[{"date_updated":"2026-06-19T09:50:33Z","date_published":"2026-06-10T00:00:00Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"external_id":{"arxiv":["2602.15935"]},"file":[{"relation":"main_file","date_updated":"2026-06-19T09:45:21Z","file_name":"2026_AstrophysicalJourLetters_Chisholm.pdf","checksum":"66949af6e620c8ef37de42688829a3e3","content_type":"application/pdf","file_size":919919,"access_level":"open_access","creator":"dernst","date_created":"2026-06-19T09:45:21Z","success":1,"file_id":"22098"}],"day":"10","year":"2026","doi":"10.3847/2041-8213/ae6dae","scopus_import":"1","has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We thank the referees for detailed and highly constructive reports that significantly improved the scope and breadth of the manuscript. J.C. thanks Hollis Akins, Volker Bromm, Rui Chaves-Marques, Steve Finkelstein, Karl Gebhardt, Keith Hawkins, Harley Katz, Stellar Offner, Daniel Schaerer, Grace Telford, and Jorick Vink for conversations that improved the Letter. A.d.G. acknowledges support from a Clay Fellowship awarded by the Smithsonian Astrophysical Observatory. M.B.K. acknowledges support from NSF grants AST-2108962 and AST-2408247; NASA grant 80NSSC22K0827; HST-GO-16686, HST-AR-17028, JWST-GO-03788, and JWST-AR-06278 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555; and from the Samuel T. and Fern Yanagisawa Regents Professorship in Astronomy at UT Austin. A.A.C.S. acknowledges support by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) in the form of an Emmy Noether Research Group—Project-ID 445674056 (SA4064/1-1, PI Sander). A.A.C.S. further acknowledges support from the Deutsches Zentrum für Luft und Raumfahrt (DLR) grant grants 50 OR 2509 (PI: A.A.C. Sander) and 50 OR 2306 (PI: V. Ramachandran/A.A.C. Sander) as well as from the Federal Ministry of Research, Technology, and Space (BMFTR) and the Baden-Württemberg Ministry of Science as part of the Excellence Strategy of the German Federal and State Governments. This project was cofunded by the European Union (Project 101183150—OCEANS).\r\n\r\nThis 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 programs 1180, 1181, 1208, 1212, 1213, 1215, 1286, 1345, 1433, 2198, 2561, 2750, 2767, 4106, 4233, 5105, 5224, 6368, and 6585.","language":[{"iso":"eng"}],"issue":"1","department":[{"_id":"JoMa"}],"intvolume":"      1004","_id":"21998","oa_version":"Published Version","type":"journal_article","title":"Little Red Dots as globular clusters in formation","OA_place":"publisher","publication_status":"published","citation":{"apa":"Chisholm, J., Berg, D. A., Boylan-Kolchin, M., De Graaff, A., Furtak, L. J., Kokorev, V., … Sander, A. A. C. (2026). Little Red Dots as globular clusters in formation. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ae6dae\">https://doi.org/10.3847/2041-8213/ae6dae</a>","ieee":"J. Chisholm <i>et al.</i>, “Little Red Dots as globular clusters in formation,” <i>The Astrophysical Journal Letters</i>, vol. 1004, no. 1. IOP Publishing, 2026.","ama":"Chisholm J, Berg DA, Boylan-Kolchin M, et al. Little Red Dots as globular clusters in formation. <i>The Astrophysical Journal Letters</i>. 2026;1004(1). doi:<a href=\"https://doi.org/10.3847/2041-8213/ae6dae\">10.3847/2041-8213/ae6dae</a>","mla":"Chisholm, John, et al. “Little Red Dots as Globular Clusters in Formation.” <i>The Astrophysical Journal Letters</i>, vol. 1004, no. 1, L4, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/2041-8213/ae6dae\">10.3847/2041-8213/ae6dae</a>.","ista":"Chisholm J, Berg DA, Boylan-Kolchin M, De Graaff A, Furtak LJ, Kokorev V, Matthee JJ, Muñoz JB, Naidu RP, Sander AAC. 2026. Little Red Dots as globular clusters in formation. The Astrophysical Journal Letters. 1004(1), L4.","chicago":"Chisholm, John, Danielle A. Berg, Michael Boylan-Kolchin, Anna De Graaff, Lukas J. Furtak, Vasily Kokorev, Jorryt J Matthee, Julian B. Muñoz, Rohan P. Naidu, and Andreas A.C. Sander. “Little Red Dots as Globular Clusters in Formation.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/2041-8213/ae6dae\">https://doi.org/10.3847/2041-8213/ae6dae</a>.","short":"J. Chisholm, D.A. Berg, M. Boylan-Kolchin, A. De Graaff, L.J. Furtak, V. Kokorev, J.J. Matthee, J.B. Muñoz, R.P. Naidu, A.A.C. Sander, The Astrophysical Journal Letters 1004 (2026)."},"author":[{"first_name":"John","last_name":"Chisholm","full_name":"Chisholm, John"},{"first_name":"Danielle A.","last_name":"Berg","full_name":"Berg, Danielle A."},{"last_name":"Boylan-Kolchin","first_name":"Michael","full_name":"Boylan-Kolchin, Michael"},{"full_name":"De Graaff, Anna","first_name":"Anna","last_name":"De Graaff"},{"last_name":"Furtak","first_name":"Lukas J.","full_name":"Furtak, Lukas J."},{"full_name":"Kokorev, Vasily","last_name":"Kokorev","first_name":"Vasily"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"first_name":"Julian B.","last_name":"Muñoz","full_name":"Muñoz, Julian B."},{"last_name":"Naidu","first_name":"Rohan P.","full_name":"Naidu, Rohan P."},{"last_name":"Sander","first_name":"Andreas A.C.","full_name":"Sander, Andreas A.C."}],"arxiv":1,"month":"06","status":"public","abstract":[{"text":"Little Red Dots (LRDs), among the most enigmatic high-redshift discoveries by JWST, are commonly believed to be powered by accreting supermassive black holes. Here, we explore the possibility that these sources are globular clusters in formation, with rest-frame UV arising from a very young stellar population and rest-frame optical from a short-lived supermassive (>104 M⊙) star. The spectral profiles of LRDs are broadly consistent with this scenario, though the observed temperatures and bolometric luminosities favor emission reprocessed by optically thick continuum-driven winds not fully captured by current models. The LRD z ∼ 5−7 UV luminosity function naturally evolves, under standard evolutionary and mass-loss prescriptions, into a present-day mass function with a turnover at log10(M*/M⊙) = 5.3 and an exponential cutoff at high masses, consistent with local globular cluster populations. We estimate the total present-day number density of LRDs formed across all redshifts to be ≈0.3 Mpc−3, similar within uncertainties to local globular clusters. The observed LRD redshift range matches the age distribution of metal-poor globular clusters, without current LRD counterparts to the metal-rich population. If LRDs are globular clusters in formation, we predict chemical abundance patterns characteristic of multiple stellar populations, including enhanced He and N, and potential Na–O and Al–Mg anticorrelations. These results offer a local perspective to explore this surprisingly abundant population of distant sources, and a potential new window into extreme stellar astrophysics in the early Universe.","lang":"eng"}],"quality_controlled":"1","date_created":"2026-06-14T22:01:42Z","oa":1,"OA_type":"gold","PlanS_conform":"1","volume":1004,"article_processing_charge":"Yes","publisher":"IOP Publishing","article_type":"original","file_date_updated":"2026-06-19T09:45:21Z","article_number":"L4","ddc":["520"],"DOAJ_listed":"1","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"publication":"The Astrophysical Journal Letters"},{"publication":"The Astrophysical Journal Letters","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"DOAJ_listed":"1","status":"public","abstract":[{"lang":"eng","text":"JWST’s “little red dots” (LRDs) are increasingly interpreted as active galactic nuclei (AGN) obscured by dense thermalized gas rather than dust as evidenced by their X-ray weakness, blackbody-like continua, and Balmer line profiles. Key questions are how LRDs connect to standard UV-luminous AGN, whether transitional phases exist, and whether they are observable. We present the “X-ray dot” (XRD), a compact source at z = 3.28 observed by the NIRSpec Wide Guaranteed Time Observation survey. The XRD exhibits LRD hallmarks: a blackbody-like (Teff ≃ 6400 K) red continuum, a faint but blue rest-UV excess, falling mid-IR emission, and broad Balmer lines (FWHM ∼ 2700–3200 km s−1). Unlike LRDs, however, it is remarkably X-ray luminous (L2−10 keV = 1044.18 erg s−1) and has a continuum inflection that is blueward of the Balmer limit. We find that the red rest-optical and blue mid-IR continuum cannot be reproduced by standard dust-attenuated AGN models without invoking extremely steep extinction curves, nor can the weak mid-IR emission be reconciled with well-established X-ray–torus scaling relations. We therefore consider an alternative scenario: the XRD may be an LRD in transition, where the gas envelope dominates the optical continuum but optically thin sight lines allow X-rays to escape. The XRD may thus provide a physical link between LRDs and standard AGN, offering direct evidence that LRDs are powered by supermassive black holes and providing insight into their accretion properties."}],"month":"03","article_number":"L18","ddc":["520"],"publisher":"IOP Publishing","file_date_updated":"2026-05-04T07:11:37Z","article_type":"original","volume":1000,"article_processing_charge":"Yes","quality_controlled":"1","OA_type":"gold","oa":1,"date_created":"2026-04-12T22:01:48Z","type":"journal_article","oa_version":"Published Version","_id":"21709","intvolume":"      1000","department":[{"_id":"JoMa"}],"arxiv":1,"OA_place":"publisher","citation":{"ama":"Hviding RE, De Graaff A, Liu H, et al. The X-ray dot: Exotic dust or a late-stage Little Red Dot? <i>The Astrophysical Journal Letters</i>. 2026;1000(1). doi:<a href=\"https://doi.org/10.3847/2041-8213/ae4c88\">10.3847/2041-8213/ae4c88</a>","ieee":"R. E. Hviding <i>et al.</i>, “The X-ray dot: Exotic dust or a late-stage Little Red Dot?,” <i>The Astrophysical Journal Letters</i>, vol. 1000, no. 1. IOP Publishing, 2026.","apa":"Hviding, R. E., De Graaff, A., Liu, H., Goulding, A. D., Ma, Y., Greene, J. E., … Wang, B. (2026). The X-ray dot: Exotic dust or a late-stage Little Red Dot? <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ae4c88\">https://doi.org/10.3847/2041-8213/ae4c88</a>","short":"R.E. Hviding, A. De Graaff, H. Liu, A.D. Goulding, Y. Ma, J.E. Greene, L.A. Boogaard, A.J. Bunker, N.J. Cleri, M. Franx, M. Hirschmann, J. Leja, J.J. Matthee, R.P. Naidu, D.J. Setton, H. Übler, G. Venturi, B. Wang, The Astrophysical Journal Letters 1000 (2026).","chicago":"Hviding, Raphael E., Anna De Graaff, Hanpu Liu, Andy D. Goulding, Yilun Ma, Jenny E. Greene, Leindert A. Boogaard, et al. “The X-Ray Dot: Exotic Dust or a Late-Stage Little Red Dot?” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/2041-8213/ae4c88\">https://doi.org/10.3847/2041-8213/ae4c88</a>.","ista":"Hviding RE, De Graaff A, Liu H, Goulding AD, Ma Y, Greene JE, Boogaard LA, Bunker AJ, Cleri NJ, Franx M, Hirschmann M, Leja J, Matthee JJ, Naidu RP, Setton DJ, Übler H, Venturi G, Wang B. 2026. The X-ray dot: Exotic dust or a late-stage Little Red Dot? The Astrophysical Journal Letters. 1000(1), L18.","mla":"Hviding, Raphael E., et al. “The X-Ray Dot: Exotic Dust or a Late-Stage Little Red Dot?” <i>The Astrophysical Journal Letters</i>, vol. 1000, no. 1, L18, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/2041-8213/ae4c88\">10.3847/2041-8213/ae4c88</a>."},"publication_status":"published","author":[{"full_name":"Hviding, Raphael E.","last_name":"Hviding","first_name":"Raphael E."},{"first_name":"Anna","last_name":"De Graaff","full_name":"De Graaff, Anna"},{"full_name":"Liu, Hanpu","first_name":"Hanpu","last_name":"Liu"},{"last_name":"Goulding","first_name":"Andy D.","full_name":"Goulding, Andy D."},{"first_name":"Yilun","last_name":"Ma","full_name":"Ma, Yilun"},{"full_name":"Greene, Jenny E.","last_name":"Greene","first_name":"Jenny E."},{"first_name":"Leindert A.","last_name":"Boogaard","full_name":"Boogaard, Leindert A."},{"last_name":"Bunker","first_name":"Andrew J.","full_name":"Bunker, Andrew J."},{"full_name":"Cleri, Nikko J.","last_name":"Cleri","first_name":"Nikko J."},{"first_name":"Marijn","last_name":"Franx","full_name":"Franx, Marijn"},{"full_name":"Hirschmann, Michaela","last_name":"Hirschmann","first_name":"Michaela"},{"last_name":"Leja","first_name":"Joel","full_name":"Leja, Joel"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."},{"full_name":"Setton, David J.","last_name":"Setton","first_name":"David J."},{"full_name":"Übler, Hannah","first_name":"Hannah","last_name":"Übler"},{"full_name":"Venturi, Giacomo","first_name":"Giacomo","last_name":"Venturi"},{"full_name":"Wang, Bingjie","first_name":"Bingjie","last_name":"Wang"}],"title":"The X-ray dot: Exotic dust or a late-stage Little Red Dot?","doi":"10.3847/2041-8213/ae4c88","year":"2026","day":"20","file":[{"file_id":"21784","success":1,"date_created":"2026-05-04T07:11:37Z","creator":"dernst","access_level":"open_access","file_size":2821786,"content_type":"application/pdf","file_name":"2026_AstrophysicalJourLetters_Hviding.pdf","checksum":"1be4f361bf59aa08b8c98ed4f475a463","date_updated":"2026-05-04T07:11:37Z","relation":"main_file"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"external_id":{"arxiv":["2601.09778"]},"date_published":"2026-03-20T00:00:00Z","date_updated":"2026-05-04T07:13:07Z","issue":"1","acknowledgement":"We would like to thank the anonymous reviewer for their constructive comments, which improved the final manuscript.\r\n\r\nWe thank Bernd Husemann for his critical contributions to the NIRSpec Wide GTO survey, and in particular his help in selecting high-priority X-ray-luminous targets.\r\n\r\nR.E.H. acknowledges support by the German Aerospace Center (DLR) and the Federal Ministry for Economic Affairs and Energy (BMWi) through program 50OR2403 “RUBIES.” A.d.G. acknowledges support from a Clay Fellowship awarded by the Smithsonian Astrophysical Observatory. A.J.B. acknowledges funding from the “FirstGalaxies” Advanced grant from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 789056). R.P.N. thanks Neil Pappalardo and Jane Pappalardo for their generous support of the MIT Pappalardo Fellowships in Physics. Support for this work was provided by the Brinson Foundation through a Brinson Prize Fellowship grant. H.Ü. acknowledges funding by the European Union (ERC APEX, 101164796). Views and opinions expressed are, however, those of the authors only and do not necessarily reflect those of the European Union or the European Research Council Executive Agency. Neither the European Union nor the granting authority can be held responsible for them. G.V. acknowledges support from European Union’s HE ERC Starting grant No. 101040227—WINGS. B.W. acknowledges support provided by NASA through Hubble Fellowship grant HST-HF2-51592.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, In., for NASA, under the contract NAS 5-26555.\r\n\r\nThe data products presented herein were retrieved from the Dawn JWST Archive (DJA). DJA is an initiative of the Cosmic Dawn Center (DAWN).\r\n\r\nThis 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 programs Nos. GTO-1213. The data described here may be obtained from the MAST archive at DOI: 10.17909/qffz-b324.\r\n\r\nThis Letter employs a list of Chandra datasets, obtained by the Chandra X-ray Observatory, contained in DOI: 10.25574/cdc.540.\r\n\r\nThis work is based on observations taken by the 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.\r\n\r\nThis work makes use of color palettes created by Martin Krzywinski designed for colorblindness. The color palettes and more information can be found at http://mkweb.bcgsc.ca/colorblind/.\r\n\r\nFacilities: CXO - Chandra X-ray Observatory satellite (ACIS), HST - Hubble Space Telescope satellite (ACS, WFC3) - , CFHT - Canada-France-Hawaii Telescope (WIRCam), JWST - James Webb Space Telescope (NIRSpec), Spitzer - Spitzer Space Telescope satellite (IRAC, MIPS) - , JCMT - James Clerk Maxwell Telescope (SCUBA).\r\n\r\nSoftware: Astropy (Astropy Collaboration et al. 2013, 2018, 2022), dust_attenuation, dust_extinction (K. Gordon 2024), jax (J. Bradbury et al. 2018), LaTeX (L. Lamport 1994), Matplotlib (J. D. Hunter 2007), NumPy (T. E. Oliphant 2006; S. van der Walt et al. 2011; C. R. Harris et al. 2020), NumPyro (D. Phan et al. 2019), scipy (P. Virtanen et al. 2020), sedpy (B. Johnson & J. Leja 2017), specutils (Astropy-Specutils Development Team 2019), unite (R. E. Hviding 2025).","language":[{"iso":"eng"}],"scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1"},{"date_created":"2026-04-12T22:01:49Z","OA_type":"gold","oa":1,"quality_controlled":"1","volume":996,"article_processing_charge":"Yes","article_type":"original","file_date_updated":"2026-05-04T09:49:53Z","publisher":"IOP Publishing","ddc":["520"],"article_number":"L44","month":"01","abstract":[{"text":"GW231123 represents the most massive binary–black hole merger detected to date, lying firmly within, or even above, the pair-instability mass gap. The component spins are both exceptionally high (a1 = 0.90 +0.10/-0.19, a2 = 0.80 +0.20/-0.51), which is difficult to explain with repeated mergers. Here we show that the black hole spin vectors are closely aligned with each other while significantly tilted relative to the binary’s orbital angular momentum, pointing to a common accretion-driven origin. We examine astrophysical formation channels capable of producing near-equal, high-mass, and mutually aligned spins consistent with GW231123—particularly binaries embedded in AGN disks and Population III remnants, which grew via coherent misaligned gas accretion. We further argue that other high-mass, high-spin events, e.g., GW190521, may share a similar evolutionary pathway. These findings underscore the critical role of sustained, coherent accretion in shaping the most extreme black hole binaries.","lang":"eng"}],"status":"public","DOAJ_listed":"1","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"publication":"The Astrophysical Journal Letters","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","scopus_import":"1","language":[{"iso":"eng"}],"acknowledgement":"The authors thank Davide Gerosa and Matthew Mould for valuable suggestions. We are grateful for support by the National Science Foundation under grant No. PHY-2309024 (I.B.) and by NASA under grants 80NSSC22K0822 and 80NSSC24K0440 (Z.H.). We used OpenAI’s ChatGPT (OpenAI 2025) during the preparation of this manuscript. This material is based upon work supported by NSF’s LIGO Laboratory, which is a major facility fully funded by the National Science Foundation.","issue":"2","date_published":"2026-01-10T00:00:00Z","date_updated":"2026-05-04T09:54:18Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"external_id":{"arxiv":["2508.08558"]},"file":[{"success":1,"file_id":"21788","access_level":"open_access","date_created":"2026-05-04T09:49:53Z","creator":"dernst","content_type":"application/pdf","checksum":"ac46ba3d13f0150ccbc42665bed3ae47","file_name":"2026_AstrophysicalJourLetters_Bartos.pdf","file_size":866725,"relation":"main_file","date_updated":"2026-05-04T09:49:53Z"}],"year":"2026","day":"10","doi":"10.3847/2041-8213/ae2bff","title":"Accretion is all you need: Black Hole spin alignment in merger GW231123 indicates accretion pathway","publication_status":"published","citation":{"mla":"Bartos, Imre, and Zoltán Haiman. “Accretion Is All You Need: Black Hole Spin Alignment in Merger GW231123 Indicates Accretion Pathway.” <i>The Astrophysical Journal Letters</i>, vol. 996, no. 2, L44, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/2041-8213/ae2bff\">10.3847/2041-8213/ae2bff</a>.","ista":"Bartos I, Haiman Z. 2026. Accretion is all you need: Black Hole spin alignment in merger GW231123 indicates accretion pathway. The Astrophysical Journal Letters. 996(2), L44.","chicago":"Bartos, Imre, and Zoltán Haiman. “Accretion Is All You Need: Black Hole Spin Alignment in Merger GW231123 Indicates Accretion Pathway.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/2041-8213/ae2bff\">https://doi.org/10.3847/2041-8213/ae2bff</a>.","short":"I. Bartos, Z. Haiman, The Astrophysical Journal Letters 996 (2026).","apa":"Bartos, I., &#38; Haiman, Z. (2026). Accretion is all you need: Black Hole spin alignment in merger GW231123 indicates accretion pathway. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ae2bff\">https://doi.org/10.3847/2041-8213/ae2bff</a>","ieee":"I. Bartos and Z. Haiman, “Accretion is all you need: Black Hole spin alignment in merger GW231123 indicates accretion pathway,” <i>The Astrophysical Journal Letters</i>, vol. 996, no. 2. IOP Publishing, 2026.","ama":"Bartos I, Haiman Z. Accretion is all you need: Black Hole spin alignment in merger GW231123 indicates accretion pathway. <i>The Astrophysical Journal Letters</i>. 2026;996(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/ae2bff\">10.3847/2041-8213/ae2bff</a>"},"author":[{"last_name":"Bartos","first_name":"Imre","full_name":"Bartos, Imre"},{"first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403"}],"OA_place":"publisher","corr_author":"1","arxiv":1,"department":[{"_id":"ZoHa"}],"intvolume":"       996","_id":"21713","oa_version":"Published Version","type":"journal_article"},{"title":"Formation of Be stars via wind accretion: Case study on Black Hole + Be star binaries","OA_place":"publisher","citation":{"ista":"Li Z, Jia S, Wei D, Ge H, Chen H, Zhang Y, Chen X, Han Z. 2026. Formation of Be stars via wind accretion: Case study on Black Hole + Be star binaries. The Astrophysical Journal Letters. 996(2), L42.","short":"Z. Li, S. Jia, D. Wei, H. Ge, H. Chen, Y. Zhang, X. Chen, Z. Han, The Astrophysical Journal Letters 996 (2026).","chicago":"Li, Zhenwei, Shi Jia, Dandan Wei, Hongwei Ge, Hailiang Chen, Yangyang Zhang, Xuefei Chen, and Zhanwen Han. “Formation of Be Stars via Wind Accretion: Case Study on Black Hole + Be Star Binaries.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/2041-8213/ae3008\">https://doi.org/10.3847/2041-8213/ae3008</a>.","mla":"Li, Zhenwei, et al. “Formation of Be Stars via Wind Accretion: Case Study on Black Hole + Be Star Binaries.” <i>The Astrophysical Journal Letters</i>, vol. 996, no. 2, L42, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/2041-8213/ae3008\">10.3847/2041-8213/ae3008</a>.","apa":"Li, Z., Jia, S., Wei, D., Ge, H., Chen, H., Zhang, Y., … Han, Z. (2026). Formation of Be stars via wind accretion: Case study on Black Hole + Be star binaries. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ae3008\">https://doi.org/10.3847/2041-8213/ae3008</a>","ieee":"Z. Li <i>et al.</i>, “Formation of Be stars via wind accretion: Case study on Black Hole + Be star binaries,” <i>The Astrophysical Journal Letters</i>, vol. 996, no. 2. IOP Publishing, 2026.","ama":"Li Z, Jia S, Wei D, et al. Formation of Be stars via wind accretion: Case study on Black Hole + Be star binaries. <i>The Astrophysical Journal Letters</i>. 2026;996(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/ae3008\">10.3847/2041-8213/ae3008</a>"},"publication_status":"published","author":[{"full_name":"Li, Zhenwei","last_name":"Li","first_name":"Zhenwei"},{"first_name":"Shi","last_name":"Jia","full_name":"Jia, Shi"},{"last_name":"Wei","id":"5dd129bd-0601-11ef-b325-833284687b76","first_name":"Dandan","full_name":"Wei, Dandan"},{"first_name":"Hongwei","last_name":"Ge","full_name":"Ge, Hongwei"},{"full_name":"Chen, Hailiang","last_name":"Chen","first_name":"Hailiang"},{"last_name":"Zhang","first_name":"Yangyang","full_name":"Zhang, Yangyang"},{"full_name":"Chen, Xuefei","first_name":"Xuefei","last_name":"Chen"},{"first_name":"Zhanwen","last_name":"Han","full_name":"Han, Zhanwen"}],"arxiv":1,"department":[{"_id":"YlGo"}],"intvolume":"       996","_id":"21714","oa_version":"Published Version","type":"journal_article","scopus_import":"1","has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We are deeply grateful to the anonymous referee for the insightful comments, which have significantly improved the quality of this work. The authors express their gratitude to Zhaoyu Zuo and I. El Mellah for sharing the grids of wind accretion efficiencies. Z.L. thanks Matthias U. Kruckow for detailed discussions about the BH formation. This work is supported by the Natural Science Foundation of China (grant Nos. 12125303, 12525304, 12288102, 12090040/3, 12473034, 12503044, 12333008, 12433009, 12422305, 12273105, 12073070, 12173081), the Strategic Priority Research Program of the Chinese Academy of Sciences (grant Nos. XDB1160303, XDB1160201, XDB1160000), the National Key R&D Program of China (grant Nos. 2021YFA1600403 and 2021YFA1600400), the CAS “Light of West China,” the Yunnan Revitalization Talent Support Program-Science & Technology Champion Project (No. 202305AB350003) and Young Talent project, the International Centre of Supernovae (ICESUN), Yunnan Key Laboratory of Supernova Research (Nos. 202302AN360001 and 202201BC070003), Yunnan Fundamental Research Projects (No. 202401AT070139), and the Natural Science Foundation of Henan Province (No. 242300420944). X.C. acknowledges the New Cornerstone Science Foundation through the XPLORER PRIZE. The authors gratefully acknowledge the “PHOENIX Supercomputing Platform” jointly operated by the Binary Population Synthesis Group and the Stellar Astrophysics Group at Yunnan Observatories, Chinese Academy of Sciences.","language":[{"iso":"eng"}],"issue":"2","date_updated":"2026-04-16T06:26:18Z","date_published":"2026-01-10T00:00:00Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"external_id":{"arxiv":["2512.18565"]},"file":[{"file_size":5202345,"content_type":"application/pdf","file_name":"2026_AstrophysicalJourLetters_Li.pdf","checksum":"09200c1cf405101abdd298ce80c9a90d","date_updated":"2026-04-16T06:24:30Z","relation":"main_file","file_id":"21741","success":1,"date_created":"2026-04-16T06:24:30Z","creator":"dernst","access_level":"open_access"}],"day":"10","year":"2026","doi":"10.3847/2041-8213/ae3008","DOAJ_listed":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"publication":"The Astrophysical Journal Letters","quality_controlled":"1","OA_type":"gold","date_created":"2026-04-12T22:01:50Z","oa":1,"volume":996,"article_processing_charge":"Yes","publisher":"IOP Publishing","file_date_updated":"2026-04-16T06:24:30Z","article_type":"original","article_number":"L42","ddc":["520"],"month":"01","status":"public","abstract":[{"lang":"eng","text":"Be stars are rapidly rotating main-sequence stars that play a crucial role in understanding stellar evolution and binary interactions. In this Letter, we propose a new formation scenario for black hole (BH) + Be star binaries (hereafter BHBe binaries), where the Be star is produced through the wind Roche lobe overflow (WRLOF) mechanism. Our analysis is based on numerical simulations of the WRLOF process in massive binaries, building on recent theoretical work. We demonstrate that the WRLOF model can efficiently form BHBe binaries under reasonable assumptions on stellar wind velocities. Using rapid binary population synthesis, we estimate the population of such systems in the Milky Way, predicting ∼1800−3200 currently existing BHBe binaries originating from the WRLOF channel. These systems are characterized by high eccentricities and exceptionally wide orbits, with typical orbital periods exceeding 1000 days and a peak distribution around ∼10,000 days. Due to their long orbital separations, these BHBe binaries are promising targets for future detection via astrometric and interferometric observations."}]},{"type":"journal_article","oa_version":"Published Version","_id":"21846","intvolume":"      1002","department":[{"_id":"ZoHa"},{"_id":"JoMa"}],"arxiv":1,"project":[{"grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization"}],"OA_place":"publisher","publication_status":"published","citation":{"mla":"Baggen, Josephine F. W., et al. “Connecting the Dots: UV-Bright Companions of Little Red Dots as Lyman–Werner Sources Enabling Direct-Collapse Black Hole Formation.” <i>The Astrophysical Journal Letters</i>, vol. 1002, no. 1, L4, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/2041-8213/ae58a5\">10.3847/2041-8213/ae58a5</a>.","chicago":"Baggen, Josephine F.W., Matthew T. Scoggins, Pieter Van Dokkum, Zoltán Haiman, Alberto Torralba Torregrosa, and Jorryt J Matthee. “Connecting the Dots: UV-Bright Companions of Little Red Dots as Lyman–Werner Sources Enabling Direct-Collapse Black Hole Formation.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/2041-8213/ae58a5\">https://doi.org/10.3847/2041-8213/ae58a5</a>.","short":"J.F.W. Baggen, M.T. Scoggins, P. Van Dokkum, Z. Haiman, A. Torralba Torregrosa, J.J. Matthee, The Astrophysical Journal Letters 1002 (2026).","ista":"Baggen JFW, Scoggins MT, Van Dokkum P, Haiman Z, Torralba Torregrosa A, Matthee JJ. 2026. Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation. The Astrophysical Journal Letters. 1002(1), L4.","ama":"Baggen JFW, Scoggins MT, Van Dokkum P, Haiman Z, Torralba Torregrosa A, Matthee JJ. Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation. <i>The Astrophysical Journal Letters</i>. 2026;1002(1). doi:<a href=\"https://doi.org/10.3847/2041-8213/ae58a5\">10.3847/2041-8213/ae58a5</a>","ieee":"J. F. W. Baggen, M. T. Scoggins, P. Van Dokkum, Z. Haiman, A. Torralba Torregrosa, and J. J. Matthee, “Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation,” <i>The Astrophysical Journal Letters</i>, vol. 1002, no. 1. IOP Publishing, 2026.","apa":"Baggen, J. F. W., Scoggins, M. T., Van Dokkum, P., Haiman, Z., Torralba Torregrosa, A., &#38; Matthee, J. J. (2026). Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ae58a5\">https://doi.org/10.3847/2041-8213/ae58a5</a>"},"author":[{"full_name":"Baggen, Josephine F.W.","last_name":"Baggen","first_name":"Josephine F.W."},{"full_name":"Scoggins, Matthew T.","first_name":"Matthew T.","last_name":"Scoggins"},{"first_name":"Pieter","last_name":"Van Dokkum","full_name":"Van Dokkum, Pieter"},{"last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","orcid":"0000-0003-3633-5403","full_name":"Haiman, Zoltán"},{"first_name":"Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","last_name":"Torralba Torregrosa","orcid":"0000-0001-5586-6950","full_name":"Torralba Torregrosa, Alberto"},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"}],"title":"Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation","doi":"10.3847/2041-8213/ae58a5","day":"10","year":"2026","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file":[{"file_size":13359642,"content_type":"application/pdf","file_name":"2026_AstrophysicalJourLetters_Baggen.pdf","checksum":"8c31d8603cd6ad39c772a72d136dc3f8","date_updated":"2026-05-11T06:44:37Z","relation":"main_file","file_id":"21851","success":1,"date_created":"2026-05-11T06:44:37Z","creator":"dernst","access_level":"open_access"}],"external_id":{"arxiv":["2602.02702"]},"date_updated":"2026-05-11T06:48:33Z","date_published":"2026-04-10T00:00:00Z","issue":"1","acknowledgement":"We thank Earl Bellinger, Fabio Pacucci, Andrea Ferrara, and Dale Kocevski for useful discussions. 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 imaging observations are associated with programs 1345, 1180, 1181, 1243, 6882, 2561, 1324, 4111, and 1895. The compiled dataset can be accessed at doi:10.17909/1m8f-9c47. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. J.M. and A.T. acknowledge funding by the European Union (ERC, AGENTS, 101076224). This work was performed in part at Aspen Center for Physics, which is supported by National Science Foundation grant PHY-2210452. This work used the following Python packages: Matplotlib (J. D. Hunter 2007), SciPy (P. Virtanen et al. 2020), NumPy (S. van der Walt et al. 2011), AstroPy (Astropy Collaboration et al. 2022), colossus (B. Diemer 2018), and photutils (L. Bradley et al. 2025).","language":[{"iso":"eng"}],"scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","publication":"The Astrophysical Journal Letters","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"DOAJ_listed":"1","status":"public","abstract":[{"text":"We compile a sample of 83 little red dots (LRDs) with JWST imaging and find that a substantial fraction (∼43%, rising to ≳80% for the most luminous LRDs) host one or more spatially offset, UV-bright companions at projected separations of 0.5 kpc ≲ d ≲ 5 kpc, with median 〈d〉 = 1.0 kpc. This fraction is even higher when smaller spatial scales are probed at high signal-to-noise ratio: the two most strongly lensed LRDs, A383-LRD1 and the newly discovered A68-LRD1, both have UV-bright companions at separations of only d ∼ 0.3 kpc, below the resolution limit of most unlensed JWST samples. We explore whether these ubiquitous red/blue configurations may be physically linked to the formation of LRDs, in analogy with the “synchronized pair” scenario originally proposed for direct-collapse black hole formation. In this picture, UV radiation from the companions, with typically modest stellar masses (M∗ ∼ 108−109 M⊙), suppresses molecular hydrogen cooling in nearby gas, allowing nearly isothermal collapse and the formation of extremely compact objects, such as massive black holes, supermassive stars, or quasi-stars. Using component-resolved photometry and spectral energy distribution modeling, we infer Lyman–Werner radiation fields of J21,LW ∼ 102.5–105 at the locations of the red components, comparable to those required in direct-collapse models, suggesting that the necessary photodissociation conditions are realized in many LRD systems. This framework provides a simple and self-consistent explanation for the extreme compactness and distinctive spectral properties of LRDs and links long-standing theoretical models for early compact object formation directly to a population now observed with JWST in the early Universe.","lang":"eng"}],"month":"04","ddc":["520"],"article_number":"L4","publisher":"IOP Publishing","article_type":"original","file_date_updated":"2026-05-11T06:44:37Z","volume":1002,"article_processing_charge":"Yes","quality_controlled":"1","date_created":"2026-05-10T22:02:15Z","OA_type":"gold","oa":1,"PlanS_conform":"1"},{"article_type":"original","file_date_updated":"2026-07-13T07:46:22Z","publisher":"IOP Publishing","ddc":["520"],"article_number":"L37","oa":1,"date_created":"2026-07-12T22:02:17Z","OA_type":"gold","quality_controlled":"1","article_processing_charge":"Yes","volume":1005,"month":"07","abstract":[{"lang":"eng","text":"Recent studies at high redshift have revealed an enigmatic class of little red dots (LRDs) with extreme Balmer breaks, stronger than in any stellar atmosphere. However, it is unclear whether such objects exist at lower redshift, especially given the low number of LRDs reported at z ≲ 2. Here, we report the discovery of PAN-BH*-1, an LRD with an extreme Balmer break at z = 1.73, identified from JWST/NIRCam pure-parallel imaging taken by the PANORAMIC survey, and confirmed by deep VLT/X-Shooter spectroscopy. The rest-optical to near-infrared spectral energy distribution of PAN-BH*-1 is consistent with a photospheric continuum with effective temperature Teff ≈ 4800 K. The broad Hα emission line shows remarkably deep absorption, stronger than previously measured in any LRD. The absorption trough spans from −520 to +267 km s−1 with respect to the systemic redshift. The presence of blue- and red-shifted absorption suggests complex dynamics of the obscuring gas along the line of sight. We speculate that the absorption trough can be produced by a thick wind launched from a thick, rotating photospheric disk, the latter being the source of the red optical continuum. While the source is unresolved in the rest-optical JWST data (reff < 47 pc), the rest-near-UV Hubble Space Telescope imaging shows an extended morphology with (formular displayed) kpc, which we interpret as a host galaxy with a stellar mass of ∼10^8 M⊙, in line with the narrow Hα emission. The discovery of this object at cosmic noon highlights the feasibility of systematic searches for extreme LRDs with wide-area facilities such as Euclid and Roman."}],"status":"public","researchdata_availability":"yes","dataavailabilitystatement":"Based on observations made with ESO Telescopes at the Paranal Observatory under program IDs 116.294D and 116.2AQ0.\r\n\r\nThis 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 programs #2514 and #9433. C.C.W. gratefully acknowledges support for program JWST-GO-2514 provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. The authors acknowledge the team led by co-PIs R. Maiolino and F. D’Eugenio for developing their observing program with a zero-exclusive-access period.\r\n\r\nThis research is based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. These observations are associated with program #15117.\r\n\r\nThe JWST and HST data presented in this article were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via doi:10.17909/ydwx-st06.\r\n\r\nThis work is based in part on observations made with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The Spitzer data used in this work can be found in doi:10.26131/IRSA3.\r\n\r\nThis work was supported by the International Space Science Institute (ISSI) in Bern, through ISSI International Team project #25-659 “Little Red Dots, Big Open Questions.”\r\n\r\nJWST cartoon in Figure 6, credit: NASA.\r\n\r\nFacilities: VLT:Kueyen - Very Large Telescope (Kueyen) (X-Shooter), VLT:Yepun (HAWK-I), JWST - James Webb Space Telescope (NIRCam, NIRspec), HST - Hubble Space Telescope satellite (ACS), Spitzer - Spitzer Space Telescope satellite (IRAC, MIPS) - .\r\n\r\nSoftware: astropy (Astropy Collaboration et al. 2013, 2018; Astropy Collaboration et al. 2022), NumPy (C. R. Harris et al. 2020), SciPy (P. Virtanen et al. 2020), pysersic (I. Pasha & T. B. Miller 2023), stpsf (M. D. Perrin et al. 2014), lmfit (M. Newville et al. 2014), EsoRex (ESO CPL Development Team 2015), Claude (used for Python coding; https://claude.ai/), SEP (K. Barbary 2016).","publication":"The Astrophysical Journal Letters","DOAJ_listed":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"language":[{"iso":"eng"}],"acknowledgement":"IOP Science home\r\nThe Astrophysical Journal Letters\r\nThe American Astronomical Society, find out more.\r\n\r\nThe following article isOpen access\r\nA Black Hole Star at Cosmic Noon: Extreme Balmer Break, Photospheric Continuum, and Broad Absorption by Thick Winds in a Little Red Dot at z = 1.7\r\nAlberto Torralba, Jorryt Matthee, Andrea Weibel, Rohan P. Naidu, Yilun Ma, Aidan P. Cloonan, Aayush Desai, Anna de Graaff, Jenny E. Greene, Christian Kragh JespersenShow full author list\r\n\r\nPublished 2026 June 30 • © 2026. The Author(s). Published by the American Astronomical Society.\r\nThe Astrophysical Journal Letters, Volume 1005, Number 2\r\nCitation Alberto Torralba et al 2026 ApJL 1005 L37\r\nDOI 10.3847/2041-8213/ae7bfd\r\n\r\nPDFOpens in a new tab.ePub\r\nAuthors\r\nFigures\r\nTables\r\nReferences\r\nArticle data\r\nPDFOpens in a new tab.ePub\r\nArticle metrics\r\n122 Total downloads\r\n\r\nShare this article\r\nArticle information\r\nAbstract\r\nRecent studies at high redshift have revealed an enigmatic class of little red dots (LRDs) with extreme Balmer breaks, stronger than in any stellar atmosphere. However, it is unclear whether such objects exist at lower redshift, especially given the low number of LRDs reported at z ≲ 2. Here, we report the discovery of PAN-BH*-1, an LRD with an extreme Balmer break at z = 1.73, identified from JWST/NIRCam pure-parallel imaging taken by the PANORAMIC survey, and confirmed by deep VLT/X-Shooter spectroscopy. The rest-optical to near-infrared spectral energy distribution of PAN-BH*-1 is consistent with a photospheric continuum with effective temperature Teff ≈ 4800 K. The broad Hα emission line shows remarkably deep absorption, stronger than previously measured in any LRD. The absorption trough spans from −520 to +267 km s−1 with respect to the systemic redshift. The presence of blue- and red-shifted absorption suggests complex dynamics of the obscuring gas along the line of sight. We speculate that the absorption trough can be produced by a thick wind launched from a thick, rotating photospheric disk, the latter being the source of the red optical continuum. While the source is unresolved in the rest-optical JWST data (reff < 47 pc), the rest-near-UV Hubble Space Telescope imaging shows an extended morphology with \r\n kpc, which we interpret as a host galaxy with a stellar mass of ∼108 M⊙, in line with the narrow Hα emission. The discovery of this object at cosmic noon highlights the feasibility of systematic searches for extreme LRDs with wide-area facilities such as Euclid and Roman.\r\n\r\nExport citation and abstract\r\nBibTeXRIS\r\n\r\nPrevious article in issue\r\nNext article in issue\r\n\r\nOriginal content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.\r\n\r\n1. Introduction\r\nThe unprecedented sensitivity of JWST has enabled the discovery of a new, abundant population of objects at redshifts z ≈ 3–9 nicknamed the “little red dots” (LRDs). These are characterized by their compact rest-frame optical morphology, broad emission lines, and a characteristic rest-UV to optical “V-shape” in their spectral energy distributions (SED; e.g., D. D. Kocevski et al. 2023; V. Kokorev et al. 2024; J. Matthee et al. 2024; I. Labbe et al. 2025).\r\n\r\nThe nature of LRDs is highly debated (see K. Inayoshi & L. C. Ho 2025, for a recent overview) as the LRDs show systematic differences with respect to other types of active galactic nuclei (AGN), such as faintness in X-rays (e.g., T. T. Ananna et al. 2024; M. Yue et al. 2024), mid-to-far-infrared dust emission (e.g., G. C. K. Leung et al. 2025; C. C. Williams et al. 2024; I. Delvecchio et al. 2025; D. J. Setton et al. 2025; M. Xiao et al. 2025), and radio (e.g., G. Mazzolari et al. 2026; M. A. Latif et al. 2025; K. Perger et al. 2025, see A. J. Gloudemans et al. 2025).\r\n\r\nA recurring spectral feature of LRDs is the presence of a strong Balmer break (e.g., D. J. Setton et al. 2025; B. Wang et al. 2024; R. E. Hviding et al. 2025; W. Q. Sun et al. 2026), in some cases stronger than any star or stellar population can produce. The two most prominent examples known to date are The Cliff at z ≈ 3.5 (A. de Graaff et al. 2025a) and MoM-BH* at z ≈ 7.8 (R. P. Naidu et al. 2025). The joint appearance of strong Balmer lines as well as strong Balmer breaks has been modeled as being due to absorption by a dense, neutral gas with a high column density in the line of sight to a highly ionizing source (K. Inayoshi & R. Maiolino 2025; X. Ji et al. 2025; A. Sneppen et al. 2026; A. Torralba et al. 2026). These observations have sparked the development of new theoretical models, ranging from a spherical envelope analogous to stellar atmospheres (e.g., M. C. Begelman & J. Dexter 2026; D. Kido et al. 2025; H. Liu et al. 2025; D. Nandal & A. Loeb 2026) or a thick accretion disk (e.g., H. Liu et al. 2025, 2026; K. Inayoshi et al. 2025; Y.-X. Chen et al. 2026).\r\n\r\nBesides their spectral features, the evolution of the LRD number densities is also in stark contrast to other types of AGNs (e.g., K. Inayoshi 2025). At 4 ≲ z ≲ 7, LRDs represent a few percent of the galaxy population (e.g., D. D. Kocevski et al. 2023, 2025; J. E. Greene et al. 2024; V. Kokorev et al. 2024; X. Lin et al. 2024; R. Maiolino et al. 2024; J. Matthee et al. 2024), with number densities of ≳10−5 Mpc−3. The number density does not appear to drop quickly beyond z > 5 (e.g., J. Zhang et al. 2026), with various LRDs having been confirmed at z  >  8 (V. Kokorev et al. 2023; A. J. Taylor et al. 2025; R. Tripodi et al. 2025), well beyond the quasar redshift record (F. Wang et al. 2021). Photometric LRD candidates exist beyond z  >  10 (T. S. Tanaka et al. 2025). In turn, the number density of LRDs seems to decline steeply at z  <  4 (e.g., Y. Ma et al. 2026), with estimates of a number density of ∼10−6 cMpc−3 at z ∼ 2 and even ∼10−10 cMpc−3 at z ≈ 0.3 (X. Lin et al. 2026). While it is challenging to ensure a uniform selection function across such a large redshift baseline and dedicated spectroscopic follow-up of such lower redshift candidates has only just started, it is challenging to attribute five orders of magnitude to such effects.\r\n\r\nMotivated by the discovery of rare objects with extreme Balmer breaks at z  >  3 and the very small number of known LRDs at lower redshift, we performed a dedicated search for extreme Balmer break objects using a template-match approach on a large compilation of JWST NIRCam data over ≈0.3 deg2 and z ≈ 1.5–7.0. This survey is presented in A. Weibel et al. (2026a). As part of an ongoing ground-based spectroscopic campaign of LRD candidates at z ∼ 2 (Y. Ma et al. 2026), we followed up the most luminous candidate with a photometric redshift of z ≈ 2 with the X-Shooter spectrograph on the Very Large Telescope (VLT). In this Letter, we present the discovery and spectroscopic confirmation of PAN-BH*-1, a luminous LRD at z = 1.73 with an extreme Balmer break comparable to the strongest observed in any LRD (and, in general, any astrophysical source). The low redshift of this source enables high-resolution spectroscopy from ground-based observatories that is otherwise impossible to obtain at high redshift.\r\n\r\nThroughout this Letter, we use a ΛCDM cosmology with Ωm = 0.31, ΩΛ = 0.69, and h = 0.677 as described by Planck Collaboration et al. (2020). All the magnitudes are given in the AB system (J. B. Oke & J. E. Gunn 1983).\r\n\r\n2. Observations\r\n2.1. Photometry and Source Selection\r\nWe identified PAN-BH*-1 (ID: PAN-1115, RA, DEC: 40.015835, −1.659363 J2000) as part of a systematic search across ≈0.3 deg2 of JWST NIRCam legacy imaging comprising at least six filters of coverage (A. Weibel et al. 2026b). Notably, this dataset includes the Cycle 1 pure parallel survey PANORAMIC (PID: 2514, PIs: Williams & Oesch; C. C. Williams et al. 2025) that contributes 28 of the 35 independent lines of sight, thereby enabling the discovery of rare objects such as PAN-BH*-1 across diverse large-scale structure environments. Specifically, this source was identified in the footprint j024000m0142 of the PANORAMIC DR1,15 which is adjacent to the A370 field (G. O. Abell et al. 1989), where archival images by the Hubble Space Telescope (HST) are available from the BUFFALO survey (C. L. Steinhardt et al. 2020). The HST/ACS images were processed with grizli and also released as part of the PANORAMIC dataset.\r\n\r\nPAN-BH*-1 is in the outskirts of the A370 lensing cluster, but the magnification is only μ ≈ 1.05 according to the models from A. Niemiec et al. (2023). Throughout the rest of the paper, we report the uncorrected flux measurements, since the effect of magnification (∼5%) is negligible given the uncertainties in the observations and the lensing model.\r\n\r\nThe search strategy and full photometric selection are described in a companion paper (A. Weibel et al. 2026a). Briefly, that work presents a new selection of LRDs as a combination of a “black hole star” template (BH*; R. P. Naidu et al. 2025) embedded in a host galaxy, instead of the typically used “V-shaped” selections (e.g., D. D. Kocevski et al. 2025; V. Kokorev et al. 2024). The host galaxies are modeled using eazy’s blue_sfhz templates. The BH*s are modeled using a novel template set comprising empirical luminosity-based stacks constructed in W. Q. Sun et al. (2026), the cloudy template from R. P. Naidu et al. (2025), and by using spectra of prominent LRDs spanning the observed effective temperature range (I. Labbe et al. 2024; A. de Graaff et al. 2025a; B. Wang et al. 2026).\r\n\r\nPAN-BH*-1 stood out as one of the few sources where the BH* template effectively dominated all the light over the full wavelength range covered by NIRCam (hence the name). The redshift of PAN-BH*-1 was estimated to be zphot = 1.85. Follow-up VLT/X-Shooter spectroscopy confirmed the redshift as zspec = 1.731 (see Section 3.2).\r\n\r\nPAN-BH*-1 is also covered by archival data from the VLT with the HAWK-I camera in the Ks band (G. B. Brammer et al. 2016) and in data from the Spitzer Space Telescope in IRAC bands 1 and 3 (3.6 and 5.7 μm), and MIPS 24 μm (P. Capak 2019). PAN-BH*-1 is detected in the Ks band and in the two IRAC filters. Performing Spitzer photometry of this source is challenging due to the large point spread function (PSF) and a neighboring source, especially in the MIPS band. However, the NIRCam photometry of the neighboring source suggests it has a limited contribution to the IRAC fluxes. The details of the photometry extraction are described in Appendix A, and the measured magnitudes in Table 2.\r\n\r\n2.2. VLT/X-Shooter Spectroscopy\r\nPAN-BH*-1 was observed for 5.8 ks with the X-Shooter spectrograph (J. Vernet et al. 2011) on the VLT as a bright backup target for program 116.294D (PI: Matthee) in visitor mode on 2025 December 17. The main aim of this program was to confirm candidate LRDs at cosmic noon (Y. Ma et al. 2026). These observations confirmed the redshift through the detection of Hα at z = 1.731. A DDT program (ID 116.2AQ0; PI: Matthee) obtained additional follow-up data of PAN-BH*-1 in service mode for 26.2 ks during 2026 January 10–26, yielding a total exposure time of 8.9 hr. X-Shooter observes with three arms simultaneously, UVB, VIS, and near-infrared (NIR), covering rest-frame wavelengths of ≈0.14–0.9 μm, albeit hampered by skyline emission and telluric absorption, primarily in the rest-frame optical.\r\n\r\nThe observing conditions were clear, with a seeing ranging from 05 to 07 (median 06). The service mode observations were primarily conducted during dark nights, with some gray (FLI = 0.03–0.6, median 0.1), and a typical airmass of 1.35. We used UVB, VIS, and NIR slits with widths 10, 09, and 09, yielding a nominal resolution of R = 5400, 8900, and 5600, respectively (FWHM ∼53 km s−1 for NIR). The target acquisition was done using blind offsets from a reference star, due to the target being too faint for direct acquisition. We used a standard nodding on the slit pattern, with 4″ nod throws in an ABBA pattern, and 1″ jitters in the NIR arm to improve the sky subtraction. In each observing block of ≈1 hr, the exposure times were 700, 655, and (2×)365 s for the three arms at each nod position.\r\n\r\nThe reduction of the X-Shooter data uses a combination of EsoRex libraries16 and Python code based on the reduction pipeline employed in J. Matthee et al. (2021). Each observing block was reduced separately. We used standard stars taken during the observing night for a first-pass flux calibration. Telluric corrections were applied using the molecfit tool (A. Smette et al. 2015) implemented in the X-Shooter EsoRex pipeline. Telluric stars were observed during the visitor nights, but they were not always observed during the service mode observations in January. For those observations, we took the telluric star that was observed at the closest observing date. Based on the variation in telluric absorption among the reference stars taken during this period, we estimate the variation in the transmission and propagate the uncertainty in the telluric correction. For each observing block, we then extracted an optimally extracted 1D spectrum using the spatial profile of the Hα line, thus accounting for seeing variations and (more importantly) minor errors in the accuracy of the slit pointing. Before median combining these spectra, we normalize them by the median Hα flux of all observations to account for variations in slit losses and flux calibrations.\r\n\r\nBesides Hα (integrated S/N = 75) and Hβ (integrated S/N = 6; Section 3.2), we also detect continuum emission in the best regions in the H and K bands at 1.6 μm and 2.1 μm, respectively, with a low signal-to-noise ratio (S/N) of ∼1 per resolution element. Unfortunately, the [O iii] λλ4960, 5008 doublet is undetectable because the observed wavelengths are impacted by very strong telluric absorption. No other lines or continuum are detected in the X-Shooter spectrum.\r\n\r\n3. Properties of PAN-BH*-1\r\n3.1. Spectral Shape: A Photospheric Continuum with Strong Hα Emission\r\nThe photometric SED of PAN-BH*-1 has remarkable similarities with The Cliff (Figure 1): luminous in the rest optical, with a sudden drop toward the rest-UV around the Balmer limit, and very weak near-to-mid infrared continuum emission. With a rough extrapolation of the two HST photometric points using a power-law fit (fλ ∝ λβ), we obtain a UV slope of β = −0.1 ± 1.2, and MUV = −16.7 ± 0.7. For the rest-frame optical to NIR data, we fit a Planck blackbody law to the JWST data points, after subtracting the measured Hα flux (see Section 3.2) from the F200W photometry. The rest-optical and NIR photometry of PAN-BH*-1 is remarkably well described by a single temperature blackbody with T = 4204 K (with a best-fit ). We measure the strength of the Balmer break from the fν ratio F115W/F814W = 7 ± 1, in line with the Balmer break strengths of The Cliff (; A. de Graaff et al. 2025a)17 and MoM-BH* (7.8 ± 1.8; R. P. Naidu et al. 2025), measured from JWST/NIRSpec PRISM spectra as fν,4000–4100/fν,3620−3720. In Figure 2, we compare the Balmer break strength with the spectroscopic sample of A. de Graaff et al. (2025b), showing that out of 134 sources, only two have breaks significantly above 5. This suggests that PAN-BH*-1 has among the most extreme Balmer breaks known, although we caution that our value is derived from wide-band photometry with pivot wavelengths corresponding to 4212 and 3042 Å, respectively, rather than from spectroscopy.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 1. SED of PAN-BH*-1 Top: cutouts from all the HST and JWST images in which PAN-BH*-1 is covered. It shows a remarkably compact morphology in all the wavelengths, resolved only in the HST F606W and F814W bands (Section 3.3). Bottom: photometry from JWST/NIRCam (blue squares), HST/ACS (purple pentagons), and Spitzer/IRAC+MIPS (red hexagons, and red triangle for the 5σ upper limit). The empty square is the F200W flux after subtracting the Hα flux measured from X-Shooter spectroscopy. We show the spectrum of The Cliff for comparison (gray line), shifted to z = 1.73 and normalized to the F150W flux of PAN-BH*-1. We also show the best-fitting blackbody spectrum (blue dashed line) and the best model from the synthetic LRD atmosphere models from H. Liu et al. (2026), shifted to z = 1.73 (green line), undersampled by a factor of 500 for clarity.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nZoom InZoom OutReset image size\r\nFigure 2. Spectroscopic sample of LRDs by redshift and Balmer break strength. We plot the redshift and Balmer break strength of PAN-BH*-1, and the JWST sample from A. de Graaff et al. (2025b) (purple diamonds), and three local LRDs in X. Lin et al. (2026), for comparison. We also highlight three sources with a particularly strong Balmer break: The Cliff (A. de Graaff et al. 2025a), MoM-BH* (R. P. Naidu et al. 2025), and CAPERS-LRDz9 (A. J. Taylor et al. 2025). The Balmer break strength of the JWST spectroscopic sample is computed as fν,4000–4100/fν,3620–3720, whereas the value for PAN-BH*-1 is directly obtained from the F115W/F814W photometry.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\n3.2. Hα and Hβ Emission Lines\r\nThe Hα profile appears as a complex combination of a broad line with strong absorption close to the systemic redshift. We fit the Hα emission line with a similar model as the one used in A. Torralba et al. (2026) and J. Matthee et al. (2026). The Hα model consists of two Gaussian emission components (with narrow and intermediate line widths), and a broad symmetric exponential convolved with the intermediate profile and parameterized as in F. D’Eugenio et al. (2025a). The absorption is implemented as an opacity law defined as e−τ(λ), where τ(λ) also follows a single Gaussian velocity distribution (F. D’Eugenio et al. 2025a, 2025b; A. Torralba et al. 2026). For simplicity, we assume a covering factor of Cf = 1 for the absorbing gas. In previous works, the width of the narrow component is tied to that of [O iii], assuming both components come from the same region, often interpreted as the interstellar medium (ISM) of the host galaxy. In this case, we have no information about [O iii] due to this doublet falling in a wavelength range heavily affected by strong telluric absorption. We fit the Hα line after masking relevant skylines and strong telluric absorption bands. The fitted Hα parameters are listed in Table 1 and the best-fit model is shown in Figure 3. The absorption feature is notably strong, with an equivalent width of EWabs = −148 ± 12 Å with respect to the fitted continuum and 12.2 ± 0.2 Å if including the broad emission component. The absorption corresponds to a Balmer optical depth at the line center of , reaching roughly the continuum level. The FWHM of the single Gaussian fitted to the absorber is 283  ±  8 km s−1, and is offset from the systemic redshift by −94 ± 4 km s−1. We note that this parameterization is somewhat arbitrary, and we discuss in detail the absorber properties in Section 4.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 3. Hα spectrum, and the best fit to our fiducial model. We show the X-Shooter R ∼ 5600 spectrum of the Hα line of PAN-BH*-1, along with the best-fit to the model described in Section 3.2; total model (red solid line) and individual components (discontinuous color lines). The red wing of the line is severely affected by telluric absorption, thus the large uncertainties.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nTable 1. Properties of PAN-BH*-1\r\n\r\nParameter\tValue\tUnit\r\nWidth (FWHM; Hα)\r\nExponential\t1257 ± 27\tkm s−1\r\nIntermediate\t687 ± 43\tkm s−1\r\nNarrow\t184 ± 12\tkm s−1\r\nAbsorption\t283 ± 8\tkm s−1\r\nFlux (Hα)\r\nExponential\t643 ± 7\t10−18 erg s−1 cm−2\r\nIntermediate\t19 ± 5\t10−18 erg s−1 cm−2\r\nNarrow\t38 ± 3\t10−18 erg s−1 cm−2\r\nTotal\t522 ± 7\t10−18 erg s−1 cm−2\r\nGeneral properties\r\n(LHα/erg s−1)\t43.046 ± 0.006\t⋯\r\nEW0(Hα)\t520 ± 20\tÅ\r\nSFR(Hα, narrow)a\t2.1 ± 0.2\tM⊙ yr−1\r\nSFR(Hα, narrow)b\t3.3 ± 0.3\tM⊙ yr−1\r\nreff,UV (F606W+F814W)\t\tkpc\r\nreff,opt (F200W)\t<0.047\tkpc\r\nHα/Hβ (total)\t>9.4\t⋯\r\nHα/Hβ (narrow)\t5 ± 1\t⋯\r\nNotes. aCalibration from I. G. Kramarenko et al. (2026). bCalibration from R. C. Kennicutt & N. J. Evans (2012). SFR values calculated assuming no dust attenuation.\r\n\r\nDownload table as: \r\nASCIITypeset image\r\n\r\nThe Hβ line is marginally detected. After undersampling the spectrum by a factor 5, a hint of a weak narrow component can be identified (Figure 4), along with a tentative absorption at the same mean velocity as in Hα. We fit the best Hα model to the Hβ spectrum, only rescaling it by a multiplicative factor, and adding a flat continuum component. By doing this, we find an Hβ flux of (47 ± 8) × 10−18 erg s−1 cm−2 (S/N ≈ 6). Conservatively, we obtain a Balmer decrement of Hα/Hβ > 9.4 (at a 3σ confidence level), in line with the high decrements found for the LRD population (e.g., G. P. Nikopoulos et al. 2026; A. de Graaff et al. 2025b; J. Matthee et al. 2026). In Figure 5, we show the Hβ spectrum compared to the rescaled Hα model. By matching the best-fit Hα profile with the data at the expected observed wavelength for Hβ (±5000 km s−1), we obtain a better agreement (, BIC = 1537) than fitting a flat continuum only (, BIC = 1658) with ΔBIC = 121 ≫ 10, strongly favoring a detection of a broad Hβ emission line, and securing the spectroscopic redshift. Similarly, we fit a narrow Gaussian to Hβ with the same width and velocity as the Hα best-fit model, assuming a completely saturated absorption. We obtain a Balmer decrement for the narrow component of Hα/Hβ = 5 ± 1, which would imply a dust extinction of using a J. A. Cardelli et al. (1989) attenuation law, under the assumption of case B recombination. However, due to the low S/N of Hβ this result is only tentative, and compatible with a standard Case B value within ∼2σ.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 4. X-Shooter spectrum of Hα and Hβ of PAN-BH*-1 (blue). We compare to the spectrum of The Cliff (gray; data from JWST DDT #9433), normalized in each panel to the flux of PAN-BH*-1 in the range v ∈ (−3000, −2000) km s−1. Due to the low S/N, the Hβ spectrum of PAN-BH*-1 is rebinned to a coarser grid by a factor 5, after masking the most relevant skylines.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nZoom InZoom OutReset image size\r\nFigure 5. Hβ spectrum. The spectrum is rebinned by a factor of 10 with inverse variance flux weighting for visual clarity, due to the low S/N. We compare to the best-fit Hα model, scaled by a factor of 0.112. In the bottom panel, we show the χ residuals between the spectrum and the rescaled Hα model in black, and for only the continuum in pink (ΔBIC = 121 strongly favoring the presence of a broad Hβ line).\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\n3.3. Spatial Morphology\r\nIn order to assess whether PAN-BH*-1 is spatially resolved, we use the Bayesian profile fitting software pysersic (I. Pasha & T. B. Miller 2023)18 to fit a single Sérsic profile to the JWST and HST imaging data of PAN-BH*-1. For JWST/NIRCam, we choose F200W as the filter with the highest S/N in the short wavelength channel, benefiting from a high spatial resolution and probing rest-frame optical wavelengths. To model its PSF, we use version 2.2.0 of the stpsf software (formerly webbpsf, M. D. Perrin et al. 2014). For the two HST bands F606W and F814W, we instead construct empirical PSFs from public imaging data in the GOODS-S field following A. Weibel et al. (2024). In all three bands, we sample the posterior with the No U-turn sampler in two chains with 1000 warm-up and 2000 sampling steps each. We find that PAN-BH*-1 is unresolved with NIRCam in F200W where the effective radius converges toward the edge of the prior at 0.25 pixels. Using the 95th percentile of the posterior chains as an upper limit on the effective radius, we find a rest-optical size of reff < 47 pc.\r\n\r\nPAN-BH*-1 appears to be resolved in the HST images corresponding to rest-frame pivot 0.2 and 0.3 μm, respectively. Due to the low signal-to-noise of the F606W and F814W photometry, we fit both bands simultaneously fixing all the morphological parameters in both images. We measure physical effective radii of  kpc (see Appendix B). The modest stretching by the foreground A370 lensing cluster could imply a correction of ∼10% to the measured radius (A. Niemiec et al. 2023), which we disregard given the uncertainties. These measured sizes are consistent with the typical sizes for galaxies with a stellar mass ≲ 109 M⊙ at z = 1.75 (A. van der Wel et al. 2014). These findings are consistent with the scenario of a compact LRD “engine” dominating the rest-optical light embedded in a host galaxy, whose contribution becomes significant blueward of the Balmer break (see A. P. Cloonan et al. 2026, for a relevant discussion).\r\n\r\n4. Absorber Kinematics\r\nAs described in Section 3.2, the velocity distribution of the absorber is empirically modeled with a Gaussian, which we find has a central velocity of −94 ± 4 km s−1 relative to the redshift of the narrow emission component (adopted as systemic). The absorption trough extends from negative to positive velocities with respect to the redshift of the narrow component, but also with respect to the center of the symmetric exponential wings. However, there are several degeneracies between the shape of the absorber and other components of the emission line, such as the narrow central emission (see Section 3.2). Furthermore, direct interpretation of the absorber center velocity shift is challenging in an optically thick gas with presumably complex dynamics, and it does not necessarily trace bulk motion. A more robust, physically motivated pair of quantities is the minimum and maximum absorber velocities. We define them as the values where the transmission of the Balmer absorber increases to 99%,  km s−1 and  km s−1. These values trace the largest velocities in the line of sight of gas with significant Balmer absorption. The absorbing trough extends over 787 ± 17 km s−1 under this definition. The values of and are relatively agnostic to the choice of the shape of the absorber, since they are determined by the wavelength where the line profile deviates from a broad, symmetric exponential profile. In Figure 6, we illustrate three proposed configurations of the velocity distribution of the absorbing gas that could explain the shape of the observed Balmer absorption, and we discuss these scenarios below.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 6. Geometric configurations for the absorber. We illustrate three scenarios that could give rise to the observed Balmer absorption in PAN-BH*-1. In scenario (a), the obscuring agent is a thick screen of gas with a certain bulk velocity, and turbulent motions produce the broadening of the absorption trough. In (b), there are two (or more) absorbers with opposite velocities in the line of sight. These first two scenarios are dynamically unstable; therefore, variability is expected in the absorption. Lastly, in (c), we observed an extended source through a disk wind with a rotational component (vϕ) in addition to the poloidal (nonazimuthal) velocity (vp). In the last scenario, the redshifted absorption is produced by streamlines that oppose the observer when projected along the line of sight, despite the fact that the gas is outflowing from the central source.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\n4.1. Unstable Gas Flows?\r\nThe fact that there is significant absorption at both negative and positive velocities with respect to the systemic redshift cannot be simply explained by an axisymmetric outflowing or inflowing wind. In the case of observing a compact object through a spherically symmetric, nonturbulent bulk flow, a classical P Cygni profile is expected, with a purely blueshifted absorption (or redshifted if the wind is infalling). The fact that we also see redshifted absorption rules out this simple scenario. In principle, turbulent motions could also produce broadening of the absorbing medium (scenario a in Figure 6). However, the required turbulent velocity dispersion σturb ≈ 120 km s−1 (from the Gaussian fit in Section 3.2) is comparable to the mean velocity of the absorption trough, meaning that turbulence dominates the gas flow. In such a case, strong variability of the absorption profile would be expected, given the typical dynamical crossing times (see Sect. 4.1 in F. D’Eugenio et al. 2025b). For example, for a radius of 1016 cm (e.g., A. Torralba et al. 2026) and a mass of 106 M⊙, the dynamical freefall time is  yr. Moreover, the turbulent velocity would be highly supersonic, and the dissipation timescale would be comparable to the dynamical time (e.g., M.-M. Mac Low 1999). Alternatively, in the context of a strong Balmer absorber at z ∼ 7, F. D’Eugenio et al. (2026) recently discussed a “breathing mode” scenario with cyclic inflows and outflows along the same line of sight, with the gas being in different phases at different depths (scenario b in Figure 6; see also K. Park et al. 2017). In this case, the same arguments regarding the stability of the absorber would apply, and absorber variability is expected on observed timescales of ∼5 yr (for a source at z = 1.7), which is testable with future observations.\r\n\r\n4.2. The Case for the Disk Wind Hypothesis\r\nAn alternative, dynamically stable scenario is a disk wind configuration (scenario c in Figure 6). Here, the wind would be launched from a thick disk near the central engine, which we speculate could be the source of the optical continuum emission (e.g., H. Liu et al. 2025, 2026; L. Zwick et al. 2025; Y.-X. Chen et al. 2026). A rotating disk would imprint to the wind an azimuthal velocity component (vϕ). Observations at specific lines of sight, particularly for high inclination angles (close to edge-on) where the rotational component dominates the poloidal velocity, can give rise to both blueshifted and redshifted absorption features (D. Proga et al. 2000; P. B. Hall et al. 2002, 2013; D. Proga & T. R. Kallman 2004; M. Giustini & D. Proga 2012). Most observed LRDs have blueshifted P Cygni–like absorbers (J. Matthee et al. 2026), which can be naively interpreted as a uniformly expanding shell. The low incidence of redshifted Balmer absorbers in LRD spectra (e.g., I. Labbe et al. 2024; A. de Graaff et al. 2025a; F. D’Eugenio et al. 2025b, 2026; Y. Ma et al. 2026) can therefore be explained by the requirement of high inclination angles to observe such features (see also A. Sneppen et al. 2026). Such a picture is broadly in line with disk wind models for AGN with broad absorption lines (e.g., P. B. Hall et al. 2002; H. Zhou et al. 2019) and around stars with circumstellar disks (e.g., J. Erkal et al. 2022), such as accreting T Tauri stars (S. Edwards et al. 2006) or cataclysmic variables (D. Proga 2003).\r\n\r\n4.3. Implications of Rotating Winds for the Emission Lines of LRDs\r\nThe disk wind hypothesis would imply that a photosphere in the shape of a rotating disk is the source of the optical continuum emission, and drives winds that can explain the observed absorption trough. Emission lines originating in a thin rotating disk would have a double-peaked profile in the idealized case (for most inclination angles), but this is not necessarily true if the disk is not sufficiently thin (e.g., N. Murray & J. Chiang 1997), for instance, in the case of a puffed-up disk associated with super-Eddington accretion (e.g., H. Liu et al. 2026). In addition, most line emission would not be produced directly at the base of the disk, but slightly outside (e.g., via collisional cooling or residual recombination; A. Torralba et al. 2026), where the rotational velocity is lower, and the dynamics are complex (e.g., G. A. Shields 1977).\r\n\r\nThe Balmer lines of most LRDs are dominated by broad, symmetric exponential components that are associated with broadening by electron scattering (e.g., V. Rusakov et al. 2026; J. Matthee et al. 2026). For PAN-BH*-1, the Hα line profile of PAN-BH*-1 is compatible with a broad exponential profile emerging through a dense wind where the absorption trough is produced. In dense gas with a large column density of neutral hydrogen, and optically thick to Balmer transitions (NHI,2s ≳ 1014 cm−2), resonant scattering effects become important. Crucially, resonant scattering impacts Hα and Hβ differently (e.g., S.-J. Chang et al. 2026), hence the 3D radiative transfer and photon redistribution of both lines may produce different profiles (see, e.g., Figure 2 in D. Proga 2003). Therefore, the empirical fitting and interpretation of the absorption profiles becomes nontrivial. Dedicated radiative transfer modeling is necessary to study such effects, and they can be tested in other emission lines with high optical depth, such as He i λ10830 Å, or resonant lines like C iv λ1550.\r\n\r\n5. Implications for the Galaxy and Black Hole Masses\r\n5.1. Properties of the Host Galaxy\r\nAssuming that the narrow component of Hα corresponds to ISM emission in the host galaxy, we compute the associated star formation rate using the local calibration from R. C. Kennicutt & N. J. Evans (2012) and assuming no dust attenuation. We obtain SFR(Hα) = 3.3 ± 0.3 M⊙ yr−1. A somewhat lower value of SFR(Hα) = 2.1 ± 0.2 M⊙ yr−1 is obtained using the high-redshift (z ≳ 4) calibrations in I. G. Kramarenko et al. (2026), which might be more appropriate for a young dwarf galaxy with a bursty star formation history. The star formation rates are low, but in line with a main-sequence galaxy with (extrapolating the relation from J. S. Speagle et al. 2014). Assuming zero dust attenuation, the UV absolute magnitude (MUV = −16.7 ± 0.7; Section 3.1) would imply SFR(UV) = 0.18 ± 0.12 M⊙ yr−1 (R. C. Kennicutt & N. J. Evans 2012). The discrepancy between the UV and Hα inferred star formation rate suggests there is some amount of dust attenuation in the host galaxy.\r\n\r\nWe derive a dynamical mass from the width of the narrow component Hα line and the estimated UV size as , adopting the empirical virial correction K(n)K(q) from A. van der Wel et al. (2022), where K(n) and K(q) are functions of the best-fit ellipticity and Sérsic index (see Appendix B). Adopting a Mdyn/M* factor of 40 as found by A. de Graaff et al. (2024) for dwarf galaxies at high redshift, we infer a stellar mass of . However, the Mdyn/M* is very uncertain in this regime, and the uncertainty can span over 1 dex (A. Saldana-Lopez et al. 2025). We advise caution in interpreting this result, as there are large uncertainties in the measurements of the narrow Hα component, the HST morphology, and the empirical relations used.\r\n\r\nAs discussed in Section 4, the absorption profile is compatible with broadening by a rotating disk wind, and numerical modeling of such configurations often predicts a narrow component arising from increased transmission due to purely kinematic effects in the wind geometry (D. Proga et al. 2000; D. Proga 2003; D. Proga & T. R. Kallman 2004). This would be an alternative explanation for at least part of the narrow component flux. On the other hand, most LRDs present narrow [O iii] emission that is often associated with the host galaxy. Indeed, the ionized gas producing [O iii] emission should have associated emission in the Hα and higher-order Balmer lines. However, constraining this component largely depends on the assumptions on dust attenuation or ISM conditions, and requires very high S/N and resolution data. Deep, space-based follow-up observations of PAN-BH*-1 would be very constraining for the wind kinematics (e.g., by the joint analysis of Hβ) and to assess whether a narrow component comes from a host galaxy (e.g., by comparing to a narrow Hβ component or [O iii] λλ4960, 5008).\r\n\r\n5.2. Black Hole Mass From Photosphere Models\r\nThe general physical setup of LRDs is an open debate, and their masses are a major unknown. Due to the multiple differences with respect to the classical AGN population, the validity of standard virial calibrations has been questioned (e.g., V. Rusakov et al. 2026; J. E. Greene et al. 2026; A. Sneppen et al. 2026; A. Torralba et al. 2026, although see, e.g., M. Brazzini et al. 2025, 2026; J. Scholtz et al. 2026 for an alternative interpretation).\r\n\r\nOne can obtain a mass estimate assuming a system in radiative equilibrium with Lbol/LEdd = 1 (e.g., H. Umeda et al. 2026); this yields a total mass of ≈106 M⊙, using the bolometric luminosity from integrating the best-fit blackbody in Section 3.1. Recently, H. Liu et al. (2026) developed a synthetic spectral library of LRD atmosphere models. In these models, the density of the photosphere is regulated by the net surface gravity of an optically thick atmosphere, enabling constraints on the mass of the system. We fit the JWST photometry of PAN-BH*-1 using the models from H. Liu et al. (2026), assuming a negligible contribution from a host galaxy to the optical continuum. The best-fit model has effective temperature Teff = 4800 K, surface gravity , and metallicity (; see Figure 1). The best-fit implies a total mass of the system (BH plus gas) of (Equation (6) in H. Liu et al. 2026, assuming hydrostatic equilibrium). For the second and third best fits, we obtain and −2, respectively (, respectively; with the same metallicity and effective temperature), which would imply lower limits to the system mass between and 4. The bolometric luminosity of PAN-BH*-1 (from the integral of the best-fit green curve in Figure 1) implies an Eddington luminosity ratio of L/LEdd ≲ 13, assuming the best-fit mass from the H. Liu et al. (2026) models. The elevated Eddington ratio is in line with the hypothesis of a radiation-driven wind discussed in Section 4, and allows for somewhat larger system masses. The low masses obtained with this model, combined with the stellar mass inferred from dynamical arguments for the host galaxy (Section 3.3) set lower limits to the BH-to-stellar mass ratio of MBH/M* ≳ 10−4–10−2, which are compatible with the relations observed in the Local Universe, within the large uncertainties (A. E. Reines & M. Volonteri 2015).\r\n\r\n6. Conclusions\r\nIn this Letter, we presented the discovery and spectroscopic confirmation of PAN-BH*-1, an LRD with an extreme Balmer break at z = 1.731. The strength of the Balmer break (F115W/F814W = 7 ± 1) is comparable to the most extreme LRDs known, The Cliff (A. de Graaff et al. 2025a) and MoM-BH* (R. P. Naidu et al. 2025). We summarize the observations and our main conclusions as follows.\r\n\r\n\r\n1.  \r\nWe obtained deep VLT/X-Shooter spectroscopy of PAN-BH*-1. The Hα emission line is luminous and broad (LHα = 1043 erg s−1), and has an unusually strong absorption. Hβ is detected with an S/N ≈ 6, and we conservatively estimate a lower limit for the Balmer decrement of Hα/Hβ > 9.4 (at a 3σ confidence level), in line with other LRDs in the literature (e.g., A. de Graaff et al. 2025b; G. P. Nikopoulos et al. 2026).\r\n2.  \r\nThe absorption trough spans from −520 to 267 km s−1 (at a transmission level of 99%). We interpret the presence of blue- and redshifted absorption as produced by a disk wind, analogous to those analyzed in the context of broad absorption line quasars or accreting stars. This hypothesis would imply that the source of the optical continuum is likely a thick photospheric disk.\r\n3.  \r\nWe detect a narrow Hα component (FWHM = 184 ± 12 km s−1), which we interpret as probing a host galaxy with M* ≈ 108 M⊙ and SFR = 2–3 M⊙. This interpretation is in line with the extended rest-NUV morphology measured in the HST bands (\r\n kpc).\r\n4.  \r\nBy fitting the synthetic atmosphere models of H. Liu et al. (2026), we estimate a system mass (BH+envelope) of 104–106 M⊙. The inferred masses, together with the stellar mass inferred from morphology and narrow emission line dynamics, imply BH-to-stellar mass ratios of 10−2–10−4, close to the extrapolated trend in the local Universe (A. E. Reines & M. Volonteri 2015).\r\n5.  \r\nThe confirmation of this source at cosmic noon (magnitude of ≈22 in the K band, Hα flux ≈5 × 10−16 erg s−1 cm−2) proves the feasibility of detecting extreme LRDs at such epochs with wide-area spectroscopic surveys like Euclid or the forthcoming Nancy Grace Roman Space Telescope.\r\n\r\nAcknowledgments\r\nA.T. thanks Debasish Dutta and Tamara Bogdanović for useful conversations about stellar and AGN winds.\r\n\r\nWe thank the scientific referee for the useful and constructive feedback, which helped improve the quality of this paper.\r\n\r\nJ.M. and A.T. acknowledge funding by the European Union (ERC, AGENTS, 101076224). The work of CCW is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. A.P.C. warmly acknowledges the support of the National Science Foundation through the NSF Graduate Research Fellowship Program. A.d.G. acknowledges support from a Clay Fellowship awarded by the Smithsonian Astrophysical Observatory.\r\n\r\nBased on observations made with ESO Telescopes at the Paranal Observatory under program IDs 116.294D and 116.2AQ0.\r\n\r\nThis 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 programs #2514 and #9433. C.C.W. gratefully acknowledges support for program JWST-GO-2514 provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. The authors acknowledge the team led by co-PIs R. Maiolino and F. D’Eugenio for developing their observing program with a zero-exclusive-access period.\r\n\r\nThis research is based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. These observations are associated with program #15117.\r\n\r\nThe JWST and HST data presented in this article were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via doi:10.17909/ydwx-st06.\r\n\r\nThis work is based in part on observations made with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The Spitzer data used in this work can be found in doi:10.26131/IRSA3.\r\n\r\nThis work was supported by the International Space Science Institute (ISSI) in Bern, through ISSI International Team project #25-659 “Little Red Dots, Big Open Questions.”\r\n\r\nJWST cartoon in Figure 6, credit: NASA.\r\n\r\nFacilities: VLT:Kueyen - Very Large Telescope (Kueyen) (X-Shooter), VLT:Yepun (HAWK-I), JWST - James Webb Space Telescope (NIRCam, NIRspec), HST - Hubble Space Telescope satellite (ACS), Spitzer - Spitzer Space Telescope satellite (IRAC, MIPS) - .\r\n\r\nSoftware: astropy (Astropy Collaboration et al. 2013, 2018; Astropy Collaboration et al. 2022), NumPy (C. R. Harris et al. 2020), SciPy (P. Virtanen et al. 2020), pysersic (I. Pasha & T. B. Miller 2023), stpsf (M. D. Perrin et al. 2014), lmfit (M. Newville et al. 2014), EsoRex (ESO CPL Development Team 2015), Claude (used for Python coding; https://claude.ai/), SEP (K. Barbary 2016).","issue":"2","has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","supplementarymaterial":"yes","year":"2026","day":"10","doi":"10.3847/2041-8213/ae7bfd","date_updated":"2026-07-13T08:08:41Z","date_published":"2026-07-10T00:00:00Z","file":[{"relation":"main_file","date_updated":"2026-07-13T07:46:22Z","file_name":"2026_AstrophysicalJourLetters_Torralba.pdf","checksum":"7600db260d799ddea45cf3bd01effe41","content_type":"application/pdf","file_size":5419071,"access_level":"open_access","creator":"dernst","date_created":"2026-07-13T07:46:22Z","success":1,"file_id":"22274"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"external_id":{"arxiv":["2603.28335"]},"arxiv":1,"title":"A black hole star at cosmic noon: Extreme Balmer break, photospheric continuum, and broad absorption by thick winds in a Little Red Dot at z = 1.7","author":[{"id":"018f0249-0e87-11f0-b167-cbce08fbd541","last_name":"Torralba Torregrosa","first_name":"Alberto","full_name":"Torralba Torregrosa, Alberto","orcid":"0000-0001-5586-6950"},{"first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"last_name":"Weibel","first_name":"Andrea","full_name":"Weibel, Andrea"},{"last_name":"Naidu","first_name":"Rohan P.","full_name":"Naidu, Rohan P."},{"first_name":"Yilun","last_name":"Ma","full_name":"Ma, Yilun"},{"last_name":"Cloonan","first_name":"Aidan P.","full_name":"Cloonan, Aidan P."},{"first_name":"Aayush A","id":"502cfd30-32c1-11ee-a9a4-d8dad5c6739e","last_name":"Desai","full_name":"Desai, Aayush A"},{"full_name":"De Graaff, Anna","last_name":"De Graaff","first_name":"Anna"},{"first_name":"Jenny E.","last_name":"Greene","full_name":"Greene, Jenny E."},{"full_name":"Jespersen, Christian Kragh","last_name":"Jespersen","first_name":"Christian Kragh"},{"orcid":"0000-0001-5346-6048","full_name":"Kramarenko, Ivan","first_name":"Ivan","last_name":"Kramarenko","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4"},{"id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","last_name":"Mascia","first_name":"Sara","full_name":"Mascia, Sara"},{"full_name":"Oesch, Pascal A.","last_name":"Oesch","first_name":"Pascal A."},{"full_name":"Sun, Wendy Q.","last_name":"Sun","first_name":"Wendy Q."},{"first_name":"Christina C.","last_name":"Williams","full_name":"Williams, Christina C."}],"citation":{"ista":"Torralba Torregrosa A, Matthee JJ, Weibel A, Naidu RP, Ma Y, Cloonan AP, Desai AA, De Graaff A, Greene JE, Jespersen CK, Kramarenko I, Mascia S, Oesch PA, Sun WQ, Williams CC. 2026. A black hole star at cosmic noon: Extreme Balmer break, photospheric continuum, and broad absorption by thick winds in a Little Red Dot at z = 1.7. The Astrophysical Journal Letters. 1005(2), L37.","short":"A. Torralba Torregrosa, J.J. Matthee, A. Weibel, R.P. Naidu, Y. Ma, A.P. Cloonan, A.A. Desai, A. De Graaff, J.E. Greene, C.K. Jespersen, I. Kramarenko, S. Mascia, P.A. Oesch, W.Q. Sun, C.C. Williams, The Astrophysical Journal Letters 1005 (2026).","chicago":"Torralba Torregrosa, Alberto, Jorryt J Matthee, Andrea Weibel, Rohan P. Naidu, Yilun Ma, Aidan P. Cloonan, Aayush A Desai, et al. “A Black Hole Star at Cosmic Noon: Extreme Balmer Break, Photospheric Continuum, and Broad Absorption by Thick Winds in a Little Red Dot at z = 1.7.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/2041-8213/ae7bfd\">https://doi.org/10.3847/2041-8213/ae7bfd</a>.","mla":"Torralba Torregrosa, Alberto, et al. “A Black Hole Star at Cosmic Noon: Extreme Balmer Break, Photospheric Continuum, and Broad Absorption by Thick Winds in a Little Red Dot at z = 1.7.” <i>The Astrophysical Journal Letters</i>, vol. 1005, no. 2, L37, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/2041-8213/ae7bfd\">10.3847/2041-8213/ae7bfd</a>.","ieee":"A. Torralba Torregrosa <i>et al.</i>, “A black hole star at cosmic noon: Extreme Balmer break, photospheric continuum, and broad absorption by thick winds in a Little Red Dot at z = 1.7,” <i>The Astrophysical Journal Letters</i>, vol. 1005, no. 2. IOP Publishing, 2026.","apa":"Torralba Torregrosa, A., Matthee, J. J., Weibel, A., Naidu, R. P., Ma, Y., Cloonan, A. P., … Williams, C. C. (2026). A black hole star at cosmic noon: Extreme Balmer break, photospheric continuum, and broad absorption by thick winds in a Little Red Dot at z = 1.7. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ae7bfd\">https://doi.org/10.3847/2041-8213/ae7bfd</a>","ama":"Torralba Torregrosa A, Matthee JJ, Weibel A, et al. A black hole star at cosmic noon: Extreme Balmer break, photospheric continuum, and broad absorption by thick winds in a Little Red Dot at z = 1.7. <i>The Astrophysical Journal Letters</i>. 2026;1005(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/ae7bfd\">10.3847/2041-8213/ae7bfd</a>"},"publication_status":"published","corr_author":"1","OA_place":"publisher","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224"}],"oa_version":"Published Version","type":"journal_article","department":[{"_id":"JoMa"},{"_id":"IlCa"},{"_id":"GradSch"}],"intvolume":"      1005","das_tickbox":"1","_id":"22263"},{"has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","language":[{"iso":"eng"}],"acknowledgement":"Support for this work was provided by The Brinson Foundation through a Brinson Prize Fellowship grant. D.S. acknowledges Zhengrong Li for kindly sharing model dust SEDs, Tim Rawle for helping with accessing archival Herschel Lensing Survey data, and Xiaohui Fan for helpful conversations that steered the direction of this work. This Letter makes use of the following ALMA data: ADS/JAO.ALMA#2024.00826.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. 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 (DOI: 10.17909/m7ks-wg55), 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 #6761.\r\n\r\nSupport for this work was provided by NSF/AAG #2306950. Support for this work for R.P.N. was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. The Cosmic Dawn Center is funded by the Danish National Research Foundation under grant DNRF140. A.Z. acknowledges support by grant No. 2020750 from the United States–Israel Binational Science Foundation (BSF) and grant No. 2109066 from the United States National Science Foundation (NSF) and by the Israel Science Foundation grant No. 864/23. The work of C.C.W. is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. S.A. acknowledges support from the JWST Mid-Infrared Instrument (MIRI) Science Team Lead, grant 80NSSC18K0555, from NASA Goddard Space Flight Center to the University of Arizona.","date_updated":"2026-02-09T07:14:08Z","date_published":"2025-09-12T00:00:00Z","external_id":{"arxiv":["2503.02059"]},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file":[{"access_level":"open_access","date_created":"2026-02-09T07:10:29Z","creator":"dernst","success":1,"file_id":"21165","relation":"main_file","date_updated":"2026-02-09T07:10:29Z","content_type":"application/pdf","file_name":"2025_AstrophysicalJournalLetters_Setton.pdf","checksum":"799518db92ded4e166df4234195af998","file_size":1394204}],"day":"12","year":"2025","doi":"10.3847/2041-8213/ade78b","title":"A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots","publication_status":"published","citation":{"ieee":"D. J. Setton <i>et al.</i>, “A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots,” <i>The Astrophysical Journal Letters</i>, vol. 991. IOP Publishing, 2025.","apa":"Setton, D. J., Greene, J. E., Spilker, J. S., Williams, C. C., Labbé, I., Ma, Y. 逸伦, … Zitrin, A. (2025). A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ade78b\">https://doi.org/10.3847/2041-8213/ade78b</a>","ama":"Setton DJ, Greene JE, Spilker JS, et al. A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots. <i>The Astrophysical Journal Letters</i>. 2025;991. doi:<a href=\"https://doi.org/10.3847/2041-8213/ade78b\">10.3847/2041-8213/ade78b</a>","ista":"Setton DJ, Greene JE, Spilker JS, Williams CC, Labbé I, Ma Y逸伦, Wang B冰洁, Whitaker KE, Leja J, de Graaff A, Alberts S, Bezanson R, Boogaard LA, Brammer G, Cutler SE, Cleri NJ, Cooper OR, Dayal P, Fujimoto S, Furtak LJ, Goulding AD, Hirschmann M, Kokorev V, Maseda MV, McConachie I, Matthee JJ, Miller TB, Naidu RP, Oesch PA, Pan R, Price SH, Suess KA, Weaver JR, Xiao M, Zhang Y, Zitrin A. 2025. A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots. The Astrophysical Journal Letters. 991, L10.","short":"D.J. Setton, J.E. Greene, J.S. Spilker, C.C. Williams, I. Labbé, Y.逸伦 Ma, B.冰洁 Wang, K.E. Whitaker, J. Leja, A. de Graaff, S. Alberts, R. Bezanson, L.A. Boogaard, G. Brammer, S.E. Cutler, N.J. Cleri, O.R. Cooper, P. Dayal, S. Fujimoto, L.J. Furtak, A.D. Goulding, M. Hirschmann, V. Kokorev, M.V. Maseda, I. McConachie, J.J. Matthee, T.B. Miller, R.P. Naidu, P.A. Oesch, R. Pan, S.H. Price, K.A. Suess, J.R. Weaver, M. Xiao, Y. Zhang, A. Zitrin, The Astrophysical Journal Letters 991 (2025).","chicago":"Setton, David J., Jenny E. Greene, Justin S. Spilker, Christina C. Williams, Ivo Labbé, Yilun 逸伦 Ma, Bingjie 冰洁 Wang, et al. “A Confirmed Deficit of Hot and Cold Dust Emission in the Most Luminous Little Red Dots.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/2041-8213/ade78b\">https://doi.org/10.3847/2041-8213/ade78b</a>.","mla":"Setton, David J., et al. “A Confirmed Deficit of Hot and Cold Dust Emission in the Most Luminous Little Red Dots.” <i>The Astrophysical Journal Letters</i>, vol. 991, L10, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/2041-8213/ade78b\">10.3847/2041-8213/ade78b</a>."},"author":[{"first_name":"David J.","last_name":"Setton","full_name":"Setton, David J."},{"full_name":"Greene, Jenny E.","first_name":"Jenny E.","last_name":"Greene"},{"full_name":"Spilker, Justin S.","last_name":"Spilker","first_name":"Justin S."},{"full_name":"Williams, Christina C.","first_name":"Christina C.","last_name":"Williams"},{"full_name":"Labbé, Ivo","first_name":"Ivo","last_name":"Labbé"},{"first_name":"Yilun 逸伦","last_name":"Ma","full_name":"Ma, Yilun 逸伦"},{"full_name":"Wang, Bingjie 冰洁","last_name":"Wang","first_name":"Bingjie 冰洁"},{"full_name":"Whitaker, Katherine E.","first_name":"Katherine E.","last_name":"Whitaker"},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"first_name":"Anna","last_name":"de Graaff","full_name":"de Graaff, Anna"},{"full_name":"Alberts, Stacey","last_name":"Alberts","first_name":"Stacey"},{"last_name":"Bezanson","first_name":"Rachel","full_name":"Bezanson, Rachel"},{"full_name":"Boogaard, Leindert A.","last_name":"Boogaard","first_name":"Leindert A."},{"first_name":"Gabriel","last_name":"Brammer","full_name":"Brammer, Gabriel"},{"full_name":"Cutler, Sam E.","first_name":"Sam E.","last_name":"Cutler"},{"full_name":"Cleri, Nikko J.","first_name":"Nikko J.","last_name":"Cleri"},{"full_name":"Cooper, Olivia R.","last_name":"Cooper","first_name":"Olivia R."},{"first_name":"Pratika","last_name":"Dayal","full_name":"Dayal, Pratika"},{"last_name":"Fujimoto","first_name":"Seiji","full_name":"Fujimoto, Seiji"},{"full_name":"Furtak, Lukas J.","last_name":"Furtak","first_name":"Lukas J."},{"first_name":"Andy D.","last_name":"Goulding","full_name":"Goulding, Andy D."},{"last_name":"Hirschmann","first_name":"Michaela","full_name":"Hirschmann, Michaela"},{"full_name":"Kokorev, Vasily","last_name":"Kokorev","first_name":"Vasily"},{"last_name":"Maseda","first_name":"Michael V.","full_name":"Maseda, Michael V."},{"full_name":"McConachie, Ian","first_name":"Ian","last_name":"McConachie"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"full_name":"Miller, Tim B.","last_name":"Miller","first_name":"Tim B."},{"last_name":"Naidu","first_name":"Rohan P.","full_name":"Naidu, Rohan P."},{"full_name":"Oesch, Pascal A.","first_name":"Pascal A.","last_name":"Oesch"},{"full_name":"Pan, Richard","last_name":"Pan","first_name":"Richard"},{"full_name":"Price, Sedona H.","first_name":"Sedona H.","last_name":"Price"},{"last_name":"Suess","first_name":"Katherine A.","full_name":"Suess, Katherine A."},{"full_name":"Weaver, John R.","last_name":"Weaver","first_name":"John R."},{"full_name":"Xiao, Mengyuan","first_name":"Mengyuan","last_name":"Xiao"},{"full_name":"Zhang, Yunchong","last_name":"Zhang","first_name":"Yunchong"},{"first_name":"Adi","last_name":"Zitrin","full_name":"Zitrin, Adi"}],"OA_place":"publisher","arxiv":1,"department":[{"_id":"JoMa"}],"intvolume":"       991","_id":"21058","oa_version":"Published Version","type":"journal_article","oa":1,"date_created":"2026-01-28T15:23:00Z","PlanS_conform":"1","OA_type":"gold","quality_controlled":"1","article_processing_charge":"Yes","volume":991,"article_type":"original","file_date_updated":"2026-02-09T07:10:29Z","publisher":"IOP Publishing","article_number":"L10","ddc":["520"],"month":"09","abstract":[{"lang":"eng","text":"Luminous broad Hα emission and red rest-optical spectral energy distributions (SEDs) are the hallmark of compact little red dots (LRDs), implying highly attenuated dusty starbursts and/or obscured active galactic nuclei (AGN). However, the lack of observed far-infrared (FIR) emission has proved difficult to reconcile with the implied attenuated luminosity in these models. Here, we utilize deep new Atacama Large Millimeter/submillimeter Array imaging, new and existing JWST/MIRI imaging, and archival Spitzer/Herschel imaging of two of the rest-optically brightest LRDs (z = 3.1 and z = 4.47) to place the strongest constraints on the IR luminosity in LRDs to date. The detections at λrest = 1–4 μm imply flat slopes in the rest-IR, ruling out a contribution from hot (T ≳ 500 K) dust. Similarly, FIR nondetections rule out any appreciable cold (T ≲ 75 K) dust component. Assuming energy balance, these observations are inconsistent with the typical FIR dust emission of dusty starbursts and quasar tori, which usually show a mixture of cold and hot dust. Additionally, our [C ii] nondetections rule out typical dusty starbursts. We compute empirical maximum IR SEDs and find that both LRDs must have log(LIR/L ) 12.2 at the 3σ level. These limits are in tension with the predictions of rest-optical spectrophotometric fits, be they galaxy-only, AGN-only, or composite. It is unlikely that LRDs are highly dust-reddened intrinsically blue sources with a dust temperature distribution that conspires to avoid current observing facilities. Rather, we favor an intrinsically redder LRD SED model that alleviates the need for strong dust attenuation."}],"status":"public","DOAJ_listed":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"publication":"The Astrophysical Journal Letters"},{"ddc":["520"],"article_number":"L67","file_date_updated":"2026-02-10T06:56:37Z","article_type":"original","publisher":"IOP Publishing","volume":995,"article_processing_charge":"Yes","oa":1,"PlanS_conform":"1","OA_type":"gold","date_created":"2026-01-31T09:27:53Z","quality_controlled":"1","abstract":[{"lang":"eng","text":"The relation between the masses of supermassive black holes (SMBHs) and their host galaxies encodes information on their mode of growth, especially at the earliest epochs. The James Webb Space Telescope (JWST) has opened such investigations by detecting the host galaxies of active galactic nuclei (AGN) and more luminous quasars within the first billion years of the Universe (z ≳ 6). Here, we evaluate the relation between the mass of SMBHs and the total stellar mass of their host galaxies using a sample of nine quasars at 6.18 ≤ z ≤ 6.4 from the Subaru High-z Exploration of Low-luminosity Quasars survey with NIRCam and NIRSpec observations. We find that the observed location of these quasars in the SMBH–galaxy mass plane (logMBH/M 8–9; logM*/M 9.5–11) is consistent with a nonevolving intrinsic mass relation with dispersion (0.80 +0.23 -0.28 dex) higher than the local value (∼0.3–0.4 dex) of their more massive descendants. Our analysis is based on a forward model of systematics and includes a consideration of the impact of selection effects and measurement uncertainties with an assumption on the slope of the mass relation. While degeneracies between parameters persist, the best-fit solution has a reasonable AGN fraction (2.3%) of galaxies at z ∼ 6 with an actively growing UV-unobscured black hole. In particular, models with a substantially higher normalisation in MBH would require an unrealistically low intrinsic dispersion (∼0.22 dex). Consequently, our results predict a large population of AGN at lower black hole masses, as are now just starting to be discovered in focused efforts with JWST."}],"status":"public","month":"12","publication":"The Astrophysical Journal Letters","DOAJ_listed":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"issue":"2","language":[{"iso":"eng"}],"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 GO #1967 and GO #3859. The specific observations analyzed can be accessed via DOI: 10.17909/719q-cn32. Support for these programs was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. This work was supported by World Premier International Research Center Initiative (WPI), MEXT, Japan. This work used computing resources at Kavli IPMU. J.S. is supported by JSPS KAKENHI (JP22H01262). M.O. is supported by the Japan Society for the Promotion of Science (JSPS) KAKENHI grant No. 24K22894. Y.M. was supported by the Japan Society for the Promotion of Science (JSPS) KAKENHI grant No. 21H04494. M.V. gratefully acknowledges financial support from the Independent Research Fund Denmark via grant numbers DFF 8021-00130 and 3103-00146 and from the Carlsberg Foundation via grant CF23-0417. S.E.I.B. is supported by the Deutsche Forschungsgemeinschaft (DFG) under Emmy Noether grant number BO 5771/1-1. K.I. acknowledges support from the National Natural Science Foundation of China (12073003, 11721303, 11991052). K.I. acknowledges support under the grant PID2022-136827NB-C44 provided by MCIN/AEI/10.13039/501100011033 / FEDER, UE. A.L. acknowledges support from PRIN MUR 2022— Project “2022935STW.” J.T.S. is supported by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)—project number 518006966. F.W. acknowledges support from NSF award AST-2513040. M.H. acknowledges support from the FNS under the SNSF starting grant 218032. B.T. acknowledges support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement number 950533) and from the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy—EXC 2094—390783311.","has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","doi":"10.3847/2041-8213/ae279c","year":"2025","day":"17","file":[{"file_id":"21202","success":1,"creator":"dernst","date_created":"2026-02-10T06:56:37Z","access_level":"open_access","file_size":997137,"file_name":"2025_AstrophysicalJounalLetters_Silvermann.pdf","checksum":"e38c0c444be9c1507eec28c62ce04cbc","content_type":"application/pdf","date_updated":"2026-02-10T06:56:37Z","relation":"main_file"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"external_id":{"arxiv":["2507.23066"]},"date_published":"2025-12-17T00:00:00Z","date_updated":"2026-02-10T07:02:39Z","arxiv":1,"author":[{"first_name":"John David","last_name":"Silverman","full_name":"Silverman, John David"},{"first_name":"Junyao","last_name":"Li","full_name":"Li, Junyao"},{"full_name":"Ding, Xuheng","last_name":"Ding","first_name":"Xuheng"},{"last_name":"Onoue","first_name":"Masafusa","full_name":"Onoue, Masafusa"},{"full_name":"Strauss, Michael A.","first_name":"Michael A.","last_name":"Strauss"},{"full_name":"Matsuoka, Yoshiki","last_name":"Matsuoka","first_name":"Yoshiki"},{"full_name":"Izumi, Takuma","last_name":"Izumi","first_name":"Takuma"},{"full_name":"Jahnke, Knud","last_name":"Jahnke","first_name":"Knud"},{"full_name":"Treu, Tommaso","last_name":"Treu","first_name":"Tommaso"},{"last_name":"Volonteri","first_name":"Marta","full_name":"Volonteri, Marta"},{"first_name":"Camryn L.","last_name":"Phillips","full_name":"Phillips, Camryn L."},{"first_name":"Irham T.","last_name":"Andika","full_name":"Andika, Irham T."},{"full_name":"Aoki, Kentaro","last_name":"Aoki","first_name":"Kentaro"},{"first_name":"Junya","last_name":"Arita","full_name":"Arita, Junya"},{"last_name":"Baba","first_name":"Shunsuke","full_name":"Baba, Shunsuke"},{"full_name":"Bosman, Sarah E. I.","last_name":"Bosman","first_name":"Sarah E. I."},{"full_name":"Eilers, Anna-Christina","first_name":"Anna-Christina","last_name":"Eilers"},{"full_name":"Fan, Xiaohui","first_name":"Xiaohui","last_name":"Fan"},{"full_name":"Fujimoto, Seiji","first_name":"Seiji","last_name":"Fujimoto"},{"first_name":"Melanie","last_name":"Habouzit","full_name":"Habouzit, Melanie"},{"full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403","first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"full_name":"Imanishi, Masatoshi","first_name":"Masatoshi","last_name":"Imanishi"},{"full_name":"Inayoshi, Kohei","first_name":"Kohei","last_name":"Inayoshi"},{"full_name":"Iwasawa, Kazushi","first_name":"Kazushi","last_name":"Iwasawa"},{"last_name":"Kashikawa","first_name":"Nobunari","full_name":"Kashikawa, Nobunari"},{"last_name":"Kawaguchi","first_name":"Toshihiro","full_name":"Kawaguchi, Toshihiro"},{"last_name":"Lee","first_name":"Chien-Hsiu","full_name":"Lee, Chien-Hsiu"},{"full_name":"Lupi, Alessandro","last_name":"Lupi","first_name":"Alessandro"},{"full_name":"Nagao, Tohru","first_name":"Tohru","last_name":"Nagao"},{"last_name":"Schindler","first_name":"Jan-Torge","full_name":"Schindler, Jan-Torge"},{"full_name":"Schramm, Malte","last_name":"Schramm","first_name":"Malte"},{"first_name":"Kazuhiro","last_name":"Shimasaku","full_name":"Shimasaku, Kazuhiro"},{"first_name":"Yoshiki","last_name":"Toba","full_name":"Toba, Yoshiki"},{"full_name":"Trakhtenbrot, Benny","first_name":"Benny","last_name":"Trakhtenbrot"},{"first_name":"Hideki","last_name":"Umehata","full_name":"Umehata, Hideki"},{"full_name":"Vestergaard, Marianne","last_name":"Vestergaard","first_name":"Marianne"},{"full_name":"Walter, Fabian","first_name":"Fabian","last_name":"Walter"},{"last_name":"Wang","first_name":"Feige","full_name":"Wang, Feige"},{"last_name":"Yang","first_name":"Jinyi","full_name":"Yang, Jinyi"}],"citation":{"mla":"Silverman, John David, et al. “SHELLQs–JWST Perspective on the Intrinsic Mass Relation between Supermassive Black Holes and Their Host Galaxies at z &#62; 6.” <i>The Astrophysical Journal Letters</i>, vol. 995, no. 2, L67, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/2041-8213/ae279c\">10.3847/2041-8213/ae279c</a>.","short":"J.D. Silverman, J. Li, X. Ding, M. Onoue, M.A. Strauss, Y. Matsuoka, T. Izumi, K. Jahnke, T. Treu, M. Volonteri, C.L. Phillips, I.T. Andika, K. Aoki, J. Arita, S. Baba, S.E.I. Bosman, A.-C. Eilers, X. Fan, S. Fujimoto, M. Habouzit, Z. Haiman, M. Imanishi, K. Inayoshi, K. Iwasawa, N. Kashikawa, T. Kawaguchi, C.-H. Lee, A. Lupi, T. Nagao, J.-T. Schindler, M. Schramm, K. Shimasaku, Y. Toba, B. Trakhtenbrot, H. Umehata, M. Vestergaard, F. Walter, F. Wang, J. Yang, The Astrophysical Journal Letters 995 (2025).","chicago":"Silverman, John David, Junyao Li, Xuheng Ding, Masafusa Onoue, Michael A. Strauss, Yoshiki Matsuoka, Takuma Izumi, et al. “SHELLQs–JWST Perspective on the Intrinsic Mass Relation between Supermassive Black Holes and Their Host Galaxies at z &#62; 6.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/2041-8213/ae279c\">https://doi.org/10.3847/2041-8213/ae279c</a>.","ista":"Silverman JD, Li J, Ding X, Onoue M, Strauss MA, Matsuoka Y, Izumi T, Jahnke K, Treu T, Volonteri M, Phillips CL, Andika IT, Aoki K, Arita J, Baba S, Bosman SEI, Eilers A-C, Fan X, Fujimoto S, Habouzit M, Haiman Z, Imanishi M, Inayoshi K, Iwasawa K, Kashikawa N, Kawaguchi T, Lee C-H, Lupi A, Nagao T, Schindler J-T, Schramm M, Shimasaku K, Toba Y, Trakhtenbrot B, Umehata H, Vestergaard M, Walter F, Wang F, Yang J. 2025. SHELLQs–JWST perspective on the intrinsic mass relation between supermassive black holes and their host galaxies at z &#62; 6. The Astrophysical Journal Letters. 995(2), L67.","ama":"Silverman JD, Li J, Ding X, et al. SHELLQs–JWST perspective on the intrinsic mass relation between supermassive black holes and their host galaxies at z &#62; 6. <i>The Astrophysical Journal Letters</i>. 2025;995(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/ae279c\">10.3847/2041-8213/ae279c</a>","apa":"Silverman, J. D., Li, J., Ding, X., Onoue, M., Strauss, M. A., Matsuoka, Y., … Yang, J. (2025). SHELLQs–JWST perspective on the intrinsic mass relation between supermassive black holes and their host galaxies at z &#62; 6. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ae279c\">https://doi.org/10.3847/2041-8213/ae279c</a>","ieee":"J. D. Silverman <i>et al.</i>, “SHELLQs–JWST perspective on the intrinsic mass relation between supermassive black holes and their host galaxies at z &#62; 6,” <i>The Astrophysical Journal Letters</i>, vol. 995, no. 2. IOP Publishing, 2025."},"publication_status":"published","OA_place":"publisher","title":"SHELLQs–JWST perspective on the intrinsic mass relation between supermassive black holes and their host galaxies at z > 6","type":"journal_article","oa_version":"Published Version","_id":"21121","intvolume":"       995","department":[{"_id":"ZoHa"}]},{"abstract":[{"text":"Accreting white dwarfs (WDs) in close binary systems, commonly known as cataclysmic variables (CVs), with orbital periods below the canonical period minimum (≈80 minutes) are rare. Such short periods can only be reached if the donor star in the CV is either significantly evolved before initiating mass transfer to the WD or is metal-poor. We present optical photometry and spectroscopy of Gaia19bxc, a high-amplitude variable identified as a polar CV with an exceptionally short orbital period of 64.42 minutes—well below the canonical CV period minimum. High-speed photometry confirms persistent double-peaked variability consistent with cyclotron beaming, thus indicating the presence of a magnetic WD. Phase-resolved Keck/Low-Resolution Imaging Spectrometer (LRIS) spectroscopy reveals strong hydrogen and helium emission lines but no donor features, indicating the accretor is a magnetic WD and the donor is hydrogen-rich, but cold and faint. The absence of a detectable donor and the low inferred temperature (≲3500 K) disfavor an evolved donor scenario. Instead, the short period and the system’s halo-like kinematics suggest Gaia19bxc may be the first known metal-poor polar. Because metal-poor donors are more compact than solar-metallicity donors of the same mass, they can reach shorter minimum periods. Gaia19bxc is one of only a handful of known metal-poor CVs below the canonical period minimum and has the shortest period of any such magnetic system discovered to date.","lang":"eng"}],"status":"public","month":"09","ddc":["520"],"article_number":"L57","file_date_updated":"2026-02-19T07:24:10Z","article_type":"original","publisher":"IOP Publishing","article_processing_charge":"Yes","volume":990,"OA_type":"gold","oa":1,"date_created":"2026-02-18T10:17:04Z","PlanS_conform":"1","quality_controlled":"1","publication":"The Astrophysical Journal Letters","DOAJ_listed":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"doi":"10.3847/2041-8213/adff82","day":"08","year":"2025","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file":[{"creator":"dernst","date_created":"2026-02-19T07:24:10Z","access_level":"open_access","file_id":"21329","success":1,"date_updated":"2026-02-19T07:24:10Z","relation":"main_file","file_size":3772189,"file_name":"2025_AstrophysicalJournal_Galiullin.pdf","checksum":"f76556d129aa0e9facc85602b0b5b54d","content_type":"application/pdf"}],"external_id":{"arxiv":["2508.20170"]},"date_published":"2025-09-08T00:00:00Z","date_updated":"2026-02-19T07:27:01Z","issue":"2","language":[{"iso":"eng"}],"acknowledgement":"Based on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grants No. AST-1440341 and AST-2034437 and a collaboration including current partners Caltech, IPAC, the Weizmann Institute of Science, the Oskar Klein Center at Stockholm University, the University of Maryland, Deutsches Elektronen-Synchrotron and Humboldt University, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, IN2P3, University of Warwick, Ruhr University Bochum, Northwestern University and former partners the University of Washington, Los Alamos National Laboratories, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. 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; https://www.cosmos.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. Some of the data presented herein were obtained at Keck Observatory, which is a private 501(c)3 nonprofit organization operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the Native Hawaiian community. We are most fortunate to have had the opportunity to conduct observations from this mountain. We are grateful to the staff of the Palomar and Keck Observatories for their work in helping us carry out our observations.\r\n\r\nI.G. acknowledges support from Kazan Federal University. A.C.R. acknowledges support from the National Science Foundation via an NSF Graduate Research Fellowship. We thank the anonymous referee for useful comments and suggestions, which contributed to the improvement of this manuscript.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","scopus_import":"1","type":"journal_article","oa_version":"Published Version","_id":"21317","intvolume":"       990","department":[{"_id":"IlCa"}],"arxiv":1,"author":[{"full_name":"Galiullin, Ilkham","first_name":"Ilkham","last_name":"Galiullin"},{"first_name":"Antonio C.","last_name":"Rodriguez","full_name":"Rodriguez, Antonio C."},{"last_name":"El-Badry","first_name":"Kareem","full_name":"El-Badry, Kareem"},{"full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","first_name":"Ilaria","last_name":"Caiazzo","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d"},{"full_name":"Szkody, Paula","last_name":"Szkody","first_name":"Paula"},{"full_name":"Nagarajan, Pranav","last_name":"Nagarajan","first_name":"Pranav"},{"full_name":"Whitebook, Samuel","first_name":"Samuel","last_name":"Whitebook"}],"publication_status":"published","citation":{"ama":"Galiullin I, Rodriguez AC, El-Badry K, et al. Optical spectroscopy of the most compact accreting binary harboring a magnetic White Dwarf and a hydrogen-rich donor. <i>The Astrophysical Journal Letters</i>. 2025;990(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/adff82\">10.3847/2041-8213/adff82</a>","ieee":"I. Galiullin <i>et al.</i>, “Optical spectroscopy of the most compact accreting binary harboring a magnetic White Dwarf and a hydrogen-rich donor,” <i>The Astrophysical Journal Letters</i>, vol. 990, no. 2. IOP Publishing, 2025.","apa":"Galiullin, I., Rodriguez, A. C., El-Badry, K., Caiazzo, I., Szkody, P., Nagarajan, P., &#38; Whitebook, S. (2025). Optical spectroscopy of the most compact accreting binary harboring a magnetic White Dwarf and a hydrogen-rich donor. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/adff82\">https://doi.org/10.3847/2041-8213/adff82</a>","chicago":"Galiullin, Ilkham, Antonio C. Rodriguez, Kareem El-Badry, Ilaria Caiazzo, Paula Szkody, Pranav Nagarajan, and Samuel Whitebook. “Optical Spectroscopy of the Most Compact Accreting Binary Harboring a Magnetic White Dwarf and a Hydrogen-Rich Donor.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/2041-8213/adff82\">https://doi.org/10.3847/2041-8213/adff82</a>.","short":"I. Galiullin, A.C. Rodriguez, K. El-Badry, I. Caiazzo, P. Szkody, P. Nagarajan, S. Whitebook, The Astrophysical Journal Letters 990 (2025).","ista":"Galiullin I, Rodriguez AC, El-Badry K, Caiazzo I, Szkody P, Nagarajan P, Whitebook S. 2025. Optical spectroscopy of the most compact accreting binary harboring a magnetic White Dwarf and a hydrogen-rich donor. The Astrophysical Journal Letters. 990(2), L57.","mla":"Galiullin, Ilkham, et al. “Optical Spectroscopy of the Most Compact Accreting Binary Harboring a Magnetic White Dwarf and a Hydrogen-Rich Donor.” <i>The Astrophysical Journal Letters</i>, vol. 990, no. 2, L57, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/2041-8213/adff82\">10.3847/2041-8213/adff82</a>."},"OA_place":"publisher","title":"Optical spectroscopy of the most compact accreting binary harboring a magnetic White Dwarf and a hydrogen-rich donor"},{"doi":"10.3847/2041-8213/adc680","day":"20","year":"2025","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file":[{"content_type":"application/pdf","checksum":"1a4fbeeb12e9022873e86c72d230a5ec","file_name":"2025_AstrophysicalJourLetters_Hu.pdf","file_size":3334014,"relation":"main_file","date_updated":"2025-05-05T11:30:34Z","success":1,"file_id":"19655","access_level":"open_access","date_created":"2025-05-05T11:30:34Z","creator":"dernst"}],"external_id":{"arxiv":["2503.03870"],"isi":["001467616800001"]},"date_updated":"2026-02-16T12:44:04Z","date_published":"2025-04-20T00:00:00Z","issue":"2","isi":1,"acknowledgement":"We thank the anonymous referee for a careful reading of our manuscript and for comments that helped improve this Letter. This work is supported by the Japan Society for the Promotion of Science (JSPS) KAKENHI grant No. 24KF0130. We acknowledge support from the National Natural Science Foundation of China (12073003, 12003003, 11721303, 11991052, 11950410493), and the China Manned Space Project (CMS-CSST-2021-A04 and CMS-CSST-2021-A06). L.C.H. is supported by the National Science Foundation of China (12233001), the National Key R&D Program of China (2022YFF0503401). Z.H. acknowledges support by US NSF grant AST-2006176 and by NASA grant 80NSSC22K0822. Some of the numerical calculation and analysis were performed with the Cray XC50 at the Center for Computational Astrophysics (CfCA) of the National Astronomical Observatory of Japan and with the High-performance Computing Platform of Peking University.","language":[{"iso":"eng"}],"scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","type":"journal_article","oa_version":"Published Version","_id":"19638","department":[{"_id":"ZoHa"}],"intvolume":"       983","arxiv":1,"OA_place":"publisher","publication_status":"published","author":[{"full_name":"Hu, Haojie","first_name":"Haojie","last_name":"Hu"},{"last_name":"Inayoshi","first_name":"Kohei","full_name":"Inayoshi, Kohei"},{"orcid":"0000-0003-3633-5403","full_name":"Haiman, Zoltán","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"},{"last_name":"Ho","first_name":"Luis C.","full_name":"Ho, Luis C."},{"last_name":"Ohsuga","first_name":"Ken","full_name":"Ohsuga, Ken"}],"citation":{"mla":"Hu, Haojie, et al. “The Convergence of Heavy and Light Seeds to Overmassive Black Holes at Cosmic Dawn.” <i>The Astrophysical Journal Letters</i>, vol. 983, no. 2, L37, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/2041-8213/adc680\">10.3847/2041-8213/adc680</a>.","ista":"Hu H, Inayoshi K, Haiman Z, Ho LC, Ohsuga K. 2025. The convergence of heavy and light seeds to overmassive black holes at cosmic dawn. The Astrophysical Journal Letters. 983(2), L37.","short":"H. Hu, K. Inayoshi, Z. Haiman, L.C. Ho, K. Ohsuga, The Astrophysical Journal Letters 983 (2025).","chicago":"Hu, Haojie, Kohei Inayoshi, Zoltán Haiman, Luis C. Ho, and Ken Ohsuga. “The Convergence of Heavy and Light Seeds to Overmassive Black Holes at Cosmic Dawn.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/2041-8213/adc680\">https://doi.org/10.3847/2041-8213/adc680</a>.","apa":"Hu, H., Inayoshi, K., Haiman, Z., Ho, L. C., &#38; Ohsuga, K. (2025). The convergence of heavy and light seeds to overmassive black holes at cosmic dawn. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/adc680\">https://doi.org/10.3847/2041-8213/adc680</a>","ieee":"H. Hu, K. Inayoshi, Z. Haiman, L. C. Ho, and K. Ohsuga, “The convergence of heavy and light seeds to overmassive black holes at cosmic dawn,” <i>The Astrophysical Journal Letters</i>, vol. 983, no. 2. IOP Publishing, 2025.","ama":"Hu H, Inayoshi K, Haiman Z, Ho LC, Ohsuga K. The convergence of heavy and light seeds to overmassive black holes at cosmic dawn. <i>The Astrophysical Journal Letters</i>. 2025;983(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/adc680\">10.3847/2041-8213/adc680</a>"},"title":"The convergence of heavy and light seeds to overmassive black holes at cosmic dawn","status":"public","abstract":[{"lang":"eng","text":"The James Webb Space Telescope has revealed low-luminosity active galactic nuclei at redshifts of z ≳ 4–7, many of which host accreting massive black holes (BHs) with BH-to-galaxy mass (MBH/M⋆) ratios exceeding the local values by more than an order of magnitude. The origin of these overmassive BHs remains unclear but requires potential contributions from heavy seeds and/or episodes of super-Eddington accretion. We present a growth model coupled with dark matter halo assembly to explore the evolution of the MBH/M⋆ ratio under different seeding and feedback scenarios. Given the gas inflow rates in protogalaxies, BHs grow episodically at moderate super-Eddington rates, and the mass ratio increases early on, despite significant mass loss through feedback. Regardless of seeding mechanisms, the mass ratio converges to a universal value ∼0.1–0.3, set by the balance between gas feeding and star formation efficiency in the nucleus. This behavior defines an attractor in the MBH–M⋆ diagram, where overmassive BHs grow more slowly than their hosts, while undermassive seeds experience rapid growth before aligning with the attractor. We derive an analytical expression for the universal mass ratio, linking it to feedback strength and halo growth. The convergence of evolutionary tracks erases seeding information from the mass ratio by z ∼ 4–6. Detecting BHs with ∼105−6 M⊙ at higher redshifts that deviate from the convergence trend would provide key diagnostics of their birth conditions."}],"month":"04","article_number":"L37","ddc":["520"],"publisher":"IOP Publishing","article_type":"letter_note","file_date_updated":"2025-05-05T11:30:34Z","article_processing_charge":"Yes","volume":983,"quality_controlled":"1","oa":1,"date_created":"2025-05-04T22:02:31Z","OA_type":"gold","publication":"The Astrophysical Journal Letters","DOAJ_listed":"1","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]}},{"DOAJ_listed":"1","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"publication":"The Astrophysical Journal Letters","month":"07","abstract":[{"text":"We report the discovery of a Lyα emitter (LAE) candidate in the immediate foreground of the quasar PSO J158-14 at zQSO = 6.0685 at a projected distance ∼29 pkpc that is associated with an extremely metal-poor absorption system. This system was found in archival observations of the quasar field with the Very Large Telescope (VLT)/Multi-Unit Spectroscopic Explorer (MUSE) and was previously missed in searches of absorption systems using quasar absorption line spectroscopy, as it imparts no detectable metal absorption lines on the background quasar spectrum. The detected Lyα emission line at a redshift of zLAE = 6.0323 is well aligned with the outer edge of the quasar’s proximity zone and can plausibly cause its observed damping wing if it is associated with a proximate subdamped Lyα absorption system with a column density of log Nhi/cm^-2 19.7. A >10 hr medium-resolution spectrum of the quasar observed with the Magellan/Folded-port InfraRed Echellette (FIRE) and VLT/X-Shooter spectrographs reveals a metallicity constraint of [Z/H] < −3. Such low metallicity makes this system an extremely metal-poor galaxy candidate and provides an exciting site to study possible signatures of Population III stars.","lang":"eng"}],"status":"public","PlanS_conform":"1","OA_type":"gold","oa":1,"date_created":"2025-07-20T22:02:01Z","quality_controlled":"1","volume":987,"article_processing_charge":"Yes","file_date_updated":"2025-07-22T08:38:14Z","article_type":"original","publisher":"IOP Publishing","ddc":["520"],"article_number":"L33","department":[{"_id":"JoMa"}],"intvolume":"       987","_id":"20030","oa_version":"Published Version","type":"journal_article","title":"An extremely metal-poor Lyα emitter candidate at z = 6 revealed through absorption spectroscopy","citation":{"mla":"Ďurovčíková, Dominika, et al. “An Extremely Metal-Poor Lyα Emitter Candidate at z = 6 Revealed through Absorption Spectroscopy.” <i>The Astrophysical Journal Letters</i>, vol. 987, no. 2, L33, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/2041-8213/ade71c\">10.3847/2041-8213/ade71c</a>.","ista":"Ďurovčíková D, Eilers AC, Simcoe RA, Welsh L, Meyer RA, Matthee JJ, Ryan-Weber EV, Yue M, Katz H, Satyavolu S, Becker G, Davies FB, Farina EP. 2025. An extremely metal-poor Lyα emitter candidate at z = 6 revealed through absorption spectroscopy. The Astrophysical Journal Letters. 987(2), L33.","chicago":"Ďurovčíková, Dominika, Anna Christina Eilers, Robert A. Simcoe, Louise Welsh, Romain A. Meyer, Jorryt J Matthee, Emma V. Ryan-Weber, et al. “An Extremely Metal-Poor Lyα Emitter Candidate at z = 6 Revealed through Absorption Spectroscopy.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/2041-8213/ade71c\">https://doi.org/10.3847/2041-8213/ade71c</a>.","short":"D. Ďurovčíková, A.C. Eilers, R.A. Simcoe, L. Welsh, R.A. Meyer, J.J. Matthee, E.V. Ryan-Weber, M. Yue, H. Katz, S. Satyavolu, G. Becker, F.B. Davies, E.P. Farina, The Astrophysical Journal Letters 987 (2025).","apa":"Ďurovčíková, D., Eilers, A. C., Simcoe, R. A., Welsh, L., Meyer, R. A., Matthee, J. J., … Farina, E. P. (2025). An extremely metal-poor Lyα emitter candidate at z = 6 revealed through absorption spectroscopy. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ade71c\">https://doi.org/10.3847/2041-8213/ade71c</a>","ieee":"D. Ďurovčíková <i>et al.</i>, “An extremely metal-poor Lyα emitter candidate at z = 6 revealed through absorption spectroscopy,” <i>The Astrophysical Journal Letters</i>, vol. 987, no. 2. IOP Publishing, 2025.","ama":"Ďurovčíková D, Eilers AC, Simcoe RA, et al. An extremely metal-poor Lyα emitter candidate at z = 6 revealed through absorption spectroscopy. <i>The Astrophysical Journal Letters</i>. 2025;987(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/ade71c\">10.3847/2041-8213/ade71c</a>"},"author":[{"last_name":"Ďurovčíková","first_name":"Dominika","full_name":"Ďurovčíková, Dominika"},{"full_name":"Eilers, Anna Christina","last_name":"Eilers","first_name":"Anna Christina"},{"last_name":"Simcoe","first_name":"Robert A.","full_name":"Simcoe, Robert A."},{"full_name":"Welsh, Louise","last_name":"Welsh","first_name":"Louise"},{"first_name":"Romain A.","last_name":"Meyer","full_name":"Meyer, Romain A."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"full_name":"Ryan-Weber, Emma V.","last_name":"Ryan-Weber","first_name":"Emma V."},{"first_name":"Minghao","last_name":"Yue","full_name":"Yue, Minghao"},{"full_name":"Katz, Harley","first_name":"Harley","last_name":"Katz"},{"first_name":"Sindhu","last_name":"Satyavolu","full_name":"Satyavolu, Sindhu"},{"last_name":"Becker","first_name":"George","full_name":"Becker, George"},{"last_name":"Davies","first_name":"Frederick B.","full_name":"Davies, Frederick B."},{"last_name":"Farina","first_name":"Emanuele Paolo","full_name":"Farina, Emanuele Paolo"}],"publication_status":"published","OA_place":"publisher","arxiv":1,"date_updated":"2026-02-16T12:44:23Z","date_published":"2025-07-10T00:00:00Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file":[{"relation":"main_file","date_updated":"2025-07-22T08:38:14Z","content_type":"application/pdf","checksum":"75d0c08514209fc6e3078fdec8e815a2","file_name":"2025_AstrophysicalJourLetters_Durovcikova.pdf","file_size":6453728,"access_level":"open_access","date_created":"2025-07-22T08:38:14Z","creator":"dernst","success":1,"file_id":"20066"}],"external_id":{"arxiv":["2505.01499"],"isi":["001524847100001"]},"day":"10","year":"2025","doi":"10.3847/2041-8213/ade71c","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","scopus_import":"1","language":[{"iso":"eng"}],"acknowledgement":"We thank the referee for the feedback and suggestions that greatly improved the quality of this manuscript. We would like to thank Carlos Contreras, Matías Díaz, Carla Fuentes, Mauricio Martínez, Alberto Pastén, Roger Leiton, Hugo Rivera, and Gabriel Prieto for their help and support during the Magellan/FIRE observations. We would also like to thank Rongmon Bordoloi for helpful discussions. R.A.M. acknowledges support from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. This Letter includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.\r\nBased on observations collected at the European Southern Observatory under ESO programs 106.215A and 096.A-0418.\r\n\r\nThe HST data presented in this Letter were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The observations analyzed in this work can be accessed via doi:10.17909/gxmz-zd87.","isi":1,"issue":"2"},{"publication":"The Astrophysical Journal Letters","DOAJ_listed":"1","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"article_number":"L40","ddc":["520"],"publisher":"IOP Publishing","file_date_updated":"2025-10-13T09:25:12Z","article_type":"original","article_processing_charge":"Yes","volume":991,"quality_controlled":"1","OA_type":"gold","PlanS_conform":"1","date_created":"2025-10-05T22:01:35Z","oa":1,"status":"public","abstract":[{"lang":"eng","text":"Ultraviolet (UV) radiation from accreting black holes ionizes the intergalactic gas around early quasars, carving out highly ionized bubbles in their surroundings. Any changes in a quasar’s luminosity are therefore predicted to produce outward-propagating ionization gradients, affecting the Lyα absorption opacity near the quasar’s systemic redshift. This “proximity effect” is well-documented in rest-UV quasar spectra but only provides a one-dimensional probe along our line of sight. Here we present deep spectroscopic observations with the James Webb Space Telescope (JWST) of galaxies in the background of a superluminous quasar at zQSO ≈ 6.3, which reveal the quasar’s “light echo” with Lyα tomography in the transverse direction. This transverse proximity effect is detected for the first time toward multiple galaxy sightlines, allowing us to map the extent and geometry of the quasar’s ionization cone. We obtain constraints on the orientation and inclination of the cone, as well as an upper limit on the obscured solid angle fraction of fobsc < 91%. Additionally, we find a timescale of the quasar’s UV radiation of tqso = 10^5.6+0.1-0.3 yr, which is significantly shorter than would be required to build up the central supermassive black hole (SMBH) with conventional growth models, but is consistent with independent measurements of the quasars’ duty cycle. Our inferred obscured fraction disfavors a scenario where short quasar lifetimes can be explained exclusively by geometric obscuration, and instead supports the idea that radiatively inefficient accretion or growth in initially heavily enshrouded cocoons plays a pivotal role in early SMBH growth. Our results pave the way for novel studies of quasars’ ionizing geometries and radiative histories at early cosmic times."}],"month":"09","arxiv":1,"OA_place":"publisher","project":[{"grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization"}],"publication_status":"published","author":[{"full_name":"Eilers, Anna Christina","last_name":"Eilers","first_name":"Anna Christina"},{"last_name":"Yue","first_name":"Minghao","full_name":"Yue, Minghao"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"first_name":"Joseph F.","last_name":"Hennawi","full_name":"Hennawi, Joseph F."},{"full_name":"Davies, Frederick B.","first_name":"Frederick B.","last_name":"Davies"},{"full_name":"Simcoe, Robert A.","first_name":"Robert A.","last_name":"Simcoe"},{"first_name":"Richard","last_name":"Teague","full_name":"Teague, Richard"},{"first_name":"Rongmon","last_name":"Bordoloi","full_name":"Bordoloi, Rongmon"},{"full_name":"Brammer, Gabriel","last_name":"Brammer","first_name":"Gabriel"},{"last_name":"Kang","first_name":"Yi","full_name":"Kang, Yi"},{"last_name":"Kashino","first_name":"Daichi","full_name":"Kashino, Daichi"},{"last_name":"Mackenzie","first_name":"Ruari","full_name":"Mackenzie, Ruari"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"first_name":"Benjamín","last_name":"Navarrete","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","full_name":"Navarrete, Benjamín"}],"citation":{"ieee":"A. C. Eilers <i>et al.</i>, “The light echo of a high-redshift quasar mapped with Lyα tomography,” <i>The Astrophysical Journal Letters</i>, vol. 991, no. 2. IOP Publishing, 2025.","apa":"Eilers, A. C., Yue, M., Matthee, J. J., Hennawi, J. F., Davies, F. B., Simcoe, R. A., … Navarrete, B. (2025). The light echo of a high-redshift quasar mapped with Lyα tomography. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ae057a\">https://doi.org/10.3847/2041-8213/ae057a</a>","ama":"Eilers AC, Yue M, Matthee JJ, et al. The light echo of a high-redshift quasar mapped with Lyα tomography. <i>The Astrophysical Journal Letters</i>. 2025;991(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/ae057a\">10.3847/2041-8213/ae057a</a>","mla":"Eilers, Anna Christina, et al. “The Light Echo of a High-Redshift Quasar Mapped with Lyα Tomography.” <i>The Astrophysical Journal Letters</i>, vol. 991, no. 2, L40, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/2041-8213/ae057a\">10.3847/2041-8213/ae057a</a>.","ista":"Eilers AC, Yue M, Matthee JJ, Hennawi JF, Davies FB, Simcoe RA, Teague R, Bordoloi R, Brammer G, Kang Y, Kashino D, Mackenzie R, Naidu RP, Navarrete B. 2025. The light echo of a high-redshift quasar mapped with Lyα tomography. The Astrophysical Journal Letters. 991(2), L40.","chicago":"Eilers, Anna Christina, Minghao Yue, Jorryt J Matthee, Joseph F. Hennawi, Frederick B. Davies, Robert A. Simcoe, Richard Teague, et al. “The Light Echo of a High-Redshift Quasar Mapped with Lyα Tomography.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/2041-8213/ae057a\">https://doi.org/10.3847/2041-8213/ae057a</a>.","short":"A.C. Eilers, M. Yue, J.J. Matthee, J.F. Hennawi, F.B. Davies, R.A. Simcoe, R. Teague, R. Bordoloi, G. Brammer, Y. Kang, D. Kashino, R. Mackenzie, R.P. Naidu, B. Navarrete, The Astrophysical Journal Letters 991 (2025)."},"title":"The light echo of a high-redshift quasar mapped with Lyα tomography","type":"journal_article","oa_version":"Published Version","_id":"20425","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"intvolume":"       991","issue":"2","isi":1,"acknowledgement":"This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with programs #1243 and #4713.\r\n\r\nAll of the data presented in this Letter were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via doi:10.17909/w7hm-qb39.\r\nJ.M. is supported by the European Union (ERC, AGENTS, 101076224).","language":[{"iso":"eng"}],"scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","doi":"10.3847/2041-8213/ae057a","day":"25","year":"2025","file":[{"file_name":"2025_AstrophysicalJour_Eilers.pdf","checksum":"3cb8099b9a915755164e5675b33f8a03","content_type":"application/pdf","file_size":23585591,"relation":"main_file","date_updated":"2025-10-13T09:25:12Z","success":1,"file_id":"20461","access_level":"open_access","creator":"dernst","date_created":"2025-10-13T09:25:12Z"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"external_id":{"arxiv":["2509.05417"],"isi":["001581023000001"]},"date_published":"2025-09-25T00:00:00Z","date_updated":"2026-02-16T12:44:42Z"},{"DOAJ_listed":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"publication":"The Astrophysical Journal Letters","status":"public","abstract":[{"lang":"eng","text":"We propose a formation pathway linking black holes (BHs) observed in gravitational-wave (GW) mergers, wide BH–stellar systems uncovered by Gaia, and accreting low-mass X-ray binaries (LMXBs). In this scenario, a stellar-mass BH binary undergoes isolated binary evolution and merges while hosting a distant, dynamically unimportant tertiary stellar companion. The tertiary becomes relevant only after the merger, when the remnant BH receives a GW recoil kick. Depending on the kick velocity and system configuration, the outcome can be: (1) a bright electromagnetic (EM) counterpart to the GW merger; (2) an LMXB; (3) a wide BH–stellar companion system resembling the Gaia BH population; or (4) an unbound isolated BH. Modeling the three-body dynamics, we find that ∼0.02% of LIGO–Virgo–KAGRA (LVK) mergers may be followed by an EM counterpart within ∼10 days, produced by tidal disruption of the star by the BH. The flare is likely brightest in the optical–UV and lasts for days to weeks; in some cases, partial disruption causes recurring flares with a period of ∼2 months. We further estimate that this channel can produce ∼1%–10% of Gaia BH systems in the Milky Way. This scenario provides the first physically motivated link between GW sources, Gaia BHs, and some X-ray binaries, and predicts a rare but robust pathway for EM counterparts to binary BH mergers, potentially detectable in LVK’s O5 run."}],"month":"10","article_processing_charge":"Yes","volume":992,"quality_controlled":"1","PlanS_conform":"1","OA_type":"gold","oa":1,"date_created":"2025-10-19T22:01:31Z","article_number":"L12","ddc":["520"],"publisher":"IOP Publishing","file_date_updated":"2025-10-23T09:09:30Z","article_type":"original","_id":"20493","department":[{"_id":"ZoHa"}],"intvolume":"       992","type":"journal_article","oa_version":"Published Version","OA_place":"publisher","publication_status":"published","citation":{"ieee":"S. Naoz, Z. Haiman, E. Quataert, and L. Holzknecht, “Triples as links between binary Black Hole mergers, their electromagnetic counterparts, and galactic Black Holes,” <i>The Astrophysical Journal Letters</i>, vol. 992, no. 1. IOP Publishing, 2025.","apa":"Naoz, S., Haiman, Z., Quataert, E., &#38; Holzknecht, L. (2025). Triples as links between binary Black Hole mergers, their electromagnetic counterparts, and galactic Black Holes. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ae0a20\">https://doi.org/10.3847/2041-8213/ae0a20</a>","ama":"Naoz S, Haiman Z, Quataert E, Holzknecht L. Triples as links between binary Black Hole mergers, their electromagnetic counterparts, and galactic Black Holes. <i>The Astrophysical Journal Letters</i>. 2025;992(1). doi:<a href=\"https://doi.org/10.3847/2041-8213/ae0a20\">10.3847/2041-8213/ae0a20</a>","mla":"Naoz, Smadar, et al. “Triples as Links between Binary Black Hole Mergers, Their Electromagnetic Counterparts, and Galactic Black Holes.” <i>The Astrophysical Journal Letters</i>, vol. 992, no. 1, L12, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/2041-8213/ae0a20\">10.3847/2041-8213/ae0a20</a>.","ista":"Naoz S, Haiman Z, Quataert E, Holzknecht L. 2025. Triples as links between binary Black Hole mergers, their electromagnetic counterparts, and galactic Black Holes. The Astrophysical Journal Letters. 992(1), L12.","chicago":"Naoz, Smadar, Zoltán Haiman, Eliot Quataert, and Liz Holzknecht. “Triples as Links between Binary Black Hole Mergers, Their Electromagnetic Counterparts, and Galactic Black Holes.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/2041-8213/ae0a20\">https://doi.org/10.3847/2041-8213/ae0a20</a>.","short":"S. Naoz, Z. Haiman, E. Quataert, L. Holzknecht, The Astrophysical Journal Letters 992 (2025)."},"author":[{"full_name":"Naoz, Smadar","last_name":"Naoz","first_name":"Smadar"},{"full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán"},{"full_name":"Quataert, Eliot","last_name":"Quataert","first_name":"Eliot"},{"first_name":"Liz","last_name":"Holzknecht","full_name":"Holzknecht, Liz"}],"title":"Triples as links between binary Black Hole mergers, their electromagnetic counterparts, and galactic Black Holes","arxiv":1,"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"external_id":{"arxiv":["2508.13270"],"isi":["001589455900001"]},"file":[{"file_size":8787316,"content_type":"application/pdf","file_name":"2025_AstrophysicalJour_Naoz.pdf","checksum":"cb81d666f6d7638a5bcf45653d25bcb3","date_updated":"2025-10-23T09:09:30Z","relation":"main_file","file_id":"20520","success":1,"date_created":"2025-10-23T09:09:30Z","creator":"dernst","access_level":"open_access"}],"date_published":"2025-10-10T00:00:00Z","date_updated":"2026-02-16T12:44:56Z","doi":"10.3847/2041-8213/ae0a20","year":"2025","day":"10","scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","issue":"1","isi":1,"acknowledgement":"We thank the anonymous referee for the useful and detailed report. S.N. acknowledges the partial support of NSF-BSF grant AST-2206428 and NASA XRP grant 80NSSC23K0262, as well as Howard and Astrid Preston for their generous support. Z.H. acknowledges support from NASA grants 80NSSC22K0822 and 80NSSC24K0440. E.Q. thanks the Gordon and Betty Moore Foundation for support through grant GBMF5076.","language":[{"iso":"eng"}]},{"arxiv":1,"title":"Escape fractions from unattenuated Lyα emitters around luminous z > 6 quasars","publication_status":"published","citation":{"ista":"Yue M, Eilers AC, Matthee JJ, Naidu RP, Bordoloi R, Davies FB, Hennawi JF, Kashino D, Mackenzie R, Simcoe RA. 2025. Escape fractions from unattenuated Lyα emitters around luminous z &#62; 6 quasars. The Astrophysical Journal Letters. 993(1), L12.","chicago":"Yue, Minghao, Anna Christina Eilers, Jorryt J Matthee, Rohan P. Naidu, Rongmon Bordoloi, Frederick B. Davies, Joseph F. Hennawi, Daichi Kashino, Ruari Mackenzie, and Robert A. Simcoe. “Escape Fractions from Unattenuated Lyα Emitters around Luminous z &#62; 6 Quasars.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/2041-8213/ae0e0e\">https://doi.org/10.3847/2041-8213/ae0e0e</a>.","short":"M. Yue, A.C. Eilers, J.J. Matthee, R.P. Naidu, R. Bordoloi, F.B. Davies, J.F. Hennawi, D. Kashino, R. Mackenzie, R.A. Simcoe, The Astrophysical Journal Letters 993 (2025).","mla":"Yue, Minghao, et al. “Escape Fractions from Unattenuated Lyα Emitters around Luminous z &#62; 6 Quasars.” <i>The Astrophysical Journal Letters</i>, vol. 993, no. 1, L12, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/2041-8213/ae0e0e\">10.3847/2041-8213/ae0e0e</a>.","apa":"Yue, M., Eilers, A. C., Matthee, J. J., Naidu, R. P., Bordoloi, R., Davies, F. B., … Simcoe, R. A. (2025). Escape fractions from unattenuated Lyα emitters around luminous z &#62; 6 quasars. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ae0e0e\">https://doi.org/10.3847/2041-8213/ae0e0e</a>","ieee":"M. Yue <i>et al.</i>, “Escape fractions from unattenuated Lyα emitters around luminous z &#62; 6 quasars,” <i>The Astrophysical Journal Letters</i>, vol. 993, no. 1. IOP Publishing, 2025.","ama":"Yue M, Eilers AC, Matthee JJ, et al. Escape fractions from unattenuated Lyα emitters around luminous z &#62; 6 quasars. <i>The Astrophysical Journal Letters</i>. 2025;993(1). doi:<a href=\"https://doi.org/10.3847/2041-8213/ae0e0e\">10.3847/2041-8213/ae0e0e</a>"},"author":[{"last_name":"Yue","first_name":"Minghao","full_name":"Yue, Minghao"},{"last_name":"Eilers","first_name":"Anna Christina","full_name":"Eilers, Anna Christina"},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"full_name":"Bordoloi, Rongmon","first_name":"Rongmon","last_name":"Bordoloi"},{"first_name":"Frederick B.","last_name":"Davies","full_name":"Davies, Frederick B."},{"first_name":"Joseph F.","last_name":"Hennawi","full_name":"Hennawi, Joseph F."},{"full_name":"Kashino, Daichi","first_name":"Daichi","last_name":"Kashino"},{"last_name":"Mackenzie","first_name":"Ruari","full_name":"Mackenzie, Ruari"},{"first_name":"Robert A.","last_name":"Simcoe","full_name":"Simcoe, Robert A."}],"OA_place":"publisher","oa_version":"Published Version","type":"journal_article","intvolume":"       993","department":[{"_id":"JoMa"}],"_id":"20649","language":[{"iso":"eng"}],"acknowledgement":"We thank the referee for valuable comments. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program ID #3117 and #4713. Support for\r\nthis work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the\r\nAssociation of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.","isi":1,"issue":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","scopus_import":"1","year":"2025","day":"01","doi":"10.3847/2041-8213/ae0e0e","date_published":"2025-11-01T00:00:00Z","date_updated":"2026-02-16T12:45:16Z","external_id":{"isi":["001600890100001"],"arxiv":["2507.05381"]},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file":[{"file_size":39736710,"file_name":"2025_AstrophysicalJour_Yue.pdf","checksum":"11d35c1c52c000f8c14bc6de2e9f4b3f","content_type":"application/pdf","date_updated":"2025-11-24T13:18:34Z","relation":"main_file","file_id":"20680","success":1,"creator":"dernst","date_created":"2025-11-24T13:18:34Z","access_level":"open_access"}],"publication":"The Astrophysical Journal Letters","DOAJ_listed":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"file_date_updated":"2025-11-24T13:18:34Z","article_type":"original","publisher":"IOP Publishing","ddc":["520"],"article_number":"L12","PlanS_conform":"1","date_created":"2025-11-16T23:01:24Z","OA_type":"gold","oa":1,"quality_controlled":"1","article_processing_charge":"Yes","volume":993,"month":"11","abstract":[{"text":"Ionized proximity zones around luminous quasars provide a unique laboratory to characterize the Lyα emission lines from z > 6 galaxies without significant attenuation from the intergalactic medium (IGM). However, Lyα line measurements for galaxies within high-redshift quasars’ proximity zones have been rare so far. Here we present deep spectroscopic observations obtained with the NIRSpec/Micro-Shutter Assembly (MSA) instrument on the James Webb Space Telescope of galaxies in two z > 6 quasar fields. We measure the Lyα line fluxes for 50 galaxies at 6 < z < 7 with UV absolute magnitude M UV < −19 (median M UV = −19.97), among which 15 are located near the luminous quasars, i.e., within Δv < 2500 km s−1. We find that galaxies near the quasars show significant flux blueward of the systemic Lyα wavelength, and have higher Lyα equivalent width compared to galaxies at similar redshifts that are not located within the quasars’ environment. Our result indicates little or no redshift evolution for the Lyα emitter fraction from z ∼ 6.4 to z ∼ 5. Leveraging the low IGM opacity in the quasars’ vicinity, we evaluate the Lyα escape fraction (f esc Ly α) of high-redshift galaxies. Our analysis suggests that galaxies at 〈z〉 ≈ 6.4 have an average f esc Ly α = 0.14 ± 0.04. This value is consistent with reionization models where the Lyman continuum escape fraction is low ( fescLyC ≲ 0.1 ) for luminous galaxies, and where the most luminous galaxies have only a minor contribution to the total ionizing photon budget. © 2025. The Author(s). Published by the American Astronomical Society.","lang":"eng"}],"status":"public"},{"oa_version":"Published Version","type":"journal_article","intvolume":"       976","department":[{"_id":"JoMa"}],"_id":"18760","arxiv":1,"title":"Ionized gas kinematics with FRESCO: An extended, massive, rapidly rotating galaxy at z = 5.4","author":[{"full_name":"Nelson, Erica","first_name":"Erica","last_name":"Nelson"},{"full_name":"Brammer, Gabriel","first_name":"Gabriel","last_name":"Brammer"},{"full_name":"Giménez-Arteaga, Clara","last_name":"Giménez-Arteaga","first_name":"Clara"},{"first_name":"Pascal A.","last_name":"Oesch","full_name":"Oesch, Pascal A."},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"full_name":"Übler, Hannah","first_name":"Hannah","last_name":"Übler"},{"first_name":"Jasleen","last_name":"Matharu","full_name":"Matharu, Jasleen"},{"full_name":"Shapley, Alice E.","first_name":"Alice E.","last_name":"Shapley"},{"full_name":"Whitaker, Katherine E.","last_name":"Whitaker","first_name":"Katherine E."},{"first_name":"Emily","last_name":"Wisnioski","full_name":"Wisnioski, Emily"},{"full_name":"Förster Schreiber, Natascha M.","first_name":"Natascha M.","last_name":"Förster Schreiber"},{"full_name":"Smit, Renske","first_name":"Renske","last_name":"Smit"},{"full_name":"Van Dokkum, Pieter","last_name":"Van Dokkum","first_name":"Pieter"},{"first_name":"John","last_name":"Chisholm","full_name":"Chisholm, John"},{"full_name":"Endsley, Ryan","last_name":"Endsley","first_name":"Ryan"},{"last_name":"Hartley","first_name":"Abigail I.","full_name":"Hartley, Abigail I."},{"full_name":"Gibson, Justus","last_name":"Gibson","first_name":"Justus"},{"first_name":"Emma","last_name":"Giovinazzo","full_name":"Giovinazzo, Emma"},{"full_name":"Illingworth, Garth","first_name":"Garth","last_name":"Illingworth"},{"full_name":"Labbe, Ivo","last_name":"Labbe","first_name":"Ivo"},{"first_name":"Michael V.","last_name":"Maseda","full_name":"Maseda, Michael V."},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"full_name":"Covelo Paz, Alba","first_name":"Alba","last_name":"Covelo Paz"},{"last_name":"Price","first_name":"Sedona H.","full_name":"Price, Sedona H."},{"full_name":"Reddy, Naveen A.","first_name":"Naveen A.","last_name":"Reddy"},{"full_name":"Shivaei, Irene","first_name":"Irene","last_name":"Shivaei"},{"full_name":"Weibel, Andrea","first_name":"Andrea","last_name":"Weibel"},{"first_name":"Stijn","last_name":"Wuyts","full_name":"Wuyts, Stijn"},{"full_name":"Xiao, Mengyuan","first_name":"Mengyuan","last_name":"Xiao"},{"full_name":"Alberts, Stacey","last_name":"Alberts","first_name":"Stacey"},{"first_name":"William M.","last_name":"Baker","full_name":"Baker, William M."},{"full_name":"Bunker, Andrew J.","first_name":"Andrew J.","last_name":"Bunker"},{"last_name":"Cameron","first_name":"Alex J.","full_name":"Cameron, Alex J."},{"full_name":"Charlot, Stephane","last_name":"Charlot","first_name":"Stephane"},{"full_name":"Eisenstein, Daniel J.","first_name":"Daniel J.","last_name":"Eisenstein"},{"first_name":"Anna","last_name":"De Graaff","full_name":"De Graaff, Anna"},{"last_name":"Ji","first_name":"Zhiyuan","full_name":"Ji, Zhiyuan"},{"last_name":"Johnson","first_name":"Benjamin D.","full_name":"Johnson, Benjamin D."},{"first_name":"Gareth C.","last_name":"Jones","full_name":"Jones, Gareth C."},{"full_name":"Maiolino, Roberto","first_name":"Roberto","last_name":"Maiolino"},{"last_name":"Robertson","first_name":"Brant","full_name":"Robertson, Brant"},{"last_name":"Sandles","first_name":"Lester","full_name":"Sandles, Lester"},{"full_name":"Suess, Katherine A.","last_name":"Suess","first_name":"Katherine A."},{"last_name":"Tacchella","first_name":"Sandro","full_name":"Tacchella, Sandro"},{"full_name":"Williams, Christina C.","first_name":"Christina C.","last_name":"Williams"},{"full_name":"Witstok, Joris","last_name":"Witstok","first_name":"Joris"}],"publication_status":"published","citation":{"ista":"Nelson E, Brammer G, Giménez-Arteaga C, Oesch PA, Naidu RP, Übler H, Matharu J, Shapley AE, Whitaker KE, Wisnioski E, Förster Schreiber NM, Smit R, Van Dokkum P, Chisholm J, Endsley R, Hartley AI, Gibson J, Giovinazzo E, Illingworth G, Labbe I, Maseda MV, Matthee JJ, Covelo Paz A, Price SH, Reddy NA, Shivaei I, Weibel A, Wuyts S, Xiao M, Alberts S, Baker WM, Bunker AJ, Cameron AJ, Charlot S, Eisenstein DJ, De Graaff A, Ji Z, Johnson BD, Jones GC, Maiolino R, Robertson B, Sandles L, Suess KA, Tacchella S, Williams CC, Witstok J. 2024. Ionized gas kinematics with FRESCO: An extended, massive, rapidly rotating galaxy at z = 5.4. Astrophysical Journal Letters. 976(2), L27.","chicago":"Nelson, Erica, Gabriel Brammer, Clara Giménez-Arteaga, Pascal A. Oesch, Rohan P. Naidu, Hannah Übler, Jasleen Matharu, et al. “Ionized Gas Kinematics with FRESCO: An Extended, Massive, Rapidly Rotating Galaxy at z = 5.4.” <i>Astrophysical Journal Letters</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.3847/2041-8213/ad7b17\">https://doi.org/10.3847/2041-8213/ad7b17</a>.","short":"E. Nelson, G. Brammer, C. Giménez-Arteaga, P.A. Oesch, R.P. Naidu, H. Übler, J. Matharu, A.E. Shapley, K.E. Whitaker, E. Wisnioski, N.M. Förster Schreiber, R. Smit, P. Van Dokkum, J. Chisholm, R. Endsley, A.I. Hartley, J. Gibson, E. Giovinazzo, G. Illingworth, I. Labbe, M.V. Maseda, J.J. Matthee, A. Covelo Paz, S.H. Price, N.A. Reddy, I. Shivaei, A. Weibel, S. Wuyts, M. Xiao, S. Alberts, W.M. Baker, A.J. Bunker, A.J. Cameron, S. Charlot, D.J. Eisenstein, A. De Graaff, Z. Ji, B.D. Johnson, G.C. Jones, R. Maiolino, B. Robertson, L. Sandles, K.A. Suess, S. Tacchella, C.C. Williams, J. Witstok, Astrophysical Journal Letters 976 (2024).","mla":"Nelson, Erica, et al. “Ionized Gas Kinematics with FRESCO: An Extended, Massive, Rapidly Rotating Galaxy at z = 5.4.” <i>Astrophysical Journal Letters</i>, vol. 976, no. 2, L27, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/2041-8213/ad7b17\">10.3847/2041-8213/ad7b17</a>.","ieee":"E. Nelson <i>et al.</i>, “Ionized gas kinematics with FRESCO: An extended, massive, rapidly rotating galaxy at z = 5.4,” <i>Astrophysical Journal Letters</i>, vol. 976, no. 2. IOP Publishing, 2024.","apa":"Nelson, E., Brammer, G., Giménez-Arteaga, C., Oesch, P. A., Naidu, R. P., Übler, H., … Witstok, J. (2024). Ionized gas kinematics with FRESCO: An extended, massive, rapidly rotating galaxy at z = 5.4. <i>Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ad7b17\">https://doi.org/10.3847/2041-8213/ad7b17</a>","ama":"Nelson E, Brammer G, Giménez-Arteaga C, et al. Ionized gas kinematics with FRESCO: An extended, massive, rapidly rotating galaxy at z = 5.4. <i>Astrophysical Journal Letters</i>. 2024;976(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/ad7b17\">10.3847/2041-8213/ad7b17</a>"},"OA_place":"publisher","year":"2024","day":"01","doi":"10.3847/2041-8213/ad7b17","date_updated":"2025-09-09T11:58:02Z","date_published":"2024-12-01T00:00:00Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file":[{"access_level":"open_access","creator":"dernst","date_created":"2025-01-08T08:18:39Z","success":1,"file_id":"18771","relation":"main_file","date_updated":"2025-01-08T08:18:39Z","file_name":"2024_AstrophysicalJour_Nelson.pdf","checksum":"5c7320196586b4340e55f215d8737185","content_type":"application/pdf","file_size":1822989}],"external_id":{"isi":["001364636000001"],"arxiv":["2310.06887"]},"language":[{"iso":"eng"}],"acknowledgement":"We thank the reviewer and editorial staff for their excellent feedback and effort—the manuscript is much stronger as a result. Support for this work was provided by NASA through grant JWST-GO-01895 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. H.Ü. gratefully acknowledges support by the Isaac Newton Trust and by the Kavli Foundation through a Newton-Kavli Junior Fellowship. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract No. MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. R.S. acknowledges an STFC Ernest Rutherford Fellowship (ST/S004831/1). R.P.N. acknowledges support for this work provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. M.V.M. acknowledges support from the National Science Foundation via AAG grant 2205519 and the Wisconsin Alumni Research Foundation via grant MSN251397. R.M. also acknowledges funding from a research professorship from the Royal Society. A.J.B., A.J.C., and G.C.J. acknowledge funding from the \"FirstGalaxies\" Advanced Grant from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 789056). I.L. acknowledges support by the Australian Research Council through Future Fellowship FT220100798. D.J.E. is supported as a Simons Investigator and by a JWST/NIRCam contract to the University of Arizona, NAS5-02015. R.M., J.W., L.S., and W.B. acknowledge support by the Science and Technology Facilities Council (STFC), the ERC through advanced grant 695671 \"QUENCH,\" and the UKRI Frontier Research grant RISEandFALL. B.E.R. acknowledges support from the NIRCam Science Team contract to the University of Arizona, NAS5-02015. The research of C.C.W. is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The HST and JWST image mosaics of the FRESCO fields are released at MAST as a High Level Science Product (P. Oesch & D. Magee 2023).","isi":1,"issue":"2","has_accepted_license":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","scopus_import":"1","publication":"Astrophysical Journal Letters","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"DOAJ_listed":"1","month":"12","abstract":[{"lang":"eng","text":"With the remarkable sensitivity and resolution of JWST in the infrared, measuring rest-optical kinematics of galaxies at z > 5 has become possible for the first time. This study pilots a new method for measuring galaxy dynamics for highly multiplexed, unbiased samples by combining FRESCO NIRCam grism spectroscopy and JADES medium-band imaging. Here we present one of the first JWST kinematic measurements for a galaxy at z > 5. We find a significant velocity gradient, which, if interpreted as rotation, yields Vrot = 305 ± 70 km s−1, and we hence refer to this galaxy as Twister-z5. With a rest-frame optical effective radius of re = 2.25 kpc, the high rotation velocity in this galaxy is not due to a compact size, as may be expected in the early Universe, but rather to a high total mass, (math formula). This is a factor of roughly 10× higher than the stellar mass within re. We also observe that the radial Hα equivalent width profile and the specific star formation rate map from resolved stellar population modeling are centrally depressed by a factor of ∼1.5 from the center to re. Combined with the morphology of the line-emitting gas in comparison to the continuum, this centrally suppressed star formation is consistent with a star-forming disk surrounding a bulge growing inside out. While large, rapidly rotating disks are common to z ∼ 2, the existence of one after only 1 Gyr of cosmic time, shown for the first time in ionized gas, adds to the growing evidence that some galaxies matured earlier than expected in the history of the Universe."}],"status":"public","file_date_updated":"2025-01-08T08:18:39Z","article_type":"letter_note","publisher":"IOP Publishing","ddc":["520"],"article_number":"L27","OA_type":"gold","oa":1,"date_created":"2025-01-05T23:01:58Z","quality_controlled":"1","article_processing_charge":"Yes","volume":976},{"oa":1,"date_created":"2024-07-14T22:01:11Z","quality_controlled":"1","article_processing_charge":"Yes","volume":969,"file_date_updated":"2024-07-16T06:24:29Z","article_type":"original","publisher":"IOP Publishing","ddc":["520"],"article_number":"L13","month":"07","abstract":[{"lang":"eng","text":"The identification of red, apparently massive galaxies at z > 7 in early James Webb Space Telescope (JWST) photometry suggests a strongly accelerated time line compared to standard models of galaxy growth. A major uncertainty in the interpretation is whether the red colors are caused by evolved stellar populations, dust, or other effects such as emission lines or active galactic nuclei (AGNs). Here we show that three of the massive galaxy candidates at z = 6.7–8.4 have prominent Balmer breaks in JWST/NIRSpec spectroscopy from the RUBIES program. The Balmer breaks demonstrate unambiguously that stellar emission dominates at λrest = 0.4 μm and require formation histories extending hundreds of millions of years into the past in galaxies only 600–800 Myr after the big bang. Two of the three galaxies also show broad Balmer lines, with Hβ FWHM > 2500 km s−1, suggesting that dust-reddened AGNs contribute to, or even dominate, the spectral energy distributions of these galaxies at λrest ≳ 0.6 μm. All three galaxies have relatively narrow [O iii] lines, seemingly ruling out a high-mass interpretation if the lines arise in dynamically relaxed, inclined disks. Yet the inferred masses also remain highly uncertain. We model the high-quality spectra using Prospector to decompose the continuum into stellar and AGN components and explore limiting cases in stellar/AGN contribution. This produces a wide range of possible stellar masses, spanning M⋆ ∼ 109−1011M⊙. Nevertheless, all fits suggest a very early and rapid formation, most of which follow with a truncation in star formation. Potential origins and evolutionary tracks for these objects are discussed, from the cores of massive galaxies to low-mass galaxies with overmassive black holes. Intriguingly, we find all of these explanations to be incomplete; deeper and redder data are needed to understand the physics of these systems."}],"status":"public","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"DOAJ_listed":"1","publication":"Astrophysical Journal Letters","has_accepted_license":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","scopus_import":"1","language":[{"iso":"eng"}],"acknowledgement":"We thank the anonymous referee for the helpful comments. B.W. and J.L. acknowledge support from JWST-GO04233.009-A. The Cosmic Dawn Center is funded by the Danish National Research Foundation (DNRF) under grant No. 140. This research was supported by the International Space Science Institute (ISSI) in Bern, through ISSI International Team project No. 562 (First Light at Cosmic Dawn: Exploiting the James Webb Space Telescope Revolution). 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. The JWST data presented in this Letter were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via doi:10.17909/3a4n-9p88. Computations for this research were performed on the Pennsylvania State University’s Institute for Computational and Data Sciences’ Roar supercomputer. This publication made use of the NASA Astrophysical Data System for bibliographic information. \r\nFacilities: HST (ACS, WFC3), JWST (NIRCam, NIRSpec). Software: Astropy (Astropy Collaboration et al. 2013, 2018, 2022), dynesty (Speagle 2020), EAzY (Brammer et al. 2008),\r\nemcee (Foreman-Mackey et al. 2013), Matplotlib (Hunter 2007), msaexp (Brammer 2023b), msafit (de Graaff et al. 2024a), NumPy (Harris et al. 2020), Prospector (Johnson et al. 2021), Python-FSPS (Johnson et al. 2023).","isi":1,"issue":"1","date_updated":"2025-09-08T08:10:21Z","date_published":"2024-07-01T00:00:00Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"external_id":{"arxiv":["2405.01473"],"isi":["001257903200001"]},"file":[{"relation":"main_file","date_updated":"2024-07-16T06:24:29Z","content_type":"application/pdf","checksum":"bb1a6725586df12e745d091b5778bb2b","file_name":"2024_AstrophysicalJourn_Wang.pdf","file_size":3273303,"access_level":"open_access","date_created":"2024-07-16T06:24:29Z","creator":"dernst","success":1,"file_id":"17243"}],"day":"01","year":"2024","doi":"10.3847/2041-8213/ad55f7","title":"RUBIES: Evolved stellar populations with extended formation histories at z ∼ 7-8 in candidate massive galaxies identified with JWST/NIRSpec","citation":{"ieee":"B. Wang <i>et al.</i>, “RUBIES: Evolved stellar populations with extended formation histories at z ∼ 7-8 in candidate massive galaxies identified with JWST/NIRSpec,” <i>Astrophysical Journal Letters</i>, vol. 969, no. 1. IOP Publishing, 2024.","apa":"Wang, B., Leja, J., De Graaff, A., Brammer, G. B., Weibel, A., Van Dokkum, P., … Williams, C. C. (2024). RUBIES: Evolved stellar populations with extended formation histories at z ∼ 7-8 in candidate massive galaxies identified with JWST/NIRSpec. <i>Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ad55f7\">https://doi.org/10.3847/2041-8213/ad55f7</a>","ama":"Wang B, Leja J, De Graaff A, et al. RUBIES: Evolved stellar populations with extended formation histories at z ∼ 7-8 in candidate massive galaxies identified with JWST/NIRSpec. <i>Astrophysical Journal Letters</i>. 2024;969(1). doi:<a href=\"https://doi.org/10.3847/2041-8213/ad55f7\">10.3847/2041-8213/ad55f7</a>","mla":"Wang, Bingjie, et al. “RUBIES: Evolved Stellar Populations with Extended Formation Histories at z ∼ 7-8 in Candidate Massive Galaxies Identified with JWST/NIRSpec.” <i>Astrophysical Journal Letters</i>, vol. 969, no. 1, L13, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/2041-8213/ad55f7\">10.3847/2041-8213/ad55f7</a>.","ista":"Wang B, Leja J, De Graaff A, Brammer GB, Weibel A, Van Dokkum P, Baggen JFW, Suess KA, Greene JE, Bezanson R, Cleri NJ, Hirschmann M, Labbé I, Matthee JJ, Mcconachie I, Naidu RP, Nelson E, Oesch PA, Setton DJ, Williams CC. 2024. RUBIES: Evolved stellar populations with extended formation histories at z ∼ 7-8 in candidate massive galaxies identified with JWST/NIRSpec. Astrophysical Journal Letters. 969(1), L13.","short":"B. Wang, J. Leja, A. De Graaff, G.B. Brammer, A. Weibel, P. Van Dokkum, J.F.W. Baggen, K.A. Suess, J.E. Greene, R. Bezanson, N.J. Cleri, M. Hirschmann, I. Labbé, J.J. Matthee, I. Mcconachie, R.P. Naidu, E. Nelson, P.A. Oesch, D.J. Setton, C.C. Williams, Astrophysical Journal Letters 969 (2024).","chicago":"Wang, Bingjie, Joel Leja, Anna De Graaff, Gabriel B. Brammer, Andrea Weibel, Pieter Van Dokkum, Josephine F.W. Baggen, et al. “RUBIES: Evolved Stellar Populations with Extended Formation Histories at z ∼ 7-8 in Candidate Massive Galaxies Identified with JWST/NIRSpec.” <i>Astrophysical Journal Letters</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.3847/2041-8213/ad55f7\">https://doi.org/10.3847/2041-8213/ad55f7</a>."},"publication_status":"published","author":[{"first_name":"Bingjie","last_name":"Wang","full_name":"Wang, Bingjie"},{"full_name":"Leja, Joel","first_name":"Joel","last_name":"Leja"},{"full_name":"De Graaff, Anna","first_name":"Anna","last_name":"De Graaff"},{"first_name":"Gabriel B.","last_name":"Brammer","full_name":"Brammer, Gabriel B."},{"full_name":"Weibel, Andrea","first_name":"Andrea","last_name":"Weibel"},{"full_name":"Van Dokkum, Pieter","first_name":"Pieter","last_name":"Van Dokkum"},{"first_name":"Josephine F.W.","last_name":"Baggen","full_name":"Baggen, Josephine F.W."},{"first_name":"Katherine A.","last_name":"Suess","full_name":"Suess, Katherine A."},{"first_name":"Jenny E.","last_name":"Greene","full_name":"Greene, Jenny E."},{"first_name":"Rachel","last_name":"Bezanson","full_name":"Bezanson, Rachel"},{"last_name":"Cleri","first_name":"Nikko J.","full_name":"Cleri, Nikko J."},{"last_name":"Hirschmann","first_name":"Michaela","full_name":"Hirschmann, Michaela"},{"full_name":"Labbé, Ivo","last_name":"Labbé","first_name":"Ivo"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"full_name":"Mcconachie, Ian","first_name":"Ian","last_name":"Mcconachie"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"first_name":"Erica","last_name":"Nelson","full_name":"Nelson, Erica"},{"first_name":"Pascal A.","last_name":"Oesch","full_name":"Oesch, Pascal A."},{"first_name":"David J.","last_name":"Setton","full_name":"Setton, David J."},{"full_name":"Williams, Christina C.","last_name":"Williams","first_name":"Christina C."}],"arxiv":1,"intvolume":"       969","department":[{"_id":"JoMa"}],"_id":"17234","oa_version":"Published Version","type":"journal_article"},{"month":"09","abstract":[{"text":"Observations of tidal disruption events (TDEs) show signs of nitrogen enrichment reminiscent of other astrophysical sources such as active galactic nuclei and star-forming galaxies. Given that TDEs probe the gas from a single star, it is possible to test whether the observed enrichment is consistent with expectations from the CNO cycle by looking at the observed nitrogen/carbon (N/C) abundance ratios. Given that ≈20% of solar-mass stars (and an even larger fraction of more massive stars) live in close binaries, it is worthwhile to also consider what TDEs from stars influenced by binary evolution would look like. We show here that TDEs from stars stripped of their hydrogen-rich (and nitrogen-poor) envelopes through previous binary-induced mass loss can produce much higher observable N/C enhancements than even TDEs from massive stars. Additionally, we predict that the time dependence of the N/C abundance ratio in the mass fallback rate of stripped stars will follow the inverse behavior of main-sequence stars, enabling a more accurate characterization of the disrupted star.","lang":"eng"}],"status":"public","article_type":"original","file_date_updated":"2024-09-30T08:54:26Z","publisher":"IOP Publishing","article_number":"L9","ddc":["520"],"oa":1,"date_created":"2024-09-22T22:01:42Z","quality_controlled":"1","volume":973,"article_processing_charge":"Yes","publication":"Astrophysical Journal Letters","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"DOAJ_listed":"1","day":"12","year":"2024","doi":"10.3847/2041-8213/ad6c34","date_updated":"2025-09-08T09:48:50Z","date_published":"2024-09-12T00:00:00Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file":[{"file_size":844227,"checksum":"050ddf873244839825714cca42b5d857","file_name":"2024_AstrophysicalJourn_Mockler.pdf","content_type":"application/pdf","date_updated":"2024-09-30T08:54:26Z","relation":"main_file","file_id":"18161","success":1,"creator":"dernst","date_created":"2024-09-30T08:54:26Z","access_level":"open_access"}],"external_id":{"isi":["001310592900001"]},"language":[{"iso":"eng"}],"acknowledgement":"This work was performed in part at Aspen Center for Physics, which is supported by National Science Foundation grant PHY-2210452. We thank the participants and organizers of the summer Aspen 2023 workshop on “Stellar Interactions and the Transients They Cause” for fruitful discussions. B.M. is grateful for support from the Carnegie Theoretical Astrophysics\r\nCenter. M.G.-G. is grateful for the support from Northwestern University’s Presidential Fellowship. E.R.-R. thanks the Heising-Simons Foundation, NSF (AST-2150255 and AST2307710), Swift (80NSSC21K1409, 80NSSC19K1391), and Chandra (22-0142) for support. ","isi":1,"issue":"1","has_accepted_license":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","scopus_import":"1","oa_version":"Published Version","type":"journal_article","department":[{"_id":"YlGo"}],"intvolume":"       973","_id":"18111","title":"Tidal disruption events from stripped stars","author":[{"last_name":"Mockler","first_name":"Brenna","full_name":"Mockler, Brenna"},{"first_name":"Monica","last_name":"Gallegos-Garcia","full_name":"Gallegos-Garcia, Monica"},{"full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","first_name":"Ylva Louise Linsdotter"},{"full_name":"Miller, Jon M.","first_name":"Jon M.","last_name":"Miller"},{"last_name":"Ramirez-Ruiz","first_name":"Enrico","full_name":"Ramirez-Ruiz, Enrico"}],"publication_status":"published","citation":{"ama":"Mockler B, Gallegos-Garcia M, Götberg YLL, Miller JM, Ramirez-Ruiz E. Tidal disruption events from stripped stars. <i>Astrophysical Journal Letters</i>. 2024;973(1). doi:<a href=\"https://doi.org/10.3847/2041-8213/ad6c34\">10.3847/2041-8213/ad6c34</a>","apa":"Mockler, B., Gallegos-Garcia, M., Götberg, Y. L. L., Miller, J. M., &#38; Ramirez-Ruiz, E. (2024). Tidal disruption events from stripped stars. <i>Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ad6c34\">https://doi.org/10.3847/2041-8213/ad6c34</a>","ieee":"B. Mockler, M. Gallegos-Garcia, Y. L. L. Götberg, J. M. Miller, and E. Ramirez-Ruiz, “Tidal disruption events from stripped stars,” <i>Astrophysical Journal Letters</i>, vol. 973, no. 1. IOP Publishing, 2024.","mla":"Mockler, Brenna, et al. “Tidal Disruption Events from Stripped Stars.” <i>Astrophysical Journal Letters</i>, vol. 973, no. 1, L9, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/2041-8213/ad6c34\">10.3847/2041-8213/ad6c34</a>.","short":"B. Mockler, M. Gallegos-Garcia, Y.L.L. Götberg, J.M. Miller, E. Ramirez-Ruiz, Astrophysical Journal Letters 973 (2024).","chicago":"Mockler, Brenna, Monica Gallegos-Garcia, Ylva Louise Linsdotter Götberg, Jon M. Miller, and Enrico Ramirez-Ruiz. “Tidal Disruption Events from Stripped Stars.” <i>Astrophysical Journal Letters</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.3847/2041-8213/ad6c34\">https://doi.org/10.3847/2041-8213/ad6c34</a>.","ista":"Mockler B, Gallegos-Garcia M, Götberg YLL, Miller JM, Ramirez-Ruiz E. 2024. Tidal disruption events from stripped stars. Astrophysical Journal Letters. 973(1), L9."}},{"acknowledgement":"The research described in this Letter was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics Space Administration, © 2024. California Institute of Technology. Government sponsorship acknowledged. A.V.O. and J.V.S. thank M. Lendl for constraints and discussions on the mass of WASP-49 A b. S.G.S acknowledges the support from FCT through Investigador FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC).","language":[{"iso":"eng"}],"issue":"2","isi":1,"scopus_import":"1","has_accepted_license":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","year":"2024","day":"01","doi":"10.3847/2041-8213/ad6b29","date_updated":"2025-09-08T14:18:18Z","date_published":"2024-10-01T00:00:00Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"external_id":{"isi":["001322169500001"],"arxiv":["2409.19844"]},"file":[{"relation":"main_file","date_updated":"2024-10-21T11:05:11Z","content_type":"application/pdf","file_name":"2024_AstrophysicalJourn_Oza.pdf","checksum":"23eea2a6a0519694a84998957ad7b7fb","file_size":1249747,"access_level":"open_access","date_created":"2024-10-21T11:05:11Z","creator":"dernst","success":1,"file_id":"18456"}],"arxiv":1,"title":"Redshifted sodium transient near exoplanet transit","OA_place":"publisher","citation":{"ieee":"A. V. Oza <i>et al.</i>, “Redshifted sodium transient near exoplanet transit,” <i>Astrophysical Journal Letters</i>, vol. 973, no. 2. IOP Publishing, 2024.","apa":"Oza, A. V., Seidel, J. V., Hoeijmakers, H. J., Unni, A., Kesseli, A. Y., Schmidt, C. A., … Johnson, R. E. (2024). Redshifted sodium transient near exoplanet transit. <i>Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ad6b29\">https://doi.org/10.3847/2041-8213/ad6b29</a>","ama":"Oza AV, Seidel JV, Hoeijmakers HJ, et al. Redshifted sodium transient near exoplanet transit. <i>Astrophysical Journal Letters</i>. 2024;973(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/ad6b29\">10.3847/2041-8213/ad6b29</a>","mla":"Oza, Apurva V., et al. “Redshifted Sodium Transient near Exoplanet Transit.” <i>Astrophysical Journal Letters</i>, vol. 973, no. 2, L53, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/2041-8213/ad6b29\">10.3847/2041-8213/ad6b29</a>.","ista":"Oza AV, Seidel JV, Hoeijmakers HJ, Unni A, Kesseli AY, Schmidt CA, Sivarani T, Bello-Arufe A, Gebek A, Meyer Zu Westram M, Sousa SG, Lopes RMC, Hu R, De Kleer K, Fisher C, Charnoz S, Baker AD, Halverson SP, Schneider NM, Psaridi A, Wyttenbach A, Torres Rodriguez S, Bhatnagar I, Johnson RE. 2024. Redshifted sodium transient near exoplanet transit. Astrophysical Journal Letters. 973(2), L53.","chicago":"Oza, Apurva V., Julia V. Seidel, H. Jens Hoeijmakers, Athira Unni, Aurora Y. Kesseli, Carl A. Schmidt, Thirupathi Sivarani, et al. “Redshifted Sodium Transient near Exoplanet Transit.” <i>Astrophysical Journal Letters</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.3847/2041-8213/ad6b29\">https://doi.org/10.3847/2041-8213/ad6b29</a>.","short":"A.V. Oza, J.V. Seidel, H.J. Hoeijmakers, A. Unni, A.Y. Kesseli, C.A. Schmidt, T. Sivarani, A. Bello-Arufe, A. Gebek, M. Meyer Zu Westram, S.G. Sousa, R.M.C. Lopes, R. Hu, K. De Kleer, C. Fisher, S. Charnoz, A.D. Baker, S.P. Halverson, N.M. Schneider, A. Psaridi, A. Wyttenbach, S. Torres Rodriguez, I. Bhatnagar, R.E. Johnson, Astrophysical Journal Letters 973 (2024)."},"publication_status":"published","author":[{"last_name":"Oza","first_name":"Apurva V.","full_name":"Oza, Apurva V."},{"full_name":"Seidel, Julia V.","first_name":"Julia V.","last_name":"Seidel"},{"first_name":"H. Jens","last_name":"Hoeijmakers","full_name":"Hoeijmakers, H. Jens"},{"first_name":"Athira","last_name":"Unni","full_name":"Unni, Athira"},{"full_name":"Kesseli, Aurora Y.","first_name":"Aurora Y.","last_name":"Kesseli"},{"first_name":"Carl A.","last_name":"Schmidt","full_name":"Schmidt, Carl A."},{"full_name":"Sivarani, Thirupathi","first_name":"Thirupathi","last_name":"Sivarani"},{"full_name":"Bello-Arufe, Aaron","last_name":"Bello-Arufe","first_name":"Aaron"},{"last_name":"Gebek","first_name":"Andrea","full_name":"Gebek, Andrea"},{"full_name":"Meyer Zu Westram, Moritz","last_name":"Meyer Zu Westram","first_name":"Moritz"},{"last_name":"Sousa","first_name":"Sérgio G.","full_name":"Sousa, Sérgio G."},{"first_name":"Rosaly M.C.","last_name":"Lopes","full_name":"Lopes, Rosaly M.C."},{"full_name":"Hu, Renyu","last_name":"Hu","first_name":"Renyu"},{"first_name":"Katherine","last_name":"De Kleer","full_name":"De Kleer, Katherine"},{"full_name":"Fisher, Chloe","first_name":"Chloe","last_name":"Fisher"},{"last_name":"Charnoz","first_name":"Sébastien","full_name":"Charnoz, Sébastien"},{"full_name":"Baker, Ashley D.","first_name":"Ashley D.","last_name":"Baker"},{"full_name":"Halverson, Samuel P.","first_name":"Samuel P.","last_name":"Halverson"},{"first_name":"Nick M.","last_name":"Schneider","full_name":"Schneider, Nick M."},{"first_name":"Angelica","last_name":"Psaridi","full_name":"Psaridi, Angelica"},{"first_name":"Aurélien","last_name":"Wyttenbach","full_name":"Wyttenbach, Aurélien"},{"orcid":"0000-0002-3150-8988","full_name":"Torres Rodriguez, Santiago","id":"a8df4360-4328-11ee-8f1a-e502d0c83fc2","last_name":"Torres Rodriguez","first_name":"Santiago"},{"first_name":"Ishita","last_name":"Bhatnagar","full_name":"Bhatnagar, Ishita"},{"full_name":"Johnson, Robert E.","last_name":"Johnson","first_name":"Robert E."}],"oa_version":"Published Version","type":"journal_article","department":[{"_id":"LiBu"}],"intvolume":"       973","_id":"18306","publisher":"IOP Publishing","article_type":"original","file_date_updated":"2024-10-21T11:05:11Z","article_number":"L53","ddc":["520"],"quality_controlled":"1","date_created":"2024-10-13T22:01:49Z","oa":1,"OA_type":"gold","article_processing_charge":"Yes","volume":973,"month":"10","status":"public","abstract":[{"text":"Neutral sodium (Na i) is an alkali metal with a favorable absorption cross section such that tenuous gases are easily illuminated at select transiting exoplanet systems. We examine both the time-averaged and time-series alkali spectral flux individually, over 4 nights at a hot Saturn system on a ∼2.8 day orbit about a Sun-like star WASP-49 A. Very Large Telescope/ESPRESSO observations are analyzed, providing new constraints. We recover the previously confirmed residual sodium flux uniquely when averaged, whereas night-to-night Na i varies by more than an order of magnitude. On HARPS/3.6 m Epoch II, we report a Doppler redshift at vΓ,NaD = + 9.7 ± 1.6 km s−1 with respect to the planet's rest frame. Upon examining the lightcurves, we confirm night-to-night variability, on the order of ∼1%–4% in NaD, rarely coinciding with exoplanet transit, not readily explained by stellar activity, starspots, tellurics, or the interstellar medium. Coincident with the ∼+10 km s−1 Doppler redshift, we detect a transient sodium absorption event dFNaD/F⋆ = 3.6% ± 1% at a relative difference of ΔFNaD(t) ∼ 4.4% ± 1%, lasting ΔtNaD ≳ 40 minutes. Since exoplanetary alkali signatures are blueshifted due to the natural vector of radiation pressure, estimated here at roughly ∼−5.7 km s−1, the radial velocity is rather at +15.4 km s−1, far larger than any known exoplanet system. Given that the redshift magnitude vΓ is in between the Roche limit and dynamically stable satellite orbits, the transient sodium may be a putative indication of a natural satellite orbiting WASP-49 A b.","lang":"eng"}],"publication":"Astrophysical Journal Letters","DOAJ_listed":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]}},{"DOAJ_listed":"1","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"publication":"The Astrophysical Journal Letters","month":"10","abstract":[{"lang":"eng","text":"The recently discovered Pa 30 nebula, the putative type Iax supernova remnant associated with the historical supernova of 1181 AD, shows puzzling characteristics that make it unique among known supernova remnants. In particular, Pa 30 exhibits a complex morphology, with a unique radial and filamentary structure, and it hosts a hot stellar remnant at its center, which displays oxygen-dominated, ultrafast winds. Because of the surviving stellar remnant and the lack of hydrogen and helium in its filaments, it has been suggested that Pa 30 is the product of a failed thermonuclear explosion in a near- or super-Chandrasekhar white dwarf, which created a subluminous transient, a rare subtype of the Ia class of supernovae called type Iax. We present here a detailed study of the 3D structure and velocities of a full radial section of the remnant. The Integral Field Unit observations, obtained with the new red channel of the Keck Cosmic Web Imager spectrograph, reveal that the ejecta are consistent with being ballistic, with velocities close to the free-expansion velocity. Additionally, we detect a large cavity inside the supernova remnant and a sharp inner edge to the filamentary structure, which coincides with the outer edge of a bright ring detected in infrared images. Finally, we detect a strong asymmetry in the amount of ejecta along the line of sight, which might hint at an asymmetric explosion. Our analysis provides strong confirmation that the explosion originated from SN 1181."}],"status":"public","oa":1,"date_created":"2024-11-19T08:12:59Z","OA_type":"gold","quality_controlled":"1","volume":975,"article_processing_charge":"Yes","article_type":"original","file_date_updated":"2024-11-20T12:24:52Z","publisher":"IOP Publishing","article_number":"L7","ddc":["520"],"intvolume":"       975","department":[{"_id":"IlCa"}],"das_tickbox":"1","_id":"18564","oa_version":"Published Version","type":"journal_article","title":"Expansion properties of the young supernova type Iax remnant Pa 30 revealed","author":[{"first_name":"Tim","last_name":"Cunningham","full_name":"Cunningham, Tim"},{"full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","last_name":"Caiazzo"},{"full_name":"Prusinski, Nikolaus Z.","first_name":"Nikolaus Z.","last_name":"Prusinski"},{"full_name":"Fuller, James","last_name":"Fuller","first_name":"James"},{"first_name":"John C.","last_name":"Raymond","full_name":"Raymond, John C."},{"last_name":"Kulkarni","first_name":"S. R.","full_name":"Kulkarni, S. R."},{"last_name":"Neill","first_name":"James D.","full_name":"Neill, James D."},{"last_name":"Duffell","first_name":"Paul","full_name":"Duffell, Paul"},{"full_name":"Martin, Chris","first_name":"Chris","last_name":"Martin"},{"full_name":"Toloza, Odette","first_name":"Odette","last_name":"Toloza"},{"first_name":"David","last_name":"Charbonneau","full_name":"Charbonneau, David"},{"first_name":"Scott J.","last_name":"Kenyon","full_name":"Kenyon, Scott J."},{"full_name":"Lin, Zeren","last_name":"Lin","first_name":"Zeren"},{"full_name":"Matuszewski, Mateusz","last_name":"Matuszewski","first_name":"Mateusz"},{"full_name":"McGurk, Rosalie","first_name":"Rosalie","last_name":"McGurk"},{"last_name":"Polin","first_name":"Abigail","full_name":"Polin, Abigail"},{"last_name":"Yao","first_name":"Philippe Z.","full_name":"Yao, Philippe Z."}],"publication_status":"published","citation":{"ieee":"T. Cunningham <i>et al.</i>, “Expansion properties of the young supernova type Iax remnant Pa 30 revealed,” <i>The Astrophysical Journal Letters</i>, vol. 975, no. 1. IOP Publishing, 2024.","apa":"Cunningham, T., Caiazzo, I., Prusinski, N. Z., Fuller, J., Raymond, J. C., Kulkarni, S. R., … Yao, P. Z. (2024). Expansion properties of the young supernova type Iax remnant Pa 30 revealed. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ad713b\">https://doi.org/10.3847/2041-8213/ad713b</a>","ama":"Cunningham T, Caiazzo I, Prusinski NZ, et al. Expansion properties of the young supernova type Iax remnant Pa 30 revealed. <i>The Astrophysical Journal Letters</i>. 2024;975(1). doi:<a href=\"https://doi.org/10.3847/2041-8213/ad713b\">10.3847/2041-8213/ad713b</a>","ista":"Cunningham T, Caiazzo I, Prusinski NZ, Fuller J, Raymond JC, Kulkarni SR, Neill JD, Duffell P, Martin C, Toloza O, Charbonneau D, Kenyon SJ, Lin Z, Matuszewski M, McGurk R, Polin A, Yao PZ. 2024. Expansion properties of the young supernova type Iax remnant Pa 30 revealed. The Astrophysical Journal Letters. 975(1), L7.","short":"T. Cunningham, I. Caiazzo, N.Z. Prusinski, J. Fuller, J.C. Raymond, S.R. Kulkarni, J.D. Neill, P. Duffell, C. Martin, O. Toloza, D. Charbonneau, S.J. Kenyon, Z. Lin, M. Matuszewski, R. McGurk, A. Polin, P.Z. Yao, The Astrophysical Journal Letters 975 (2024).","chicago":"Cunningham, Tim, Ilaria Caiazzo, Nikolaus Z. Prusinski, James Fuller, John C. Raymond, S. R. Kulkarni, James D. Neill, et al. “Expansion Properties of the Young Supernova Type Iax Remnant Pa 30 Revealed.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.3847/2041-8213/ad713b\">https://doi.org/10.3847/2041-8213/ad713b</a>.","mla":"Cunningham, Tim, et al. “Expansion Properties of the Young Supernova Type Iax Remnant Pa 30 Revealed.” <i>The Astrophysical Journal Letters</i>, vol. 975, no. 1, L7, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/2041-8213/ad713b\">10.3847/2041-8213/ad713b</a>."},"OA_place":"publisher","project":[{"_id":"B67AFEDC-15C9-11EA-A837-991A96BB2854","name":"IST Austria Open Access Fund"}],"arxiv":1,"date_published":"2024-10-24T00:00:00Z","date_updated":"2026-07-06T12:21:32Z","external_id":{"arxiv":["2410.10940"],"isi":["001340831400001"]},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file":[{"file_size":90328868,"content_type":"application/pdf","checksum":"51e790dd3d85ca984e656734f9f611da","file_name":"2024_AstrophysJourLetters_Cunningham.pdf","date_updated":"2024-11-20T12:24:52Z","relation":"main_file","file_id":"18573","success":1,"date_created":"2024-11-20T12:24:52Z","creator":"dernst","access_level":"open_access"}],"year":"2024","day":"24","doi":"10.3847/2041-8213/ad713b","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","scopus_import":"1","APC_amount":"3080,76 EUR","language":[{"iso":"eng"}],"acknowledgement":"We thank Rob Fesen for providing the [S ii] narrowband imaging and providing helpful comments on the Letter. We also thank Eliot Quartert for the helpful discussions. T.C. was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51527.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. I.C. was also supported by NASA through grants from the Space Telescope Science Institute, under NASA contracts NASA.22K1813, NAS5-26555, and NAS5-03127. This research was supported in part by grant NSF PHY-1748958 to the Kavli Institute for Theoretical Physics (KITP). O.T. was supported by FONDECYT grant 11241186.\r\n\r\nThis publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.\r\n\r\nThis research made use of Montage. It is funded by the National Science Foundation under grant No. ACI-1440620, and was previously funded by the National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology.","isi":1,"issue":"1"},{"publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"publication":"The Astrophysical Journal Letters","month":"10","status":"public","abstract":[{"text":"We searched the Gaia DR3 database for ultramassive white dwarfs with kinematics consistent with having escaped the nearby Hyades open cluster, identifying three such candidates. Two of these candidates have masses estimated from Gaia photometry of approximately 1.1 solar masses; their status as products of single-stellar evolution that have escaped the cluster was deemed too questionable for immediate follow-up analysis. The remaining candidate has an expected mass >1.3 solar masses, significantly reducing the probability of it being an interloper. Analysis of follow-up Gemini GMOS spectroscopy for this source reveals a nonmagnetized hydrogen atmosphere white dwarf with a mass and age consistent with having formed from a single star. Assuming a single-stellar-evolution formation channel, we estimate a 97.8% chance that the candidate is a true escapee from the Hyades. With a determined mass of 1.317 solar masses, this is potentially the most massive known single-evolution white dwarf and is by far the most massive with a strong association with an open cluster.","lang":"eng"}],"quality_controlled":"1","date_created":"2024-03-26T09:45:38Z","oa":1,"volume":956,"article_processing_charge":"No","publisher":"American Astronomical Society","article_type":"original","article_number":"L41","intvolume":"       956","_id":"15192","oa_version":"Published Version","type":"journal_article","extern":"1","title":"An extremely massive white dwarf escaped from the Hyades star cluster","author":[{"full_name":"Miller, David R.","last_name":"Miller","first_name":"David R."},{"full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","last_name":"Caiazzo"},{"last_name":"Heyl","first_name":"Jeremy","full_name":"Heyl, Jeremy"},{"full_name":"Richer, Harvey B.","first_name":"Harvey B.","last_name":"Richer"},{"full_name":"El-Badry, Kareem","first_name":"Kareem","last_name":"El-Badry"},{"full_name":"Rodriguez, Antonio C.","first_name":"Antonio C.","last_name":"Rodriguez"},{"first_name":"Zachary P.","last_name":"Vanderbosch","full_name":"Vanderbosch, Zachary P."},{"full_name":"van Roestel, Jan","last_name":"van Roestel","first_name":"Jan"}],"publication_status":"published","citation":{"ama":"Miller DR, Caiazzo I, Heyl J, et al. An extremely massive white dwarf escaped from the Hyades star cluster. <i>The Astrophysical Journal Letters</i>. 2023;956(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/acffc4\">10.3847/2041-8213/acffc4</a>","ieee":"D. R. Miller <i>et al.</i>, “An extremely massive white dwarf escaped from the Hyades star cluster,” <i>The Astrophysical Journal Letters</i>, vol. 956, no. 2. American Astronomical Society, 2023.","apa":"Miller, D. R., Caiazzo, I., Heyl, J., Richer, H. B., El-Badry, K., Rodriguez, A. C., … van Roestel, J. (2023). An extremely massive white dwarf escaped from the Hyades star cluster. <i>The Astrophysical Journal Letters</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/2041-8213/acffc4\">https://doi.org/10.3847/2041-8213/acffc4</a>","chicago":"Miller, David R., Ilaria Caiazzo, Jeremy Heyl, Harvey B. Richer, Kareem El-Badry, Antonio C. Rodriguez, Zachary P. Vanderbosch, and Jan van Roestel. “An Extremely Massive White Dwarf Escaped from the Hyades Star Cluster.” <i>The Astrophysical Journal Letters</i>. American Astronomical Society, 2023. <a href=\"https://doi.org/10.3847/2041-8213/acffc4\">https://doi.org/10.3847/2041-8213/acffc4</a>.","short":"D.R. Miller, I. Caiazzo, J. Heyl, H.B. Richer, K. El-Badry, A.C. Rodriguez, Z.P. Vanderbosch, J. van Roestel, The Astrophysical Journal Letters 956 (2023).","ista":"Miller DR, Caiazzo I, Heyl J, Richer HB, El-Badry K, Rodriguez AC, Vanderbosch ZP, van Roestel J. 2023. An extremely massive white dwarf escaped from the Hyades star cluster. The Astrophysical Journal Letters. 956(2), L41.","mla":"Miller, David R., et al. “An Extremely Massive White Dwarf Escaped from the Hyades Star Cluster.” <i>The Astrophysical Journal Letters</i>, vol. 956, no. 2, L41, American Astronomical Society, 2023, doi:<a href=\"https://doi.org/10.3847/2041-8213/acffc4\">10.3847/2041-8213/acffc4</a>."},"arxiv":1,"date_published":"2023-10-19T00:00:00Z","date_updated":"2024-04-02T06:56:01Z","external_id":{"arxiv":["2310.03204"]},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"year":"2023","day":"19","doi":"10.3847/2041-8213/acffc4","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"issue":"2","main_file_link":[{"open_access":"1","url":"https://doi.org/10.3847/2041-8213/acffc4"}]}]