[{"date_updated":"2026-02-16T07:46:53Z","publisher":"EDP Sciences","article_type":"original","publication_status":"published","status":"public","file":[{"file_name":"2026_AstronomyAstrophysics_Torralba.pdf","file_id":"21224","success":1,"checksum":"3782e03bc0843438aae8487f6af779c5","date_created":"2026-02-16T07:35:03Z","relation":"main_file","access_level":"open_access","creator":"dernst","file_size":2259914,"content_type":"application/pdf","date_updated":"2026-02-16T07:35:03Z"}],"year":"2026","PlanS_conform":"1","day":"14","author":[{"orcid":"0000-0001-5586-6950","id":"018f0249-0e87-11f0-b167-cbce08fbd541","full_name":"Torralba Torregrosa, Alberto","last_name":"Torralba Torregrosa","first_name":"Alberto"},{"first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"full_name":"Pezzulli, Gabriele","last_name":"Pezzulli","first_name":"Gabriele"},{"full_name":"Urrutia, Tanya","first_name":"Tanya","last_name":"Urrutia"},{"full_name":"Gronke, Max","last_name":"Gronke","first_name":"Max"},{"first_name":"Sara","last_name":"Mascia","full_name":"Mascia, Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29"},{"full_name":"D’Eugenio, Francesco","last_name":"D’Eugenio","first_name":"Francesco"},{"first_name":"Claudia","last_name":"Di Cesare","full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb"},{"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","full_name":"Iani, Edoardo","orcid":"0000-0001-8386-3546","last_name":"Iani","first_name":"Edoardo"},{"full_name":"Ishikawa, Yuzo","first_name":"Yuzo","last_name":"Ishikawa"},{"full_name":"Mackenzie, Ruari","first_name":"Ruari","last_name":"Mackenzie"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"full_name":"Navarrete, Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","first_name":"Benjamín","last_name":"Navarrete"},{"first_name":"Gauri","last_name":"Kotiwale","full_name":"Kotiwale, Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875"}],"OA_type":"diamond","corr_author":"1","ddc":["520"],"date_published":"2026-01-14T00:00:00Z","has_accepted_license":"1","intvolume":"       705","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"01","citation":{"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 and Astrophysics. 705, A147.","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 and Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202555596\">https://doi.org/10.1051/0004-6361/202555596</a>","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 and Astrophysics 705 (2026).","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 and 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>.","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 and Astrophysics</i>, vol. 705. EDP Sciences, 2026.","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 and Astrophysics</i>. 2026;705. doi:<a href=\"https://doi.org/10.1051/0004-6361/202555596\">10.1051/0004-6361/202555596</a>","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 and Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202555596\">https://doi.org/10.1051/0004-6361/202555596</a>."},"scopus_import":"1","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.","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"_id":"21045","date_created":"2026-01-25T23:01:41Z","doi":"10.1051/0004-6361/202555596","oa":1,"oa_version":"Published Version","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"OA_place":"publisher","quality_controlled":"1","language":[{"iso":"eng"}],"article_number":"A147","title":"A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth","volume":705,"publication":"Astronomy and Astrophysics","abstract":[{"lang":"eng","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."}],"file_date_updated":"2026-02-16T07:35:03Z","external_id":{"arxiv":["2505.09542"]},"article_processing_charge":"No","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"arxiv":1},{"quality_controlled":"1","language":[{"iso":"eng"}],"OA_place":"publisher","DOAJ_listed":"1","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"oa_version":"Published Version","oa":1,"doi":"10.1051/0004-6361/202556597","date_created":"2026-02-22T23:01:35Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"_id":"21341","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).","scopus_import":"1","citation":{"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>.","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>","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.","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).","apa":"Kotiwale, G., Matthee, J. J., Kashino, D., Vijayan, A. P., Torralba Torregrosa, A., Di Cesare, C., … Sobral, D. (2026). Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202556597\">https://doi.org/10.1051/0004-6361/202556597</a>","ista":"Kotiwale G, Matthee JJ, Kashino D, Vijayan AP, Torralba Torregrosa A, Di Cesare C, Iani E, Bordoloi R, Leja J, Maseda MV, Tacchella S, Shivaei I, Heintz KE, Danhaive AL, Mascia S, Kramarenko I, Navarrete B, Mackenzie R, Naidu RP, Sobral D. 2026. Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy. Astronomy &#38; Astrophysics. 706, A165."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"02","type":"journal_article","arxiv":1,"project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"external_id":{"arxiv":["2510.19959"]},"article_processing_charge":"No","file_date_updated":"2026-02-24T07:46:47Z","publication":"Astronomy & Astrophysics","abstract":[{"lang":"eng","text":"We aim to characterise the mass-metallicity relation (MZR) and the 3D correlation between the stellar mass, metallicity, and star formation rate (SFR) known as the fundamental metallicity relation (FMR) for galaxies at 5 < z < 7. Using ∼800 [O III] selected galaxies from deep NIRCam grism surveys, we present our stacked measurements of direct-Te metallicities, which we used to test recent strong-line metallicity calibrations. Our measured direct-Te metallicities (0.1–0.2 Z⊙ for M★ ≈ 5 × 107 − 9 M⊙, respectively) match recent JWST/NIRSpec-based results. However, there are significant inconsistencies between observations and hydrodynamical simulations. We observe a flatter MZR slope than the SPHINX20 and FLARES simulations, which cannot be attributed to selection effects. With simple models, we show that the effect of an [O III] flux-limited sample on the observed shape of the MZR is strongly dependent on the FMR. If the FMR is similar to the one in the local Universe, the intrinsic high-redshift MZR should be even flatter than is observed. In turn, a 3D relation where SFR correlates positively with metallicity at fixed mass would imply an intrinsically steeper MZR. Our measurements indicate that metallicity variations at fixed mass show little dependence on the SFR, suggesting a flat intrinsic MZR. This could indicate that the low-mass galaxies at these redshifts are out of equilibrium and that metal enrichment occurs rapidly in low-mass galaxies. However, being limited by our stacking analysis, we are yet to probe the scatter in the MZR and its dependence on SFR. Large carefully selected samples of galaxies with robust metallicity measurements can put tight constraints on the high-redshift FMR and help us to understand the interplay between gas flows, star formation, and feedback in early galaxies."}],"volume":706,"article_number":"A165","title":"Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy","day":"01","PlanS_conform":"1","year":"2026","file":[{"access_level":"open_access","relation":"main_file","date_created":"2026-02-24T07:46:47Z","checksum":"6f5849d29ad43bee32f90152f6fc0294","file_size":6531719,"date_updated":"2026-02-24T07:46:47Z","content_type":"application/pdf","creator":"dernst","file_id":"21355","file_name":"2026_AstronomyAstrophysics_Kotiwale.pdf","success":1}],"status":"public","publication_status":"published","publisher":"EDP Sciences","article_type":"original","date_updated":"2026-02-24T07:49:42Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"intvolume":"       706","has_accepted_license":"1","ddc":["520"],"date_published":"2026-02-01T00:00:00Z","corr_author":"1","OA_type":"diamond","author":[{"id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","full_name":"Kotiwale, Gauri","last_name":"Kotiwale","first_name":"Gauri"},{"first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"full_name":"Kashino, Daichi","last_name":"Kashino","first_name":"Daichi"},{"full_name":"Vijayan, Aswin P.","last_name":"Vijayan","first_name":"Aswin P."},{"id":"018f0249-0e87-11f0-b167-cbce08fbd541","full_name":"Torralba Torregrosa, Alberto","orcid":"0000-0001-5586-6950","last_name":"Torralba Torregrosa","first_name":"Alberto"},{"id":"2d002343-372f-11ef-98ec-a164d20427cb","full_name":"Di Cesare, Claudia","last_name":"Di Cesare","first_name":"Claudia"},{"id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","full_name":"Iani, Edoardo","orcid":"0000-0001-8386-3546","last_name":"Iani","first_name":"Edoardo"},{"full_name":"Bordoloi, Rongmon","last_name":"Bordoloi","first_name":"Rongmon"},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"full_name":"Maseda, Michael V.","first_name":"Michael V.","last_name":"Maseda"},{"full_name":"Tacchella, Sandro","first_name":"Sandro","last_name":"Tacchella"},{"full_name":"Shivaei, Irene","first_name":"Irene","last_name":"Shivaei"},{"first_name":"Kasper E.","last_name":"Heintz","full_name":"Heintz, Kasper E."},{"full_name":"Danhaive, A. Lola","first_name":"A. Lola","last_name":"Danhaive"},{"last_name":"Mascia","first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","full_name":"Mascia, Sara"},{"first_name":"Ivan","last_name":"Kramarenko","full_name":"Kramarenko, Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","orcid":"0000-0001-5346-6048"},{"first_name":"Benjamín","last_name":"Navarrete","full_name":"Navarrete, Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148"},{"last_name":"Mackenzie","first_name":"Ruari","full_name":"Mackenzie, Ruari"},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"}]},{"title":"The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings","article_number":"A75","volume":707,"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":"Astronomy & Astrophysics","file_date_updated":"2026-03-16T10:57:49Z","external_id":{"arxiv":["2510.00103"]},"article_processing_charge":"No","project":[{"grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization"}],"arxiv":1,"type":"journal_article","month":"03","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","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>.","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>","mla":"Torralba Torregrosa, Alberto, et al. “The Warm Outer Layer of a Little Red Dot as the Source of [Fe Ii] and Collisional Balmer Lines with Scattering Wings.” <i>Astronomy &#38; Astrophysics</i>, vol. 707, A75, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557537\">10.1051/0004-6361/202557537</a>.","ieee":"A. Torralba Torregrosa <i>et al.</i>, “The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings,” <i>Astronomy &#38; Astrophysics</i>, vol. 707. EDP Sciences, 2026.","short":"A. Torralba Torregrosa, J.J. Matthee, G. Pezzulli, R.P. Naidu, Y. Ishikawa, G.B. Brammer, S.J. Chang, J. Chisholm, A. De Graaff, F. D’Eugenio, C. Di Cesare, A.C. Eilers, J.E. Greene, M. Gronke, E. Iani, V. Kokorev, G. Kotiwale, I. Kramarenko, Y. Ma, S. Mascia, B. Navarrete, E. Nelson, P. Oesch, R.A. Simcoe, S. Wuyts, Astronomy &#38; Astrophysics 707 (2026).","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."},"scopus_import":"1","acknowledgement":"We thank the scientific referee for useful and constructive comments. We thank Ylva Götberg and Zoltan Haiman for insightful discussions about the physics of gaseous envelopes and accretion into black holes. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. This work is based in part on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program #5664. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349.","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"_id":"21451","doi":"10.1051/0004-6361/202557537","date_created":"2026-03-15T23:01:36Z","oa_version":"Published Version","oa":1,"department":[{"_id":"JoMa"}],"DOAJ_listed":"1","OA_place":"publisher","quality_controlled":"1","language":[{"iso":"eng"}],"author":[{"first_name":"Alberto","last_name":"Torralba Torregrosa","full_name":"Torralba Torregrosa, Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","orcid":"0000-0001-5586-6950"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"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.","last_name":"Brammer","first_name":"Gabriel B."},{"first_name":"Seok Jun","last_name":"Chang","full_name":"Chang, Seok Jun"},{"full_name":"Chisholm, John","first_name":"John","last_name":"Chisholm"},{"last_name":"De Graaff","first_name":"Anna","full_name":"De Graaff, Anna"},{"full_name":"D’Eugenio, Francesco","last_name":"D’Eugenio","first_name":"Francesco"},{"first_name":"Claudia","last_name":"Di Cesare","full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb"},{"full_name":"Eilers, Anna Christina","last_name":"Eilers","first_name":"Anna Christina"},{"full_name":"Greene, Jenny E.","first_name":"Jenny E.","last_name":"Greene"},{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","full_name":"Iani, Edoardo","orcid":"0000-0001-8386-3546","last_name":"Iani","first_name":"Edoardo"},{"last_name":"Kokorev","first_name":"Vasily","full_name":"Kokorev, Vasily"},{"full_name":"Kotiwale, Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","first_name":"Gauri","last_name":"Kotiwale"},{"first_name":"Ivan","last_name":"Kramarenko","full_name":"Kramarenko, Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","orcid":"0000-0001-5346-6048"},{"full_name":"Ma, Yilun","first_name":"Yilun","last_name":"Ma"},{"full_name":"Mascia, Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","first_name":"Sara","last_name":"Mascia"},{"first_name":"Benjamín","last_name":"Navarrete","full_name":"Navarrete, Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148"},{"first_name":"Erica","last_name":"Nelson","full_name":"Nelson, Erica"},{"last_name":"Oesch","first_name":"Pascal","full_name":"Oesch, Pascal"},{"last_name":"Simcoe","first_name":"Robert A.","full_name":"Simcoe, Robert A."},{"full_name":"Wuyts, Stijn","first_name":"Stijn","last_name":"Wuyts"}],"OA_type":"diamond","corr_author":"1","ddc":["520"],"date_published":"2026-03-01T00:00:00Z","has_accepted_license":"1","intvolume":"       707","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"date_updated":"2026-03-16T10:59:16Z","article_type":"original","publisher":"EDP Sciences","publication_status":"published","status":"public","file":[{"file_id":"21460","file_name":"2026_AstronomyAstrophysics_Torralba2.pdf","success":1,"access_level":"open_access","checksum":"fcab9cb3dcf1d68612e1fdc8191643c1","relation":"main_file","date_created":"2026-03-16T10:57:49Z","date_updated":"2026-03-16T10:57:49Z","content_type":"application/pdf","file_size":2510157,"creator":"dernst"}],"year":"2026","PlanS_conform":"1","day":"01"},{"title":"The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations","article_number":"A129","volume":707,"publication":"Astronomy & Astrophysics","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"}],"file_date_updated":"2026-03-16T10:48:07Z","external_id":{"arxiv":["2510.19044"]},"article_processing_charge":"No","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224"}],"arxiv":1,"type":"journal_article","month":"03","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"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>","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>.","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.","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>.","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>","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."},"scopus_import":"1","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).","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"_id":"21452","doi":"10.1051/0004-6361/202557790","date_created":"2026-03-15T23:01:36Z","oa_version":"Published Version","oa":1,"DOAJ_listed":"1","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"OA_place":"publisher","quality_controlled":"1","language":[{"iso":"eng"}],"author":[{"first_name":"Claudia","last_name":"Di Cesare","full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J"},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."},{"full_name":"Torralba, Alberto","last_name":"Torralba","first_name":"Alberto"},{"last_name":"Kotiwale","first_name":"Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","full_name":"Kotiwale, Gauri"},{"full_name":"Kramarenko, Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","orcid":"0000-0001-5346-6048","first_name":"Ivan","last_name":"Kramarenko"},{"full_name":"Blaizot, Jeremy","last_name":"Blaizot","first_name":"Jeremy"},{"last_name":"Rosdahl","first_name":"Joakim","full_name":"Rosdahl, Joakim"},{"full_name":"Leja, Joel","last_name":"Leja","first_name":"Joel"},{"id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","full_name":"Iani, Edoardo","orcid":"0000-0001-8386-3546","last_name":"Iani","first_name":"Edoardo"},{"full_name":"Adamo, Angela","last_name":"Adamo","first_name":"Angela"},{"last_name":"Covelo-Paz","first_name":"Alba","full_name":"Covelo-Paz, Alba"},{"last_name":"Furtak","first_name":"Lukas J.","full_name":"Furtak, Lukas J."},{"full_name":"Heintz, Kasper E.","first_name":"Kasper E.","last_name":"Heintz"},{"last_name":"Mascia","first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","full_name":"Mascia, Sara"},{"last_name":"Navarrete","first_name":"Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","full_name":"Navarrete, Benjamín"},{"first_name":"Pascal A.","last_name":"Oesch","full_name":"Oesch, Pascal A."},{"full_name":"Romano, Michael","first_name":"Michael","last_name":"Romano"},{"full_name":"Shivaei, Irene","last_name":"Shivaei","first_name":"Irene"},{"first_name":"Sandro","last_name":"Tacchella","full_name":"Tacchella, Sandro"}],"OA_type":"diamond","corr_author":"1","ddc":["520"],"date_published":"2026-03-01T00:00:00Z","has_accepted_license":"1","intvolume":"       707","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"date_updated":"2026-03-16T10:52:44Z","article_type":"original","publisher":"EDP Sciences","publication_status":"published","status":"public","file":[{"access_level":"open_access","relation":"main_file","date_created":"2026-03-16T10:48:07Z","checksum":"c056b00ce7324849754521fde10fb7ca","content_type":"application/pdf","date_updated":"2026-03-16T10:48:07Z","file_size":1821411,"creator":"dernst","file_id":"21459","file_name":"2026_AstronomyAstrophysics_DiCesare.pdf","success":1}],"year":"2026","PlanS_conform":"1","day":"01"},{"ddc":["520"],"date_published":"2025-09-25T00:00:00Z","OA_type":"gold","author":[{"first_name":"Anna Christina","last_name":"Eilers","full_name":"Eilers, Anna Christina"},{"last_name":"Yue","first_name":"Minghao","full_name":"Yue, Minghao"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Hennawi, Joseph F.","first_name":"Joseph F.","last_name":"Hennawi"},{"full_name":"Davies, Frederick B.","first_name":"Frederick B.","last_name":"Davies"},{"last_name":"Simcoe","first_name":"Robert A.","full_name":"Simcoe, Robert A."},{"first_name":"Richard","last_name":"Teague","full_name":"Teague, Richard"},{"last_name":"Bordoloi","first_name":"Rongmon","full_name":"Bordoloi, Rongmon"},{"full_name":"Brammer, Gabriel","last_name":"Brammer","first_name":"Gabriel"},{"first_name":"Yi","last_name":"Kang","full_name":"Kang, Yi"},{"full_name":"Kashino, Daichi","last_name":"Kashino","first_name":"Daichi"},{"full_name":"Mackenzie, Ruari","first_name":"Ruari","last_name":"Mackenzie"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"first_name":"Benjamín","last_name":"Navarrete","full_name":"Navarrete, Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148"}],"isi":1,"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"intvolume":"       991","has_accepted_license":"1","publication_status":"published","status":"public","publisher":"IOP Publishing","article_type":"original","date_updated":"2026-02-16T12:44:42Z","PlanS_conform":"1","day":"25","year":"2025","file":[{"file_id":"20461","file_name":"2025_AstrophysicalJour_Eilers.pdf","success":1,"access_level":"open_access","relation":"main_file","date_created":"2025-10-13T09:25:12Z","checksum":"3cb8099b9a915755164e5675b33f8a03","file_size":23585591,"content_type":"application/pdf","date_updated":"2025-10-13T09:25:12Z","creator":"dernst"}],"file_date_updated":"2025-10-13T09:25:12Z","volume":991,"publication":"The Astrophysical Journal Letters","abstract":[{"lang":"eng","text":"Ultraviolet (UV) radiation from accreting black holes ionizes the intergalactic gas around early quasars, carving out highly ionized bubbles in their surroundings. Any changes in a quasar’s luminosity are therefore predicted to produce outward-propagating ionization gradients, affecting the Lyα absorption opacity near the quasar’s systemic redshift. This “proximity effect” is well-documented in rest-UV quasar spectra but only provides a one-dimensional probe along our line of sight. Here we present deep spectroscopic observations with the James Webb Space Telescope (JWST) of galaxies in the background of a superluminous quasar at zQSO ≈ 6.3, which reveal the quasar’s “light echo” with Lyα tomography in the transverse direction. This transverse proximity effect is detected for the first time toward multiple galaxy sightlines, allowing us to map the extent and geometry of the quasar’s ionization cone. We obtain constraints on the orientation and inclination of the cone, as well as an upper limit on the obscured solid angle fraction of fobsc < 91%. Additionally, we find a timescale of the quasar’s UV radiation of tqso = 10^5.6+0.1-0.3 yr, which is significantly shorter than would be required to build up the central supermassive black hole (SMBH) with conventional growth models, but is consistent with independent measurements of the quasars’ duty cycle. Our inferred obscured fraction disfavors a scenario where short quasar lifetimes can be explained exclusively by geometric obscuration, and instead supports the idea that radiatively inefficient accretion or growth in initially heavily enshrouded cocoons plays a pivotal role in early SMBH growth. Our results pave the way for novel studies of quasars’ ionizing geometries and radiative histories at early cosmic times."}],"article_number":"L40","title":"The light echo of a high-redshift quasar mapped with Lyα tomography","arxiv":1,"project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224"}],"article_processing_charge":"Yes","external_id":{"isi":["001581023000001"],"arxiv":["2509.05417"]},"_id":"20425","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"date_created":"2025-10-05T22:01:35Z","doi":"10.3847/2041-8213/ae057a","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 #1243 and #4713.\r\n\r\nAll of the data presented in this Letter were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via doi:10.17909/w7hm-qb39.\r\nJ.M. is supported by the European Union (ERC, AGENTS, 101076224).","citation":{"mla":"Eilers, Anna Christina, et al. “The Light Echo of a High-Redshift Quasar Mapped with Lyα Tomography.” <i>The Astrophysical Journal Letters</i>, vol. 991, no. 2, L40, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/2041-8213/ae057a\">10.3847/2041-8213/ae057a</a>.","ieee":"A. C. Eilers <i>et al.</i>, “The light echo of a high-redshift quasar mapped with Lyα tomography,” <i>The Astrophysical Journal Letters</i>, vol. 991, no. 2. IOP Publishing, 2025.","short":"A.C. Eilers, M. Yue, J.J. Matthee, J.F. Hennawi, F.B. Davies, R.A. Simcoe, R. Teague, R. Bordoloi, G. Brammer, Y. Kang, D. Kashino, R. Mackenzie, R.P. Naidu, B. Navarrete, The Astrophysical Journal Letters 991 (2025).","chicago":"Eilers, Anna Christina, Minghao Yue, Jorryt J Matthee, Joseph F. Hennawi, Frederick B. Davies, Robert A. Simcoe, Richard Teague, et al. “The Light Echo of a High-Redshift Quasar Mapped with Lyα Tomography.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/2041-8213/ae057a\">https://doi.org/10.3847/2041-8213/ae057a</a>.","ama":"Eilers AC, Yue M, Matthee JJ, et al. The light echo of a high-redshift quasar mapped with Lyα tomography. <i>The Astrophysical Journal Letters</i>. 2025;991(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/ae057a\">10.3847/2041-8213/ae057a</a>","ista":"Eilers AC, Yue M, Matthee JJ, Hennawi JF, Davies FB, Simcoe RA, Teague R, Bordoloi R, Brammer G, Kang Y, Kashino D, Mackenzie R, Naidu RP, Navarrete B. 2025. The light echo of a high-redshift quasar mapped with Lyα tomography. The Astrophysical Journal Letters. 991(2), L40.","apa":"Eilers, A. C., Yue, M., Matthee, J. J., Hennawi, J. F., Davies, F. B., Simcoe, R. A., … Navarrete, B. (2025). The light echo of a high-redshift quasar mapped with Lyα tomography. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ae057a\">https://doi.org/10.3847/2041-8213/ae057a</a>"},"scopus_import":"1","type":"journal_article","month":"09","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","language":[{"iso":"eng"}],"issue":"2","OA_place":"publisher","DOAJ_listed":"1","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"oa":1,"oa_version":"Published Version"}]