[{"DOAJ_listed":"1","abstract":[{"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.","lang":"eng"}],"quality_controlled":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"date_published":"2026-01-10T00:00:00Z","external_id":{"arxiv":["2512.18565"]},"date_updated":"2026-04-16T06:26:18Z","title":"Formation of Be stars via wind accretion: Case study on Black Hole + Be star binaries","publication_status":"published","arxiv":1,"publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"publication":"The Astrophysical Journal Letters","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"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>.","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>","short":"Z. Li, S. Jia, D. Wei, H. Ge, H. Chen, Y. Zhang, X. Chen, Z. Han, The Astrophysical Journal Letters 996 (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>","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.","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.","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>."},"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.","type":"journal_article","OA_place":"publisher","file":[{"file_size":5202345,"file_id":"21741","checksum":"09200c1cf405101abdd298ce80c9a90d","content_type":"application/pdf","relation":"main_file","date_created":"2026-04-16T06:24:30Z","file_name":"2026_AstrophysicalJourLetters_Li.pdf","creator":"dernst","access_level":"open_access","success":1,"date_updated":"2026-04-16T06:24:30Z"}],"date_created":"2026-04-12T22:01:50Z","volume":996,"author":[{"full_name":"Li, Zhenwei","last_name":"Li","first_name":"Zhenwei"},{"first_name":"Shi","full_name":"Jia, Shi","last_name":"Jia"},{"full_name":"Wei, Dandan","last_name":"Wei","first_name":"Dandan","id":"5dd129bd-0601-11ef-b325-833284687b76"},{"last_name":"Ge","full_name":"Ge, Hongwei","first_name":"Hongwei"},{"first_name":"Hailiang","full_name":"Chen, Hailiang","last_name":"Chen"},{"full_name":"Zhang, Yangyang","last_name":"Zhang","first_name":"Yangyang"},{"first_name":"Xuefei","full_name":"Chen, Xuefei","last_name":"Chen"},{"first_name":"Zhanwen","full_name":"Han, Zhanwen","last_name":"Han"}],"intvolume":"       996","scopus_import":"1","doi":"10.3847/2041-8213/ae3008","article_number":"L42","oa_version":"Published Version","status":"public","_id":"21714","file_date_updated":"2026-04-16T06:24:30Z","ddc":["520"],"month":"01","oa":1,"license":"https://creativecommons.org/licenses/by/4.0/","language":[{"iso":"eng"}],"year":"2026","OA_type":"gold","department":[{"_id":"YlGo"}],"has_accepted_license":"1","article_processing_charge":"Yes","day":"10","issue":"2","publisher":"IOP Publishing","article_type":"original"},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"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>.","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.","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.","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>","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>.","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>"},"publication":"The Astrophysical Journal Letters","file":[{"file_id":"21784","file_size":2821786,"checksum":"1be4f361bf59aa08b8c98ed4f475a463","content_type":"application/pdf","relation":"main_file","date_created":"2026-05-04T07:11:37Z","file_name":"2026_AstrophysicalJourLetters_Hviding.pdf","creator":"dernst","access_level":"open_access","success":1,"date_updated":"2026-05-04T07:11:37Z"}],"type":"journal_article","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).","OA_place":"publisher","date_published":"2026-03-20T00:00:00Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"external_id":{"arxiv":["2601.09778"]},"date_updated":"2026-05-04T07:13:07Z","title":"The X-ray dot: Exotic dust or a late-stage Little Red Dot?","publication_status":"published","DOAJ_listed":"1","quality_controlled":"1","abstract":[{"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.","lang":"eng"}],"publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"arxiv":1,"language":[{"iso":"eng"}],"year":"2026","OA_type":"gold","day":"20","issue":"1","publisher":"IOP Publishing","article_type":"original","department":[{"_id":"JoMa"}],"has_accepted_license":"1","article_processing_charge":"Yes","intvolume":"      1000","scopus_import":"1","doi":"10.3847/2041-8213/ae4c88","date_created":"2026-04-12T22:01:48Z","volume":1000,"author":[{"first_name":"Raphael E.","full_name":"Hviding, Raphael E.","last_name":"Hviding"},{"first_name":"Anna","last_name":"De Graaff","full_name":"De Graaff, Anna"},{"last_name":"Liu","full_name":"Liu, Hanpu","first_name":"Hanpu"},{"last_name":"Goulding","full_name":"Goulding, Andy D.","first_name":"Andy D."},{"first_name":"Yilun","last_name":"Ma","full_name":"Ma, Yilun"},{"first_name":"Jenny E.","last_name":"Greene","full_name":"Greene, Jenny E."},{"first_name":"Leindert A.","last_name":"Boogaard","full_name":"Boogaard, Leindert A."},{"last_name":"Bunker","full_name":"Bunker, Andrew J.","first_name":"Andrew J."},{"first_name":"Nikko J.","last_name":"Cleri","full_name":"Cleri, Nikko J."},{"first_name":"Marijn","full_name":"Franx, Marijn","last_name":"Franx"},{"full_name":"Hirschmann, Michaela","last_name":"Hirschmann","first_name":"Michaela"},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."},{"first_name":"David J.","full_name":"Setton, David J.","last_name":"Setton"},{"full_name":"Übler, Hannah","last_name":"Übler","first_name":"Hannah"},{"last_name":"Venturi","full_name":"Venturi, Giacomo","first_name":"Giacomo"},{"last_name":"Wang","full_name":"Wang, Bingjie","first_name":"Bingjie"}],"month":"03","oa":1,"article_number":"L18","oa_version":"Published Version","status":"public","file_date_updated":"2026-05-04T07:11:37Z","_id":"21709","ddc":["520"]},{"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"external_id":{"arxiv":["2508.08558"]},"date_published":"2026-01-10T00:00:00Z","publication_status":"published","title":"Accretion is all you need: Black Hole spin alignment in merger GW231123 indicates accretion pathway","date_updated":"2026-05-04T09:54:18Z","DOAJ_listed":"1","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"}],"quality_controlled":"1","corr_author":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"arxiv":1,"citation":{"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>","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>.","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.","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>.","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>"},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"The Astrophysical Journal Letters","file":[{"relation":"main_file","content_type":"application/pdf","checksum":"ac46ba3d13f0150ccbc42665bed3ae47","file_size":866725,"file_id":"21788","success":1,"date_updated":"2026-05-04T09:49:53Z","creator":"dernst","access_level":"open_access","file_name":"2026_AstrophysicalJourLetters_Bartos.pdf","date_created":"2026-05-04T09:49:53Z"}],"OA_place":"publisher","type":"journal_article","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.","intvolume":"       996","doi":"10.3847/2041-8213/ae2bff","scopus_import":"1","volume":996,"date_created":"2026-04-12T22:01:49Z","author":[{"last_name":"Bartos","full_name":"Bartos, Imre","first_name":"Imre"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","full_name":"Haiman, Zoltán","last_name":"Haiman","orcid":"0000-0003-3633-5403"}],"month":"01","oa":1,"article_number":"L44","_id":"21713","ddc":["520"],"file_date_updated":"2026-05-04T09:49:53Z","status":"public","oa_version":"Published Version","year":"2026","language":[{"iso":"eng"}],"OA_type":"gold","day":"10","issue":"2","article_type":"original","publisher":"IOP Publishing","department":[{"_id":"ZoHa"}],"article_processing_charge":"Yes","has_accepted_license":"1"},{"article_type":"original","publisher":"IOP Publishing","day":"10","issue":"1","article_processing_charge":"Yes","has_accepted_license":"1","department":[{"_id":"ZoHa"},{"_id":"JoMa"}],"OA_type":"gold","year":"2026","language":[{"iso":"eng"}],"oa":1,"month":"04","_id":"21846","file_date_updated":"2026-05-11T06:44:37Z","ddc":["520"],"oa_version":"Published Version","status":"public","article_number":"L4","doi":"10.3847/2041-8213/ae58a5","scopus_import":"1","intvolume":"      1002","author":[{"first_name":"Josephine F.W.","last_name":"Baggen","full_name":"Baggen, Josephine F.W."},{"first_name":"Matthew T.","last_name":"Scoggins","full_name":"Scoggins, Matthew T."},{"first_name":"Pieter","last_name":"Van Dokkum","full_name":"Van Dokkum, Pieter"},{"first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","orcid":"0000-0003-3633-5403","full_name":"Haiman, Zoltán","last_name":"Haiman"},{"first_name":"Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","orcid":"0000-0001-5586-6950","last_name":"Torralba Torregrosa","full_name":"Torralba Torregrosa, Alberto"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"}],"volume":1002,"date_created":"2026-05-10T22:02:15Z","file":[{"date_created":"2026-05-11T06:44:37Z","file_name":"2026_AstrophysicalJourLetters_Baggen.pdf","creator":"dernst","access_level":"open_access","success":1,"date_updated":"2026-05-11T06:44:37Z","file_size":13359642,"file_id":"21851","checksum":"8c31d8603cd6ad39c772a72d136dc3f8","content_type":"application/pdf","relation":"main_file"}],"OA_place":"publisher","type":"journal_article","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).","citation":{"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).","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>.","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>","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.","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>.","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."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"The Astrophysical Journal Letters","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"PlanS_conform":"1","arxiv":1,"project":[{"grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"title":"Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation","publication_status":"published","date_updated":"2026-05-11T06:48:33Z","external_id":{"arxiv":["2602.02702"]},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"date_published":"2026-04-10T00:00:00Z","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"}],"quality_controlled":"1","DOAJ_listed":"1"},{"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"date_published":"2025-07-10T00:00:00Z","external_id":{"isi":["001524847100001"],"arxiv":["2505.01499"]},"isi":1,"publication_status":"published","title":"An extremely metal-poor Lyα emitter candidate at z = 6 revealed through absorption spectroscopy","date_updated":"2026-02-16T12:44:23Z","DOAJ_listed":"1","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"}],"quality_controlled":"1","PlanS_conform":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"arxiv":1,"citation":{"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>","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.","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>.","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>.","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>","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)."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"The Astrophysical Journal Letters","file":[{"checksum":"75d0c08514209fc6e3078fdec8e815a2","relation":"main_file","content_type":"application/pdf","file_size":6453728,"file_id":"20066","creator":"dernst","access_level":"open_access","date_updated":"2025-07-22T08:38:14Z","success":1,"file_name":"2025_AstrophysicalJourLetters_Durovcikova.pdf","date_created":"2025-07-22T08:38:14Z"}],"OA_place":"publisher","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.","type":"journal_article","intvolume":"       987","doi":"10.3847/2041-8213/ade71c","scopus_import":"1","volume":987,"date_created":"2025-07-20T22:02:01Z","author":[{"first_name":"Dominika","last_name":"Ďurovčíková","full_name":"Ďurovčíková, Dominika"},{"last_name":"Eilers","full_name":"Eilers, Anna Christina","first_name":"Anna Christina"},{"first_name":"Robert A.","full_name":"Simcoe, Robert A.","last_name":"Simcoe"},{"first_name":"Louise","full_name":"Welsh, Louise","last_name":"Welsh"},{"last_name":"Meyer","full_name":"Meyer, Romain A.","first_name":"Romain A."},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"last_name":"Ryan-Weber","full_name":"Ryan-Weber, Emma V.","first_name":"Emma V."},{"first_name":"Minghao","full_name":"Yue, Minghao","last_name":"Yue"},{"full_name":"Katz, Harley","last_name":"Katz","first_name":"Harley"},{"first_name":"Sindhu","full_name":"Satyavolu, Sindhu","last_name":"Satyavolu"},{"last_name":"Becker","full_name":"Becker, George","first_name":"George"},{"first_name":"Frederick B.","full_name":"Davies, Frederick B.","last_name":"Davies"},{"full_name":"Farina, Emanuele Paolo","last_name":"Farina","first_name":"Emanuele Paolo"}],"month":"07","oa":1,"article_number":"L33","_id":"20030","file_date_updated":"2025-07-22T08:38:14Z","ddc":["520"],"oa_version":"Published Version","status":"public","year":"2025","language":[{"iso":"eng"}],"OA_type":"gold","day":"10","issue":"2","publisher":"IOP Publishing","article_type":"original","department":[{"_id":"JoMa"}],"article_processing_charge":"Yes","has_accepted_license":"1"},{"arxiv":1,"PlanS_conform":"1","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"DOAJ_listed":"1","abstract":[{"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.","lang":"eng"}],"quality_controlled":"1","isi":1,"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"external_id":{"arxiv":["2509.05417"],"isi":["001581023000001"]},"date_published":"2025-09-25T00:00:00Z","date_updated":"2026-02-16T12:44:42Z","publication_status":"published","project":[{"grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"title":"The light echo of a high-redshift quasar mapped with Lyα tomography","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).","type":"journal_article","OA_place":"publisher","file":[{"creator":"dernst","access_level":"open_access","date_updated":"2025-10-13T09:25:12Z","success":1,"file_name":"2025_AstrophysicalJour_Eilers.pdf","date_created":"2025-10-13T09:25:12Z","checksum":"3cb8099b9a915755164e5675b33f8a03","relation":"main_file","content_type":"application/pdf","file_id":"20461","file_size":23585591}],"publication":"The Astrophysical Journal Letters","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"mla":"Eilers, Anna Christina, et al. “The Light Echo of a High-Redshift Quasar Mapped with Lyα Tomography.” <i>The Astrophysical Journal Letters</i>, vol. 991, no. 2, L40, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/2041-8213/ae057a\">10.3847/2041-8213/ae057a</a>.","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.","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.","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>","short":"A.C. Eilers, M. Yue, J.J. Matthee, J.F. Hennawi, F.B. Davies, R.A. Simcoe, R. Teague, R. Bordoloi, G. Brammer, Y. Kang, D. Kashino, R. Mackenzie, R.P. Naidu, B. Navarrete, The Astrophysical Journal Letters 991 (2025).","chicago":"Eilers, Anna Christina, Minghao Yue, Jorryt J Matthee, Joseph F. Hennawi, Frederick B. Davies, Robert A. Simcoe, Richard Teague, et al. “The Light Echo of a High-Redshift Quasar Mapped with Lyα Tomography.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/2041-8213/ae057a\">https://doi.org/10.3847/2041-8213/ae057a</a>.","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>"},"article_number":"L40","oa_version":"Published Version","status":"public","_id":"20425","ddc":["520"],"file_date_updated":"2025-10-13T09:25:12Z","month":"09","oa":1,"date_created":"2025-10-05T22:01:35Z","volume":991,"author":[{"first_name":"Anna Christina","last_name":"Eilers","full_name":"Eilers, Anna Christina"},{"full_name":"Yue, Minghao","last_name":"Yue","first_name":"Minghao"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"full_name":"Hennawi, Joseph F.","last_name":"Hennawi","first_name":"Joseph F."},{"last_name":"Davies","full_name":"Davies, Frederick B.","first_name":"Frederick B."},{"first_name":"Robert A.","full_name":"Simcoe, Robert A.","last_name":"Simcoe"},{"first_name":"Richard","last_name":"Teague","full_name":"Teague, Richard"},{"full_name":"Bordoloi, Rongmon","last_name":"Bordoloi","first_name":"Rongmon"},{"first_name":"Gabriel","last_name":"Brammer","full_name":"Brammer, Gabriel"},{"first_name":"Yi","last_name":"Kang","full_name":"Kang, Yi"},{"last_name":"Kashino","full_name":"Kashino, Daichi","first_name":"Daichi"},{"first_name":"Ruari","last_name":"Mackenzie","full_name":"Mackenzie, Ruari"},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"first_name":"Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","last_name":"Navarrete","full_name":"Navarrete, Benjamín"}],"intvolume":"       991","scopus_import":"1","doi":"10.3847/2041-8213/ae057a","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"has_accepted_license":"1","article_processing_charge":"Yes","day":"25","issue":"2","publisher":"IOP Publishing","article_type":"original","language":[{"iso":"eng"}],"year":"2025","OA_type":"gold"},{"OA_type":"gold","year":"2025","language":[{"iso":"eng"}],"article_processing_charge":"Yes","has_accepted_license":"1","department":[{"_id":"ZoHa"}],"publisher":"IOP Publishing","article_type":"original","issue":"1","day":"10","author":[{"first_name":"Smadar","full_name":"Naoz, Smadar","last_name":"Naoz"},{"last_name":"Haiman","full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán"},{"first_name":"Eliot","last_name":"Quataert","full_name":"Quataert, Eliot"},{"first_name":"Liz","last_name":"Holzknecht","full_name":"Holzknecht, Liz"}],"volume":992,"date_created":"2025-10-19T22:01:31Z","doi":"10.3847/2041-8213/ae0a20","scopus_import":"1","intvolume":"       992","file_date_updated":"2025-10-23T09:09:30Z","_id":"20493","ddc":["520"],"status":"public","oa_version":"Published Version","article_number":"L12","oa":1,"month":"10","publication":"The Astrophysical Journal Letters","citation":{"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>","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.","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.","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>","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)."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","OA_place":"publisher","type":"journal_article","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.","file":[{"file_id":"20520","file_size":8787316,"checksum":"cb81d666f6d7638a5bcf45653d25bcb3","relation":"main_file","content_type":"application/pdf","file_name":"2025_AstrophysicalJour_Naoz.pdf","date_created":"2025-10-23T09:09:30Z","creator":"dernst","access_level":"open_access","date_updated":"2025-10-23T09:09:30Z","success":1}],"quality_controlled":"1","abstract":[{"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.","lang":"eng"}],"DOAJ_listed":"1","publication_status":"published","title":"Triples as links between binary Black Hole mergers, their electromagnetic counterparts, and galactic Black Holes","date_updated":"2026-02-16T12:44:56Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"external_id":{"isi":["001589455900001"],"arxiv":["2508.13270"]},"isi":1,"date_published":"2025-10-10T00:00:00Z","arxiv":1,"publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"PlanS_conform":"1"},{"article_processing_charge":"Yes","has_accepted_license":"1","department":[{"_id":"JoMa"}],"article_type":"original","publisher":"IOP Publishing","day":"01","issue":"1","OA_type":"gold","year":"2025","language":[{"iso":"eng"}],"file_date_updated":"2025-11-24T13:18:34Z","_id":"20649","ddc":["520"],"oa_version":"Published Version","status":"public","article_number":"L12","oa":1,"month":"11","author":[{"first_name":"Minghao","full_name":"Yue, Minghao","last_name":"Yue"},{"first_name":"Anna Christina","full_name":"Eilers, Anna Christina","last_name":"Eilers"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"last_name":"Bordoloi","full_name":"Bordoloi, Rongmon","first_name":"Rongmon"},{"first_name":"Frederick B.","full_name":"Davies, Frederick B.","last_name":"Davies"},{"full_name":"Hennawi, Joseph F.","last_name":"Hennawi","first_name":"Joseph F."},{"full_name":"Kashino, Daichi","last_name":"Kashino","first_name":"Daichi"},{"last_name":"Mackenzie","full_name":"Mackenzie, Ruari","first_name":"Ruari"},{"full_name":"Simcoe, Robert A.","last_name":"Simcoe","first_name":"Robert A."}],"volume":993,"date_created":"2025-11-16T23:01:24Z","doi":"10.3847/2041-8213/ae0e0e","scopus_import":"1","intvolume":"       993","OA_place":"publisher","type":"journal_article","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.","file":[{"file_size":39736710,"file_id":"20680","checksum":"11d35c1c52c000f8c14bc6de2e9f4b3f","relation":"main_file","content_type":"application/pdf","file_name":"2025_AstrophysicalJour_Yue.pdf","date_created":"2025-11-24T13:18:34Z","access_level":"open_access","creator":"dernst","date_updated":"2025-11-24T13:18:34Z","success":1}],"publication":"The Astrophysical Journal Letters","citation":{"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>","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.","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>.","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.","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>","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)."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"PlanS_conform":"1","abstract":[{"lang":"eng","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."}],"quality_controlled":"1","DOAJ_listed":"1","title":"Escape fractions from unattenuated Lyα emitters around luminous z > 6 quasars","publication_status":"published","date_updated":"2026-02-16T12:45:16Z","date_published":"2025-11-01T00:00:00Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"isi":1,"external_id":{"isi":["001600890100001"],"arxiv":["2507.05381"]}},{"month":"04","oa":1,"article_number":"L37","oa_version":"Published Version","status":"public","_id":"19638","file_date_updated":"2025-05-05T11:30:34Z","ddc":["520"],"intvolume":"       983","scopus_import":"1","doi":"10.3847/2041-8213/adc680","date_created":"2025-05-04T22:02:31Z","volume":983,"author":[{"last_name":"Hu","full_name":"Hu, Haojie","first_name":"Haojie"},{"last_name":"Inayoshi","full_name":"Inayoshi, Kohei","first_name":"Kohei"},{"last_name":"Haiman","full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán"},{"first_name":"Luis C.","last_name":"Ho","full_name":"Ho, Luis C."},{"last_name":"Ohsuga","full_name":"Ohsuga, Ken","first_name":"Ken"}],"issue":"2","day":"20","article_type":"letter_note","publisher":"IOP Publishing","department":[{"_id":"ZoHa"}],"has_accepted_license":"1","article_processing_charge":"Yes","language":[{"iso":"eng"}],"year":"2025","OA_type":"gold","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"arxiv":1,"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"external_id":{"arxiv":["2503.03870"],"isi":["001467616800001"]},"date_published":"2025-04-20T00:00:00Z","isi":1,"date_updated":"2026-02-16T12:44:04Z","publication_status":"published","title":"The convergence of heavy and light seeds to overmassive black holes at cosmic dawn","DOAJ_listed":"1","quality_controlled":"1","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."}],"file":[{"creator":"dernst","access_level":"open_access","success":1,"date_updated":"2025-05-05T11:30:34Z","file_name":"2025_AstrophysicalJourLetters_Hu.pdf","date_created":"2025-05-05T11:30:34Z","checksum":"1a4fbeeb12e9022873e86c72d230a5ec","relation":"main_file","content_type":"application/pdf","file_size":3334014,"file_id":"19655"}],"type":"journal_article","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.","OA_place":"publisher","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"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>","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.","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.","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>","short":"H. Hu, K. Inayoshi, Z. Haiman, L.C. Ho, K. Ohsuga, The Astrophysical Journal Letters 983 (2025)."},"publication":"The Astrophysical Journal Letters"},{"PlanS_conform":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"arxiv":1,"external_id":{"arxiv":["2503.02059"]},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"date_published":"2025-09-12T00:00:00Z","date_updated":"2026-02-09T07:14:08Z","publication_status":"published","title":"A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots","DOAJ_listed":"1","quality_controlled":"1","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."}],"file":[{"creator":"dernst","access_level":"open_access","success":1,"date_updated":"2026-02-09T07:10:29Z","file_name":"2025_AstrophysicalJournalLetters_Setton.pdf","date_created":"2026-02-09T07:10:29Z","checksum":"799518db92ded4e166df4234195af998","relation":"main_file","content_type":"application/pdf","file_size":1394204,"file_id":"21165"}],"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.","type":"journal_article","OA_place":"publisher","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"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>.","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.","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.","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>","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).","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>","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>."},"publication":"The Astrophysical Journal Letters","month":"09","oa":1,"article_number":"L10","oa_version":"Published Version","status":"public","_id":"21058","file_date_updated":"2026-02-09T07:10:29Z","ddc":["520"],"intvolume":"       991","scopus_import":"1","doi":"10.3847/2041-8213/ade78b","date_created":"2026-01-28T15:23:00Z","volume":991,"author":[{"first_name":"David J.","last_name":"Setton","full_name":"Setton, David J."},{"last_name":"Greene","full_name":"Greene, Jenny E.","first_name":"Jenny E."},{"first_name":"Justin S.","full_name":"Spilker, Justin S.","last_name":"Spilker"},{"last_name":"Williams","full_name":"Williams, Christina C.","first_name":"Christina C."},{"full_name":"Labbé, Ivo","last_name":"Labbé","first_name":"Ivo"},{"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"},{"last_name":"Whitaker","full_name":"Whitaker, Katherine E.","first_name":"Katherine E."},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"last_name":"de Graaff","full_name":"de Graaff, Anna","first_name":"Anna"},{"full_name":"Alberts, Stacey","last_name":"Alberts","first_name":"Stacey"},{"first_name":"Rachel","full_name":"Bezanson, Rachel","last_name":"Bezanson"},{"full_name":"Boogaard, Leindert A.","last_name":"Boogaard","first_name":"Leindert A."},{"full_name":"Brammer, Gabriel","last_name":"Brammer","first_name":"Gabriel"},{"first_name":"Sam E.","last_name":"Cutler","full_name":"Cutler, Sam E."},{"full_name":"Cleri, Nikko J.","last_name":"Cleri","first_name":"Nikko J."},{"first_name":"Olivia R.","full_name":"Cooper, Olivia R.","last_name":"Cooper"},{"last_name":"Dayal","full_name":"Dayal, Pratika","first_name":"Pratika"},{"last_name":"Fujimoto","full_name":"Fujimoto, Seiji","first_name":"Seiji"},{"last_name":"Furtak","full_name":"Furtak, Lukas J.","first_name":"Lukas J."},{"full_name":"Goulding, Andy D.","last_name":"Goulding","first_name":"Andy D."},{"full_name":"Hirschmann, Michaela","last_name":"Hirschmann","first_name":"Michaela"},{"full_name":"Kokorev, Vasily","last_name":"Kokorev","first_name":"Vasily"},{"first_name":"Michael V.","full_name":"Maseda, Michael V.","last_name":"Maseda"},{"first_name":"Ian","full_name":"McConachie, Ian","last_name":"McConachie"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Miller, Tim B.","last_name":"Miller","first_name":"Tim B."},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."},{"first_name":"Pascal A.","last_name":"Oesch","full_name":"Oesch, Pascal A."},{"last_name":"Pan","full_name":"Pan, Richard","first_name":"Richard"},{"first_name":"Sedona H.","last_name":"Price","full_name":"Price, Sedona H."},{"first_name":"Katherine A.","full_name":"Suess, Katherine A.","last_name":"Suess"},{"first_name":"John R.","last_name":"Weaver","full_name":"Weaver, John R."},{"first_name":"Mengyuan","last_name":"Xiao","full_name":"Xiao, Mengyuan"},{"full_name":"Zhang, Yunchong","last_name":"Zhang","first_name":"Yunchong"},{"full_name":"Zitrin, Adi","last_name":"Zitrin","first_name":"Adi"}],"day":"12","article_type":"original","publisher":"IOP Publishing","department":[{"_id":"JoMa"}],"has_accepted_license":"1","article_processing_charge":"Yes","language":[{"iso":"eng"}],"year":"2025","OA_type":"gold"},{"file":[{"date_created":"2026-02-10T06:56:37Z","file_name":"2025_AstrophysicalJounalLetters_Silvermann.pdf","access_level":"open_access","creator":"dernst","success":1,"date_updated":"2026-02-10T06:56:37Z","file_id":"21202","file_size":997137,"checksum":"e38c0c444be9c1507eec28c62ce04cbc","content_type":"application/pdf","relation":"main_file"}],"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.","type":"journal_article","OA_place":"publisher","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","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>.","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.","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.","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>","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>.","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>"},"publication":"The Astrophysical Journal Letters","PlanS_conform":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"arxiv":1,"external_id":{"arxiv":["2507.23066"]},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"date_published":"2025-12-17T00:00:00Z","date_updated":"2026-02-10T07:02:39Z","title":"SHELLQs–JWST perspective on the intrinsic mass relation between supermassive black holes and their host galaxies at z > 6","publication_status":"published","DOAJ_listed":"1","abstract":[{"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.","lang":"eng"}],"quality_controlled":"1","day":"17","issue":"2","article_type":"original","publisher":"IOP Publishing","department":[{"_id":"ZoHa"}],"has_accepted_license":"1","article_processing_charge":"Yes","language":[{"iso":"eng"}],"year":"2025","OA_type":"gold","month":"12","oa":1,"article_number":"L67","status":"public","oa_version":"Published Version","file_date_updated":"2026-02-10T06:56:37Z","_id":"21121","ddc":["520"],"intvolume":"       995","doi":"10.3847/2041-8213/ae279c","date_created":"2026-01-31T09:27:53Z","volume":995,"author":[{"last_name":"Silverman","full_name":"Silverman, John David","first_name":"John David"},{"first_name":"Junyao","last_name":"Li","full_name":"Li, Junyao"},{"first_name":"Xuheng","full_name":"Ding, Xuheng","last_name":"Ding"},{"last_name":"Onoue","full_name":"Onoue, Masafusa","first_name":"Masafusa"},{"first_name":"Michael A.","last_name":"Strauss","full_name":"Strauss, Michael A."},{"first_name":"Yoshiki","last_name":"Matsuoka","full_name":"Matsuoka, Yoshiki"},{"first_name":"Takuma","last_name":"Izumi","full_name":"Izumi, Takuma"},{"full_name":"Jahnke, Knud","last_name":"Jahnke","first_name":"Knud"},{"first_name":"Tommaso","full_name":"Treu, Tommaso","last_name":"Treu"},{"last_name":"Volonteri","full_name":"Volonteri, Marta","first_name":"Marta"},{"full_name":"Phillips, Camryn L.","last_name":"Phillips","first_name":"Camryn L."},{"full_name":"Andika, Irham T.","last_name":"Andika","first_name":"Irham T."},{"full_name":"Aoki, Kentaro","last_name":"Aoki","first_name":"Kentaro"},{"last_name":"Arita","full_name":"Arita, Junya","first_name":"Junya"},{"first_name":"Shunsuke","full_name":"Baba, Shunsuke","last_name":"Baba"},{"first_name":"Sarah E. I.","full_name":"Bosman, Sarah E. I.","last_name":"Bosman"},{"full_name":"Eilers, Anna-Christina","last_name":"Eilers","first_name":"Anna-Christina"},{"first_name":"Xiaohui","full_name":"Fan, Xiaohui","last_name":"Fan"},{"first_name":"Seiji","last_name":"Fujimoto","full_name":"Fujimoto, Seiji"},{"first_name":"Melanie","full_name":"Habouzit, Melanie","last_name":"Habouzit"},{"first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","orcid":"0000-0003-3633-5403","last_name":"Haiman","full_name":"Haiman, Zoltán"},{"first_name":"Masatoshi","last_name":"Imanishi","full_name":"Imanishi, Masatoshi"},{"last_name":"Inayoshi","full_name":"Inayoshi, Kohei","first_name":"Kohei"},{"first_name":"Kazushi","last_name":"Iwasawa","full_name":"Iwasawa, Kazushi"},{"last_name":"Kashikawa","full_name":"Kashikawa, Nobunari","first_name":"Nobunari"},{"full_name":"Kawaguchi, Toshihiro","last_name":"Kawaguchi","first_name":"Toshihiro"},{"last_name":"Lee","full_name":"Lee, Chien-Hsiu","first_name":"Chien-Hsiu"},{"full_name":"Lupi, Alessandro","last_name":"Lupi","first_name":"Alessandro"},{"full_name":"Nagao, Tohru","last_name":"Nagao","first_name":"Tohru"},{"first_name":"Jan-Torge","last_name":"Schindler","full_name":"Schindler, Jan-Torge"},{"first_name":"Malte","full_name":"Schramm, Malte","last_name":"Schramm"},{"full_name":"Shimasaku, Kazuhiro","last_name":"Shimasaku","first_name":"Kazuhiro"},{"first_name":"Yoshiki","last_name":"Toba","full_name":"Toba, Yoshiki"},{"first_name":"Benny","last_name":"Trakhtenbrot","full_name":"Trakhtenbrot, Benny"},{"first_name":"Hideki","last_name":"Umehata","full_name":"Umehata, Hideki"},{"last_name":"Vestergaard","full_name":"Vestergaard, Marianne","first_name":"Marianne"},{"first_name":"Fabian","last_name":"Walter","full_name":"Walter, Fabian"},{"first_name":"Feige","full_name":"Wang, Feige","last_name":"Wang"},{"first_name":"Jinyi","full_name":"Yang, Jinyi","last_name":"Yang"}]},{"day":"08","issue":"2","publisher":"IOP Publishing","article_type":"original","department":[{"_id":"IlCa"}],"article_processing_charge":"Yes","has_accepted_license":"1","year":"2025","language":[{"iso":"eng"}],"OA_type":"gold","month":"09","oa":1,"article_number":"L57","_id":"21317","file_date_updated":"2026-02-19T07:24:10Z","ddc":["520"],"status":"public","oa_version":"Published Version","intvolume":"       990","doi":"10.3847/2041-8213/adff82","scopus_import":"1","volume":990,"date_created":"2026-02-18T10:17:04Z","author":[{"last_name":"Galiullin","full_name":"Galiullin, Ilkham","first_name":"Ilkham"},{"last_name":"Rodriguez","full_name":"Rodriguez, Antonio C.","first_name":"Antonio C."},{"last_name":"El-Badry","full_name":"El-Badry, Kareem","first_name":"Kareem"},{"first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","orcid":"0000-0002-4770-5388","last_name":"Caiazzo","full_name":"Caiazzo, Ilaria"},{"first_name":"Paula","last_name":"Szkody","full_name":"Szkody, Paula"},{"first_name":"Pranav","full_name":"Nagarajan, Pranav","last_name":"Nagarajan"},{"last_name":"Whitebook","full_name":"Whitebook, Samuel","first_name":"Samuel"}],"file":[{"access_level":"open_access","creator":"dernst","success":1,"date_updated":"2026-02-19T07:24:10Z","date_created":"2026-02-19T07:24:10Z","file_name":"2025_AstrophysicalJournal_Galiullin.pdf","checksum":"f76556d129aa0e9facc85602b0b5b54d","content_type":"application/pdf","relation":"main_file","file_size":3772189,"file_id":"21329"}],"OA_place":"publisher","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.","type":"journal_article","citation":{"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.","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>","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>.","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.","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)."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"The Astrophysical Journal Letters","PlanS_conform":"1","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"arxiv":1,"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"date_published":"2025-09-08T00:00:00Z","external_id":{"arxiv":["2508.20170"]},"title":"Optical spectroscopy of the most compact accreting binary harboring a magnetic White Dwarf and a hydrogen-rich donor","publication_status":"published","date_updated":"2026-02-19T07:27:01Z","DOAJ_listed":"1","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"}],"quality_controlled":"1"},{"language":[{"iso":"eng"}],"year":"2024","issue":"1","day":"12","article_type":"original","publisher":"IOP Publishing","department":[{"_id":"YlGo"}],"has_accepted_license":"1","article_processing_charge":"Yes","intvolume":"       973","scopus_import":"1","doi":"10.3847/2041-8213/ad6c34","date_created":"2024-09-22T22:01:42Z","volume":973,"author":[{"full_name":"Mockler, Brenna","last_name":"Mockler","first_name":"Brenna"},{"first_name":"Monica","last_name":"Gallegos-Garcia","full_name":"Gallegos-Garcia, Monica"},{"first_name":"Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","orcid":"0000-0002-6960-6911","last_name":"Götberg","full_name":"Götberg, Ylva Louise Linsdotter"},{"first_name":"Jon M.","full_name":"Miller, Jon M.","last_name":"Miller"},{"first_name":"Enrico","full_name":"Ramirez-Ruiz, Enrico","last_name":"Ramirez-Ruiz"}],"month":"09","oa":1,"article_number":"L9","status":"public","oa_version":"Published Version","ddc":["520"],"_id":"18111","file_date_updated":"2024-09-30T08:54:26Z","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","citation":{"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>.","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>","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>.","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.","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.","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>"},"publication":"Astrophysical Journal Letters","file":[{"date_created":"2024-09-30T08:54:26Z","file_name":"2024_AstrophysicalJourn_Mockler.pdf","date_updated":"2024-09-30T08:54:26Z","success":1,"creator":"dernst","access_level":"open_access","file_id":"18161","file_size":844227,"content_type":"application/pdf","relation":"main_file","checksum":"050ddf873244839825714cca42b5d857"}],"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. ","type":"journal_article","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"external_id":{"isi":["001310592900001"]},"date_published":"2024-09-12T00:00:00Z","isi":1,"date_updated":"2025-09-08T09:48:50Z","publication_status":"published","title":"Tidal disruption events from stripped stars","DOAJ_listed":"1","abstract":[{"lang":"eng","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."}],"quality_controlled":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]}},{"OA_type":"gold","language":[{"iso":"eng"}],"year":"2024","publisher":"IOP Publishing","article_type":"original","day":"01","issue":"2","has_accepted_license":"1","article_processing_charge":"Yes","department":[{"_id":"LiBu"}],"scopus_import":"1","doi":"10.3847/2041-8213/ad6b29","intvolume":"       973","author":[{"first_name":"Apurva V.","last_name":"Oza","full_name":"Oza, Apurva V."},{"last_name":"Seidel","full_name":"Seidel, Julia V.","first_name":"Julia V."},{"first_name":"H. Jens","full_name":"Hoeijmakers, H. Jens","last_name":"Hoeijmakers"},{"full_name":"Unni, Athira","last_name":"Unni","first_name":"Athira"},{"last_name":"Kesseli","full_name":"Kesseli, Aurora Y.","first_name":"Aurora Y."},{"full_name":"Schmidt, Carl A.","last_name":"Schmidt","first_name":"Carl A."},{"first_name":"Thirupathi","last_name":"Sivarani","full_name":"Sivarani, Thirupathi"},{"last_name":"Bello-Arufe","full_name":"Bello-Arufe, Aaron","first_name":"Aaron"},{"full_name":"Gebek, Andrea","last_name":"Gebek","first_name":"Andrea"},{"first_name":"Moritz","last_name":"Meyer Zu Westram","full_name":"Meyer Zu Westram, Moritz"},{"first_name":"Sérgio G.","full_name":"Sousa, Sérgio G.","last_name":"Sousa"},{"full_name":"Lopes, Rosaly M.C.","last_name":"Lopes","first_name":"Rosaly M.C."},{"first_name":"Renyu","full_name":"Hu, Renyu","last_name":"Hu"},{"first_name":"Katherine","last_name":"De Kleer","full_name":"De Kleer, Katherine"},{"full_name":"Fisher, Chloe","last_name":"Fisher","first_name":"Chloe"},{"first_name":"Sébastien","last_name":"Charnoz","full_name":"Charnoz, Sébastien"},{"first_name":"Ashley D.","full_name":"Baker, Ashley D.","last_name":"Baker"},{"last_name":"Halverson","full_name":"Halverson, Samuel P.","first_name":"Samuel P."},{"first_name":"Nick M.","last_name":"Schneider","full_name":"Schneider, Nick M."},{"first_name":"Angelica","full_name":"Psaridi, Angelica","last_name":"Psaridi"},{"first_name":"Aurélien","full_name":"Wyttenbach, Aurélien","last_name":"Wyttenbach"},{"full_name":"Torres Rodriguez, Santiago","last_name":"Torres Rodriguez","orcid":"0000-0002-3150-8988","id":"a8df4360-4328-11ee-8f1a-e502d0c83fc2","first_name":"Santiago"},{"full_name":"Bhatnagar, Ishita","last_name":"Bhatnagar","first_name":"Ishita"},{"first_name":"Robert E.","full_name":"Johnson, Robert E.","last_name":"Johnson"}],"date_created":"2024-10-13T22:01:49Z","volume":973,"oa":1,"month":"10","oa_version":"Published Version","status":"public","ddc":["520"],"_id":"18306","file_date_updated":"2024-10-21T11:05:11Z","article_number":"L53","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","citation":{"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.","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>.","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>","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.","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).","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>.","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>"},"publication":"Astrophysical Journal Letters","file":[{"file_name":"2024_AstrophysicalJourn_Oza.pdf","date_created":"2024-10-21T11:05:11Z","creator":"dernst","access_level":"open_access","date_updated":"2024-10-21T11:05:11Z","success":1,"file_id":"18456","file_size":1249747,"checksum":"23eea2a6a0519694a84998957ad7b7fb","relation":"main_file","content_type":"application/pdf"}],"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).","type":"journal_article","OA_place":"publisher","date_updated":"2025-09-08T14:18:18Z","title":"Redshifted sodium transient near exoplanet transit","publication_status":"published","date_published":"2024-10-01T00:00:00Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"external_id":{"arxiv":["2409.19844"],"isi":["001322169500001"]},"isi":1,"quality_controlled":"1","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"}],"DOAJ_listed":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"arxiv":1},{"DOAJ_listed":"1","quality_controlled":"1","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."}],"date_published":"2024-10-24T00:00:00Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"external_id":{"arxiv":["2410.10940"],"isi":["001340831400001"]},"isi":1,"title":"Expansion properties of the young supernova type Iax remnant Pa 30 revealed","publication_status":"published","project":[{"name":"IST Austria Open Access Fund","_id":"B67AFEDC-15C9-11EA-A837-991A96BB2854"}],"APC_amount":"3080,76 EUR","date_updated":"2025-09-08T14:43:36Z","arxiv":1,"publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"publication":"The Astrophysical Journal Letters","citation":{"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, American Astronomical Society, 2024, 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.","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. American Astronomical Society, 2024.","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>","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).","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>. American Astronomical Society. <a href=\"https://doi.org/10.3847/2041-8213/ad713b\">https://doi.org/10.3847/2041-8213/ad713b</a>","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>. American Astronomical Society, 2024. <a href=\"https://doi.org/10.3847/2041-8213/ad713b\">https://doi.org/10.3847/2041-8213/ad713b</a>."},"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","OA_place":"publisher","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.","type":"journal_article","file":[{"date_updated":"2024-11-20T12:24:52Z","success":1,"creator":"dernst","access_level":"open_access","date_created":"2024-11-20T12:24:52Z","file_name":"2024_AstrophysJourLetters_Cunningham.pdf","content_type":"application/pdf","relation":"main_file","checksum":"51e790dd3d85ca984e656734f9f611da","file_size":90328868,"file_id":"18573"}],"volume":975,"date_created":"2024-11-19T08:12:59Z","author":[{"last_name":"Cunningham","full_name":"Cunningham, Tim","first_name":"Tim"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","last_name":"Caiazzo","full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388"},{"full_name":"Prusinski, Nikolaus Z.","last_name":"Prusinski","first_name":"Nikolaus Z."},{"first_name":"James","last_name":"Fuller","full_name":"Fuller, James"},{"first_name":"John C.","last_name":"Raymond","full_name":"Raymond, John C."},{"last_name":"Kulkarni","full_name":"Kulkarni, S. R.","first_name":"S. R."},{"first_name":"James D.","last_name":"Neill","full_name":"Neill, James D."},{"full_name":"Duffell, Paul","last_name":"Duffell","first_name":"Paul"},{"full_name":"Martin, Chris","last_name":"Martin","first_name":"Chris"},{"full_name":"Toloza, Odette","last_name":"Toloza","first_name":"Odette"},{"last_name":"Charbonneau","full_name":"Charbonneau, David","first_name":"David"},{"first_name":"Scott J.","full_name":"Kenyon, Scott J.","last_name":"Kenyon"},{"last_name":"Lin","full_name":"Lin, Zeren","first_name":"Zeren"},{"full_name":"Matuszewski, Mateusz","last_name":"Matuszewski","first_name":"Mateusz"},{"last_name":"McGurk","full_name":"McGurk, Rosalie","first_name":"Rosalie"},{"first_name":"Abigail","full_name":"Polin, Abigail","last_name":"Polin"},{"first_name":"Philippe Z.","full_name":"Yao, Philippe Z.","last_name":"Yao"}],"intvolume":"       975","doi":"10.3847/2041-8213/ad713b","scopus_import":"1","article_number":"L7","_id":"18564","ddc":["520"],"file_date_updated":"2024-11-20T12:24:52Z","status":"public","oa_version":"Published Version","month":"10","oa":1,"year":"2024","language":[{"iso":"eng"}],"OA_type":"gold","department":[{"_id":"IlCa"}],"article_processing_charge":"Yes","has_accepted_license":"1","issue":"1","day":"24","publisher":"American Astronomical Society","article_type":"original"},{"publication":"Astrophysical Journal Letters","citation":{"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>.","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>","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).","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.","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>","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.","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>."},"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","OA_place":"publisher","type":"journal_article","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).","file":[{"checksum":"5c7320196586b4340e55f215d8737185","relation":"main_file","content_type":"application/pdf","file_size":1822989,"file_id":"18771","access_level":"open_access","creator":"dernst","success":1,"date_updated":"2025-01-08T08:18:39Z","file_name":"2024_AstrophysicalJour_Nelson.pdf","date_created":"2025-01-08T08:18:39Z"}],"DOAJ_listed":"1","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."}],"quality_controlled":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"isi":1,"date_published":"2024-12-01T00:00:00Z","external_id":{"isi":["001364636000001"],"arxiv":["2310.06887"]},"publication_status":"published","title":"Ionized gas kinematics with FRESCO: An extended, massive, rapidly rotating galaxy at z = 5.4","date_updated":"2025-09-09T11:58:02Z","arxiv":1,"publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"year":"2024","language":[{"iso":"eng"}],"OA_type":"gold","department":[{"_id":"JoMa"}],"article_processing_charge":"Yes","has_accepted_license":"1","issue":"2","day":"01","publisher":"IOP Publishing","article_type":"letter_note","volume":976,"date_created":"2025-01-05T23:01:58Z","author":[{"last_name":"Nelson","full_name":"Nelson, Erica","first_name":"Erica"},{"first_name":"Gabriel","last_name":"Brammer","full_name":"Brammer, Gabriel"},{"last_name":"Giménez-Arteaga","full_name":"Giménez-Arteaga, Clara","first_name":"Clara"},{"first_name":"Pascal A.","full_name":"Oesch, Pascal A.","last_name":"Oesch"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"first_name":"Hannah","last_name":"Übler","full_name":"Übler, Hannah"},{"last_name":"Matharu","full_name":"Matharu, Jasleen","first_name":"Jasleen"},{"last_name":"Shapley","full_name":"Shapley, Alice E.","first_name":"Alice E."},{"first_name":"Katherine E.","last_name":"Whitaker","full_name":"Whitaker, Katherine E."},{"full_name":"Wisnioski, Emily","last_name":"Wisnioski","first_name":"Emily"},{"full_name":"Förster Schreiber, Natascha M.","last_name":"Förster Schreiber","first_name":"Natascha M."},{"first_name":"Renske","full_name":"Smit, Renske","last_name":"Smit"},{"full_name":"Van Dokkum, Pieter","last_name":"Van Dokkum","first_name":"Pieter"},{"full_name":"Chisholm, John","last_name":"Chisholm","first_name":"John"},{"first_name":"Ryan","full_name":"Endsley, Ryan","last_name":"Endsley"},{"first_name":"Abigail I.","last_name":"Hartley","full_name":"Hartley, Abigail I."},{"last_name":"Gibson","full_name":"Gibson, Justus","first_name":"Justus"},{"last_name":"Giovinazzo","full_name":"Giovinazzo, Emma","first_name":"Emma"},{"first_name":"Garth","full_name":"Illingworth, 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."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"first_name":"Alba","last_name":"Covelo Paz","full_name":"Covelo Paz, Alba"},{"first_name":"Sedona H.","last_name":"Price","full_name":"Price, Sedona H."},{"full_name":"Reddy, Naveen A.","last_name":"Reddy","first_name":"Naveen A."},{"first_name":"Irene","last_name":"Shivaei","full_name":"Shivaei, Irene"},{"full_name":"Weibel, Andrea","last_name":"Weibel","first_name":"Andrea"},{"first_name":"Stijn","full_name":"Wuyts, Stijn","last_name":"Wuyts"},{"first_name":"Mengyuan","full_name":"Xiao, Mengyuan","last_name":"Xiao"},{"first_name":"Stacey","full_name":"Alberts, Stacey","last_name":"Alberts"},{"first_name":"William M.","last_name":"Baker","full_name":"Baker, William M."},{"first_name":"Andrew J.","full_name":"Bunker, Andrew J.","last_name":"Bunker"},{"last_name":"Cameron","full_name":"Cameron, Alex J.","first_name":"Alex J."},{"first_name":"Stephane","last_name":"Charlot","full_name":"Charlot, Stephane"},{"first_name":"Daniel J.","last_name":"Eisenstein","full_name":"Eisenstein, Daniel J."},{"first_name":"Anna","last_name":"De Graaff","full_name":"De Graaff, Anna"},{"first_name":"Zhiyuan","full_name":"Ji, Zhiyuan","last_name":"Ji"},{"full_name":"Johnson, Benjamin D.","last_name":"Johnson","first_name":"Benjamin D."},{"last_name":"Jones","full_name":"Jones, Gareth C.","first_name":"Gareth C."},{"full_name":"Maiolino, Roberto","last_name":"Maiolino","first_name":"Roberto"},{"last_name":"Robertson","full_name":"Robertson, Brant","first_name":"Brant"},{"first_name":"Lester","last_name":"Sandles","full_name":"Sandles, Lester"},{"first_name":"Katherine A.","last_name":"Suess","full_name":"Suess, Katherine A."},{"full_name":"Tacchella, Sandro","last_name":"Tacchella","first_name":"Sandro"},{"last_name":"Williams","full_name":"Williams, Christina C.","first_name":"Christina C."},{"first_name":"Joris","last_name":"Witstok","full_name":"Witstok, Joris"}],"intvolume":"       976","doi":"10.3847/2041-8213/ad7b17","scopus_import":"1","article_number":"L27","ddc":["520"],"_id":"18760","file_date_updated":"2025-01-08T08:18:39Z","status":"public","oa_version":"Published Version","month":"12","oa":1},{"publication":"Astrophysical Journal Letters","citation":{"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>.","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>","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.","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>","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."},"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","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).","type":"journal_article","file":[{"content_type":"application/pdf","relation":"main_file","checksum":"bb1a6725586df12e745d091b5778bb2b","file_id":"17243","file_size":3273303,"success":1,"date_updated":"2024-07-16T06:24:29Z","access_level":"open_access","creator":"dernst","date_created":"2024-07-16T06:24:29Z","file_name":"2024_AstrophysicalJourn_Wang.pdf"}],"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."}],"quality_controlled":"1","DOAJ_listed":"1","publication_status":"published","title":"RUBIES: Evolved stellar populations with extended formation histories at z ∼ 7-8 in candidate massive galaxies identified with JWST/NIRSpec","date_updated":"2025-09-08T08:10:21Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"external_id":{"isi":["001257903200001"],"arxiv":["2405.01473"]},"date_published":"2024-07-01T00:00:00Z","isi":1,"arxiv":1,"publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"year":"2024","language":[{"iso":"eng"}],"article_processing_charge":"Yes","has_accepted_license":"1","department":[{"_id":"JoMa"}],"article_type":"original","publisher":"IOP Publishing","day":"01","issue":"1","author":[{"first_name":"Bingjie","last_name":"Wang","full_name":"Wang, Bingjie"},{"last_name":"Leja","full_name":"Leja, Joel","first_name":"Joel"},{"first_name":"Anna","full_name":"De Graaff, Anna","last_name":"De Graaff"},{"last_name":"Brammer","full_name":"Brammer, Gabriel B.","first_name":"Gabriel B."},{"full_name":"Weibel, Andrea","last_name":"Weibel","first_name":"Andrea"},{"first_name":"Pieter","last_name":"Van Dokkum","full_name":"Van Dokkum, Pieter"},{"last_name":"Baggen","full_name":"Baggen, Josephine F.W.","first_name":"Josephine F.W."},{"last_name":"Suess","full_name":"Suess, Katherine A.","first_name":"Katherine A."},{"first_name":"Jenny E.","full_name":"Greene, Jenny E.","last_name":"Greene"},{"full_name":"Bezanson, Rachel","last_name":"Bezanson","first_name":"Rachel"},{"last_name":"Cleri","full_name":"Cleri, Nikko J.","first_name":"Nikko J."},{"last_name":"Hirschmann","full_name":"Hirschmann, Michaela","first_name":"Michaela"},{"first_name":"Ivo","full_name":"Labbé, Ivo","last_name":"Labbé"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Mcconachie, Ian","last_name":"Mcconachie","first_name":"Ian"},{"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.","full_name":"Oesch, Pascal A.","last_name":"Oesch"},{"full_name":"Setton, David J.","last_name":"Setton","first_name":"David J."},{"first_name":"Christina C.","full_name":"Williams, Christina C.","last_name":"Williams"}],"volume":969,"date_created":"2024-07-14T22:01:11Z","doi":"10.3847/2041-8213/ad55f7","scopus_import":"1","intvolume":"       969","_id":"17234","file_date_updated":"2024-07-16T06:24:29Z","ddc":["520"],"oa_version":"Published Version","status":"public","article_number":"L13","oa":1,"month":"07"},{"oa":1,"month":"10","_id":"15192","status":"public","oa_version":"Published Version","article_number":"L41","doi":"10.3847/2041-8213/acffc4","extern":"1","scopus_import":"1","intvolume":"       956","author":[{"full_name":"Miller, David R.","last_name":"Miller","first_name":"David R."},{"orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria","last_name":"Caiazzo","first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d"},{"full_name":"Heyl, Jeremy","last_name":"Heyl","first_name":"Jeremy"},{"first_name":"Harvey B.","full_name":"Richer, Harvey B.","last_name":"Richer"},{"first_name":"Kareem","full_name":"El-Badry, Kareem","last_name":"El-Badry"},{"last_name":"Rodriguez","full_name":"Rodriguez, Antonio C.","first_name":"Antonio C."},{"first_name":"Zachary P.","last_name":"Vanderbosch","full_name":"Vanderbosch, Zachary P."},{"full_name":"van Roestel, Jan","last_name":"van Roestel","first_name":"Jan"}],"main_file_link":[{"open_access":"1","url":"https://doi.org/10.3847/2041-8213/acffc4"}],"volume":956,"date_created":"2024-03-26T09:45:38Z","article_type":"original","publisher":"American Astronomical Society","issue":"2","day":"19","article_processing_charge":"No","year":"2023","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"arxiv":1,"publication_status":"published","title":"An extremely massive white dwarf escaped from the Hyades star cluster","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)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"date_published":"2023-10-19T00:00:00Z","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","type":"journal_article","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.","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>.","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.","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)."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"The Astrophysical Journal Letters"},{"citation":{"ista":"Burdge KB, El-Badry K, Rappaport S, Sunny Wong TL, Bauer EB, Bildsten L, Caiazzo I, Chakrabarty D, Chickles E, Graham MJ, Kara E, Kulkarni SR, Marsh TR, Nynka M, Prince TA, Simcoe RA, van Roestel J, Vanderbosch Z, Bellm EC, Dekany RG, Drake AJ, Helou G, Masci FJ, Milburn J, Riddle R, Rusholme B, Smith R. 2023. Orbital decay in an accreting and eclipsing 13.7 minute orbital period binary with a luminous donor. The Astrophysical Journal Letters. 953(1), L1.","mla":"Burdge, Kevin B., et al. “Orbital Decay in an Accreting and Eclipsing 13.7 Minute Orbital Period Binary with a Luminous Donor.” <i>The Astrophysical Journal Letters</i>, vol. 953, no. 1, L1, American Astronomical Society, 2023, doi:<a href=\"https://doi.org/10.3847/2041-8213/ace7cf\">10.3847/2041-8213/ace7cf</a>.","ieee":"K. B. Burdge <i>et al.</i>, “Orbital decay in an accreting and eclipsing 13.7 minute orbital period binary with a luminous donor,” <i>The Astrophysical Journal Letters</i>, vol. 953, no. 1. American Astronomical Society, 2023.","ama":"Burdge KB, El-Badry K, Rappaport S, et al. Orbital decay in an accreting and eclipsing 13.7 minute orbital period binary with a luminous donor. <i>The Astrophysical Journal Letters</i>. 2023;953(1). doi:<a href=\"https://doi.org/10.3847/2041-8213/ace7cf\">10.3847/2041-8213/ace7cf</a>","short":"K.B. Burdge, K. El-Badry, S. Rappaport, T.L. Sunny Wong, E.B. Bauer, L. Bildsten, I. Caiazzo, D. Chakrabarty, E. Chickles, M.J. Graham, E. Kara, S.R. Kulkarni, T.R. Marsh, M. Nynka, T.A. Prince, R.A. Simcoe, J. van Roestel, Z. Vanderbosch, E.C. Bellm, R.G. Dekany, A.J. Drake, G. Helou, F.J. Masci, J. Milburn, R. Riddle, B. Rusholme, R. Smith, The Astrophysical Journal Letters 953 (2023).","apa":"Burdge, K. B., El-Badry, K., Rappaport, S., Sunny Wong, T. L., Bauer, E. B., Bildsten, L., … Smith, R. (2023). Orbital decay in an accreting and eclipsing 13.7 minute orbital period binary with a luminous donor. <i>The Astrophysical Journal Letters</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/2041-8213/ace7cf\">https://doi.org/10.3847/2041-8213/ace7cf</a>","chicago":"Burdge, Kevin B., Kareem El-Badry, Saul Rappaport, Tin Long Sunny Wong, Evan B. Bauer, Lars Bildsten, Ilaria Caiazzo, et al. “Orbital Decay in an Accreting and Eclipsing 13.7 Minute Orbital Period Binary with a Luminous Donor.” <i>The Astrophysical Journal Letters</i>. American Astronomical Society, 2023. <a href=\"https://doi.org/10.3847/2041-8213/ace7cf\">https://doi.org/10.3847/2041-8213/ace7cf</a>."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"The Astrophysical Journal Letters","type":"journal_article","publication_status":"published","title":"Orbital decay in an accreting and eclipsing 13.7 minute orbital period binary with a luminous donor","date_updated":"2024-04-02T07:01:46Z","external_id":{"arxiv":["2303.13573"]},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"date_published":"2023-08-08T00:00:00Z","quality_controlled":"1","abstract":[{"text":"We report the discovery of ZTF J0127+5258, a compact mass-transferring binary with an orbital period of 13.7 minutes. The system contains a white dwarf accretor, which likely originated as a post–common envelope carbon–oxygen (CO) white dwarf, and a warm donor (Teff,donor = 16,400 ± 1000 K). The donor probably formed during a common envelope phase between the CO white dwarf and an evolving giant that left behind a helium star or white dwarf in a close orbit with the CO white dwarf. We measure gravitational wave–driven orbital inspiral with ∼51σ significance, which yields a joint constraint on the component masses and mass transfer rate. While the accretion disk in the system is dominated by ionized helium emission, the donor exhibits a mixture of hydrogen and helium absorption lines. Phase-resolved spectroscopy yields a donor radial velocity semiamplitude of 771 ± 27 km s−1, and high-speed photometry reveals that the system is eclipsing. We detect a Chandra X-ray counterpart with LX ∼ 3 × 1031 erg s−1. Depending on the mass transfer rate, the system will likely either evolve into a stably mass-transferring helium cataclysmic variable, merge to become an R CrB star, or explode as a Type Ia supernova in the next million years. We predict that the Laser Space Interferometer Antenna (LISA) will detect the source with a signal-to-noise ratio of 24 ± 6 after 4 yr of observations. The system is the first LISA-loud mass-transferring binary with an intrinsically luminous donor, a class of sources that provide the opportunity to leverage the synergy between optical and infrared time domain surveys, X-ray facilities, and gravitational-wave observatories to probe general relativity, accretion physics, and binary evolution.","lang":"eng"}],"publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"arxiv":1,"year":"2023","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"publisher":"American Astronomical Society","article_type":"original","day":"08","issue":"1","article_processing_charge":"No","extern":"1","doi":"10.3847/2041-8213/ace7cf","scopus_import":"1","intvolume":"       953","author":[{"first_name":"Kevin B.","last_name":"Burdge","full_name":"Burdge, Kevin B."},{"first_name":"Kareem","full_name":"El-Badry, Kareem","last_name":"El-Badry"},{"last_name":"Rappaport","full_name":"Rappaport, Saul","first_name":"Saul"},{"first_name":"Tin Long","full_name":"Sunny Wong, Tin Long","last_name":"Sunny Wong"},{"last_name":"Bauer","full_name":"Bauer, Evan B.","first_name":"Evan B."},{"full_name":"Bildsten, Lars","last_name":"Bildsten","first_name":"Lars"},{"first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria","last_name":"Caiazzo"},{"first_name":"Deepto","full_name":"Chakrabarty, Deepto","last_name":"Chakrabarty"},{"last_name":"Chickles","full_name":"Chickles, Emma","first_name":"Emma"},{"full_name":"Graham, Matthew J.","last_name":"Graham","first_name":"Matthew J."},{"first_name":"Erin","last_name":"Kara","full_name":"Kara, Erin"},{"first_name":"S. R.","full_name":"Kulkarni, S. R.","last_name":"Kulkarni"},{"full_name":"Marsh, Thomas R.","last_name":"Marsh","first_name":"Thomas R."},{"first_name":"Melania","full_name":"Nynka, Melania","last_name":"Nynka"},{"last_name":"Prince","full_name":"Prince, Thomas A.","first_name":"Thomas A."},{"first_name":"Robert A.","full_name":"Simcoe, Robert A.","last_name":"Simcoe"},{"last_name":"van Roestel","full_name":"van Roestel, Jan","first_name":"Jan"},{"first_name":"Zach","last_name":"Vanderbosch","full_name":"Vanderbosch, Zach"},{"last_name":"Bellm","full_name":"Bellm, Eric C.","first_name":"Eric C."},{"first_name":"Richard G.","full_name":"Dekany, Richard G.","last_name":"Dekany"},{"first_name":"Andrew J.","full_name":"Drake, Andrew J.","last_name":"Drake"},{"full_name":"Helou, George","last_name":"Helou","first_name":"George"},{"last_name":"Masci","full_name":"Masci, Frank J.","first_name":"Frank J."},{"first_name":"Jennifer","last_name":"Milburn","full_name":"Milburn, Jennifer"},{"first_name":"Reed","full_name":"Riddle, Reed","last_name":"Riddle"},{"full_name":"Rusholme, Ben","last_name":"Rusholme","first_name":"Ben"},{"last_name":"Smith","full_name":"Smith, Roger","first_name":"Roger"}],"main_file_link":[{"open_access":"1","url":"https://doi.org/10.3847/2041-8213/ace7cf"}],"volume":953,"date_created":"2024-03-26T09:47:22Z","oa":1,"month":"08","_id":"15196","oa_version":"Published Version","status":"public","article_number":"L1"},{"author":[{"first_name":"Silvia","full_name":"Zane, Silvia","last_name":"Zane"},{"full_name":"Taverna, Roberto","last_name":"Taverna","first_name":"Roberto"},{"first_name":"Denis","last_name":"González–Caniulef","full_name":"González–Caniulef, Denis"},{"first_name":"Fabio","full_name":"Muleri, Fabio","last_name":"Muleri"},{"first_name":"Roberto","last_name":"Turolla","full_name":"Turolla, Roberto"},{"first_name":"Jeremy","last_name":"Heyl","full_name":"Heyl, Jeremy"},{"first_name":"Keisuke","full_name":"Uchiyama, Keisuke","last_name":"Uchiyama"},{"first_name":"Mason","full_name":"Ng, Mason","last_name":"Ng"},{"full_name":"Tamagawa, Toru","last_name":"Tamagawa","first_name":"Toru"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","last_name":"Caiazzo","full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388"},{"last_name":"Di Lalla","full_name":"Di Lalla, Niccolò","first_name":"Niccolò"},{"last_name":"Marshall","full_name":"Marshall, Herman L.","first_name":"Herman L."},{"first_name":"Matteo","full_name":"Bachetti, Matteo","last_name":"Bachetti"},{"first_name":"Fabio","last_name":"La Monaca","full_name":"La Monaca, Fabio"},{"last_name":"Gau","full_name":"Gau, Ephraim","first_name":"Ephraim"},{"last_name":"Di Marco","full_name":"Di Marco, Alessandro","first_name":"Alessandro"},{"first_name":"Luca","full_name":"Baldini, Luca","last_name":"Baldini"},{"first_name":"Michela","full_name":"Negro, Michela","last_name":"Negro"},{"first_name":"Nicola","last_name":"Omodei","full_name":"Omodei, Nicola"},{"first_name":"John","last_name":"Rankin","full_name":"Rankin, John"},{"first_name":"Giorgio","last_name":"Matt","full_name":"Matt, Giorgio"},{"last_name":"Pavlov","full_name":"Pavlov, George G.","first_name":"George G."},{"last_name":"Kitaguchi","full_name":"Kitaguchi, Takao","first_name":"Takao"},{"last_name":"Krawczynski","full_name":"Krawczynski, Henric","first_name":"Henric"},{"first_name":"Fabian","full_name":"Kislat, Fabian","last_name":"Kislat"},{"last_name":"Kelly","full_name":"Kelly, Ruth","first_name":"Ruth"},{"first_name":"Iván","last_name":"Agudo","full_name":"Agudo, Iván"},{"last_name":"Antonelli","full_name":"Antonelli, Lucio A.","first_name":"Lucio A."},{"first_name":"Wayne H.","last_name":"Baumgartner","full_name":"Baumgartner, Wayne H."},{"full_name":"Bellazzini, Ronaldo","last_name":"Bellazzini","first_name":"Ronaldo"},{"full_name":"Bianchi, Stefano","last_name":"Bianchi","first_name":"Stefano"},{"full_name":"Bongiorno, Stephen D.","last_name":"Bongiorno","first_name":"Stephen D."},{"first_name":"Raffaella","full_name":"Bonino, Raffaella","last_name":"Bonino"},{"full_name":"Brez, Alessandro","last_name":"Brez","first_name":"Alessandro"},{"first_name":"Niccolò","last_name":"Bucciantini","full_name":"Bucciantini, Niccolò"},{"first_name":"Fiamma","last_name":"Capitanio","full_name":"Capitanio, Fiamma"},{"first_name":"Simone","full_name":"Castellano, Simone","last_name":"Castellano"},{"first_name":"Elisabetta","last_name":"Cavazzuti","full_name":"Cavazzuti, Elisabetta"},{"first_name":"Chieng-Ting","full_name":"Chen, Chieng-Ting","last_name":"Chen"},{"full_name":"Ciprini, Stefano","last_name":"Ciprini","first_name":"Stefano"},{"full_name":"Costa, Enrico","last_name":"Costa","first_name":"Enrico"},{"first_name":"Alessandra","full_name":"De Rosa, Alessandra","last_name":"De Rosa"},{"first_name":"Ettore","last_name":"Del Monte","full_name":"Del Monte, Ettore"},{"last_name":"Di Gesu","full_name":"Di Gesu, Laura","first_name":"Laura"},{"first_name":"Immacolata","last_name":"Donnarumma","full_name":"Donnarumma, Immacolata"},{"last_name":"Doroshenko","full_name":"Doroshenko, Victor","first_name":"Victor"},{"full_name":"Dovčiak, Michal","last_name":"Dovčiak","first_name":"Michal"},{"first_name":"Steven R.","full_name":"Ehlert, Steven R.","last_name":"Ehlert"},{"first_name":"Teruaki","last_name":"Enoto","full_name":"Enoto, Teruaki"},{"last_name":"Evangelista","full_name":"Evangelista, Yuri","first_name":"Yuri"},{"last_name":"Fabiani","full_name":"Fabiani, Sergio","first_name":"Sergio"},{"first_name":"Riccardo","full_name":"Ferrazzoli, Riccardo","last_name":"Ferrazzoli"},{"first_name":"Javier A.","full_name":"Garcia, Javier A.","last_name":"Garcia"},{"first_name":"Shuichi","last_name":"Gunji","full_name":"Gunji, Shuichi"},{"last_name":"Hayashida","full_name":"Hayashida, Kiyoshi","first_name":"Kiyoshi"},{"last_name":"Iwakiri","full_name":"Iwakiri, Wataru","first_name":"Wataru"},{"first_name":"Svetlana G.","full_name":"Jorstad, Svetlana G.","last_name":"Jorstad"},{"first_name":"Philip","full_name":"Kaaret, Philip","last_name":"Kaaret"},{"first_name":"Vladimir","full_name":"Karas, Vladimir","last_name":"Karas"},{"first_name":"Jeffery J.","full_name":"Kolodziejczak, Jeffery J.","last_name":"Kolodziejczak"},{"first_name":"Luca","last_name":"Latronico","full_name":"Latronico, Luca"},{"first_name":"Ioannis","full_name":"Liodakis, Ioannis","last_name":"Liodakis"},{"last_name":"Maldera","full_name":"Maldera, Simone","first_name":"Simone"},{"first_name":"Alberto","last_name":"Manfreda","full_name":"Manfreda, Alberto"},{"last_name":"Marin","full_name":"Marin, Frédéric","first_name":"Frédéric"},{"first_name":"Andrea","last_name":"Marinucci","full_name":"Marinucci, Andrea"},{"last_name":"Marscher","full_name":"Marscher, Alan P.","first_name":"Alan P."},{"last_name":"Massaro","full_name":"Massaro, Francesco","first_name":"Francesco"},{"full_name":"Mitsuishi, Ikuyuki","last_name":"Mitsuishi","first_name":"Ikuyuki"},{"first_name":"Tsunefumi","last_name":"Mizuno","full_name":"Mizuno, Tsunefumi"},{"first_name":"C.-Y.","last_name":"Ng","full_name":"Ng, C.-Y."},{"first_name":"Stephen L.","last_name":"O’Dell","full_name":"O’Dell, Stephen L."},{"first_name":"Chiara","full_name":"Oppedisano, Chiara","last_name":"Oppedisano"},{"first_name":"Alessandro","full_name":"Papitto, Alessandro","last_name":"Papitto"},{"last_name":"Peirson","full_name":"Peirson, Abel L.","first_name":"Abel L."},{"full_name":"Perri, Matteo","last_name":"Perri","first_name":"Matteo"},{"full_name":"Pesce-Rollins, Melissa","last_name":"Pesce-Rollins","first_name":"Melissa"},{"full_name":"Petrucci, Pierre-Olivier","last_name":"Petrucci","first_name":"Pierre-Olivier"},{"full_name":"Pilia, Maura","last_name":"Pilia","first_name":"Maura"},{"first_name":"Andrea","last_name":"Possenti","full_name":"Possenti, Andrea"},{"first_name":"Juri","full_name":"Poutanen, Juri","last_name":"Poutanen"},{"first_name":"Simonetta","last_name":"Puccetti","full_name":"Puccetti, Simonetta"},{"first_name":"Brian D.","full_name":"Ramsey, Brian D.","last_name":"Ramsey"},{"first_name":"Ajay","last_name":"Ratheesh","full_name":"Ratheesh, Ajay"},{"last_name":"Roberts","full_name":"Roberts, Oliver J.","first_name":"Oliver J."},{"first_name":"Roger W.","last_name":"Romani","full_name":"Romani, Roger W."},{"last_name":"Sgró","full_name":"Sgró, Carmelo","first_name":"Carmelo"},{"first_name":"Patrick","last_name":"Slane","full_name":"Slane, Patrick"},{"last_name":"Soffitta","full_name":"Soffitta, Paolo","first_name":"Paolo"},{"first_name":"Gloria","last_name":"Spandre","full_name":"Spandre, Gloria"},{"first_name":"Douglas A.","full_name":"Swartz, Douglas A.","last_name":"Swartz"},{"full_name":"Tavecchio, Fabrizio","last_name":"Tavecchio","first_name":"Fabrizio"},{"full_name":"Tawara, Yuzuru","last_name":"Tawara","first_name":"Yuzuru"},{"first_name":"Allyn F.","last_name":"Tennant","full_name":"Tennant, Allyn F."},{"last_name":"Thomas","full_name":"Thomas, Nicholas E.","first_name":"Nicholas E."},{"full_name":"Tombesi, Francesco","last_name":"Tombesi","first_name":"Francesco"},{"first_name":"Alessio","full_name":"Trois, Alessio","last_name":"Trois"},{"last_name":"Tsygankov","full_name":"Tsygankov, Sergey S.","first_name":"Sergey S."},{"first_name":"Jacco","last_name":"Vink","full_name":"Vink, Jacco"},{"first_name":"Martin C.","last_name":"Weisskopf","full_name":"Weisskopf, Martin C."},{"full_name":"Wu, Kinwah","last_name":"Wu","first_name":"Kinwah"},{"first_name":"Fei","last_name":"Xie","full_name":"Xie, Fei"}],"main_file_link":[{"open_access":"1","url":"https://doi.org/10.3847/2041-8213/acb703"}],"volume":944,"date_created":"2024-03-26T09:50:12Z","doi":"10.3847/2041-8213/acb703","extern":"1","scopus_import":"1","intvolume":"       944","_id":"15202","oa_version":"Published Version","status":"public","article_number":"L27","oa":1,"month":"02","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"year":"2023","language":[{"iso":"eng"}],"article_processing_charge":"No","publisher":"American Astronomical Society","article_type":"original","issue":"2","day":"15","abstract":[{"text":"Magnetars are the most strongly magnetized neutron stars, and one of the most promising targets for X-ray polarimetric measurements. We present here the first Imaging X-ray Polarimetry Explorer observation of the magnetar 1RXS J170849.0-400910, jointly analyzed with a new Swift observation and archival NICER data. The total (energy- and phase-integrated) emission in the 2–8 keV energy range is linerarly polarized, at a ∼35% level. The phase-averaged polarization signal shows a marked increase with energy, ranging from ∼20% at 2–3 keV up to ∼80% at 6–8 keV, while the polarization angle remains constant. This indicates that radiation is mostly polarized in a single direction. The spectrum is well reproduced by a combination of either two thermal (blackbody) components or a blackbody and a power law. Both the polarization degree and angle also show a variation with the spin phase, and the former is almost anticorrelated with the source counts in the 2–8 and 2–4 keV bands. We discuss the possible implications and interpretations, based on a joint analysis of the spectral, polarization, and pulsation properties of the source. A scenario in which the surface temperature is not homogeneous, with a hotter cap covered by a gaseous atmosphere and a warmer region in a condensed state, provides a satisfactory description of both the phase- and energy-dependent spectro-polarimetric data. The (comparatively) small size of the two emitting regions, required to explain the observed pulsations, does not allow to reach a robust conclusion about the presence of vacuum birefringence effects.","lang":"eng"}],"quality_controlled":"1","publication_status":"published","title":"A strong x-ray polarization signal from the magnetar 1RXS J170849.0-400910","date_updated":"2024-04-02T07:15:41Z","date_published":"2023-02-15T00:00:00Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"external_id":{"arxiv":["2301.12919"]},"arxiv":1,"publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"publication":"The Astrophysical Journal Letters","citation":{"ista":"Zane S et al. 2023. A strong x-ray polarization signal from the magnetar 1RXS J170849.0-400910. The Astrophysical Journal Letters. 944(2), L27.","mla":"Zane, Silvia, et al. “A Strong X-Ray Polarization Signal from the Magnetar 1RXS J170849.0-400910.” <i>The Astrophysical Journal Letters</i>, vol. 944, no. 2, L27, American Astronomical Society, 2023, doi:<a href=\"https://doi.org/10.3847/2041-8213/acb703\">10.3847/2041-8213/acb703</a>.","ama":"Zane S, Taverna R, González–Caniulef D, et al. A strong x-ray polarization signal from the magnetar 1RXS J170849.0-400910. <i>The Astrophysical Journal Letters</i>. 2023;944(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/acb703\">10.3847/2041-8213/acb703</a>","ieee":"S. Zane <i>et al.</i>, “A strong x-ray polarization signal from the magnetar 1RXS J170849.0-400910,” <i>The Astrophysical Journal Letters</i>, vol. 944, no. 2. American Astronomical Society, 2023.","short":"S. Zane, R. Taverna, D. González–Caniulef, F. Muleri, R. Turolla, J. Heyl, K. Uchiyama, M. Ng, T. Tamagawa, I. Caiazzo, N. Di Lalla, H.L. Marshall, M. Bachetti, F. La Monaca, E. Gau, A. Di Marco, L. Baldini, M. Negro, N. Omodei, J. Rankin, G. Matt, G.G. Pavlov, T. Kitaguchi, H. Krawczynski, F. Kislat, R. Kelly, I. Agudo, L.A. Antonelli, W.H. Baumgartner, R. Bellazzini, S. Bianchi, S.D. Bongiorno, R. Bonino, A. Brez, N. Bucciantini, F. Capitanio, S. Castellano, E. Cavazzuti, C.-T. Chen, S. Ciprini, E. Costa, A. De Rosa, E. Del Monte, L. Di Gesu, I. Donnarumma, V. Doroshenko, M. Dovčiak, S.R. Ehlert, T. Enoto, Y. Evangelista, S. Fabiani, R. Ferrazzoli, J.A. Garcia, S. Gunji, K. Hayashida, W. Iwakiri, S.G. Jorstad, P. Kaaret, V. Karas, J.J. Kolodziejczak, L. Latronico, I. Liodakis, S. Maldera, A. Manfreda, F. Marin, A. Marinucci, A.P. Marscher, F. Massaro, I. Mitsuishi, T. Mizuno, C.-Y. Ng, S.L. O’Dell, C. Oppedisano, A. Papitto, A.L. Peirson, M. Perri, M. Pesce-Rollins, P.-O. Petrucci, M. Pilia, A. Possenti, J. Poutanen, S. Puccetti, B.D. Ramsey, A. Ratheesh, O.J. Roberts, R.W. Romani, C. Sgró, P. Slane, P. Soffitta, G. Spandre, D.A. Swartz, F. Tavecchio, Y. Tawara, A.F. Tennant, N.E. Thomas, F. Tombesi, A. Trois, S.S. Tsygankov, J. Vink, M.C. Weisskopf, K. Wu, F. Xie, The Astrophysical Journal Letters 944 (2023).","chicago":"Zane, Silvia, Roberto Taverna, Denis González–Caniulef, Fabio Muleri, Roberto Turolla, Jeremy Heyl, Keisuke Uchiyama, et al. “A Strong X-Ray Polarization Signal from the Magnetar 1RXS J170849.0-400910.” <i>The Astrophysical Journal Letters</i>. American Astronomical Society, 2023. <a href=\"https://doi.org/10.3847/2041-8213/acb703\">https://doi.org/10.3847/2041-8213/acb703</a>.","apa":"Zane, S., Taverna, R., González–Caniulef, D., Muleri, F., Turolla, R., Heyl, J., … Xie, F. (2023). A strong x-ray polarization signal from the magnetar 1RXS J170849.0-400910. <i>The Astrophysical Journal Letters</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/2041-8213/acb703\">https://doi.org/10.3847/2041-8213/acb703</a>"},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article"}]