--- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '20974' abstract: - lang: eng text: "Thus far, Lyman-α damping wings towards quasars have been used to probe the global ionization state of the foreground intergalactic medium (IGM). A new parametrization has demonstrated that the damping wing signature also carries local information about the distribution of neutral hydrogen (H I) in front of the quasar before it started shining. Leveraging a recently introduced Bayesian JAX-based Hamiltonian Monte Carlo inference framework, we derive constraints on the Lorentzian-weighted H I column density NDW H I , the quasar’s distance rpatch to the first neutral patch, and its lifetime tQ based on James Webb Space\r\nTelescope (JWST) Near Infrared Spectrograph (NIRSpec) spectra of the two z ∼ 7.5 quasars J1007+2115 and J1342+0928. After folding in model-dependent topology information, we find that J1007+2115 (and J1342+0928) is most likely to reside in a (xH1)= 0.32+0.22 −0.20 (0.58+0.23 −0.23) neutral IGM while shining for a remarkably short lifetime of log10 tQ/yr = 4.14+0.74 −0.18 (an intermediate lifetime of 5.64+0.25 −0.43) along a sightline with log10 NDW\r\nH I /cm−2 = 19.70+0.35 −0.86 (20.24+0.25 −0.22) and rpatch = 28.9+54.0 −14.4 cMpc\r\n(10.9+5.6−5.9 cMpc). In light of the potential presence of local absorbers in the foreground of J1342+0928 as has been recently suggested, we also demonstrate how the Lorentzian-weighted column density NDW H I provides a natural means for quantifying their contribution to the observed damping wing signal." acknowledgement: 'We acknowledge helpful conversations with the ENIGMA group at UC Santa Barbara and Leiden University. This work is based on observations made with the NASA/ESA/CSA JWST. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with programmes #1219 and #1764. This work made use of numpy (C. R. Harris et al. 2020), scipy (P. Virtanen et al. 2020), jax (J. Bradbury et al. 2018), numpyro (E. Bingham et al. 2018; D. Phan, N. Pradhan & M. Jankowiak 2019), sklearn (F. Pedregosa et al. 2011), astropy (Astropy Collaboration 2013, 2018, 2022), PypeIt (J. Prochaska et al. 2020), skycalc_ipy (K. Leschinski 2021), h5py (A. Collette 2013), matplotlib (J. D. Hunter 2007), corner.py (D. Foreman-Mackey 2016), and IPython (F. Pérez & B. E. Granger 2007). TK and JFH acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 885301). JFH acknowledges support from NSF grant no. 2307180. SEIB was supported by the Deutsche Forschungsgemeinschaft (DFG) under Emmy Noether grant number BO 5771/1-1. FW acknowledges support from NSF award AST-2513040.' article_number: staf2219 article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: Timo full_name: Kist, Timo last_name: Kist - first_name: Joseph F. full_name: Hennawi, Joseph F. last_name: Hennawi - first_name: Frederick B. full_name: Davies, Frederick B. last_name: Davies - first_name: Eduardo full_name: Bañados, Eduardo last_name: Bañados - first_name: Sarah E.I. full_name: Bosman, Sarah E.I. last_name: Bosman - first_name: Zheng full_name: Cai, Zheng last_name: Cai - first_name: Anna Christina full_name: Eilers, Anna Christina last_name: Eilers - first_name: Xiaohui full_name: Fan, Xiaohui last_name: Fan - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 - first_name: Hyunsung D. full_name: Jun, Hyunsung D. last_name: Jun - first_name: Yichen full_name: Liu, Yichen last_name: Liu - first_name: Jinyi full_name: Yang, Jinyi last_name: Yang - first_name: Feige full_name: Wang, Feige last_name: Wang citation: ama: Kist T, Hennawi JF, Davies FB, et al. First constraints on the local ionization topology in front of two quasars at z ∼ 7.5. Monthly Notices of the Royal Astronomical Society. 2026;545(3). doi:10.1093/mnras/staf2219 apa: Kist, T., Hennawi, J. F., Davies, F. B., Bañados, E., Bosman, S. E. I., Cai, Z., … Wang, F. (2026). First constraints on the local ionization topology in front of two quasars at z ∼ 7.5. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf2219 chicago: Kist, Timo, Joseph F. Hennawi, Frederick B. Davies, Eduardo Bañados, Sarah E.I. Bosman, Zheng Cai, Anna Christina Eilers, et al. “First Constraints on the Local Ionization Topology in Front of Two Quasars at z ∼ 7.5.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2026. https://doi.org/10.1093/mnras/staf2219. ieee: T. Kist et al., “First constraints on the local ionization topology in front of two quasars at z ∼ 7.5,” Monthly Notices of the Royal Astronomical Society, vol. 545, no. 3. Oxford University Press, 2026. ista: Kist T, Hennawi JF, Davies FB, Bañados E, Bosman SEI, Cai Z, Eilers AC, Fan X, Haiman Z, Jun HD, Liu Y, Yang J, Wang F. 2026. First constraints on the local ionization topology in front of two quasars at z ∼ 7.5. Monthly Notices of the Royal Astronomical Society. 545(3), staf2219. mla: Kist, Timo, et al. “First Constraints on the Local Ionization Topology in Front of Two Quasars at z ∼ 7.5.” Monthly Notices of the Royal Astronomical Society, vol. 545, no. 3, staf2219, Oxford University Press, 2026, doi:10.1093/mnras/staf2219. short: T. Kist, J.F. Hennawi, F.B. Davies, E. Bañados, S.E.I. Bosman, Z. Cai, A.C. Eilers, X. Fan, Z. Haiman, H.D. Jun, Y. Liu, J. Yang, F. Wang, Monthly Notices of the Royal Astronomical Society 545 (2026). date_created: 2026-01-11T23:01:34Z date_published: 2026-01-01T00:00:00Z date_updated: 2026-01-12T09:45:54Z day: '01' ddc: - '520' department: - _id: ZoHa doi: 10.1093/mnras/staf2219 external_id: arxiv: - '2508.21818' file: - access_level: open_access checksum: 68f04ab0fdcee4f12341d116c5f794cd content_type: application/pdf creator: dernst date_created: 2026-01-12T09:43:07Z date_updated: 2026-01-12T09:43:07Z file_id: '20979' file_name: 2026_MonthNoticesRAS_Kist.pdf file_size: 2174272 relation: main_file success: 1 file_date_updated: 2026-01-12T09:43:07Z has_accepted_license: '1' intvolume: ' 545' issue: '3' language: - iso: eng month: '01' oa: 1 oa_version: Published Version publication: Monthly Notices of the Royal Astronomical Society publication_identifier: eissn: - 1365-2966 issn: - 0035-8711 publication_status: published publisher: Oxford University Press quality_controlled: '1' scopus_import: '1' status: public title: First constraints on the local ionization topology in front of two quasars at z ∼ 7.5 tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 545 year: '2026' ... --- OA_place: repository OA_type: green _id: '20193' abstract: - lang: eng text: Understanding the rapid formation of supermassive black holes in the early Universe requires insights into stellar mass growth in host galaxies. Here we present NIRSpec rest-frame optical spectra and NIRCam imaging from JWST of two galaxies at z > 6, both hosting moderate-luminosity quasars. These galaxies exhibit Balmer absorption lines, like low-redshift post-starburst galaxies. Our analyses of the medium-resolution spectra and multiband photometry show that the bulk of the stellar mass (log(M*/M☉) ≥ 10.6) formed in starburst episodes at redshift 9 and 7. One of the galaxies shows a clear Balmer break and lacks spatially resolved Hα emission. It falls well below the star-formation main sequence at z = 6, indicating quiescence. The other is transitioning to quiescence; together, these massive galaxies are among the most distant post-starburst systems known. The blueshifted wings of the quasar [O iii] emission lines indicate quasar-driven outflow, which possibly influences star formation. Direct stellar velocity dispersion measurements reveal that one galaxy follows the local black hole mass versus σ* relation whereas the other is overmassive. The existence of massive post-starburst galaxies hosting billion-solar-mass black holes in short-lived quasar phases indicates that supermassive black holes and host galaxies played a principal role in each other’s rapid early formation. acknowledgement: We thank A. C. Carnall for supporting our use of Bagpipes. We thank Y. Fu for his help on the use of QSOFitMORE. We thank J. Greene, S. Toft, T. Kakimoto and M. Tanaka for fruitful discussions. This work is based on observations made with the NASA/ESA/CSA JWST. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, under NASA contract NAS 5-03127 for JWST. These observations are associated with programmes GO 1967 and GO 3859. Support for these programmes was provided by NASA through a grant from the Space Telescope Science Institute. This work was supported by World Premier International Research Center Initiative, MEXT, Japan. This work used computing resources at Kavli IPMU. M.O., X.D., J.D.S., Y.M., T.I., K. Ito, K.K. and H.U. are supported by the Japan Society for the Promotion of Science (KAKENHI Grant Numbers JP24K22894, JP22K14071, JP18H01251, JP22H01262, JP21H04494, JP20K14531, JP23K13141, JP17H06130 and JP20H01953). M.O. and K. Inayoshi acknowledge support from the National Natural Science Foundation of China (Grant Numbers 12150410307, 12073003, 11721303, 11991052 and 11950410493). K. Inayoshi acknowledges support from the China Manned Space Project (Grant Numbers CMS-CSST-2021-A04 and CMS-CSST-2021-A06). S.E.I.B. is funded by the Deutsche Forschungsgemeinschaft (German Research Foundation) under Emmy Noether Grant Number BO 5771/1-1. Z.H., T.T. and M.S. acknowledge support from the NSF (Grant Numbers AST-2006176, AST-1907208 and AST-2006177). A.L. acknowledges funding from MUR (Grant Number PRIN 2022935STW). B.T. acknowledges support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant Agreement Number 950533) and from the Israel Science Foundation (Grant Number 1849/19). F. Walter acknowledges support from the ERC (Grant Cosmic_gas). J.-T.S. is supported by the Deutsche Forschungsgemeinschaft (Project Number 518006966). M.T. acknowledges support from the NWO (Grant Number 0.16.VIDI.189.162, ODIN). S.F. acknowledges support from NASA through the NASA Hubble Fellowship (Grant Number HST-HF2-51505.001-A awarded by the Space Telescope Science Institute). K. Iwasawa acknowledges support under Grant Number PID2022-136827NB-C44 funded by MCIN/AEI/10.13039/501100011033 /FEDER, EU. M. Vestergaard gratefully acknowledges financial support from the Independent Research Fund Denmark (Grant Numbers DFF 8021-00130 and 3103-00146). F. Wang acknowledges support from the NSF (Award Number AST-2513040). R.B. is supported by the SNSF through the Ambizione Grant PZ00P2_223532. article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Masafusa full_name: Onoue, Masafusa last_name: Onoue - first_name: Xuheng full_name: Ding, Xuheng last_name: Ding - first_name: John D. full_name: Silverman, John D. last_name: Silverman - first_name: Yoshiki full_name: Matsuoka, Yoshiki last_name: Matsuoka - first_name: Takuma full_name: Izumi, Takuma last_name: Izumi - first_name: Michael A. full_name: Strauss, Michael A. last_name: Strauss - first_name: Charlotte full_name: Ward, Charlotte last_name: Ward - first_name: Camryn L. full_name: Phillips, Camryn L. last_name: Phillips - first_name: Kei full_name: Ito, Kei last_name: Ito - first_name: Irham T. full_name: Andika, Irham T. last_name: Andika - first_name: Kentaro full_name: Aoki, Kentaro last_name: Aoki - first_name: Junya full_name: Arita, Junya last_name: Arita - first_name: Shunsuke full_name: Baba, Shunsuke last_name: Baba - first_name: Rebekka full_name: Bieri, Rebekka last_name: Bieri - first_name: Sarah E.I. full_name: Bosman, Sarah E.I. last_name: Bosman - first_name: Anna Christina full_name: Eilers, Anna Christina last_name: Eilers - first_name: Seiji full_name: Fujimoto, Seiji last_name: Fujimoto - first_name: Melanie full_name: Habouzit, Melanie last_name: Habouzit - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 - first_name: Masatoshi full_name: Imanishi, Masatoshi last_name: Imanishi - first_name: Kohei full_name: Inayoshi, Kohei last_name: Inayoshi - first_name: Kazushi full_name: Iwasawa, Kazushi last_name: Iwasawa - first_name: Knud full_name: Jahnke, Knud last_name: Jahnke - first_name: Nobunari full_name: Kashikawa, Nobunari last_name: Kashikawa - first_name: Toshihiro full_name: Kawaguchi, Toshihiro last_name: Kawaguchi - first_name: Kotaro full_name: Kohno, Kotaro last_name: Kohno - first_name: Chien Hsiu full_name: Lee, Chien Hsiu last_name: Lee - first_name: Junyao full_name: Li, Junyao last_name: Li - first_name: Alessandro full_name: Lupi, Alessandro last_name: Lupi - first_name: Jianwei full_name: Lyu, Jianwei last_name: Lyu - first_name: Tohru full_name: Nagao, Tohru last_name: Nagao - first_name: Roderik full_name: Overzier, Roderik last_name: Overzier - first_name: Jan Torge full_name: Schindler, Jan Torge last_name: Schindler - first_name: Malte full_name: Schramm, Malte last_name: Schramm - first_name: Matthew T. full_name: Scoggins, Matthew T. last_name: Scoggins - first_name: Kazuhiro full_name: Shimasaku, Kazuhiro last_name: Shimasaku - first_name: Yoshiki full_name: Toba, Yoshiki last_name: Toba - first_name: Benny full_name: Trakhtenbrot, Benny last_name: Trakhtenbrot - first_name: Maxime full_name: Trebitsch, Maxime last_name: Trebitsch - first_name: Tommaso full_name: Treu, Tommaso last_name: Treu - first_name: Hideki full_name: Umehata, Hideki last_name: Umehata - first_name: Bram full_name: Venemans, Bram last_name: Venemans - first_name: Marianne full_name: Vestergaard, Marianne last_name: Vestergaard - first_name: Marta full_name: Volonteri, Marta last_name: Volonteri - first_name: Fabian full_name: Walter, Fabian last_name: Walter - first_name: Feige full_name: Wang, Feige last_name: Wang - first_name: Jinyi full_name: Yang, Jinyi last_name: Yang - first_name: Haowen full_name: Zhang, Haowen last_name: Zhang citation: ama: Onoue M, Ding X, Silverman JD, et al. A post-starburst pathway for the formation of massive galaxies and black holes at z > 6. Nature Astronomy. 2025;9:1541-1552. doi:10.1038/s41550-025-02628-1 apa: Onoue, M., Ding, X., Silverman, J. D., Matsuoka, Y., Izumi, T., Strauss, M. A., … Zhang, H. (2025). A post-starburst pathway for the formation of massive galaxies and black holes at z > 6. Nature Astronomy. Springer Nature. https://doi.org/10.1038/s41550-025-02628-1 chicago: Onoue, Masafusa, Xuheng Ding, John D. Silverman, Yoshiki Matsuoka, Takuma Izumi, Michael A. Strauss, Charlotte Ward, et al. “A Post-Starburst Pathway for the Formation of Massive Galaxies and Black Holes at z > 6.” Nature Astronomy. Springer Nature, 2025. https://doi.org/10.1038/s41550-025-02628-1. ieee: M. Onoue et al., “A post-starburst pathway for the formation of massive galaxies and black holes at z > 6,” Nature Astronomy, vol. 9. Springer Nature, pp. 1541–1552, 2025. ista: Onoue M, Ding X, Silverman JD, Matsuoka Y, Izumi T, Strauss MA, Ward C, Phillips CL, Ito K, Andika IT, Aoki K, Arita J, Baba S, Bieri R, Bosman SEI, Eilers AC, Fujimoto S, Habouzit M, Haiman Z, Imanishi M, Inayoshi K, Iwasawa K, Jahnke K, Kashikawa N, Kawaguchi T, Kohno K, Lee CH, Li J, Lupi A, Lyu J, Nagao T, Overzier R, Schindler JT, Schramm M, Scoggins MT, Shimasaku K, Toba Y, Trakhtenbrot B, Trebitsch M, Treu T, Umehata H, Venemans B, Vestergaard M, Volonteri M, Walter F, Wang F, Yang J, Zhang H. 2025. A post-starburst pathway for the formation of massive galaxies and black holes at z > 6. Nature Astronomy. 9, 1541–1552. mla: Onoue, Masafusa, et al. “A Post-Starburst Pathway for the Formation of Massive Galaxies and Black Holes at z > 6.” Nature Astronomy, vol. 9, Springer Nature, 2025, pp. 1541–52, doi:10.1038/s41550-025-02628-1. short: M. Onoue, X. Ding, J.D. Silverman, Y. Matsuoka, T. Izumi, M.A. Strauss, C. Ward, C.L. Phillips, K. Ito, I.T. Andika, K. Aoki, J. Arita, S. Baba, R. Bieri, S.E.I. Bosman, A.C. Eilers, S. Fujimoto, M. Habouzit, Z. Haiman, M. Imanishi, K. Inayoshi, K. Iwasawa, K. Jahnke, N. Kashikawa, T. Kawaguchi, K. Kohno, C.H. Lee, J. Li, A. Lupi, J. Lyu, T. Nagao, R. Overzier, J.T. Schindler, M. Schramm, M.T. Scoggins, K. Shimasaku, Y. Toba, B. Trakhtenbrot, M. Trebitsch, T. Treu, H. Umehata, B. Venemans, M. Vestergaard, M. Volonteri, F. Walter, F. Wang, J. Yang, H. Zhang, Nature Astronomy 9 (2025) 1541–1552. date_created: 2025-08-17T22:01:38Z date_published: 2025-10-01T00:00:00Z date_updated: 2025-12-30T13:08:12Z day: '01' department: - _id: ZoHa doi: 10.1038/s41550-025-02628-1 external_id: arxiv: - '2409.07113' isi: - '001548138600001' intvolume: ' 9' isi: 1 language: - iso: eng main_file_link: - open_access: '1' url: https://arxiv.org/abs/2409.07113 month: '10' oa: 1 oa_version: Preprint page: 1541-1552 publication: Nature Astronomy publication_identifier: eissn: - 2397-3366 publication_status: published publisher: Springer Nature quality_controlled: '1' scopus_import: '1' status: public title: A post-starburst pathway for the formation of massive galaxies and black holes at z > 6 type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 9 year: '2025' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '20250' abstract: - lang: eng text: "Population III stars are possible precursors to early supermassive black holes (BHs). The presence of soft UV Lyman–Werner (LW) background radiation can suppress Population III star formation in minihaloes and allow them to form in pristine atomic-cooling haloes. In the absence of molecular hydrogen (⁠H2⁠) cooling, atomic-cooling haloes enable rapid collapse with suppressed fragmentation. High background LW fluxes from preceding star-formation have been proposed to dissociate H2⁠. This flux can be supplemented by LW radiation from one or more Population III star(s) in the same halo, reducing the necessary background level. Here, we consider atomic-cooling haloes in which multiple protostellar cores form close to one another nearly simultaneously. We assess whether the first star’s LW radiation can dissociate nearby \r\n⁠, enabling rapid accretion on to a nearby protostellar core, and the prompt formation of a second, supermassive star (SMS) from warm, atomically-cooled gas. We use a set of hydrodynamical simulations with the code enzo, with identical LW backgrounds centred on a halo with two adjacent collapsing gas clumps. When an additional large local LW flux is introduced, we observe immediate reductions in both the accretion rates and the stellar masses that form within these clumps. While the LW flux reduces the H2 fraction and increases the gas temperature, the halo core’s potential well is too shallow to promptly heat the gas to >1000 K and increase the second protostar’s accretion rate. We conclude that this internal LW feedback scenario is unlikely to facilitate SMS or massive BH seed formation." acknowledgement: We thank the anonymous referee for comments that helped us improve the clarity of this manuscript. We acknowledge support from the United States National Science Foundation (NSF) grant AST-2006176 and the National Aeronautics and Space Administration (NASA) grants 80NSSC24K0440 and 80NSSC22K0822 (ZH). We also acknowledge support from NSF grant AST-2009309, NASA Astrophysics Theory Program grant 80NSSC22K0629, and Space Telescope Science Institute grant JWST-AR-05238 (EV). The simulations in this work were run on Texas Advanced Computing Center’s Stampede2 and Stampede3 systems. We used Stampede2 and Purdue University’s computing system Anvil for data analysis. article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: James full_name: Sullivan, James last_name: Sullivan - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 - first_name: Mihir full_name: Kulkarni, Mihir last_name: Kulkarni - first_name: Eli full_name: Visbal, Eli last_name: Visbal citation: ama: Sullivan J, Haiman Z, Kulkarni M, Visbal E. Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback? Monthly Notices of the Royal Astronomical Society. 2025;542(2):822-838. doi:10.1093/mnras/staf1269 apa: Sullivan, J., Haiman, Z., Kulkarni, M., & Visbal, E. (2025). Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback? Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf1269 chicago: Sullivan, James, Zoltán Haiman, Mihir Kulkarni, and Eli Visbal. “Can Supermassive Stars Form in Protogalaxies Due to Internal Lyman-Werner Feedback?” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf1269. ieee: J. Sullivan, Z. Haiman, M. Kulkarni, and E. Visbal, “Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback?,” Monthly Notices of the Royal Astronomical Society, vol. 542, no. 2. Oxford University Press, pp. 822–838, 2025. ista: Sullivan J, Haiman Z, Kulkarni M, Visbal E. 2025. Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback? Monthly Notices of the Royal Astronomical Society. 542(2), 822–838. mla: Sullivan, James, et al. “Can Supermassive Stars Form in Protogalaxies Due to Internal Lyman-Werner Feedback?” Monthly Notices of the Royal Astronomical Society, vol. 542, no. 2, Oxford University Press, 2025, pp. 822–38, doi:10.1093/mnras/staf1269. short: J. Sullivan, Z. Haiman, M. Kulkarni, E. Visbal, Monthly Notices of the Royal Astronomical Society 542 (2025) 822–838. date_created: 2025-08-31T22:01:31Z date_published: 2025-09-01T00:00:00Z date_updated: 2025-09-30T14:28:05Z day: '01' ddc: - '520' department: - _id: ZoHa doi: 10.1093/mnras/staf1269 external_id: arxiv: - '2501.12986' isi: - '001553472000001' file: - access_level: open_access checksum: 2a06796b27da0b33d479dba170ba4b3f content_type: application/pdf creator: dernst date_created: 2025-09-03T05:44:47Z date_updated: 2025-09-03T05:44:47Z file_id: '20279' file_name: 2025_MonthlyNoticesRAS_Sullivan.pdf file_size: 2780496 relation: main_file success: 1 file_date_updated: 2025-09-03T05:44:47Z has_accepted_license: '1' intvolume: ' 542' isi: 1 issue: '2' language: - iso: eng month: '09' oa: 1 oa_version: Published Version page: 822-838 publication: Monthly Notices of the Royal Astronomical Society publication_identifier: eissn: - 1365-2966 issn: - 0035-8711 publication_status: published publisher: Oxford University Press quality_controlled: '1' scopus_import: '1' status: public title: Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback? tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 542 year: '2025' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '20493' abstract: - lang: eng text: 'We propose a formation pathway linking black holes (BHs) observed in gravitational-wave (GW) mergers, wide BH–stellar systems uncovered by Gaia, and accreting low-mass X-ray binaries (LMXBs). In this scenario, a stellar-mass BH binary undergoes isolated binary evolution and merges while hosting a distant, dynamically unimportant tertiary stellar companion. The tertiary becomes relevant only after the merger, when the remnant BH receives a GW recoil kick. Depending on the kick velocity and system configuration, the outcome can be: (1) a bright electromagnetic (EM) counterpart to the GW merger; (2) an LMXB; (3) a wide BH–stellar companion system resembling the Gaia BH population; or (4) an unbound isolated BH. Modeling the three-body dynamics, we find that ∼0.02% of LIGO–Virgo–KAGRA (LVK) mergers may be followed by an EM counterpart within ∼10 days, produced by tidal disruption of the star by the BH. The flare is likely brightest in the optical–UV and lasts for days to weeks; in some cases, partial disruption causes recurring flares with a period of ∼2 months. We further estimate that this channel can produce ∼1%–10% of Gaia BH systems in the Milky Way. This scenario provides the first physically motivated link between GW sources, Gaia BHs, and some X-ray binaries, and predicts a rare but robust pathway for EM counterparts to binary BH mergers, potentially detectable in LVK’s O5 run.' acknowledgement: We thank the anonymous referee for the useful and detailed report. S.N. acknowledges the partial support of NSF-BSF grant AST-2206428 and NASA XRP grant 80NSSC23K0262, as well as Howard and Astrid Preston for their generous support. Z.H. acknowledges support from NASA grants 80NSSC22K0822 and 80NSSC24K0440. E.Q. thanks the Gordon and Betty Moore Foundation for support through grant GBMF5076. article_number: L12 article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: Smadar full_name: Naoz, Smadar last_name: Naoz - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 - first_name: Eliot full_name: Quataert, Eliot last_name: Quataert - first_name: Liz full_name: Holzknecht, Liz last_name: Holzknecht citation: ama: Naoz S, Haiman Z, Quataert E, Holzknecht L. Triples as links between binary Black Hole mergers, their electromagnetic counterparts, and galactic Black Holes. The Astrophysical Journal Letters. 2025;992(1). doi:10.3847/2041-8213/ae0a20 apa: Naoz, S., Haiman, Z., Quataert, E., & Holzknecht, L. (2025). Triples as links between binary Black Hole mergers, their electromagnetic counterparts, and galactic Black Holes. The Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ae0a20 chicago: Naoz, Smadar, Zoltán Haiman, Eliot Quataert, and Liz Holzknecht. “Triples as Links between Binary Black Hole Mergers, Their Electromagnetic Counterparts, and Galactic Black Holes.” The Astrophysical Journal Letters. IOP Publishing, 2025. https://doi.org/10.3847/2041-8213/ae0a20. ieee: S. Naoz, Z. Haiman, E. Quataert, and L. Holzknecht, “Triples as links between binary Black Hole mergers, their electromagnetic counterparts, and galactic Black Holes,” The Astrophysical Journal Letters, vol. 992, no. 1. IOP Publishing, 2025. ista: Naoz S, Haiman Z, Quataert E, Holzknecht L. 2025. Triples as links between binary Black Hole mergers, their electromagnetic counterparts, and galactic Black Holes. The Astrophysical Journal Letters. 992(1), L12. mla: Naoz, Smadar, et al. “Triples as Links between Binary Black Hole Mergers, Their Electromagnetic Counterparts, and Galactic Black Holes.” The Astrophysical Journal Letters, vol. 992, no. 1, L12, IOP Publishing, 2025, doi:10.3847/2041-8213/ae0a20. short: S. Naoz, Z. Haiman, E. Quataert, L. Holzknecht, The Astrophysical Journal Letters 992 (2025). date_created: 2025-10-19T22:01:31Z date_published: 2025-10-10T00:00:00Z date_updated: 2026-02-16T12:44:56Z day: '10' ddc: - '520' department: - _id: ZoHa doi: 10.3847/2041-8213/ae0a20 external_id: arxiv: - '2508.13270' isi: - '001589455900001' file: - access_level: open_access checksum: cb81d666f6d7638a5bcf45653d25bcb3 content_type: application/pdf creator: dernst date_created: 2025-10-23T09:09:30Z date_updated: 2025-10-23T09:09:30Z file_id: '20520' file_name: 2025_AstrophysicalJour_Naoz.pdf file_size: 8787316 relation: main_file success: 1 file_date_updated: 2025-10-23T09:09:30Z has_accepted_license: '1' intvolume: ' 992' isi: 1 issue: '1' language: - iso: eng month: '10' oa: 1 oa_version: Published Version publication: The Astrophysical Journal Letters publication_identifier: eissn: - 2041-8213 issn: - 2041-8205 publication_status: published publisher: IOP Publishing quality_controlled: '1' scopus_import: '1' status: public title: Triples as links between binary Black Hole mergers, their electromagnetic counterparts, and galactic Black Holes tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 992 year: '2025' ... --- OA_place: repository OA_type: green _id: '20651' abstract: - lang: eng text: "The origin of merging binary black holes detected through gravitational waves remains a fundamental question in astrophysics. While stellar evolution imposes an upper mass limit of ∼50⁢\U0001D440⊙ for black holes, some observed mergers—most notably GW190521—involve significantly more massive components, suggesting alternative formation channels. Here we investigate the maximum masses attainable by black hole mergers within active galactic nucleus (AGN) disks. Using a comprehensive semianalytic model incorporating 27 binary and environmental parameters, we explore the role of AGN disk conditions in shaping the upper end of the black hole mass spectrum. We find that an AGN disk lifetime is the dominant factor, with high-mass mergers (≳200⁢\U0001D440⊙) only possible if disks persist for ≳40  Myr. The joint electromagnetic observation of an AGN-assisted merger could therefore lead to a direct measurement of the age of an AGN disk." acknowledgement: The authors are thankful for Yang Yang and Yue Yu for valuable discussions and assistance with the programming process. H. T. was supported by the National Key R&D Program of China (Grant No. 2021YFC2203002). Z. H. is grateful for support from NASA under Grants No. 80NSSC22K0822 and No. 80NSSC24K0440. I. B. acknowledges support from the National Science Foundation under Grant No. PHY-2309024. article_number: '063034' article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Ling Qin full_name: Xue, Ling Qin last_name: Xue - first_name: Hiromichi full_name: Tagawa, Hiromichi last_name: Tagawa - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 - first_name: Imre full_name: Bartos, Imre last_name: Bartos citation: ama: Xue LQ, Tagawa H, Haiman Z, Bartos I. What determines the maximum mass of AGN-assisted black hole mergers? Physical Review D. 2025;112(6). doi:10.1103/5m1n-qh9v apa: Xue, L. Q., Tagawa, H., Haiman, Z., & Bartos, I. (2025). What determines the maximum mass of AGN-assisted black hole mergers? Physical Review D. American Physical Society. https://doi.org/10.1103/5m1n-qh9v chicago: Xue, Ling Qin, Hiromichi Tagawa, Zoltán Haiman, and Imre Bartos. “What Determines the Maximum Mass of AGN-Assisted Black Hole Mergers?” Physical Review D. American Physical Society, 2025. https://doi.org/10.1103/5m1n-qh9v. ieee: L. Q. Xue, H. Tagawa, Z. Haiman, and I. Bartos, “What determines the maximum mass of AGN-assisted black hole mergers?,” Physical Review D, vol. 112, no. 6. American Physical Society, 2025. ista: Xue LQ, Tagawa H, Haiman Z, Bartos I. 2025. What determines the maximum mass of AGN-assisted black hole mergers? Physical Review D. 112(6), 063034. mla: Xue, Ling Qin, et al. “What Determines the Maximum Mass of AGN-Assisted Black Hole Mergers?” Physical Review D, vol. 112, no. 6, 063034, American Physical Society, 2025, doi:10.1103/5m1n-qh9v. short: L.Q. Xue, H. Tagawa, Z. Haiman, I. Bartos, Physical Review D 112 (2025). date_created: 2025-11-16T23:01:24Z date_published: 2025-09-18T00:00:00Z date_updated: 2025-12-01T15:29:42Z day: '18' department: - _id: ZoHa doi: 10.1103/5m1n-qh9v external_id: arxiv: - '2504.19570' isi: - '001583255800010' intvolume: ' 112' isi: 1 issue: '6' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.48550/arXiv.2504.19570 month: '09' oa: 1 oa_version: Preprint publication: Physical Review D publication_identifier: eissn: - 2470-0029 issn: - 2470-0010 publication_status: published publisher: American Physical Society quality_controlled: '1' scopus_import: '1' status: public title: What determines the maximum mass of AGN-assisted black hole mergers? type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 112 year: '2025' ... --- OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '20686' abstract: - lang: eng text: Emission from two massive black holes (MBHs) bound in a close binary is expected to be modulated by different processes, such as the Doppler boost due to the orbital motion, accretion rate variability generated by the interaction with a circumbinary disc, and binary gravitational self-lensing. When the binary is compact enough, the two black holes are thought to be surrounded by a common broad-line region that reprocesses the impinging periodically varying ionising flux, creating broad emission lines with variable line shapes. Therefore, the study of broad emission line variability through multi-epoch spectroscopic campaigns is of paramount importance for the unambiguous identification of a binary. In this work, we study the response of a disc-like broad-line region to the Doppler-boosted ionising flux emitted by sub-milliparsec MBH binaries on a circular orbit and compare it with the response of a broad-line region illuminated by a single MBH with a periodically but isotropically varying intrinsic luminosity. We show that in the binary case, the time lags of the blue and red wings of the broad emission lines, arising from diametrically opposite sides of the circumbinary disc, are out of phase by half of the binary’s orbital period, as they each respond to the periodic ‘lighthouse’ modulation from the binary’s continuum emission. This asymmetric time lag represents a new binary signature that cannot be mimicked by a single MBH. acknowledgement: MD acknowledge funding from MIUR under the grant PRIN 2017-MB8AEZ, and financial support from ICSC – Centro Nazionale di Ricerca in High Performance Computing, Big Data and Quantum Computing, funded by European Union – NextGenerationEU. This study is supported by the Italian Ministry for Research and University (MUR) under Grant ‘Progetto Dipartimenti di Eccellenza 2023-2027’ (BiCoQ). FR acknowledges the support from the Next Generation EU funds within the National Recovery and Resilience Plan (PNRR), Mission 4 – Education and Research, Component 2 – From Research to Business (M4C2), Investment Line 3.1 – Strengthening and creation of Research Infrastructures, Project IR0000012 – CTA+ – Cherenkov Telescope Array Plus. DJD acknowledges support from the Danish Independent Research Fund through Sapere Aude Starting Grant No. 121587 ZH acknowledges support from NSF grant AST-2006176 and NASA grants 80NSSC22K0822 and 80NSSC24K0440. article_number: A165 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Lorenzo full_name: Bertassi, Lorenzo last_name: Bertassi - first_name: Erika full_name: Sottocorno, Erika last_name: Sottocorno - first_name: Fabio full_name: Rigamonti, Fabio last_name: Rigamonti - first_name: Daniel full_name: D’Orazio, Daniel last_name: D’Orazio - first_name: Michael full_name: Eracleous, Michael last_name: Eracleous - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 - first_name: Massimo full_name: Dotti, Massimo last_name: Dotti citation: ama: Bertassi L, Sottocorno E, Rigamonti F, et al. Testing compact massive black hole binary candidates through multi-epoch spectroscopy. Astronomy & Astrophysics. 2025;702. doi:10.1051/0004-6361/202554574 apa: Bertassi, L., Sottocorno, E., Rigamonti, F., D’Orazio, D., Eracleous, M., Haiman, Z., & Dotti, M. (2025). Testing compact massive black hole binary candidates through multi-epoch spectroscopy. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202554574 chicago: Bertassi, Lorenzo, Erika Sottocorno, Fabio Rigamonti, Daniel D’Orazio, Michael Eracleous, Zoltán Haiman, and Massimo Dotti. “Testing Compact Massive Black Hole Binary Candidates through Multi-Epoch Spectroscopy.” Astronomy & Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202554574. ieee: L. Bertassi et al., “Testing compact massive black hole binary candidates through multi-epoch spectroscopy,” Astronomy & Astrophysics, vol. 702. EDP Sciences, 2025. ista: Bertassi L, Sottocorno E, Rigamonti F, D’Orazio D, Eracleous M, Haiman Z, Dotti M. 2025. Testing compact massive black hole binary candidates through multi-epoch spectroscopy. Astronomy & Astrophysics. 702, A165. mla: Bertassi, Lorenzo, et al. “Testing Compact Massive Black Hole Binary Candidates through Multi-Epoch Spectroscopy.” Astronomy & Astrophysics, vol. 702, A165, EDP Sciences, 2025, doi:10.1051/0004-6361/202554574. short: L. Bertassi, E. Sottocorno, F. Rigamonti, D. D’Orazio, M. Eracleous, Z. Haiman, M. Dotti, Astronomy & Astrophysics 702 (2025). date_created: 2025-11-24T14:23:22Z date_published: 2025-10-20T00:00:00Z date_updated: 2025-12-01T15:31:55Z day: '20' ddc: - '520' department: - _id: ZoHa doi: 10.1051/0004-6361/202554574 external_id: arxiv: - '2504.06349' isi: - '001597841900015' file: - access_level: open_access checksum: dbaf156cb6684bf5c3f5fb76fc890d5a content_type: application/pdf creator: dernst date_created: 2025-11-25T12:56:18Z date_updated: 2025-11-25T12:56:18Z file_id: '20693' file_name: 2025_AstronomyAstrophysics_Bertassi.pdf file_size: 2035081 relation: main_file success: 1 file_date_updated: 2025-11-25T12:56:18Z has_accepted_license: '1' intvolume: ' 702' isi: 1 language: - iso: eng month: '10' oa: 1 oa_version: Published Version publication: Astronomy & Astrophysics publication_identifier: eissn: - 1432-0746 issn: - 0004-6361 publication_status: published publisher: EDP Sciences quality_controlled: '1' scopus_import: '1' status: public title: Testing compact massive black hole binary candidates through multi-epoch spectroscopy tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 702 year: '2025' ... --- OA_place: repository OA_type: green _id: '19497' abstract: - lang: eng text: The stochastic gravitational wave (GW) background recently discovered by several pulsar timing array experiments is consistent with arising from a population of coalescing super-massive black hole binaries. The amplitude of the background is somewhat higher than expected in most previous population models or from the local mass density observations. Such binaries are expected to be produced in galaxy mergers, which are also thought to trigger bright quasar activity. Under the assumptions that (i) a fraction fbin∼1 of all quasars are associated with mergers, (ii) the typical quasar lifetime is tQ∼108 yr, and (iii) adopting Eddington ratios fEdd∼0.25 for the luminosity of quasars, we compute the GW background associated directly with the empirically measured quasar luminosity function. This approach bypasses the need to model the cosmological evolution of black holes or galaxy mergers from simulations or semi-analytical models. We find the amplitude matching the value measured by NANOGrav. Our results are consistent with most quasars being associated with black hole binaries and being the sources of the GW background, and imply a joint constraint on tQ, fEdd and the typical mass ratio q≡M2/M1. The signal in this case would be dominated by relatively distant ∼109M⊙ sources at z≈2−3, at the peak of quasar activity. Similarly to other models, our results remain in tension with the local super-massive black hole mass density. acknowledgement: We thank Chengcheng Xin and Girish Kulkarni for useful discussions. ZH gratefully acknowledges the hospitality of Eötvös University during an extended sabbatical visit, where this work began. ZH acknowledges support from NSF Grant AST-2006176 and NASA Grants 80NSSC22K0822 and 80NSSC24K0440. ZF acknowledges support from the Hungarian National Research, Development and Innovation Office (NKFIH) through the Institutional Excellence Program No. TKP2021-NKTA-64. article_number: '075007' article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Ágnes full_name: Kis-Tóth, Ágnes last_name: Kis-Tóth - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 - first_name: Zsolt full_name: Frei, Zsolt last_name: Frei citation: ama: Kis-Tóth Á, Haiman Z, Frei Z. Can quasars, triggered by mergers, account for NANOGrav’s stochastic gravitational wave background? Classical and Quantum Gravity. 2025;42(7). doi:10.1088/1361-6382/adbda6 apa: Kis-Tóth, Á., Haiman, Z., & Frei, Z. (2025). Can quasars, triggered by mergers, account for NANOGrav’s stochastic gravitational wave background? Classical and Quantum Gravity. IOP Publishing. https://doi.org/10.1088/1361-6382/adbda6 chicago: Kis-Tóth, Ágnes, Zoltán Haiman, and Zsolt Frei. “Can Quasars, Triggered by Mergers, Account for NANOGrav’s Stochastic Gravitational Wave Background?” Classical and Quantum Gravity. IOP Publishing, 2025. https://doi.org/10.1088/1361-6382/adbda6. ieee: Á. Kis-Tóth, Z. Haiman, and Z. Frei, “Can quasars, triggered by mergers, account for NANOGrav’s stochastic gravitational wave background?,” Classical and Quantum Gravity, vol. 42, no. 7. IOP Publishing, 2025. ista: Kis-Tóth Á, Haiman Z, Frei Z. 2025. Can quasars, triggered by mergers, account for NANOGrav’s stochastic gravitational wave background? Classical and Quantum Gravity. 42(7), 075007. mla: Kis-Tóth, Ágnes, et al. “Can Quasars, Triggered by Mergers, Account for NANOGrav’s Stochastic Gravitational Wave Background?” Classical and Quantum Gravity, vol. 42, no. 7, 075007, IOP Publishing, 2025, doi:10.1088/1361-6382/adbda6. short: Á. Kis-Tóth, Z. Haiman, Z. Frei, Classical and Quantum Gravity 42 (2025). date_created: 2025-04-06T22:01:32Z date_published: 2025-04-04T00:00:00Z date_updated: 2025-09-30T11:30:11Z day: '04' department: - _id: ZoHa doi: 10.1088/1361-6382/adbda6 external_id: arxiv: - '2412.12726' isi: - '001448904700001' intvolume: ' 42' isi: 1 issue: '7' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.48550/arXiv.2412.12726 month: '04' oa: 1 oa_version: Preprint publication: Classical and Quantum Gravity publication_identifier: eissn: - 1361-6382 issn: - 0264-9381 publication_status: published publisher: IOP Publishing quality_controlled: '1' scopus_import: '1' status: public title: Can quasars, triggered by mergers, account for NANOGrav’s stochastic gravitational wave background? type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 42 year: '2025' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold _id: '19638' abstract: - lang: eng text: The James Webb Space Telescope has revealed low-luminosity active galactic nuclei at redshifts of z ≳ 4–7, many of which host accreting massive black holes (BHs) with BH-to-galaxy mass (MBH/M⋆) ratios exceeding the local values by more than an order of magnitude. The origin of these overmassive BHs remains unclear but requires potential contributions from heavy seeds and/or episodes of super-Eddington accretion. We present a growth model coupled with dark matter halo assembly to explore the evolution of the MBH/M⋆ ratio under different seeding and feedback scenarios. Given the gas inflow rates in protogalaxies, BHs grow episodically at moderate super-Eddington rates, and the mass ratio increases early on, despite significant mass loss through feedback. Regardless of seeding mechanisms, the mass ratio converges to a universal value ∼0.1–0.3, set by the balance between gas feeding and star formation efficiency in the nucleus. This behavior defines an attractor in the MBH–M⋆ diagram, where overmassive BHs grow more slowly than their hosts, while undermassive seeds experience rapid growth before aligning with the attractor. We derive an analytical expression for the universal mass ratio, linking it to feedback strength and halo growth. The convergence of evolutionary tracks erases seeding information from the mass ratio by z ∼ 4–6. Detecting BHs with ∼105−6 M⊙ at higher redshifts that deviate from the convergence trend would provide key diagnostics of their birth conditions. acknowledgement: We thank the anonymous referee for a careful reading of our manuscript and for comments that helped improve this Letter. This work is supported by the Japan Society for the Promotion of Science (JSPS) KAKENHI grant No. 24KF0130. We acknowledge support from the National Natural Science Foundation of China (12073003, 12003003, 11721303, 11991052, 11950410493), and the China Manned Space Project (CMS-CSST-2021-A04 and CMS-CSST-2021-A06). L.C.H. is supported by the National Science Foundation of China (12233001), the National Key R&D Program of China (2022YFF0503401). Z.H. acknowledges support by US NSF grant AST-2006176 and by NASA grant 80NSSC22K0822. Some of the numerical calculation and analysis were performed with the Cray XC50 at the Center for Computational Astrophysics (CfCA) of the National Astronomical Observatory of Japan and with the High-performance Computing Platform of Peking University. article_number: L37 article_processing_charge: Yes article_type: letter_note arxiv: 1 author: - first_name: Haojie full_name: Hu, Haojie last_name: Hu - first_name: Kohei full_name: Inayoshi, Kohei last_name: Inayoshi - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 - first_name: Luis C. full_name: Ho, Luis C. last_name: Ho - first_name: Ken full_name: Ohsuga, Ken last_name: Ohsuga citation: ama: Hu H, Inayoshi K, Haiman Z, Ho LC, Ohsuga K. The convergence of heavy and light seeds to overmassive black holes at cosmic dawn. The Astrophysical Journal Letters. 2025;983(2). doi:10.3847/2041-8213/adc680 apa: Hu, H., Inayoshi, K., Haiman, Z., Ho, L. C., & Ohsuga, K. (2025). The convergence of heavy and light seeds to overmassive black holes at cosmic dawn. The Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/adc680 chicago: Hu, Haojie, Kohei Inayoshi, Zoltán Haiman, Luis C. Ho, and Ken Ohsuga. “The Convergence of Heavy and Light Seeds to Overmassive Black Holes at Cosmic Dawn.” The Astrophysical Journal Letters. IOP Publishing, 2025. https://doi.org/10.3847/2041-8213/adc680. ieee: H. Hu, K. Inayoshi, Z. Haiman, L. C. Ho, and K. Ohsuga, “The convergence of heavy and light seeds to overmassive black holes at cosmic dawn,” The Astrophysical Journal Letters, vol. 983, no. 2. IOP Publishing, 2025. ista: Hu H, Inayoshi K, Haiman Z, Ho LC, Ohsuga K. 2025. The convergence of heavy and light seeds to overmassive black holes at cosmic dawn. The Astrophysical Journal Letters. 983(2), L37. mla: Hu, Haojie, et al. “The Convergence of Heavy and Light Seeds to Overmassive Black Holes at Cosmic Dawn.” The Astrophysical Journal Letters, vol. 983, no. 2, L37, IOP Publishing, 2025, doi:10.3847/2041-8213/adc680. short: H. Hu, K. Inayoshi, Z. Haiman, L.C. Ho, K. Ohsuga, The Astrophysical Journal Letters 983 (2025). date_created: 2025-05-04T22:02:31Z date_published: 2025-04-20T00:00:00Z date_updated: 2026-02-16T12:44:04Z day: '20' ddc: - '520' department: - _id: ZoHa doi: 10.3847/2041-8213/adc680 external_id: arxiv: - '2503.03870' isi: - '001467616800001' file: - access_level: open_access checksum: 1a4fbeeb12e9022873e86c72d230a5ec content_type: application/pdf creator: dernst date_created: 2025-05-05T11:30:34Z date_updated: 2025-05-05T11:30:34Z file_id: '19655' file_name: 2025_AstrophysicalJourLetters_Hu.pdf file_size: 3334014 relation: main_file success: 1 file_date_updated: 2025-05-05T11:30:34Z has_accepted_license: '1' intvolume: ' 983' isi: 1 issue: '2' language: - iso: eng month: '04' oa: 1 oa_version: Published Version publication: The Astrophysical Journal Letters publication_identifier: eissn: - 2041-8213 issn: - 2041-8205 publication_status: published publisher: IOP Publishing quality_controlled: '1' scopus_import: '1' status: public title: The convergence of heavy and light seeds to overmassive black holes at cosmic dawn tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 983 year: '2025' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold _id: '19699' abstract: - lang: eng text: We demonstrate that gas disks around binary systems might deliver gas to the binary components only when the circumbinary disk is relatively warm. We present new grid-based hydrodynamics simulations, performed with the binary on the grid and a locally isothermal equation of state, in which the binary is seen to functionally "stop accreting" if the orbital Mach number in the disk exceeds a threshold value of about 40. Above this threshold, the disk continues to extract angular momentum from the binary orbit, but it delivers very little mass to the black holes and instead piles up mass in a ring surrounding the binary. This ring will eventually become viscously relaxed and deliver mass to the binary at the large-scale inflow rate. However, we show that the timescale for such relaxation can far exceed the implied binary lifetime. We demonstrate that the ability of a binary–disk system to equilibrate is dependent on the efficiency at which accretion streams deposit mass onto the binary, which, in turn is highly sensitive to the thermodynamic conditions of the inner disk. If disks around massive black hole binaries do operate in such nonaccreting regimes, it suggests these systems may be dimmer than their single black hole counterparts but could exhibit dramatic rebrightening after the black holes inspiral and merge. This dimming begins in the UV/optical and could completely choke high-energy emission, such that these systems would likely be intrinsically X-ray weak with reddened continua, potentially resembling the spectra of "little red dots" recently identified in JWST observations. acknowledgement: C.T. sincerely thanks Daniel J. D'Orazio for useful and illuminating discussions. This work was supported by the European Union's Horizon 2023 research and innovation program under Marie Sklodowska-Curie grant agreement No. 101148364, by Sapere Aude Starting grant No. 121587 through the Danish Independent Research Fund, by the LISA Preparatory Science Program (LPS) through NASA grant 80NSSC24K0440, and by NASA Astrophysics Theory Program (ATP) grant 80NSSC22K0822. Computation time for this work was supported through the NYU IT High Performance Computing resources as well as the Tycho supercomputer hosted at the SCIENCE HPC center at the University of Copenhagen. article_number: '144' article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: Christopher full_name: Tiede, Christopher last_name: Tiede - first_name: Jonathan full_name: Zrake, Jonathan last_name: Zrake - first_name: Andrew full_name: Macfadyen, Andrew last_name: Macfadyen - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 citation: ama: Tiede C, Zrake J, Macfadyen A, Haiman Z. Suppressed accretion onto massive black hole binaries surrounded by thin disks. The Astrophysical Journal. 2025;984(2). doi:10.3847/1538-4357/adc727 apa: Tiede, C., Zrake, J., Macfadyen, A., & Haiman, Z. (2025). Suppressed accretion onto massive black hole binaries surrounded by thin disks. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/adc727 chicago: Tiede, Christopher, Jonathan Zrake, Andrew Macfadyen, and Zoltán Haiman. “Suppressed Accretion onto Massive Black Hole Binaries Surrounded by Thin Disks.” The Astrophysical Journal. IOP Publishing, 2025. https://doi.org/10.3847/1538-4357/adc727. ieee: C. Tiede, J. Zrake, A. Macfadyen, and Z. Haiman, “Suppressed accretion onto massive black hole binaries surrounded by thin disks,” The Astrophysical Journal, vol. 984, no. 2. IOP Publishing, 2025. ista: Tiede C, Zrake J, Macfadyen A, Haiman Z. 2025. Suppressed accretion onto massive black hole binaries surrounded by thin disks. The Astrophysical Journal. 984(2), 144. mla: Tiede, Christopher, et al. “Suppressed Accretion onto Massive Black Hole Binaries Surrounded by Thin Disks.” The Astrophysical Journal, vol. 984, no. 2, 144, IOP Publishing, 2025, doi:10.3847/1538-4357/adc727. short: C. Tiede, J. Zrake, A. Macfadyen, Z. Haiman, The Astrophysical Journal 984 (2025). date_created: 2025-05-18T22:02:49Z date_published: 2025-05-09T00:00:00Z date_updated: 2026-02-16T12:42:56Z day: '09' ddc: - '520' department: - _id: ZoHa doi: 10.3847/1538-4357/adc727 external_id: arxiv: - '2410.03830' isi: - '001483889000001' file: - access_level: open_access checksum: 0d4c57ee944599c0789f3db467c5ca2f content_type: application/pdf creator: dernst date_created: 2025-05-19T07:20:30Z date_updated: 2025-05-19T07:20:30Z file_id: '19708' file_name: 2025_AstrophysicalJour_Tiede.pdf file_size: 1058601 relation: main_file success: 1 file_date_updated: 2025-05-19T07:20:30Z has_accepted_license: '1' intvolume: ' 984' isi: 1 issue: '2' language: - iso: eng month: '05' oa: 1 oa_version: Published Version publication: The Astrophysical Journal publication_identifier: eissn: - 1538-4357 issn: - 0004-637X publication_status: published publisher: IOP Publishing quality_controlled: '1' scopus_import: '1' status: public title: Suppressed accretion onto massive black hole binaries surrounded by thin disks tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 984 year: '2025' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21121' abstract: - lang: eng text: The relation between the masses of supermassive black holes (SMBHs) and their host galaxies encodes information on their mode of growth, especially at the earliest epochs. The James Webb Space Telescope (JWST) has opened such investigations by detecting the host galaxies of active galactic nuclei (AGN) and more luminous quasars within the first billion years of the Universe (z ≳ 6). Here, we evaluate the relation between the mass of SMBHs and the total stellar mass of their host galaxies using a sample of nine quasars at 6.18 ≤ z ≤ 6.4 from the Subaru High-z Exploration of Low-luminosity Quasars survey with NIRCam and NIRSpec observations. We find that the observed location of these quasars in the SMBH–galaxy mass plane (logMBH/M 8–9; logM*/M 9.5–11) is consistent with a nonevolving intrinsic mass relation with dispersion (0.80 +0.23 -0.28 dex) higher than the local value (∼0.3–0.4 dex) of their more massive descendants. Our analysis is based on a forward model of systematics and includes a consideration of the impact of selection effects and measurement uncertainties with an assumption on the slope of the mass relation. While degeneracies between parameters persist, the best-fit solution has a reasonable AGN fraction (2.3%) of galaxies at z ∼ 6 with an actively growing UV-unobscured black hole. In particular, models with a substantially higher normalisation in MBH would require an unrealistically low intrinsic dispersion (∼0.22 dex). Consequently, our results predict a large population of AGN at lower black hole masses, as are now just starting to be discovered in focused efforts with JWST. acknowledgement: 'This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with programs GO #1967 and GO #3859. The specific observations analyzed can be accessed via DOI: 10.17909/719q-cn32. Support for these programs was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. This work was supported by World Premier International Research Center Initiative (WPI), MEXT, Japan. This work used computing resources at Kavli IPMU. J.S. is supported by JSPS KAKENHI (JP22H01262). M.O. is supported by the Japan Society for the Promotion of Science (JSPS) KAKENHI grant No. 24K22894. Y.M. was supported by the Japan Society for the Promotion of Science (JSPS) KAKENHI grant No. 21H04494. M.V. gratefully acknowledges financial support from the Independent Research Fund Denmark via grant numbers DFF 8021-00130 and 3103-00146 and from the Carlsberg Foundation via grant CF23-0417. S.E.I.B. is supported by the Deutsche Forschungsgemeinschaft (DFG) under Emmy Noether grant number BO 5771/1-1. K.I. acknowledges support from the National Natural Science Foundation of China (12073003, 11721303, 11991052). K.I. acknowledges support under the grant PID2022-136827NB-C44 provided by MCIN/AEI/10.13039/501100011033 / FEDER, UE. A.L. acknowledges support from PRIN MUR 2022— Project “2022935STW.” J.T.S. is supported by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)—project number 518006966. F.W. acknowledges support from NSF award AST-2513040. M.H. acknowledges support from the FNS under the SNSF starting grant 218032. B.T. acknowledges support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement number 950533) and from the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy—EXC 2094—390783311.' article_number: L67 article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: John David full_name: Silverman, John David last_name: Silverman - first_name: Junyao full_name: Li, Junyao last_name: Li - first_name: Xuheng full_name: Ding, Xuheng last_name: Ding - first_name: Masafusa full_name: Onoue, Masafusa last_name: Onoue - first_name: Michael A. full_name: Strauss, Michael A. last_name: Strauss - first_name: Yoshiki full_name: Matsuoka, Yoshiki last_name: Matsuoka - first_name: Takuma full_name: Izumi, Takuma last_name: Izumi - first_name: Knud full_name: Jahnke, Knud last_name: Jahnke - first_name: Tommaso full_name: Treu, Tommaso last_name: Treu - first_name: Marta full_name: Volonteri, Marta last_name: Volonteri - first_name: Camryn L. full_name: Phillips, Camryn L. last_name: Phillips - first_name: Irham T. full_name: Andika, Irham T. last_name: Andika - first_name: Kentaro full_name: Aoki, Kentaro last_name: Aoki - first_name: Junya full_name: Arita, Junya last_name: Arita - first_name: Shunsuke full_name: Baba, Shunsuke last_name: Baba - first_name: Sarah E. I. full_name: Bosman, Sarah E. I. last_name: Bosman - first_name: Anna-Christina full_name: Eilers, Anna-Christina last_name: Eilers - first_name: Xiaohui full_name: Fan, Xiaohui last_name: Fan - first_name: Seiji full_name: Fujimoto, Seiji last_name: Fujimoto - first_name: Melanie full_name: Habouzit, Melanie last_name: Habouzit - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 - first_name: Masatoshi full_name: Imanishi, Masatoshi last_name: Imanishi - first_name: Kohei full_name: Inayoshi, Kohei last_name: Inayoshi - first_name: Kazushi full_name: Iwasawa, Kazushi last_name: Iwasawa - first_name: Nobunari full_name: Kashikawa, Nobunari last_name: Kashikawa - first_name: Toshihiro full_name: Kawaguchi, Toshihiro last_name: Kawaguchi - first_name: Chien-Hsiu full_name: Lee, Chien-Hsiu last_name: Lee - first_name: Alessandro full_name: Lupi, Alessandro last_name: Lupi - first_name: Tohru full_name: Nagao, Tohru last_name: Nagao - first_name: Jan-Torge full_name: Schindler, Jan-Torge last_name: Schindler - first_name: Malte full_name: Schramm, Malte last_name: Schramm - first_name: Kazuhiro full_name: Shimasaku, Kazuhiro last_name: Shimasaku - first_name: Yoshiki full_name: Toba, Yoshiki last_name: Toba - first_name: Benny full_name: Trakhtenbrot, Benny last_name: Trakhtenbrot - first_name: Hideki full_name: Umehata, Hideki last_name: Umehata - first_name: Marianne full_name: Vestergaard, Marianne last_name: Vestergaard - first_name: Fabian full_name: Walter, Fabian last_name: Walter - first_name: Feige full_name: Wang, Feige last_name: Wang - first_name: Jinyi full_name: Yang, Jinyi last_name: Yang citation: ama: Silverman JD, Li J, Ding X, et al. SHELLQs–JWST perspective on the intrinsic mass relation between supermassive black holes and their host galaxies at z > 6. The Astrophysical Journal Letters. 2025;995(2). doi:10.3847/2041-8213/ae279c apa: Silverman, J. D., Li, J., Ding, X., Onoue, M., Strauss, M. A., Matsuoka, Y., … Yang, J. (2025). SHELLQs–JWST perspective on the intrinsic mass relation between supermassive black holes and their host galaxies at z > 6. The Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ae279c chicago: Silverman, John David, Junyao Li, Xuheng Ding, Masafusa Onoue, Michael A. Strauss, Yoshiki Matsuoka, Takuma Izumi, et al. “SHELLQs–JWST Perspective on the Intrinsic Mass Relation between Supermassive Black Holes and Their Host Galaxies at z > 6.” The Astrophysical Journal Letters. IOP Publishing, 2025. https://doi.org/10.3847/2041-8213/ae279c. ieee: J. D. Silverman et al., “SHELLQs–JWST perspective on the intrinsic mass relation between supermassive black holes and their host galaxies at z > 6,” The Astrophysical Journal Letters, vol. 995, no. 2. IOP Publishing, 2025. ista: Silverman JD, Li J, Ding X, Onoue M, Strauss MA, Matsuoka Y, Izumi T, Jahnke K, Treu T, Volonteri M, Phillips CL, Andika IT, Aoki K, Arita J, Baba S, Bosman SEI, Eilers A-C, Fan X, Fujimoto S, Habouzit M, Haiman Z, Imanishi M, Inayoshi K, Iwasawa K, Kashikawa N, Kawaguchi T, Lee C-H, Lupi A, Nagao T, Schindler J-T, Schramm M, Shimasaku K, Toba Y, Trakhtenbrot B, Umehata H, Vestergaard M, Walter F, Wang F, Yang J. 2025. SHELLQs–JWST perspective on the intrinsic mass relation between supermassive black holes and their host galaxies at z > 6. The Astrophysical Journal Letters. 995(2), L67. mla: Silverman, John David, et al. “SHELLQs–JWST Perspective on the Intrinsic Mass Relation between Supermassive Black Holes and Their Host Galaxies at z > 6.” The Astrophysical Journal Letters, vol. 995, no. 2, L67, IOP Publishing, 2025, doi:10.3847/2041-8213/ae279c. short: J.D. Silverman, J. Li, X. Ding, M. Onoue, M.A. Strauss, Y. Matsuoka, T. Izumi, K. Jahnke, T. Treu, M. Volonteri, C.L. Phillips, I.T. Andika, K. Aoki, J. Arita, S. Baba, S.E.I. Bosman, A.-C. Eilers, X. Fan, S. Fujimoto, M. Habouzit, Z. Haiman, M. Imanishi, K. Inayoshi, K. Iwasawa, N. Kashikawa, T. Kawaguchi, C.-H. Lee, A. Lupi, T. Nagao, J.-T. Schindler, M. Schramm, K. Shimasaku, Y. Toba, B. Trakhtenbrot, H. Umehata, M. Vestergaard, F. Walter, F. Wang, J. Yang, The Astrophysical Journal Letters 995 (2025). date_created: 2026-01-31T09:27:53Z date_published: 2025-12-17T00:00:00Z date_updated: 2026-02-10T07:02:39Z day: '17' ddc: - '520' department: - _id: ZoHa doi: 10.3847/2041-8213/ae279c external_id: arxiv: - '2507.23066' file: - access_level: open_access checksum: e38c0c444be9c1507eec28c62ce04cbc content_type: application/pdf creator: dernst date_created: 2026-02-10T06:56:37Z date_updated: 2026-02-10T06:56:37Z file_id: '21202' file_name: 2025_AstrophysicalJounalLetters_Silvermann.pdf file_size: 997137 relation: main_file success: 1 file_date_updated: 2026-02-10T06:56:37Z has_accepted_license: '1' intvolume: ' 995' issue: '2' language: - iso: eng month: '12' oa: 1 oa_version: Published Version publication: The Astrophysical Journal Letters publication_identifier: eissn: - 2041-8213 issn: - 2041-8205 publication_status: published publisher: IOP Publishing quality_controlled: '1' status: public title: SHELLQs–JWST perspective on the intrinsic mass relation between supermassive black holes and their host galaxies at z > 6 tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 995 year: '2025' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21122' abstract: - lang: eng text: The multimessenger combination of gravitational waves (GWs) from merging massive black hole binaries (MBHBs) and the electromagnetic (EM) counterpart from the surrounding circumbinary disc (CBD) will open avenues to new scientific pursuits. In order to realize this science, we need to correctly localize the host galaxy of the merging MBHB. Multiwavelength, time-dependent EM signatures can greatly facilitate the identification of the unique EM counterpart among many sources in LISA’s localization volume. To this end, we studied merging unequal-mass MBHBs embedded in a CBD using high-resolution 2D simulations, with a $\Gamma$-law equation of state, incorporating viscous heating, shock heating, and radiative cooling. We simulate each binary starting from before it decouples from the CBD until just after the merger. We compute EM signatures and identify distinct features before, during, and after the merger. We corroborate previous findings of a several orders of magnitude drop in the thermal X-ray luminosity near the time of merger, but with delayed timing compared to an equal-mass system. The source remains X-ray dark for hours post-merger. Our main results are a potential new signature of a sharp spike in the thermal X-ray emission just before the tell-tale steep drop occurs. This feature may further help to identify EM counterparts of LISA’s unequal MBHBs before merger without the need for extensive pre-merger monitoring. Additionally, we find a role-reversal in which the primary out-accretes the secondary during late inspiral, which may diminish signatures originating from Doppler modulation. acknowledgement: 'We acknowledge support from the Nationale Wetenschapsagenda Roadmap grant ‘Gravitational Waves Laser Interferometer Space Antenna/Einstein Telescope: Shivers from the Deep Universe: A National Infrastructure for Gravitational Wave Research’ (LMK), National Science Foundation grant AST-2006176 (ZH), and National Aeronautics and Space Administration Astrophysics Theory Program grant 80NSSC22K0822 (AM and ZH). JD was supported by National Aeronautics and Space Administration through the National Aeronautics and Space Administration Hubble Fellowship grant HST-HF2-51552.001A, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under National Aeronautics and Space Administration contract NAS5-26555. This research was supported in part by the National Science Foundation under grant no. NSF PHY-1748958. This research has made use of National Aeronautics and Space Administration’s Astrophysics Data System. Resources supporting this work were provided by the National Aeronautics and Space Administration High-End Computing (HEC) Program through the National Aeronautics and Space Administration Advanced Supercomputing (NAS) Division at Ames Research Center. Software: python (Oliphant 2007; Millman & Aivazis 2011), scipy (Jones et al. 2001), numpy (van der Walt, Colbert & Varoquaux 2011), and matplotlib (Hunter 2007).' article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: Luke Major full_name: Krauth, Luke Major last_name: Krauth - first_name: Jordy full_name: Davelaar, Jordy last_name: Davelaar - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 - first_name: John Ryan full_name: Westernacher-Schneider, John Ryan last_name: Westernacher-Schneider - first_name: Jonathan full_name: Zrake, Jonathan last_name: Zrake - first_name: Andrew full_name: MacFadyen, Andrew last_name: MacFadyen citation: ama: Krauth LM, Davelaar J, Haiman Z, Westernacher-Schneider JR, Zrake J, MacFadyen A. Thermal X-ray signatures in late-stage unequal-mass massive black hole binary mergers. Monthly Notices of the Royal Astronomical Society. 2025;543(3):2670-2685. doi:10.1093/mnras/staf1583 apa: Krauth, L. M., Davelaar, J., Haiman, Z., Westernacher-Schneider, J. R., Zrake, J., & MacFadyen, A. (2025). Thermal X-ray signatures in late-stage unequal-mass massive black hole binary mergers. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf1583 chicago: Krauth, Luke Major, Jordy Davelaar, Zoltán Haiman, John Ryan Westernacher-Schneider, Jonathan Zrake, and Andrew MacFadyen. “Thermal X-Ray Signatures in Late-Stage Unequal-Mass Massive Black Hole Binary Mergers.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf1583. ieee: L. M. Krauth, J. Davelaar, Z. Haiman, J. R. Westernacher-Schneider, J. Zrake, and A. MacFadyen, “Thermal X-ray signatures in late-stage unequal-mass massive black hole binary mergers,” Monthly Notices of the Royal Astronomical Society, vol. 543, no. 3. Oxford University Press, pp. 2670–2685, 2025. ista: Krauth LM, Davelaar J, Haiman Z, Westernacher-Schneider JR, Zrake J, MacFadyen A. 2025. Thermal X-ray signatures in late-stage unequal-mass massive black hole binary mergers. Monthly Notices of the Royal Astronomical Society. 543(3), 2670–2685. mla: Krauth, Luke Major, et al. “Thermal X-Ray Signatures in Late-Stage Unequal-Mass Massive Black Hole Binary Mergers.” Monthly Notices of the Royal Astronomical Society, vol. 543, no. 3, Oxford University Press, 2025, pp. 2670–85, doi:10.1093/mnras/staf1583. short: L.M. Krauth, J. Davelaar, Z. Haiman, J.R. Westernacher-Schneider, J. Zrake, A. MacFadyen, Monthly Notices of the Royal Astronomical Society 543 (2025) 2670–2685. date_created: 2026-01-31T09:28:28Z date_published: 2025-11-01T00:00:00Z date_updated: 2026-02-10T07:10:21Z day: '01' ddc: - '520' department: - _id: ZoHa doi: 10.1093/mnras/staf1583 external_id: arxiv: - '2503.01494' file: - access_level: open_access checksum: f9b4c6a606df9493f6eb6af5ebcca6db content_type: application/pdf creator: dernst date_created: 2026-02-10T07:07:17Z date_updated: 2026-02-10T07:07:17Z file_id: '21203' file_name: 2025_MonthlyNoticesRAS_Krauth.pdf file_size: 3689696 relation: main_file success: 1 file_date_updated: 2026-02-10T07:07:17Z has_accepted_license: '1' intvolume: ' 543' issue: '3' language: - iso: eng month: '11' oa: 1 oa_version: Published Version page: 2670-2685 publication: Monthly Notices of the Royal Astronomical Society publication_identifier: eissn: - 1365-2966 issn: - 0035-8711 publication_status: published publisher: Oxford University Press quality_controlled: '1' status: public title: Thermal X-ray signatures in late-stage unequal-mass massive black hole binary mergers tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 543 year: '2025' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21123' abstract: - lang: eng text: We present a study of the late-time interaction between supermassive black hole binaries and retrograde circumbinary disks during the period of gravitational wave-driven inspiral. While mergers in prograde disks have received extensive study, retrograde disks offer distinct dynamics that could promote mergers and produce unique observational signatures. Through 2D numerical hydrodynamical simulations, we explore the process of binary-disk decoupling, where the binary’s orbital decay rate is faster than the disk’s viscous response rate. We find the point of decoupling to be comparable in prograde and retrograde disks, suggesting that any associated electromagnetic (EM) signatures will be produced at comparable times preceding the merger. However, we find smaller central cavities for retrograde disks, likely leading to higher-frequency EM emissions and shorter postmerger rebrightening timescales compared to their prograde counterparts. Retrograde disks form intrabinary bridges, which are prone to instabilities when the viscosity is low. These instabilities manifest as quasiperiodic flares in the accretion rate, which may produce distinctive EM signatures for retrograde disks. acknowledgement: 'D.J.D., C.T., and D.O.N. acknowledge support from the Danish Independent Research Fund through Sapere Aude Starting grant No. 121587, led by D.J.D. We are grateful to the anonymous referee for the insightful comments and suggestions for improving the manuscript. This work was also supported in part by the LISA Preparatory Science Program (LPS) through NASA grant 80NSSC24K0440, by NASA Astrophysics Theory Program (ATP) grant 80NSSC22K0822, and by the European Union’s Horizon research and innovation program under Marie Sklodowska-Curie grant agreement No. 101148364. This work made use of the following software packages: Sailfish (J. Zrake & A. MacFadyen 2024), numpy (C. R. Harris et al. 2020), Python (G. Van Rossum & F. L. Drake 2009), and scipy (P. Virtanen et al. 2020; R. Gommers et al. 2024). Software citation information aggregated using The Software Citation Station (T. Wagg & F. S. Broekgaarden 2024; T. Wagg et al. 2024). The Tycho supercomputer hosted at the SCIENCE HPC center at the University of Copenhagen was used in this work.' article_number: '206' article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: David full_name: O’Neill, David last_name: O’Neill - first_name: Christopher full_name: Tiede, Christopher last_name: Tiede - first_name: Daniel J. full_name: D’Orazio, Daniel J. last_name: D’Orazio - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 - first_name: Andrew full_name: MacFadyen, Andrew last_name: MacFadyen citation: ama: O’Neill D, Tiede C, D’Orazio DJ, Haiman Z, MacFadyen A. Gravitational wave decoupling in retrograde circumbinary disks. The Astrophysical Journal. 2025;993(2). doi:10.3847/1538-4357/ae0ca8 apa: O’Neill, D., Tiede, C., D’Orazio, D. J., Haiman, Z., & MacFadyen, A. (2025). Gravitational wave decoupling in retrograde circumbinary disks. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae0ca8 chicago: O’Neill, David, Christopher Tiede, Daniel J. D’Orazio, Zoltán Haiman, and Andrew MacFadyen. “Gravitational Wave Decoupling in Retrograde Circumbinary Disks.” The Astrophysical Journal. IOP Publishing, 2025. https://doi.org/10.3847/1538-4357/ae0ca8. ieee: D. O’Neill, C. Tiede, D. J. D’Orazio, Z. Haiman, and A. MacFadyen, “Gravitational wave decoupling in retrograde circumbinary disks,” The Astrophysical Journal, vol. 993, no. 2. IOP Publishing, 2025. ista: O’Neill D, Tiede C, D’Orazio DJ, Haiman Z, MacFadyen A. 2025. Gravitational wave decoupling in retrograde circumbinary disks. The Astrophysical Journal. 993(2), 206. mla: O’Neill, David, et al. “Gravitational Wave Decoupling in Retrograde Circumbinary Disks.” The Astrophysical Journal, vol. 993, no. 2, 206, IOP Publishing, 2025, doi:10.3847/1538-4357/ae0ca8. short: D. O’Neill, C. Tiede, D.J. D’Orazio, Z. Haiman, A. MacFadyen, The Astrophysical Journal 993 (2025). date_created: 2026-01-31T09:28:50Z date_published: 2025-11-05T00:00:00Z date_updated: 2026-02-10T07:22:28Z day: '05' ddc: - '520' department: - _id: ZoHa doi: 10.3847/1538-4357/ae0ca8 external_id: arxiv: - '2501.11679' file: - access_level: open_access checksum: 65d0a3af314b5706407ad1b57a4ea89d content_type: application/pdf creator: dernst date_created: 2026-02-10T07:19:52Z date_updated: 2026-02-10T07:19:52Z file_id: '21205' file_name: 2025_AstrophysicalJournal_ONeill.pdf file_size: 8071909 relation: main_file success: 1 file_date_updated: 2026-02-10T07:19:52Z has_accepted_license: '1' intvolume: ' 993' issue: '2' language: - iso: eng month: '11' oa: 1 oa_version: Published Version publication: The Astrophysical Journal publication_identifier: eissn: - 1538-4357 issn: - 0004-637X publication_status: published publisher: IOP Publishing quality_controlled: '1' status: public title: Gravitational wave decoupling in retrograde circumbinary disks tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 993 year: '2025' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21124' abstract: - lang: eng text: The advent of the James Webb Space Telescope (JWST) has opened new horizons in the study of quasar host galaxies during the reionization epoch (z > 6). Building upon our previous initial measurements of stellar light from two quasar host galaxies at these redshifts, we now report the detection of the stellar light from the full Cycle 1 sample of 12 distant moderate-luminosity quasar (M1450 > −24 mag) host galaxies at z > 6 from the Hyper Suprime-Cam Subaru Strategic Program. Using JWST/NIRCam observations at 1.5 and 3.6 μm combined with 2D image decomposition analysis, we successfully detect the host galaxies in 11 of the 12 targets, underscoring the high detection rates achievable with moderate-luminosity quasars. Based on two-band photometry and spectral energy distribution fitting, we find that our host galaxies are massive, with log M*/M⊙ = 9.5–11.0. The effective radii range from 0.6 to 3.2 kpc, comparable to the sizes of inactive galaxies with similar masses at z ∼ 6 as measured with imaging from COSMOS-Web. Intriguingly, the two quasar hosts with post-starburst features, which reside at the high-mass end of our sample and exhibit relatively compact morphologies, have similar size and stellar mass surface densities to quiescent galaxies at z ∼ 4–5. These findings suggest that the so-called galaxy compaction scenario is already in place at the reionization epoch, in which gas inflows during starburst phases drive centrally concentrated star formation followed by rapid quenching, bridging the structural transition of massive galaxies from relatively extended star-forming disks to compact quiescent systems. acknowledgement: "We sincerely thank Xiaohui Fan and Shenli Tang for their valuable discussions and insightful suggestions.\r\n\r\nThis work is based on observations made with the NASA/ESA/CSA JWST. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with programs GO #1967, GO #3859, and GO #1727. Support for these programs was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. This work was supported by the World Premier International Research Center Initiative (WPI), MEXT, Japan. This work used computing resources at Kavli IPMU. All the JWST data used in this paper can be found in MAST: doi:10.17909/hqaf-an74.\r\n\r\nSupport for this work was provided by NASA through grant JWST-GO-01727 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. X.D. is supported by Wuhan University's Double First-Class funding. M.O. is supported by the Japan Society for the Promotion of Science (JSPS) KAKENHI grant No. G24K22894. Y.M. is supported by the Japan Society for the Promotion of Science (JSPS) KAKENHI grant No. 21H04494. S.E.I.B. is supported by the Deutsche Forschungsgemeinschaft (DFG) under Emmy Noether grant No. B.O. 5771/1-1. J.S. is supported by JSPS KAKENHI (JP22H01262) and the World Premier International Research Center Initiative (WPI), MEXT, Japan. K.I. acknowledges support from the National Natural Science Foundation of China (12073003, 11721303, 11991052). A.L. acknowledges support from PRIN MUR 2022—Project “2022935STW” J.T.S. is supported by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)—Project No. 518006966. M.V. gratefully acknowledges financial support from the Independent Research Fund Denmark via grant Nos. DFF 8021-00130 and 3103-00146. K.I. acknowledges support under grant PID2022-136827NB-C44 provided by MCIN/AEI/10.13039/501100011033/FEDER, UE. F.W. acknowledges support from NSF award AST-2513040." article_number: '91' article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: Xuheng full_name: Ding, Xuheng last_name: Ding - first_name: Masafusa full_name: Onoue, Masafusa last_name: Onoue - first_name: John D. full_name: Silverman, John D. last_name: Silverman - first_name: Yoshiki full_name: Matsuoka, Yoshiki last_name: Matsuoka - first_name: Takuma full_name: Izumi, Takuma last_name: Izumi - first_name: Michael A. full_name: Strauss, Michael A. last_name: Strauss - first_name: Lilan full_name: Yang, Lilan last_name: Yang - first_name: Knud full_name: Jahnke, Knud last_name: Jahnke - first_name: Camryn L. full_name: Phillips, Camryn L. last_name: Phillips - first_name: Tommaso full_name: Treu, Tommaso last_name: Treu - first_name: Irham T. full_name: Andika, Irham T. last_name: Andika - first_name: Kentaro full_name: Aoki, Kentaro last_name: Aoki - first_name: Junya full_name: Arita, Junya last_name: Arita - first_name: Shunsuke full_name: Baba, Shunsuke last_name: Baba - first_name: Sarah E. I. full_name: Bosman, Sarah E. I. last_name: Bosman - first_name: Anna-Christina full_name: Eilers, Anna-Christina last_name: Eilers - first_name: Seiji full_name: Fujimoto, Seiji last_name: Fujimoto - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 - first_name: Masatoshi full_name: Imanishi, Masatoshi last_name: Imanishi - first_name: Kohei full_name: Inayoshi, Kohei last_name: Inayoshi - first_name: Kazushi full_name: Iwasawa, Kazushi last_name: Iwasawa - first_name: Jeyhan full_name: Kartaltepe, Jeyhan last_name: Kartaltepe - first_name: Nobunari full_name: Kashikawa, Nobunari last_name: Kashikawa - first_name: Toshihiro full_name: Kawaguchi, Toshihiro last_name: Kawaguchi - first_name: Junyao full_name: Li, Junyao last_name: Li - first_name: Chien-Hsiu full_name: Lee, Chien-Hsiu last_name: Lee - first_name: Alessandro full_name: Lupi, Alessandro last_name: Lupi - first_name: Jan-Torge full_name: Schindler, Jan-Torge last_name: Schindler - first_name: Malte full_name: Schramm, Malte last_name: Schramm - first_name: Kazuhiro full_name: Shimasaku, Kazuhiro last_name: Shimasaku - first_name: Marko full_name: Shuntov, Marko last_name: Shuntov - first_name: Takumi S. full_name: Tanaka, Takumi S. last_name: Tanaka - first_name: Yoshiki full_name: Toba, Yoshiki last_name: Toba - first_name: Benny full_name: Trakhtenbrot, Benny last_name: Trakhtenbrot - first_name: Hideki full_name: Umehata, Hideki last_name: Umehata - first_name: Marianne full_name: Vestergaard, Marianne last_name: Vestergaard - first_name: Feige full_name: Wang, Feige last_name: Wang - first_name: Jinyi full_name: Yang, Jinyi last_name: Yang citation: ama: Ding X, Onoue M, Silverman JD, et al. SHELLQs-JWST unveils the host galaxies of 12 quasars at z > 6. The Astrophysical Journal. 2025;993(1). doi:10.3847/1538-4357/ae045b apa: Ding, X., Onoue, M., Silverman, J. D., Matsuoka, Y., Izumi, T., Strauss, M. A., … Yang, J. (2025). SHELLQs-JWST unveils the host galaxies of 12 quasars at z > 6. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae045b chicago: Ding, Xuheng, Masafusa Onoue, John D. Silverman, Yoshiki Matsuoka, Takuma Izumi, Michael A. Strauss, Lilan Yang, et al. “SHELLQs-JWST Unveils the Host Galaxies of 12 Quasars at z > 6.” The Astrophysical Journal. IOP Publishing, 2025. https://doi.org/10.3847/1538-4357/ae045b. ieee: X. Ding et al., “SHELLQs-JWST unveils the host galaxies of 12 quasars at z > 6,” The Astrophysical Journal, vol. 993, no. 1. IOP Publishing, 2025. ista: Ding X, Onoue M, Silverman JD, Matsuoka Y, Izumi T, Strauss MA, Yang L, Jahnke K, Phillips CL, Treu T, Andika IT, Aoki K, Arita J, Baba S, Bosman SEI, Eilers A-C, Fujimoto S, Haiman Z, Imanishi M, Inayoshi K, Iwasawa K, Kartaltepe J, Kashikawa N, Kawaguchi T, Li J, Lee C-H, Lupi A, Schindler J-T, Schramm M, Shimasaku K, Shuntov M, Tanaka TS, Toba Y, Trakhtenbrot B, Umehata H, Vestergaard M, Wang F, Yang J. 2025. SHELLQs-JWST unveils the host galaxies of 12 quasars at z > 6. The Astrophysical Journal. 993(1), 91. mla: Ding, Xuheng, et al. “SHELLQs-JWST Unveils the Host Galaxies of 12 Quasars at z > 6.” The Astrophysical Journal, vol. 993, no. 1, 91, IOP Publishing, 2025, doi:10.3847/1538-4357/ae045b. short: X. Ding, M. Onoue, J.D. Silverman, Y. Matsuoka, T. Izumi, M.A. Strauss, L. Yang, K. Jahnke, C.L. Phillips, T. Treu, I.T. Andika, K. Aoki, J. Arita, S. Baba, S.E.I. Bosman, A.-C. Eilers, S. Fujimoto, Z. Haiman, M. Imanishi, K. Inayoshi, K. Iwasawa, J. Kartaltepe, N. Kashikawa, T. Kawaguchi, J. Li, C.-H. Lee, A. Lupi, J.-T. Schindler, M. Schramm, K. Shimasaku, M. Shuntov, T.S. Tanaka, Y. Toba, B. Trakhtenbrot, H. Umehata, M. Vestergaard, F. Wang, J. Yang, The Astrophysical Journal 993 (2025). date_created: 2026-01-31T09:29:11Z date_published: 2025-10-28T00:00:00Z date_updated: 2026-02-10T07:44:42Z day: '28' ddc: - '520' department: - _id: ZoHa doi: 10.3847/1538-4357/ae045b external_id: arxiv: - '2505.03876' file: - access_level: open_access checksum: 36decd55832a270ce62086c1a279a254 content_type: application/pdf creator: dernst date_created: 2026-02-10T07:42:21Z date_updated: 2026-02-10T07:42:21Z file_id: '21206' file_name: 2025_AstrophysicalJournal_Ding.pdf file_size: 10064937 relation: main_file success: 1 file_date_updated: 2026-02-10T07:42:21Z has_accepted_license: '1' intvolume: ' 993' issue: '1' language: - iso: eng month: '10' oa: 1 oa_version: Published Version publication: The Astrophysical Journal publication_identifier: eissn: - 1538-4357 issn: - 0004-637X publication_status: published publisher: IOP Publishing quality_controlled: '1' status: public title: SHELLQs-JWST unveils the host galaxies of 12 quasars at z > 6 tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 993 year: '2025' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21724' abstract: - lang: eng text: 'The next generation of weak-gravitational-lensing surveys has the potential to place stringent constraints on cosmological parameters. However, their analysis is limited by systematics such as the intrinsic alignments of galaxies, which alter weak-lensing convergence and can lead to biases in cosmological parameter estimations. For the first time, in this work, we investigate the impact of intrinsic alignments on non-Gaussian statistics of the weak-lensing field using galaxy shapes derived from the IllustrisTNG hydrodynamical simulation. We create two catalogs of ray-traced convergence maps: one that includes the measured intrinsic shape of each galaxy and another where all galaxies are randomly rotated to eliminate intrinsic alignments. We compare a range of weak-lensing statistics between the two catalogs, including the shear–shear correlation function, the map-level angular power spectrum, one-point, peak count, and minimum distribution functions, and Minkowski functionals. For each statistic, we assess the level of statistical distinguishability between catalogs for a set of future survey angular areas. Our results reveal strong small-scale correlation in the alignment of galaxies and statistically significant boosts in weak-lensing convergence in both positive and negative directions for high-significance peaks and minima, respectively. We note that our analysis is at a fixed number density of ˜ 5 arcmin^-2, drawn from a single realization of initial conditions, and does not include observational uncertainties or supersample covariance contributions. Weak-lensing analyses utilizing non-Gaussian statistics must account for intrinsic alignments to avoid significantly compromised cosmological inferences.' acknowledgement: We thank Fulvio Ferlito, Ana Maria Delgado, and Ken Osato for helpful conversations during this work. M.E.L. is supported by NSF grant DGE-2036197. Z.H. acknowledges financial support from NASA ATP grant 80NSSC24K1093. The Flatiron Institute is supported by the Simons Foundation. article_number: '36' article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: Max E. full_name: Lee, Max E. last_name: Lee - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 - first_name: Shivam full_name: Pandey, Shivam last_name: Pandey - first_name: Shy full_name: Genel, Shy last_name: Genel citation: ama: Lee ME, Haiman Z, Pandey S, Genel S. The effect of intrinsic alignments on weak-lensing statistics in hydrodynamical simulations. The Astrophysical Journal. 2025;996(1). doi:10.3847/1538-4357/ae1ca7 apa: Lee, M. E., Haiman, Z., Pandey, S., & Genel, S. (2025). The effect of intrinsic alignments on weak-lensing statistics in hydrodynamical simulations. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae1ca7 chicago: Lee, Max E., Zoltán Haiman, Shivam Pandey, and Shy Genel. “The Effect of Intrinsic Alignments on Weak-Lensing Statistics in Hydrodynamical Simulations.” The Astrophysical Journal. IOP Publishing, 2025. https://doi.org/10.3847/1538-4357/ae1ca7. ieee: M. E. Lee, Z. Haiman, S. Pandey, and S. Genel, “The effect of intrinsic alignments on weak-lensing statistics in hydrodynamical simulations,” The Astrophysical Journal, vol. 996, no. 1. IOP Publishing, 2025. ista: Lee ME, Haiman Z, Pandey S, Genel S. 2025. The effect of intrinsic alignments on weak-lensing statistics in hydrodynamical simulations. The Astrophysical Journal. 996(1), 36. mla: Lee, Max E., et al. “The Effect of Intrinsic Alignments on Weak-Lensing Statistics in Hydrodynamical Simulations.” The Astrophysical Journal, vol. 996, no. 1, 36, IOP Publishing, 2025, doi:10.3847/1538-4357/ae1ca7. short: M.E. Lee, Z. Haiman, S. Pandey, S. Genel, The Astrophysical Journal 996 (2025). date_created: 2026-04-12T22:01:52Z date_published: 2025-12-23T00:00:00Z date_updated: 2026-04-13T08:30:52Z day: '23' ddc: - '520' department: - _id: ZoHa doi: 10.3847/1538-4357/ae1ca7 external_id: arxiv: - '2504.12460' file: - access_level: open_access checksum: 0d8fa05617420230eac39944b36839e9 content_type: application/pdf creator: dernst date_created: 2026-04-13T08:20:16Z date_updated: 2026-04-13T08:20:16Z file_id: '21732' file_name: 2025_AstrophysicalJournal_Lee.pdf file_size: 4122087 relation: main_file success: 1 file_date_updated: 2026-04-13T08:20:16Z has_accepted_license: '1' intvolume: ' 996' issue: '1' language: - iso: eng month: '12' oa: 1 oa_version: Published Version publication: The Astrophysical Journal publication_identifier: eissn: - 1538-4357 issn: - 0004-637X publication_status: published publisher: IOP Publishing quality_controlled: '1' scopus_import: '1' status: public title: The effect of intrinsic alignments on weak-lensing statistics in hydrodynamical simulations tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 996 year: '2025' ...