--- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21274' abstract: - lang: eng text: "Many white dwarfs are observed in compact double white dwarf binaries, and through the emission of gravitational waves, a large fraction are destined to merge. The merger remnants that do not explode in a Type Ia supernova are expected to initially be rapidly rotating and highly magnetized. In this work, we present our discovery of the variable white dwarf ZTF J200832.79+444939.67, hereafter ZTF J2008+4449, as a likely merger remnant showing signs of circumstellar material without a stellar or substellar companion. The nature of ZTF J2008+4449 as a merger remnant is supported by its physical properties: it is hot (35 500 ± 300 K) and massive (1.12 ± 0.03 M\r\n ⊙\r\n ), rapidly rotating with a period of ≈6.6 minutes, and likely possesses exceptionally strong magnetic fields (∼400−600 MG) at its surface. Remarkably, we detect a significant period derivative of (1.80 ± 0.09)×10\r\n −12\r\n \ s/s, indicating that the white dwarf is spinning down, and a soft X-ray emission that is inconsistent with photospheric emission. As the presence of a mass-transferring stellar or brown dwarf companion is excluded by infrared photometry, the detected spin-down and X-ray emission could be tell-tale signs of a magnetically driven wind or of interaction with circumstellar material, possibly originating from the fallback of gravitationally bound merger ejecta or from the tidal disruption of a planetary object. We also detect Balmer emission, which requires the presence of ionized hydrogen in the vicinity of the white dwarf, showing Doppler shifts as high as ≈2000 km s\r\n −1\r\n \ . The unusual variability of the Balmer emission on the spin period of the white dwarf is consistent with the trapping of a half ring of ionized gas in the magnetosphere of the white dwarf.\r\n " acknowledgement: "We thank Lynne Hillenbrand and Soumyadeep Bhattacharjee for helpful discussions, and Kishalay De for his help with the WIRC\r\nreduction pipeline. IC was supported by NASA through grants from the Space\r\nTelescope Science Institute, under NASA contracts NASA.22K1813, NAS5-\r\n26555 and NAS5-03127. TC was supported by NASA through the NASA Hubble\r\nFellowship grant HST-HF2-51527.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research\r\nin Astronomy, Inc., for NASA, under contract NAS5-26555. This project has\r\nreceived funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 101020057). This work was based on observations obtained with the\r\nSamuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar\r\nObservatory as part of the Zwicky Transient Facility project. ZTF is supported\r\nby the National Science Foundation under Grants No. AST-1440341, AST2034437, and currently Award #2407588. ZTF receives additional funding from\r\nthe ZTF partnership. Current members include Caltech, USA; Caltech/IPAC,\r\nUSA; University of Maryland, USA; University of California, Berkeley, USA;\r\nUniversity of Wisconsin at Milwaukee, USA; Cornell University, USA; Drexel\r\nUniversity, USA; University of North Carolina at Chapel Hill, USA; Institute\r\nof Science and Technology, Austria; National Central University, Taiwan, and\r\nOKC, University of Stockholm, Sweden. Operations are conducted by Caltech’s\r\nOptical Observatory (COO), Caltech/IPAC, and the University of Washington at\r\nSeattle, USA. This work has made use of data from the European Space Agency\r\n(ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by\r\nthe Gaia Data Processing and Analysis Consortium (DPAC, https://www.\r\ncosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The Pan-STARRS1 Surveys (PS1)\r\nand the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the PanSTARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck\r\nInstitute for Extraterrestrial Physics, Garching, The Johns Hopkins University,\r\nDurham University, the University of Edinburgh, the Queen’s University Belfast,\r\nthe Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through\r\nthe Planetary Science Division of the NASA Science Mission Directorate, the\r\nNational Science Foundation Grant No. AST–1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory,\r\nand the Gordon and Betty Moore Foundation. This work made use of Astropy\r\n(http://www.astropy.org): a community-developed core Python package\r\nand an ecosystem of tools and resources for astronomy (Astropy Collaboration\r\n2013, 2018, 2022)." article_number: A188 article_processing_charge: Yes article_type: original author: - first_name: Andrei-Alexandru full_name: Cristea, Andrei-Alexandru id: 4d500bea-31f8-11ee-a48d-d4904fb363c7 last_name: Cristea - first_name: Ilaria full_name: Caiazzo, Ilaria id: 8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d last_name: Caiazzo orcid: 0000-0002-4770-5388 - first_name: Tim full_name: Cunningham, Tim last_name: Cunningham - first_name: John C. full_name: Raymond, John C. last_name: Raymond - first_name: Stephane full_name: Vennes, Stephane last_name: Vennes - first_name: Adela full_name: Kawka, Adela last_name: Kawka - first_name: Aayush A full_name: Desai, Aayush A id: 502cfd30-32c1-11ee-a9a4-d8dad5c6739e last_name: Desai - first_name: David R. full_name: Miller, David R. last_name: Miller - first_name: J. J. full_name: Hermes, J. J. last_name: Hermes - first_name: Jim full_name: Fuller, Jim last_name: Fuller - first_name: Jeremy full_name: Heyl, Jeremy last_name: Heyl - first_name: Jan full_name: van Roestel, Jan last_name: van Roestel - first_name: Kevin B. full_name: Burdge, Kevin B. last_name: Burdge - first_name: Antonio C. full_name: Rodriguez, Antonio C. last_name: Rodriguez - first_name: Ingrid full_name: Pelisoli, Ingrid last_name: Pelisoli - first_name: Boris T. full_name: Gänsicke, Boris T. last_name: Gänsicke - first_name: Paula full_name: Szkody, Paula last_name: Szkody - first_name: Scott J. full_name: Kenyon, Scott J. last_name: Kenyon - first_name: Zach full_name: Vanderbosch, Zach last_name: Vanderbosch - first_name: Andrew full_name: Drake, Andrew last_name: Drake - first_name: Lilia full_name: Ferrario, Lilia last_name: Ferrario - first_name: Dayal full_name: Wickramasinghe, Dayal last_name: Wickramasinghe - first_name: Viraj R. full_name: Karambelkar, Viraj R. last_name: Karambelkar - first_name: Stephen full_name: Justham, Stephen last_name: Justham - first_name: Ruediger full_name: Pakmor, Ruediger last_name: Pakmor - first_name: Kareem full_name: El-Badry, Kareem last_name: El-Badry - first_name: Thomas full_name: Prince, Thomas last_name: Prince - first_name: S. R. full_name: Kulkarni, S. R. last_name: Kulkarni - first_name: Matthew J. full_name: Graham, Matthew J. last_name: Graham - first_name: Frank J. full_name: Masci, Frank J. last_name: Masci - first_name: Steven L. full_name: Groom, Steven L. last_name: Groom - first_name: Josiah full_name: Purdum, Josiah last_name: Purdum - first_name: Richard full_name: Dekany, Richard last_name: Dekany - first_name: Eric C. full_name: Bellm, Eric C. last_name: Bellm citation: ama: Cristea A-A, Caiazzo I, Cunningham T, et al. A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant. Astronomy & Astrophysics. 2026;706. doi:10.1051/0004-6361/202556432 apa: Cristea, A.-A., Caiazzo, I., Cunningham, T., Raymond, J. C., Vennes, S., Kawka, A., … Bellm, E. C. (2026). A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202556432 chicago: Cristea, Andrei-Alexandru, Ilaria Caiazzo, Tim Cunningham, John C. Raymond, Stephane Vennes, Adela Kawka, Aayush A Desai, et al. “A Half Ring of Ionized Circumstellar Material Trapped in the Magnetosphere of a White Dwarf Merger Remnant.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202556432. ieee: A.-A. Cristea et al., “A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant,” Astronomy & Astrophysics, vol. 706. EDP Sciences, 2026. ista: Cristea A-A, Caiazzo I, Cunningham T, Raymond JC, Vennes S, Kawka A, Desai AA, Miller DR, Hermes JJ, Fuller J, Heyl J, van Roestel J, Burdge KB, Rodriguez AC, Pelisoli I, Gänsicke BT, Szkody P, Kenyon SJ, Vanderbosch Z, Drake A, Ferrario L, Wickramasinghe D, Karambelkar VR, Justham S, Pakmor R, El-Badry K, Prince T, Kulkarni SR, Graham MJ, Masci FJ, Groom SL, Purdum J, Dekany R, Bellm EC. 2026. A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant. Astronomy & Astrophysics. 706, A188. mla: Cristea, Andrei-Alexandru, et al. “A Half Ring of Ionized Circumstellar Material Trapped in the Magnetosphere of a White Dwarf Merger Remnant.” Astronomy & Astrophysics, vol. 706, A188, EDP Sciences, 2026, doi:10.1051/0004-6361/202556432. short: A.-A. Cristea, I. Caiazzo, T. Cunningham, J.C. Raymond, S. Vennes, A. Kawka, A.A. Desai, D.R. Miller, J.J. Hermes, J. Fuller, J. Heyl, J. van Roestel, K.B. Burdge, A.C. Rodriguez, I. Pelisoli, B.T. Gänsicke, P. Szkody, S.J. Kenyon, Z. Vanderbosch, A. Drake, L. Ferrario, D. Wickramasinghe, V.R. Karambelkar, S. Justham, R. Pakmor, K. El-Badry, T. Prince, S.R. Kulkarni, M.J. Graham, F.J. Masci, S.L. Groom, J. Purdum, R. Dekany, E.C. Bellm, Astronomy & Astrophysics 706 (2026). corr_author: '1' date_created: 2026-02-17T08:12:05Z date_published: 2026-02-10T00:00:00Z date_updated: 2026-04-28T12:01:21Z day: '10' ddc: - '520' department: - _id: IlCa - _id: GradSch doi: 10.1051/0004-6361/202556432 file: - access_level: open_access checksum: 229b688e6e78cab5bb8e2bac366d1575 content_type: application/pdf creator: dernst date_created: 2026-02-23T12:04:37Z date_updated: 2026-02-23T12:04:37Z file_id: '21350' file_name: 2026_AstronomyAstrophysics_Cristea.pdf file_size: 5352853 relation: main_file success: 1 file_date_updated: 2026-02-23T12:04:37Z has_accepted_license: '1' intvolume: ' 706' language: - iso: eng month: '02' oa: 1 oa_version: Published Version publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' related_material: link: - description: News on ISTA website relation: press_release url: https://ista.ac.at/en/news/twos-company-new-class-of-star-remnants/ status: public title: A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: ba8df636-2132-11f1-aed0-ed93e2281fdd volume: 706 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '21341' abstract: - lang: eng text: We aim to characterise the mass-metallicity relation (MZR) and the 3D correlation between the stellar mass, metallicity, and star formation rate (SFR) known as the fundamental metallicity relation (FMR) for galaxies at 5 < z < 7. Using ∼800 [O III] selected galaxies from deep NIRCam grism surveys, we present our stacked measurements of direct-Te metallicities, which we used to test recent strong-line metallicity calibrations. Our measured direct-Te metallicities (0.1–0.2 Z⊙ for M★ ≈ 5 × 107 − 9 M⊙, respectively) match recent JWST/NIRSpec-based results. However, there are significant inconsistencies between observations and hydrodynamical simulations. We observe a flatter MZR slope than the SPHINX20 and FLARES simulations, which cannot be attributed to selection effects. With simple models, we show that the effect of an [O III] flux-limited sample on the observed shape of the MZR is strongly dependent on the FMR. If the FMR is similar to the one in the local Universe, the intrinsic high-redshift MZR should be even flatter than is observed. In turn, a 3D relation where SFR correlates positively with metallicity at fixed mass would imply an intrinsically steeper MZR. Our measurements indicate that metallicity variations at fixed mass show little dependence on the SFR, suggesting a flat intrinsic MZR. This could indicate that the low-mass galaxies at these redshifts are out of equilibrium and that metal enrichment occurs rapidly in low-mass galaxies. However, being limited by our stacking analysis, we are yet to probe the scatter in the MZR and its dependence on SFR. Large carefully selected samples of galaxies with robust metallicity measurements can put tight constraints on the high-redshift FMR and help us to understand the interplay between gas flows, star formation, and feedback in early galaxies. 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).' article_number: A165 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Gauri full_name: Kotiwale, Gauri id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875 last_name: Kotiwale - first_name: Jorryt J full_name: Matthee, Jorryt J id: 7439a258-f3c0-11ec-9501-9df22fe06720 last_name: Matthee orcid: 0000-0003-2871-127X - first_name: Daichi full_name: Kashino, Daichi last_name: Kashino - first_name: Aswin P. full_name: Vijayan, Aswin P. last_name: Vijayan - first_name: Alberto full_name: Torralba Torregrosa, Alberto id: 018f0249-0e87-11f0-b167-cbce08fbd541 last_name: Torralba Torregrosa orcid: 0000-0001-5586-6950 - first_name: Claudia full_name: Di Cesare, Claudia id: 2d002343-372f-11ef-98ec-a164d20427cb last_name: Di Cesare - first_name: Edoardo full_name: Iani, Edoardo id: 4053390a-6b68-11ef-9828-a3b8adef8d0a last_name: Iani orcid: 0000-0001-8386-3546 - first_name: Rongmon full_name: Bordoloi, Rongmon last_name: Bordoloi - first_name: Joel full_name: Leja, Joel last_name: Leja - first_name: Michael V. full_name: Maseda, Michael V. last_name: Maseda - first_name: Sandro full_name: Tacchella, Sandro last_name: Tacchella - first_name: Irene full_name: Shivaei, Irene last_name: Shivaei - first_name: Kasper E. full_name: Heintz, Kasper E. last_name: Heintz - first_name: A. Lola full_name: Danhaive, A. Lola last_name: Danhaive - first_name: Sara full_name: Mascia, Sara id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29 last_name: Mascia - first_name: Ivan full_name: Kramarenko, Ivan id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4 last_name: Kramarenko orcid: 0000-0001-5346-6048 - first_name: Benjamín full_name: Navarrete, Benjamín id: aa14a535-50c9-11ef-b52e-e0c373d10148 last_name: Navarrete - first_name: Ruari full_name: Mackenzie, Ruari last_name: Mackenzie - first_name: Rohan P. full_name: Naidu, Rohan P. last_name: Naidu - first_name: David full_name: Sobral, David last_name: Sobral citation: 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. Astronomy & Astrophysics. 2026;706. doi:10.1051/0004-6361/202556597 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. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202556597 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.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202556597. ieee: G. Kotiwale et al., “Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy,” Astronomy & Astrophysics, vol. 706. EDP Sciences, 2026. 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 & Astrophysics. 706, A165. 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.” Astronomy & Astrophysics, vol. 706, A165, EDP Sciences, 2026, doi:10.1051/0004-6361/202556597. 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 & Astrophysics 706 (2026). corr_author: '1' date_created: 2026-02-22T23:01:35Z date_published: 2026-02-01T00:00:00Z date_updated: 2026-02-24T07:49:42Z day: '01' ddc: - '520' department: - _id: JoMa - _id: GradSch doi: 10.1051/0004-6361/202556597 external_id: arxiv: - '2510.19959' file: - access_level: open_access checksum: 6f5849d29ad43bee32f90152f6fc0294 content_type: application/pdf creator: dernst date_created: 2026-02-24T07:46:47Z date_updated: 2026-02-24T07:46:47Z file_id: '21355' file_name: 2026_AstronomyAstrophysics_Kotiwale.pdf file_size: 6531719 relation: main_file success: 1 file_date_updated: 2026-02-24T07:46:47Z has_accepted_license: '1' intvolume: ' 706' language: - iso: eng month: '02' oa: 1 oa_version: Published Version project: - _id: bd9b2118-d553-11ed-ba76-db24564edfea grant_number: '101076224' name: Young galaxies as tracers and agents of cosmic reionization publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' scopus_import: '1' status: public title: Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 706 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: diamond _id: '21380' abstract: - lang: eng text: "Context. Extreme emission line galaxies (EELGs) are believed to significantly contribute to the star formation activity and mass assembly in galaxies. EELGs likely also play a leading role in the cosmic re-ionization as their interstellar medium may allow a significant fraction of their ionizing photons to escape (> 5%). Finding low-redshift analogues of these high-z galaxies is therefore essential to characterizing the physical conditions in the interstellar medium of these galaxies and understanding the processes that re-ionized the Universe.\r\n\r\nAims. We aimed to develop a robust and efficient method for the photometric identification of EELGs using the J-PAS survey. J-PAS will cover approximately 8500 deg2 of the sky with 54 narrow-band filters in the optical range plus i-SDSS, enabling detailed studies of the physical properties of these galaxies. In this work we focused on an initial subset of the survey: a 30 square degree area with complete observations in all bands.\r\n\r\nMethods. We combine equivalent width (EW) measurements from J-PAS narrow-band photometry with artificial intelligence techniques to identify galaxies with emission lines exceeding 300 Å. We validated our selection using spectroscopic data from DESI DR1 and characterized the selected sample through spectral energy distribution fitting with CIGALE.\r\n\r\nResults. We identify 917 EELGs up to z = 0.8 over 30 deg2, achieving a purity of 95% and a completeness of 96% for i-SDSS < 22.5 mag. Importantly, active galactic nucleus contamination was carefully considered and is estimated to be around 5%. Furthermore, a cross-match with DESI yielded 79 counterparts; their redshifts are in excellent agreement with our photometric estimates, thereby confirming the reliability of our redshift determination. In addition, the derived emission line fluxes are in good agreement with spectroscopic measurements. Moreover, the selected sample reveals strong correlations between the ionizing photon production efficiency (ξion) and EW(Hβ), which are consistent with previous observational studies at low and high redshifts and theoretical expectations. Finally, most of the sources surpass the ionizing efficiency threshold required for re-ionization, highlighting their relevance as local analogues of early-Universe galaxies." acknowledgement: "We thank the referee for several helpful suggestions. AGA, MGO and IM acknowledge financial support from the Severo Ochoa grant CEX2021-001131-S, funded by MICIU/AEI/10.13039/501100011033. AGA also acknowledges FPI support under grant code CEX2021-001131-S20-7. Both AGA and MGO acknowledge support from the research grant\r\nPID2022-136598NB-C32 (“Estallidos8”). MGO also acknowledges the support by the project ref. AST22_00001_Subp_11 funded from the EU – NextGenerationEU. RA acknowledges support from PID2023-147386NB-I00 funded by MICIU/AEI/10.13039/501100011033 and ERDF/EU. IM acknowledges support from PID2022-140871NB-C21 funded by MICIU/AEI/10.13039/501100011033 and FEDER/UE. RGD acknowledge financial support from the project PID2022-141755NB-I00, and the Severo Ochoa grant CEX2021-001131-S funded\r\nby MICIU/AEI/ 10.13039/501100011033. JAFO and AE acknowledge support from the Spanish Ministry of Science and Innovation and the EU–NextGenerationEU through the RRF project ICTS-MRR-2021-03-CEFCA. AHC and ALC acknowledge support from MCIN/AEI/10.13039/501100011033, “ERDF A way of making Europe”, and “EU NextGenerationEU/PRTR” through PID2021-124918NB-C44 and CNS2023-145339, as well as from the RRF project ICTS-MRR-2021-03-CEFCA ALC and RPT acknowledge the financial\r\nsupport from the European Union – NextGenerationEU through the RRF program Planes Complementarios con las CCAA de Astrofísica y Física de Altas Energías – LA4. I.B. acknowledges support from the EU Horizon 2020 programme (Marie Sklodowska-Curie Grant 101059532) and the Franziska Seidl Funding Program, University of Vienna. This paper has gone through internal‘ review by the J-PAS collaboration. Based on observations made with the\r\nJST/T250 telescope and JPCam at the Observatorio Astrofísico de Javalambre (OAJ), in Teruel, owned, managed, and operated by the Centro de Estudios de Física del Cosmos de Aragón (CEFCA). We acknowledge the OAJ Data Processing and Archiving Unit (UPAD) for reducing and calibrating the OAJ data used in this work. Funding for the J-PAS Project has been provided by the Governments of Spain and Aragón through the Fondo de Inversiones de Teruel; the Aragonese Government through the Research Groups E96, E103, E16_17R, E16_20R, and E16_23R; the Spanish Ministry of Science and Innovation (MCIN/AEI/10.13039/501100011033 y FEDER, Una manera de hacer Europa) with grants PID2021-124918NB-C41, PID2021-124918NB-C42, PID2021-124918NA-C43, and PID2021-124918NB-C44; the Spanish Ministry\r\nof Science, Innovation and Universities (MCIU/AEI/FEDER, UE) with grants\r\nPGC2018-097585-B-C21 and PGC2018-097585-B-C22; the Spanish Ministry of Economy and Competitiveness (MINECO) under AYA2015-66211-C2-1-P, AYA2015-66211-C2-2, and AYA2012-30789; and European FEDER funding (FCDD10-4E-867, FCDD13-4E-2685)." article_number: A261 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: A. full_name: Giménez-Alcázar, A. last_name: Giménez-Alcázar - first_name: R. full_name: Amorín, R. last_name: Amorín - first_name: J. M. full_name: Vílchez, J. M. last_name: Vílchez - first_name: A. full_name: Hernán-Caballero, A. last_name: Hernán-Caballero - first_name: M. full_name: González-Otero, M. last_name: González-Otero - first_name: A. full_name: Arroyo-Polonio, A. last_name: Arroyo-Polonio - first_name: J. full_name: Iglesias-Páramo, J. last_name: Iglesias-Páramo - first_name: A. full_name: Lumbreras-Calle, A. last_name: Lumbreras-Calle - first_name: J. A. full_name: Fernández-Ontiveros, J. A. last_name: Fernández-Ontiveros - first_name: C. full_name: López-Sanjuan, C. last_name: López-Sanjuan - first_name: L. full_name: Bonatto, L. last_name: Bonatto - first_name: R. M. full_name: González Delgado, R. M. last_name: González Delgado - first_name: C. full_name: Kehrig, C. last_name: Kehrig - first_name: Alberto full_name: Torralba Torregrosa, Alberto id: 018f0249-0e87-11f0-b167-cbce08fbd541 last_name: Torralba Torregrosa orcid: 0000-0001-5586-6950 - first_name: P. T. full_name: Rahna, P. T. last_name: Rahna - first_name: Y. full_name: Jiménez-Teja, Y. last_name: Jiménez-Teja - first_name: I. full_name: Márquez, I. last_name: Márquez - first_name: I. full_name: Breda, I. last_name: Breda - first_name: A. full_name: Álvarez-Candal, A. last_name: Álvarez-Candal - first_name: R. full_name: Abramo, R. last_name: Abramo - first_name: J. full_name: Alcaniz, J. last_name: Alcaniz - first_name: N. full_name: Benitez, N. last_name: Benitez - first_name: S. full_name: Bonoli, S. last_name: Bonoli - first_name: S. full_name: Carneiro, S. last_name: Carneiro - first_name: J. full_name: Cenarro, J. last_name: Cenarro - first_name: D. full_name: Cristóbal-Hornillos, D. last_name: Cristóbal-Hornillos - first_name: R. full_name: Dupke, R. last_name: Dupke - first_name: A. full_name: Ederoclite, A. last_name: Ederoclite - first_name: C. full_name: Hernández-Monteagudo, C. last_name: Hernández-Monteagudo - first_name: A. full_name: Marín-Franch, A. last_name: Marín-Franch - first_name: C. full_name: Mendes de Oliveira, C. last_name: Mendes de Oliveira - first_name: M. full_name: Moles, M. last_name: Moles - first_name: L. full_name: Sodré, L. last_name: Sodré - first_name: K. full_name: Taylor, K. last_name: Taylor - first_name: J. full_name: Varela, J. last_name: Varela - first_name: H. full_name: Vázquez Ramió, H. last_name: Vázquez Ramió citation: ama: 'Giménez-Alcázar A, Amorín R, Vílchez JM, et al. J-PAS: First identification, physical properties, and ionization efficiency of extreme emission line galaxies. Astronomy & Astrophysics. 2026;706. doi:10.1051/0004-6361/202557358' apa: 'Giménez-Alcázar, A., Amorín, R., Vílchez, J. M., Hernán-Caballero, A., González-Otero, M., Arroyo-Polonio, A., … Vázquez Ramió, H. (2026). J-PAS: First identification, physical properties, and ionization efficiency of extreme emission line galaxies. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557358' chicago: 'Giménez-Alcázar, A., R. Amorín, J. M. Vílchez, A. Hernán-Caballero, M. González-Otero, A. Arroyo-Polonio, J. Iglesias-Páramo, et al. “J-PAS: First Identification, Physical Properties, and Ionization Efficiency of Extreme Emission Line Galaxies.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557358.' ieee: 'A. Giménez-Alcázar et al., “J-PAS: First identification, physical properties, and ionization efficiency of extreme emission line galaxies,” Astronomy & Astrophysics, vol. 706. EDP Sciences, 2026.' ista: 'Giménez-Alcázar A, Amorín R, Vílchez JM, Hernán-Caballero A, González-Otero M, Arroyo-Polonio A, Iglesias-Páramo J, Lumbreras-Calle A, Fernández-Ontiveros JA, López-Sanjuan C, Bonatto L, González Delgado RM, Kehrig C, Torralba Torregrosa A, Rahna PT, Jiménez-Teja Y, Márquez I, Breda I, Álvarez-Candal A, Abramo R, Alcaniz J, Benitez N, Bonoli S, Carneiro S, Cenarro J, Cristóbal-Hornillos D, Dupke R, Ederoclite A, Hernández-Monteagudo C, Marín-Franch A, Mendes de Oliveira C, Moles M, Sodré L, Taylor K, Varela J, Vázquez Ramió H. 2026. J-PAS: First identification, physical properties, and ionization efficiency of extreme emission line galaxies. Astronomy & Astrophysics. 706, A261.' mla: 'Giménez-Alcázar, A., et al. “J-PAS: First Identification, Physical Properties, and Ionization Efficiency of Extreme Emission Line Galaxies.” Astronomy & Astrophysics, vol. 706, A261, EDP Sciences, 2026, doi:10.1051/0004-6361/202557358.' short: A. Giménez-Alcázar, R. Amorín, J.M. Vílchez, A. Hernán-Caballero, M. González-Otero, A. Arroyo-Polonio, J. Iglesias-Páramo, A. Lumbreras-Calle, J.A. Fernández-Ontiveros, C. López-Sanjuan, L. Bonatto, R.M. González Delgado, C. Kehrig, A. Torralba Torregrosa, P.T. Rahna, Y. Jiménez-Teja, I. Márquez, I. Breda, A. Álvarez-Candal, R. Abramo, J. Alcaniz, N. Benitez, S. Bonoli, S. Carneiro, J. Cenarro, D. Cristóbal-Hornillos, R. Dupke, A. Ederoclite, C. Hernández-Monteagudo, A. Marín-Franch, C. Mendes de Oliveira, M. Moles, L. Sodré, K. Taylor, J. Varela, H. Vázquez Ramió, Astronomy & Astrophysics 706 (2026). date_created: 2026-03-02T10:06:10Z date_published: 2026-02-01T00:00:00Z date_updated: 2026-03-02T15:10:27Z day: '01' ddc: - '520' department: - _id: JoMa doi: 10.1051/0004-6361/202557358 external_id: arxiv: - '2512.08484' file: - access_level: open_access checksum: cd25a05386ab5638ae5baf8add0ecbee content_type: application/pdf creator: dernst date_created: 2026-03-02T14:51:57Z date_updated: 2026-03-02T14:51:57Z file_id: '21391' file_name: 2026_AstronomyAstrophysics_GimenezAlcazar.pdf file_size: 1813456 relation: main_file success: 1 file_date_updated: 2026-03-02T14:51:57Z has_accepted_license: '1' intvolume: ' 706' language: - iso: eng month: '02' oa: 1 oa_version: Published Version publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' scopus_import: '1' status: public title: 'J-PAS: First identification, physical properties, and ionization efficiency of extreme emission line galaxies' tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 706 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '21450' abstract: - lang: eng text: Stellar wind mass loss of massive stars is often assumed to depend on their metallicity Z. Therefore, evolutionary models predict that massive stars in lower-Z environments are able to retain more of their hydrogen-rich layers and evolve into brighter cool supergiants (cool SGs; Teff < 7 kK). Surprisingly, in galaxies in the metallicity range 0.2 ≲ Z/Z⊙ ≲ 1.5, previous studies have not found a metallicity dependence on the upper luminosity limit Lmax of cool SGs. Here, we add four galaxies to the sample studied for this purpose with data from the Hubble Space Telescope and the James Webb Space Telescope (JWST). Observations of the extremely metal-poor dwarf galaxy I Zw 18 from JWST allow us to extend the studied metallicity range down to Z/Z⊙ ≈ 1/40. For cool SGs in all studied galaxies, including I Zw 18, we find a constant value of Lmax ≈ 105.6 L⊙, similar to literature results for 0.2 ≲ Z/Z⊙ ≲ 1.5. In I Zw 18 and the other studied galaxies, the presence of Wolf-Rayet stars has been previously inferred. Although we cannot rule out that some of them become intermediate-temperature objects, this paints a picture in which evolved stars with L > 105.6 L⊙ burn helium as hot, helium-rich stars down to extremely low metallicity. We argue that metallicity-independent late-phase mass loss would be the most likely mechanism responsible for this. Regardless of the exact stripping mechanism (winds or, for example, binary interaction), for the Early Universe our results imply a limitation on black hole masses and a contribution of stars born with M ≳ 30 M⊙ to its surprisingly strong nitrogen enrichment. We propose a scenario in which single stars at low metallicity emit sufficiently hard ionizing radiation to produce He II and C IV lines. In this scenario, late-phase metallicity-independent mass loss produces hot, helium-rich stars. Due to the well-understood metallicity dependence on the radiation-driven winds of hot stars, a window of opportunity would open below 0.2 Z⊙, where self-stripped helium-rich stars can exist without dense Wolf-Rayet winds that absorb hard ionizing radiation. acknowledgement: "We thank our anonymous referee for carefully reading the manuscript and providing a constructive report with helpful feedback. 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 #1233. The specific observations analyzed can be accessed via DOI: 10.17909/3c1d-6182. Moreover, this research is based in part on observations made with the NASA/ESA Hubble Space Telescope obtained from the\r\nSpace Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. These observations are associated with programs #13664, GO-10915, and DD-11307. This research was supported in part by grant NSF PHY-2309135 to the Kavli Institute for Theoretical Physics (KITP). LRP acknowledges support by grants PID2019-105552RB-C41 and PID2022-137779OB-C41 funded\r\nby MCIN/AEI/10.13039/501100011033 by “ERDF A way of making Europe”. LRP acknowledges support from grant PID2022-140483NB-C22 funded by MCIN/AEI/10.13039/501100011033." article_number: A116 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Abel full_name: Schootemeijer, Abel last_name: Schootemeijer - first_name: Ylva Louise Linsdotter full_name: Götberg, Ylva Louise Linsdotter id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d last_name: Götberg orcid: 0000-0002-6960-6911 - first_name: Norbert full_name: Langer, Norbert last_name: Langer - first_name: Giacomo full_name: Bortolini, Giacomo last_name: Bortolini - first_name: Alec S. full_name: Hirschauer, Alec S. last_name: Hirschauer - first_name: Lee full_name: Patrick, Lee last_name: Patrick citation: ama: Schootemeijer A, Götberg YLL, Langer N, Bortolini G, Hirschauer AS, Patrick L. A constant upper luminosity limit of cool supergiant stars down to the extremely low metallicity of I Zw 18. Astronomy & Astrophysics. 2026;707. doi:10.1051/0004-6361/202557675 apa: Schootemeijer, A., Götberg, Y. L. L., Langer, N., Bortolini, G., Hirschauer, A. S., & Patrick, L. (2026). A constant upper luminosity limit of cool supergiant stars down to the extremely low metallicity of I Zw 18. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557675 chicago: Schootemeijer, Abel, Ylva Louise Linsdotter Götberg, Norbert Langer, Giacomo Bortolini, Alec S. Hirschauer, and Lee Patrick. “A Constant Upper Luminosity Limit of Cool Supergiant Stars down to the Extremely Low Metallicity of I Zw 18.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557675. ieee: A. Schootemeijer, Y. L. L. Götberg, N. Langer, G. Bortolini, A. S. Hirschauer, and L. Patrick, “A constant upper luminosity limit of cool supergiant stars down to the extremely low metallicity of I Zw 18,” Astronomy & Astrophysics, vol. 707. EDP Sciences, 2026. ista: Schootemeijer A, Götberg YLL, Langer N, Bortolini G, Hirschauer AS, Patrick L. 2026. A constant upper luminosity limit of cool supergiant stars down to the extremely low metallicity of I Zw 18. Astronomy & Astrophysics. 707, A116. mla: Schootemeijer, Abel, et al. “A Constant Upper Luminosity Limit of Cool Supergiant Stars down to the Extremely Low Metallicity of I Zw 18.” Astronomy & Astrophysics, vol. 707, A116, EDP Sciences, 2026, doi:10.1051/0004-6361/202557675. short: A. Schootemeijer, Y.L.L. Götberg, N. Langer, G. Bortolini, A.S. Hirschauer, L. Patrick, Astronomy & Astrophysics 707 (2026). date_created: 2026-03-15T23:01:35Z date_published: 2026-03-01T00:00:00Z date_updated: 2026-03-16T09:07:55Z day: '01' ddc: - '520' department: - _id: YlGo doi: 10.1051/0004-6361/202557675 external_id: arxiv: - '2510.12594' file: - access_level: open_access checksum: 02a0cd932340207c96fdd3059490ad29 content_type: application/pdf creator: dernst date_created: 2026-03-16T09:05:06Z date_updated: 2026-03-16T09:05:06Z file_id: '21455' file_name: 2026_AstronomyAstrophysics_Schootemeijer.pdf file_size: 2102107 relation: main_file success: 1 file_date_updated: 2026-03-16T09:05:06Z has_accepted_license: '1' intvolume: ' 707' language: - iso: eng month: '03' oa: 1 oa_version: Published Version publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' scopus_import: '1' status: public title: A constant upper luminosity limit of cool supergiant stars down to the extremely low metallicity of I Zw 18 tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 707 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '21451' 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. 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.' article_number: A75 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Alberto full_name: Torralba Torregrosa, Alberto id: 018f0249-0e87-11f0-b167-cbce08fbd541 last_name: Torralba Torregrosa orcid: 0000-0001-5586-6950 - first_name: Jorryt J full_name: Matthee, Jorryt J id: 7439a258-f3c0-11ec-9501-9df22fe06720 last_name: Matthee orcid: 0000-0003-2871-127X - first_name: Gabriele full_name: Pezzulli, Gabriele last_name: Pezzulli - first_name: Rohan P. full_name: Naidu, Rohan P. last_name: Naidu - first_name: Yuzo full_name: Ishikawa, Yuzo last_name: Ishikawa - first_name: Gabriel B. full_name: Brammer, Gabriel B. last_name: Brammer - first_name: Seok Jun full_name: Chang, Seok Jun last_name: Chang - first_name: John full_name: Chisholm, John last_name: Chisholm - first_name: Anna full_name: De Graaff, Anna last_name: De Graaff - first_name: Francesco full_name: D’Eugenio, Francesco last_name: D’Eugenio - first_name: Claudia full_name: Di Cesare, Claudia id: 2d002343-372f-11ef-98ec-a164d20427cb last_name: Di Cesare - first_name: Anna Christina full_name: Eilers, Anna Christina last_name: Eilers - first_name: Jenny E. full_name: Greene, Jenny E. last_name: Greene - first_name: Max full_name: Gronke, Max last_name: Gronke - first_name: Edoardo full_name: Iani, Edoardo id: 4053390a-6b68-11ef-9828-a3b8adef8d0a last_name: Iani orcid: 0000-0001-8386-3546 - first_name: Vasily full_name: Kokorev, Vasily last_name: Kokorev - first_name: Gauri full_name: Kotiwale, Gauri id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875 last_name: Kotiwale - first_name: Ivan full_name: Kramarenko, Ivan id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4 last_name: Kramarenko orcid: 0000-0001-5346-6048 - first_name: Yilun full_name: Ma, Yilun last_name: Ma - first_name: Sara full_name: Mascia, Sara id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29 last_name: Mascia - first_name: Benjamín full_name: Navarrete, Benjamín id: aa14a535-50c9-11ef-b52e-e0c373d10148 last_name: Navarrete - first_name: Erica full_name: Nelson, Erica last_name: Nelson - first_name: Pascal full_name: Oesch, Pascal last_name: Oesch - first_name: Robert A. full_name: Simcoe, Robert A. last_name: Simcoe - first_name: Stijn full_name: Wuyts, Stijn last_name: Wuyts citation: 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. Astronomy & Astrophysics. 2026;707. doi:10.1051/0004-6361/202557537 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. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557537 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.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557537. ieee: A. Torralba Torregrosa et al., “The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings,” Astronomy & Astrophysics, vol. 707. EDP Sciences, 2026. 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 & Astrophysics. 707, A75. mla: Torralba Torregrosa, Alberto, et al. “The Warm Outer Layer of a Little Red Dot as the Source of [Fe Ii] and Collisional Balmer Lines with Scattering Wings.” Astronomy & Astrophysics, vol. 707, A75, EDP Sciences, 2026, doi:10.1051/0004-6361/202557537. 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 & Astrophysics 707 (2026). corr_author: '1' date_created: 2026-03-15T23:01:36Z date_published: 2026-03-01T00:00:00Z date_updated: 2026-03-16T10:59:16Z day: '01' ddc: - '520' department: - _id: JoMa doi: 10.1051/0004-6361/202557537 external_id: arxiv: - '2510.00103' file: - access_level: open_access checksum: fcab9cb3dcf1d68612e1fdc8191643c1 content_type: application/pdf creator: dernst date_created: 2026-03-16T10:57:49Z date_updated: 2026-03-16T10:57:49Z file_id: '21460' file_name: 2026_AstronomyAstrophysics_Torralba2.pdf file_size: 2510157 relation: main_file success: 1 file_date_updated: 2026-03-16T10:57:49Z has_accepted_license: '1' intvolume: ' 707' language: - iso: eng month: '03' oa: 1 oa_version: Published Version project: - _id: bd9b2118-d553-11ed-ba76-db24564edfea grant_number: '101076224' name: Young galaxies as tracers and agents of cosmic reionization publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' scopus_import: '1' status: public title: The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 707 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '21452' 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. 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)." article_number: A129 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Claudia full_name: Di Cesare, Claudia id: 2d002343-372f-11ef-98ec-a164d20427cb last_name: Di Cesare - first_name: Jorryt J full_name: Matthee, Jorryt J id: 7439a258-f3c0-11ec-9501-9df22fe06720 last_name: Matthee orcid: 0000-0003-2871-127X - first_name: Rohan P. full_name: Naidu, Rohan P. last_name: Naidu - first_name: Alberto full_name: Torralba, Alberto last_name: Torralba - first_name: Gauri full_name: Kotiwale, Gauri id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875 last_name: Kotiwale - first_name: Ivan full_name: Kramarenko, Ivan id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4 last_name: Kramarenko orcid: 0000-0001-5346-6048 - first_name: Jeremy full_name: Blaizot, Jeremy last_name: Blaizot - first_name: Joakim full_name: Rosdahl, Joakim last_name: Rosdahl - first_name: Joel full_name: Leja, Joel last_name: Leja - first_name: Edoardo full_name: Iani, Edoardo id: 4053390a-6b68-11ef-9828-a3b8adef8d0a last_name: Iani orcid: 0000-0001-8386-3546 - first_name: Angela full_name: Adamo, Angela last_name: Adamo - first_name: Alba full_name: Covelo-Paz, Alba last_name: Covelo-Paz - first_name: Lukas J. full_name: Furtak, Lukas J. last_name: Furtak - first_name: Kasper E. full_name: Heintz, Kasper E. last_name: Heintz - first_name: Sara full_name: Mascia, Sara id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29 last_name: Mascia - first_name: Benjamín full_name: Navarrete, Benjamín id: aa14a535-50c9-11ef-b52e-e0c373d10148 last_name: Navarrete - first_name: Pascal A. full_name: Oesch, Pascal A. last_name: Oesch - first_name: Michael full_name: Romano, Michael last_name: Romano - first_name: Irene full_name: Shivaei, Irene last_name: Shivaei - first_name: Sandro full_name: Tacchella, Sandro last_name: Tacchella 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. Astronomy & Astrophysics. 2026;707. doi:10.1051/0004-6361/202557790' 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. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557790' 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.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557790.' ieee: 'C. Di Cesare et al., “The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations,” Astronomy & Astrophysics, vol. 707. EDP Sciences, 2026.' 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 & Astrophysics. 707, A129.' mla: 'Di Cesare, Claudia, et al. “The Slope and Scatter of the Star-Forming Main Sequence at z ∼ 5: Reconciling Observations with Simulations.” Astronomy & Astrophysics, vol. 707, A129, EDP Sciences, 2026, doi:10.1051/0004-6361/202557790.' 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 & Astrophysics 707 (2026). corr_author: '1' date_created: 2026-03-15T23:01:36Z date_published: 2026-03-01T00:00:00Z date_updated: 2026-03-16T10:52:44Z day: '01' ddc: - '520' department: - _id: JoMa - _id: GradSch doi: 10.1051/0004-6361/202557790 external_id: arxiv: - '2510.19044' file: - access_level: open_access checksum: c056b00ce7324849754521fde10fb7ca content_type: application/pdf creator: dernst date_created: 2026-03-16T10:48:07Z date_updated: 2026-03-16T10:48:07Z file_id: '21459' file_name: 2026_AstronomyAstrophysics_DiCesare.pdf file_size: 1821411 relation: main_file success: 1 file_date_updated: 2026-03-16T10:48:07Z has_accepted_license: '1' intvolume: ' 707' language: - iso: eng month: '03' oa: 1 oa_version: Published Version project: - _id: bd9b2118-d553-11ed-ba76-db24564edfea grant_number: '101076224' name: Young galaxies as tracers and agents of cosmic reionization publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' scopus_import: '1' status: public title: 'The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations' tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 707 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '21481' abstract: - lang: eng text: 'The Hα emission line in galaxies is a powerful tracer of their recent star formation activity. With the advent of JWST, we are now able to routinely observe Hα in galaxies at high redshift (z ≳ 3) and thus measure their star formation rates (SFRs). However, using classical SFR(Hα) calibrations to derive the SFRs leads to biased results because high-redshift galaxies are commonly characterized by low metallicities and bursty star formation histories, affecting the conversion factor between the Hα luminosity (LHα) and the SFR. We developed a set of new SFR(Hα) calibrations that allowed us to predict the SFRs of Hα-emitters at z ≳ 3 with very little error. We used the SPHINX cosmological simulations to select a sample of star-forming galaxies representative of the Hα-emitter population observed with JWST. We then derived linear corrections to the classical SFR(Hα) calibrations that took variations in the physical properties (e.g., stellar metallicities) among individual galaxies into account. We obtained two new SFR(Hα) calibrations that compared to the classical calibrations reduce the root mean squared error (RMSE) in the predicted SFRs by ΔRMSE ≈ 0.04 dex and ΔRMSE ≈ 0.06 dex, respectively. Using the recent JWST NIRCam/grism observations of Hα-emitters at z ∼ 6, we show that the new calibrations affect the high-redshift galaxy population statistics: (i) the estimated cosmic SFR density decreases by ΔρSFR ≈ 12%, and (ii) the observed slope of the star formation main sequence increases by Δ∂logSFR/∂logM★ = 0.08 ± 0.02.' acknowledgement: "We thank the anonymous referee for the insightful comments that helped improve the manuscript. We also thank Thibault Garel, Pascal Oesch, Irene Shivaei, Charlotte Simmonds, Andrew Hopkins, Daniel Schaerer, and Rashmi Gottumukkala for useful comments and productive discussions. We gratefully acknowledge support from the CBPsmn (PSMN, Pôle Scientifique de Modélisation Numérique) of the ENS de Lyon for the computing resources.\r\nFunded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. This work made extensive use of several open-source software packages, and we gratefully acknowledge the efforts of their authors: numpy (Harris et al. 2020), astropy (Astropy Collaboration 2022), matplotlib (Hunter 2007), ipython (Perez & Granger 2007), and scikit-learn (Pedregosa et al. 2011)." article_number: A184 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Ivan full_name: Kramarenko, Ivan id: 9a9394cb-3200-11ee-973b-f5ba2a8b16e4 last_name: Kramarenko orcid: 0000-0001-5346-6048 - first_name: J. full_name: Rosdahl, J. last_name: Rosdahl - first_name: J. full_name: Blaizot, J. last_name: Blaizot - first_name: Jorryt J full_name: Matthee, Jorryt J id: 7439a258-f3c0-11ec-9501-9df22fe06720 last_name: Matthee orcid: 0000-0003-2871-127X - first_name: H. full_name: Katz, H. last_name: Katz - first_name: Claudia full_name: Di Cesare, Claudia id: 2d002343-372f-11ef-98ec-a164d20427cb last_name: Di Cesare citation: ama: Kramarenko I, Rosdahl J, Blaizot J, Matthee JJ, Katz H, Di Cesare C. H α as a tracer of star formation in the SPHINX cosmological simulations. Astronomy & Astrophysics. 2026;707. doi:10.1051/0004-6361/202557114 apa: Kramarenko, I., Rosdahl, J., Blaizot, J., Matthee, J. J., Katz, H., & Di Cesare, C. (2026). H α as a tracer of star formation in the SPHINX cosmological simulations. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557114 chicago: Kramarenko, Ivan, J. Rosdahl, J. Blaizot, Jorryt J Matthee, H. Katz, and Claudia Di Cesare. “H α as a Tracer of Star Formation in the SPHINX Cosmological Simulations.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557114. ieee: I. Kramarenko, J. Rosdahl, J. Blaizot, J. J. Matthee, H. Katz, and C. Di Cesare, “H α as a tracer of star formation in the SPHINX cosmological simulations,” Astronomy & Astrophysics, vol. 707. EDP Sciences, 2026. ista: Kramarenko I, Rosdahl J, Blaizot J, Matthee JJ, Katz H, Di Cesare C. 2026. H α as a tracer of star formation in the SPHINX cosmological simulations. Astronomy & Astrophysics. 707, A184. mla: Kramarenko, Ivan, et al. “H α as a Tracer of Star Formation in the SPHINX Cosmological Simulations.” Astronomy & Astrophysics, vol. 707, A184, EDP Sciences, 2026, doi:10.1051/0004-6361/202557114. short: I. Kramarenko, J. Rosdahl, J. Blaizot, J.J. Matthee, H. Katz, C. Di Cesare, Astronomy & Astrophysics 707 (2026). corr_author: '1' date_created: 2026-03-23T14:58:03Z date_published: 2026-03-05T00:00:00Z date_updated: 2026-03-23T15:46:31Z day: '05' ddc: - '520' department: - _id: JoMa doi: 10.1051/0004-6361/202557114 external_id: arxiv: - '2509.05403' file: - access_level: open_access checksum: 7429076b381dd498084f40ffd199e714 content_type: application/pdf creator: dernst date_created: 2026-03-23T15:44:09Z date_updated: 2026-03-23T15:44:09Z file_id: '21492' file_name: 2026_AstronomyAstrophysics_Kramarenko.pdf file_size: 904565 relation: main_file success: 1 file_date_updated: 2026-03-23T15:44:09Z has_accepted_license: '1' intvolume: ' 707' language: - iso: eng month: '03' oa: 1 oa_version: Published Version project: - _id: bd9b2118-d553-11ed-ba76-db24564edfea grant_number: '101076224' name: Young galaxies as tracers and agents of cosmic reionization publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' status: public title: H α as a tracer of star formation in the SPHINX cosmological simulations tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 707 year: '2026' ... --- OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '21160' abstract: - lang: eng text: "Context. AM Canum Venaticorum (AM CVn) stars are ultra-compact binary systems composed of a white dwarf primary accreting from a hydrogen-deficient donor. They play a crucial role in astrophysics as potential progenitors of Type Ia supernovae and as laboratories for gravitational wave studies. However, their formation and evolutionary history remain incomplete. Three formation channels have been discussed in the literature: the white dwarf, He-star, and cataclysmic variable channels.\r\n\r\nAims. The chemical composition of the accretor atmosphere reflects the material transferred from the donor. In this work we took the first accurate measurements of the fundamental parameters of the accreting white dwarf in ZTF J225237.05−051917.4, including the abundances of key elements such as carbon, nitrogen, and silicon, by analysing ultraviolet spectra obtained with the Hubble Space Telescope (HST). These measurements provide new insight into the evolutionary history of the system and, together with existing optical observations, establish it as a benchmark to develop our pipeline, paving the way for its application to a larger sample of AM CVn systems.\r\n\r\nMethods. We determined the binary parameters through photometric analysis and constrained the atmospheric parameters of the white dwarf accretor, including its effective temperature, surface gravity, and chemical abundances, by fitting the HST ultraviolet spectrum with synthetic spectral models. We then inferred the system’s formation channel by comparing the results with theoretical evolutionary models.\r\n\r\nResults. According to our measurements, the accretor’s effective temperature (Teff) is 23 300 ± 600 K and the surface gravity (log g) is 8.4 ± 0.3, which imply an accretor mass (MWD) of 0.86 ± 0.16 M⊙. We find a high nitrogen-to-carbon abundance ratio by mass of > 153.\r\n\r\nConclusions. The accretor is significantly hotter than previous estimates based on simplified blackbody fits to the spectral energy distribution, underscoring the importance of detailed spectral modelling for accurately determining system parameters. Our results show that ultraviolet spectroscopy is well suited to constraining the formation channels of AM CVn systems. Of the three proposed formation channels, the He-star channel can be excluded given the high nitrogen-to-carbon ratio. Our results are consistent with both the white dwarf and cataclysmic variable channels." acknowledgement: "We thank Lars Bildsten for valuable insights and discussions. We acknowledge with thanks the variable star observations from the\r\nAAVSO International Database contributed by observers worldwide and used in this research. We thank the members of the Spanish Observers of Supernovae\r\n(ObSN) group for their valuable photometric contributions. This research was\r\nsupported by Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy – EXC 2121 “Quantum Universe”\r\n– 390833306. Co-funded by the European Union (ERC, CompactBINARIES,\r\n101078773). Views and opinions expressed are however those of the author(s)\r\nonly and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority\r\ncan be held responsible for them. DB acknowledges support from the São Paulo\r\nResearch Foundation (FAPESP), Brazil, Process Numbers #2024/03736-2 and\r\n#2025/00817-4. MRS is supported by Fondecyt (grant 1221059). MJG acknowledges support from the European Research Council through ERC Advanced\r\nGrant No. 101054731, from the National Aeronautics and Space Administration under grants 80NSSC24K0436, 80NSSC22K0479, and 80NSSC24K0380,\r\nand from the National Science Foundation under grant AST-2205736. PJG\r\nis supported by NRF SARChI grant 111692. PR-G acknowledges support by\r\nthe Agencia Estatal de Investigación del Ministerio de Ciencia e Innovación\r\n(MCIN/AEI) and the European Regional Development Fund (ERDF) under grant\r\nPID2021–124879NB–I00. DS is supported by the UK Science and Technology Facilities Council (STFC, grant numbers ST/T007184/1, ST/T003103/1,\r\nand ST/T000406/1). OT acknowledges Proyectos Internos USM 2025, PI-LII2025-03. GT was supported by grants IN109723 from the Programa de Apoyo a\r\nProyectos de Investigación e Innovación Tecnológica (PAPIIT). This project has\r\nreceived funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 101020057)." article_number: A14 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: W. full_name: Yu, W. last_name: Yu - first_name: A. F. full_name: Pala, A. F. last_name: Pala - first_name: T. full_name: Kupfer, T. last_name: Kupfer - first_name: B. T. full_name: Gänsicke, B. T. last_name: Gänsicke - first_name: D. full_name: Koester, D. last_name: Koester - first_name: D. full_name: Belloni, D. last_name: Belloni - first_name: T. L.S. full_name: Wong, T. L.S. last_name: Wong - first_name: M. R. full_name: Schreiber, M. R. last_name: Schreiber - first_name: Joannes C full_name: van Roestel, Joannes C id: 4d122fc8-6083-11f0-87a5-97d68b860333 last_name: van Roestel - first_name: A. J. full_name: Brown, A. J. last_name: Brown - first_name: E. O. full_name: Waagen, E. O. last_name: Waagen - first_name: J. L. full_name: González-Carballo, J. L. last_name: González-Carballo - first_name: S. full_name: Bednarz, S. last_name: Bednarz - first_name: K. full_name: Bernacki, K. last_name: Bernacki - first_name: D. full_name: De Martino, D. last_name: De Martino - first_name: E. full_name: Fernández Mañanes, E. last_name: Fernández Mañanes - first_name: R. full_name: González Farfán, R. last_name: González Farfán - first_name: M. J. full_name: Green, M. J. last_name: Green - first_name: P. J. full_name: Groot, P. J. last_name: Groot - first_name: F. J. full_name: Hambsch, F. J. last_name: Hambsch - first_name: C. full_name: Knigge, C. last_name: Knigge - first_name: J. L. full_name: Martin-Velasco, J. L. last_name: Martin-Velasco - first_name: M. full_name: Morales-Aimar, M. last_name: Morales-Aimar - first_name: G. full_name: Myers, G. last_name: Myers - first_name: R. full_name: Naves Nogues, R. last_name: Naves Nogues - first_name: R. full_name: Poggiani, R. last_name: Poggiani - first_name: A. full_name: Popowicz, A. last_name: Popowicz - first_name: G. full_name: Ramsay, G. last_name: Ramsay - first_name: E. full_name: Reina-Lorenz, E. last_name: Reina-Lorenz - first_name: P. full_name: Rodríguez-Gil, P. last_name: Rodríguez-Gil - first_name: J. L. full_name: Salto-González, J. L. last_name: Salto-González - first_name: E. M. full_name: Sion, E. M. last_name: Sion - first_name: D. full_name: Steeghs, D. last_name: Steeghs - first_name: P. full_name: Szkody, P. last_name: Szkody - first_name: O. full_name: Toloza, O. last_name: Toloza - first_name: G. full_name: Tovmassian, G. last_name: Tovmassian citation: ama: 'Yu W, Pala AF, Kupfer T, et al. The evolutionary history of ultra-compact accreting binaries: I. Chemical abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy. Astronomy & Astrophysics. 2026;706. doi:10.1051/0004-6361/202557568' apa: 'Yu, W., Pala, A. F., Kupfer, T., Gänsicke, B. T., Koester, D., Belloni, D., … Tovmassian, G. (2026). The evolutionary history of ultra-compact accreting binaries: I. Chemical abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557568' chicago: 'Yu, W., A. F. Pala, T. Kupfer, B. T. Gänsicke, D. Koester, D. Belloni, T. L.S. Wong, et al. “The Evolutionary History of Ultra-Compact Accreting Binaries: I. Chemical Abundances and the Formation Channel of the Eclipsing AM CVn System ZTF J225237.05-051917.4 from HST Spectroscopy.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557568.' ieee: 'W. Yu et al., “The evolutionary history of ultra-compact accreting binaries: I. Chemical abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy,” Astronomy & Astrophysics, vol. 706. EDP Sciences, 2026.' ista: 'Yu W, Pala AF, Kupfer T, Gänsicke BT, Koester D, Belloni D, Wong TLS, Schreiber MR, van Roestel JC, Brown AJ, Waagen EO, González-Carballo JL, Bednarz S, Bernacki K, De Martino D, Fernández Mañanes E, González Farfán R, Green MJ, Groot PJ, Hambsch FJ, Knigge C, Martin-Velasco JL, Morales-Aimar M, Myers G, Naves Nogues R, Poggiani R, Popowicz A, Ramsay G, Reina-Lorenz E, Rodríguez-Gil P, Salto-González JL, Sion EM, Steeghs D, Szkody P, Toloza O, Tovmassian G. 2026. The evolutionary history of ultra-compact accreting binaries: I. Chemical abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy. Astronomy & Astrophysics. 706, A14.' mla: 'Yu, W., et al. “The Evolutionary History of Ultra-Compact Accreting Binaries: I. Chemical Abundances and the Formation Channel of the Eclipsing AM CVn System ZTF J225237.05-051917.4 from HST Spectroscopy.” Astronomy & Astrophysics, vol. 706, A14, EDP Sciences, 2026, doi:10.1051/0004-6361/202557568.' short: W. Yu, A.F. Pala, T. Kupfer, B.T. Gänsicke, D. Koester, D. Belloni, T.L.S. Wong, M.R. Schreiber, J.C. van Roestel, A.J. Brown, E.O. Waagen, J.L. González-Carballo, S. Bednarz, K. Bernacki, D. De Martino, E. Fernández Mañanes, R. González Farfán, M.J. Green, P.J. Groot, F.J. Hambsch, C. Knigge, J.L. Martin-Velasco, M. Morales-Aimar, G. Myers, R. Naves Nogues, R. Poggiani, A. Popowicz, G. Ramsay, E. Reina-Lorenz, P. Rodríguez-Gil, J.L. Salto-González, E.M. Sion, D. Steeghs, P. Szkody, O. Toloza, G. Tovmassian, Astronomy & Astrophysics 706 (2026). das_tickbox: '1' date_created: 2026-02-08T23:02:49Z date_published: 2026-02-01T00:00:00Z date_updated: 2026-07-08T06:38:46Z day: '01' ddc: - '520' department: - _id: IlCa doi: 10.1051/0004-6361/202557568 external_id: arxiv: - '2512.04147' file: - access_level: open_access checksum: 2faec710fd04f927aa43deb57e35c9b2 content_type: application/pdf creator: dernst date_created: 2026-02-16T09:33:56Z date_updated: 2026-02-16T09:33:56Z file_id: '21227' file_name: 2026_AstronomyAstrophysics_Yu.pdf file_size: 4020466 relation: main_file success: 1 file_date_updated: 2026-02-16T09:33:56Z has_accepted_license: '1' intvolume: ' 706' language: - iso: eng month: '02' oa: 1 oa_version: Published Version publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' scopus_import: '1' status: public title: 'The evolutionary history of ultra-compact accreting binaries: I. Chemical abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy' tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 706 year: '2026' ... --- OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '21045' 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.' 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.' article_number: A147 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Alberto full_name: Torralba Torregrosa, Alberto id: 018f0249-0e87-11f0-b167-cbce08fbd541 last_name: Torralba Torregrosa orcid: 0000-0001-5586-6950 - first_name: Jorryt J full_name: Matthee, Jorryt J id: 7439a258-f3c0-11ec-9501-9df22fe06720 last_name: Matthee orcid: 0000-0003-2871-127X - first_name: Gabriele full_name: Pezzulli, Gabriele last_name: Pezzulli - first_name: Tanya full_name: Urrutia, Tanya last_name: Urrutia - first_name: Max full_name: Gronke, Max last_name: Gronke - first_name: Sara full_name: Mascia, Sara id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29 last_name: Mascia - first_name: Francesco full_name: D’Eugenio, Francesco last_name: D’Eugenio - first_name: Claudia full_name: Di Cesare, Claudia id: 2d002343-372f-11ef-98ec-a164d20427cb last_name: Di Cesare - first_name: Anna Christina full_name: Eilers, Anna Christina last_name: Eilers - first_name: Jenny E. full_name: Greene, Jenny E. last_name: Greene - first_name: Edoardo full_name: Iani, Edoardo id: 4053390a-6b68-11ef-9828-a3b8adef8d0a last_name: Iani orcid: 0000-0001-8386-3546 - first_name: Yuzo full_name: Ishikawa, Yuzo last_name: Ishikawa - first_name: Ruari full_name: Mackenzie, Ruari last_name: Mackenzie - first_name: Rohan P. full_name: Naidu, Rohan P. last_name: Naidu - first_name: Benjamín full_name: Navarrete, Benjamín id: aa14a535-50c9-11ef-b52e-e0c373d10148 last_name: Navarrete - first_name: Gauri full_name: Kotiwale, Gauri id: 1438afc8-1ff6-11ee-9fa6-cd4a75d66875 last_name: Kotiwale 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. Astronomy & Astrophysics. 2026;705. doi:10.1051/0004-6361/202555596 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. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202555596 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.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202555596. ieee: A. Torralba Torregrosa et al., “A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth,” Astronomy & Astrophysics, vol. 705. EDP Sciences, 2026. 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 & Astrophysics. 705, A147. 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.” Astronomy & Astrophysics, vol. 705, A147, EDP Sciences, 2026, doi:10.1051/0004-6361/202555596. 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 & Astrophysics 705 (2026). corr_author: '1' das_tickbox: '1' date_created: 2026-01-25T23:01:41Z date_published: 2026-01-14T00:00:00Z date_updated: 2026-07-08T06:38:23Z day: '14' ddc: - '520' department: - _id: JoMa - _id: GradSch doi: 10.1051/0004-6361/202555596 external_id: arxiv: - '2505.09542' file: - access_level: open_access checksum: 3782e03bc0843438aae8487f6af779c5 content_type: application/pdf creator: dernst date_created: 2026-02-16T07:35:03Z date_updated: 2026-02-16T07:35:03Z file_id: '21224' file_name: 2026_AstronomyAstrophysics_Torralba.pdf file_size: 2259914 relation: main_file success: 1 file_date_updated: 2026-02-16T07:35:03Z has_accepted_license: '1' intvolume: ' 705' language: - iso: eng month: '01' oa: 1 oa_version: Published Version project: - _id: bd9b2118-d553-11ed-ba76-db24564edfea grant_number: '101076224' name: Young galaxies as tracers and agents of cosmic reionization publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' scopus_import: '1' status: public title: A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 705 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '21658' abstract: - lang: eng text: Dipolar (ℓ = 1) mixed modes have revealed a surprisingly weak differential rotation between the core and the envelope of evolved solar-like stars. Quadrupolar (ℓ = 2) mixed modes also contain information regarding internal dynamics but are very rarely characterised due to their low amplitude and the challenging identification of adjacent or overlapping rotationally split multiplets affected by near-degeneracy effects. We aim to extend the broadly used asymptotic seismic diagnostics beyond ℓ = 1 mixed modes by developing an analogue asymptotic description of ℓ = 2 mixed modes while explicitly accounting for near-degeneracy effects that distort their rotational multiplets. We have derived a new asymptotic formulation of near-degenerate mixed ℓ = 2 modes that describes off-diagonal terms representing the interaction between modes of adjacent radial orders. This formalism, expressed directly in the mixed-mode basis, provides analytical expressions for the near-degeneracy effects. We implemented the formalism within a global Bayesian mode-fitting framework for a direct fit of all ℓ = 0, 1, 2 modes in the power spectrum density. We were able to asymptotically model the asymmetric rotational splitting present in various radial orders of ℓ = 2 modes observed in young red giant stars without the need for any numerical stellar modelling. We applied our formalism to the Kepler target KIC 7341231, and it yielded core and envelope rotation rates consistent with previous numerical modelling while providing improved constraints from the global and model-independent approach. We also characterised the new target, KIC 8179973, measuring its rotation rate and mixed-mode parameters for the first time. As our framework relies on a direct global fit, it allows for much better precision on the asteroseismic parameters and rotation rate estimates than standard methods, yielding better constraints for rotation inversions. We have placed the first observational constraints on the asymptotic ℓ = 2 mixed-mode parameters (ΔΠ2, q2, and εg, 2), thus paving the way towards the use of asymptotic seismology beyond ℓ = 1 mixed modes. acknowledgement: 'We thank the referee for their careful and constructive report, which has substantially enhanced both the quality and clarity of the manuscript. L. Bugnet and L. Einramhof gratefully acknowledge support from the European Research Council (ERC) under the Horizon Europe programme (Calcifer; Starting Grant agreement N°101165631). While partially funded by the European Union, 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. Neither the European Union nor the granting authority can be held responsible for them. The authors acknowledge the great support and feedback provided during the redaction of this article by Pr. Rafael García and Pr. Savita Mathur. We would also like to thank Dr. Emily Hatt for her insights on uncertainty estimates. The authors also thank the members of the Asteroseismology and Stellar Dynamics group of the Institute of Science and Technology Austria (ISTA) for very useful discussions: L. Barrault, S.B. Das, K. Smith. This paper includes data collected by the Kepler mission and obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the Kepler mission is provided by the NASA Science Mission Directorate. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. Software: AstroPy (Astropy Collaboration 2013, 2018), Matplotlib (Hunter 2007), NumPy (Harris et al. 2020), SciPy (Virtanen et al. 2020), emcee (Foreman-Mackey et al. 2013), celerite (Foreman-Mackey et al. 2017), slepc4py (Dalcin et al. 2011; Hernandez et al. 2005), KADACS (García et al. 2011), sloscillations (Kuszlewicz et al. 2019, 2023).' article_number: A321 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Bastien Raymond Bernard full_name: Liagre, Bastien Raymond Bernard id: 662f1873-cab4-11f0-a719-8087d302868d last_name: Liagre - first_name: Aayush A full_name: Desai, Aayush A id: 502cfd30-32c1-11ee-a9a4-d8dad5c6739e last_name: Desai - first_name: Lukas full_name: Einramhof, Lukas id: f1497a1a-72ef-11ef-b75a-fd877bbf6e8c last_name: Einramhof - first_name: Lisa Annabelle full_name: Bugnet, Lisa Annabelle id: d9edb345-f866-11ec-9b37-d119b5234501 last_name: Bugnet orcid: 0000-0003-0142-4000 citation: ama: 'Liagre BRB, Desai AA, Einramhof L, Bugnet LA. Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting. Astronomy & Astrophysics. 2026;707. doi:10.1051/0004-6361/202558023' apa: 'Liagre, B. R. B., Desai, A. A., Einramhof, L., & Bugnet, L. A. (2026). Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202558023' chicago: 'Liagre, Bastien Raymond Bernard, Aayush A Desai, Lukas Einramhof, and Lisa Annabelle Bugnet. “Near-Degeneracy Effects in Quadrupolar Mixed Modes: From an Asymptotic Description to Data Fitting.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202558023.' ieee: 'B. R. B. Liagre, A. A. Desai, L. Einramhof, and L. A. Bugnet, “Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting,” Astronomy & Astrophysics, vol. 707. EDP Sciences, 2026.' ista: 'Liagre BRB, Desai AA, Einramhof L, Bugnet LA. 2026. Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting. Astronomy & Astrophysics. 707, A321.' mla: 'Liagre, Bastien Raymond Bernard, et al. “Near-Degeneracy Effects in Quadrupolar Mixed Modes: From an Asymptotic Description to Data Fitting.” Astronomy & Astrophysics, vol. 707, A321, EDP Sciences, 2026, doi:10.1051/0004-6361/202558023.' short: B.R.B. Liagre, A.A. Desai, L. Einramhof, L.A. Bugnet, Astronomy & Astrophysics 707 (2026). corr_author: '1' das_tickbox: '1' date_created: 2026-04-05T22:01:32Z date_published: 2026-03-01T00:00:00Z date_updated: 2026-07-08T06:39:05Z day: '01' ddc: - '520' department: - _id: LiBu - _id: IlCa - _id: GradSch doi: 10.1051/0004-6361/202558023 external_id: arxiv: - '2511.05314 ' file: - access_level: open_access checksum: 560cac19dc70184626b85e71a26ee22e content_type: application/pdf creator: dernst date_created: 2026-04-07T09:00:50Z date_updated: 2026-04-07T09:00:50Z file_id: '21664' file_name: 2026_AstronomyAstrophysics_Liagre.pdf file_size: 12287607 relation: main_file success: 1 file_date_updated: 2026-04-07T09:00:50Z has_accepted_license: '1' intvolume: ' 707' language: - iso: eng month: '03' oa: 1 oa_version: Published Version publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' scopus_import: '1' status: public title: 'Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting' tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 707 year: '2026' ... --- OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '22369' abstract: - lang: eng text: The high-redshift progenitors of present-day galaxy clusters are believed to substantially contribute to the global star formation rate density and drive the large-scale reionisation of the Universe. Here we present a blind and unbiased search for and characterisation of galaxy overdensities during the reionisation epoch at redshifts z ∼ 5.5 − 7 based on rest-frame optical JWST/NIRCam grism spectroscopy of the Abell 2744 lensing field as part of the JWST All the Little Things (ALT) survey. Using a physically motivated, cosmological inference friends-of-friends (FoF) algorithm, we identified six galaxy overdensities, including five robust systems at z = 5.66–6.77. They are all characterised by total halo masses of Mhalo ≳ 1011 M⊙, inferred from a range of proxies. We find that the galaxy members in these overdense environments are on average less massive though equally metal-rich, and generally comprised of younger stellar populations, as indicated by their bluer spectral slopes and less prominent Balmer breaks compared to field galaxies at similar redshifts. Further, we use this novel rest-frame optical selection of galaxy proto-clusters to infer the fraction and 3D distribution of strong Lyman-α emitters (LAEs) and damped Lyman-α absorbers (DLAs) in the overdensity environments. We find that two out of the six galaxy overdensities have excess H I absorption compared to the field average, while the other four are consistent within their large scatter in density. These results present the first direct observational constraints on the tomography of the dense, neutral gas reservoirs in large-scale galaxy overdensities at z > 5 and highlight the limitations of pre-JWST searches for reionisation-era galaxy overdensities relying on the detection of strong LAEs alone. acknowledgement: 'We would like to thank the anonymous referee for their positive and constructive report and all the observers world-wide for their substantial effort in securing all the public JWST data that were essential for this work. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. KEH acknowledges support from the Independent Research Fund Denmark (DFF) under grant 5251-00009B and co-funding by the European Union (ERC, HEAVYMETAL, 101071865). 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. 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 (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. We used the following software for this work: Python, and the scientific Python ecosystem, in particular NumPy (Harris et al. 2020), SciPy (including cKDTree) (Virtanen et al. 2021), Matplotlib (Hunter 2007), and Astropy (Astropy Collaboration 2013, 2018, 2022).' article_number: A290 article_processing_charge: No article_type: original author: - first_name: Chamilla full_name: Terp, Chamilla last_name: Terp - first_name: Kasper E. full_name: Heintz, Kasper E. last_name: Heintz - first_name: Jorryt J full_name: Matthee, Jorryt J id: 7439a258-f3c0-11ec-9501-9df22fe06720 last_name: Matthee orcid: 0000-0003-2871-127X - first_name: Rohan P. full_name: Naidu, Rohan P. last_name: Naidu - first_name: Pascal A. full_name: Oesch, Pascal A. last_name: Oesch - first_name: Callum full_name: Witten, Callum last_name: Witten - first_name: Daichi full_name: Kashino, Daichi last_name: Kashino - first_name: Clara L. full_name: Pollock, Clara L. last_name: Pollock - first_name: Claudia full_name: Di Cesare, Claudia id: 2d002343-372f-11ef-98ec-a164d20427cb last_name: Di Cesare - first_name: Alberto full_name: Torralba Torregrosa, Alberto id: 018f0249-0e87-11f0-b167-cbce08fbd541 last_name: Torralba Torregrosa orcid: 0000-0001-5586-6950 citation: ama: 'Terp C, Heintz KE, Matthee JJ, et al. All the massive galaxy overdensities during reionisation: JWST rest-frame optical selection reveals young, chemically evolved galaxies embedded in dense, neutral gas at z > 5. Astronomy & Astrophysics. 2026;710. doi:10.1051/0004-6361/202659436' apa: 'Terp, C., Heintz, K. E., Matthee, J. J., Naidu, R. P., Oesch, P. A., Witten, C., … Torralba Torregrosa, A. (2026). All the massive galaxy overdensities during reionisation: JWST rest-frame optical selection reveals young, chemically evolved galaxies embedded in dense, neutral gas at z > 5. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202659436' chicago: 'Terp, Chamilla, Kasper E. Heintz, Jorryt J Matthee, Rohan P. Naidu, Pascal A. Oesch, Callum Witten, Daichi Kashino, Clara L. Pollock, Claudia Di Cesare, and Alberto Torralba Torregrosa. “All the Massive Galaxy Overdensities during Reionisation: JWST Rest-Frame Optical Selection Reveals Young, Chemically Evolved Galaxies Embedded in Dense, Neutral Gas at z > 5.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202659436.' ieee: 'C. Terp et al., “All the massive galaxy overdensities during reionisation: JWST rest-frame optical selection reveals young, chemically evolved galaxies embedded in dense, neutral gas at z > 5,” Astronomy & Astrophysics, vol. 710. EDP Sciences, 2026.' ista: 'Terp C, Heintz KE, Matthee JJ, Naidu RP, Oesch PA, Witten C, Kashino D, Pollock CL, Di Cesare C, Torralba Torregrosa A. 2026. All the massive galaxy overdensities during reionisation: JWST rest-frame optical selection reveals young, chemically evolved galaxies embedded in dense, neutral gas at z > 5. Astronomy & Astrophysics. 710, A290.' mla: 'Terp, Chamilla, et al. “All the Massive Galaxy Overdensities during Reionisation: JWST Rest-Frame Optical Selection Reveals Young, Chemically Evolved Galaxies Embedded in Dense, Neutral Gas at z > 5.” Astronomy & Astrophysics, vol. 710, A290, EDP Sciences, 2026, doi:10.1051/0004-6361/202659436.' short: C. Terp, K.E. Heintz, J.J. Matthee, R.P. Naidu, P.A. Oesch, C. Witten, D. Kashino, C.L. Pollock, C. Di Cesare, A. Torralba Torregrosa, Astronomy & Astrophysics 710 (2026). das_tickbox: '1' dataavailabilitystatement: The specific observations analysed in this work can be accessed via https://doi.org/10.5281/zenodo.13871850 date_created: 2026-07-19T22:01:47Z date_published: 2026-06-01T00:00:00Z date_updated: 2026-07-20T13:42:20Z day: '01' ddc: - '520' department: - _id: JoMa doi: 10.1051/0004-6361/202659436 file: - access_level: open_access checksum: 0a63db666cfac8e4e6271b75419a26f2 content_type: application/pdf creator: dernst date_created: 2026-07-20T13:41:19Z date_updated: 2026-07-20T13:41:19Z file_id: '22378' file_name: 2026_AstronomyAstrophysics_Terp.pdf file_size: 6156048 relation: main_file success: 1 file_date_updated: 2026-07-20T13:41:19Z has_accepted_license: '1' intvolume: ' 710' language: - iso: eng month: '06' oa: 1 oa_version: Published Version publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' researchdata_availability: yes scopus_import: '1' status: public supplementarymaterial: yes title: 'All the massive galaxy overdensities during reionisation: JWST rest-frame optical selection reveals young, chemically evolved galaxies embedded in dense, neutral gas at z > 5' tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 710 year: '2026' ... --- OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '22381' abstract: - lang: eng text: "Context. X-ray binaries exhibit complex variability patterns studied in the power spectrum. These include the broadband noise (BBN)\r\ncomponents and various types of narrow components called quasi-periodic oscillations (QPOs). There is currently no consensus about\r\nwhat determines the presence or absence of the BBN or what generates the QPOs. Many believe that QPO generation is due to framedragging effects caused by Lense–Thirring torques.\r\nAims. We investigated the potential impact of frame-dragging effects on the accretion disk itself. In particular, we focused on its\r\nimpact on the observed variability and on the presence (and types) of associated QPOs.\r\nMethods. We made analytical estimates to assess the potential presence of a geometric warp in the inner accretion disk during state\r\ntransitions.\r\nResults. We show that the presence of a warp can modify the spectral-timing properties in a way that matches the observed transition\r\nbetween QPO types during outbursts. We also discuss the peculiar case of Cyg X-1, as well as how the hard-to-soft transition could\r\nbe driven by the warp itself.\r\nConclusions. The (expected) emergence of a warp provides a consistent explanation for the evolution of both the BBN and the QPO\r\nproperties during state transitions. This offers a first path toward unifying the variability of black hole X-ray binaries." acknowledgement: "GM acknowledges support from the Polish National Science Center grant 2023/48/Q/ST9/00138 and the Academy of Finland grant 355672. The authors thank the Editor for their insightful comments and effective stewardship of the review process. SGDT acknowledges support under\r\nSTFC Grant ST/X001113/1. This work made use of the python packages\r\nMatplotlib (Hunter 2007), NumPy (Harris et al. 2020), and Stingray v2.2\r\n(Huppenkothen et al. 2019; Bachetti et al. 2024b,a)." article_number: A387 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: G. full_name: Marcel, G. last_name: Marcel - first_name: S. G. D. full_name: Turner, S. G. D. last_name: Turner - first_name: B. J. full_name: Ricketts, B. J. last_name: Ricketts - first_name: V. full_name: López-Barquero, V. last_name: López-Barquero - first_name: D. J. K. full_name: Buisson, D. J. K. last_name: Buisson - first_name: F. full_name: Vincentelli, F. last_name: Vincentelli - first_name: M. full_name: Middleton, M. last_name: Middleton - first_name: C.S. full_name: Reynolds, C.S. last_name: Reynolds - first_name: Mark full_name: Avara, Mark id: 24edc561-7790-11f0-acf5-82cd0823fe7e last_name: Avara citation: ama: 'Marcel G, Turner SGD, Ricketts BJ, et al. Disk warping and black hole X-ray binaries: I. Tentative unification of low-frequency quasi-periodic oscillations. Astronomy & Astrophysics. 2026;710. doi:10.1051/0004-6361/202558103' apa: 'Marcel, G., Turner, S. G. D., Ricketts, B. J., López-Barquero, V., Buisson, D. J. K., Vincentelli, F., … Avara, M. (2026). Disk warping and black hole X-ray binaries: I. Tentative unification of low-frequency quasi-periodic oscillations. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202558103' chicago: 'Marcel, G., S. G. D. Turner, B. J. Ricketts, V. López-Barquero, D. J. K. Buisson, F. Vincentelli, M. Middleton, C.S. Reynolds, and Mark Avara. “Disk Warping and Black Hole X-Ray Binaries: I. Tentative Unification of Low-Frequency Quasi-Periodic Oscillations.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202558103.' ieee: 'G. Marcel et al., “Disk warping and black hole X-ray binaries: I. Tentative unification of low-frequency quasi-periodic oscillations,” Astronomy & Astrophysics, vol. 710. EDP Sciences, 2026.' ista: 'Marcel G, Turner SGD, Ricketts BJ, López-Barquero V, Buisson DJK, Vincentelli F, Middleton M, Reynolds CS, Avara M. 2026. Disk warping and black hole X-ray binaries: I. Tentative unification of low-frequency quasi-periodic oscillations. Astronomy & Astrophysics. 710, A387.' mla: 'Marcel, G., et al. “Disk Warping and Black Hole X-Ray Binaries: I. Tentative Unification of Low-Frequency Quasi-Periodic Oscillations.” Astronomy & Astrophysics, vol. 710, A387, EDP Sciences, 2026, doi:10.1051/0004-6361/202558103.' short: G. Marcel, S.G.D. Turner, B.J. Ricketts, V. López-Barquero, D.J.K. Buisson, F. Vincentelli, M. Middleton, C.S. Reynolds, M. Avara, Astronomy & Astrophysics 710 (2026). das_tickbox: '0' date_created: 2026-07-21T10:29:36Z date_published: 2026-06-01T00:00:00Z date_updated: 2026-07-21T12:22:52Z day: '01' ddc: - '520' department: - _id: ZoHa doi: 10.1051/0004-6361/202558103 external_id: arxiv: - '2511.10474' file: - access_level: open_access checksum: 95c1695f3c7183b2ad9d58167500b18d content_type: application/pdf creator: dernst date_created: 2026-07-21T12:20:49Z date_updated: 2026-07-21T12:20:49Z file_id: '22382' file_name: 2026_AstronomyAstrophysics_Marcel.pdf file_size: 3286905 relation: main_file success: 1 file_date_updated: 2026-07-21T12:20:49Z has_accepted_license: '1' intvolume: ' 710' language: - iso: eng month: '06' oa: 1 oa_version: Published Version publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' researchdata_availability: no scopus_import: '1' status: public supplementarymaterial: yes title: 'Disk warping and black hole X-ray binaries: I. Tentative unification of low-frequency quasi-periodic oscillations' tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 710 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '22663' abstract: - lang: eng text: The detection of strong, large-scale magnetic fields at the surfaces of the oldest white dwarfs might point toward a hidden internal magnetic field slowly rising to the surface. In addition, strong magnetic fields have recently been measured through asteroseismology in the radiative interiors of red giant stars, the progenitors of white dwarfs. To investigate the potential connection between these observations, we revisited the fossil field framework using asteroseismic detections to constrain the strength of such magnetic fields as red giants evolve into the white dwarf stage. We assumed that the magnetic field was either created during the core convection on the main sequence or that it fills the radiative interior as the star evolves on the red giant branch. From these initial conditions, we evolved the magnetic flux, allowing for magnetic diffusion along the evolution of a modeled 1.5 M⊙ star. We find that measured field strengths in red giants attributed to the hydrogen-burning shell are compatible with the field amplitudes and emergence timescales of magnetized white dwarfs. On the contrary, magnetic fields generated solely from a convective-core dynamo on the main sequence and detectable on the red giant branch would be buried too deep in the star and would not match the breakout timescales or the field strengths of magnetic white dwarfs. Therefore, for us to connect magnetic fields observed along the late evolution of stars via a fossil field we would need to find a broadly magnetized internal radiative zone on the red giant branch. acknowledgement: "The authors thank the referee for their helpful and constructive report, which has significantly enhanced the quality of the manuscript.\r\nThe authors thank I. Caiazzo, L. Ferrario, and L. Buchele for very useful discussions. L. Barrault, L. Bugnet, and L. Einramhof gratefully acknowledge support from the European Research Council (ERC) under the Horizon Europe\r\nprogramme (Calcifer; Starting Grant agreement N◦101165631). L. Barrault\r\nacknowledges the support of the Austrian Academy of Sciences through the Doctoral Fellowship Programme (DOC) of the Austrian Academy of Sciences 27648.\r\nWhile partially funded by the European Union, views and opinions expressed\r\nare, however, those of the authors only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union\r\nnor the granting authority can be held responsible for them." article_number: L14 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Lukas full_name: Einramhof, Lukas id: f1497a1a-72ef-11ef-b75a-fd877bbf6e8c last_name: Einramhof - first_name: Lisa Annabelle full_name: Bugnet, Lisa Annabelle id: d9edb345-f866-11ec-9b37-d119b5234501 last_name: Bugnet orcid: 0000-0003-0142-4000 - first_name: L. M. full_name: Calcaferro, L. M. last_name: Calcaferro - first_name: Lucas full_name: Barrault, Lucas id: 4471a8fd-32c1-11ee-a9a4-fb670d398f64 last_name: Barrault - first_name: S. B. full_name: Das, S. B. last_name: Das citation: ama: Einramhof L, Bugnet LA, Calcaferro LM, Barrault L, Das SB. Magneto-archeology of white dwarfs. Astronomy & Astrophysics. 2026;708. doi:10.1051/0004-6361/202659069 apa: Einramhof, L., Bugnet, L. A., Calcaferro, L. M., Barrault, L., & Das, S. B. (2026). Magneto-archeology of white dwarfs. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202659069 chicago: Einramhof, Lukas, Lisa Annabelle Bugnet, L. M. Calcaferro, Lucas Barrault, and S. B. Das. “Magneto-Archeology of White Dwarfs.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202659069. ieee: L. Einramhof, L. A. Bugnet, L. M. Calcaferro, L. Barrault, and S. B. Das, “Magneto-archeology of white dwarfs,” Astronomy & Astrophysics, vol. 708. EDP Sciences, 2026. ista: Einramhof L, Bugnet LA, Calcaferro LM, Barrault L, Das SB. 2026. Magneto-archeology of white dwarfs. Astronomy & Astrophysics. 708, L14. mla: Einramhof, Lukas, et al. “Magneto-Archeology of White Dwarfs.” Astronomy & Astrophysics, vol. 708, L14, EDP Sciences, 2026, doi:10.1051/0004-6361/202659069. short: L. Einramhof, L.A. Bugnet, L.M. Calcaferro, L. Barrault, S.B. Das, Astronomy & Astrophysics 708 (2026). corr_author: '1' das_tickbox: '1' dataavailabilitystatement: We used MESA version 24.08.1. All inlists and relevant files are available on Zenodo at https://doi.org/10.5281/zenodo.19232789 date_created: 2026-08-10T07:53:32Z date_published: 2026-04-01T00:00:00Z date_updated: 2026-08-11T05:49:20Z day: '01' ddc: - '520' department: - _id: LiBu - _id: GradSch doi: 10.1051/0004-6361/202659069 external_id: arxiv: - '2601.15203' file: - access_level: open_access checksum: 61edee776603d7b879b06b3ea8d2bc89 content_type: application/pdf creator: dernst date_created: 2026-08-11T05:46:02Z date_updated: 2026-08-11T05:46:02Z file_id: '22671' file_name: 2026_AstronomyAstrophysics_Einramhof.pdf file_size: 3739424 relation: main_file success: 1 file_date_updated: 2026-08-11T05:46:02Z has_accepted_license: '1' intvolume: ' 708' language: - iso: eng month: '04' oa: 1 oa_version: Published Version project: - _id: 914d8549-16d5-11f0-9cad-bbe6324c93a9 grant_number: '101165631' name: 'Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology' - _id: 5b62812b-ab3d-11f0-914f-8f3a9cdb4af7 grant_number: '27648' name: Unveiling the structure and dynamics of the deep convective core - radiative zone boundary throughout stellar evolution publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' researchdata_availability: yes scopus_import: '1' status: public supplementarymaterial: yes title: Magneto-archeology of white dwarfs tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 708 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '22265' abstract: - lang: eng text: 'The well-known bimodality between star-forming discs and quiescent spheroids requires the existence of two main processes: galaxy quenching, causing the strong reduction of star formation, and morphological transformation, causing the transition from disc-dominated structures to bulge-dominated ones. In this paper, we aim to understand the link between these two processes and their relation with the stellar mass of galaxies and their local environment. Taking advantage of the first data released by the Euclid Collaboration, covering more than 60 deg2 with space-based imaging and photometry, we analyse a mass-complete sample of nearly one million galaxies in the range 0.25 < z < 1 with M* > 109.5 M⊙, using a combination of photometric and spectroscopic redshifts. We divide the sample into four sub-populations of galaxies, based on their star-formation activity (star-forming and quiescent) and morphology (disc-dominated and bulge-dominated). We then analyse the physical properties of these populations and their relative abundances in the stellar mass versus local density plane. Together with confirming the passivity-density relation and the morphology-density relation, we find that quiescent discy galaxies are more abundant in the low-mass regime of high-density environment where log10(1 + δ) > 1.3. At the same time, star-forming bulge-dominated galaxies are more common in field regions with log10(1 + δ) < 0.8, preferentially at high masses. Building on these results and interpreting them through comparison with simulations, we propose a scenario where the evolution of galaxies in the field significantly differs from that in higher-density environments. The morphological transformation in the majority of field galaxies takes place before the onset of quenching and is mainly driven by secular processes taking place within the main sequence, leading to the formation of star-forming bulge-dominated galaxies as intermediate-stage galaxies. Conversely, quenching of star formation precedes morphological transformation for most galaxies in higher-density environments. This causes the formation of quiescent disc-dominated galaxies before their transition into bulge-dominated ones.' acknowledgement: 'FaGe, AnEn, EmDa, LoGa, SaQu, GaDe, MaTa, ChDe, LuPo acknowledge support from the ELSA project. “ELSA: Euclid Legacy Science Advanced analysis tools” (Grant Agreement no. 101135203) is funded by the European Union. Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or Innovate UK. Neither the European Union nor the granting authority can be held responsible for them. UK participation is funded through the UK HORIZON guarantee scheme under Innovate UK grant 10093177. AnEn acknowledge support from the INAF MiniGrant 2023 “ADIEU: Anomaly Detections In EUclid”. CaLo acknowledges support by FCT-Fundação para a Ciência e a Tecnologia through grants UIDB/04434/2020 DOI: 10.54499/UIDB/04434/2020, UIDP/04434/2020 DOI: 10.54499/UIDP/04434/2020. The Euclid Consortium acknowledges the European Space Agency and a number of agencies and institutes that have supported the development of Euclid, in particular the Agenzia Spaziale Italiana, the Austrian Forschungsförderungsgesellschaft funded through BMK, the Belgian Science Policy, the Canadian Euclid Consortium, the Deutsches Zentrum für Luft-und Raumfahrt, the DTU Space and the Niels Bohr Institute in Denmark, the French Centre National d’Etudes Spatiales, the Fundação para a Ciência e a Tecnologia, the Hungarian Academy of Sciences, the Ministerio de Ciencia, Innovación y Universidades, the National Aeronautics and Space Administration, the National Astronomical Observatory of Japan, the Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space Agency, the Research Council of Finland, the Romanian Space Agency, the State Secretariat for Education, Research, and Innovation (SERI) at the Swiss Space Office (SSO), and the United Kingdom Space Agency. A complete and detailed list is available on the Euclid website (www.euclid-ec.org). This work has made use of the Euclid Quick Release Q1 data from the Euclid mission of the European Space Agency (ESA), 2025, https://doi.org/10.57780/esa-2853f3b. This work has made use of CosmoHub, developed by PIC (maintained by IFAE and CIEMAT) in collaboration with ICE-CSIC. CosmoHub received funding from the Spanish government (MCIN/AEI/10.13039/501100011033), the EU NextGeneration/PRTR (PRTR-C17.I1), and the Generalitat de Catalunya. Based on data from UNIONS, a scientific collaboration using three Hawaii-based telescopes: CFHT, Pan-STARRS, and Subaru www.skysurvey.cc. Based on data from the Dark Energy Camera (DECam) on the Blanco 4-m Telescope at CTIO in Chile https://www.darkenergysurvey.org' article_number: A12 article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: F. full_name: Gentile, F. last_name: Gentile - first_name: E. full_name: Daddi, E. last_name: Daddi - first_name: D. full_name: Elbaz, D. last_name: Elbaz - first_name: A. full_name: Enia, A. last_name: Enia - first_name: B. full_name: Magnelli, B. last_name: Magnelli - first_name: J. B. full_name: Billand, J. 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A. last_name: Stanford - first_name: K. full_name: Tanidis, K. last_name: Tanidis - first_name: G. full_name: Testera, G. last_name: Testera - first_name: R. full_name: Teyssier, R. last_name: Teyssier - first_name: S. full_name: Tosi, S. last_name: Tosi - first_name: A. full_name: Troja, A. last_name: Troja - first_name: M. full_name: Tucci, M. last_name: Tucci - first_name: C. full_name: Valieri, C. last_name: Valieri - first_name: A. full_name: Venhola, A. last_name: Venhola - first_name: D. full_name: Vergani, D. last_name: Vergani - first_name: G. full_name: Verza, G. last_name: Verza - first_name: P. full_name: Vielzeuf, P. last_name: Vielzeuf - first_name: N. A. full_name: Walton, N. A. last_name: Walton citation: ama: 'Gentile F, Daddi E, Elbaz D, et al. Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field. Astronomy & Astrophysics. 2026;711. doi:10.1051/0004-6361/202557633' apa: 'Gentile, F., Daddi, E., Elbaz, D., Enia, A., Magnelli, B., Billand, J. B., … Walton, N. A. (2026). Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557633' chicago: 'Gentile, F., E. Daddi, D. Elbaz, A. Enia, B. Magnelli, J. B. Billand, P. Corcho-Caballero, et al. “Euclid Quick Data Release (Q1): XII. Quenching Precedes Bulge Formation in Dense Environments but Follows It in the Field.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557633.' ieee: 'F. Gentile et al., “Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field,” Astronomy & Astrophysics, vol. 711. EDP Sciences, 2026.' ista: 'Gentile F et al. 2026. Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field. Astronomy & Astrophysics. 711, A12.' mla: 'Gentile, F., et al. “Euclid Quick Data Release (Q1): XII. Quenching Precedes Bulge Formation in Dense Environments but Follows It in the Field.” Astronomy & Astrophysics, vol. 711, A12, EDP Sciences, 2026, doi:10.1051/0004-6361/202557633.' short: F. Gentile, E. Daddi, D. Elbaz, A. Enia, B. Magnelli, J.B. Billand, P. Corcho-Caballero, C. Cleland, G. De Lucia, C. D’Eugenio, M. Fossati, M. Franco, C. Lobo, Y. Lyu, M. Magliocchetti, G.A. Mamon, L. Quilley, J.G. Sorce, M. Tarrasse, M. Bolzonella, F. Durret, L. Gabarra, S. Guo, L. Pozzetti, S. Quai, F. Shankar, V. Sangalli, M. Talia, M. Baes, H. Fu, M. Girardi, J.J. Matthee, P.A. Oesch, D. Roberts, J. Schaye, D. Scott, L. Spinoglio, B. Altieri, A. Amara, S. Andreon, N. Auricchio, C. Baccigalupi, M. Baldi, A. Balestra, S. Bardelli, R. Bender, A. Biviano, E. Branchini, M. Brescia, J. Brinchmann, S. Camera, G. Cañas-Herrera, V. Capobianco, C. Carbone, J. Carretero, S. Casas, M. Castellano, G. Castignani, S. Cavuoti, K.C. Chambers, A. Cimatti, C. Colodro-Conde, G. Congedo, L. Conversi, Y. Copin, F. Courbin, H.M. Courtois, M. Cropper, A. Da Silva, H. Degaudenzi, C. Dolding, H. Dole, F. Dubath, C.A.J. Duncan, X. Dupac, S. Dusini, S. Escoffier, M. Fabricius, M. Farina, R. Farinelli, S. Ferriol, F. Finelli, N. Fourmanoit, M. Frailis, E. Franceschi, M. Fumana, S. Galeotta, K. George, B. Gillis, C. Giocoli, J. Gracia-Carpio, A. Grazian, F. Grupp, S. Gwyn, S.V.H. Haugan, J. Hoar, W. Holmes, I.M. Hook, F. Hormuth, A. Hornstrup, K. Jahnke, M. Jhabvala, B. Joachimi, E. Keihänen, S. Kermiche, A. Kiessling, B. Kubik, M. Kümmel, M. Kunz, H. Kurki-Suonio, A.M.C. Le Brun, S. Ligori, P.B. Lilje, V. Lindholm, I. Lloro, G. Mainetti, D. Maino, E. Maiorano, O. Mansutti, O. Marggraf, M. Martinelli, N. Martinet, F. Marulli, R.J. Massey, E. Medinaceli, S. Mei, M. Melchior, Y. Mellier, M. Meneghetti, E. Merlin, G. Meylan, A. Mora, M. Moresco, L. Moscardini, R. Nakajima, S.M. Niemi, C. Padilla, S. Paltani, F. Pasian, K. Pedersen, W.J. Percival, V. Pettorino, S. Pires, G. Polenta, M. Poncet, L.A. Popa, F. Raison, A. Renzi, J. Rhodes, G. Riccio, E. Romelli, M. Roncarelli, R. Saglia, Z. Sakr, D. Sapone, B. Sartoris, P. Schneider, T. Schrabback, A. Secroun, G. Seidel, S. Serrano, P. Simon, C. Sirignano, G. Sirri, J. Skottfelt, L. Stanco, J. Steinwagner, P. Tallada-Crespí, A.N. Taylor, H.I. Teplitz, I. Tereno, N. Tessore, S. Toft, R. Toledo-Moreo, F. Torradeflot, I. Tutusaus, L. Valenziano, J. Valiviita, T. Vassallo, G. Verdoes Kleijn, A. Veropalumbo, Y. Wang, J. Weller, A. Zacchei, G. Zamorani, I.A. Zinchenko, E. Zucca, V. Allevato, M. Ballardini, E. Bozzo, C. Burigana, R. Cabanac, M. Calabrese, A. Cappi, D. Di Ferdinando, J.A. Escartin Vigo, W.G. Hartley, M. Huertas-Company, J. Martín-Fleitas, S. Matthew, N. Mauri, R.B. Metcalf, A. Pezzotta, M. Pöntinen, I. Risso, V. Scottez, M. Sereno, M. Tenti, M. Viel, M. Wiesmann, Y. Akrami, I.T. Andika, S. Anselmi, M. Archidiacono, F. Atrio-Barandela, D. Bertacca, M. Bethermin, L. Bisigello, A. Blanchard, L. Blot, H. Böhringer, M. Bonici, S. Borgani, M.L. Brown, S. Bruton, A. Calabro, B. Camacho Quevedo, F. Caro, C.S. Carvalho, T. Castro, F. Cogato, S. Conseil, T. Contini, A.R. Cooray, O. Cucciati, G. Desprez, A. Díaz-Sánchez, S. Di Domizio, J.M. Diego, P. Dimauro, P.A. Duc, M.Y. Elkhashab, Y. Fang, A. Finoguenov, A. Fontana, F. Fontanot, A. Franco, K. Ganga, J. García-Bellido, T. Gasparetto, V. Gautard, R. Gavazzi, E. Gaztanaga, F. Giacomini, F. Gianotti, A.H. Gonzalez, G. Gozaliasl, M. Guidi, C.M. Gutierrez, A. Hall, S. Hemmati, H. Hildebrandt, J. Hjorth, J.J.E. Kajava, Y. Kang, V. Kansal, D. Karagiannis, K. Kiiveri, J. Kim, C.C. Kirkpatrick, S. Kruk, L. Legrand, M. Lembo, F. Lepori, G. Leroy, G.F. Lesci, J. Lesgourgues, L. Leuzzi, T.I. Liaudat, A. Loureiro, J. Macias-Perez, E.A. Magnier, F. Mannucci, R. Maoli, C.J.A.P. Martins, L. Maurin, M. Miluzio, P. Monaco, C. Moretti, G. Morgante, K. Naidoo, A. Navarro-Alsina, S. Nesseris, D. Paoletti, F. Passalacqua, K. Paterson, L. Patrizii, A. Pisani, D. Potter, M. Radovich, G. Rodighiero, S. Sacquegna, M. Sahlén, D.B. Sanders, E. Sarpa, C. Scarlata, A. Schneider, M. Schultheis, D. Sciotti, E. Sellentin, L.C. Smith, S.A. Stanford, K. Tanidis, G. Testera, R. Teyssier, S. Tosi, A. Troja, M. Tucci, C. Valieri, A. Venhola, D. Vergani, G. Verza, P. Vielzeuf, N.A. Walton, Astronomy & Astrophysics 711 (2026). das_tickbox: '1' dataavailabilitystatement: 'This work has made use of the Euclid Quick Release Q1 data from the Euclid mission of the European Space Agency (ESA), 2025, https://doi.org/10.57780/esa-2853f3b. This work has made use of CosmoHub, developed by PIC (maintained by IFAE and CIEMAT) in collaboration with ICE-CSIC. CosmoHub received funding from the Spanish government (MCIN/AEI/10.13039/501100011033), the EU NextGeneration/PRTR (PRTR-C17.I1), and the Generalitat de Catalunya. Based on data from UNIONS, a scientific collaboration using three Hawaii-based telescopes: CFHT, Pan-STARRS, and Subaru www.skysurvey.cc. Based on data from the Dark Energy Camera (DECam) on the Blanco 4-m Telescope at CTIO in Chile https://www.darkenergysurvey.org' date_created: 2026-07-12T22:02:18Z date_published: 2026-07-01T00:00:00Z date_updated: 2026-08-12T09:27:50Z day: '01' ddc: - '520' department: - _id: JoMa doi: 10.1051/0004-6361/202557633 external_id: arxiv: - '2511.02964' file: - access_level: open_access checksum: 29c087abb97eed26d4aa2a19bbb46666 content_type: application/pdf creator: dernst date_created: 2026-07-13T08:42:10Z date_updated: 2026-07-13T08:42:10Z file_id: '22277' file_name: 2026_AstronomyAstrophysics_Euclid.pdf file_size: 3482066 relation: main_file success: 1 file_date_updated: 2026-07-13T08:42:10Z has_accepted_license: '1' intvolume: ' 711' keyword: - 'galaxies: evolution' - 'galaxies: interactions' - 'galaxies: statistics' language: - iso: eng month: '07' oa: 1 oa_version: Published Version publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' researchdata_availability: no scopus_import: '1' status: public supplementarymaterial: no title: 'Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field' tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 711 year: '2026' ... --- OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '22621' abstract: - lang: eng text: We present very deep (≈11 hours on-source) JWST/MIRI low-resolution spectroscopy of the rest-frame optical emission of U37126, a UV-bright (MUV ≃ −20) mildly lensed (μ ≃ 2.2) galaxy at z = 10.255. The continuum emission is well detected in the NIRSpec and MIRI spectra, but no nebular recombination or metal emission lines are observed (EW0 (Hβ+[O III]) ≤ 300 Å and EW0 (Hα) ≤ 400 Å at 3σ). Combined with the exceptionally blue UV continuum slope, βUV ≃ −2.9, and flat Balmer break, these constraints indicate a stellar population dominated by very young and massive stars with a strongly suppressed nebular contribution. Comparisons with synthetic stellar population models indicate that U37126 requires a very high ionizing photon production efficiency, log(ξion/Hz erg−1) ≃ 25.75, and a nearly unity Lyman continuum escape fraction, of fesc ≥ 86% (3σ) based on the Hα flux limit and fesc = 0.94 ± 0.06 derived independently from fitting the spectral energy distribution (SED). The best-fit SED yields a (delensed) stellar mass of M★ ≃ 107.8 M⊙ and a star formation rate SFR ≃ 10 M⊙ yr−1 (specific SFR ∼ 160 Gyr−1). Together with its very compact size, reff ≃ 61 pc, this yields a very high stellar mass and SFR surface densities, ΣM★ ≃ 3 × 103 M⊙ pc−2 and ΣSFR ≃ 400 M⊙ yr−1 kpc−2. Together with the lack of detectable nebular emission, these properties suggest that U37126 is undergoing a so-called interstellar medium-naked starburst phase, possibly driven by an extremely efficient gas-to-star conversion followed by strong feedback that has cleared the remaining gas from its stellar core, which allowed most Lyman continuum photons to escape. Finally, we show that even a small fraction of galaxies such as U37126 (≃3–6%), with an extreme Lyman continuum production and escape, might contribute disproportionately (≃50–100%) to the ionizing photon budget during cosmic reionization. acknowledgement: 'We thank the anonymous referee for the useful comments and suggestions. 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 #8051. J.A.-M., C.P.-J., B.R.P. acknowledge support from grant PID2024-158856NA-I00, J.A.-M., L.C., C.P.-J., B.R.P. acknowledge support from grant PID2021-127718NB-100, P.G.P.-G. acknowledges support from grant 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”. J.A.-M., L.C., C.P.-J., B.R.P., P.G.P.-G. acknowledge support by grant CSIC/BILATERALES2025/BIJSP25022. M.C. acknowledges INAF GO Grant 2024 “Revealing the nature of bright galaxies at cosmic dawn with deep JWST spectroscopy”. T.H. was supported by JSPS KAKENHI 25K00020. Y.H. acknowledges support from the Japan Society for the Promotion of Science (JSPS) Grant-in-Aid for Scientific Research (24H00245), the JSPS Core-to-Core Program (JPJSCCA20210003), and the JSPS International Leading Research (22K21349). Y.F. is supported by JSPS KAKENHI Grant Numbers JP22K21349 and JP23K13149. D.L. was supported by research grants (VIL16599,VIL54489) from VILLUM FONDEN. P.S. acknowledges support from INAF RF2024 Large Grant “UNDUST: UNveiling the Dawn of the Universe with JWST” 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; and from the European JWST archive (eJWST) operated by the ESDC. This research made use of Photutils, an Astropy package for detection and photometry of astronomical sources (Bradley et al. 2022).' article_number: A301 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: R. full_name: Marques-Chaves, R. last_name: Marques-Chaves - first_name: J. full_name: Álvarez-Márquez, J. last_name: Álvarez-Márquez - first_name: L. full_name: Colina, L. last_name: Colina - first_name: S. full_name: Kendrew, S. last_name: Kendrew - first_name: Unknown full_name: Abdurro’Uf, Unknown last_name: Abdurro’Uf - first_name: C. full_name: Blanco-Prieto, C. last_name: Blanco-Prieto - first_name: L. A. full_name: Boogaard, L. A. last_name: Boogaard - first_name: M. full_name: Castellano, M. last_name: Castellano - first_name: K. I. full_name: Caputi, K. I. last_name: Caputi - first_name: A. full_name: Crespo-Gómez, A. last_name: Crespo-Gómez - first_name: A. full_name: Fontana, A. last_name: Fontana - first_name: Y. full_name: Fudamoto, Y. last_name: Fudamoto - first_name: S. full_name: Fujimoto, S. last_name: Fujimoto - first_name: M. full_name: García-Marín, M. last_name: García-Marín - first_name: Y. full_name: Harikane, Y. last_name: Harikane - first_name: S. full_name: Harish, S. last_name: Harish - first_name: T. full_name: Hashimoto, T. last_name: Hashimoto - first_name: T. full_name: Hsiao, T. last_name: Hsiao - first_name: Edoardo full_name: Iani, Edoardo id: 4053390a-6b68-11ef-9828-a3b8adef8d0a last_name: Iani orcid: 0000-0001-8386-3546 - first_name: A. K. full_name: Inoue, A. K. last_name: Inoue - first_name: D. full_name: Langeroodi, D. last_name: Langeroodi - first_name: R. full_name: Lin, R. last_name: Lin - first_name: J. full_name: Melinder, J. last_name: Melinder - first_name: L. full_name: Napolitano, L. last_name: Napolitano - first_name: G. full_name: Östlin, G. last_name: Östlin - first_name: P. G. full_name: Pérez-González, P. G. last_name: Pérez-González - first_name: C. full_name: Prieto-Jiménez, C. last_name: Prieto-Jiménez - first_name: P. full_name: Rinaldi, P. last_name: Rinaldi - first_name: B. full_name: Rodríguez Del Pino, B. last_name: Rodríguez Del Pino - first_name: P. full_name: Santini, P. last_name: Santini - first_name: Y. full_name: Sugahara, Y. last_name: Sugahara - first_name: A. full_name: Varo-O’Ferrall, A. last_name: Varo-O’Ferrall - first_name: G. full_name: Wright, G. last_name: Wright - first_name: J. full_name: Zavala, J. last_name: Zavala citation: ama: 'Marques-Chaves R, Álvarez-Márquez J, Colina L, et al. PRISMS: U37126, a very blue ISM-naked starburst at z = 10.255 with a nearly 100% Lyman continuum escape fraction. Astronomy & Astrophysics. 2026;711. doi:10.1051/0004-6361/202659281' apa: 'Marques-Chaves, R., Álvarez-Márquez, J., Colina, L., Kendrew, S., Abdurro’Uf, U., Blanco-Prieto, C., … Zavala, J. (2026). PRISMS: U37126, a very blue ISM-naked starburst at z = 10.255 with a nearly 100% Lyman continuum escape fraction. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202659281' chicago: 'Marques-Chaves, R., J. Álvarez-Márquez, L. Colina, S. Kendrew, Unknown Abdurro’Uf, C. Blanco-Prieto, L. A. Boogaard, et al. “PRISMS: U37126, a Very Blue ISM-Naked Starburst at z = 10.255 with a Nearly 100% Lyman Continuum Escape Fraction.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202659281.' ieee: 'R. Marques-Chaves et al., “PRISMS: U37126, a very blue ISM-naked starburst at z = 10.255 with a nearly 100% Lyman continuum escape fraction,” Astronomy & Astrophysics, vol. 711. EDP Sciences, 2026.' ista: 'Marques-Chaves R, Álvarez-Márquez J, Colina L, Kendrew S, Abdurro’Uf U, Blanco-Prieto C, Boogaard LA, Castellano M, Caputi KI, Crespo-Gómez A, Fontana A, Fudamoto Y, Fujimoto S, García-Marín M, Harikane Y, Harish S, Hashimoto T, Hsiao T, Iani E, Inoue AK, Langeroodi D, Lin R, Melinder J, Napolitano L, Östlin G, Pérez-González PG, Prieto-Jiménez C, Rinaldi P, Rodríguez Del Pino B, Santini P, Sugahara Y, Varo-O’Ferrall A, Wright G, Zavala J. 2026. PRISMS: U37126, a very blue ISM-naked starburst at z = 10.255 with a nearly 100% Lyman continuum escape fraction. Astronomy & Astrophysics. 711, A301.' mla: 'Marques-Chaves, R., et al. “PRISMS: U37126, a Very Blue ISM-Naked Starburst at z = 10.255 with a Nearly 100% Lyman Continuum Escape Fraction.” Astronomy & Astrophysics, vol. 711, A301, EDP Sciences, 2026, doi:10.1051/0004-6361/202659281.' short: R. Marques-Chaves, J. Álvarez-Márquez, L. Colina, S. Kendrew, U. Abdurro’Uf, C. Blanco-Prieto, L.A. Boogaard, M. Castellano, K.I. Caputi, A. Crespo-Gómez, A. Fontana, Y. Fudamoto, S. Fujimoto, M. García-Marín, Y. Harikane, S. Harish, T. Hashimoto, T. Hsiao, E. Iani, A.K. Inoue, D. Langeroodi, R. Lin, J. Melinder, L. Napolitano, G. Östlin, P.G. Pérez-González, C. Prieto-Jiménez, P. Rinaldi, B. Rodríguez Del Pino, P. Santini, Y. Sugahara, A. Varo-O’Ferrall, G. Wright, J. Zavala, Astronomy & Astrophysics 711 (2026). das_tickbox: '0' date_created: 2026-08-02T22:01:53Z date_published: 2026-07-24T00:00:00Z date_updated: 2026-08-12T09:28:30Z day: '24' ddc: - '520' department: - _id: JoMa doi: 10.1051/0004-6361/202659281 external_id: arxiv: - '2602.02322' file: - access_level: open_access checksum: 8debbe56211a456539d8b3479f837b10 content_type: application/pdf creator: dernst date_created: 2026-08-03T08:49:31Z date_updated: 2026-08-03T08:49:31Z file_id: '22634' file_name: 2026_AstronomyAstrophysics_MarquesChaves.pdf file_size: 1127121 relation: main_file success: 1 file_date_updated: 2026-08-03T08:49:31Z has_accepted_license: '1' intvolume: ' 711' language: - iso: eng month: '07' oa: 1 oa_version: Published Version publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' researchdata_availability: no scopus_import: '1' status: public supplementarymaterial: yes title: 'PRISMS: U37126, a very blue ISM-naked starburst at z = 10.255 with a nearly 100% Lyman continuum escape fraction' tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 711 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '21659' abstract: - lang: eng text: The recent detection of solar equatorial Rossby waves has renewed interest in the study of gravito-inertial waves propagating in the convective envelope of solar-type stars. In particular, the ability of these envelope gravito-inertial modes to couple with those trapped in the radiative interior could open up new opportunities for probing the deep-layer dynamics of solar-type stars. The possibility for such a coupling to occur is particularly favoured among pre-main-sequence (PMS) solar-type stars. Indeed, due to the contraction of the protostellar object, they are able to reach high rotation frequencies before nuclear reactions are ignited and magnetic braking becomes the driving mechanism for their rotational evolution. In this work, we studied the coupling between the envelope inertial waves and the radiative interior g modes in PMS stars, focussing on the case of prograde dipolar modes. We considered the cases of 0.5 M⊙ and 1 M⊙ PMS models, each with three different scenarios of rotational evolution. We show that for stars that have formed with a sufficient amount of angular momentum, this coupling can occur in frequency ranges that are accessible to space-borne photometry, creating inertial dips in the period spacing pattern. Using an asymptotic analysis, we characterised the shape of these inertial dips to show that they depend on rotation and on the stiffness of the convective-radiative interface. acknowledgement: 'The authors want to thank the anonymous referee for useful comments. SNB acknowledges support from PLATO ASI-INAF agreement no. 2022-28-HH.0 “PLATO Fase D”. SNB and AFL acknowledge support from the INAF grant MASTODINT. CP thanks the Belgian Federal Science Policy Office (BELSPO) for the financial support in the framework of the PRODEX Program of the European Space Agency (ESA) under contract number 4000141194. S.M acknowledges support from the CNES GOLF-SOHO and PLATO grants at CEA/DAp. LB and SM gratefully acknowledge support from the European Research Council (ERC) under the Horizon Europe programme (LB: Calcifer; Starting Grant agreement N°101165631; SM: 4D-STAR; Synergy Grant agreement N°101071505). While partially funded by the European Union, 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. Neither the European Union nor the granting authority can be held responsible for them. The authors acknowledge G. Buldgen, H. Dhouib, and M.A. Dupret for fruitful discussions.' article_number: L16 article_processing_charge: No article_type: letter_editor arxiv: 1 author: - first_name: S. N. full_name: Breton, S. N. last_name: Breton - first_name: C. full_name: Pezzotti, C. last_name: Pezzotti - first_name: S. full_name: Mathis, S. last_name: Mathis - first_name: Lisa Annabelle full_name: Bugnet, Lisa Annabelle id: d9edb345-f866-11ec-9b37-d119b5234501 last_name: Bugnet orcid: 0000-0003-0142-4000 - first_name: M. P. full_name: Di Mauro, M. P. last_name: Di Mauro - first_name: J. full_name: Joergensen, J. last_name: Joergensen - first_name: K. full_name: Zwintz, K. last_name: Zwintz - first_name: A. F. full_name: Lanza, A. F. last_name: Lanza citation: ama: Breton SN, Pezzotti C, Mathis S, et al. Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars. Astronomy & Astrophysics. 2026;707. doi:10.1051/0004-6361/202659309 apa: Breton, S. N., Pezzotti, C., Mathis, S., Bugnet, L. A., Di Mauro, M. P., Joergensen, J., … Lanza, A. F. (2026). Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202659309 chicago: Breton, S. N., C. Pezzotti, S. Mathis, Lisa Annabelle Bugnet, M. P. Di Mauro, J. Joergensen, K. Zwintz, and A. F. Lanza. “Core-Envelope Coupling of Gravito-Inertial Waves in Pre-Main-Sequence Solar-Type Stars.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202659309. ieee: S. N. Breton et al., “Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars,” Astronomy & Astrophysics, vol. 707. EDP Sciences, 2026. ista: Breton SN, Pezzotti C, Mathis S, Bugnet LA, Di Mauro MP, Joergensen J, Zwintz K, Lanza AF. 2026. Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars. Astronomy & Astrophysics. 707, L16. mla: Breton, S. N., et al. “Core-Envelope Coupling of Gravito-Inertial Waves in Pre-Main-Sequence Solar-Type Stars.” Astronomy & Astrophysics, vol. 707, L16, EDP Sciences, 2026, doi:10.1051/0004-6361/202659309. short: S.N. Breton, C. Pezzotti, S. Mathis, L.A. Bugnet, M.P. Di Mauro, J. Joergensen, K. Zwintz, A.F. Lanza, Astronomy & Astrophysics 707 (2026). date_created: 2026-04-05T22:01:32Z date_published: 2026-03-01T00:00:00Z date_updated: 2026-08-12T09:29:13Z day: '01' ddc: - '520' department: - _id: LiBu doi: 10.1051/0004-6361/202659309 external_id: arxiv: - '2603.01979' file: - access_level: open_access checksum: a7fd798bf450d67d4166fdf54ff2c70c content_type: application/pdf creator: dernst date_created: 2026-04-07T09:20:02Z date_updated: 2026-04-07T09:20:02Z file_id: '21666' file_name: 2026_AstronomyAstrophysics_Breton.pdf file_size: 1535506 relation: main_file success: 1 file_date_updated: 2026-04-07T09:20:02Z has_accepted_license: '1' intvolume: ' 707' language: - iso: eng month: '03' oa: 1 oa_version: Published Version project: - _id: 914d8549-16d5-11f0-9cad-bbe6324c93a9 grant_number: '101165631' name: 'Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology' publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' scopus_import: '1' status: public title: Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 707 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '20930' abstract: - lang: eng text: "Context. Beta Pictoris is an A-type star that hosts a complex planetary system with two massive gas giants and a prominent debris disc. Variable absorption lines in its stellar spectrum have been interpreted as signatures of exocomets – comet-like bodies transiting the star. Stellar flybys can gravitationally perturb objects in the outer comet reservoir, altering their orbits and potentially injecting them into the inner system, thereby triggering exocomet showers.\r\nAims. We assessed the contribution of stellar flybys to the observed exocomet activity by reconstructing the stellar encounter history of β Pictoris in the past and future.\r\nMethods. We used Gaia DR3 data, supplemented with radial velocities from complementary spectroscopic surveys, to compile a catalogue of stars currently within 80 pc of β Pictoris. Their orbits were integrated backwards and forwards in time in an axisymmetric Galactic potential (via the GALA package) to identify encounters within 2 pc of the system.\r\nResults. We identified 99 416 stars currently within 80 pc of β Pictoris with resolved kinematics. Among these, 49 stars (including the eight components of five binaries) encounter β Pictoris within 2 pc between –1.5 Myr and +2 Myr. For four of the binaries, the centre-of-mass trajectories also pass within 2 pc. We estimated the sample to be more than 60% complete within 0.5 Myr of today.\r\nConclusions. Despite β Pictoris being the eponym of its famous moving group, none of the identified encounters involved its moving group members; all are unrelated field stars. We found no encounter capable of shaping the observed disc structures, although stellar flybys may contribute to the long-term evolution of an Oort Cloud-like structure. Our catalogue constitutes the most complete reconstruction of the β Pictoris encounter history to date and provides a robust foundation for future dynamical simulations." acknowledgement: We thank the referee for their suggestions and comments, which helped us improve the quality and clarity of the paper. JLGM and EV acknowledge the support from the Spanish Ministry of Science and Innovation/State Agency of Research (MCIN/AEI) under the grant PID2021-127289-NB-I00. ST acknowledges the funding from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 101034413. AJM acknowledges support from the Swedish National Space Agency (Career Grant 2023-00146) and from the Swedish Research Council (Project Grant 2022-04043). JLGM also sincerely thanks AMP for his careful final reading of this manuscript. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. We acknowledge the use of the public data products from RAVE (https://www.rave-survey.org), GALAH (https://galah-survey.org), APOGEE ((https://www.sdss.org) and LAMOST (http://www.lamost.org) surveys. This research has also made use of the SIMBAD database and the VizieR catalogue access tool, operated at CDS, Strasbourg, France, as well as the NASA Astrophysics Data System Bibliographic Services and the arXiv pre-print server operated by Cornell University. Computational analyses in this work relied extensively on the NumPy and SciPy libraries for numerical computing, matplotlib and seaborn for data visualization, and the Gala package for Galactic dynamics. This work also made use of Astropy, a community-developed core PYTHON package and an ecosystem of tools and resources for astronomy. We thank the developers and maintainers of these open-source resources for their invaluable contributions to the astronomical community. article_number: A237 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: J. L. full_name: Gragera-Más, J. L. last_name: Gragera-Más - first_name: Santiago full_name: Torres Rodriguez, Santiago id: a8df4360-4328-11ee-8f1a-e502d0c83fc2 last_name: Torres Rodriguez orcid: 0000-0002-3150-8988 - first_name: A. J. full_name: Mustill, A. J. last_name: Mustill - first_name: E. full_name: Villaver, E. last_name: Villaver citation: ama: Gragera-Más JL, Torres Rodriguez S, Mustill AJ, Villaver E. A kinematic history of stellar encounters with Beta Pictoris. Astronomy & Astrophysics. 2025;704. doi:10.1051/0004-6361/202555940 apa: Gragera-Más, J. L., Torres Rodriguez, S., Mustill, A. J., & Villaver, E. (2025). A kinematic history of stellar encounters with Beta Pictoris. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202555940 chicago: Gragera-Más, J. L., Santiago Torres Rodriguez, A. J. Mustill, and E. Villaver. “A Kinematic History of Stellar Encounters with Beta Pictoris.” Astronomy & Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202555940. ieee: J. L. Gragera-Más, S. Torres Rodriguez, A. J. Mustill, and E. Villaver, “A kinematic history of stellar encounters with Beta Pictoris,” Astronomy & Astrophysics, vol. 704. EDP Sciences, 2025. ista: Gragera-Más JL, Torres Rodriguez S, Mustill AJ, Villaver E. 2025. A kinematic history of stellar encounters with Beta Pictoris. Astronomy & Astrophysics. 704, A237. mla: Gragera-Más, J. L., et al. “A Kinematic History of Stellar Encounters with Beta Pictoris.” Astronomy & Astrophysics, vol. 704, A237, EDP Sciences, 2025, doi:10.1051/0004-6361/202555940. short: J.L. Gragera-Más, S. Torres Rodriguez, A.J. Mustill, E. Villaver, Astronomy & Astrophysics 704 (2025). date_created: 2026-01-04T23:01:34Z date_published: 2025-12-01T00:00:00Z date_updated: 2026-02-16T12:15:07Z day: '01' ddc: - '520' department: - _id: LiBu doi: 10.1051/0004-6361/202555940 ec_funded: 1 external_id: arxiv: - '2510.02509' file: - access_level: open_access checksum: 2fb4d5a1603043aa7931a31f2c180877 content_type: application/pdf creator: dernst date_created: 2026-01-05T11:06:16Z date_updated: 2026-01-05T11:06:16Z file_id: '20942' file_name: 2025_AstronomyAstrophysics_GrageraMas.pdf file_size: 11021467 relation: main_file success: 1 file_date_updated: 2026-01-05T11:06:16Z has_accepted_license: '1' intvolume: ' 704' language: - iso: eng month: '12' oa: 1 oa_version: Published Version project: - _id: fc2ed2f7-9c52-11eb-aca3-c01059dda49c call_identifier: H2020 grant_number: '101034413' name: 'IST-BRIDGE: International postdoctoral program' publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' scopus_import: '1' status: public title: A kinematic history of stellar encounters with Beta Pictoris tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 704 year: '2025' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '20932' abstract: - lang: eng text: Identifying Lyman continuum (LyC) leakers at intermediate redshifts is crucial for understanding the properties of cosmic reionizers because the opacity of the intergalactic medium (IGM) prevents the direct detection of LyC emission from sources during the Epoch of Reionization (EoR). In this study, we confirm two new LyC candidate leakers at z ∼ 3 in the Abell 2744 cluster field, with absolute escape fractions (fesc) of 0.83−0.80+0.15 and 0.74−0.70+0.23, respectively. The LyC emission was detected using HST/WFC3/F275W and F336W imaging. These two candidate leakers appear to be faint (MUV = −17.61 ± 0.06 and −18.22 ± 0.10), exhibit blue UV continuum slopes (β = −2.43 ± 0.05 and −1.92 ± 0.09), have low masses (M★ ∼ 107.51 ± 0.03 and 107.17 ± 0.15 M⊙) and Lyα equivalent widths of 90 ± 3 Å and 28 ± 12 Å, respectively. These two LyC candidate leakers were detected in a catalog of 91 spectroscopically confirmed sources using public spectra from the JWST and/or MUSE. We also analyzed properties that were proposed as indirect indicators of LyC emission, such as Lyα, the O32 ratio, and M★. We created a galaxy subsample that was selected according to these properties, stacked the LyC observations of this subsample, and assessed the limits of the escape fractions in the stacks. We aim to enhance our understanding of LyC escape mechanisms and improve our predictions of the LyC fesc during the EoR by analyzing the individual candidates and the stacks in the context of the currently limited sample of known LyC leakers at z ∼ 3. acknowledgement: 'We acknowledge support from the National Science Foundation of China – 12225301, INAF Large grant “Spectroscopic survey with JWST” jand from PRIN 2022 MUR project 2022CB3PJ3 – First Light And Galaxy aSsembly (FLAGS) funded by the European Union – Next Generation EU, and Postgraduate Scholarship Program under the grant of China Scholarship Council. P.W. and B.V. acknowledge support from the INAF Mini Grant ‘1.05.24.07.01 RSN1: Spatially Resolved Near-IR Emission of Intermediate-Redshift Jellyfish Galaxies’ (PI Watson). We acknowledge A. Acebron, C. Grillo, and P. Rosati for their fundamental contribution to the strong lensing analysis and results. We also extend our gratitude to the JWST and HST teams for their efforts in designing, building, and operating these transformative missions.' article_number: A328 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Y. full_name: Liu, Y. last_name: Liu - first_name: Sara full_name: Mascia, Sara id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29 last_name: Mascia - first_name: L. full_name: Pentericci, L. last_name: Pentericci - first_name: P. full_name: Watson, P. last_name: Watson - first_name: A. full_name: Alavi, A. last_name: Alavi - first_name: P. full_name: Bergamini, P. last_name: Bergamini - first_name: M. full_name: Bradač, M. last_name: Bradač - first_name: A. full_name: Calabrò, A. last_name: Calabrò - first_name: K. full_name: Glazebrook, K. last_name: Glazebrook - first_name: A. full_name: Henry, A. last_name: Henry - first_name: M. full_name: Llerena, M. last_name: Llerena - first_name: E. full_name: Merlin, E. last_name: Merlin - first_name: B. full_name: Metha, B. last_name: Metha - first_name: T. full_name: Nanayakkara, T. last_name: Nanayakkara - first_name: L. full_name: Napolitano, L. last_name: Napolitano - first_name: N. full_name: Roy, N. last_name: Roy - first_name: B. full_name: Siana, B. last_name: Siana - first_name: E. full_name: Vanzella, E. last_name: Vanzella - first_name: B. full_name: Vulcani, B. last_name: Vulcani - first_name: X. full_name: Wang, X. last_name: Wang citation: ama: Liu Y, Mascia S, Pentericci L, et al. A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field. Astronomy & Astrophysics. 2025;704. doi:10.1051/0004-6361/202556410 apa: Liu, Y., Mascia, S., Pentericci, L., Watson, P., Alavi, A., Bergamini, P., … Wang, X. (2025). A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202556410 chicago: Liu, Y., Sara Mascia, L. Pentericci, P. Watson, A. Alavi, P. Bergamini, M. Bradač, et al. “A Lyman Continuum Analysis of ∼100 Galaxies at z Spec∼ 3 in the Abell 2744 Cluster Field.” Astronomy & Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202556410. ieee: Y. Liu et al., “A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field,” Astronomy & Astrophysics, vol. 704. EDP Sciences, 2025. ista: Liu Y, Mascia S, Pentericci L, Watson P, Alavi A, Bergamini P, Bradač M, Calabrò A, Glazebrook K, Henry A, Llerena M, Merlin E, Metha B, Nanayakkara T, Napolitano L, Roy N, Siana B, Vanzella E, Vulcani B, Wang X. 2025. A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field. Astronomy & Astrophysics. 704, A328. mla: Liu, Y., et al. “A Lyman Continuum Analysis of ∼100 Galaxies at z Spec∼ 3 in the Abell 2744 Cluster Field.” Astronomy & Astrophysics, vol. 704, A328, EDP Sciences, 2025, doi:10.1051/0004-6361/202556410. short: Y. Liu, S. Mascia, L. Pentericci, P. Watson, A. Alavi, P. Bergamini, M. Bradač, A. Calabrò, K. Glazebrook, A. Henry, M. Llerena, E. Merlin, B. Metha, T. Nanayakkara, L. Napolitano, N. Roy, B. Siana, E. Vanzella, B. Vulcani, X. Wang, Astronomy & Astrophysics 704 (2025). date_created: 2026-01-04T23:01:35Z date_published: 2025-12-01T00:00:00Z date_updated: 2026-02-16T12:14:52Z day: '01' ddc: - '520' department: - _id: JoMa doi: 10.1051/0004-6361/202556410 external_id: arxiv: - '2507.11045' file: - access_level: open_access checksum: 3e6061f3c4bfb521b3333ea4913c241a content_type: application/pdf creator: dernst date_created: 2026-01-05T09:26:17Z date_updated: 2026-01-05T09:26:17Z file_id: '20938' file_name: 2025_AstronomyAstrophysics_Liu.pdf file_size: 4642530 relation: main_file success: 1 file_date_updated: 2026-01-05T09:26:17Z has_accepted_license: '1' intvolume: ' 704' language: - iso: eng month: '12' oa: 1 oa_version: Published Version publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' scopus_import: '1' status: public title: A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 704 year: '2025' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '21060' abstract: - lang: eng text: "Compact, star-forming galaxies with high star formation rate surface densities (ΣSFR) are often efficient Lyman continuum (LyC) emitters at z ≤ 4.5, likely because intense stellar feedback creates low-density channels that allow photons to escape. Irregular or disturbed morphologies, such as those resulting from mergers, can also facilitate LyC escape by creating anisotropic gas distributions. We investigated the influence of galaxy morphology on LyC production and escape at redshifts 5 ≤ z ≤ 7 using observations from various James Webb Space Telescope (JWST) surveys. Our sample consists of 436 sources, which are predominantly low-mass (∼10^8.15 M\f), star-forming galaxies with ionizing photon efficiency (ξion) values consistent with canonical expectations. Since direct measurements of fesc are not possible during the Epoch of Reionization (EoR), we predicted fesc for high-redshift galaxies by applying survival analysis to a subsample of LyC emitters from the Low-Redshift Lyman Continuum Survey (LzLCS), selected to be direct analogs of reionization-era galaxies. We find that these galaxies exhibit, on average, modest predicted escape fractions (∼0.04). In addition, we evaluated the correlation between morphological features and LyC emission. Our findings indicate that neither ξion nor the predicted fesc values show a significant correlation with the presence of merger signatures. This suggests that in low-mass galaxies at z ≥ 5, strong morphological disturbances are not the primary mechanism driving LyC emission and leakage. Instead, compactness and star formation activity likely play a more pivotal role in regulating LyC escape. " acknowledgement: This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with programs GTO 1243, ERS 1345, DDT 2750, and GTO 1180, 1181, 3215, 1210, 1286. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. We acknowledge support from the INAF Large Grant 2022 “Extragalactic Surveys with JWST” (PI Pentericci). We acknowledge support from INAF Mini-grant “Reionization and Fundamental Cosmology with High-Redshift Galaxies” and from PRIN 2022 MUR project 2022CB3PJ3 - First Light And Galaxy aSsembly (FLAGS) funded by the European Union – Next Generation EU. RA acknowledges support of Grant PID2023-147386NB-I00 funded by MICIU/AEI/10.13039/501100011033 and by ERDF/EU, and the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/50110001103. The project that gave rise to these results received the support of a fellowship from the “la Caixa” Foundation (ID 100010434). The fellowship code is LCF/BQ/PR24/12050015. LC acknowledges support from grants PID2022-139567NB-I00 and PIB2021-127718NB-I00 funded by the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/10.13039/501100011033 and by “ERDF A way of making Europe”. article_number: A122 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Sara full_name: Mascia, Sara id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29 last_name: Mascia - first_name: L. full_name: Pentericci, L. last_name: Pentericci - first_name: M. full_name: Llerena, M. last_name: Llerena - first_name: A. full_name: Calabrò, A. last_name: Calabrò - first_name: Jorryt J full_name: Matthee, Jorryt J id: 7439a258-f3c0-11ec-9501-9df22fe06720 last_name: Matthee orcid: 0000-0003-2871-127X - first_name: S. full_name: Flury, S. last_name: Flury - first_name: F. full_name: Pacucci, F. last_name: Pacucci - first_name: A. full_name: Jaskot, A. last_name: Jaskot - first_name: R. O. full_name: Amorín, R. O. last_name: Amorín - first_name: R. full_name: Bhatawdekar, R. last_name: Bhatawdekar - first_name: M. full_name: Castellano, M. last_name: Castellano - first_name: N. full_name: Cleri, N. last_name: Cleri - first_name: L. full_name: Costantin, L. last_name: Costantin - first_name: K. full_name: Davis, K. last_name: Davis - first_name: Claudia full_name: Di Cesare, Claudia id: 2d002343-372f-11ef-98ec-a164d20427cb last_name: Di Cesare - first_name: M. full_name: Dickinson, M. last_name: Dickinson - first_name: A. full_name: Fontana, A. last_name: Fontana - first_name: Y. full_name: Guo, Y. last_name: Guo - first_name: M. full_name: Giavalisco, M. last_name: Giavalisco - first_name: B. W. full_name: Holwerda, B. W. last_name: Holwerda - first_name: W. full_name: Hu, W. last_name: Hu - first_name: M. full_name: Huertas-Company, M. last_name: Huertas-Company - first_name: Intae full_name: Jung, Intae last_name: Jung - first_name: J. full_name: Kartaltepe, J. last_name: Kartaltepe - first_name: D. full_name: Kashino, D. last_name: Kashino - first_name: A. M. full_name: Koekemoer, A. M. last_name: Koekemoer - first_name: R. A. full_name: Lucas, R. A. last_name: Lucas - first_name: J. full_name: Lotz, J. last_name: Lotz - first_name: L. full_name: Napolitano, L. last_name: Napolitano - first_name: S. full_name: Jogee, S. last_name: Jogee - first_name: S. full_name: Wilkins, S. last_name: Wilkins citation: ama: Mascia S, Pentericci L, Llerena M, et al. Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe. Astronomy & Astrophysics. 2025;701. doi:10.1051/0004-6361/202553760 apa: Mascia, S., Pentericci, L., Llerena, M., Calabrò, A., Matthee, J. J., Flury, S., … Wilkins, S. (2025). Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202553760 chicago: Mascia, Sara, L. Pentericci, M. Llerena, A. Calabrò, Jorryt J Matthee, S. Flury, F. Pacucci, et al. “Little Impact of Mergers and Galaxy Morphology on the Production and Escape of Ionizing Photons in the Early Universe.” Astronomy & Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202553760. ieee: S. Mascia et al., “Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe,” Astronomy & Astrophysics, vol. 701. EDP Sciences, 2025. ista: Mascia S, Pentericci L, Llerena M, Calabrò A, Matthee JJ, Flury S, Pacucci F, Jaskot A, Amorín RO, Bhatawdekar R, Castellano M, Cleri N, Costantin L, Davis K, Di Cesare C, Dickinson M, Fontana A, Guo Y, Giavalisco M, Holwerda BW, Hu W, Huertas-Company M, Jung I, Kartaltepe J, Kashino D, Koekemoer AM, Lucas RA, Lotz J, Napolitano L, Jogee S, Wilkins S. 2025. Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe. Astronomy & Astrophysics. 701, A122. mla: Mascia, Sara, et al. “Little Impact of Mergers and Galaxy Morphology on the Production and Escape of Ionizing Photons in the Early Universe.” Astronomy & Astrophysics, vol. 701, A122, EDP Sciences, 2025, doi:10.1051/0004-6361/202553760. short: S. Mascia, L. Pentericci, M. Llerena, A. Calabrò, J.J. Matthee, S. Flury, F. Pacucci, A. Jaskot, R.O. Amorín, R. Bhatawdekar, M. Castellano, N. Cleri, L. Costantin, K. Davis, C. Di Cesare, M. Dickinson, A. Fontana, Y. Guo, M. Giavalisco, B.W. Holwerda, W. Hu, M. Huertas-Company, I. Jung, J. Kartaltepe, D. Kashino, A.M. Koekemoer, R.A. Lucas, J. Lotz, L. Napolitano, S. Jogee, S. Wilkins, Astronomy & Astrophysics 701 (2025). corr_author: '1' date_created: 2026-01-28T15:24:24Z date_published: 2025-09-01T00:00:00Z date_updated: 2026-02-09T07:33:46Z day: '01' ddc: - '520' department: - _id: JoMa doi: 10.1051/0004-6361/202553760 external_id: arxiv: - '2501.08268' file: - access_level: open_access checksum: 990e384ca19e14b35296712d3b9e2919 content_type: application/pdf creator: dernst date_created: 2026-02-09T07:28:08Z date_updated: 2026-02-09T07:28:08Z file_id: '21166' file_name: 2025_AstronomyAstrophysics_Mascia.pdf file_size: 9994234 relation: main_file success: 1 file_date_updated: 2026-02-09T07:28:08Z has_accepted_license: '1' intvolume: ' 701' language: - iso: eng month: '09' oa: 1 oa_version: Published Version project: - _id: bd9b2118-d553-11ed-ba76-db24564edfea grant_number: '101076224' name: Young galaxies as tracers and agents of cosmic reionization publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' scopus_import: '1' status: public title: Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 701 year: '2025' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21252' abstract: - lang: eng text: "Context. Recent observational results from asteroseismic studies show that an important fraction of solar-like stars do not present detectable stochastically excited acoustic oscillations. This non-detectability seems to correlate with a high rotation rate in the convective envelope and a high surface magnetic activity. At the same time, the properties of stellar convection are affected by rotation and magnetism.\r\nAims. We investigate the role of rotation in the excitation of acoustic modes in the convective envelope of solar-like stars, to evaluate its impact on the energy injected in the oscillations.\r\nMethods. We derived theoretical prescriptions for the excitation of acoustic waves in the convective envelope of rotating solar-like stars. We adopted the rotating mixing-length Theory to model the influence of rotation on convection. We used the MESA stellar evolution code and the GYRE stellar oscillation code to estimate the power injected in the oscillations from our theoretical prescriptions.\r\nResults. We demonstrate that the power injected in the acoustic modes is insensitive to rotation if a Gaussian time-correlation function is assumed, while it can decrease by up to 60% for a Lorentzian time-correlation function, for a 20 Ω⊙ rotation rate. We show that the modification of the excitation rate by rotation depends not only on the rotation rate but also on the radial and angular orders of the considered oscillation mode. This result can allow for better constraints on the properties of stellar convection by studying observationally acoustic mode excitation.\r\nConclusions. These results demonstrate how important it is to take into account the modification of stellar convection by rotation when evaluating the amplitude of the stellar oscillations it stochastically excites. They open the path for understanding the large variety of observed acoustic-mode amplitudes at the surface of solar-like stars as a function of surface rotation rates." acknowledgement: 'The authors thank the referee for detailed comments that allow them to improve their work. The authors thank Jordan Philidet and Kevin Belkacem for fruitful discussions. L.B. and Stéphane M. acknowledge support from the European Research Council (ERC) under the Horizon Europe program (Synergy Grant agreement 101071505: 4D-STAR), from the CNES SOHO-GOLF and PLATO grants at CEA-DAp, and from PNPS (CNRS/INSU). While partially funded by the European Union, views and opinions expressed are however those of the author 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. Savita M. acknowledges support from the Spanish Ministry of Science and Innovation with the grant no. PID2019-107061GB-C66 and through AEI under the Severo Ochoa Centres of Excellence Programme 2020–2023 (CEX2019-000920-S).' article_number: A25 article_processing_charge: Yes article_type: original author: - first_name: L. full_name: Bessila, L. last_name: Bessila - first_name: A. full_name: Deckx van Ruys, A. last_name: Deckx van Ruys - first_name: V. full_name: Buriasco, V. last_name: Buriasco - first_name: S. full_name: Mathis, S. last_name: Mathis - first_name: Lisa Annabelle full_name: Bugnet, Lisa Annabelle id: d9edb345-f866-11ec-9b37-d119b5234501 last_name: Bugnet orcid: 0000-0003-0142-4000 - first_name: R. A. full_name: García, R. A. last_name: García - first_name: S. full_name: Mathur, S. last_name: Mathur citation: ama: Bessila L, Deckx van Ruys A, Buriasco V, et al. The impact of rotation on the stochastic excitation of stellar acoustic modes in solar-like pulsators. Astronomy & Astrophysics. 2025;700. doi:10.1051/0004-6361/202452093 apa: Bessila, L., Deckx van Ruys, A., Buriasco, V., Mathis, S., Bugnet, L. A., García, R. A., & Mathur, S. (2025). The impact of rotation on the stochastic excitation of stellar acoustic modes in solar-like pulsators. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202452093 chicago: Bessila, L., A. Deckx van Ruys, V. Buriasco, S. Mathis, Lisa Annabelle Bugnet, R. A. García, and S. Mathur. “The Impact of Rotation on the Stochastic Excitation of Stellar Acoustic Modes in Solar-like Pulsators.” Astronomy & Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202452093. ieee: L. Bessila et al., “The impact of rotation on the stochastic excitation of stellar acoustic modes in solar-like pulsators,” Astronomy & Astrophysics, vol. 700. EDP Sciences, 2025. ista: Bessila L, Deckx van Ruys A, Buriasco V, Mathis S, Bugnet LA, García RA, Mathur S. 2025. The impact of rotation on the stochastic excitation of stellar acoustic modes in solar-like pulsators. Astronomy & Astrophysics. 700, A25. mla: Bessila, L., et al. “The Impact of Rotation on the Stochastic Excitation of Stellar Acoustic Modes in Solar-like Pulsators.” Astronomy & Astrophysics, vol. 700, A25, EDP Sciences, 2025, doi:10.1051/0004-6361/202452093. short: L. Bessila, A. Deckx van Ruys, V. Buriasco, S. Mathis, L.A. Bugnet, R.A. García, S. Mathur, Astronomy & Astrophysics 700 (2025). date_created: 2026-02-16T15:46:59Z date_published: 2025-08-01T00:00:00Z date_updated: 2026-02-17T13:10:18Z day: '01' ddc: - '520' department: - _id: LiBu doi: 10.1051/0004-6361/202452093 file: - access_level: open_access checksum: b8a0927307c1d82025bcb5af47b20b26 content_type: application/pdf creator: dernst date_created: 2026-02-17T13:07:45Z date_updated: 2026-02-17T13:07:45Z file_id: '21306' file_name: 2025_AstronomyAstrophysics_Bessila.pdf file_size: 7161755 relation: main_file success: 1 file_date_updated: 2026-02-17T13:07:45Z has_accepted_license: '1' intvolume: ' 700' language: - iso: eng month: '08' oa: 1 oa_version: Published Version publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' status: public title: The impact of rotation on the stochastic excitation of stellar acoustic modes in solar-like pulsators tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 700 year: '2025' ...