[{"ddc":["520"],"article_type":"original","publication_status":"published","author":[{"last_name":"Cristea","id":"4d500bea-31f8-11ee-a48d-d4904fb363c7","first_name":"Andrei-Alexandru","full_name":"Cristea, Andrei-Alexandru"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria","last_name":"Caiazzo"},{"last_name":"Cunningham","first_name":"Tim","full_name":"Cunningham, Tim"},{"full_name":"Raymond, John C.","first_name":"John C.","last_name":"Raymond"},{"last_name":"Vennes","first_name":"Stephane","full_name":"Vennes, Stephane"},{"last_name":"Kawka","full_name":"Kawka, Adela","first_name":"Adela"},{"first_name":"Aayush A","full_name":"Desai, Aayush A","id":"502cfd30-32c1-11ee-a9a4-d8dad5c6739e","last_name":"Desai"},{"full_name":"Miller, David R.","first_name":"David R.","last_name":"Miller"},{"last_name":"Hermes","full_name":"Hermes, J. J.","first_name":"J. J."},{"full_name":"Fuller, Jim","first_name":"Jim","last_name":"Fuller"},{"last_name":"Heyl","first_name":"Jeremy","full_name":"Heyl, Jeremy"},{"last_name":"van Roestel","full_name":"van Roestel, Jan","first_name":"Jan"},{"last_name":"Burdge","full_name":"Burdge, Kevin B.","first_name":"Kevin B."},{"last_name":"Rodriguez","first_name":"Antonio C.","full_name":"Rodriguez, Antonio C."},{"full_name":"Pelisoli, Ingrid","first_name":"Ingrid","last_name":"Pelisoli"},{"full_name":"Gänsicke, Boris T.","first_name":"Boris T.","last_name":"Gänsicke"},{"last_name":"Szkody","first_name":"Paula","full_name":"Szkody, Paula"},{"full_name":"Kenyon, Scott J.","first_name":"Scott J.","last_name":"Kenyon"},{"last_name":"Vanderbosch","full_name":"Vanderbosch, Zach","first_name":"Zach"},{"full_name":"Drake, Andrew","first_name":"Andrew","last_name":"Drake"},{"full_name":"Ferrario, Lilia","first_name":"Lilia","last_name":"Ferrario"},{"first_name":"Dayal","full_name":"Wickramasinghe, Dayal","last_name":"Wickramasinghe"},{"last_name":"Karambelkar","full_name":"Karambelkar, Viraj R.","first_name":"Viraj R."},{"last_name":"Justham","full_name":"Justham, Stephen","first_name":"Stephen"},{"last_name":"Pakmor","full_name":"Pakmor, Ruediger","first_name":"Ruediger"},{"full_name":"El-Badry, Kareem","first_name":"Kareem","last_name":"El-Badry"},{"first_name":"Thomas","full_name":"Prince, Thomas","last_name":"Prince"},{"last_name":"Kulkarni","first_name":"S. R.","full_name":"Kulkarni, S. R."},{"last_name":"Graham","first_name":"Matthew J.","full_name":"Graham, Matthew J."},{"last_name":"Masci","full_name":"Masci, Frank J.","first_name":"Frank J."},{"first_name":"Steven L.","full_name":"Groom, Steven L.","last_name":"Groom"},{"first_name":"Josiah","full_name":"Purdum, Josiah","last_name":"Purdum"},{"last_name":"Dekany","full_name":"Dekany, Richard","first_name":"Richard"},{"full_name":"Bellm, Eric C.","first_name":"Eric C.","last_name":"Bellm"}],"oa_version":"Published Version","intvolume":" 706","month":"02","article_processing_charge":"Yes","year":"2026","oa":1,"publication":"Astronomy & Astrophysics","department":[{"_id":"IlCa"},{"_id":"GradSch"}],"date_created":"2026-02-17T08:12:05Z","related_material":{"link":[{"relation":"press_release","description":"News on ISTA website","url":"https://ista.ac.at/en/news/twos-company-new-class-of-star-remnants/"}]},"has_accepted_license":"1","corr_author":"1","citation":{"ama":"Cristea A-A, Caiazzo I, Cunningham T, et al. A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant. Astronomy & Astrophysics. 2026;706. doi:10.1051/0004-6361/202556432","mla":"Cristea, Andrei-Alexandru, et al. “A Half Ring of Ionized Circumstellar Material Trapped in the Magnetosphere of a White Dwarf Merger Remnant.” Astronomy & Astrophysics, vol. 706, A188, EDP Sciences, 2026, doi:10.1051/0004-6361/202556432.","ista":"Cristea A-A, Caiazzo I, Cunningham T, Raymond JC, Vennes S, Kawka A, Desai AA, Miller DR, Hermes JJ, Fuller J, Heyl J, van Roestel J, Burdge KB, Rodriguez AC, Pelisoli I, Gänsicke BT, Szkody P, Kenyon SJ, Vanderbosch Z, Drake A, Ferrario L, Wickramasinghe D, Karambelkar VR, Justham S, Pakmor R, El-Badry K, Prince T, Kulkarni SR, Graham MJ, Masci FJ, Groom SL, Purdum J, Dekany R, Bellm EC. 2026. A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant. Astronomy & Astrophysics. 706, A188.","chicago":"Cristea, Andrei-Alexandru, Ilaria Caiazzo, Tim Cunningham, John C. Raymond, Stephane Vennes, Adela Kawka, Aayush A Desai, et al. “A Half Ring of Ionized Circumstellar Material Trapped in the Magnetosphere of a White Dwarf Merger Remnant.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202556432.","ieee":"A.-A. Cristea et al., “A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant,” Astronomy & Astrophysics, vol. 706. EDP Sciences, 2026.","apa":"Cristea, A.-A., Caiazzo, I., Cunningham, T., Raymond, J. C., Vennes, S., Kawka, A., … Bellm, E. C. (2026). A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202556432","short":"A.-A. Cristea, I. Caiazzo, T. Cunningham, J.C. Raymond, S. Vennes, A. Kawka, A.A. Desai, D.R. Miller, J.J. Hermes, J. Fuller, J. Heyl, J. van Roestel, K.B. Burdge, A.C. Rodriguez, I. Pelisoli, B.T. Gänsicke, P. Szkody, S.J. Kenyon, Z. Vanderbosch, A. Drake, L. Ferrario, D. Wickramasinghe, V.R. Karambelkar, S. Justham, R. Pakmor, K. El-Badry, T. Prince, S.R. Kulkarni, M.J. Graham, F.J. Masci, S.L. Groom, J. Purdum, R. Dekany, E.C. Bellm, Astronomy & Astrophysics 706 (2026)."},"OA_type":"gold","PlanS_conform":"1","OA_place":"publisher","quality_controlled":"1","volume":706,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"acknowledgement":"We thank Lynne Hillenbrand and Soumyadeep Bhattacharjee for helpful discussions, and Kishalay De for his help with the WIRC\r\nreduction pipeline. IC was supported by NASA through grants from the Space\r\nTelescope Science Institute, under NASA contracts NASA.22K1813, NAS5-\r\n26555 and NAS5-03127. TC was supported by NASA through the NASA Hubble\r\nFellowship grant HST-HF2-51527.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research\r\nin Astronomy, Inc., for NASA, under contract NAS5-26555. This project has\r\nreceived funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 101020057). This work was based on observations obtained with the\r\nSamuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar\r\nObservatory as part of the Zwicky Transient Facility project. ZTF is supported\r\nby the National Science Foundation under Grants No. AST-1440341, AST2034437, and currently Award #2407588. ZTF receives additional funding from\r\nthe ZTF partnership. Current members include Caltech, USA; Caltech/IPAC,\r\nUSA; University of Maryland, USA; University of California, Berkeley, USA;\r\nUniversity of Wisconsin at Milwaukee, USA; Cornell University, USA; Drexel\r\nUniversity, USA; University of North Carolina at Chapel Hill, USA; Institute\r\nof Science and Technology, Austria; National Central University, Taiwan, and\r\nOKC, University of Stockholm, Sweden. Operations are conducted by Caltech’s\r\nOptical Observatory (COO), Caltech/IPAC, and the University of Washington at\r\nSeattle, USA. This work has made use of data from the European Space Agency\r\n(ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by\r\nthe Gaia Data Processing and Analysis Consortium (DPAC, https://www.\r\ncosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The Pan-STARRS1 Surveys (PS1)\r\nand the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the PanSTARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck\r\nInstitute for Extraterrestrial Physics, Garching, The Johns Hopkins University,\r\nDurham University, the University of Edinburgh, the Queen’s University Belfast,\r\nthe Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through\r\nthe Planetary Science Division of the NASA Science Mission Directorate, the\r\nNational Science Foundation Grant No. AST–1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory,\r\nand the Gordon and Betty Moore Foundation. This work made use of Astropy\r\n(http://www.astropy.org): a community-developed core Python package\r\nand an ecosystem of tools and resources for astronomy (Astropy Collaboration\r\n2013, 2018, 2022).","article_number":"A188","date_published":"2026-02-10T00:00:00Z","day":"10","fulldoi":"https://doi.org/10.1051/0004-6361/202556432","file":[{"success":1,"creator":"dernst","date_created":"2026-02-23T12:04:37Z","relation":"main_file","date_updated":"2026-02-23T12:04:37Z","checksum":"229b688e6e78cab5bb8e2bac366d1575","file_size":5352853,"file_name":"2026_AstronomyAstrophysics_Cristea.pdf","content_type":"application/pdf","file_id":"21350","access_level":"open_access"}],"language":[{"iso":"eng"}],"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","image":"/images/cc_by.png","short":"CC BY (4.0)"},"file_date_updated":"2026-02-23T12:04:37Z","abstract":[{"lang":"eng","text":"Many white dwarfs are observed in compact double white dwarf binaries, and through the emission of gravitational waves, a large fraction are destined to merge. The merger remnants that do not explode in a Type Ia supernova are expected to initially be rapidly rotating and highly magnetized. In this work, we present our discovery of the variable white dwarf ZTF J200832.79+444939.67, hereafter ZTF J2008+4449, as a likely merger remnant showing signs of circumstellar material without a stellar or substellar companion. The nature of ZTF J2008+4449 as a merger remnant is supported by its physical properties: it is hot (35 500 ± 300 K) and massive (1.12 ± 0.03 M\r\n ⊙\r\n ), rapidly rotating with a period of ≈6.6 minutes, and likely possesses exceptionally strong magnetic fields (∼400−600 MG) at its surface. Remarkably, we detect a significant period derivative of (1.80 ± 0.09)×10\r\n −12\r\n s/s, indicating that the white dwarf is spinning down, and a soft X-ray emission that is inconsistent with photospheric emission. As the presence of a mass-transferring stellar or brown dwarf companion is excluded by infrared photometry, the detected spin-down and X-ray emission could be tell-tale signs of a magnetically driven wind or of interaction with circumstellar material, possibly originating from the fallback of gravitationally bound merger ejecta or from the tidal disruption of a planetary object. We also detect Balmer emission, which requires the presence of ionized hydrogen in the vicinity of the white dwarf, showing Doppler shifts as high as ≈2000 km s\r\n −1\r\n . The unusual variability of the Balmer emission on the spin period of the white dwarf is consistent with the trapping of a half ring of ionized gas in the magnetosphere of the white dwarf.\r\n "}],"title":"A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant","date_updated":"2026-04-28T12:01:21Z","type":"journal_article","_id":"21274","status":"public","doi":"10.1051/0004-6361/202556432","publisher":"EDP Sciences","DOAJ_listed":"1","user_id":"ba8df636-2132-11f1-aed0-ed93e2281fdd"},{"fulldoi":"https://doi.org/10.3847/1538-4357/ae18c8","file":[{"checksum":"65a8237a519188af83b6dc4d47ad85fa","date_updated":"2026-04-13T08:36:50Z","file_size":19310053,"creator":"dernst","success":1,"relation":"main_file","date_created":"2026-04-13T08:36:50Z","file_id":"21733","access_level":"open_access","file_name":"2026_AstrophysicalJournal_Miller.pdf","content_type":"application/pdf"}],"language":[{"iso":"eng"}],"external_id":{"arxiv":["2510.24877"]},"date_published":"2026-01-01T00:00:00Z","day":"01","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","image":"/images/cc_by.png","short":"CC BY (4.0)"},"keyword":["White dwarf stars","Open star clusters","Compact objects","Stellar evolution"],"date_updated":"2026-04-13T08:39:39Z","file_date_updated":"2026-04-13T08:36:50Z","abstract":[{"lang":"eng","text":"The initial–final mass relation (IFMR) links a star’s birth mass to the mass of its white dwarf (WD) remnant, providing key constraints on stellar evolution. Open clusters offer the most straightforward way to empirically determine the IFMR, as their well-defined ages allow for direct progenitor lifetime estimates. We construct the most comprehensive open cluster WD IFMR to date by combining new spectroscopy of 22 WDs with an extensive literature review of WDs with strong cluster associations. To minimize systematics, we restrict our analysis to spectroscopically confirmed hydrogen-atmosphere (DA) WDs consistent with single-stellar origins. We separately analyze a subset with reliable Gaia-based astrometric membership assessments, as well as a full sample that adds WDs with strong cluster associations whose membership cannot be reliably assessed with Gaia. The Gaia-based sample includes 69 spectroscopically confirmed DA WDs, more than doubling the sample size of previous Gaia-based open cluster IFMRs. The full sample, which includes 53 additional literature WDs,\r\nincreases the total number of cluster WDs by over 50% relative to earlier works. We provide functional forms for both the Gaia-based and full-sample IFMRs. The Gaia-based result useful for Mi � 2.67 M⊙ is Mf = [0.179 0.100H (Mi 3.84 M )] × (Mi 3.84 M ) + 0.628 M , where H(x) is the Heaviside step function. Comparing our IFMR to recent literature, we identify significant deviations from best-fit IFMRs derived from both Gaia-based volume-limited samples of field WDs and double WD binaries, with the largest discrepancy occurring for initial masses of about 5 M⊙."}],"title":"The White Dwarf initial–final mass relation from open clusters in Gaia DR3","doi":"10.3847/1538-4357/ae18c8","publisher":"IOP Publishing","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","DOAJ_listed":"1","type":"journal_article","_id":"21725","status":"public","article_type":"original","publication_status":"published","author":[{"last_name":"Miller","first_name":"David R.","full_name":"Miller, David R."},{"full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","last_name":"Caiazzo"},{"last_name":"Heyl","first_name":"Jeremy","full_name":"Heyl, Jeremy"},{"last_name":"Richer","full_name":"Richer, Harvey B.","first_name":"Harvey B."},{"last_name":"Hollands","first_name":"Mark A.","full_name":"Hollands, Mark A."},{"last_name":"Tremblay","full_name":"Tremblay, Pier Emmanuel","first_name":"Pier Emmanuel"},{"last_name":"El-Badry","first_name":"Kareem","full_name":"El-Badry, Kareem"},{"first_name":"Antonio C.","full_name":"Rodriguez, Antonio C.","last_name":"Rodriguez"},{"full_name":"Vanderbosch, Zachary P.","first_name":"Zachary P.","last_name":"Vanderbosch"}],"ddc":["520"],"article_processing_charge":"Yes","oa":1,"year":"2026","oa_version":"Published Version","issue":"1","intvolume":" 996","month":"01","has_accepted_license":"1","citation":{"mla":"Miller, David R., et al. “The White Dwarf Initial–Final Mass Relation from Open Clusters in Gaia DR3.” The Astrophysical Journal, vol. 996, no. 1, 69, IOP Publishing, 2026, doi:10.3847/1538-4357/ae18c8.","ama":"Miller DR, Caiazzo I, Heyl J, et al. The White Dwarf initial–final mass relation from open clusters in Gaia DR3. The Astrophysical Journal. 2026;996(1). doi:10.3847/1538-4357/ae18c8","ista":"Miller DR, Caiazzo I, Heyl J, Richer HB, Hollands MA, Tremblay PE, El-Badry K, Rodriguez AC, Vanderbosch ZP. 2026. The White Dwarf initial–final mass relation from open clusters in Gaia DR3. The Astrophysical Journal. 996(1), 69.","chicago":"Miller, David R., Ilaria Caiazzo, Jeremy Heyl, Harvey B. Richer, Mark A. Hollands, Pier Emmanuel Tremblay, Kareem El-Badry, Antonio C. Rodriguez, and Zachary P. Vanderbosch. “The White Dwarf Initial–Final Mass Relation from Open Clusters in Gaia DR3.” The Astrophysical Journal. IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae18c8.","short":"D.R. Miller, I. Caiazzo, J. Heyl, H.B. Richer, M.A. Hollands, P.E. Tremblay, K. El-Badry, A.C. Rodriguez, Z.P. Vanderbosch, The Astrophysical Journal 996 (2026).","apa":"Miller, D. R., Caiazzo, I., Heyl, J., Richer, H. B., Hollands, M. A., Tremblay, P. E., … Vanderbosch, Z. P. (2026). The White Dwarf initial–final mass relation from open clusters in Gaia DR3. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae18c8","ieee":"D. R. Miller et al., “The White Dwarf initial–final mass relation from open clusters in Gaia DR3,” The Astrophysical Journal, vol. 996, no. 1. IOP Publishing, 2026."},"publication":"The Astrophysical Journal","department":[{"_id":"IlCa"}],"scopus_import":"1","date_created":"2026-04-12T22:01:52Z","acknowledgement":"The authors would like to thank the anonymous referee for their constructive feedback, which helped improve the clarify of the manuscript. This work was supported in part by the Natural Sciences and Engineering Research Council of Canada Discovery grants Nos. DG-RGPIN-2022-03051 and DG-RGPIN-2023-04486. This research received funding from the European Research Council under the European Union’s Horizon 2020 research and innovation program number 101002408 (MOS100PC). This work includes results based on observations obtained at the international Gemini Observatory, a program of NSF’s NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini Observatory partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). 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 the W. M. Keck Observatory, which is 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. Gemini spectra were processed using the DRAGONS package (K. Labrie et al. 2023). LRIS spectra were reduced using the Lpipe pipeline (D. A. Perley 2019).\r\n\r\nFacilities: Gaia - (DR2 & DR3), Gemini:Gillett - Gillett Gemini North Telescope (GMOS-N), Gemini:South - Gemini South Telescope (GMOS-S), Keck:I - KECK I Telescope (LRIS).\r\n\r\nSoftware: Astropy (Astropy Collaboration et al. 2013,2018, 2022), emcee (D. Foreman-Mackey et al. 2013).","article_number":"69","PlanS_conform":"1","OA_type":"gold","arxiv":1,"OA_place":"publisher","quality_controlled":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"volume":996},{"ddc":["520"],"publication_status":"published","article_type":"original","author":[{"full_name":"Elms, Abbigail K.","first_name":"Abbigail K.","last_name":"Elms"},{"last_name":"Bagnulo","first_name":"Stefano","full_name":"Bagnulo, Stefano"},{"full_name":"Tremblay, Pier Emmanuel","first_name":"Pier Emmanuel","last_name":"Tremblay"},{"first_name":"Tim","full_name":"Cunningham, Tim","last_name":"Cunningham"},{"last_name":"Munday","first_name":"James","full_name":"Munday, James"},{"first_name":"John","full_name":"Landstreet, John","last_name":"Landstreet"},{"last_name":"El-Badry","first_name":"Kareem","full_name":"El-Badry, Kareem"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria","first_name":"Ilaria","last_name":"Caiazzo"},{"last_name":"Melis","full_name":"Melis, Carl","first_name":"Carl"},{"last_name":"Pinter","first_name":"Viktoria","full_name":"Pinter, Viktoria"},{"full_name":"Weinberger, Alycia","first_name":"Alycia","last_name":"Weinberger"}],"month":"05","oa_version":"Published Version","intvolume":" 548","issue":"1","article_processing_charge":"Yes","year":"2026","oa":1,"scopus_import":"1","department":[{"_id":"IlCa"}],"date_created":"2026-04-19T22:07:42Z","publication":"Monthly Notices of the Royal Astronomical Society","citation":{"chicago":"Elms, Abbigail K., Stefano Bagnulo, Pier Emmanuel Tremblay, Tim Cunningham, James Munday, John Landstreet, Kareem El-Badry, et al. “Detection of a Weak Magnetic Field in the Balmer Emission Line White Dwarf WDJ1653−1001.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2026. https://doi.org/10.1093/mnras/stag505.","ieee":"A. K. Elms et al., “Detection of a weak magnetic field in the Balmer emission line white dwarf WDJ1653−1001,” Monthly Notices of the Royal Astronomical Society, vol. 548, no. 1. Oxford University Press, 2026.","apa":"Elms, A. K., Bagnulo, S., Tremblay, P. E., Cunningham, T., Munday, J., Landstreet, J., … Weinberger, A. (2026). Detection of a weak magnetic field in the Balmer emission line white dwarf WDJ1653−1001. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stag505","short":"A.K. Elms, S. Bagnulo, P.E. Tremblay, T. Cunningham, J. Munday, J. Landstreet, K. El-Badry, I. Caiazzo, C. Melis, V. Pinter, A. Weinberger, Monthly Notices of the Royal Astronomical Society 548 (2026).","mla":"Elms, Abbigail K., et al. “Detection of a Weak Magnetic Field in the Balmer Emission Line White Dwarf WDJ1653−1001.” Monthly Notices of the Royal Astronomical Society, vol. 548, no. 1, stag505, Oxford University Press, 2026, doi:10.1093/mnras/stag505.","ama":"Elms AK, Bagnulo S, Tremblay PE, et al. Detection of a weak magnetic field in the Balmer emission line white dwarf WDJ1653−1001. Monthly Notices of the Royal Astronomical Society. 2026;548(1). doi:10.1093/mnras/stag505","ista":"Elms AK, Bagnulo S, Tremblay PE, Cunningham T, Munday J, Landstreet J, El-Badry K, Caiazzo I, Melis C, Pinter V, Weinberger A. 2026. Detection of a weak magnetic field in the Balmer emission line white dwarf WDJ1653−1001. Monthly Notices of the Royal Astronomical Society. 548(1), stag505."},"has_accepted_license":"1","volume":548,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"OA_type":"gold","arxiv":1,"quality_controlled":"1","OA_place":"publisher","acknowledgement":"This project has received funding from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (Grant agreement numbers 101002408). The observationsfrom the FOcal Reducer/low dispersion Spectrograph 2 (FORS2) instrument were collected at the European Southern Observatory (ESO) under ESO programme(s) 113.26ES.001. This work has made use of data from the European Space\r\nAgency (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/conso\r\nrtium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. 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 for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, Deutsches Elektronen-Synchrotron and\r\nHumboldt University, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, IN2P3, University\r\nof 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 Asteroid Terrestrialimpact Last Alert System (ATLAS) project. The Asteroid Terrestrial-impact Last Alert System (ATLAS) project is primarily funded to search for near earth asteroids through NASA grants NN12AR55G, 80NSSC18K0284, and 80NSSC18K1575; byproducts of the NEO search include images and catalogs from the survey area. This work was partially funded by Kepler/K2 grant J1944/80NSSC19K0112 and HST GO-15889, and STFC grants ST/T000198/1 and ST/S006109/1. The ATLAS science products have been made possible through the contributions of the University of Hawaii Institute for Astronomy, the Queen’s University Belfast, the Space Telescope Science Institute, the South African\r\nAstronomical Observatory, and The Millennium Institute of Astrophysics (MAS), Chile.\r\nThis work makes use of observations from the Las Cumbres Observatory global telescope network. Research at Lick Observatory is partially supported by a generous gift from Google. A major upgrade of the Kast spectrograph on the Shane 3 m telescope at Lick Observatory was made possible through generous gifts from William and Marina Kast as well as the Heising–Simons Foundation. The Isaac Newton Telescope is operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias.This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile. Observations reported here were obtained at the Multiple Mirror Telescope (MMT) Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. Based on observations collected at Centro Astronómico Hispano en Andalucía (CAHA) at Calar Alto, operated jointly by Junta de Andalucía and Consejo Superior de Investigaciones Científicas (IAA-CSIC).","article_number":"stag505","day":"01","date_published":"2026-05-01T00:00:00Z","external_id":{"arxiv":["2603.12048"]},"fulldoi":"https://doi.org/10.1093/mnras/stag505","file":[{"file_size":4991495,"checksum":"75c48d70d10a9a48875f577e04da80bc","date_updated":"2026-05-04T12:10:40Z","date_created":"2026-05-04T12:10:40Z","relation":"main_file","creator":"dernst","success":1,"access_level":"open_access","file_id":"21794","file_name":"2026_MNRAS_Elms.pdf","content_type":"application/pdf"}],"language":[{"iso":"eng"}],"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","image":"/images/cc_by.png","short":"CC BY (4.0)"},"title":"Detection of a weak magnetic field in the Balmer emission line white dwarf WDJ1653−1001","file_date_updated":"2026-05-04T12:10:40Z","abstract":[{"text":"The small DAHe and DAe spectral classes comprise isolated, hydrogen-dominated atmosphere white dwarfs that exhibit variable photometric flux and Balmer line emission. These mysterious systems offer unique insight into the complex interplay between magnetic fields, stellar rotation and atmospheric activity in single white dwarfs. DAHe stars have detectable magnetic fields through Zeeman-split spectral lines, whereas DAe stars lack such splitting. We report the first discovery and characterization of magnetism in the DAe white dwarf WD J165335.21−100116.33 with new time-resolved spectropolarimetry from FORS2. We detect a weak but variable longitudinal magnetic field with values Bz > −9.2 ± 2.4 kG and Bz < −2.2 ± 1.0 kG. Independent ZTF and ATLAS photometry reveal a consistent period of P = 80.3070 ± 0.0007 h. Time-resolved optical spectroscopy obtained with six ground-based instruments demonstrates strong modulation in the strength of the Hα and Hβ Balmer line emission with P = 80.2922 ± 0.0108 h. The photometric flux and Balmer emission strength vary in antiphase, with the strongest magnetic detections coinciding with phases of low photometric flux and strong line emission. These characteristicssupport the theory that a magnetically active, temperature-inverted spot/region is producing an optically thin chromospheric emission region. Comparison with other DAe and DAHe white dwarfsreveals all systems have a strikingly similar antiphase phenomenology, reinforcing the theory that they are subject to a unified physical mechanism. With the detection of a weak magnetic field, we reclassify WD J165335.21−100116.33 as a low-field DAHe white dwarf. ","lang":"eng"}],"date_updated":"2026-05-04T12:11:53Z","type":"journal_article","_id":"21745","status":"public","publisher":"Oxford University Press","DOAJ_listed":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","doi":"10.1093/mnras/stag505"},{"external_id":{"arxiv":["2606.11293"]},"language":[{"iso":"eng"}],"fulldoi":"https://doi.org/10.33232/001c.164326","file":[{"date_created":"2026-07-13T09:05:36Z","relation":"main_file","success":1,"creator":"dernst","file_size":1994596,"date_updated":"2026-07-13T09:05:36Z","checksum":"6320fd19e5ea3399f332be5aab022736","content_type":"application/pdf","file_name":"2026_OpenJourAstrophysics_ElBadry.pdf","access_level":"open_access","file_id":"22282"}],"date_published":"2026-06-30T00:00:00Z","day":"30","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","image":"/images/cc_by.png","short":"CC BY (4.0)"},"keyword":["white dwarfs","binaries: close","stars: chemically peculiar"],"supplementarymaterial":"no","date_updated":"2026-07-13T09:09:34Z","title":"A systematic survey for hypervelocity runaways from thermonuclear supernovae","abstract":[{"lang":"eng","text":"The explosion of a white dwarf (WD) in a close binary can launch a surviving runaway star at\r\nvelocities of ≳ 1000 km s−1\r\n. Such runaways provide a direct probe of thermonuclear supernovae (SNe)\r\nin double-degenerate binaries. Several candidate runaways are known, but their evolutionary states\r\nand the demographics of the broader population are uncertain. To enable robust population inference,\r\nwe carry out a systematic survey for hypervelocity runaways with a simple selection function, selecting\r\ncandidates based on large Gaia-inferred tangential velocities and blue colors. We classify 100% of the\r\nresulting 92 candidates using a combination of spectroscopic follow-up and archival data. The search\r\nyields ten suspected D6\r\nstars and three LP 40-365 stars. Three D6\r\nstars are new discoveries, including\r\ntwo hot (Teff ≳ 50,000 K) objects and one cool (Teff ≈ 7,000 K) object. We forward-model our survey\r\nunder several proposed D6\r\nstar evolutionary models, coupling each to a Galactic model and the survey\r\nselection function. No single model reproduces the observed diversity of D6\r\nstars, which likely reflects\r\na range of remnant masses, ages, and heating mechanisms. Models in which runaway companions\r\nare heated by SN shocks alone are too faint and short-lived to explain most of the observed sample,\r\nwhile fully reheated models are too luminous and long-lived. Models with intermediate heating,\r\nas occurs in some simulations of violent mergers and partially disrupted remnants, best match the\r\nobserved magnitude, distance, and kinematic-age distributions. The inferred D6\r\nstar birth rate is\r\nmodel dependent, but the models that best match the observed population require rates of only a\r\nfew percent of the Galactic SN Ia rate, perhaps implying that most SNe Ia result from WD binaries\r\nin which both components explode. If most SNe Ia do produce surviving runaways, these must be\r\nfainter or shorter-lived than the currently known runaways."}],"file_date_updated":"2026-07-13T09:05:36Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","DOAJ_listed":"1","publisher":"Maynooth Academic Publishing","doi":"10.33232/001c.164326","status":"public","_id":"22270","type":"journal_article","author":[{"last_name":"El-Badry","first_name":"Kareem","full_name":"El-Badry, Kareem"},{"first_name":"Klaus","full_name":"Werner, Klaus","last_name":"Werner"},{"last_name":"Shen","first_name":"Ken J.","full_name":"Shen, Ken J."},{"full_name":"Strader, Jay","first_name":"Jay","last_name":"Strader"},{"first_name":"Antonio C.","full_name":"Rodriguez, Antonio C.","last_name":"Rodriguez"},{"full_name":"Han, Jiwon Jesse","first_name":"Jiwon Jesse","last_name":"Han"},{"last_name":"Chandra","first_name":"Vedant","full_name":"Chandra, Vedant"},{"first_name":"Laura","full_name":"Chomiuk, Laura","last_name":"Chomiuk"},{"first_name":"Zachary P.","full_name":"Vanderbosch, Zachary P.","last_name":"Vanderbosch"},{"full_name":"Blomberg, Lisa","first_name":"Lisa","last_name":"Blomberg"},{"last_name":"Yamaguchi","first_name":"Natsuko","full_name":"Yamaguchi, Natsuko"},{"full_name":"Nagarajan, Pranav","first_name":"Pranav","last_name":"Nagarajan"},{"last_name":"Caiazzo","first_name":"Ilaria","orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d"},{"id":"4d122fc8-6083-11f0-87a5-97d68b860333","full_name":"van Roestel, Joannes C","first_name":"Joannes C","last_name":"van Roestel"},{"last_name":"Glanz","first_name":"Hila","full_name":"Glanz, Hila"},{"full_name":"Wong, Tin Long Sunny","first_name":"Tin Long Sunny","last_name":"Wong"},{"last_name":"Bhat","full_name":"Bhat, Aakash","first_name":"Aakash"},{"first_name":"Mark A.","full_name":"Hollands, Mark A.","last_name":"Hollands"}],"article_type":"original","publication_status":"published","ddc":["520"],"oa":1,"year":"2026","article_processing_charge":"No","month":"06","oa_version":"Published Version","intvolume":" 9","citation":{"chicago":"El-Badry, Kareem, Klaus Werner, Ken J. Shen, Jay Strader, Antonio C. Rodriguez, Jiwon Jesse Han, Vedant Chandra, et al. “A Systematic Survey for Hypervelocity Runaways from Thermonuclear Supernovae.” The Open Journal of Astrophysics. Maynooth Academic Publishing, 2026. https://doi.org/10.33232/001c.164326.","short":"K. El-Badry, K. Werner, K.J. Shen, J. Strader, A.C. Rodriguez, J.J. Han, V. Chandra, L. Chomiuk, Z.P. Vanderbosch, L. Blomberg, N. Yamaguchi, P. Nagarajan, I. Caiazzo, J.C. van Roestel, H. Glanz, T.L.S. Wong, A. Bhat, M.A. Hollands, The Open Journal of Astrophysics 9 (2026).","apa":"El-Badry, K., Werner, K., Shen, K. J., Strader, J., Rodriguez, A. C., Han, J. J., … Hollands, M. A. (2026). A systematic survey for hypervelocity runaways from thermonuclear supernovae. The Open Journal of Astrophysics. Maynooth Academic Publishing. https://doi.org/10.33232/001c.164326","ieee":"K. El-Badry et al., “A systematic survey for hypervelocity runaways from thermonuclear supernovae,” The Open Journal of Astrophysics, vol. 9. Maynooth Academic Publishing, 2026.","mla":"El-Badry, Kareem, et al. “A Systematic Survey for Hypervelocity Runaways from Thermonuclear Supernovae.” The Open Journal of Astrophysics, vol. 9, Maynooth Academic Publishing, 2026, doi:10.33232/001c.164326.","ama":"El-Badry K, Werner K, Shen KJ, et al. A systematic survey for hypervelocity runaways from thermonuclear supernovae. The Open Journal of Astrophysics. 2026;9. doi:10.33232/001c.164326","ista":"El-Badry K, Werner K, Shen KJ, Strader J, Rodriguez AC, Han JJ, Chandra V, Chomiuk L, Vanderbosch ZP, Blomberg L, Yamaguchi N, Nagarajan P, Caiazzo I, van Roestel JC, Glanz H, Wong TLS, Bhat A, Hollands MA. 2026. A systematic survey for hypervelocity runaways from thermonuclear supernovae. The Open Journal of Astrophysics. 9."},"has_accepted_license":"1","das_tickbox":"1","date_created":"2026-07-12T22:02:19Z","scopus_import":"1","department":[{"_id":"IlCa"}],"publication":"The Open Journal of Astrophysics","researchdata_availability":"no","acknowledgement":"We thank Lars Bildsten, Evan Bauer, Ruediger Pakmor, Jim Fuller, Logan Proust, Abinaya Rajamuthukumar, and Stephan Geier for useful discussion related to\r\nthis work.\r\nThis work was supported by NSF grants AST-2508988\r\nand AST-2205631, NASA/ESA Hubble Space Telescope\r\nprogram No. 17441, and Scialog grant #SA-LSST-2024-\r\n114c from the Research Corporation for Science Advancement. The Kavli Institute for Theoretical Physics\r\n(KITP) hosted the program, “White Dwarfs as Probes of\r\nthe Evolution of Planets, Stars, the Milky Way, and the\r\nExpanding Universe,” during which this project was initiated. This research was supported in part by the U.S.\r\nNational Science Foundation (NSF) under grants PHY1748958. This research benefited from discussions that\r\nwere funded by the Gordon and Betty Moore Foundation\r\nthrough Grant GBMF5076.\r\nWe thank the staffs of the various observatories at\r\nwhich data were obtained. This work is partially based\r\non observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project\r\nof the Minist´erio da Ciˆencia, Tecnologia e Inova¸c˜oes\r\n(MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina\r\nat Chapel Hill (UNC), and Michigan State University\r\n(MSU). Some of the data presented herein were obtained\r\nat the W. M. Keck Observatory, which is operated as a\r\nscientific partnership among the California Institute of\r\nTechnology, the University of California, and NASA; the observatory was made possible by the generous financial\r\nsupport of the W. M. Keck Foundation.\r\nThis research has made use of the Keck Observatory\r\nArchive (KOA), which is operated by the W. M. Keck\r\nObservatory and the NASA Exoplanet Science Institute\r\n(NExScI), under contract with the National Aeronautics\r\nand Space Administration.\r\nThis work has made use of data from the\r\nEuropean Space Agency (ESA) mission Gaia\r\n(https://www.cosmos.esa.int/gaia), processed\r\nby the Gaia Data Processing and Analysis Consortium\r\n(DPAC, https://www.cosmos.esa.int/web/gaia/\r\ndpac/consortium). Funding for the DPAC has been\r\nprovided by national institutions, in particular the\r\ninstitutions participating in the Gaia Multilateral\r\nAgreement.","dataavailabilitystatement":"We thank the staffs of the various observatories at\r\nwhich data were obtained. This work is partially based\r\non observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project\r\nof the Minist´erio da Ciˆencia, Tecnologia e Inova¸c˜oes\r\n(MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina\r\nat Chapel Hill (UNC), and Michigan State University\r\n(MSU). Some of the data presented herein were obtained\r\nat the W. M. Keck Observatory, which is operated as a\r\nscientific partnership among the California Institute of\r\nTechnology, the University of California, and NASA; the\r\nobservatory was made possible by the generous financial\r\nsupport of the W. M. Keck Foundation.\r\nThis research has made use of the Keck Observatory\r\nArchive (KOA), which is operated by the W. M. Keck\r\nObservatory and the NASA Exoplanet Science Institute\r\n(NExScI), under contract with the National Aeronautics\r\nand Space Administration.\r\nThis work has made use of data from the\r\nEuropean Space Agency (ESA) mission Gaia\r\n(https://www.cosmos.esa.int/gaia), processed\r\nby the Gaia Data Processing and Analysis Consortium\r\n(DPAC, https://www.cosmos.esa.int/web/gaia/\r\ndpac/consortium). Funding for the DPAC has been\r\nprovided by national institutions, in particular the\r\ninstitutions participating in the Gaia Multilateral\r\nAgreement.","volume":9,"publication_identifier":{"eissn":["2565-6120"]},"arxiv":1,"OA_place":"publisher","quality_controlled":"1","OA_type":"gold","PlanS_conform":"1"},{"file_date_updated":"2026-07-13T14:35:34Z","abstract":[{"text":"We present the discovery of AT 2024wpp (‘Whippet’), a fast and luminous 18cow-like transient. At a redshift of z = 0 . 0868 , revealed by Keck Cosmic Web Imager spectroscopy of its faint star-forming host, it is the fourth-nearest example of its class to date. Rapid identification of the source in the Zwicky Transient Facility data stream permitted ultraviolet-through- optical observations to be obtained prior to peak, allowing the first determination of the peak bolometric luminosity ( 2 ×1045 erg s−1 ), maximum photospheric radius ( 1015 cm), and total radiated energy ( 1051 erg) of an 18cow-like object. We present results from a comprehensive multiwavelength observing campaign, including a far-ultraviolet spectrum from the Cosmic Origins Spectrograph on the Hubble Space Telescope and deep imaging extending > 100 d post-explosion from the Very Large Telescope, Hubble Space Telescope , Very Large Array, and Atacama Large Millimetre Array. We interpret the observations under a model in which a rapidly accreting central engine blows a fast ( ∼0.2 c ) wind into the surrounding medium and irradiates it with X-rays. The high Doppler velocities and intense ionization within this wind prevent identifiable spectroscopic features from appearing in the ejecta or in the surrounding circumstellar material. Weak H and He signatures do emerge in the spectra after 35 d in the form of double-peaked narrow lines. Each peak is individually narrow (full width δv ∼3000 km s−1 ) but the two components are separated by \u0003v ∼6600 km s−1 , indicating stable structures of denser material, possibly representing streams of tidal ejecta or an ablated companion star.","lang":"eng"}],"title":"AT 2024wpp: An extremely luminous fast ultraviolet transient powered by accretion onto a black hole","date_updated":"2026-07-13T14:36:24Z","type":"journal_article","_id":"22303","status":"public","doi":"10.1093/mnras/stag678","publisher":"Oxford University Press","DOAJ_listed":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","day":"01","date_published":"2026-06-01T00:00:00Z","file":[{"file_id":"22314","access_level":"open_access","content_type":"application/pdf","file_name":"2026_MNRAS_Perley.pdf","date_updated":"2026-07-13T14:35:34Z","checksum":"a5827b9f68f1731b8c8df18142c0ef38","file_size":6208809,"creator":"dernst","success":1,"date_created":"2026-07-13T14:35:34Z","relation":"main_file"}],"fulldoi":"https://doi.org/10.1093/mnras/stag678","language":[{"iso":"eng"}],"external_id":{"arxiv":["2601.03337"]},"supplementarymaterial":"yes","keyword":["stars: black holes","supernovae: individual: AT2024wpp","radio continuum: transients"],"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","image":"/images/cc_by.png","short":"CC BY (4.0)"},"researchdata_availability":"upon request","publication":"Monthly Notices of the Royal Astronomical Society","department":[{"_id":"IlCa"}],"scopus_import":"1","das_tickbox":"1","date_created":"2026-07-13T10:50:10Z","has_accepted_license":"1","citation":{"chicago":"Perley, Daniel A, Anna Y Q Ho, Zoë McGrath, Michael Camilo, Cassie Sevilla, Ping Chen, Genevieve Schroeder, et al. “AT 2024wpp: An Extremely Luminous Fast Ultraviolet Transient Powered by Accretion onto a Black Hole.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2026. https://doi.org/10.1093/mnras/stag678.","apa":"Perley, D. A., Ho, A. Y. Q., McGrath, Z., Camilo, M., Sevilla, C., Chen, P., … Young, D. R. (2026). AT 2024wpp: An extremely luminous fast ultraviolet transient powered by accretion onto a black hole. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stag678","ieee":"D. A. Perley et al., “AT 2024wpp: An extremely luminous fast ultraviolet transient powered by accretion onto a black hole,” Monthly Notices of the Royal Astronomical Society, vol. 549, no. 1. Oxford University Press, 2026.","short":"D.A. Perley, A.Y.Q. Ho, Z. McGrath, M. Camilo, C. Sevilla, P. Chen, G. Schroeder, T. Govreen-Segal, A. Bochenek, Y.-J. Qin, J.H. Gillanders, B. Amend, J.P. Anderson, I. Andreoni, A. Aryan, E.C. Bellm, J.S. Bloom, T. de Boer, J. Carney, I. Caiazzo, K.C. Chambers, P. Charalampopoulos, T.-W. Chen, T.X. Chen, E.R. Coughlin, M. Coughlin, M. Dennefeld, G. Dimitriadis, C. Fremling, D. Frostig, A. Gal-Yam, L. Galbany, A. Gangopadhyay, M. Ghendrih, M.J. Graham, M. Gromadzki, S.L. Groom, C.P. Gutiérrez, K.-R. Hinds, M.E. Huber, C. Inserra, B.C. Kaiser, M.M. Kasliwal, N.E. Koivisto, C.-C. Lin, C. Liu, T.B. Lowe, E. Magnier, A.A. Mahabal, A. Milligan, P. Minguez, G. Mo, T.E. Müller-Bravo, M. Nicholl, P.J. Pessi, G. Pignata, J. Purdum, N. Rehemtulla, R.M. Rich, A. Sahu, A. Singh, S.J. Smartt, I.A. Smith, J. Sollerman, G. Srinivasaragavan, S. Srivastav, R.D. Stein, S. Schulze, J.W. Tweddle, R. Wainscoat, J.L. Wise, L. Yan, D.R. Young, Monthly Notices of the Royal Astronomical Society 549 (2026).","ama":"Perley DA, Ho AYQ, McGrath Z, et al. AT 2024wpp: An extremely luminous fast ultraviolet transient powered by accretion onto a black hole. Monthly Notices of the Royal Astronomical Society. 2026;549(1). doi:10.1093/mnras/stag678","mla":"Perley, Daniel A., et al. “AT 2024wpp: An Extremely Luminous Fast Ultraviolet Transient Powered by Accretion onto a Black Hole.” Monthly Notices of the Royal Astronomical Society, vol. 549, no. 1, stag678, Oxford University Press, 2026, doi:10.1093/mnras/stag678.","ista":"Perley DA, Ho AYQ, McGrath Z, Camilo M, Sevilla C, Chen P, Schroeder G, Govreen-Segal T, Bochenek A, Qin Y-J, Gillanders JH, Amend B, Anderson JP, Andreoni I, Aryan A, Bellm EC, Bloom JS, de Boer T, Carney J, Caiazzo I, Chambers KC, Charalampopoulos P, Chen T-W, Chen TX, Coughlin ER, Coughlin M, Dennefeld M, Dimitriadis G, Fremling C, Frostig D, Gal-Yam A, Galbany L, Gangopadhyay A, Ghendrih M, Graham MJ, Gromadzki M, Groom SL, Gutiérrez CP, Hinds K-R, Huber ME, Inserra C, Kaiser BC, Kasliwal MM, Koivisto NE, Lin C-C, Liu C, Lowe TB, Magnier E, Mahabal AA, Milligan A, Minguez P, Mo G, Müller-Bravo TE, Nicholl M, Pessi PJ, Pignata G, Purdum J, Rehemtulla N, Rich RM, Sahu A, Singh A, Smartt SJ, Smith IA, Sollerman J, Srinivasaragavan G, Srivastav S, Stein RD, Schulze S, Tweddle JW, Wainscoat R, Wise JL, Yan L, Young DR. 2026. AT 2024wpp: An extremely luminous fast ultraviolet transient powered by accretion onto a black hole. Monthly Notices of the Royal Astronomical Society. 549(1), stag678."},"PlanS_conform":"1","OA_type":"gold","OA_place":"publisher","quality_controlled":"1","arxiv":1,"volume":549,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"acknowledgement":"We thank Eliot Quataert, Luc Dessart, Ben Margalit, Ross Ferguson, Aaron Tohuvavohu, Brad Cenko, and Jamie Kennea for useful discussions. We thank the referee for helpful suggestions that improved the manuscript.\r\n\r\nBased on observations obtained with the Samuel Oschin Telescope 48-in. and the 60-in. Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant no. AST-2034437 and a collaboration including Caltech, IPAC, the Oskar Klein Center at Stockholm University, the University of Maryland, University of California, Berkeley, the University of Wisconsin at Milwaukee, University of Warwick, Ruhr University Bochum, Cornell University, Northwestern University and Drexel University. Operations are conducted by COO, IPAC, and UW.\r\n\r\nThe Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council.\r\n\r\nBased on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The NOT data were obtained under program ID 68–501.\r\n\r\nThis work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We are grateful to Phil Evans, Aaron Tohuvavohu, and Jamie Kennea for advice on the Swift/XRT data reduction.\r\n\r\nSome of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\r\n\r\nSome observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution.\r\n\r\nThe National Radio Astronomy Observatory and Green Bank Observatory are facilities of the U.S. National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO.ALMA no. 2023.1.01730.T ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSTC 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.\r\n\r\nBased on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 2114.D-5014(E). We thank John Pritchard and Paula Sanchez Saez, and the entire observatory staff, for their excellent support.\r\n\r\nBased on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, as part of ePESSTO+ (the advanced Public ESO Spectroscopic Survey for Transient Objects Survey – PI: Inserra). ePESSTO+ observations were obtained under ESO program ID 112.25JQ.\r\n\r\nThis research is based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. These observations are associated with programs 16714, 17477, and 17889.\r\n\r\nBased on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia e Inovações (MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU).\r\n\r\nThe Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant no. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant no. AST–1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation.\r\n\r\nThis research made use of ccdproc, an astropy package for image reduction (M. Craig et al. 2025).\r\n\r\nGS and AYQH acknowledge support in part from a Sloan Research Fellowship (award no. FG-2024-21320) from the Alfred P. Sloan Foundation. CS and AYQH acknowledge support in part from National Aeronautics and Space Administration (NASA) grant 80NSSC24K0377, from HST grant HST-GO-17477.006-A, and from a Scialog award from the Research Corporation for Science Advancement (‘Early Science with the LSST’).\r\n\r\nPC acknowledges support from the Zhejiang Provincial Top-Level Research Support Program.\r\n\r\nIA and JC are supported by the National Science Foundation award AST 2505775, NASA grant 24-ADAP24-0159, Scialog award SA-LSST-2024-102a, and the Discovery Alliance Catalyst Fellowship Mentors award 2025-62192-CM-19\r\n\r\nAA acknowledges support from the Ministry of Education Yushan Fellow Program (MOE-111-YSFMS-0008-001-P1) and from the National Science and Technology Council, Taiwan (NSTC 114-2112-M-008-021-MY3).\r\n\r\nT-WC acknowledges support from the Ministry of Education Yushan Fellow Program (MOE-111-YSFMS-0008-001-P1) and from the National Science and Technology Council, Taiwan (NSTC 114-2112-M-008-021-MY3).\r\n\r\nERC acknowledges support from the National Aeronautics and Space Administration through the Astrophysics Theory Program, grant 80NSSC24K0897.\r\n\r\nGD acknowledges support from the European Union’s Horizon Europe research and innovation programme under the Marie Skłodowska-Curie grant agreement no. 101199369.\r\n\r\nDF’s contribution to this material is based upon work supported by the National Science Foundation under award no. AST-2401779.\r\n\r\nAGY’s research is supported by ISF, IMOS, and BSF grants, as well as the André Deloro Institute for Space and Optics Research, the Center for Experimental Physics, a WIS-MIT Sagol grant, the Norman E Alexander Family M Foundation ULTRASAT Data Center Fund, and Yeda-Sela; AGY is the incumbent of the The Arlyn Imberman Professorial Chair.\r\n\r\nLG acknowledges financial support from AGAUR, CSIC, MCIN, and AEI 10.13039/501100011033 under projects PID2023-151307NB-I00, PIE 20215AT016, and CEX2020-001058-M.\r\n\r\nMG acknowledges support from an STFC PhD studentship and from the Faculty of Science and Technology at Lancaster University.\r\n\r\nCPG acknowledges financial support from the Secretary of Universities and Research (Government of Catalonia) and by the Horizon 2020 Research and Innovation Programme of the European Union under the Marie Skłodowska-Curie and the Beatriu de Pinós 2021 BP 00168 programme, from the Spanish Ministerio de Ciencia e Innovación (MCIN) and the Agencia Estatal de Investigación (AEI) 10.13039/501100011033 under the PID2023-151307NB-I00 SNNEXT project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016 and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M, and from the Departament de Recerca i Universitats de la Generalitat de Catalunya through the 2021-SGR-01270 grant.\r\n\r\nCL is supported by DoE award no. DE-SC0025599.\r\n\r\nZwicky Transient Facility, W. M. Keck Observatory, and MMT Observatory access was supported by Northwestern University and the Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA).\r\n\r\nAM gratefully acknowledges support from an STFC PhD studentship and the Faculty of Science and Technology at Lancaster University.\r\n\r\nTEMB is funded by Horizon Europe ERC grant no. 101125877.\r\n\r\nMN is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 948381).\r\n\r\nNR is supported by a Northwestern University Presidential Fellowship Award. We gratefully acknowledge the support of the NSF-Simons AI-Institute for the Sky (SkAI) via grants NSF AST-2421845 and Simons Foundation MPS-AI-00010513.\r\n\r\nAS acknowledges the Warwick Astrophysics PhD prize scholarship made possible thanks to a generous philanthropic donation.\r\n\r\nSJS acknowledges funding from STFC grant ST/Y001605/1, a Royal Society Research Professorship and the Hintze Family Charitable Foundation.","dataavailabilitystatement":"All photometry is provided in the supplementary data files. Spectroscopy will be made available on WISEREP, and is available on request to the lead author.","article_number":"stag678","ddc":["520"],"article_type":"original","publication_status":"published","author":[{"full_name":"Perley, Daniel A","first_name":"Daniel A","last_name":"Perley"},{"full_name":"Ho, Anna Y Q","first_name":"Anna Y Q","last_name":"Ho"},{"full_name":"McGrath, Zoë","first_name":"Zoë","last_name":"McGrath"},{"full_name":"Camilo, Michael","first_name":"Michael","last_name":"Camilo"},{"last_name":"Sevilla","full_name":"Sevilla, Cassie","first_name":"Cassie"},{"last_name":"Chen","first_name":"Ping","full_name":"Chen, Ping"},{"full_name":"Schroeder, Genevieve","first_name":"Genevieve","last_name":"Schroeder"},{"last_name":"Govreen-Segal","first_name":"Taya","full_name":"Govreen-Segal, Taya"},{"first_name":"Aleksandra","full_name":"Bochenek, Aleksandra","last_name":"Bochenek"},{"full_name":"Qin, Yu-Jing","first_name":"Yu-Jing","last_name":"Qin"},{"full_name":"Gillanders, James H","first_name":"James H","last_name":"Gillanders"},{"first_name":"Benjamin","full_name":"Amend, Benjamin","last_name":"Amend"},{"full_name":"Anderson, Joseph P","first_name":"Joseph P","last_name":"Anderson"},{"last_name":"Andreoni","full_name":"Andreoni, Igor","first_name":"Igor"},{"last_name":"Aryan","first_name":"Amar","full_name":"Aryan, Amar"},{"first_name":"Eric C","full_name":"Bellm, Eric C","last_name":"Bellm"},{"first_name":"Joshua S","full_name":"Bloom, Joshua S","last_name":"Bloom"},{"last_name":"de Boer","first_name":"Thomas","full_name":"de Boer, Thomas"},{"first_name":"Jonathan","full_name":"Carney, Jonathan","last_name":"Carney"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","last_name":"Caiazzo"},{"last_name":"Chambers","full_name":"Chambers, Ken C","first_name":"Ken C"},{"last_name":"Charalampopoulos","first_name":"Panos","full_name":"Charalampopoulos, Panos"},{"first_name":"Ting-Wan","full_name":"Chen, Ting-Wan","last_name":"Chen"},{"full_name":"Chen, Tracy X","first_name":"Tracy X","last_name":"Chen"},{"last_name":"Coughlin","first_name":"Eric R","full_name":"Coughlin, Eric R"},{"first_name":"Michael","full_name":"Coughlin, Michael","last_name":"Coughlin"},{"last_name":"Dennefeld","first_name":"Michel","full_name":"Dennefeld, Michel"},{"last_name":"Dimitriadis","first_name":"Georgios","full_name":"Dimitriadis, Georgios"},{"last_name":"Fremling","first_name":"Christoffer","full_name":"Fremling, Christoffer"},{"last_name":"Frostig","first_name":"Danielle","full_name":"Frostig, Danielle"},{"last_name":"Gal-Yam","full_name":"Gal-Yam, Avishay","first_name":"Avishay"},{"last_name":"Galbany","first_name":"Lluís","full_name":"Galbany, Lluís"},{"first_name":"Anjashay","full_name":"Gangopadhyay, Anjashay","last_name":"Gangopadhyay"},{"last_name":"Ghendrih","full_name":"Ghendrih, Melzie","first_name":"Melzie"},{"first_name":"Matthew J","full_name":"Graham, Matthew J","last_name":"Graham"},{"full_name":"Gromadzki, Mariusz","first_name":"Mariusz","last_name":"Gromadzki"},{"full_name":"Groom, Steven L","first_name":"Steven L","last_name":"Groom"},{"full_name":"Gutiérrez, Claudia P","first_name":"Claudia P","last_name":"Gutiérrez"},{"last_name":"Hinds","full_name":"Hinds, K -Ryan","first_name":"K -Ryan"},{"full_name":"Huber, Mark E","first_name":"Mark E","last_name":"Huber"},{"full_name":"Inserra, Cosimo","first_name":"Cosimo","last_name":"Inserra"},{"last_name":"Kaiser","first_name":"Benjamin C","full_name":"Kaiser, Benjamin C"},{"first_name":"Mansi M","full_name":"Kasliwal, Mansi M","last_name":"Kasliwal"},{"first_name":"Niilo E","full_name":"Koivisto, Niilo E","last_name":"Koivisto"},{"full_name":"Lin, Chien-Cheng","first_name":"Chien-Cheng","last_name":"Lin"},{"first_name":"Chang","full_name":"Liu, Chang","last_name":"Liu"},{"last_name":"Lowe","full_name":"Lowe, Thomas B","first_name":"Thomas B"},{"last_name":"Magnier","full_name":"Magnier, Eugene","first_name":"Eugene"},{"last_name":"Mahabal","first_name":"Ashish A","full_name":"Mahabal, Ashish A"},{"full_name":"Milligan, Andrew","first_name":"Andrew","last_name":"Milligan"},{"last_name":"Minguez","full_name":"Minguez, Paloma","first_name":"Paloma"},{"full_name":"Mo, Geoffrey","first_name":"Geoffrey","last_name":"Mo"},{"first_name":"Tomás E","full_name":"Müller-Bravo, Tomás E","last_name":"Müller-Bravo"},{"last_name":"Nicholl","full_name":"Nicholl, Matt","first_name":"Matt"},{"first_name":"Priscila J","full_name":"Pessi, Priscila J","last_name":"Pessi"},{"first_name":"Giuliano","full_name":"Pignata, Giuliano","last_name":"Pignata"},{"first_name":"Josiah","full_name":"Purdum, Josiah","last_name":"Purdum"},{"first_name":"Nabeel","full_name":"Rehemtulla, Nabeel","last_name":"Rehemtulla"},{"first_name":"R Michael","full_name":"Rich, R Michael","last_name":"Rich"},{"last_name":"Sahu","full_name":"Sahu, Anwesha","first_name":"Anwesha"},{"last_name":"Singh","full_name":"Singh, Avinash","first_name":"Avinash"},{"first_name":"Stephen J","full_name":"Smartt, Stephen J","last_name":"Smartt"},{"last_name":"Smith","first_name":"Ian A","full_name":"Smith, Ian A"},{"first_name":"Jesper","full_name":"Sollerman, Jesper","last_name":"Sollerman"},{"full_name":"Srinivasaragavan, Gokul","first_name":"Gokul","last_name":"Srinivasaragavan"},{"last_name":"Srivastav","full_name":"Srivastav, Shubham","first_name":"Shubham"},{"last_name":"Stein","full_name":"Stein, Robert D","first_name":"Robert D"},{"first_name":"Steve","full_name":"Schulze, Steve","last_name":"Schulze"},{"first_name":"Jack W","full_name":"Tweddle, Jack W","last_name":"Tweddle"},{"last_name":"Wainscoat","full_name":"Wainscoat, Richard","first_name":"Richard"},{"last_name":"Wise","first_name":"Jacob L","full_name":"Wise, Jacob L"},{"last_name":"Yan","full_name":"Yan, Lin","first_name":"Lin"},{"last_name":"Young","first_name":"David R","full_name":"Young, David R"}],"intvolume":" 549","issue":"1","oa_version":"Published Version","month":"06","article_processing_charge":"Yes","oa":1,"year":"2026"},{"ddc":["520"],"article_type":"original","publication_status":"published","author":[{"last_name":"Stein","full_name":"Stein, Robert","first_name":"Robert"},{"full_name":"Carney, Jonathan","first_name":"Jonathan","last_name":"Carney"},{"last_name":"Ward","full_name":"Ward, Charlotte","first_name":"Charlotte"},{"full_name":"Margutti, Raffaella","first_name":"Raffaella","last_name":"Margutti"},{"last_name":"Hall","full_name":"Hall, Xander J.","first_name":"Xander J."},{"last_name":"Sfaradi","first_name":"Itai","full_name":"Sfaradi, Itai"},{"full_name":"Andreoni, Igor","first_name":"Igor","last_name":"Andreoni"},{"full_name":"Charalampopoulos, Panos","first_name":"Panos","last_name":"Charalampopoulos"},{"full_name":"Chornock, Ryan","first_name":"Ryan","last_name":"Chornock"},{"first_name":"Suvi","full_name":"Gezari, Suvi","last_name":"Gezari"},{"full_name":"Mo, Geoffrey","first_name":"Geoffrey","last_name":"Mo"},{"first_name":"Yuhan","full_name":"Yao, Yuhan","last_name":"Yao"},{"first_name":"Akash","full_name":"Anumarlapudi, Akash","last_name":"Anumarlapudi"},{"last_name":"Bellm","first_name":"Eric C.","full_name":"Bellm, Eric C."},{"last_name":"Bloom","full_name":"Bloom, Joshua S.","first_name":"Joshua S."},{"last_name":"Busmann","full_name":"Busmann, Malte","first_name":"Malte"},{"first_name":"Ilaria","full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","last_name":"Caiazzo"},{"full_name":"Cenko, S. Bradley","first_name":"S. Bradley","last_name":"Cenko"},{"last_name":"Graham","full_name":"Graham, Matthew J.","first_name":"Matthew J."},{"last_name":"Groom","first_name":"Steven L.","full_name":"Groom, Steven L."},{"last_name":"Gruen","first_name":"Daniel","full_name":"Gruen, Daniel"},{"full_name":"Hammerstein, Erica","first_name":"Erica","last_name":"Hammerstein"},{"last_name":"Kaiser","first_name":"Benjamin C.","full_name":"Kaiser, Benjamin C."},{"full_name":"Kasliwal, Mansi M.","first_name":"Mansi M.","last_name":"Kasliwal"},{"first_name":"Brendan","full_name":"O’Connor, Brendan","last_name":"O’Connor"},{"full_name":"Palmese, Antonella","first_name":"Antonella","last_name":"Palmese"},{"first_name":"Josiah","full_name":"Purdum, Josiah","last_name":"Purdum"},{"last_name":"Rastinejad","full_name":"Rastinejad, Jillian C.","first_name":"Jillian C."},{"last_name":"Riddle","full_name":"Riddle, Reed","first_name":"Reed"},{"first_name":"Ben","full_name":"Rusholme, Ben","last_name":"Rusholme"},{"first_name":"Jesper","full_name":"Sollerman, Jesper","last_name":"Sollerman"},{"full_name":"Somalwar, Jean J.","first_name":"Jean J.","last_name":"Somalwar"},{"full_name":"Veilleux, Sylvain","first_name":"Sylvain","last_name":"Veilleux"}],"intvolume":" 1006","issue":"2","oa_version":"Published Version","month":"07","article_processing_charge":"Yes","year":"2026","oa":1,"researchdata_availability":"no","publication":"The Astrophysical Journal Letters","scopus_import":"1","department":[{"_id":"IlCa"}],"date_created":"2026-08-11T06:19:19Z","das_tickbox":"0","has_accepted_license":"1","citation":{"chicago":"Stein, Robert, Jonathan Carney, Charlotte Ward, Raffaella Margutti, Xander J. Hall, Itai Sfaradi, Igor Andreoni, et al. “TDE 2025abcr: A Tidal Disruption Event in the Outskirts of a Massive Galaxy.” The Astrophysical Journal Letters. IOP Publishing, 2026. https://doi.org/10.3847/2041-8213/ae77f3.","ieee":"R. Stein et al., “TDE 2025abcr: A tidal disruption event in the outskirts of a massive galaxy,” The Astrophysical Journal Letters, vol. 1006, no. 2. IOP Publishing, 2026.","apa":"Stein, R., Carney, J., Ward, C., Margutti, R., Hall, X. J., Sfaradi, I., … Veilleux, S. (2026). TDE 2025abcr: A tidal disruption event in the outskirts of a massive galaxy. The Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ae77f3","short":"R. Stein, J. Carney, C. Ward, R. Margutti, X.J. Hall, I. Sfaradi, I. Andreoni, P. Charalampopoulos, R. Chornock, S. Gezari, G. Mo, Y. Yao, A. Anumarlapudi, E.C. Bellm, J.S. Bloom, M. Busmann, I. Caiazzo, S.B. Cenko, M.J. Graham, S.L. Groom, D. Gruen, E. Hammerstein, B.C. Kaiser, M.M. Kasliwal, B. O’Connor, A. Palmese, J. Purdum, J.C. Rastinejad, R. Riddle, B. Rusholme, J. Sollerman, J.J. Somalwar, S. Veilleux, The Astrophysical Journal Letters 1006 (2026).","mla":"Stein, Robert, et al. “TDE 2025abcr: A Tidal Disruption Event in the Outskirts of a Massive Galaxy.” The Astrophysical Journal Letters, vol. 1006, no. 2, L57, IOP Publishing, 2026, doi:10.3847/2041-8213/ae77f3.","ama":"Stein R, Carney J, Ward C, et al. TDE 2025abcr: A tidal disruption event in the outskirts of a massive galaxy. The Astrophysical Journal Letters. 2026;1006(2). doi:10.3847/2041-8213/ae77f3","ista":"Stein R, Carney J, Ward C, Margutti R, Hall XJ, Sfaradi I, Andreoni I, Charalampopoulos P, Chornock R, Gezari S, Mo G, Yao Y, Anumarlapudi A, Bellm EC, Bloom JS, Busmann M, Caiazzo I, Cenko SB, Graham MJ, Groom SL, Gruen D, Hammerstein E, Kaiser BC, Kasliwal MM, O’Connor B, Palmese A, Purdum J, Rastinejad JC, Riddle R, Rusholme B, Sollerman J, Somalwar JJ, Veilleux S. 2026. TDE 2025abcr: A tidal disruption event in the outskirts of a massive galaxy. The Astrophysical Journal Letters. 1006(2), L57."},"OA_type":"gold","PlanS_conform":"1","quality_controlled":"1","arxiv":1,"OA_place":"publisher","volume":1006,"publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"acknowledgement":"We thank Muryel Guolo, Dan Perley, and Carl Rodriguez for the fruitful discussions about off-nuclear TDEs.\r\n\r\nBased on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the ZTF project. ZTF is supported by the National Science Foundation under award #2407588 and a partnership including Caltech, USA; Caltech/IPAC, USA; University of Maryland, USA; University of California, Berkeley, USA; Cornell University, USA; Drexel University, USA; University of North Carolina at Chapel Hill, USA; Institute of Science and Technology, Austria; National Central University, Taiwan, and the German Center for Astrophysics (DZA), Germany. Operations are conducted by Caltech’s Optical Observatory (COO), Caltech/IPAC, and the University of Washington at Seattle, USA.\r\n\r\nSED Machine is based upon work supported by the National Science Foundation under grant No. 1106171.\r\n\r\nThe Gordon and Betty Moore Foundation, through both the Data-Driven Investigator Program and a dedicated grant, provided critical funding for SkyPortal.\r\n\r\nThese results were obtained with the use of LDT, owned and operated by the Lowell Observatory\r\n\r\nSome 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. The authors 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 the opportunity to conduct observations from this mountain.\r\n\r\nA major upgrade of the Kast spectrograph on the Shane 3 m telescope at Lick Observatory, led by Brad Holden, was made possible through gifts from the Heising-Simons Foundation, William and Marina Kast, and the University of California Observatories. Research at Lick Observatory is partially supported by a generous gift from Google.\r\n\r\nThis work is based (in part) on observations made with NOT, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias under NOT programmes 72-504. The NOT data presented here were obtained with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOT.\r\n\r\nThis work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester.\r\n\r\nThis paper contains data obtained at the Wendelstein Observatory of the Ludwig-Maximilians University Munich. We thank Christoph Ries for carrying out the observations. Funded in part by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy—EXC-2094/2—390783311.\r\n\r\nThe national facility capability for SkyMapper has been funded through ARC LIEF grant LE130100104 from the Australian Research Council, awarded to the University of Sydney, the Australian National University, Swinburne University of Technology, the University of Queensland, the University of Western Australia, the University of Melbourne, Curtin University of Technology, Monash University, and the Australian Astronomical Observatory. SkyMapper is owned and operated by The Australian National University’s Research School of Astronomy and Astrophysics. The survey data were processed and provided by the SkyMapper Team at ANU. The SkyMapper node of the All-Sky Virtual Observatory (ASVO) is hosted at the National Computational Infrastructure (NCI). Development and support of the SkyMapper node of the ASVO has been funded in part by Astronomy Australia Limited (AAL) and the Australian Government through the Commonwealth’s Education Investment Fund (EIF) and National Collaborative Research Infrastructure Strategy (NCRIS), particularly the National eResearch Collaboration Tools and Resources (NeCTAR) and the Australian National Data Service Projects (ANDS).\r\n\r\nThe National Radio Astronomy Observatory (NRAO) is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank the NRAO for carrying out the Karl G. Jansky VLA observation.\r\n\r\nNote Added - Shortly before this work was accepted, we became aware of a later preprint by K. Patra et al. (2026). The work reaches many similar conclusions to our own, and presents additional JWST data of TDE 2025abcr. We also thank the authors for highlighting a typo on an earlier version of this manuscript, with the projected offset incorrectly given as 10.3 kpc rather than 9.3 kpc.\r\n\r\nFacilities: PO:1.2m - Palomar Observatory's 1.2 meter Samuel Oschin Telescope (ZTF), Hale - Palomar Observatory's 5.1m Hale Telescope (protoCerberus), Keck:I - KECK I Telescope (LRIS), LDT - (DeVeney, LMI), NOT - Nordic Optical Telescope (ALFOSC), PO:1.5m - Palomar Observatory's 1.5 meter Telescope (SEDM), SOAR - The Southern Astrophysical Research Telescope (Goodman), Swift - Swift Gamma-Ray Burst Mission (XRT, UVOT) - , VLA - Very Large Array, WO:2m - (3KK).\r\n\r\nSoftware: astroquery (B. D. Johnson et al. 2021), emcee (D. Foreman-Mackey et al. 2013), HEASoft, galsynthspec (R. D. Stein 2025), mirar (R. D. Stein et al. 2025), prospector (B. D. Johnson et al. 2021), SCAMP (E. Bertin 2006), scarlet (P. Melchior et al. 2018), Source Extractor (E. Bertin & S. Arnouts 1996), swifttools, tdescore (R. Stein et al. 2024), uvotredux (R. D. Stein & J. Carney 2025).","article_number":"L57","date_published":"2026-07-27T00:00:00Z","day":"27","fulldoi":"https://doi.org/10.3847/2041-8213/ae77f3","file":[{"file_size":10322417,"date_updated":"2026-08-11T07:45:16Z","checksum":"42b983f18497bb644f422709de7dc68c","relation":"main_file","date_created":"2026-08-11T07:45:16Z","success":1,"creator":"dernst","access_level":"open_access","file_id":"22682","file_name":"2026_AstrophysicalJourLetters_Stein.pdf","content_type":"application/pdf"}],"language":[{"iso":"eng"}],"external_id":{"arxiv":["2602.10180"]},"supplementarymaterial":"yes","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","image":"/images/cc_by.png","short":"CC BY (4.0)"},"file_date_updated":"2026-08-11T07:45:16Z","abstract":[{"text":"Tidal disruption events (TDEs) have traditionally been discovered in optical sky surveys through targeted searches of nuclear transients. However, it is expected that some TDEs will occur outside the galaxy nucleus, arising from wandering black holes (BHs) originating in galaxy mergers. Here, we present observations of TDE 2025abcr, the first optical TDE discovered in the outskirts of a host galaxy. The TDE was identified by a custom “off-nuclear” implementation of the machine learning classifier tdescore, which classifies new ZTF transients based on their lightcurves. Follow-up observations confirm that TDE 2025abcr is a TDE-H+He, occurring 9\r\n5 (9.3 kpc projected distance) from the nucleus of a massive galaxy (M⋆ = 1011.18±0.03M⊙) with a central BH mass of 108.82±0.65M⊙. TDE 2025abcr itself was likely disrupted by a much lighter BH (106.09±0.53M⊙, as estimated with peak luminosity scaling relations). The BH was either dynamically ejected from the nucleus or lies at the center of a very faint tidally stripped dwarf galaxy undergoing a minor merger. Late-time observations of TDE 2025abcr could confirm the origin of this apparent “wandering” BH. The rate of highly offset (≳3 kpc) TDEs can be constrained to <10% of the nuclear TDE rate, but our discovery implies that many dozens of similar sources will be detected by the Vera C. Rubin Observatory each year with resolvable offsets.","lang":"eng"}],"title":"TDE 2025abcr: A tidal disruption event in the outskirts of a massive galaxy","date_updated":"2026-08-11T07:45:27Z","type":"journal_article","status":"public","_id":"22675","doi":"10.3847/2041-8213/ae77f3","publisher":"IOP Publishing","DOAJ_listed":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"_id":"21241","status":"public","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"IOP Publishing","doi":"10.1088/1538-3873/ade0ea","title":"A ZTF search for circumstellar debris transits in White Dwarfs: Six new candidates, one with gas disk emission, identified in a novel metric space","abstract":[{"text":"White dwarfs (WDs) showing transits from orbiting planetary debris provide significant insights into the structure and dynamics of debris disks, which are eventually accreted to produce metal pollution. This is a rare class of objects with only eight published systems. In this work, we perform a systematic search for such systems within 500 pc in the Gaia-eDR3 catalog of WDs using the light curves from the Zwicky Transient Facility (ZTF) and present six new candidates. Our selection process targets the top 1% most photometrically variable sources identified using a combined variability metric from ZTF and Gaia eDR3 photometry, boosted by a metric space we define using von Neumann statistics and Pearson-Skew as a novel discovery tool to identify these systems. This is followed by optical spectroscopic observations of visually selected variables to confirm metal pollution. Four of the six systems show long-timescale photometric variability spanning several months to years, resulting either from long-term evolution of transit activity or dust and debris clouds at wide orbits. Among them, WD J1013–0427 shows an indication of reddening during the long-duration dip. Interpreting this as dust extinction makes it the first system to indicate an abundance of dust grains with radius ≲0.3 μm in the occulting material. The same object also shows metal emission lines that map an optically thick eccentric gas disk orbiting within the star’s Roche limit. For each candidate, we infer the abundances of the photospheric metals and estimate accretion rates. We show that transiting debris systems tend to have higher inferred accretion rates compared to the general population of metal-polluted WDs. Growing the number of these systems will further illuminate such comparative properties in the near future. Separately, we also serendipitously discovered an AM Canis Venaticorum showing a very long-duration outburst—only the fourth such system to be known.","lang":"eng"}],"file_date_updated":"2026-02-17T11:30:29Z","date_updated":"2026-02-17T11:35:53Z","license":"https://creativecommons.org/licenses/by/3.0/","tmp":{"short":"CC BY (3.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/3.0/legalcode","name":"Creative Commons Attribution 3.0 Unported (CC BY 3.0)"},"date_published":"2025-07-09T00:00:00Z","day":"09","external_id":{"arxiv":["2502.05502"]},"language":[{"iso":"eng"}],"file":[{"file_size":8900420,"date_updated":"2026-02-17T11:30:29Z","checksum":"237eddc36e3823b3092fab6aa5bc8655","relation":"main_file","date_created":"2026-02-17T11:30:29Z","creator":"dernst","success":1,"access_level":"open_access","file_id":"21289","file_name":"2025_PASP_Bhattacharjee.pdf","content_type":"application/pdf"}],"fulldoi":"https://doi.org/10.1088/1538-3873/ade0ea","publication_identifier":{"issn":["1538-3873"]},"volume":137,"arxiv":1,"quality_controlled":"1","OA_place":"publisher","OA_type":"hybrid","PlanS_conform":"1","article_number":"074202","acknowledgement":"This work is 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. Z.T.F. is supported by the National Science Foundation under grants No. AST-1440341 and AST-2034437 and a collaboration including current partners Caltech, IPAC, the Oskar Klein Center at Stockholm University, the University of Maryland, University of California, Berkeley, the University of Wisconsin at Milwaukee, University of Warwick, Ruhr University Bochum, Cornell University, Northwestern University, and Drexel University. Operations are conducted by COO, IPAC, and UW.\r\n\r\nThis 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. This 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 has made use of the VizieR catalog access tool, CDS, Strasbourg, France https://vizier.cds.unistra.fr/. The original description of the VizieR service was published in Ochsenbein et al. (2000).\r\n\r\nWe are grateful to the staffs of Palomar and Keck Observatory for assistance with the observations and data management.\r\n\r\nThe authors thank the anonymous referee for very extensive and useful comments which improved the presentation of the paper significantly. S.B. acknowledges the support from the Kishore Vaigyanik Protsahan Yojana (KVPY) scheme of the Department of Science and Technology, Government of India (a former fellowship program for undergraduate studies in basic science) during his undergraduate studies at IISc. S.B. thanks the Summer Undergraduate Research Fellowship (SURF) at Caltech and Shrinivas R. Kulkarni for hosting him as a summer research student in 2022. S.B. acknowledges the financial support from the Wallace L. W. Sargent Graduate Fellowship during the first year of his graduate studies at Caltech. P.E.T. received funding from the European Research Council under the European Union’s Horizon 2020 research and innovation program number 101002408. S.X. 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. J.A.G. is supported by the National Science Foundation Graduate Research Fellowship Program under grant No. 2234657. This material is based upon work supported by the National Aeronautics and Space Administration under grant No. 80NSSC23K1068 issued through the Science Mission Directorate.\r\n\r\nWe have used Python packages Numpy (Harris et al. 2020), SciPy (Virtanen et al. 2020), Matplotlib (Hunter 2007), Pandas (The pandas development team 2020), Astropy (Astropy Collaboration et al. 2013, 2018), and Astroquery (Ginsburg et al. 2019) at various stages of this research.","date_created":"2026-02-16T15:10:51Z","department":[{"_id":"IlCa"}],"publication":"Publications of the Astronomical Society of the Pacific","citation":{"chicago":"Bhattacharjee, Soumyadeep , Zachary P. Vanderbosch, Mark A. Hollands, Pier-Emmanuel Tremblay, Siyi Xu, Joseph A. Guidry, J.J. Hermes, et al. “A ZTF Search for Circumstellar Debris Transits in White Dwarfs: Six New Candidates, One with Gas Disk Emission, Identified in a Novel Metric Space.” Publications of the Astronomical Society of the Pacific. IOP Publishing, 2025. https://doi.org/10.1088/1538-3873/ade0ea.","apa":"Bhattacharjee, S., Vanderbosch, Z. P., Hollands, M. A., Tremblay, P.-E., Xu, S., Guidry, J. A., … Toloza, O. (2025). A ZTF search for circumstellar debris transits in White Dwarfs: Six new candidates, one with gas disk emission, identified in a novel metric space. Publications of the Astronomical Society of the Pacific. IOP Publishing. https://doi.org/10.1088/1538-3873/ade0ea","ieee":"S. Bhattacharjee et al., “A ZTF search for circumstellar debris transits in White Dwarfs: Six new candidates, one with gas disk emission, identified in a novel metric space,” Publications of the Astronomical Society of the Pacific, vol. 137, no. 7. IOP Publishing, 2025.","short":"S. Bhattacharjee, Z.P. Vanderbosch, M.A. Hollands, P.-E. Tremblay, S. Xu, J.A. Guidry, J.J. Hermes, I. Caiazzo, A.C. Rodriguez, J. van Roestel, K. El-Badry, A.J. Drake, B.R. Roulston, R. Riddle, B. Rusholme, S.L. Groom, R. Smith, O. Toloza, Publications of the Astronomical Society of the Pacific 137 (2025).","ama":"Bhattacharjee S, Vanderbosch ZP, Hollands MA, et al. A ZTF search for circumstellar debris transits in White Dwarfs: Six new candidates, one with gas disk emission, identified in a novel metric space. Publications of the Astronomical Society of the Pacific. 2025;137(7). doi:10.1088/1538-3873/ade0ea","mla":"Bhattacharjee, Soumyadeep, et al. “A ZTF Search for Circumstellar Debris Transits in White Dwarfs: Six New Candidates, One with Gas Disk Emission, Identified in a Novel Metric Space.” Publications of the Astronomical Society of the Pacific, vol. 137, no. 7, 074202, IOP Publishing, 2025, doi:10.1088/1538-3873/ade0ea.","ista":"Bhattacharjee S, Vanderbosch ZP, Hollands MA, Tremblay P-E, Xu S, Guidry JA, Hermes JJ, Caiazzo I, Rodriguez AC, van Roestel J, El-Badry K, Drake AJ, Roulston BR, Riddle R, Rusholme B, Groom SL, Smith R, Toloza O. 2025. A ZTF search for circumstellar debris transits in White Dwarfs: Six new candidates, one with gas disk emission, identified in a novel metric space. Publications of the Astronomical Society of the Pacific. 137(7), 074202."},"has_accepted_license":"1","month":"07","issue":"7","intvolume":" 137","oa_version":"Published Version","oa":1,"year":"2025","article_processing_charge":"Yes (in subscription journal)","ddc":["520"],"author":[{"first_name":"Soumyadeep ","full_name":"Bhattacharjee, Soumyadeep ","last_name":"Bhattacharjee"},{"full_name":"Vanderbosch, Zachary P.","first_name":"Zachary P.","last_name":"Vanderbosch"},{"first_name":"Mark A.","full_name":"Hollands, Mark A.","last_name":"Hollands"},{"first_name":"Pier-Emmanuel","full_name":"Tremblay, Pier-Emmanuel","last_name":"Tremblay"},{"last_name":"Xu","first_name":"Siyi","full_name":"Xu, Siyi"},{"last_name":"Guidry","full_name":"Guidry, Joseph A.","first_name":"Joseph A."},{"last_name":"Hermes","first_name":"J.J.","full_name":"Hermes, J.J."},{"last_name":"Caiazzo","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria"},{"full_name":"Rodriguez, Antonio C.","first_name":"Antonio C.","last_name":"Rodriguez"},{"last_name":"van Roestel","full_name":"van Roestel, Jan","first_name":"Jan"},{"last_name":"El-Badry","first_name":"Kareem ","full_name":"El-Badry, Kareem "},{"last_name":"Drake","first_name":"Andrew J.","full_name":"Drake, Andrew J."},{"last_name":"Roulston","first_name":"Benjamin R.","full_name":"Roulston, Benjamin R."},{"full_name":"Riddle, Reed","first_name":"Reed","last_name":"Riddle"},{"last_name":"Rusholme","first_name":"Ben","full_name":"Rusholme, Ben"},{"last_name":"Groom","first_name":"Steven L.","full_name":"Groom, Steven L."},{"first_name":"Roger","full_name":"Smith, Roger","last_name":"Smith"},{"last_name":"Toloza","full_name":"Toloza, Odette","first_name":"Odette"}],"publication_status":"published","article_type":"original"},{"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"}],"file_date_updated":"2026-02-19T07:24:10Z","title":"Optical spectroscopy of the most compact accreting binary harboring a magnetic White Dwarf and a hydrogen-rich donor","date_updated":"2026-02-19T07:27:01Z","status":"public","_id":"21317","type":"journal_article","doi":"10.3847/2041-8213/adff82","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","DOAJ_listed":"1","publisher":"IOP Publishing","day":"08","date_published":"2025-09-08T00:00:00Z","language":[{"iso":"eng"}],"file":[{"access_level":"open_access","file_id":"21329","file_name":"2025_AstrophysicalJournal_Galiullin.pdf","content_type":"application/pdf","file_size":3772189,"checksum":"f76556d129aa0e9facc85602b0b5b54d","date_updated":"2026-02-19T07:24:10Z","relation":"main_file","date_created":"2026-02-19T07:24:10Z","creator":"dernst","success":1}],"fulldoi":"https://doi.org/10.3847/2041-8213/adff82","external_id":{"arxiv":["2508.20170"]},"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","image":"/images/cc_by.png","short":"CC BY (4.0)"},"publication":"The Astrophysical Journal Letters","date_created":"2026-02-18T10:17:04Z","scopus_import":"1","department":[{"_id":"IlCa"}],"has_accepted_license":"1","citation":{"ama":"Galiullin I, Rodriguez AC, El-Badry K, et al. Optical spectroscopy of the most compact accreting binary harboring a magnetic White Dwarf and a hydrogen-rich donor. The Astrophysical Journal Letters. 2025;990(2). doi:10.3847/2041-8213/adff82","mla":"Galiullin, Ilkham, et al. “Optical Spectroscopy of the Most Compact Accreting Binary Harboring a Magnetic White Dwarf and a Hydrogen-Rich Donor.” The Astrophysical Journal Letters, vol. 990, no. 2, L57, IOP Publishing, 2025, doi:10.3847/2041-8213/adff82.","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.","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.” The Astrophysical Journal Letters. IOP Publishing, 2025. https://doi.org/10.3847/2041-8213/adff82.","ieee":"I. Galiullin et al., “Optical spectroscopy of the most compact accreting binary harboring a magnetic White Dwarf and a hydrogen-rich donor,” The Astrophysical Journal Letters, vol. 990, no. 2. IOP Publishing, 2025.","apa":"Galiullin, I., Rodriguez, A. C., 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. IOP Publishing. https://doi.org/10.3847/2041-8213/adff82","short":"I. Galiullin, A.C. Rodriguez, K. El-Badry, I. Caiazzo, P. Szkody, P. Nagarajan, S. Whitebook, The Astrophysical Journal Letters 990 (2025)."},"OA_place":"publisher","arxiv":1,"quality_controlled":"1","OA_type":"gold","PlanS_conform":"1","volume":990,"publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"article_number":"L57","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.","ddc":["520"],"author":[{"first_name":"Ilkham","full_name":"Galiullin, Ilkham","last_name":"Galiullin"},{"last_name":"Rodriguez","full_name":"Rodriguez, Antonio C.","first_name":"Antonio C."},{"last_name":"El-Badry","first_name":"Kareem","full_name":"El-Badry, Kareem"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria","last_name":"Caiazzo"},{"first_name":"Paula","full_name":"Szkody, Paula","last_name":"Szkody"},{"full_name":"Nagarajan, Pranav","first_name":"Pranav","last_name":"Nagarajan"},{"full_name":"Whitebook, Samuel","first_name":"Samuel","last_name":"Whitebook"}],"article_type":"original","publication_status":"published","issue":"2","oa_version":"Published Version","intvolume":" 990","month":"09","oa":1,"year":"2025","article_processing_charge":"Yes"},{"year":"2025","oa":1,"article_processing_charge":"No","oa_version":"Published Version","intvolume":" 137","issue":"1","month":"01","author":[{"last_name":"Rodriguez","first_name":"Antonio C.","full_name":"Rodriguez, Antonio C."},{"first_name":"Kareem","full_name":"El-Badry, Kareem","last_name":"El-Badry"},{"last_name":"Suleimanov","first_name":"Valery","full_name":"Suleimanov, Valery"},{"last_name":"Pala","full_name":"Pala, Anna F.","first_name":"Anna F."},{"full_name":"Kulkarni, Shrinivas R.","first_name":"Shrinivas R.","last_name":"Kulkarni"},{"last_name":"Gaensicke","first_name":"Boris","full_name":"Gaensicke, Boris"},{"full_name":"Mori, Kaya","first_name":"Kaya","last_name":"Mori"},{"last_name":"Rich","full_name":"Rich, R. Michael","first_name":"R. Michael"},{"full_name":"Sarkar, Arnab","first_name":"Arnab","last_name":"Sarkar"},{"last_name":"Bao","full_name":"Bao, Tong","first_name":"Tong"},{"full_name":"De Oliveira, Raimundo Lopes","first_name":"Raimundo Lopes","last_name":"De Oliveira"},{"last_name":"Ramsay","first_name":"Gavin","full_name":"Ramsay, Gavin"},{"last_name":"Szkody","full_name":"Szkody, Paula","first_name":"Paula"},{"first_name":"Matthew","full_name":"Graham, Matthew","last_name":"Graham"},{"last_name":"Prince","full_name":"Prince, Thomas A.","first_name":"Thomas A."},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","first_name":"Ilaria","last_name":"Caiazzo"},{"last_name":"Vanderbosch","full_name":"Vanderbosch, Zachary P.","first_name":"Zachary P."},{"full_name":"Roestel, Jan Van","first_name":"Jan Van","last_name":"Roestel"},{"first_name":"Kaustav K.","full_name":"Das, Kaustav K.","last_name":"Das"},{"last_name":"Qin","first_name":"Yu Jing","full_name":"Qin, Yu Jing"},{"full_name":"Kasliwal, Mansi M.","first_name":"Mansi M.","last_name":"Kasliwal"},{"first_name":"Avery","full_name":"Wold, Avery","last_name":"Wold"},{"first_name":"Steven L.","full_name":"Groom, Steven L.","last_name":"Groom"},{"first_name":"Daniel","full_name":"Reiley, Daniel","last_name":"Reiley"},{"last_name":"Riddle","full_name":"Riddle, Reed","first_name":"Reed"}],"publication_status":"published","article_type":"original","ddc":["520"],"article_number":"014201","acknowledgement":"We thank Roman Krivonos for insightful feedback, Kevin Burdge, Dovi Poznanski, and Jim Fuller for useful discussions, and Sunny Wong for providing AM CVn evolutionary models. A.C.R. acknowledges support from an NSF Graduate Fellowship.\r\n\r\nA.C.R. thanks the LSST-DA Data Science Fellowship Program, which is funded by LSST-DA, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. RLO is a Research Fellow of the Brazilian institution CNPq (PQ-315632/2023-2).\r\n\r\nThis work is based on data from eROSITA, the soft X-ray instrument aboard SRG, a joint Russian-German science mission supported by the Russian Space Agency (Roskosmos), in the interests of the Russian Academy of Sciences represented by its Space Research Institute (IKI), and the Deutsches Zentrum für Luft- und Raumfahrt (DLR). The SRG spacecraft was built by Lavochkin Association (NPOL) and its subcontractors, and is operated by NPOL with support from the Max Planck Institute for Extraterrestrial Physics (MPE). The development and construction of the eROSITA X-ray instrument was led by MPE, with contributions from the Dr. Karl Remeis Observatory Bamberg & ECAP (FAU Erlangen-Nuernberg), the University of Hamburg Observatory, the Leibniz Institute for Astrophysics Potsdam (AIP), and the Institute for Astronomy and Astrophysics of the University of Tübingen, with the support of DLR and the Max Planck Society. The Argelander Institute for Astronomy of the University of Bonn and the Ludwig Maximilians Universität Munich also participated in the science preparation for eROSITA.\r\n\r\nThis work presents results from the European Space Agency (ESA) space mission Gaia. Gaia data are being processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC is provided by national institutions, in particular the institutions participating in the Gaia MultiLateral Agreement (MLA). The Gaia mission website is https://www.cosmos.esa.int/gaia. The Gaia archive website is https://archives.esac.esa.int/gaia.\r\n\r\nSome of the data presented herein were obtained at Keck Observatory, which is a private 501(c)3 non-profit 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. The authors 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 the opportunity to conduct observations from this mountain. We are also grateful to the staff of Palomar Observatory and that of Lick Observatory for their assistance in carrying out observations used in this work.\r\n\r\nBased 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.\r\n\r\nSoftware: used: Python and the following libraries: matplotlib (Hunter 2007), scipy (Virtanen et al. 2020), astropy (Astropy Collaboration et al. 2013), numpy (van der Walt et al. 2011). PypeIt (Prochaska et al. 2020), lpipe (Perley 2019), and Tool for OPerations on Catalogues And Tables (TOPCAT) (Taylor 2005).","OA_place":"publisher","quality_controlled":"1","arxiv":1,"OA_type":"hybrid","publication_identifier":{"issn":["0004-6280"]},"volume":137,"has_accepted_license":"1","citation":{"ieee":"A. C. Rodriguez et al., “Cataclysmic variables and AM CVn binaries in SRG/eROSITA + Gaia: Volume limited samples, X-ray luminosity functions, and space densities,” Publications of the Astronomical Society of the Pacific, vol. 137, no. 1. IOP Publishing, 2025.","apa":"Rodriguez, A. C., El-Badry, K., Suleimanov, V., Pala, A. F., Kulkarni, S. R., Gaensicke, B., … Riddle, R. (2025). Cataclysmic variables and AM CVn binaries in SRG/eROSITA + Gaia: Volume limited samples, X-ray luminosity functions, and space densities. Publications of the Astronomical Society of the Pacific. IOP Publishing. https://doi.org/10.1088/1538-3873/ada185","short":"A.C. Rodriguez, K. El-Badry, V. Suleimanov, A.F. Pala, S.R. Kulkarni, B. Gaensicke, K. Mori, R.M. Rich, A. Sarkar, T. Bao, R.L. De Oliveira, G. Ramsay, P. Szkody, M. Graham, T.A. Prince, I. Caiazzo, Z.P. Vanderbosch, J.V. Roestel, K.K. Das, Y.J. Qin, M.M. Kasliwal, A. Wold, S.L. Groom, D. Reiley, R. Riddle, Publications of the Astronomical Society of the Pacific 137 (2025).","chicago":"Rodriguez, Antonio C., Kareem El-Badry, Valery Suleimanov, Anna F. Pala, Shrinivas R. Kulkarni, Boris Gaensicke, Kaya Mori, et al. “Cataclysmic Variables and AM CVn Binaries in SRG/EROSITA + Gaia: Volume Limited Samples, X-Ray Luminosity Functions, and Space Densities.” Publications of the Astronomical Society of the Pacific. IOP Publishing, 2025. https://doi.org/10.1088/1538-3873/ada185.","ista":"Rodriguez AC, El-Badry K, Suleimanov V, Pala AF, Kulkarni SR, Gaensicke B, Mori K, Rich RM, Sarkar A, Bao T, De Oliveira RL, Ramsay G, Szkody P, Graham M, Prince TA, Caiazzo I, Vanderbosch ZP, Roestel JV, Das KK, Qin YJ, Kasliwal MM, Wold A, Groom SL, Reiley D, Riddle R. 2025. Cataclysmic variables and AM CVn binaries in SRG/eROSITA + Gaia: Volume limited samples, X-ray luminosity functions, and space densities. Publications of the Astronomical Society of the Pacific. 137(1), 014201.","mla":"Rodriguez, Antonio C., et al. “Cataclysmic Variables and AM CVn Binaries in SRG/EROSITA + Gaia: Volume Limited Samples, X-Ray Luminosity Functions, and Space Densities.” Publications of the Astronomical Society of the Pacific, vol. 137, no. 1, 014201, IOP Publishing, 2025, doi:10.1088/1538-3873/ada185.","ama":"Rodriguez AC, El-Badry K, Suleimanov V, et al. Cataclysmic variables and AM CVn binaries in SRG/eROSITA + Gaia: Volume limited samples, X-ray luminosity functions, and space densities. Publications of the Astronomical Society of the Pacific. 2025;137(1). doi:10.1088/1538-3873/ada185"},"publication":"Publications of the Astronomical Society of the Pacific","date_created":"2025-01-19T23:01:51Z","scopus_import":"1","department":[{"_id":"IlCa"}],"tmp":{"short":"CC BY (3.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/3.0/legalcode","name":"Creative Commons Attribution 3.0 Unported (CC BY 3.0)"},"language":[{"iso":"eng"}],"isi":1,"fulldoi":"https://doi.org/10.1088/1538-3873/ada185","file":[{"file_size":5155631,"checksum":"02a9be04a6704fc272ed5a976e5fa8c5","date_updated":"2025-01-20T09:52:34Z","date_created":"2025-01-20T09:52:34Z","relation":"main_file","creator":"dernst","success":1,"access_level":"open_access","file_id":"18860","file_name":"2025_PASP_Rodriguez.pdf","content_type":"application/pdf"}],"external_id":{"arxiv":["2408.16053"],"isi":["001393204700001"]},"date_published":"2025-01-01T00:00:00Z","day":"01","doi":"10.1088/1538-3873/ada185","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"IOP Publishing","status":"public","_id":"18851","type":"journal_article","date_updated":"2025-02-27T12:46:32Z","abstract":[{"lang":"eng","text":"We present volume-limited samples of cataclysmic variables (CVs) and AM CVn binaries jointly selected from SRG/eROSITA eRASS1 and Gaia DR3 using an X-ray + optical color–color diagram (the \"X-ray Main Sequence\"). This tool identifies all CV subtypes, including magnetic and low-accretion rate systems, in contrast to most previous surveys. We find 23 CVs, 3 of which are AM CVns, out to 150 pc in the Western Galactic Hemisphere. Our 150 pc sample is spectroscopically verified and complete down to LX = 1.3 × 1029 erg s−1 in the 0.2–2.3 keV band, and we also present CV candidates out to 300 pc and 1000 pc. We discovered two previously unknown systems in our 150 pc sample: the third nearest AM CVn and a magnetic period bouncer. We find the mean LX of CVs to be 〈LX〉 ≈ 4.6 × 1030 erg s−1, in contrast to previous surveys which yielded 〈LX〉 ∼ 1031−1032 erg s−1. We construct X-ray luminosity functions that, for the first time, flatten out at LX ∼ 1030 erg s−1. We infer average number, mass, and luminosity densities of ρN,CV = (3.7 ± 0.7) × 10−6pc−3, (math formular), and (math formular), respectively, in the solar neighborhood. Our uniform selection method also allows us to place meaningful estimates on the space density of AM CVns, ρN,AM CVn = (5.5 ± 3.7) × 10−7 pc−3. Magnetic CVs and period bouncers make up 35% and 25% of our sample, respectively. This work, through a novel discovery technique, shows that the observed number densities of CVs and AM CVns, as well as the fraction of period bouncers, are still in tension with population synthesis estimates."}],"file_date_updated":"2025-01-20T09:52:34Z","title":"Cataclysmic variables and AM CVn binaries in SRG/eROSITA + Gaia: Volume limited samples, X-ray luminosity functions, and space densities"},{"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"volume":693,"OA_type":"diamond","OA_place":"publisher","arxiv":1,"quality_controlled":"1","acknowledgement":"This project was originally started as part of the Kavli Summer Program which took place in the Max Planck Institute for Astrophysics in Garching in July 2023, supported by the Kavli Foundation. We are grateful to Stephen Justham, Selma de Mink, and Jim Fuller for enriching discussions. We would like to thank the anonymous referee for their helpful report. A.B. was supported by the Deutsche Forschungsgemeinschaft (DFG) through grant GE2506/18-1. K.J.S. was supported by NASA through the Astrophysics Theory Program (80NSSC20K0544) and by NASA/ESA Hubble Space Telescope programs #15871 and #15918. W.E.K. was supported by NSF Grants OAC-2311323, AST-2206523, and NASA/ESA HST-AR-Theory HSTAR-16613.002-A. K.E. was supported in part by HST-GO-17441.001-A. AB and ASR would like to thank Rob Farmer for his support with PyMESA.","article_number":"A114","department":[{"_id":"IlCa"}],"scopus_import":"1","date_created":"2025-01-19T23:01:51Z","publication":"Astronomy & Astrophysics","citation":{"chicago":"Bhat, Aakash, Evan B. Bauer, Rüdiger Pakmor, Ken J. Shen, Ilaria Caiazzo, Abinaya Swaruba Rajamuthukumar, Kareem El-Badry, and Wolfgang E. Kerzendorf. “Supernova Shocks Cannot Explain the Inflated State of Hypervelocity Runaways from White Dwarf Binaries.” Astronomy & Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202451371.","short":"A. Bhat, E.B. Bauer, R. Pakmor, K.J. Shen, I. Caiazzo, A.S. Rajamuthukumar, K. El-Badry, W.E. Kerzendorf, Astronomy & Astrophysics 693 (2025).","apa":"Bhat, A., Bauer, E. B., Pakmor, R., Shen, K. J., Caiazzo, I., Rajamuthukumar, A. S., … Kerzendorf, W. E. (2025). Supernova shocks cannot explain the inflated state of hypervelocity runaways from white dwarf binaries. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202451371","ieee":"A. Bhat et al., “Supernova shocks cannot explain the inflated state of hypervelocity runaways from white dwarf binaries,” Astronomy & Astrophysics, vol. 693, no. 1. EDP Sciences, 2025.","ama":"Bhat A, Bauer EB, Pakmor R, et al. Supernova shocks cannot explain the inflated state of hypervelocity runaways from white dwarf binaries. Astronomy & Astrophysics. 2025;693(1). doi:10.1051/0004-6361/202451371","mla":"Bhat, Aakash, et al. “Supernova Shocks Cannot Explain the Inflated State of Hypervelocity Runaways from White Dwarf Binaries.” Astronomy & Astrophysics, vol. 693, no. 1, A114, EDP Sciences, 2025, doi:10.1051/0004-6361/202451371.","ista":"Bhat A, Bauer EB, Pakmor R, Shen KJ, Caiazzo I, Rajamuthukumar AS, El-Badry K, Kerzendorf WE. 2025. Supernova shocks cannot explain the inflated state of hypervelocity runaways from white dwarf binaries. Astronomy & Astrophysics. 693(1), A114."},"has_accepted_license":"1","month":"01","oa_version":"Published Version","intvolume":" 693","issue":"1","article_processing_charge":"No","oa":1,"year":"2025","ddc":["520"],"article_type":"original","publication_status":"published","author":[{"last_name":"Bhat","first_name":"Aakash","full_name":"Bhat, Aakash"},{"last_name":"Bauer","first_name":"Evan B.","full_name":"Bauer, Evan B."},{"last_name":"Pakmor","first_name":"Rüdiger","full_name":"Pakmor, Rüdiger"},{"first_name":"Ken J.","full_name":"Shen, Ken J.","last_name":"Shen"},{"last_name":"Caiazzo","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388"},{"first_name":"Abinaya Swaruba","full_name":"Rajamuthukumar, Abinaya Swaruba","last_name":"Rajamuthukumar"},{"last_name":"El-Badry","full_name":"El-Badry, Kareem","first_name":"Kareem"},{"full_name":"Kerzendorf, Wolfgang E.","first_name":"Wolfgang E.","last_name":"Kerzendorf"}],"type":"journal_article","status":"public","_id":"18852","publisher":"EDP Sciences","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","doi":"10.1051/0004-6361/202451371","title":"Supernova shocks cannot explain the inflated state of hypervelocity runaways from white dwarf binaries","file_date_updated":"2025-01-20T09:57:00Z","abstract":[{"text":"Recent observations have found a growing number of hypervelocity stars with speeds of ≈1500 − 2500 km s−1 that could have only been produced through thermonuclear supernovae in white dwarf binaries. Most of the observed hypervelocity runaways in this class display a surprising inflated structure: their current radii are roughly an order of magnitude greater than they would have been as white dwarfs filling their Roche lobe. While many simulations exist studying the dynamical phase leading to supernova detonation in these systems, no detailed calculations of the long-term structure of the runaways have yet been performed. We used an existing AREPO hydrodynamical simulation of a supernova in a white dwarf binary as a starting point for the evolution of these stars with the one-dimensional stellar evolution code MESA. We show that the supernova shock is not energetic enough to inflate the white dwarf over timescales longer than a few thousand years, significantly shorter than the 105 − 6 year lifetimes inferred for observed hypervelocity runaways. Although they experience a shock from a supernova less than ≈0.02 R⊙ away, our models do not experience significant interior heating, and all contract back to radii of around 0.01 R⊙ within about 104 years. Explaining the observed inflated states requires either an additional source of significant heating or some other physics that is not yet accounted for in the subsequent evolution.","lang":"eng"}],"date_updated":"2026-02-16T12:08:05Z","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","image":"/images/cc_by.png","short":"CC BY (4.0)"},"day":"07","date_published":"2025-01-07T00:00:00Z","external_id":{"isi":["001406577300001"],"arxiv":["2407.03424"]},"isi":1,"fulldoi":"https://doi.org/10.1051/0004-6361/202451371","file":[{"file_id":"18861","access_level":"open_access","content_type":"application/pdf","file_name":"2025_AstronomyAstrophysics_Bhat.pdf","checksum":"e532b9c8123c29cfb0ee758e6d00453c","date_updated":"2025-01-20T09:57:00Z","file_size":1692527,"success":1,"creator":"dernst","relation":"main_file","date_created":"2025-01-20T09:57:00Z"}],"language":[{"iso":"eng"}]},{"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","image":"/images/cc_by.png","short":"CC BY (4.0)"},"date_published":"2025-02-01T00:00:00Z","day":"01","fulldoi":"https://doi.org/10.1088/1538-3873/adb0f1","file":[{"file_id":"19455","access_level":"open_access","file_name":"2025_PubAstronomSocPacific_Rodriguez.pdf","content_type":"application/pdf","checksum":"42d5aa504479c3fdf2a10165a9e3319f","date_updated":"2025-03-25T10:01:24Z","file_size":3291933,"success":1,"creator":"dernst","relation":"main_file","date_created":"2025-03-25T10:01:24Z"}],"isi":1,"language":[{"iso":"eng"}],"external_id":{"isi":["001427877700001"],"arxiv":["2501.01490"]},"type":"journal_article","status":"public","_id":"19439","doi":"10.1088/1538-3873/adb0f1","publisher":"IOP Publishing","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","file_date_updated":"2025-03-25T10:01:24Z","abstract":[{"lang":"eng","text":"White dwarfs (WDs) are the most abundant compact objects, and recent surveys have suggested that over a third of WDs in accreting binaries host a strong (B ≳ 1 MG) magnetic field. However, the origin and evolution of WD magnetism remain under debate. Two WD pulsars, AR Sco and J191213.72–441045.1 (J1912), have been found, which are non-accreting binaries hosting rapidly spinning (1.97 minutes and 5.30 minutes, respectively) magnetic WDs. The WD in AR Sco is slowing down on a (math formular) yr timescale. It is believed they will eventually become polars, accreting systems in which a magnetic WD (B ≈ 10−240 MG) accretes from a Roche lobe-filling donor spinning in sync with the orbit (≳78 minutes). Here, we present multiwavelength data and analysis of Gaia22ayj, which outbursted in 2022 March. We find that Gaia22ayj is a magnetic accreting WD that is rapidly spinning down (math formular\r\n yr) like WD pulsars, but shows clear evidence of accretion, like polars. Strong linear polarization (40%) is detected in Gaia22ayj; such high levels have only been seen in the WD pulsar AR Sco and demonstrate the WD is magnetic. High speed photometry reveals a 9.36 minutes period accompanying a high amplitude (∼2 mag) modulation. We associate this with a WD spin or spin–orbit beat period, not an orbital period as was previously suggested. Fast (60 s) optical spectroscopy reveals a broad \"hump,\" reminiscent of cyclotron emission in polars, between 4000 and 8000 Å. We find an X-ray luminosity of (math formular) in the 0.3–8 keV energy range, while two very large array radio campaigns resulted in a non-detection with a Fr < 15.8 μJy 3σ upper limit. The shared properties of both WD pulsars and polars suggest that Gaia22ayj is a missing link between the two classes of magnetic WD binaries."}],"title":"A link between White Dwarf pulsars and polars: Multiwavelength observations of the 9.36-minute period variable Gaia22ayj","date_updated":"2025-09-30T11:15:10Z","intvolume":" 137","issue":"2","oa_version":"Published Version","month":"02","article_processing_charge":"Yes (in subscription journal)","year":"2025","oa":1,"ddc":["520"],"publication_status":"published","article_type":"original","author":[{"full_name":"Rodriguez, Antonio C.","first_name":"Antonio C.","last_name":"Rodriguez"},{"first_name":"Kareem","full_name":"El-Badry, Kareem","last_name":"El-Badry"},{"last_name":"Hakala","full_name":"Hakala, Pasi","first_name":"Pasi"},{"last_name":"Rodríguez-Gil","first_name":"Pablo","full_name":"Rodríguez-Gil, Pablo"},{"first_name":"Tong","full_name":"Bao, Tong","last_name":"Bao"},{"last_name":"Galiullin","first_name":"Ilkham","full_name":"Galiullin, Ilkham"},{"first_name":"Jacob A.","full_name":"Kurlander, Jacob A.","last_name":"Kurlander"},{"first_name":"Casey J.","full_name":"Law, Casey J.","last_name":"Law"},{"last_name":"Pelisoli","full_name":"Pelisoli, Ingrid","first_name":"Ingrid"},{"last_name":"Schreiber","first_name":"Matthias R.","full_name":"Schreiber, Matthias R."},{"full_name":"Burdge, Kevin","first_name":"Kevin","last_name":"Burdge"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","last_name":"Caiazzo"},{"full_name":"Roestel, Jan Van","first_name":"Jan Van","last_name":"Roestel"},{"full_name":"Szkody, Paula","first_name":"Paula","last_name":"Szkody"},{"last_name":"Drake","full_name":"Drake, Andrew J.","first_name":"Andrew J."},{"full_name":"Buckley, David A.H.","first_name":"David A.H.","last_name":"Buckley"},{"full_name":"Potter, Stephen B.","first_name":"Stephen B.","last_name":"Potter"},{"full_name":"Gaensicke, Boris","first_name":"Boris","last_name":"Gaensicke"},{"first_name":"Kaya","full_name":"Mori, Kaya","last_name":"Mori"},{"last_name":"Bellm","first_name":"Eric C.","full_name":"Bellm, Eric C."},{"first_name":"Shrinivas R.","full_name":"Kulkarni, Shrinivas R.","last_name":"Kulkarni"},{"last_name":"Prince","first_name":"Thomas A.","full_name":"Prince, Thomas A."},{"last_name":"Graham","first_name":"Matthew","full_name":"Graham, Matthew"},{"full_name":"Kasliwal, Mansi M.","first_name":"Mansi M.","last_name":"Kasliwal"},{"last_name":"Rose","full_name":"Rose, Sam","first_name":"Sam"},{"last_name":"Sharma","first_name":"Yashvi","full_name":"Sharma, Yashvi"},{"first_name":"Tomás","full_name":"Ahumada, Tomás","last_name":"Ahumada"},{"full_name":"Anand, Shreya","first_name":"Shreya","last_name":"Anand"},{"full_name":"Viitanen, Akke","first_name":"Akke","last_name":"Viitanen"},{"full_name":"Wold, Avery","first_name":"Avery","last_name":"Wold"},{"full_name":"Chen, Tracy X.","first_name":"Tracy X.","last_name":"Chen"},{"full_name":"Riddle, Reed","first_name":"Reed","last_name":"Riddle"},{"last_name":"Smith","full_name":"Smith, Roger","first_name":"Roger"}],"OA_type":"hybrid","quality_controlled":"1","OA_place":"publisher","arxiv":1,"volume":137,"publication_identifier":{"issn":["0004-6280"]},"acknowledgement":"We wish to dedicate this work to the memory of our colleague and friend Tom Marsh. Tom's enthusiasm to work on this object and rapid efforts to facilitate data collection truly made this project possible.\r\n\r\nA.C.R. acknowledges support from an NSF Graduate Fellowship. A.C.R. thanks the LSST-DA Data Science Fellowship Program, which is funded by LSST-DA, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. P.R.-G. acknowledges support by the Spanish Agencia Estatal de Investigación del Ministerio de Ciencia e Innovación (MCIN/AEI) and the European Regional Development Fund (ERDF) under grant PID2021–124879NB–I00. M.R.S. is supported by FONDECYT (grant No. 1221059) and eRO-STEP (SA 2131/15-2 project number 414059771). I.P. acknowledges support from a Royal Society University Research Fellowship (URF/R1/231496). We thank the referee for feedback that improved the clarity of this paper.\r\n\r\nBased on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofìsica de Canarias, on the island of La Palma. Based on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the ZTF 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.\r\n\r\nSome of the data presented herein were obtained at Keck Observatory, which is a private 501(c)3 non-profit 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. The authors 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 the opportunity to conduct observations from this mountain. We are also grateful to the staff of Palomar Observatory for their assistance in carrying out observations used in this work.\r\n\r\nPartly based on observations made with the NOT, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The data presented here were obtained with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOT. The observation with the SALT was obtained under program 2021-2-LSP-001 (PI: D. Buckley). Polish participation in SALT is funded by grant No. MEiN nr 2021/WK/01. D.A.H.B. acknowledges support from the National Research Foundation.\r\n\r\nThis work presents results from the European Space Agency (ESA) space mission Gaia. Gaia data are being processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC is provided by national institutions, in particular the institutions participating in the Gaia MultiLateral Agreement (MLA). The Gaia mission website is https://www.cosmos.esa.int/gaia. The Gaia archive website is https://archives.esac.esa.int/gaia. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester\r\n\r\nE.C.B. and J.K. acknowledge support from the DIRAC Institute in the Department of Astronomy at the University of Washington. The DIRAC Institute is supported through generous gifts from the Charles and Lisa Simonyi Fund for Arts and Sciences, and the Washington Research Foundation.","article_number":"024202","publication":"Publications of the Astronomical Society of the Pacific","department":[{"_id":"IlCa"}],"scopus_import":"1","date_created":"2025-03-23T23:01:26Z","has_accepted_license":"1","citation":{"apa":"Rodriguez, A. C., El-Badry, K., Hakala, P., Rodríguez-Gil, P., Bao, T., Galiullin, I., … Smith, R. (2025). A link between White Dwarf pulsars and polars: Multiwavelength observations of the 9.36-minute period variable Gaia22ayj. Publications of the Astronomical Society of the Pacific. IOP Publishing. https://doi.org/10.1088/1538-3873/adb0f1","ieee":"A. C. Rodriguez et al., “A link between White Dwarf pulsars and polars: Multiwavelength observations of the 9.36-minute period variable Gaia22ayj,” Publications of the Astronomical Society of the Pacific, vol. 137, no. 2. IOP Publishing, 2025.","short":"A.C. Rodriguez, K. El-Badry, P. Hakala, P. Rodríguez-Gil, T. Bao, I. Galiullin, J.A. Kurlander, C.J. Law, I. Pelisoli, M.R. Schreiber, K. Burdge, I. Caiazzo, J.V. Roestel, P. Szkody, A.J. Drake, D.A.H. Buckley, S.B. Potter, B. Gaensicke, K. Mori, E.C. Bellm, S.R. Kulkarni, T.A. Prince, M. Graham, M.M. Kasliwal, S. Rose, Y. Sharma, T. Ahumada, S. Anand, A. Viitanen, A. Wold, T.X. Chen, R. Riddle, R. Smith, Publications of the Astronomical Society of the Pacific 137 (2025).","chicago":"Rodriguez, Antonio C., Kareem El-Badry, Pasi Hakala, Pablo Rodríguez-Gil, Tong Bao, Ilkham Galiullin, Jacob A. Kurlander, et al. “A Link between White Dwarf Pulsars and Polars: Multiwavelength Observations of the 9.36-Minute Period Variable Gaia22ayj.” Publications of the Astronomical Society of the Pacific. IOP Publishing, 2025. https://doi.org/10.1088/1538-3873/adb0f1.","ista":"Rodriguez AC, El-Badry K, Hakala P, Rodríguez-Gil P, Bao T, Galiullin I, Kurlander JA, Law CJ, Pelisoli I, Schreiber MR, Burdge K, Caiazzo I, Roestel JV, Szkody P, Drake AJ, Buckley DAH, Potter SB, Gaensicke B, Mori K, Bellm EC, Kulkarni SR, Prince TA, Graham M, Kasliwal MM, Rose S, Sharma Y, Ahumada T, Anand S, Viitanen A, Wold A, Chen TX, Riddle R, Smith R. 2025. A link between White Dwarf pulsars and polars: Multiwavelength observations of the 9.36-minute period variable Gaia22ayj. Publications of the Astronomical Society of the Pacific. 137(2), 024202.","ama":"Rodriguez AC, El-Badry K, Hakala P, et al. A link between White Dwarf pulsars and polars: Multiwavelength observations of the 9.36-minute period variable Gaia22ayj. Publications of the Astronomical Society of the Pacific. 2025;137(2). doi:10.1088/1538-3873/adb0f1","mla":"Rodriguez, Antonio C., et al. “A Link between White Dwarf Pulsars and Polars: Multiwavelength Observations of the 9.36-Minute Period Variable Gaia22ayj.” Publications of the Astronomical Society of the Pacific, vol. 137, no. 2, 024202, IOP Publishing, 2025, doi:10.1088/1538-3873/adb0f1."}},{"day":"01","date_published":"2025-06-01T00:00:00Z","language":[{"iso":"eng"}],"fulldoi":"https://doi.org/10.1093/mnras/staf561","file":[{"file_id":"19864","access_level":"open_access","content_type":"application/pdf","file_name":"2025_MonthlyNoticesRAS_Cunningham.pdf","date_updated":"2025-06-23T07:28:36Z","checksum":"5e675d3696c222e919d6916bad194b01","file_size":3212636,"creator":"dernst","success":1,"relation":"main_file","date_created":"2025-06-23T07:28:36Z"}],"isi":1,"external_id":{"arxiv":["2503.12675"],"isi":["001493143700001"]},"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","image":"/images/cc_by.png","short":"CC BY (4.0)"},"abstract":[{"text":"We report the discovery of two new magnetic cataclysmic variables with brown dwarf companions and long orbital periods (P_{\\rm orb}=95\\pm1 and 104\\pm2 min). This discovery increases the sample of candidate magnetic period bouncers with confirmed sub-stellar donors from four to six. We also find their X-ray luminosity from archival XMM–Newton observations to be in the range L_{\\rm X}\\approx10^{28}-10^{29} \\mathrm{erg\\,s^{-1}} in the 0.25–10 keV band. This low luminosity is comparable with the other candidates, and at least an order of magnitude lower than the X-ray luminosities typically measured in cataclysmic variables. The X-ray fluxes imply mass transfer rates that are much lower than predicted by evolutionary models, even if some of the discrepancy is due to the accretion energy being emitted in other bands, such as via cyclotron emission at infrared wavelengths. Although it is possible that some or all of these systems formed directly as binaries containing a brown dwarf, it is likely that the donor used to be a low-mass star and that the systems followed the evolutionary track for cataclysmic variables, evolving past the period bounce. The donor in long period systems is expected to be a low-mass, cold brown dwarf. This hypothesis is supported by near-infrared photometric observations that constrain the donors in the two systems to be brown dwarfs cooler than \r\n1100 K (spectral types T5 or later), most likely losing mass via Roche Lobe overflow or winds. The serendipitous discovery of two magnetic period bouncers in the small footprint of the XMM–Newton catalogue implies a large space density of these type of systems, possibly compatible with the prediction of 40–70 per cent of magnetic cataclysmic variables to be period bouncers.","lang":"eng"}],"file_date_updated":"2025-06-23T07:28:36Z","title":"Discovery of two new polars evolved past the period bounce","date_updated":"2025-09-30T12:50:33Z","page":"633-649","status":"public","_id":"19840","type":"journal_article","doi":"10.1093/mnras/staf561","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publisher":"Oxford University Press","ddc":["520"],"author":[{"first_name":"Tim","full_name":"Cunningham, Tim","last_name":"Cunningham"},{"last_name":"Caiazzo","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388"},{"full_name":"Sienkiewicz, Gracjan","first_name":"Gracjan","last_name":"Sienkiewicz"},{"last_name":"Wheatley","full_name":"Wheatley, Peter J.","first_name":"Peter J."},{"last_name":"Gänsicke","first_name":"Boris T.","full_name":"Gänsicke, Boris T."},{"last_name":"El-Badry","first_name":"Kareem","full_name":"El-Badry, Kareem"},{"last_name":"Arcodia","first_name":"Riccardo","full_name":"Arcodia, Riccardo"},{"last_name":"Charbonneau","first_name":"David","full_name":"Charbonneau, David"},{"first_name":"Liam","full_name":"Connor, Liam","last_name":"Connor"},{"last_name":"De","first_name":"Kishalay","full_name":"De, Kishalay"},{"last_name":"Hakala","first_name":"Pasi","full_name":"Hakala, Pasi"},{"last_name":"Kenyon","first_name":"Scott J.","full_name":"Kenyon, Scott J."},{"full_name":"Maheshwari, Sumit Kumar","first_name":"Sumit Kumar","last_name":"Maheshwari"},{"last_name":"Rodriguez","first_name":"Antonio C.","full_name":"Rodriguez, Antonio C."},{"last_name":"Van Roestel","first_name":"Jan","full_name":"Van Roestel, Jan"},{"full_name":"Tremblay, Pier Emmanuel","first_name":"Pier Emmanuel","last_name":"Tremblay"}],"article_type":"original","publication_status":"published","oa_version":"Published Version","intvolume":" 540","issue":"1","month":"06","year":"2025","oa":1,"article_processing_charge":"Yes","publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2025-06-15T22:01:29Z","scopus_import":"1","department":[{"_id":"IlCa"}],"has_accepted_license":"1","citation":{"ista":"Cunningham T, Caiazzo I, Sienkiewicz G, Wheatley PJ, Gänsicke BT, El-Badry K, Arcodia R, Charbonneau D, Connor L, De K, Hakala P, Kenyon SJ, Maheshwari SK, Rodriguez AC, Van Roestel J, Tremblay PE. 2025. Discovery of two new polars evolved past the period bounce. Monthly Notices of the Royal Astronomical Society. 540(1), 633–649.","ama":"Cunningham T, Caiazzo I, Sienkiewicz G, et al. Discovery of two new polars evolved past the period bounce. Monthly Notices of the Royal Astronomical Society. 2025;540(1):633-649. doi:10.1093/mnras/staf561","mla":"Cunningham, Tim, et al. “Discovery of Two New Polars Evolved Past the Period Bounce.” Monthly Notices of the Royal Astronomical Society, vol. 540, no. 1, Oxford University Press, 2025, pp. 633–49, doi:10.1093/mnras/staf561.","ieee":"T. Cunningham et al., “Discovery of two new polars evolved past the period bounce,” Monthly Notices of the Royal Astronomical Society, vol. 540, no. 1. Oxford University Press, pp. 633–649, 2025.","apa":"Cunningham, T., Caiazzo, I., Sienkiewicz, G., Wheatley, P. J., Gänsicke, B. T., El-Badry, K., … Tremblay, P. E. (2025). Discovery of two new polars evolved past the period bounce. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf561","short":"T. Cunningham, I. Caiazzo, G. Sienkiewicz, P.J. Wheatley, B.T. Gänsicke, K. El-Badry, R. Arcodia, D. Charbonneau, L. Connor, K. De, P. Hakala, S.J. Kenyon, S.K. Maheshwari, A.C. Rodriguez, J. Van Roestel, P.E. Tremblay, Monthly Notices of the Royal Astronomical Society 540 (2025) 633–649.","chicago":"Cunningham, Tim, Ilaria Caiazzo, Gracjan Sienkiewicz, Peter J. Wheatley, Boris T. Gänsicke, Kareem El-Badry, Riccardo Arcodia, et al. “Discovery of Two New Polars Evolved Past the Period Bounce.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf561."},"quality_controlled":"1","arxiv":1,"OA_place":"publisher","OA_type":"gold","volume":540,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"acknowledgement":"We thank Matthias Schreiber for his insightful comments. Support for this work was provided 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. Support for this work was provided by NASA through Chandra Award Number GO4-25014X issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. IC was also supported by NASA through grants from the Space Telescope Science Institute, under NASA contracts NASA.22K1813, NAS5-26555, and NAS5-03127. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 101020057). This research was supported in part by grant NSF PHY-1748958 to the Kavli Institute for Theoretical Physics (KITP). PJW acknowledges support from the UK Science and Technology Facilities Council (STFC) through consolidated grants ST/T000406/1 and ST/X001121/1. RA was supported by NASA through the NASA Hubble Fellowship grant #HST-HF2-51499.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.\r\n\r\nThis research has made use of data obtained from the 4XMM XMM–Newton Serendipitous Source Catalogue compiled by the 10 institutes of the XMM–Newton Survey Science Centre selected by ESA. 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. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard–Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant no. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant no. AST–1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. This work is based in part on data obtained as part of the UKIDSS. This research made use of hips2fits,4 a service provided by CDS, and of astropy (Astropy Collaboration 2013)."},{"oa":1,"year":"2025","article_processing_charge":"Yes","issue":"1","oa_version":"Published Version","intvolume":" 170","month":"07","author":[{"last_name":"Cheng","first_name":"Sihao","full_name":"Cheng, Sihao"},{"last_name":"Schlaufman","first_name":"Kevin C.","full_name":"Schlaufman, Kevin C."},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","first_name":"Ilaria","last_name":"Caiazzo"}],"publication_status":"published","article_type":"original","ddc":["520"],"article_number":"47","acknowledgement":"We thank Jay Farihi, Guangwei Fu, J. J. Hermes, Mary Anne Limbach, and Daniel Thorngren for useful discussions. S.C. thanks Siyu Yao for her constant inspiration and encouragement. S.C. acknowledges the support of the Martin A. and Helen Chooljian Member Fund, funding from the Zurich Insurance Company, and the Fund for Natural Sciences at the Institute for Advanced Study. 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. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This 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. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research has made use of NASA’s Astrophysics Data System.\r\nFacilities: ADS - , ESO:VISTA - European Southern Observatory's 4.1 meter Visible and Infrared Survey Telescope for Astronomy, Exoplanet Archive - , Gaia - , IRSA - , NEOWISE - , Spitzer - Spitzer Space Telescope satellite, UKIRT - United Kingdom Infrared Telescope, WISE - Wide-field Infrared Survey Explorer.\r\nSoftware: astropy (Astropy Collaboration et al. 2013, 2018, 2022), numpy (C. R. Harris et al. 2020), matplotlib (J. D. Hunter 2007), R (R Core Team 2024), SciPy (P. Virtanen et al. 2020).","arxiv":1,"quality_controlled":"1","OA_place":"publisher","OA_type":"gold","publication_identifier":{"eissn":["1538-3881"],"issn":["0004-6256"]},"volume":170,"has_accepted_license":"1","citation":{"chicago":"Cheng, Sihao, Kevin C. Schlaufman, and Ilaria Caiazzo. “A Candidate Giant Planet Companion to the Massive, Young White Dwarf GALEX J071816.4+373139 Informs the Occurrence of Giant Planets Orbiting B Stars.” The Astronomical Journal. IOP Publishing, 2025. https://doi.org/10.3847/1538-3881/addd21.","short":"S. Cheng, K.C. Schlaufman, I. Caiazzo, The Astronomical Journal 170 (2025).","apa":"Cheng, S., Schlaufman, K. C., & Caiazzo, I. (2025). A candidate giant planet companion to the massive, young White Dwarf GALEX J071816.4+373139 informs the occurrence of giant planets orbiting B stars. The Astronomical Journal. IOP Publishing. https://doi.org/10.3847/1538-3881/addd21","ieee":"S. Cheng, K. C. Schlaufman, and I. Caiazzo, “A candidate giant planet companion to the massive, young White Dwarf GALEX J071816.4+373139 informs the occurrence of giant planets orbiting B stars,” The Astronomical Journal, vol. 170, no. 1. IOP Publishing, 2025.","ama":"Cheng S, Schlaufman KC, Caiazzo I. A candidate giant planet companion to the massive, young White Dwarf GALEX J071816.4+373139 informs the occurrence of giant planets orbiting B stars. The Astronomical Journal. 2025;170(1). doi:10.3847/1538-3881/addd21","mla":"Cheng, Sihao, et al. “A Candidate Giant Planet Companion to the Massive, Young White Dwarf GALEX J071816.4+373139 Informs the Occurrence of Giant Planets Orbiting B Stars.” The Astronomical Journal, vol. 170, no. 1, 47, IOP Publishing, 2025, doi:10.3847/1538-3881/addd21.","ista":"Cheng S, Schlaufman KC, Caiazzo I. 2025. A candidate giant planet companion to the massive, young White Dwarf GALEX J071816.4+373139 informs the occurrence of giant planets orbiting B stars. The Astronomical Journal. 170(1), 47."},"publication":"The Astronomical Journal","date_created":"2025-07-06T22:01:22Z","department":[{"_id":"IlCa"}],"scopus_import":"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","image":"/images/cc_by.png","short":"CC BY (4.0)"},"language":[{"iso":"eng"}],"isi":1,"fulldoi":"https://doi.org/10.3847/1538-3881/addd21","file":[{"file_name":"2025_AstronomicalJour_Cheng.pdf","content_type":"application/pdf","file_id":"19975","access_level":"open_access","success":1,"creator":"dernst","relation":"main_file","date_created":"2025-07-08T06:40:54Z","checksum":"144b0e46aa3dff0cdf8c6ee7d4fe2fe4","date_updated":"2025-07-08T06:40:54Z","file_size":931173}],"external_id":{"isi":["001514518100001"],"arxiv":["2408.03985"]},"date_published":"2025-07-01T00:00:00Z","day":"01","doi":"10.3847/1538-3881/addd21","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","DOAJ_listed":"1","publisher":"IOP Publishing","status":"public","_id":"19964","type":"journal_article","date_updated":"2026-02-19T09:31:41Z","abstract":[{"lang":"eng","text":"It has been suggested that giant planet occurrence peaks for stars with M* ≈ 3 M⊙ at a value a factor of 4 higher than observed for solar-mass stars. This population of giant planets predicted to frequently orbit main-sequence B stars at a ≈ 10 au is difficult to characterize during the few hundred million years while fusion persists in their host stars. By the time those stars become massive, young white dwarfs, any giant planets present would still be luminous as a consequence of their recent formation. From an initial sample of 2195 Gaia-identified massive, young white dwarfs, we use homogeneous Spitzer Infrared Array Camera (IRAC) photometry to search for evidence of unresolved giant planets. For 30 systems, these IRAC data provide sensitivity to objects with M ≲ 10 MJup, and we identify one candidate with M ≈ 4 MJup orbiting the white dwarf GALEX J071816.4+373139. Correcting for the possibility that some of the white dwarfs in our sample result from mergers, we find a giant planet occurrence n GP = 0.11+0.13-0.07 for stars with initial masses M* ≳ 3 M⊙. Our occurrence inference is consistent with both the Doppler-inferred occurrence of giant planets orbiting M* ≈ 2 M⊙ giant stars and the theoretically predicted factor of 4 enhancement in the occurrence of giant planets orbiting M* ≈ 3 M⊙ stars relative to solar-mass stars. Future James Webb Space Telescope NIRCam observations of our sample would provide sensitivity to Saturn-mass planets and thereby a definitive estimate of the occurrence of giant planets orbiting stars with M* ≳ 3 M⊙."}],"file_date_updated":"2025-07-08T06:40:54Z","title":"A candidate giant planet companion to the massive, young White Dwarf GALEX J071816.4+373139 informs the occurrence of giant planets orbiting B stars"},{"publication":"The Astrophysical Journal","scopus_import":"1","department":[{"_id":"IlCa"}],"date_created":"2025-11-02T23:01:33Z","has_accepted_license":"1","citation":{"chicago":"Guidry, Joseph A., Zachary P. Vanderbosch, J. J. Hermes, Dimitri Veras, Mark A. Hollands, Soumyadeep Bhattacharjee, Ilaria Caiazzo, et al. “Transiting Planetary Debris near the Roche Limit of a White Dwarf on a 4.97 Hr Orbit—and Its Vanishing.” The Astrophysical Journal. IOP Publishing, 2025. https://doi.org/10.3847/1538-4357/adfecb.","short":"J.A. Guidry, Z.P. Vanderbosch, J.J. Hermes, D. Veras, M.A. Hollands, S. Bhattacharjee, I. Caiazzo, K. El-Badry, M.L. Kao, L.B. Ould Rouis, A.C. Rodriguez, J. Van Roestel, The Astrophysical Journal 992 (2025).","ieee":"J. A. Guidry et al., “Transiting planetary debris near the Roche limit of a white dwarf on a 4.97 hr orbit—and its vanishing,” The Astrophysical Journal, vol. 992, no. 2. IOP Publishing, 2025.","apa":"Guidry, J. A., Vanderbosch, Z. P., Hermes, J. J., Veras, D., Hollands, M. A., Bhattacharjee, S., … Van Roestel, J. (2025). Transiting planetary debris near the Roche limit of a white dwarf on a 4.97 hr orbit—and its vanishing. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/adfecb","ama":"Guidry JA, Vanderbosch ZP, Hermes JJ, et al. Transiting planetary debris near the Roche limit of a white dwarf on a 4.97 hr orbit—and its vanishing. The Astrophysical Journal. 2025;992(2). doi:10.3847/1538-4357/adfecb","mla":"Guidry, Joseph A., et al. “Transiting Planetary Debris near the Roche Limit of a White Dwarf on a 4.97 Hr Orbit—and Its Vanishing.” The Astrophysical Journal, vol. 992, no. 2, 167, IOP Publishing, 2025, doi:10.3847/1538-4357/adfecb.","ista":"Guidry JA, Vanderbosch ZP, Hermes JJ, Veras D, Hollands MA, Bhattacharjee S, Caiazzo I, El-Badry K, Kao ML, Ould Rouis LB, Rodriguez AC, Van Roestel J. 2025. Transiting planetary debris near the Roche limit of a white dwarf on a 4.97 hr orbit—and its vanishing. The Astrophysical Journal. 992(2), 167."},"PlanS_conform":"1","OA_type":"gold","arxiv":1,"OA_place":"publisher","quality_controlled":"1","volume":992,"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"acknowledgement":"We first extend our gratitude to our anonymous referee, whose careful review and recommendations enhanced this manuscript. In fruitful conversations and correspondence with Tim Cunningham, Jay Farihi, Jim Fuller, Philip Muirhead, Saul Rappaport, Siyi Xu (许偲艺), and Nadia Zakamska, we found guidance that improved our interpretation of these results. We are deeply grateful for the observing support by John Kuehne at McDonald Observatory and Colt Pauley at the Perkins Telescope Observatory. This material is based upon work supported by the National Aeronautics and Space Administration under grant No. 80NSSC23K1068 issued through the Science Mission Directorate. J.A.G. is supported by the National Science Foundation Graduate Research Fellowship Program under grant No. 2234657.\r\n\r\nThis worked is 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 Oskar Klein Center at Stockholm University, the University of Maryland, University of California, Berkeley, the University of Wisconsin at Milwaukee, University of Warwick, Ruhr University, Cornell University, Northwestern University and Drexel University. Operations are conducted by COO, IPAC, and UW.\r\n\r\nSome of the data presented herein were obtained at Keck Observatory, which is a private 501(c)3 non-profit 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. The authors 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 the opportunity to conduct observations from this mountain.\r\n\r\nThis 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.\r\n\r\nThis publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration.\r\n\r\nThis work is based in part on observations made with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA.\r\n\r\nThe Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation.\r\n\r\nThis research relied upon the SIMBAD and VizieR databases operated by CDS (Strasbourg, France) and the bibliographic resources of The SAO Astrophysics Data System.\r\n\r\nFacilities: PO:1.2m - Palomar Observatory's 1.2 meter Samuel Oschin Telescope (Zwicky Transient Facility) - , Hale (CHIMERA, DBSP), Struve - McDonald Observatory's 2.1m Otto Struve Telescope(ProEM), Perkins - Lowell Observatory's 72in Perkins Telescope (PRISM), LDT - (LMI), Keck:I - KECK I Telescope (LRIS), Gaia - , PS1 - Panoramic Survey Telescope and Rapid Response System Telescope #1 (Pan-STARRS), Spitzer (IRAC) - , WISE - Wide-field Infrared Survey Explorer.\r\n\r\nSoftware: Astropy (Astropy Collaboration et al. 2013, 2018, 2022), astroquery (A. Ginsburg et al. 2019), ccdproc (M. Craig et al. 2017), cuvarbase (J. Hoffman 2022), extinction (K. Barbary 2016), hipercam (V. S. Dhillon et al. 2021), lmfit (M. Newville et al. 2014), matplotlib (J. D. Hunter 2007), numpy (C. R. Harris et al. 2020), pandas (The pandas Development Team 2025), phot2lc (Z. Vanderbosch 2023), photutils (L. Bradley et al. 2024), Pyriod (K. Bell 2022), scipy (P. Virtanen et al. 2020).","article_number":"167","ddc":["520"],"article_type":"original","publication_status":"published","author":[{"last_name":"Guidry","first_name":"Joseph A.","full_name":"Guidry, Joseph A."},{"last_name":"Vanderbosch","full_name":"Vanderbosch, Zachary P.","first_name":"Zachary P."},{"full_name":"Hermes, J. J.","first_name":"J. J.","last_name":"Hermes"},{"first_name":"Dimitri","full_name":"Veras, Dimitri","last_name":"Veras"},{"last_name":"Hollands","full_name":"Hollands, Mark A.","first_name":"Mark A."},{"full_name":"Bhattacharjee, Soumyadeep","first_name":"Soumyadeep","last_name":"Bhattacharjee"},{"last_name":"Caiazzo","first_name":"Ilaria","orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d"},{"last_name":"El-Badry","first_name":"Kareem","full_name":"El-Badry, Kareem"},{"full_name":"Kao, Malia L.","first_name":"Malia L.","last_name":"Kao"},{"last_name":"Ould Rouis","first_name":"Lou Baya","full_name":"Ould Rouis, Lou Baya"},{"first_name":"Antonio C.","full_name":"Rodriguez, Antonio C.","last_name":"Rodriguez"},{"full_name":"Van Roestel, Jan","first_name":"Jan","last_name":"Van Roestel"}],"intvolume":" 992","oa_version":"Published Version","issue":"2","month":"10","article_processing_charge":"Yes","year":"2025","oa":1,"file_date_updated":"2025-11-04T12:33:51Z","abstract":[{"lang":"eng","text":"We present the discovery of deep, irregular, periodic transits toward the white dwarf ZTF J1944+4557 using follow-up time-series photometry and spectroscopy from Palomar, Keck, McDonald, Perkins, and Lowell observatories. We find a predominant period of 4.9704 hr, consistent with an orbit near the Roche limit of the white dwarf, with individual dips over 30% deep and lasting between 15 and 40 minutes. Similar to the first known white dwarf with transiting debris, WD 1145+017, the transit events are well-defined with prominent out-of-transit phases where the white dwarf appears unobscured. Spectroscopy concurrent with transit photometry reveals that the average Ca K equivalent width remains constant in and out of transit. The broadening observed in several absorption features cannot be reproduced by synthetic photospheric models, suggesting the presence of circumstellar gas. Simultaneous g + r- and g + i-band light curves from the CHIMERA instrument reveal no color dependence to the transit depths, requiring transiting dust grains to have sizes s ≳ 0.2 μm. The transit morphologies appear to be constantly changing at a rate faster than the orbital period. Overall transit activity varies in the system, with transit features completely disappearing during the seven months between our 2023 and 2024 observing seasons and then reappearing in 2025 March, still repeating at 4.9704 hr. Our observations of the complete cessation and resumption of transit activity provide a novel laboratory for constraining the evolution of disrupted debris and processes like disk exhaustion and replenishment timescales at white dwarfs."}],"title":"Transiting planetary debris near the Roche limit of a white dwarf on a 4.97 hr orbit—and its vanishing","date_updated":"2026-02-16T12:43:29Z","type":"journal_article","status":"public","_id":"20586","doi":"10.3847/1538-4357/adfecb","publisher":"IOP Publishing","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","DOAJ_listed":"1","day":"20","date_published":"2025-10-20T00:00:00Z","fulldoi":"https://doi.org/10.3847/1538-4357/adfecb","file":[{"creator":"dernst","success":1,"relation":"main_file","date_created":"2025-11-04T12:33:51Z","date_updated":"2025-11-04T12:33:51Z","checksum":"24892d1b5bfa1867eb0a353f10c31b82","file_size":5323398,"file_name":"2025_AstrophysicalJour_Guidry.pdf","content_type":"application/pdf","file_id":"20601","access_level":"open_access"}],"isi":1,"language":[{"iso":"eng"}],"external_id":{"isi":["001592080300001"],"arxiv":["2508.18348"]},"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","image":"/images/cc_by.png","short":"CC BY (4.0)"}},{"date_published":"2025-10-01T00:00:00Z","day":"01","external_id":{"arxiv":["2502.18651"],"isi":["001595690000001"]},"language":[{"iso":"eng"}],"fulldoi":"https://doi.org/10.1088/1538-3873/ae051e","isi":1,"file":[{"file_name":"2025_PASP_BhattacharjeeS.pdf","content_type":"application/pdf","file_id":"20599","access_level":"open_access","success":1,"creator":"dernst","relation":"main_file","date_created":"2025-11-04T08:26:39Z","checksum":"cc7d00c349d48458accb0d3df67e4879","date_updated":"2025-11-04T08:26:39Z","file_size":12677603}],"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","image":"/images/cc_by.png","short":"CC BY (4.0)"},"title":"Variability of central stars of planetary nebulae with the Zwicky Transient Facility. II. Long-timescale variables including wide binary and late thermal pulse candidates","abstract":[{"text":"In this second paper on our variability survey of central stars of planetary nebulae (CSPNe) using the Zwicky Transient Facility (ZTF), we report 11 long-timescale variables with variability timescales ranging from months to years. We also present preliminary analyses based on spectroscopic and/or photometric follow-up observations for six of them. Among them is NGC 6833, which shows a 980 days periodic variability with strange characteristics: “triangle-shaped” brightening in r, i, and WISE bands but almost coincidental shallow dips in the g-band. The most plausible explanation is a wide binary with the photometric period being the orbital period. Long-period near-sinusoidal variability was detected in two other systems, NGC 6905 and Kn 26, with periods of 700 days and 230 days, respectively, making them additional wide-binary candidates. The latter also shows a short period at 1.18 hr. We then present CTSS 2 and K 3-5, which show brightening and significant reddening over the whole ZTF baseline. A stellar model fit to the optical spectrum of CTSS 2 reveals it to be one of the youngest post-AGB CSPNe known. Both show high-density emission-line cores. We propose these to be late-thermal-pulse candidates, currently evolving towards the AGB phase. We then present recent HST/COS ultraviolet spectroscopy of the known wide-binary candidate LoTr 1, showing that the hot star is a spectroscopic twin of the extremely hot white dwarf in UCAC2 46706450. Similar to this object, LoTr 1 also has a fast rotating wide subgiant companion. We suggest that the long photometric period of 11 yr is the binary orbital period. Finally, we briefly discuss the ZTF light curves of the remaining variables, namely Tan 2, K 3-20, WHTZ 3, Kn J1857+3931, and IPHAS J1927+0814. With these examples, we present the effectiveness of the von Neumann statistics and Pearson Skew-based metric space in searching for long-timescale variables.","lang":"eng"}],"file_date_updated":"2025-11-04T08:26:39Z","date_updated":"2025-12-01T15:13:50Z","status":"public","_id":"20588","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"IOP Publishing","doi":"10.1088/1538-3873/ae051e","ddc":["520"],"author":[{"last_name":"Bhattacharjee","first_name":"Soumyadeep","full_name":"Bhattacharjee, Soumyadeep"},{"full_name":"Reindl, Nicole","first_name":"Nicole","last_name":"Reindl"},{"full_name":"Bond, Howard E.","first_name":"Howard E.","last_name":"Bond"},{"last_name":"Werner","full_name":"Werner, Klaus","first_name":"Klaus"},{"last_name":"Zeimann","full_name":"Zeimann, Gregory R.","first_name":"Gregory R."},{"first_name":"David","full_name":"Jones, David","last_name":"Jones"},{"last_name":"El-Badry","full_name":"El-Badry, Kareem","first_name":"Kareem"},{"first_name":"Nina","full_name":"Mackensen, Nina","last_name":"Mackensen"},{"last_name":"Chornay","full_name":"Chornay, Nicholas","first_name":"Nicholas"},{"first_name":"S. R.","full_name":"Kulkarni, S. R.","last_name":"Kulkarni"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria","first_name":"Ilaria","last_name":"Caiazzo"},{"full_name":"Van Roestel, Jan","first_name":"Jan","last_name":"Van Roestel"},{"first_name":"Antonio C.","full_name":"Rodriguez, Antonio C.","last_name":"Rodriguez"},{"last_name":"Prince","first_name":"Thomas A.","full_name":"Prince, Thomas A."},{"last_name":"Rusholme","first_name":"Ben","full_name":"Rusholme, Ben"},{"last_name":"Laher","first_name":"Russ R.","full_name":"Laher, Russ R."},{"full_name":"Smith, Roger","first_name":"Roger","last_name":"Smith"}],"article_type":"original","publication_status":"published","month":"10","intvolume":" 137","issue":"10","oa_version":"Published Version","year":"2025","oa":1,"article_processing_charge":"Yes (in subscription journal)","date_created":"2025-11-02T23:01:34Z","department":[{"_id":"IlCa"}],"scopus_import":"1","publication":"Publications of the Astronomical Society of the Pacific","citation":{"short":"S. Bhattacharjee, N. Reindl, H.E. Bond, K. Werner, G.R. Zeimann, D. Jones, K. El-Badry, N. Mackensen, N. Chornay, S.R. Kulkarni, I. Caiazzo, J. Van Roestel, A.C. Rodriguez, T.A. Prince, B. Rusholme, R.R. Laher, R. Smith, Publications of the Astronomical Society of the Pacific 137 (2025).","ieee":"S. Bhattacharjee et al., “Variability of central stars of planetary nebulae with the Zwicky Transient Facility. II. Long-timescale variables including wide binary and late thermal pulse candidates,” Publications of the Astronomical Society of the Pacific, vol. 137, no. 10. IOP Publishing, 2025.","apa":"Bhattacharjee, S., Reindl, N., Bond, H. E., Werner, K., Zeimann, G. R., Jones, D., … Smith, R. (2025). Variability of central stars of planetary nebulae with the Zwicky Transient Facility. II. Long-timescale variables including wide binary and late thermal pulse candidates. Publications of the Astronomical Society of the Pacific. IOP Publishing. https://doi.org/10.1088/1538-3873/ae051e","chicago":"Bhattacharjee, Soumyadeep, Nicole Reindl, Howard E. Bond, Klaus Werner, Gregory R. Zeimann, David Jones, Kareem El-Badry, et al. “Variability of Central Stars of Planetary Nebulae with the Zwicky Transient Facility. II. Long-Timescale Variables Including Wide Binary and Late Thermal Pulse Candidates.” Publications of the Astronomical Society of the Pacific. IOP Publishing, 2025. https://doi.org/10.1088/1538-3873/ae051e.","ista":"Bhattacharjee S, Reindl N, Bond HE, Werner K, Zeimann GR, Jones D, El-Badry K, Mackensen N, Chornay N, Kulkarni SR, Caiazzo I, Van Roestel J, Rodriguez AC, Prince TA, Rusholme B, Laher RR, Smith R. 2025. Variability of central stars of planetary nebulae with the Zwicky Transient Facility. II. Long-timescale variables including wide binary and late thermal pulse candidates. Publications of the Astronomical Society of the Pacific. 137(10), 104206.","ama":"Bhattacharjee S, Reindl N, Bond HE, et al. Variability of central stars of planetary nebulae with the Zwicky Transient Facility. II. Long-timescale variables including wide binary and late thermal pulse candidates. Publications of the Astronomical Society of the Pacific. 2025;137(10). doi:10.1088/1538-3873/ae051e","mla":"Bhattacharjee, Soumyadeep, et al. “Variability of Central Stars of Planetary Nebulae with the Zwicky Transient Facility. II. Long-Timescale Variables Including Wide Binary and Late Thermal Pulse Candidates.” Publications of the Astronomical Society of the Pacific, vol. 137, no. 10, 104206, IOP Publishing, 2025, doi:10.1088/1538-3873/ae051e."},"has_accepted_license":"1","publication_identifier":{"issn":["1538-3873"]},"volume":137,"quality_controlled":"1","arxiv":1,"OA_place":"publisher","PlanS_conform":"1","OA_type":"hybrid","article_number":"104206","acknowledgement":"This work is 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 grant Nos. AST-1440341 and AST-2034437 and a collaboration including current partners Caltech, IPAC, the Oskar Klein Center at Stockholm University, the University of Maryland, University of California, Berkeley, the University of Wisconsin at Milwaukee, University of Warwick, Ruhr University Bochum, Cornell University, Northwestern University, and Drexel University. Operations are conducted by COO, IPAC, and UW.\r\n\r\nThis 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.\r\n\r\nWe are grateful to the staffs of Palomar Observatory and the Hobby-Eberly Telescope for assistance with the observations and data management. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council.\r\n\r\nThe Low-Resolution Spectrograph 2 (LRS2) on HET was developed and funded by the University of Texas at Austin McDonald Observatory and Department of Astronomy, and by Pennsylvania State University. We thank the Leibniz-Institut für Astrophysik Potsdam (AIP) and the Institut für Astrophysik Göttingen (IAG) for their contributions to the construction of the integral field units. We acknowledge the Texas Advanced Computing Center (TACC) at The University of Texas at Austin for providing high performance computing, visualization, and storage resources that have contributed to the results reported within this paper.\r\n\r\nThe Isaac Newton Telescope is operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias\r\n\r\nS.B. thanks Frank J. Masci and Zachary P. Vanderbosch for useful discussions and suggestions regarding solving the issues with ZTF forced photometry on extended sources. S.B. also thanks Jim Fuller, Charles C. Steidel, Lynne Hillenbrand, and Adolfo Carvalho for useful discussions on methods and science. S.B. acknowledges financial support from the Wallace L. W. Sargent Graduate Fellowship during the first year of his graduate studies at Caltech. N.C. was supported through the Cancer Research UK grant A24042.\r\n\r\nN.R. is supported by the Deutsche Forschungsgemeinschaft (DFG) through grant RE3915/2-1.\r\n\r\nD.J. acknowledges support from the Agencia Estatal de Investigación del Ministerio de Ciencia, Innovación y Universidades (MICIU/AEI) under grant “Nebulosas planetarias como clave para comprender la evolución de estrellas binarias” and the European Regional Development Fund (ERDF) with reference PID-2022-136653NA-I00 (DOI:10.13039/501100011033). D.J. also acknowledges support from the Agencia Estatal de Investigación del Ministerio de Ciencia, Innovación y Universidades (MICIU/AEI) under grant “Revolucionando el conocimiento de la evolución de estrellas poco masivas” and the the European Union NextGenerationEU/PRTR with reference CNS2023-143910 (DOI:10.13039/501100011033).\r\n\r\nWe have used Python packages Numpy (Harris et al. 2020), SciPy (Virtanen et al. 2020), Matplotlib (Hunter 2007), Pandas (pandas development team 2020), Astropy (Astropy Collaboration et al. 2013, 2018), and Astroquery (Ginsburg et al. 2019) at various stages of this research."},{"volume":137,"publication_identifier":{"issnl":["0004-6280"],"issn":["0004-6280"]},"arxiv":1,"OA_place":"publisher","quality_controlled":"1","OA_type":"hybrid","article_number":"024201","acknowledgement":"This work is 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 Oskar Klein Center at Stockholm University, the University of Maryland, University of California, Berkeley, the University of Wisconsin at Milwaukee, University of Warwick, Ruhr University Bochum, Cornell University, Northwestern University, and Drexel University. Operations are conducted by COO, IPAC, and UW.\r\n\r\nThis 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.\r\n\r\nWe are grateful to the staffs of Palomar Observatory and the Hobby-Eberly Telescope for assistance with the observations and data management. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council.\r\n\r\nThe Low-Resolution Spectrograph 2 (LRS2) on HET was developed and funded by the University of Texas at Austin McDonald Observatory and Department of Astronomy, and by Pennsylvania State University. We thank the Leibniz-Institut für Astrophysik Potsdam (AIP) and the Institut für Astrophysik Göttingen (IAG) for their contributions to the construction of the integral field units. We acknowledge the Texas Advanced Computing Center (TACC) at The University of Texas at Austin for providing high performance computing, visualization, and storage resources that have contributed to the results reported within this paper.\r\n\r\nWe thank the anonymous referee for the detailed comments, which improved the clarity of the manuscript significantly. We also thank Gunter Cibis for pointing out typographical errors in the names of a few PNe in the first draft. S.B. expresses gratitude to Kishalay De for providing the Gattini-IR and WISE data. S.B. thanks Frank J. Masci and Zachary P. Vanderbosch for useful discussions and suggestions regarding solving the issues with ZTF forced photometry on extended sources. S.B. also thanks Jim Fuller, Charles C. Steidel, Lynne Hillenbrand, and Adolfo Carvalho for useful discussions on methods and science. S.B. also thanks David O. Cook for providing access to his CLU image cutout service to generate the WeSb 1 image. S.B. acknowledges the financial support from the Wallace L. W. Sargent Graduate Fellowship during the first year of his graduate studies at Caltech. N.C. was supported through the Cancer Research UK grant A24042. S.B. thanks Martina Veresvarka for drawing our attention to the TESS light curves of WeSb 1.\r\n\r\nWe have used Python packages Numpy (Harris et al. 2020), SciPy (Virtanen et al. 2020), Matplotlib (Hunter 2007), Pandas (pandas development team 2020), Astropy (Astropy Collaboration et al. 2013, 2018), and Astroquery (Ginsburg et al. 2019) at various stages of this research.","das_tickbox":"1","date_created":"2025-02-16T23:02:33Z","scopus_import":"1","department":[{"_id":"IlCa"}],"publication":"Publications of the Astronomical Society of the Pacific","citation":{"ista":"Bhattacharjee S, Kulkarni SR, Kong AKH, Tam MS, Bond HE, El-Badry K, Caiazzo I, Chornay N, Graham MJ, Rodriguez AC, Zeimann GR, Fremling C, Drake AJ, Werner K, Rodriguez H, Prince TA, Laher RR, Chen TX, Riddle R. 2025. Variability of central stars of planetary nebulae with the zwicky transient facility. I. Methods, short-timescale variables, and the unusual nucleus of WeSb 1. Publications of the Astronomical Society of the Pacific. 137(2), 024201.","mla":"Bhattacharjee, Soumyadeep, et al. “Variability of Central Stars of Planetary Nebulae with the Zwicky Transient Facility. I. Methods, Short-Timescale Variables, and the Unusual Nucleus of WeSb 1.” Publications of the Astronomical Society of the Pacific, vol. 137, no. 2, 024201, IOP Publishing, 2025, doi:10.1088/1538-3873/ada702.","ama":"Bhattacharjee S, Kulkarni SR, Kong AKH, et al. Variability of central stars of planetary nebulae with the zwicky transient facility. I. Methods, short-timescale variables, and the unusual nucleus of WeSb 1. Publications of the Astronomical Society of the Pacific. 2025;137(2). doi:10.1088/1538-3873/ada702","apa":"Bhattacharjee, S., Kulkarni, S. R., Kong, A. K. H., Tam, M. S., Bond, H. E., El-Badry, K., … Riddle, R. (2025). Variability of central stars of planetary nebulae with the zwicky transient facility. I. Methods, short-timescale variables, and the unusual nucleus of WeSb 1. Publications of the Astronomical Society of the Pacific. IOP Publishing. https://doi.org/10.1088/1538-3873/ada702","ieee":"S. Bhattacharjee et al., “Variability of central stars of planetary nebulae with the zwicky transient facility. I. Methods, short-timescale variables, and the unusual nucleus of WeSb 1,” Publications of the Astronomical Society of the Pacific, vol. 137, no. 2. IOP Publishing, 2025.","short":"S. Bhattacharjee, S.R. Kulkarni, A.K.H. Kong, M.S. Tam, H.E. Bond, K. El-Badry, I. Caiazzo, N. Chornay, M.J. Graham, A.C. Rodriguez, G.R. Zeimann, C. Fremling, A.J. Drake, K. Werner, H. Rodriguez, T.A. Prince, R.R. Laher, T.X. Chen, R. Riddle, Publications of the Astronomical Society of the Pacific 137 (2025).","chicago":"Bhattacharjee, Soumyadeep, S. R. Kulkarni, Albert K.H. Kong, M. S. Tam, Howard E. Bond, Kareem El-Badry, Ilaria Caiazzo, et al. “Variability of Central Stars of Planetary Nebulae with the Zwicky Transient Facility. I. Methods, Short-Timescale Variables, and the Unusual Nucleus of WeSb 1.” Publications of the Astronomical Society of the Pacific. IOP Publishing, 2025. https://doi.org/10.1088/1538-3873/ada702."},"has_accepted_license":"1","related_material":{"link":[{"url":"https://doi.org/10.1088/1538-3873/adbcd8","relation":"erratum"}]},"month":"02","intvolume":" 137","oa_version":"Published Version","issue":"2","oa":1,"year":"2025","article_processing_charge":"No","ddc":["520"],"author":[{"last_name":"Bhattacharjee","full_name":"Bhattacharjee, Soumyadeep","first_name":"Soumyadeep"},{"first_name":"S. R.","full_name":"Kulkarni, S. R.","last_name":"Kulkarni"},{"last_name":"Kong","full_name":"Kong, Albert K.H.","first_name":"Albert K.H."},{"full_name":"Tam, M. S.","first_name":"M. S.","last_name":"Tam"},{"full_name":"Bond, Howard E.","first_name":"Howard E.","last_name":"Bond"},{"last_name":"El-Badry","first_name":"Kareem","full_name":"El-Badry, Kareem"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","last_name":"Caiazzo"},{"last_name":"Chornay","first_name":"Nicholas","full_name":"Chornay, Nicholas"},{"full_name":"Graham, Matthew J.","first_name":"Matthew J.","last_name":"Graham"},{"first_name":"Antonio C.","full_name":"Rodriguez, Antonio C.","last_name":"Rodriguez"},{"first_name":"Gregory R.","full_name":"Zeimann, Gregory R.","last_name":"Zeimann"},{"last_name":"Fremling","full_name":"Fremling, Christoffer","first_name":"Christoffer"},{"full_name":"Drake, Andrew J.","first_name":"Andrew J.","last_name":"Drake"},{"last_name":"Werner","first_name":"Klaus","full_name":"Werner, Klaus"},{"last_name":"Rodriguez","full_name":"Rodriguez, Hector","first_name":"Hector"},{"full_name":"Prince, Thomas A.","first_name":"Thomas A.","last_name":"Prince"},{"first_name":"Russ R.","full_name":"Laher, Russ R.","last_name":"Laher"},{"last_name":"Chen","first_name":"Tracy X.","full_name":"Chen, Tracy X."},{"last_name":"Riddle","first_name":"Reed","full_name":"Riddle, Reed"}],"publication_status":"published","article_type":"original","_id":"19025","status":"public","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"IOP Publishing","doi":"10.1088/1538-3873/ada702","title":"Variability of central stars of planetary nebulae with the zwicky transient facility. I. Methods, short-timescale variables, and the unusual nucleus of WeSb 1","abstract":[{"text":"A complete understanding of the central stars of planetary nebulae (CSPNe) remains elusive. Over the past several decades, time-series photometry of CSPNe has yielded significant results including, but not limited to, discoveries of nearly 100 binary systems, insights into pulsations and winds in young white dwarfs, and studies of stars undergoing very late thermal pulses. We have undertaken a systematic study of optical photometric variability of cataloged CSPNe, using the light curves from the Zwicky Transient Facility (ZTF). By applying appropriate variability metrics, we arrive at a list of 94 highly variable CSPN candidates. Based on the timescales of the light-curve activity, we classify the variables broadly into short- and long-timescale variables. In this first paper in this series, we focus on the former, which is the majority class comprising 83 objects. We report periods for six sources for the first time, and recover several known periodic variables. Among the aperiodic sources, most exhibit a jitter around a median flux with a stable amplitude, and a few show outbursts. We draw attention to WeSb 1, which shows a different kind of variability: prominent deep and aperiodic dips, resembling transits from a dust/debris disk. We find strong evidence for a binary nature of WeSb 1 (possibly an F-type subgiant companion). The compactness of the emission lines and inferred high electron densities make WeSb 1 a candidate for either an EGB 6-type planetary nucleus, or a symbiotic system inside an evolved planetary nebula, both of which are rare objects. To demonstrate further promise with ZTF, we report three additional newly identified periodic sources that do not appear in the list of highly variable sources. Finally, we also introduce a two-dimensional metric space defined by the von Neumann statistics and Pearson Skew and demonstrate its effectiveness in identifying unique variables of astrophysical interest, like WeSb 1.","lang":"eng"}],"file_date_updated":"2025-02-17T09:13:41Z","date_updated":"2026-07-22T06:39:53Z","tmp":{"short":"CC BY (3.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/3.0/legalcode","name":"Creative Commons Attribution 3.0 Unported (CC BY 3.0)"},"day":"01","date_published":"2025-02-01T00:00:00Z","external_id":{"isi":["001416903300001"],"arxiv":["2410.03589"]},"language":[{"iso":"eng"}],"file":[{"file_size":3657568,"date_updated":"2025-02-17T09:13:41Z","checksum":"42b942ee1bf32ed225024e168174be92","date_created":"2025-02-17T09:13:41Z","relation":"main_file","success":1,"creator":"dernst","access_level":"open_access","file_id":"19034","file_name":"2025_PASP_Bhattacharjee.pdf","content_type":"application/pdf"}],"fulldoi":"https://doi.org/10.1088/1538-3873/ada702","isi":1},{"article_processing_charge":"Yes","oa":1,"year":"2025","intvolume":" 694","oa_version":"Published Version","month":"02","article_type":"original","publication_status":"published","author":[{"first_name":"M.","full_name":"Scalco, M.","last_name":"Scalco"},{"full_name":"Gerasimov, R.","first_name":"R.","last_name":"Gerasimov"},{"last_name":"Bedin","first_name":"L. R.","full_name":"Bedin, L. R."},{"first_name":"E.","full_name":"Vesperini, E.","last_name":"Vesperini"},{"first_name":"M.","full_name":"Correnti, M.","last_name":"Correnti"},{"last_name":"Nardiello","full_name":"Nardiello, D.","first_name":"D."},{"last_name":"Burgasser","full_name":"Burgasser, A.","first_name":"A."},{"last_name":"Richer","first_name":"H.","full_name":"Richer, H."},{"full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","last_name":"Caiazzo"},{"first_name":"J.","full_name":"Heyl, J.","last_name":"Heyl"},{"last_name":"Libralato","first_name":"M.","full_name":"Libralato, M."},{"full_name":"Anderson, J.","first_name":"J.","last_name":"Anderson"},{"first_name":"M.","full_name":"Griggio, M.","last_name":"Griggio"}],"ddc":["520"],"acknowledgement":"We dedicate this paper to the memory of our colleague Prof. Harvey Richer (⋆ April 1944 —† 13 November 2023), a highly accomplished astronomer and expert in stellar populations and in particular within globular clusters, who passed away during this project. Harvey grew up in Montreal and was at least the second star man to graduate from his high school, having been preceded by William Shatner by more than a decade. He worked at the University of British Columbia for most of his career, and his focus was the late stages of stellar evolution, in particular carbon stars and white dwarfs. We thank the referee for his valuable suggestions and comments, which helped improve the paper, as well as for his prompt revision.","article_number":"A68","OA_type":"diamond","quality_controlled":"1","arxiv":1,"OA_place":"publisher","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"volume":694,"has_accepted_license":"1","citation":{"chicago":"Scalco, M., R. Gerasimov, L. R. Bedin, E. Vesperini, M. Correnti, D. Nardiello, A. Burgasser, et al. “JWST Photometry and Astrometry of 47 Tucanæ. Discontinuity in the Stellar Sequence at the Star--Brown Dwarf Transition.” Astronomy & Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202452907.","short":"M. Scalco, R. Gerasimov, L.R. Bedin, E. Vesperini, M. Correnti, D. Nardiello, A. Burgasser, H. Richer, I. Caiazzo, J. Heyl, M. Libralato, J. Anderson, M. Griggio, Astronomy & Astrophysics 694 (2025).","apa":"Scalco, M., Gerasimov, R., Bedin, L. R., Vesperini, E., Correnti, M., Nardiello, D., … Griggio, M. (2025). JWST photometry and astrometry of 47 Tucanæ. Discontinuity in the stellar sequence at the star--brown dwarf transition. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202452907","ieee":"M. Scalco et al., “JWST photometry and astrometry of 47 Tucanæ. Discontinuity in the stellar sequence at the star--brown dwarf transition,” Astronomy & Astrophysics, vol. 694. EDP Sciences, 2025.","mla":"Scalco, M., et al. “JWST Photometry and Astrometry of 47 Tucanæ. Discontinuity in the Stellar Sequence at the Star--Brown Dwarf Transition.” Astronomy & Astrophysics, vol. 694, A68, EDP Sciences, 2025, doi:10.1051/0004-6361/202452907.","ama":"Scalco M, Gerasimov R, Bedin LR, et al. JWST photometry and astrometry of 47 Tucanæ. Discontinuity in the stellar sequence at the star--brown dwarf transition. Astronomy & Astrophysics. 2025;694. doi:10.1051/0004-6361/202452907","ista":"Scalco M, Gerasimov R, Bedin LR, Vesperini E, Correnti M, Nardiello D, Burgasser A, Richer H, Caiazzo I, Heyl J, Libralato M, Anderson J, Griggio M. 2025. JWST photometry and astrometry of 47 Tucanæ. Discontinuity in the stellar sequence at the star--brown dwarf transition. Astronomy & Astrophysics. 694, A68."},"publication":"Astronomy & Astrophysics","department":[{"_id":"IlCa"}],"scopus_import":"1","date_created":"2025-01-21T15:29:36Z","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","image":"/images/cc_by.png","short":"CC BY (4.0)"},"fulldoi":"https://doi.org/10.1051/0004-6361/202452907","isi":1,"file":[{"access_level":"open_access","file_id":"19569","file_name":"2025_AstronomyAstrophysics_Scalco.pdf","content_type":"application/pdf","file_size":18080704,"date_updated":"2025-04-16T07:13:31Z","checksum":"db765ce222df60a1e7c19da1968906a8","date_created":"2025-04-16T07:13:31Z","relation":"main_file","success":1,"creator":"dernst"}],"language":[{"iso":"eng"}],"external_id":{"arxiv":["2501.04446"],"isi":["001414753300007"]},"day":"04","date_published":"2025-02-04T00:00:00Z","doi":"10.1051/0004-6361/202452907","publisher":"EDP Sciences","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","_id":"18866","status":"public","date_updated":"2026-09-24T13:45:58Z","file_date_updated":"2025-04-16T07:13:31Z","abstract":[{"lang":"eng","text":"Using JWST Near Infrared Camera (NIRCam) images of the globular cluster 47,Tucanæ, (or NGC,104), taken at two epochs just 7 months apart, we derived proper-motion membership down to F322W2 ∼ 27. We identified an intriguing feature at the very low-mass end of the main sequence, around ∼ 0.08,M_⋅, at magnitudes F322W2 ∼ 24 and m_ F150W2 ∼ 25. This feature, dubbed 'kink', is characterized by a prominent discontinuity in the slope of the main sequence. A similar discontinuity is seen in theoretical isochrones with oxygen-poor chemistries, related to the rapid onset of absorption. We therefore hypothesize that the cluster hosts disproportionately more oxygen-poor stars near the bottom of the main sequence compared to the upper main sequence and the red giant branch. Our results show no strong or conclusive evidence of a rise in the brown dwarf luminosity function at faint magnitudes, in contrast to previous findings likely affected by faint red background galaxies. In our analysis, we accounted for this contamination by using proper motion membership."}],"title":"JWST photometry and astrometry of 47 Tucanæ. Discontinuity in the stellar sequence at the star--brown dwarf transition"},{"arxiv":1,"quality_controlled":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"volume":528,"publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2024-03-26T09:43:55Z","scopus_import":"1","extern":"1","citation":{"apa":"Galiullin, I., Rodriguez, A. C., Kulkarni, S. R., Sunyaev, R., Gilfanov, M., Bikmaev, I., … Vanderbosch, Z. P. (2024). A joint SRG/eROSITA + ZTF search: Discovery of a 97-min period eclipsing cataclysmic variable with evidence of a brown dwarf secondary. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stae012","ieee":"I. Galiullin et al., “A joint SRG/eROSITA + ZTF search: Discovery of a 97-min period eclipsing cataclysmic variable with evidence of a brown dwarf secondary,” Monthly Notices of the Royal Astronomical Society, vol. 528, no. 1. Oxford University Press, pp. 676–692, 2024.","short":"I. Galiullin, A.C. Rodriguez, S.R. Kulkarni, R. Sunyaev, M. Gilfanov, I. Bikmaev, L. Yungelson, J. van Roestel, B.T. Gänsicke, I. Khamitov, P. Szkody, K. El-Badry, M. Suslikov, T.A. Prince, M. Buntov, I. Caiazzo, M. Gorbachev, M.J. Graham, R. Gumerov, E. Irtuganov, R.R. Laher, P. Medvedev, R. Riddle, B. Rusholme, N. Sakhibullin, A. Sklyanov, Z.P. Vanderbosch, Monthly Notices of the Royal Astronomical Society 528 (2024) 676–692.","chicago":"Galiullin, Ilkham, Antonio C Rodriguez, Shrinivas R Kulkarni, Rashid Sunyaev, Marat Gilfanov, Ilfan Bikmaev, Lev Yungelson, et al. “A Joint SRG/EROSITA + ZTF Search: Discovery of a 97-Min Period Eclipsing Cataclysmic Variable with Evidence of a Brown Dwarf Secondary.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2024. https://doi.org/10.1093/mnras/stae012.","ista":"Galiullin I, Rodriguez AC, Kulkarni SR, Sunyaev R, Gilfanov M, Bikmaev I, Yungelson L, van Roestel J, Gänsicke BT, Khamitov I, Szkody P, El-Badry K, Suslikov M, Prince TA, Buntov M, Caiazzo I, Gorbachev M, Graham MJ, Gumerov R, Irtuganov E, Laher RR, Medvedev P, Riddle R, Rusholme B, Sakhibullin N, Sklyanov A, Vanderbosch ZP. 2024. A joint SRG/eROSITA + ZTF search: Discovery of a 97-min period eclipsing cataclysmic variable with evidence of a brown dwarf secondary. Monthly Notices of the Royal Astronomical Society. 528(1), 676–692.","mla":"Galiullin, Ilkham, et al. “A Joint SRG/EROSITA + ZTF Search: Discovery of a 97-Min Period Eclipsing Cataclysmic Variable with Evidence of a Brown Dwarf Secondary.” Monthly Notices of the Royal Astronomical Society, vol. 528, no. 1, Oxford University Press, 2024, pp. 676–92, doi:10.1093/mnras/stae012.","ama":"Galiullin I, Rodriguez AC, Kulkarni SR, et al. A joint SRG/eROSITA + ZTF search: Discovery of a 97-min period eclipsing cataclysmic variable with evidence of a brown dwarf secondary. Monthly Notices of the Royal Astronomical Society. 2024;528(1):676-692. doi:10.1093/mnras/stae012"},"issue":"1","intvolume":" 528","oa_version":"Published Version","main_file_link":[{"url":"https://doi.org/10.1093/mnras/stae012","open_access":"1"}],"month":"01","oa":1,"year":"2024","article_processing_charge":"No","author":[{"first_name":"Ilkham","full_name":"Galiullin, Ilkham","last_name":"Galiullin"},{"first_name":"Antonio C","full_name":"Rodriguez, Antonio C","last_name":"Rodriguez"},{"last_name":"Kulkarni","full_name":"Kulkarni, Shrinivas R","first_name":"Shrinivas R"},{"last_name":"Sunyaev","full_name":"Sunyaev, Rashid","first_name":"Rashid"},{"last_name":"Gilfanov","first_name":"Marat","full_name":"Gilfanov, Marat"},{"last_name":"Bikmaev","full_name":"Bikmaev, Ilfan","first_name":"Ilfan"},{"last_name":"Yungelson","first_name":"Lev","full_name":"Yungelson, Lev"},{"first_name":"Jan","full_name":"van Roestel, Jan","last_name":"van Roestel"},{"full_name":"Gänsicke, Boris T","first_name":"Boris T","last_name":"Gänsicke"},{"last_name":"Khamitov","full_name":"Khamitov, Irek","first_name":"Irek"},{"last_name":"Szkody","full_name":"Szkody, Paula","first_name":"Paula"},{"first_name":"Kareem","full_name":"El-Badry, Kareem","last_name":"El-Badry"},{"full_name":"Suslikov, Mikhail","first_name":"Mikhail","last_name":"Suslikov"},{"first_name":"Thomas A","full_name":"Prince, Thomas A","last_name":"Prince"},{"last_name":"Buntov","full_name":"Buntov, Mikhail","first_name":"Mikhail"},{"last_name":"Caiazzo","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","first_name":"Ilaria"},{"full_name":"Gorbachev, Mark","first_name":"Mark","last_name":"Gorbachev"},{"last_name":"Graham","first_name":"Matthew J","full_name":"Graham, Matthew J"},{"last_name":"Gumerov","full_name":"Gumerov, Rustam","first_name":"Rustam"},{"first_name":"Eldar","full_name":"Irtuganov, Eldar","last_name":"Irtuganov"},{"first_name":"Russ R","full_name":"Laher, Russ R","last_name":"Laher"},{"last_name":"Medvedev","full_name":"Medvedev, Pavel","first_name":"Pavel"},{"last_name":"Riddle","full_name":"Riddle, Reed","first_name":"Reed"},{"full_name":"Rusholme, Ben","first_name":"Ben","last_name":"Rusholme"},{"first_name":"Nail","full_name":"Sakhibullin, Nail","last_name":"Sakhibullin"},{"last_name":"Sklyanov","full_name":"Sklyanov, Alexander","first_name":"Alexander"},{"last_name":"Vanderbosch","first_name":"Zachary P","full_name":"Vanderbosch, Zachary P"}],"publication_status":"published","article_type":"original","_id":"15189","status":"public","type":"journal_article","doi":"10.1093/mnras/stae012","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"Oxford University Press","abstract":[{"text":"Cataclysmic variables (CVs) that have evolved past the period minimum during their lifetimes are predicted to be systems with a brown dwarf donor. While population synthesis models predict that around 40–70 per cent of the Galactic CVs are post-period minimum systems referred to as ‘period bouncers’, only a few dozen confirmed systems are known. We report the study and characterization of a new eclipsing CV, SRGeJ041130.3+685350 (SRGeJ0411), discovered from a joint SRG/eROSITA and ZTF programme. The optical spectrum of SRGeJ0411 shows prominent hydrogen and helium emission lines, typical for CVs. We obtained optical high-speed photometry to confirm the eclipse of SRGeJ0411 and determine the orbital period to be Porb ≈ 97.530 min. The spectral energy distribution suggests that the donor has an effective temperature of ≲ 1800 K. We constrain the donor mass with the period–density relationship for Roche lobe-filling stars and find that Mdonor ≲ 0.04 M⊙. The binary parameters are consistent with evolutionary models for post-period minimum CVs, suggesting that SRGeJ0411 is a new period bouncer. The optical emission lines of SRGeJ0411 are single-peaked despite the system being eclipsing, which is typically only seen due to stream-fed accretion in polars. X-ray spectroscopy hints that the white dwarf in SRGeJ0411 could be magnetic, but verifying the magnetic nature of SRGeJ0411 requires further investigation. The lack of optical outbursts has made SRGeJ0411 elusive in previous surveys, and joint X-ray and optical surveys highlight the potential for discovering similar systems in the near future.","lang":"eng"}],"title":"A joint SRG/eROSITA + ZTF search: Discovery of a 97-min period eclipsing cataclysmic variable with evidence of a brown dwarf secondary","date_updated":"2024-04-02T06:50:01Z","page":"676-692","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"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","image":"/images/cc_by.png","short":"CC BY (4.0)"},"date_published":"2024-01-04T00:00:00Z","day":"04","language":[{"iso":"eng"}],"fulldoi":"https://doi.org/10.1093/mnras/stae012","external_id":{"arxiv":["2401.04178"]}},{"main_file_link":[{"open_access":"1","url":"https://doi.org/10.3847/1538-4357/ad08bf"}],"issue":"1","intvolume":" 961","oa_version":"Published Version","month":"01","oa":1,"year":"2024","article_processing_charge":"No","author":[{"full_name":"Gerasimov, Roman","first_name":"Roman","last_name":"Gerasimov"},{"last_name":"Burgasser","first_name":"Adam J.","full_name":"Burgasser, Adam J."},{"last_name":"Caiazzo","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","first_name":"Ilaria"},{"first_name":"Derek","full_name":"Homeier, Derek","last_name":"Homeier"},{"last_name":"Richer","first_name":"Harvey B.","full_name":"Richer, Harvey B."},{"full_name":"Correnti, Matteo","first_name":"Matteo","last_name":"Correnti"},{"full_name":"Heyl, Jeremy","first_name":"Jeremy","last_name":"Heyl"}],"article_type":"original","publication_status":"published","quality_controlled":"1","arxiv":1,"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"volume":961,"article_number":"139","publication":"The Astrophysical Journal","date_created":"2024-03-26T09:44:50Z","scopus_import":"1","extern":"1","citation":{"short":"R. Gerasimov, A.J. Burgasser, I. Caiazzo, D. Homeier, H.B. Richer, M. Correnti, J. Heyl, The Astrophysical Journal 961 (2024).","ieee":"R. Gerasimov et al., “Exploring the chemistry and mass function of the globular cluster 47 Tucanae with new theoretical color–magnitude diagrams,” The Astrophysical Journal, vol. 961, no. 1. American Astronomical Society, 2024.","apa":"Gerasimov, R., Burgasser, A. J., Caiazzo, I., Homeier, D., Richer, H. B., Correnti, M., & Heyl, J. (2024). Exploring the chemistry and mass function of the globular cluster 47 Tucanae with new theoretical color–magnitude diagrams. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/ad08bf","chicago":"Gerasimov, Roman, Adam J. Burgasser, Ilaria Caiazzo, Derek Homeier, Harvey B. Richer, Matteo Correnti, and Jeremy Heyl. “Exploring the Chemistry and Mass Function of the Globular Cluster 47 Tucanae with New Theoretical Color–Magnitude Diagrams.” The Astrophysical Journal. American Astronomical Society, 2024. https://doi.org/10.3847/1538-4357/ad08bf.","ista":"Gerasimov R, Burgasser AJ, Caiazzo I, Homeier D, Richer HB, Correnti M, Heyl J. 2024. Exploring the chemistry and mass function of the globular cluster 47 Tucanae with new theoretical color–magnitude diagrams. The Astrophysical Journal. 961(1), 139.","ama":"Gerasimov R, Burgasser AJ, Caiazzo I, et al. Exploring the chemistry and mass function of the globular cluster 47 Tucanae with new theoretical color–magnitude diagrams. The Astrophysical Journal. 2024;961(1). doi:10.3847/1538-4357/ad08bf","mla":"Gerasimov, Roman, et al. “Exploring the Chemistry and Mass Function of the Globular Cluster 47 Tucanae with New Theoretical Color–Magnitude Diagrams.” The Astrophysical Journal, vol. 961, no. 1, 139, American Astronomical Society, 2024, doi:10.3847/1538-4357/ad08bf."},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"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","image":"/images/cc_by.png","short":"CC BY (4.0)"},"day":"22","date_published":"2024-01-22T00:00:00Z","language":[{"iso":"eng"}],"fulldoi":"https://doi.org/10.3847/1538-4357/ad08bf","external_id":{"arxiv":["2310.11800"]},"status":"public","_id":"15191","type":"journal_article","doi":"10.3847/1538-4357/ad08bf","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"American Astronomical Society","abstract":[{"text":"Despite their shared origin, members of globular clusters display star-to-star variations in composition. The observed pattern of element abundances is unique to these stellar environments and cannot be fully explained by any proposed mechanism. It remains unclear whether stars form with chemical heterogeneity or inherit it from interactions with other members. These scenarios may be differentiated by the dependence of chemical spread on stellar mass; however, obtaining a sufficiently large mass baseline requires abundance measurements on the lower main sequence, which is too faint for spectroscopy even in the nearest globular clusters. We developed a stellar modeling method to obtain precise chemical abundances for stars near the end of the main sequence from multiband photometry, and we applied it to the globular cluster 47 Tucanae. The computational efficiency is attained by matching chemical elements to the model components that are most sensitive to their abundance. We determined [O/Fe] for ∼5000 members below the main-sequence knee at the level of accuracy, comparable to the spectroscopic measurements of evolved members in the literature. The inferred distribution disfavors stellar interactions as the origin of chemical spread; however, an accurate theory of accretion is required to draw a more definitive conclusion. We anticipate that future observations of 47 Tucanae with the James Webb Space Telescope will extend the mass baseline of our analysis into the substellar regime. Therefore, we present predicted color–magnitude diagrams and mass–magnitude relations for the brown dwarf members of 47 Tucanae.","lang":"eng"}],"title":"Exploring the chemistry and mass function of the globular cluster 47 Tucanae with new theoretical color–magnitude diagrams","date_updated":"2024-04-02T06:52:43Z"},{"has_accepted_license":"1","citation":{"ama":"Blomberg L, El-Badry K, Breivik K, et al. The companion mass distribution of post common envelope hot subdwarf binaries: Evidence for boosted and disrupted magnetic braking? Publications of the Astronomical Society of the Pacific. 2024;136(12). doi:10.1088/1538-3873/ad94a2","mla":"Blomberg, Lisa, et al. “The Companion Mass Distribution of Post Common Envelope Hot Subdwarf Binaries: Evidence for Boosted and Disrupted Magnetic Braking?” Publications of the Astronomical Society of the Pacific, vol. 136, no. 12, 124201, IOP Publishing, 2024, doi:10.1088/1538-3873/ad94a2.","ista":"Blomberg L, El-Badry K, Breivik K, Caiazzo I, Nagarajan P, Rodriguez A, Van Roestel J, Vanderbosch ZP, Yamaguchi N. 2024. The companion mass distribution of post common envelope hot subdwarf binaries: Evidence for boosted and disrupted magnetic braking? Publications of the Astronomical Society of the Pacific. 136(12), 124201.","chicago":"Blomberg, Lisa, Kareem El-Badry, Katelyn Breivik, Ilaria Caiazzo, Pranav Nagarajan, Antonio Rodriguez, Jan Van Roestel, Zachary P. Vanderbosch, and Natsuko Yamaguchi. “The Companion Mass Distribution of Post Common Envelope Hot Subdwarf Binaries: Evidence for Boosted and Disrupted Magnetic Braking?” Publications of the Astronomical Society of the Pacific. IOP Publishing, 2024. https://doi.org/10.1088/1538-3873/ad94a2.","short":"L. Blomberg, K. El-Badry, K. Breivik, I. Caiazzo, P. Nagarajan, A. Rodriguez, J. Van Roestel, Z.P. Vanderbosch, N. Yamaguchi, Publications of the Astronomical Society of the Pacific 136 (2024).","apa":"Blomberg, L., El-Badry, K., Breivik, K., Caiazzo, I., Nagarajan, P., Rodriguez, A., … Yamaguchi, N. (2024). The companion mass distribution of post common envelope hot subdwarf binaries: Evidence for boosted and disrupted magnetic braking? Publications of the Astronomical Society of the Pacific. IOP Publishing. https://doi.org/10.1088/1538-3873/ad94a2","ieee":"L. Blomberg et al., “The companion mass distribution of post common envelope hot subdwarf binaries: Evidence for boosted and disrupted magnetic braking?,” Publications of the Astronomical Society of the Pacific, vol. 136, no. 12. IOP Publishing, 2024."},"publication":"Publications of the Astronomical Society of the Pacific","date_created":"2024-12-29T23:01:57Z","department":[{"_id":"IlCa"}],"scopus_import":"1","article_number":"124201","acknowledgement":"We thank the referee for their constructive comments. We also thank Jim Fuller and Stefan Geier for helpful discussions. The Kavli Institute for Theoretical Physics (KITP) hosted the program, \"White Dwarfs as Probes of the Evolution of Planets, Stars, the Milky Way, and the Expanding Universe,\" during which this project was initiated.\r\n\r\nThis research was supported in part by the U.S. National Science Foundation (NSF) grant AST-2307232, and in part by grants PHY-1748958 and AST-2107070.\r\n\r\nThis 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.\r\n\r\nThis work is based in part on observations obtained with the Samuel Oschin 48 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the NSF under grant AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and the Lawrence Berkeley National Laboratory. Operations are conducted by the Caltech Optical Observatories (COO), the Infrared Processing and Analysis Center (IPAC), and the University of Washington (UW).\r\n\r\nSome of the data presented herein were obtained at Keck Observatory, which is a private 501(c)3 non-profit 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.","arxiv":1,"OA_place":"publisher","quality_controlled":"1","OA_type":"hybrid","volume":136,"publication_identifier":{"issn":["0004-6280"]},"author":[{"first_name":"Lisa","full_name":"Blomberg, Lisa","last_name":"Blomberg"},{"full_name":"El-Badry, Kareem","first_name":"Kareem","last_name":"El-Badry"},{"last_name":"Breivik","first_name":"Katelyn","full_name":"Breivik, Katelyn"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria","first_name":"Ilaria","last_name":"Caiazzo"},{"last_name":"Nagarajan","first_name":"Pranav","full_name":"Nagarajan, Pranav"},{"last_name":"Rodriguez","full_name":"Rodriguez, Antonio","first_name":"Antonio"},{"last_name":"Van Roestel","full_name":"Van Roestel, Jan","first_name":"Jan"},{"first_name":"Zachary P.","full_name":"Vanderbosch, Zachary P.","last_name":"Vanderbosch"},{"last_name":"Yamaguchi","full_name":"Yamaguchi, Natsuko","first_name":"Natsuko"}],"publication_status":"published","article_type":"original","ddc":["520"],"oa":1,"year":"2024","article_processing_charge":"No","intvolume":" 136","issue":"12","oa_version":"Published Version","month":"12","date_updated":"2025-09-09T11:55:13Z","abstract":[{"text":"We measure the mass distribution of main-sequence (MS) companions to hot subdwarf B stars (sdBs) in post-common envelope binaries (PCEBs). We carried out a spectroscopic survey of 14 eclipsing systems (\"HW Vir binaries\") with orbital periods of 3.8 < Porb < 12 hr, resulting in a well-understood selection function and a near-complete sample of HW Vir binaries with G < 16. We constrain companion masses from the radial velocity curves of the sdB stars. The companion mass distribution peaks at MMS ≈ 0.15 M⊙ and drops off at MMS > 0.2 M⊙, with only two systems hosting companions above the fully convective limit. There is no correlation between Porb and MMS within the sample. A similar drop-off in the companion mass distribution of white dwarf (WD) + MS PCEBs has been attributed to disrupted magnetic braking (MB) below the fully convective limit. We compare the sdB companion mass distribution to predictions of binary evolution simulations with a range of MB laws. Because sdBs have short lifetimes compared to WDs, explaining the lack of higher-mass MS companions to sdBs with disrupted MB requires MB to be boosted by a factor of 20–100 relative to MB laws inferred from the rotation evolution of single stars. We speculate that such boosting may be a result of irradiation-driven enhancement of the MS stars' winds. An alternative possibility is that common envelope evolution favors low-mass companions in short-period orbits, but the existence of massive WD companions to sdBs with similar periods disfavors this scenario.","lang":"eng"}],"file_date_updated":"2025-01-02T09:34:25Z","title":"The companion mass distribution of post common envelope hot subdwarf binaries: Evidence for boosted and disrupted magnetic braking?","doi":"10.1088/1538-3873/ad94a2","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publisher":"IOP Publishing","status":"public","_id":"18709","type":"journal_article","language":[{"iso":"eng"}],"file":[{"file_size":7539133,"checksum":"56fe719e26bc0c2a99ac5322791107e5","date_updated":"2025-01-02T09:34:25Z","date_created":"2025-01-02T09:34:25Z","relation":"main_file","success":1,"creator":"dernst","access_level":"open_access","file_id":"18719","content_type":"application/pdf","file_name":"2024_PASP_Blomberg.pdf"}],"fulldoi":"https://doi.org/10.1088/1538-3873/ad94a2","isi":1,"external_id":{"arxiv":["2408.15334"],"isi":["001379604600001"]},"date_published":"2024-12-01T00:00:00Z","day":"01","tmp":{"short":"CC BY (3.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/3.0/legalcode","name":"Creative Commons Attribution 3.0 Unported (CC BY 3.0)"}}]