[{"arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","DOAJ_listed":"1","type":"journal_article","oa_version":"Published Version","article_type":"original","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","department":[{"_id":"IlCa"}],"article_processing_charge":"Yes","language":[{"iso":"eng"}],"OA_type":"gold","ddc":["520"],"_id":"19964","file":[{"access_level":"open_access","date_updated":"2025-07-08T06:40:54Z","file_name":"2025_AstronomicalJour_Cheng.pdf","checksum":"144b0e46aa3dff0cdf8c6ee7d4fe2fe4","success":1,"content_type":"application/pdf","date_created":"2025-07-08T06:40:54Z","creator":"dernst","file_id":"19975","relation":"main_file","file_size":931173}],"intvolume":"       170","scopus_import":"1","doi":"10.3847/1538-3881/addd21","status":"public","publication_status":"published","issue":"1","date_updated":"2026-02-19T09:31:41Z","month":"07","quality_controlled":"1","author":[{"last_name":"Cheng","first_name":"Sihao","full_name":"Cheng, Sihao"},{"full_name":"Schlaufman, Kevin C.","first_name":"Kevin C.","last_name":"Schlaufman"},{"orcid":"0000-0002-4770-5388","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","last_name":"Caiazzo","first_name":"Ilaria","full_name":"Caiazzo, Ilaria"}],"oa":1,"date_created":"2025-07-06T22:01:22Z","day":"01","article_number":"47","year":"2025","volume":170,"has_accepted_license":"1","publisher":"IOP Publishing","isi":1,"tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"date_published":"2025-07-01T00:00:00Z","file_date_updated":"2025-07-08T06:40:54Z","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).","external_id":{"arxiv":["2408.03985"],"isi":["001514518100001"]},"publication_identifier":{"eissn":["1538-3881"],"issn":["0004-6256"]},"OA_place":"publisher","publication":"The Astronomical Journal","citation":{"apa":"Cheng, S., Schlaufman, K. C., &#38; 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. <i>The Astronomical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-3881/addd21\">https://doi.org/10.3847/1538-3881/addd21</a>","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.” <i>The Astronomical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-3881/addd21\">https://doi.org/10.3847/1538-3881/addd21</a>.","short":"S. Cheng, K.C. Schlaufman, I. Caiazzo, The Astronomical Journal 170 (2025).","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,” <i>The Astronomical Journal</i>, vol. 170, no. 1. IOP Publishing, 2025.","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.","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.” <i>The Astronomical Journal</i>, vol. 170, no. 1, 47, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-3881/addd21\">10.3847/1538-3881/addd21</a>.","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. <i>The Astronomical Journal</i>. 2025;170(1). doi:<a href=\"https://doi.org/10.3847/1538-3881/addd21\">10.3847/1538-3881/addd21</a>"},"abstract":[{"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⊙.","lang":"eng"}]},{"type":"journal_article","oa_version":"Published Version","PlanS_conform":"1","article_type":"original","title":"Transiting planetary debris near the Roche limit of a white dwarf on a 4.97 hr orbit—and its vanishing","department":[{"_id":"IlCa"}],"arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","DOAJ_listed":"1","intvolume":"       992","doi":"10.3847/1538-4357/adfecb","scopus_import":"1","status":"public","publication_status":"published","issue":"2","date_updated":"2026-02-16T12:43:29Z","article_processing_charge":"Yes","language":[{"iso":"eng"}],"OA_type":"gold","ddc":["520"],"file":[{"date_created":"2025-11-04T12:33:51Z","content_type":"application/pdf","success":1,"checksum":"24892d1b5bfa1867eb0a353f10c31b82","file_name":"2025_AstrophysicalJour_Guidry.pdf","date_updated":"2025-11-04T12:33:51Z","access_level":"open_access","file_size":5323398,"relation":"main_file","creator":"dernst","file_id":"20601"}],"_id":"20586","date_created":"2025-11-02T23:01:33Z","article_number":"167","day":"20","year":"2025","volume":992,"month":"10","quality_controlled":"1","author":[{"full_name":"Guidry, Joseph A.","last_name":"Guidry","first_name":"Joseph A."},{"full_name":"Vanderbosch, Zachary P.","first_name":"Zachary P.","last_name":"Vanderbosch"},{"first_name":"J. J.","last_name":"Hermes","full_name":"Hermes, J. J."},{"full_name":"Veras, Dimitri","first_name":"Dimitri","last_name":"Veras"},{"full_name":"Hollands, Mark A.","first_name":"Mark A.","last_name":"Hollands"},{"full_name":"Bhattacharjee, Soumyadeep","last_name":"Bhattacharjee","first_name":"Soumyadeep"},{"last_name":"Caiazzo","first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria"},{"last_name":"El-Badry","first_name":"Kareem","full_name":"El-Badry, Kareem"},{"full_name":"Kao, Malia L.","last_name":"Kao","first_name":"Malia L."},{"full_name":"Ould Rouis, Lou Baya","first_name":"Lou Baya","last_name":"Ould Rouis"},{"full_name":"Rodriguez, Antonio C.","last_name":"Rodriguez","first_name":"Antonio C."},{"first_name":"Jan","last_name":"Van Roestel","full_name":"Van Roestel, Jan"}],"oa":1,"publication":"The Astrophysical Journal","citation":{"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.” <i>The Astrophysical Journal</i>, vol. 992, no. 2, 167, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/adfecb\">10.3847/1538-4357/adfecb</a>.","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. <i>The Astrophysical Journal</i>. 2025;992(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/adfecb\">10.3847/1538-4357/adfecb</a>","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.","ieee":"J. A. Guidry <i>et al.</i>, “Transiting planetary debris near the Roche limit of a white dwarf on a 4.97 hr orbit—and its vanishing,” <i>The Astrophysical Journal</i>, 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. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/adfecb\">https://doi.org/10.3847/1538-4357/adfecb</a>","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).","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.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/adfecb\">https://doi.org/10.3847/1538-4357/adfecb</a>."},"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."}],"has_accepted_license":"1","publisher":"IOP Publishing","isi":1,"tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"external_id":{"isi":["001592080300001"],"arxiv":["2508.18348"]},"date_published":"2025-10-20T00:00:00Z","file_date_updated":"2025-11-04T12:33:51Z","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).","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"OA_place":"publisher"},{"month":"10","author":[{"full_name":"Bhattacharjee, Soumyadeep","first_name":"Soumyadeep","last_name":"Bhattacharjee"},{"full_name":"Reindl, Nicole","first_name":"Nicole","last_name":"Reindl"},{"full_name":"Bond, Howard E.","first_name":"Howard E.","last_name":"Bond"},{"first_name":"Klaus","last_name":"Werner","full_name":"Werner, Klaus"},{"first_name":"Gregory R.","last_name":"Zeimann","full_name":"Zeimann, Gregory R."},{"full_name":"Jones, David","last_name":"Jones","first_name":"David"},{"first_name":"Kareem","last_name":"El-Badry","full_name":"El-Badry, Kareem"},{"full_name":"Mackensen, Nina","last_name":"Mackensen","first_name":"Nina"},{"last_name":"Chornay","first_name":"Nicholas","full_name":"Chornay, Nicholas"},{"full_name":"Kulkarni, S. R.","first_name":"S. R.","last_name":"Kulkarni"},{"full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","last_name":"Caiazzo"},{"full_name":"Van Roestel, Jan","last_name":"Van Roestel","first_name":"Jan"},{"first_name":"Antonio C.","last_name":"Rodriguez","full_name":"Rodriguez, Antonio C."},{"full_name":"Prince, Thomas A.","last_name":"Prince","first_name":"Thomas A."},{"full_name":"Rusholme, Ben","first_name":"Ben","last_name":"Rusholme"},{"full_name":"Laher, Russ R.","first_name":"Russ R.","last_name":"Laher"},{"first_name":"Roger","last_name":"Smith","full_name":"Smith, Roger"}],"quality_controlled":"1","oa":1,"date_created":"2025-11-02T23:01:34Z","year":"2025","day":"01","article_number":"104206","volume":137,"has_accepted_license":"1","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"publisher":"IOP Publishing","isi":1,"OA_place":"publisher","publication_identifier":{"issn":["1538-3873"]},"file_date_updated":"2025-11-04T08:26:39Z","date_published":"2025-10-01T00:00:00Z","external_id":{"arxiv":["2502.18651"],"isi":["001595690000001"]},"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.","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).","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.” <i>Publications of the Astronomical Society of the Pacific</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.1088/1538-3873/ae051e\">https://doi.org/10.1088/1538-3873/ae051e</a>.","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. <i>Publications of the Astronomical Society of the Pacific</i>. IOP Publishing. <a href=\"https://doi.org/10.1088/1538-3873/ae051e\">https://doi.org/10.1088/1538-3873/ae051e</a>","ieee":"S. Bhattacharjee <i>et al.</i>, “Variability of central stars of planetary nebulae with the Zwicky Transient Facility. II. Long-timescale variables including wide binary and late thermal pulse candidates,” <i>Publications of the Astronomical Society of the Pacific</i>, vol. 137, no. 10. IOP Publishing, 2025.","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. <i>Publications of the Astronomical Society of the Pacific</i>. 2025;137(10). doi:<a href=\"https://doi.org/10.1088/1538-3873/ae051e\">10.1088/1538-3873/ae051e</a>","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.” <i>Publications of the Astronomical Society of the Pacific</i>, vol. 137, no. 10, 104206, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.1088/1538-3873/ae051e\">10.1088/1538-3873/ae051e</a>."},"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"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"oa_version":"Published Version","PlanS_conform":"1","type":"journal_article","article_type":"original","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","department":[{"_id":"IlCa"}],"OA_type":"hybrid","article_processing_charge":"Yes (in subscription journal)","language":[{"iso":"eng"}],"file":[{"relation":"main_file","file_size":12677603,"file_id":"20599","creator":"dernst","date_created":"2025-11-04T08:26:39Z","content_type":"application/pdf","success":1,"checksum":"cc7d00c349d48458accb0d3df67e4879","file_name":"2025_PASP_BhattacharjeeS.pdf","date_updated":"2025-11-04T08:26:39Z","access_level":"open_access"}],"_id":"20588","ddc":["520"],"intvolume":"       137","scopus_import":"1","doi":"10.1088/1538-3873/ae051e","publication_status":"published","issue":"10","status":"public","date_updated":"2025-12-01T15:13:50Z"},{"arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","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","department":[{"_id":"IlCa"}],"type":"journal_article","oa_version":"Published Version","article_type":"original","language":[{"iso":"eng"}],"OA_type":"hybrid","article_processing_charge":"No","ddc":["520"],"file":[{"date_updated":"2025-02-17T09:13:41Z","access_level":"open_access","checksum":"42b942ee1bf32ed225024e168174be92","file_name":"2025_PASP_Bhattacharjee.pdf","success":1,"date_created":"2025-02-17T09:13:41Z","content_type":"application/pdf","file_id":"19034","creator":"dernst","relation":"main_file","file_size":3657568}],"_id":"19025","status":"public","issue":"2","publication_status":"published","date_updated":"2026-07-22T06:39:53Z","intvolume":"       137","doi":"10.1088/1538-3873/ada702","scopus_import":"1","oa":1,"month":"02","quality_controlled":"1","author":[{"full_name":"Bhattacharjee, Soumyadeep","last_name":"Bhattacharjee","first_name":"Soumyadeep"},{"first_name":"S. R.","last_name":"Kulkarni","full_name":"Kulkarni, S. R."},{"full_name":"Kong, Albert K.H.","first_name":"Albert K.H.","last_name":"Kong"},{"full_name":"Tam, M. S.","first_name":"M. S.","last_name":"Tam"},{"last_name":"Bond","first_name":"Howard E.","full_name":"Bond, Howard E."},{"full_name":"El-Badry, Kareem","last_name":"El-Badry","first_name":"Kareem"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","orcid":"0000-0002-4770-5388","first_name":"Ilaria","last_name":"Caiazzo","full_name":"Caiazzo, Ilaria"},{"last_name":"Chornay","first_name":"Nicholas","full_name":"Chornay, Nicholas"},{"full_name":"Graham, Matthew J.","first_name":"Matthew J.","last_name":"Graham"},{"full_name":"Rodriguez, Antonio C.","first_name":"Antonio C.","last_name":"Rodriguez"},{"first_name":"Gregory R.","last_name":"Zeimann","full_name":"Zeimann, Gregory R."},{"full_name":"Fremling, Christoffer","first_name":"Christoffer","last_name":"Fremling"},{"full_name":"Drake, Andrew J.","first_name":"Andrew J.","last_name":"Drake"},{"first_name":"Klaus","last_name":"Werner","full_name":"Werner, Klaus"},{"last_name":"Rodriguez","first_name":"Hector","full_name":"Rodriguez, Hector"},{"last_name":"Prince","first_name":"Thomas A.","full_name":"Prince, Thomas A."},{"full_name":"Laher, Russ R.","first_name":"Russ R.","last_name":"Laher"},{"first_name":"Tracy X.","last_name":"Chen","full_name":"Chen, Tracy X."},{"first_name":"Reed","last_name":"Riddle","full_name":"Riddle, Reed"}],"related_material":{"link":[{"url":"https://doi.org/10.1088/1538-3873/adbcd8","relation":"erratum"}]},"volume":137,"date_created":"2025-02-16T23:02:33Z","article_number":"024201","day":"01","year":"2025","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.","external_id":{"isi":["001416903300001"],"arxiv":["2410.03589"]},"file_date_updated":"2025-02-17T09:13:41Z","date_published":"2025-02-01T00:00:00Z","OA_place":"publisher","publication_identifier":{"issnl":["0004-6280"],"issn":["0004-6280"]},"has_accepted_license":"1","das_tickbox":"1","isi":1,"publisher":"IOP Publishing","tmp":{"image":"/images/cc_by.png","short":"CC BY (3.0)","name":"Creative Commons Attribution 3.0 Unported (CC BY 3.0)","legal_code_url":"https://creativecommons.org/licenses/by/3.0/legalcode"},"citation":{"ieee":"S. Bhattacharjee <i>et al.</i>, “Variability of central stars of planetary nebulae with the zwicky transient facility. I. Methods, short-timescale variables, and the unusual nucleus of WeSb 1,” <i>Publications of the Astronomical Society of the Pacific</i>, vol. 137, no. 2. IOP Publishing, 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.” <i>Publications of the Astronomical Society of the Pacific</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.1088/1538-3873/ada702\">https://doi.org/10.1088/1538-3873/ada702</a>.","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).","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. <i>Publications of the Astronomical Society of the Pacific</i>. IOP Publishing. <a href=\"https://doi.org/10.1088/1538-3873/ada702\">https://doi.org/10.1088/1538-3873/ada702</a>","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. <i>Publications of the Astronomical Society of the Pacific</i>. 2025;137(2). doi:<a href=\"https://doi.org/10.1088/1538-3873/ada702\">10.1088/1538-3873/ada702</a>","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.” <i>Publications of the Astronomical Society of the Pacific</i>, vol. 137, no. 2, 024201, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.1088/1538-3873/ada702\">10.1088/1538-3873/ada702</a>.","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."},"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"}],"publication":"Publications of the Astronomical Society of the Pacific"},{"title":"The companion mass distribution of post common envelope hot subdwarf binaries: Evidence for boosted and disrupted magnetic braking?","department":[{"_id":"IlCa"}],"oa_version":"Published Version","type":"journal_article","article_type":"original","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","arxiv":1,"issue":"12","publication_status":"published","status":"public","date_updated":"2025-09-09T11:55:13Z","intvolume":"       136","doi":"10.1088/1538-3873/ad94a2","scopus_import":"1","language":[{"iso":"eng"}],"article_processing_charge":"No","OA_type":"hybrid","_id":"18709","file":[{"success":1,"date_created":"2025-01-02T09:34:25Z","content_type":"application/pdf","date_updated":"2025-01-02T09:34:25Z","access_level":"open_access","checksum":"56fe719e26bc0c2a99ac5322791107e5","file_name":"2024_PASP_Blomberg.pdf","relation":"main_file","file_size":7539133,"creator":"dernst","file_id":"18719"}],"ddc":["520"],"volume":136,"date_created":"2024-12-29T23:01:57Z","year":"2024","day":"01","article_number":"124201","oa":1,"month":"12","author":[{"full_name":"Blomberg, Lisa","last_name":"Blomberg","first_name":"Lisa"},{"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","last_name":"Caiazzo","first_name":"Ilaria","full_name":"Caiazzo, Ilaria"},{"full_name":"Nagarajan, Pranav","last_name":"Nagarajan","first_name":"Pranav"},{"full_name":"Rodriguez, Antonio","first_name":"Antonio","last_name":"Rodriguez"},{"full_name":"Van Roestel, Jan","last_name":"Van Roestel","first_name":"Jan"},{"full_name":"Vanderbosch, Zachary P.","first_name":"Zachary P.","last_name":"Vanderbosch"},{"full_name":"Yamaguchi, Natsuko","last_name":"Yamaguchi","first_name":"Natsuko"}],"quality_controlled":"1","citation":{"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.","mla":"Blomberg, Lisa, et al. “The Companion Mass Distribution of Post Common Envelope Hot Subdwarf Binaries: Evidence for Boosted and Disrupted Magnetic Braking?” <i>Publications of the Astronomical Society of the Pacific</i>, vol. 136, no. 12, 124201, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.1088/1538-3873/ad94a2\">10.1088/1538-3873/ad94a2</a>.","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? <i>Publications of the Astronomical Society of the Pacific</i>. 2024;136(12). doi:<a href=\"https://doi.org/10.1088/1538-3873/ad94a2\">10.1088/1538-3873/ad94a2</a>","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? <i>Publications of the Astronomical Society of the Pacific</i>. IOP Publishing. <a href=\"https://doi.org/10.1088/1538-3873/ad94a2\">https://doi.org/10.1088/1538-3873/ad94a2</a>","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?” <i>Publications of the Astronomical Society of the Pacific</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.1088/1538-3873/ad94a2\">https://doi.org/10.1088/1538-3873/ad94a2</a>.","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).","ieee":"L. Blomberg <i>et al.</i>, “The companion mass distribution of post common envelope hot subdwarf binaries: Evidence for boosted and disrupted magnetic braking?,” <i>Publications of the Astronomical Society of the Pacific</i>, vol. 136, no. 12. IOP Publishing, 2024."},"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"}],"publication":"Publications of the Astronomical Society of the Pacific","OA_place":"publisher","publication_identifier":{"issn":["0004-6280"]},"external_id":{"isi":["001379604600001"],"arxiv":["2408.15334"]},"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.","date_published":"2024-12-01T00:00:00Z","file_date_updated":"2025-01-02T09:34:25Z","has_accepted_license":"1","tmp":{"image":"/images/cc_by.png","short":"CC BY (3.0)","name":"Creative Commons Attribution 3.0 Unported (CC BY 3.0)","legal_code_url":"https://creativecommons.org/licenses/by/3.0/legalcode"},"publisher":"IOP Publishing","isi":1},{"scopus_import":"1","doi":"10.3847/2041-8213/ad713b","intvolume":"       975","date_updated":"2026-07-06T12:21:32Z","publication_status":"published","issue":"1","status":"public","file":[{"creator":"dernst","file_id":"18573","file_size":90328868,"relation":"main_file","checksum":"51e790dd3d85ca984e656734f9f611da","file_name":"2024_AstrophysJourLetters_Cunningham.pdf","date_updated":"2024-11-20T12:24:52Z","access_level":"open_access","date_created":"2024-11-20T12:24:52Z","content_type":"application/pdf","success":1}],"_id":"18564","ddc":["520"],"language":[{"iso":"eng"}],"OA_type":"gold","article_processing_charge":"Yes","article_type":"original","oa_version":"Published Version","type":"journal_article","department":[{"_id":"IlCa"}],"title":"Expansion properties of the young supernova type Iax remnant Pa 30 revealed","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"DOAJ_listed":"1","project":[{"name":"IST Austria Open Access Fund","_id":"B67AFEDC-15C9-11EA-A837-991A96BB2854"}],"publication":"The Astrophysical Journal Letters","abstract":[{"lang":"eng","text":"The recently discovered Pa 30 nebula, the putative type Iax supernova remnant associated with the historical supernova of 1181 AD, shows puzzling characteristics that make it unique among known supernova remnants. In particular, Pa 30 exhibits a complex morphology, with a unique radial and filamentary structure, and it hosts a hot stellar remnant at its center, which displays oxygen-dominated, ultrafast winds. Because of the surviving stellar remnant and the lack of hydrogen and helium in its filaments, it has been suggested that Pa 30 is the product of a failed thermonuclear explosion in a near- or super-Chandrasekhar white dwarf, which created a subluminous transient, a rare subtype of the Ia class of supernovae called type Iax. We present here a detailed study of the 3D structure and velocities of a full radial section of the remnant. The Integral Field Unit observations, obtained with the new red channel of the Keck Cosmic Web Imager spectrograph, reveal that the ejecta are consistent with being ballistic, with velocities close to the free-expansion velocity. Additionally, we detect a large cavity inside the supernova remnant and a sharp inner edge to the filamentary structure, which coincides with the outer edge of a bright ring detected in infrared images. Finally, we detect a strong asymmetry in the amount of ejecta along the line of sight, which might hint at an asymmetric explosion. Our analysis provides strong confirmation that the explosion originated from SN 1181."}],"citation":{"mla":"Cunningham, Tim, et al. “Expansion Properties of the Young Supernova Type Iax Remnant Pa 30 Revealed.” <i>The Astrophysical Journal Letters</i>, vol. 975, no. 1, L7, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/2041-8213/ad713b\">10.3847/2041-8213/ad713b</a>.","ama":"Cunningham T, Caiazzo I, Prusinski NZ, et al. Expansion properties of the young supernova type Iax remnant Pa 30 revealed. <i>The Astrophysical Journal Letters</i>. 2024;975(1). doi:<a href=\"https://doi.org/10.3847/2041-8213/ad713b\">10.3847/2041-8213/ad713b</a>","ista":"Cunningham T, Caiazzo I, Prusinski NZ, Fuller J, Raymond JC, Kulkarni SR, Neill JD, Duffell P, Martin C, Toloza O, Charbonneau D, Kenyon SJ, Lin Z, Matuszewski M, McGurk R, Polin A, Yao PZ. 2024. Expansion properties of the young supernova type Iax remnant Pa 30 revealed. The Astrophysical Journal Letters. 975(1), L7.","ieee":"T. Cunningham <i>et al.</i>, “Expansion properties of the young supernova type Iax remnant Pa 30 revealed,” <i>The Astrophysical Journal Letters</i>, vol. 975, no. 1. IOP Publishing, 2024.","apa":"Cunningham, T., Caiazzo, I., Prusinski, N. Z., Fuller, J., Raymond, J. C., Kulkarni, S. R., … Yao, P. Z. (2024). Expansion properties of the young supernova type Iax remnant Pa 30 revealed. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ad713b\">https://doi.org/10.3847/2041-8213/ad713b</a>","short":"T. Cunningham, I. Caiazzo, N.Z. Prusinski, J. Fuller, J.C. Raymond, S.R. Kulkarni, J.D. Neill, P. Duffell, C. Martin, O. Toloza, D. Charbonneau, S.J. Kenyon, Z. Lin, M. Matuszewski, R. McGurk, A. Polin, P.Z. Yao, The Astrophysical Journal Letters 975 (2024).","chicago":"Cunningham, Tim, Ilaria Caiazzo, Nikolaus Z. Prusinski, James Fuller, John C. Raymond, S. R. Kulkarni, James D. Neill, et al. “Expansion Properties of the Young Supernova Type Iax Remnant Pa 30 Revealed.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.3847/2041-8213/ad713b\">https://doi.org/10.3847/2041-8213/ad713b</a>."},"tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"APC_amount":"3080,76 EUR","publisher":"IOP Publishing","isi":1,"has_accepted_license":"1","das_tickbox":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"OA_place":"publisher","file_date_updated":"2024-11-20T12:24:52Z","date_published":"2024-10-24T00:00:00Z","external_id":{"isi":["001340831400001"],"arxiv":["2410.10940"]},"acknowledgement":"We thank Rob Fesen for providing the [S ii] narrowband imaging and providing helpful comments on the Letter. We also thank Eliot Quartert for the helpful discussions. T.C. was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51527.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. I.C. was also supported by NASA through grants from the Space Telescope Science Institute, under NASA contracts NASA.22K1813, NAS5-26555, and NAS5-03127. This research was supported in part by grant NSF PHY-1748958 to the Kavli Institute for Theoretical Physics (KITP). O.T. was supported by FONDECYT grant 11241186.\r\n\r\nThis publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.\r\n\r\nThis research made use of Montage. It is funded by the National Science Foundation under grant No. ACI-1440620, and was previously funded by the National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology.","year":"2024","article_number":"L7","day":"24","date_created":"2024-11-19T08:12:59Z","volume":975,"author":[{"full_name":"Cunningham, Tim","first_name":"Tim","last_name":"Cunningham"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","orcid":"0000-0002-4770-5388","first_name":"Ilaria","last_name":"Caiazzo","full_name":"Caiazzo, Ilaria"},{"first_name":"Nikolaus Z.","last_name":"Prusinski","full_name":"Prusinski, Nikolaus Z."},{"full_name":"Fuller, James","last_name":"Fuller","first_name":"James"},{"last_name":"Raymond","first_name":"John C.","full_name":"Raymond, John C."},{"last_name":"Kulkarni","first_name":"S. R.","full_name":"Kulkarni, S. R."},{"full_name":"Neill, James D.","last_name":"Neill","first_name":"James D."},{"full_name":"Duffell, Paul","first_name":"Paul","last_name":"Duffell"},{"full_name":"Martin, Chris","last_name":"Martin","first_name":"Chris"},{"full_name":"Toloza, Odette","first_name":"Odette","last_name":"Toloza"},{"last_name":"Charbonneau","first_name":"David","full_name":"Charbonneau, David"},{"last_name":"Kenyon","first_name":"Scott J.","full_name":"Kenyon, Scott J."},{"full_name":"Lin, Zeren","last_name":"Lin","first_name":"Zeren"},{"last_name":"Matuszewski","first_name":"Mateusz","full_name":"Matuszewski, Mateusz"},{"full_name":"McGurk, Rosalie","last_name":"McGurk","first_name":"Rosalie"},{"first_name":"Abigail","last_name":"Polin","full_name":"Polin, Abigail"},{"full_name":"Yao, Philippe Z.","first_name":"Philippe Z.","last_name":"Yao"}],"quality_controlled":"1","month":"10","oa":1}]