRI Deep Imaging Survey observations of the Hubble Ultra Deep Field. Virgil is an Lyα emitter (LAE) at zspec = 6.6312 ± 0.0019 (from the Very Large Telescope/MUSE) with a rest-frame UV-to-optical spectral energy distribution (SED) typical of LAEs at similar redshifts. However, MIRI observations reveal an unexpected extremely red color at rest-frame near-infrared (NIR) wavelengths, F444W − F1000W = 2.33 ± 0.06. Such a steep\r\nrise in the NIR, completely missed without MIRI imaging, is poorly reproduced by models including only stellar populations and hints toward the presence of an active galactic nucleus, although alternative explanations such as extreme dust obscuration and strong nebular continuum and emission lines contribution due to young stellar ages cannot be completely ruled out. According to the shape of its overall SED, Virgil belongs to the recently discovered\r\npopulation of little red dots but displays an extended rest-frame UV-optical wavelength morphology following a 2DSérsic profile with an average index of n = 0.93+0.85_0.31 and re = 0.49+0.05_0.11  pkpc. Only at MIRI wavelengths, Virgil is unresolved due to the coarser point-spread function. This discovery demonstrates the crucial importance of deep MIRI surveys to reveal the true nature and properties of high-z galaxies that otherwise would be misinterpreted and raises the question of how common Virgil-like objects could be in the early Universe."}],"department":[{"_id":"JoMa"}],"issue":"2","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)"},"doi":"10.3847/1538-4357/ade5a6","scopus_import":"1","oa":1,"year":"2025","external_id":{"arxiv":["2406.18207"],"isi":["001548132000001"]},"status":"public","type":"journal_article","language":[{"iso":"eng"}],"file_date_updated":"2025-09-02T06:40:23Z","date_created":"2025-08-24T22:01:29Z","file":[{"content_type":"application/pdf","date_created":"2025-09-02T06:40:23Z","creator":"dernst","checksum":"92196e8352dddb1f305c253da1996ab6","access_level":"open_access","date_updated":"2025-09-02T06:40:23Z","file_name":"2025_AstrophysicalJour_Iani.pdf","success":1,"file_size":5474992,"relation":"main_file","file_id":"20268"}],"article_processing_charge":"Yes","OA_place":"publisher","DOAJ_listed":"1","volume":989,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"IOP Publishing","acknowledgement":"The authors thank R. Cooper, G. Yang, V. Kokorev, D. Wen, C. Williams, and H. Übler for useful discussions and comments.\r\nE.I. and K.I.C. acknowledge funding from the Netherlands Research School for Astronomy (NOVA). K.I.C. acknowledges funding from the Dutch Research Council (NWO) through the award of the Vici grant VI.C.212.036. A.A.-H. acknowledges support from grant PID2021-124665NB-I00 funded by MCIN/AEI/10.13039/ 501100011033 and by “ERDF A way of making Europe.” P.G.P.-G. acknowledges support from grant PID2022-139567NB-I00 funded by the Spanish Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033, FEDER Una manera de hacer Europa. J.A.-M., A.C.-G., and L.C. acknowledge support by grant PIB2021-127718NB-100 from the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/10.13039/501100011033 and by “ERDF A way of making Europe.” L.C. thanks the support from the Cosmic Dawn Center received during visits to DAWN as an international associate. L.C. acknowledges support by grants PIB2021-127718NB-100 and PID2022-139567NB-I00 from the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/10.13039/501100011033 and by “ERDF A way of making Europe.” T.R.G. acknowledges support from the Carlsberg Foundation (grant No. CF20-0534). S.G. acknowledges financial support from the Cosmic Dawn Center (DAWN), funded by the Danish National Research Foundation (DNRF) under grant No. 140. This work was supported by research grants (VIL16599, VIL54489) from VILLUM FONDEN. J.P.P. and T.V.T. acknowledge financial support from the UK Science and Technology Facilities Council and the UK Space Agency.\r\n\r\nThis work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the MAST 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 GO #1963, GO #1895, and GTO #1283. The authors acknowledge the team led by co-PIs: C. Williams, M. Maseda, and S. Tacchella, and PI P. Oesch, for developing their respective observing programs with a zero-exclusive-access period. Also based on observations made with the NASA/ESA HST obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. The work presented here is the effort of the entire MIRI team, and the enthusiasm within the MIRI partnership is a significant factor in its success. MIRI draws on the scientific and technical expertise of the following organizations: Ames Research Center, USA; Airbus Defence and Space, UK; CEA-Irfu, Saclay, France; Centre Spatial de Liège, Belgium; Consejo Superior de Investigaciones Científicas, Spain; Carl Zeiss Optronics, Germany; Chalmers University of Technology, Sweden; Danish Space Research Institute, Denmark; Dublin Institute for Advanced Studies, Ireland; European Space Agency, Netherlands; ETCA, Belgium; ETH Zurich, Switzerland; Goddard Space Flight Center, USA; Institute d’Astrophysique Spatiale, France; Instituto Nacional de Técnica Aeroespacial, Spain; Institute for Astronomy, Edinburgh, UK; Jet Propulsion Laboratory, USA; Laboratoire d’Astrophysique de Marseille (LAM), France; Leiden University, Netherlands; Lockheed Advanced Technology Center (USA); NOVA Opt-IR group at Dwingeloo, Netherlands; Northrop Grumman, USA; Max-Planck Institut für Astronomie (MPIA), Heidelberg, Germany; Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique (LESIA), France; Paul Scherrer Institut, Switzerland; Raytheon Vision Systems, USA; RUAG Aerospace, Switzerland; Rutherford Appleton Laboratory (RAL Space), UK; Space Telescope Science Institute, USA; Toegepast-Natuurwetenschappelijk Onderzoek (TNO-TPD), Netherlands; UK Astronomy Technology Centre, UK; University College London, UK; University of Amsterdam, Netherlands; University of Arizona, USA; University of Cardiff, UK; University of Cologne, Germany; University of Ghent; University of Groningen, Netherlands; University of Leicester, UK; University of Leuven, Belgium; University of Stockholm, Sweden; Utah State University, USA.\r\nFor the purpose of open access, the author has applied a Creative Commons Attribution (CC BY) licence to the Author Accepted Manuscript version arising from this submission.","date_updated":"2026-02-16T12:43:12Z","ddc":["520"],"day":"20","OA_type":"gold","author":[{"full_name":"Iani, Edoardo","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","first_name":"Edoardo","orcid":"0000-0001-8386-3546","last_name":"Iani"},{"last_name":"Rinaldi","first_name":"Pierluigi","full_name":"Rinaldi, Pierluigi"},{"last_name":"Caputi","first_name":"Karina I.","full_name":"Caputi, Karina I."},{"last_name":"Annunziatella","first_name":"Marianna","full_name":"Annunziatella, Marianna"},{"full_name":"Langeroodi, Danial","last_name":"Langeroodi","first_name":"Danial"},{"full_name":"Melinder, Jens","first_name":"Jens","last_name":"Melinder"},{"full_name":"Pérez-González, Pablo G.","first_name":"Pablo G.","last_name":"Pérez-González"},{"full_name":"Álvarez-Márquez, Javier","first_name":"Javier","last_name":"Álvarez-Márquez"},{"last_name":"Boogaard","first_name":"Leindert A.","full_name":"Boogaard, Leindert A."},{"full_name":"Bosman, Sarah E.I.","first_name":"Sarah E.I.","last_name":"Bosman"},{"first_name":"Luca","last_name":"Costantin","full_name":"Costantin, Luca"},{"first_name":"Thibaud","last_name":"Moutard","full_name":"Moutard, Thibaud"},{"full_name":"Colina, Luis","last_name":"Colina","first_name":"Luis"},{"last_name":"Östlin","first_name":"Göran","full_name":"Östlin, Göran"},{"full_name":"Greve, Thomas R.","first_name":"Thomas R.","last_name":"Greve"},{"first_name":"Gillian","last_name":"Wright","full_name":"Wright, Gillian"},{"first_name":"Almudena","last_name":"Alonso-Herrero","full_name":"Alonso-Herrero, Almudena"},{"full_name":"Bik, Arjan","last_name":"Bik","first_name":"Arjan"},{"first_name":"Steven","last_name":"Gillman","full_name":"Gillman, Steven"},{"last_name":"Crespo Gómez","first_name":"Alejandro","full_name":"Crespo Gómez, Alejandro"},{"full_name":"Hjorth, Jens","last_name":"Hjorth","first_name":"Jens"},{"last_name":"Kendrew","first_name":"Sarah","full_name":"Kendrew, Sarah"},{"full_name":"Labiano, Alvaro","first_name":"Alvaro","last_name":"Labiano"},{"full_name":"Pye, John P.","first_name":"John P.","last_name":"Pye"},{"full_name":"Tikkanen, Tuomo V.","first_name":"Tuomo V.","last_name":"Tikkanen"},{"last_name":"Walter","first_name":"Fabian","full_name":"Walter, Fabian"},{"full_name":"Güdel, Manuel","last_name":"Güdel","first_name":"Manuel"},{"full_name":"Henning, Thomas","last_name":"Henning","first_name":"Thomas"},{"last_name":"Van Der Werf","first_name":"Paul P.","full_name":"Van Der Werf, Paul P."}]},{"volume":702,"file":[{"file_id":"20600","relation":"main_file","file_size":5107702,"success":1,"file_name":"2025_AstronomyAstrophysics_Annunziatella.pdf","date_updated":"2025-11-04T09:36:30Z","access_level":"open_access","checksum":"0cd0c3fc75b7f6589088a2b7bd60c0ed","creator":"dernst","content_type":"application/pdf","date_created":"2025-11-04T09:36:30Z"}],"article_processing_charge":"No","OA_place":"publisher","day":"24","date_updated":"2026-02-16T12:14:12Z","ddc":["520"],"OA_type":"diamond","author":[{"full_name":"Annunziatella, M.","last_name":"Annunziatella","first_name":"M."},{"last_name":"P’Erez-Gonz’Alez","first_name":"P. G.","full_name":"P’Erez-Gonz’Alez, P. G."},{"full_name":"Álvarez-Márquez, J.","first_name":"J.","last_name":"Álvarez-Márquez"},{"last_name":"Costantin","first_name":"L.","full_name":"Costantin, L."},{"orcid":"0000-0001-8386-3546","first_name":"Edoardo","last_name":"Iani","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","full_name":"Iani, Edoardo"},{"last_name":"Labiano","first_name":"Unknown","full_name":"Labiano, Unknown"},{"last_name":"Rinaldi","first_name":"P.","full_name":"Rinaldi, P."},{"full_name":"Boogaard, L.","last_name":"Boogaard","first_name":"L."},{"full_name":"Meyer, R. A.","first_name":"R. A.","last_name":"Meyer"},{"first_name":"G.","last_name":"Östlin","full_name":"Östlin, G."},{"first_name":"L.","last_name":"Colina","full_name":"Colina, L."},{"full_name":"Melinder, J.","first_name":"J.","last_name":"Melinder"},{"full_name":"Jermann, I.","first_name":"I.","last_name":"Jermann"},{"full_name":"Gillman, S.","first_name":"S.","last_name":"Gillman"},{"full_name":"Langeroodi, D.","last_name":"Langeroodi","first_name":"D."},{"last_name":"Hjorth","first_name":"J.","full_name":"Hjorth, J."},{"full_name":"Alonso-Herrero, A.","first_name":"A.","last_name":"Alonso-Herrero"},{"full_name":"Eckart, A.","last_name":"Eckart","first_name":"A."},{"full_name":"Walter, F.","first_name":"F.","last_name":"Walter"},{"full_name":"Van Der Werf, P. P.","last_name":"Van Der Werf","first_name":"P. P."},{"full_name":"Bik, A.","first_name":"A.","last_name":"Bik"},{"full_name":"Peißker, F.","first_name":"F.","last_name":"Peißker"},{"full_name":"Caputi, K. I.","first_name":"K. I.","last_name":"Caputi"},{"full_name":"García-Marín, M.","first_name":"M.","last_name":"García-Marín"},{"first_name":"G.","last_name":"Wright","full_name":"Wright, G."},{"first_name":"T. R.","last_name":"Greve","full_name":"Greve, T. R."}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"EDP Sciences","acknowledgement":"MA acknowledges financial support from Comunidad de Madrid under Atracción de Talento grant 2020-T2/TIC-19971. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Centro de Astrobiología (CAB/INTA), partnered with the University of California Observatories at Santa Cruz (UCO/Lick,UCSC). 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”. This work is based on observations made with the NASA/ ESA/CSA JWST. The data were obtained from the Mikulski Archive for Space Telescopes (MAST) 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.","type":"journal_article","doi":"10.1051/0004-6361/202453298","scopus_import":"1","year":"2025","oa":1,"status":"public","external_id":{"arxiv":["2508.16951"],"isi":["001600932400021"]},"file_date_updated":"2025-11-04T09:36:30Z","date_created":"2025-11-02T23:01:34Z","language":[{"iso":"eng"}],"publication_status":"published","article_type":"original","_id":"20589","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":"2025-10-24T00:00:00Z","month":"10","PlanS_conform":"1","abstract":[{"lang":"eng","text":"Context. This paper investigates the star formation histories (SFHs) of a sample of massive galaxies (M⋆ ≥ 1010 M⊙) in the redshift range 1 < z < 4.5.\r\nMethods. We analyzed spectro-photometric data, combining broadband photometry from HST and JWST with low-resolution grism spectroscopy from JWST/NIRISS, obtained as part of the MIRI Deep Imaging Survey program. SFHs were derived through spectral energy distribution fitting using two independent codes, BAGPIPES and synthesizer, under various SFH assumptions. This approach enables a comprehensive assessment of the biases introduced by different modeling choices.\r\nResults. The inclusion of NIRISS spectroscopy, even with its low resolution, significantly improves constraints on key physical parameters, such as the mass-weighted stellar age (tM) and formation redshift (zform), by narrowing their posterior distributions. The massive galaxies in our sample exhibit rapid stellar mass assembly, forming 50% of their mass between 3 ≤ z ≤ 9. The highest inferred formation redshifts are compatible with elevated star formation efficiencies (ϵ) at early epochs. Nonparametric SFHs generally imply an earlier and slower mass assembly compared to parametric forms, highlighting the sensitivity of inferred formation timescales to the chosen SFH model–particularly for galaxies at z < 2. We find that quiescent galaxies are, on average, older (tM ∼ 1.1 Gyr) and assembled more rapidly at earlier times than their star-forming counterparts. These findings support the “downsizing” scenario, in which more massive and passive systems form earlier and more efficiently."}],"department":[{"_id":"JoMa"}],"arxiv":1,"title":"MIDIS: Unveiling the star formation history in massive galaxies at 1 < z < 4.5 with spectro-photometric analysis","publication":"Astronomy & Astrophysics","has_accepted_license":"1","oa_version":"Published Version","article_number":"A224","intvolume":"       702","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"quality_controlled":"1","citation":{"short":"M. Annunziatella, P.G. P’Erez-Gonz’Alez, J. Álvarez-Márquez, L. Costantin, E. Iani, U. Labiano, P. Rinaldi, L. Boogaard, R.A. Meyer, G. Östlin, L. Colina, J. Melinder, I. Jermann, S. Gillman, D. Langeroodi, J. Hjorth, A. Alonso-Herrero, A. Eckart, F. Walter, P.P. Van Der Werf, A. Bik, F. Peißker, K.I. Caputi, M. García-Marín, G. Wright, T.R. Greve, Astronomy &#38; Astrophysics 702 (2025).","ieee":"M. Annunziatella <i>et al.</i>, “MIDIS: Unveiling the star formation history in massive galaxies at 1 &#60; z &#60; 4.5 with spectro-photometric analysis,” <i>Astronomy &#38; Astrophysics</i>, vol. 702. EDP Sciences, 2025.","apa":"Annunziatella, M., P’Erez-Gonz’Alez, P. G., Álvarez-Márquez, J., Costantin, L., Iani, E., Labiano, U., … Greve, T. R. (2025). MIDIS: Unveiling the star formation history in massive galaxies at 1 &#60; z &#60; 4.5 with spectro-photometric analysis. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202453298\">https://doi.org/10.1051/0004-6361/202453298</a>","ama":"Annunziatella M, P’Erez-Gonz’Alez PG, Álvarez-Márquez J, et al. MIDIS: Unveiling the star formation history in massive galaxies at 1 &#60; z &#60; 4.5 with spectro-photometric analysis. <i>Astronomy &#38; Astrophysics</i>. 2025;702. doi:<a href=\"https://doi.org/10.1051/0004-6361/202453298\">10.1051/0004-6361/202453298</a>","ista":"Annunziatella M, P’Erez-Gonz’Alez PG, Álvarez-Márquez J, Costantin L, Iani E, Labiano U, Rinaldi P, Boogaard L, Meyer RA, Östlin G, Colina L, Melinder J, Jermann I, Gillman S, Langeroodi D, Hjorth J, Alonso-Herrero A, Eckart A, Walter F, Van Der Werf PP, Bik A, Peißker F, Caputi KI, García-Marín M, Wright G, Greve TR. 2025. MIDIS: Unveiling the star formation history in massive galaxies at 1 &#60; z &#60; 4.5 with spectro-photometric analysis. Astronomy &#38; Astrophysics. 702, A224.","chicago":"Annunziatella, M., P. G. P’Erez-Gonz’Alez, J. Álvarez-Márquez, L. Costantin, Edoardo Iani, Unknown Labiano, P. Rinaldi, et al. “MIDIS: Unveiling the Star Formation History in Massive Galaxies at 1 &#60; z &#60; 4.5 with Spectro-Photometric Analysis.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202453298\">https://doi.org/10.1051/0004-6361/202453298</a>.","mla":"Annunziatella, M., et al. “MIDIS: Unveiling the Star Formation History in Massive Galaxies at 1 &#60; z &#60; 4.5 with Spectro-Photometric Analysis.” <i>Astronomy &#38; Astrophysics</i>, vol. 702, A224, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202453298\">10.1051/0004-6361/202453298</a>."},"isi":1}]