--- 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 fulldoi: https://doi.org/10.1093/mnras/staf2219 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' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold _id: '21712' abstract: - lang: eng text: Supermassive black hole binary (SMBHB) systems are expected to form as a consequence of galaxy mergers. At subparsec separations, SMBHBs can be identified as quasars with periodic variability, with previous periodicity searches uncovering significant candidates. However, these searches focused primarily on sinusoidal signals, while theoretical models and hydrodynamical simulations predict that binaries produce more complex non-sinusoidal pulse shapes. Here we examine the efficacy of the Lomb–Scargle periodogram (LSP; one of the most popular tools for periodicity searches in unevenly sampled lightcurves) to detect periodicities with a sawtooth shape mimicking results of hydrodynamical simulations. We simulate idealized well-sampled lightcurves, lightcurves that mimic the data in the Palomar Transient Factory (PTF) analyzed in M. Charisi et al. (2016), and lightcurves that resemble our expectations for single-band data in the upcoming Legacy Survey of Space and Time (LSST) of the Rubin Observatory. We approximate quasar variability with a damped random walk (DRW) model, inject sinusoidal and sawtooth pulse shapes, and assess their statistical significance. We find that in the presence of red noise, the LSP detects a relatively low fraction of the sinusoidal signals (∼45%, ∼24%, and ∼23%, in the PTF-like, idealized, and LSST-like lightcurves, respectively). The fraction is significantly reduced for sawtooth periodicity (with only ∼9% in PTF-like and ∼1% in idealized and LSST-like lightcurves). These low recovery rates imply that previous searches have missed the large majority of binaries. They also have significant implications for the detection of SMBHBs in upcoming LSST necessitating the development of advanced tools that go beyond the simple LSP. acknowledgement: M.C. acknowledges support by the European Union (ERC; MMMonsters, 101117624). This work was also supported in part by NASA grants 80NSSC24K0440 and 80NSSC22K0822. This research used the resources of the Center for Institutional Research Computing at Washington State University. article_number: '316' article_processing_charge: Yes article_type: original author: - first_name: Allison full_name: Lin, Allison last_name: Lin - first_name: Maria full_name: Charisi, Maria last_name: Charisi - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 citation: ama: Lin A, Charisi M, Haiman Z. Lomb-scargle periodogram struggles with non-sinusoidal supermassive Black Hole binary signatures in quasar lightcurves. The Astrophysical Journal. 2026;997(2). doi:10.3847/1538-4357/ae29a7 apa: Lin, A., Charisi, M., & Haiman, Z. (2026). Lomb-scargle periodogram struggles with non-sinusoidal supermassive Black Hole binary signatures in quasar lightcurves. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae29a7 chicago: Lin, Allison, Maria Charisi, and Zoltán Haiman. “Lomb-Scargle Periodogram Struggles with Non-Sinusoidal Supermassive Black Hole Binary Signatures in Quasar Lightcurves.” The Astrophysical Journal. IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae29a7. ieee: A. Lin, M. Charisi, and Z. Haiman, “Lomb-scargle periodogram struggles with non-sinusoidal supermassive Black Hole binary signatures in quasar lightcurves,” The Astrophysical Journal, vol. 997, no. 2. IOP Publishing, 2026. ista: Lin A, Charisi M, Haiman Z. 2026. Lomb-scargle periodogram struggles with non-sinusoidal supermassive Black Hole binary signatures in quasar lightcurves. The Astrophysical Journal. 997(2), 316. mla: Lin, Allison, et al. “Lomb-Scargle Periodogram Struggles with Non-Sinusoidal Supermassive Black Hole Binary Signatures in Quasar Lightcurves.” The Astrophysical Journal, vol. 997, no. 2, 316, IOP Publishing, 2026, doi:10.3847/1538-4357/ae29a7. short: A. Lin, M. Charisi, Z. Haiman, The Astrophysical Journal 997 (2026). date_created: 2026-04-12T22:01:49Z date_published: 2026-02-01T00:00:00Z date_updated: 2026-05-04T10:26:59Z day: '01' ddc: - '520' department: - _id: ZoHa doi: 10.3847/1538-4357/ae29a7 file: - access_level: open_access checksum: 5162d1539ef7d10927ef73d8b4500017 content_type: application/pdf creator: dernst date_created: 2026-05-04T10:24:49Z date_updated: 2026-05-04T10:24:49Z file_id: '21789' file_name: 2026_AstrophysicalJour_Lin.pdf file_size: 2619679 relation: main_file success: 1 file_date_updated: 2026-05-04T10:24:49Z fulldoi: https://doi.org/10.3847/1538-4357/ae29a7 has_accepted_license: '1' intvolume: ' 997' issue: '2' language: - iso: eng month: '02' 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: Lomb-scargle periodogram struggles with non-sinusoidal supermassive Black Hole binary signatures in quasar lightcurves 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: 997 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold _id: '21713' abstract: - lang: eng text: GW231123 represents the most massive binary–black hole merger detected to date, lying firmly within, or even above, the pair-instability mass gap. The component spins are both exceptionally high (a1 = 0.90 +0.10/-0.19, a2 = 0.80 +0.20/-0.51), which is difficult to explain with repeated mergers. Here we show that the black hole spin vectors are closely aligned with each other while significantly tilted relative to the binary’s orbital angular momentum, pointing to a common accretion-driven origin. We examine astrophysical formation channels capable of producing near-equal, high-mass, and mutually aligned spins consistent with GW231123—particularly binaries embedded in AGN disks and Population III remnants, which grew via coherent misaligned gas accretion. We further argue that other high-mass, high-spin events, e.g., GW190521, may share a similar evolutionary pathway. These findings underscore the critical role of sustained, coherent accretion in shaping the most extreme black hole binaries. acknowledgement: The authors thank Davide Gerosa and Matthew Mould for valuable suggestions. We are grateful for support by the National Science Foundation under grant No. PHY-2309024 (I.B.) and by NASA under grants 80NSSC22K0822 and 80NSSC24K0440 (Z.H.). We used OpenAI’s ChatGPT (OpenAI 2025) during the preparation of this manuscript. This material is based upon work supported by NSF’s LIGO Laboratory, which is a major facility fully funded by the National Science Foundation. article_number: L44 article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: Imre full_name: Bartos, Imre last_name: Bartos - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 citation: ama: 'Bartos I, Haiman Z. Accretion is all you need: Black Hole spin alignment in merger GW231123 indicates accretion pathway. The Astrophysical Journal Letters. 2026;996(2). doi:10.3847/2041-8213/ae2bff' apa: 'Bartos, I., & Haiman, Z. (2026). Accretion is all you need: Black Hole spin alignment in merger GW231123 indicates accretion pathway. The Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ae2bff' chicago: 'Bartos, Imre, and Zoltán Haiman. “Accretion Is All You Need: Black Hole Spin Alignment in Merger GW231123 Indicates Accretion Pathway.” The Astrophysical Journal Letters. IOP Publishing, 2026. https://doi.org/10.3847/2041-8213/ae2bff.' ieee: 'I. Bartos and Z. Haiman, “Accretion is all you need: Black Hole spin alignment in merger GW231123 indicates accretion pathway,” The Astrophysical Journal Letters, vol. 996, no. 2. IOP Publishing, 2026.' ista: 'Bartos I, Haiman Z. 2026. Accretion is all you need: Black Hole spin alignment in merger GW231123 indicates accretion pathway. The Astrophysical Journal Letters. 996(2), L44.' mla: 'Bartos, Imre, and Zoltán Haiman. “Accretion Is All You Need: Black Hole Spin Alignment in Merger GW231123 Indicates Accretion Pathway.” The Astrophysical Journal Letters, vol. 996, no. 2, L44, IOP Publishing, 2026, doi:10.3847/2041-8213/ae2bff.' short: I. Bartos, Z. Haiman, The Astrophysical Journal Letters 996 (2026). corr_author: '1' date_created: 2026-04-12T22:01:49Z date_published: 2026-01-10T00:00:00Z date_updated: 2026-05-04T09:54:18Z day: '10' ddc: - '520' department: - _id: ZoHa doi: 10.3847/2041-8213/ae2bff external_id: arxiv: - '2508.08558' file: - access_level: open_access checksum: ac46ba3d13f0150ccbc42665bed3ae47 content_type: application/pdf creator: dernst date_created: 2026-05-04T09:49:53Z date_updated: 2026-05-04T09:49:53Z file_id: '21788' file_name: 2026_AstrophysicalJourLetters_Bartos.pdf file_size: 866725 relation: main_file success: 1 file_date_updated: 2026-05-04T09:49:53Z fulldoi: https://doi.org/10.3847/2041-8213/ae2bff has_accepted_license: '1' intvolume: ' 996' issue: '2' language: - iso: eng month: '01' 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: 'Accretion is all you need: Black Hole spin alignment in merger GW231123 indicates accretion pathway' 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: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21844' abstract: - lang: eng text: Little red dots (LRDs) are a newly identified class of broad-line active galactic nuclei (AGNs) with a distinctive V-shaped spectrum characterized by red optical and blue UV continuum emission. Their high abundance at redshifts of z ∼ 6–8 and decline at lower redshifts suggest a transient origin. We propose that the spectral shape of LRDs originates from compact binary black hole systems, in which each black hole is surrounded by a mini-disk and embedded within a larger circumbinary disk. With a binary separation of ≲103 Schwarzschild radii, the Wien tail of a T ≃ 5000 K blackbody spectrum at the inner edge of the circumbinary disk produces the red optical emission, while the mini-disks power the UV continuum. Binary torques carve out a gap between the circumbinary disk and the mini-disks, setting the turnover wavelength of the V-shaped spectrum around the Balmer limit. This scenario naturally reproduces LRD spectra requiring only modest dust attenuation (AV ≲ 1 mag), resolving overestimated luminosities for LRDs in previous studies and alleviating a tension with the so-called Sołtan argument. This model predicts distinct spectral evolution as the binary orbit decays through binary disk interactions and gravitational-wave (GW) emission, linking early-stage “proto-LRD” binaries to the broader AGN population and late-stage “LRD descendants” to coalescing binaries detectable in GW experiments. acknowledgement: We greatly thank Kenta Hotokezaka and Hanpu Liu for constructive discussions. K.I., J.S., X.C., and L.C.H. acknowledge support from National Natural Science Foundation of China (grant Nos. 12573015, 1251101148, 12233001, and 12473037), the Beijing Natural Science Foundation (grant No. IS25003), and the China Manned Space Program (grant No. CMS-CSST-2025-A09). J.S. is also supported by “The Fundamental Research Funds for the Central Universities, Peking University” (grant No. 7100604896). Z.H. acknowledges support by US NSF grant AST-2006176 and by NASA grant Nos. 80NSSC24K0440 and 80NSSC22K0822. article_number: '25' article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: Kohei full_name: Inayoshi, Kohei last_name: Inayoshi - first_name: Jinyi full_name: Shangguan, Jinyi last_name: Shangguan - first_name: Xian full_name: Chen, Xian last_name: Chen - first_name: Luis C. full_name: Ho, Luis C. last_name: Ho - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 citation: ama: Inayoshi K, Shangguan J, Chen X, Ho LC, Haiman Z. The emergence of Little Red Dots from binary massive black holes. The Astrophysical Journal. 2026;1002(1). doi:10.3847/1538-4357/ae548d apa: Inayoshi, K., Shangguan, J., Chen, X., Ho, L. C., & Haiman, Z. (2026). The emergence of Little Red Dots from binary massive black holes. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae548d chicago: Inayoshi, Kohei, Jinyi Shangguan, Xian Chen, Luis C. Ho, and Zoltán Haiman. “The Emergence of Little Red Dots from Binary Massive Black Holes.” The Astrophysical Journal. IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae548d. ieee: K. Inayoshi, J. Shangguan, X. Chen, L. C. Ho, and Z. Haiman, “The emergence of Little Red Dots from binary massive black holes,” The Astrophysical Journal, vol. 1002, no. 1. IOP Publishing, 2026. ista: Inayoshi K, Shangguan J, Chen X, Ho LC, Haiman Z. 2026. The emergence of Little Red Dots from binary massive black holes. The Astrophysical Journal. 1002(1), 25. mla: Inayoshi, Kohei, et al. “The Emergence of Little Red Dots from Binary Massive Black Holes.” The Astrophysical Journal, vol. 1002, no. 1, 25, IOP Publishing, 2026, doi:10.3847/1538-4357/ae548d. short: K. Inayoshi, J. Shangguan, X. Chen, L.C. Ho, Z. Haiman, The Astrophysical Journal 1002 (2026). date_created: 2026-05-10T22:02:14Z date_published: 2026-05-01T00:00:00Z date_updated: 2026-05-11T07:09:12Z day: '01' ddc: - '520' department: - _id: ZoHa doi: 10.3847/1538-4357/ae548d external_id: arxiv: - '2505.05322' file: - access_level: open_access checksum: b4506dfef3dd6da335775071d8f2a0a6 content_type: application/pdf creator: dernst date_created: 2026-05-11T07:07:22Z date_updated: 2026-05-11T07:07:22Z file_id: '21853' file_name: 2026_AstrophysicalJour_Inayoshi.pdf file_size: 3041897 relation: main_file success: 1 file_date_updated: 2026-05-11T07:07:22Z fulldoi: https://doi.org/10.3847/1538-4357/ae548d has_accepted_license: '1' intvolume: ' 1002' issue: '1' 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: The emergence of Little Red Dots from binary massive 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: 1002 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21846' abstract: - lang: eng text: 'We compile a sample of 83 little red dots (LRDs) with JWST imaging and find that a substantial fraction (∼43%, rising to ≳80% for the most luminous LRDs) host one or more spatially offset, UV-bright companions at projected separations of 0.5 kpc ≲ d ≲ 5 kpc, with median 〈d〉 = 1.0 kpc. This fraction is even higher when smaller spatial scales are probed at high signal-to-noise ratio: the two most strongly lensed LRDs, A383-LRD1 and the newly discovered A68-LRD1, both have UV-bright companions at separations of only d ∼ 0.3 kpc, below the resolution limit of most unlensed JWST samples. We explore whether these ubiquitous red/blue configurations may be physically linked to the formation of LRDs, in analogy with the “synchronized pair” scenario originally proposed for direct-collapse black hole formation. In this picture, UV radiation from the companions, with typically modest stellar masses (M∗ ∼ 108−109 M⊙), suppresses molecular hydrogen cooling in nearby gas, allowing nearly isothermal collapse and the formation of extremely compact objects, such as massive black holes, supermassive stars, or quasi-stars. Using component-resolved photometry and spectral energy distribution modeling, we infer Lyman–Werner radiation fields of J21,LW ∼ 102.5–105 at the locations of the red components, comparable to those required in direct-collapse models, suggesting that the necessary photodissociation conditions are realized in many LRD systems. This framework provides a simple and self-consistent explanation for the extreme compactness and distinctive spectral properties of LRDs and links long-standing theoretical models for early compact object formation directly to a population now observed with JWST in the early Universe.' acknowledgement: 'We thank Earl Bellinger, Fabio Pacucci, Andrea Ferrara, and Dale Kocevski for useful discussions. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These imaging observations are associated with programs 1345, 1180, 1181, 1243, 6882, 2561, 1324, 4111, and 1895. The compiled dataset can be accessed at doi:10.17909/1m8f-9c47. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. J.M. and A.T. acknowledge funding by the European Union (ERC, AGENTS, 101076224). This work was performed in part at Aspen Center for Physics, which is supported by National Science Foundation grant PHY-2210452. This work used the following Python packages: Matplotlib (J. D. Hunter 2007), SciPy (P. Virtanen et al. 2020), NumPy (S. van der Walt et al. 2011), AstroPy (Astropy Collaboration et al. 2022), colossus (B. Diemer 2018), and photutils (L. Bradley et al. 2025).' article_number: L4 article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: Josephine F.W. full_name: Baggen, Josephine F.W. last_name: Baggen - first_name: Matthew T. full_name: Scoggins, Matthew T. last_name: Scoggins - first_name: Pieter full_name: Van Dokkum, Pieter last_name: Van Dokkum - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 - first_name: Alberto full_name: Torralba Torregrosa, Alberto id: 018f0249-0e87-11f0-b167-cbce08fbd541 last_name: Torralba Torregrosa orcid: 0000-0001-5586-6950 - first_name: Jorryt J full_name: Matthee, Jorryt J id: 7439a258-f3c0-11ec-9501-9df22fe06720 last_name: Matthee orcid: 0000-0003-2871-127X citation: ama: 'Baggen JFW, Scoggins MT, Van Dokkum P, Haiman Z, Torralba Torregrosa A, Matthee JJ. Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation. The Astrophysical Journal Letters. 2026;1002(1). doi:10.3847/2041-8213/ae58a5' apa: 'Baggen, J. F. W., Scoggins, M. T., Van Dokkum, P., Haiman, Z., Torralba Torregrosa, A., & Matthee, J. J. (2026). Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation. The Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ae58a5' chicago: 'Baggen, Josephine F.W., Matthew T. Scoggins, Pieter Van Dokkum, Zoltán Haiman, Alberto Torralba Torregrosa, and Jorryt J Matthee. “Connecting the Dots: UV-Bright Companions of Little Red Dots as Lyman–Werner Sources Enabling Direct-Collapse Black Hole Formation.” The Astrophysical Journal Letters. IOP Publishing, 2026. https://doi.org/10.3847/2041-8213/ae58a5.' ieee: 'J. F. W. Baggen, M. T. Scoggins, P. Van Dokkum, Z. Haiman, A. Torralba Torregrosa, and J. J. Matthee, “Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation,” The Astrophysical Journal Letters, vol. 1002, no. 1. IOP Publishing, 2026.' ista: 'Baggen JFW, Scoggins MT, Van Dokkum P, Haiman Z, Torralba Torregrosa A, Matthee JJ. 2026. Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation. The Astrophysical Journal Letters. 1002(1), L4.' mla: 'Baggen, Josephine F. W., et al. “Connecting the Dots: UV-Bright Companions of Little Red Dots as Lyman–Werner Sources Enabling Direct-Collapse Black Hole Formation.” The Astrophysical Journal Letters, vol. 1002, no. 1, L4, IOP Publishing, 2026, doi:10.3847/2041-8213/ae58a5.' short: J.F.W. Baggen, M.T. Scoggins, P. Van Dokkum, Z. Haiman, A. Torralba Torregrosa, J.J. Matthee, The Astrophysical Journal Letters 1002 (2026). date_created: 2026-05-10T22:02:15Z date_published: 2026-04-10T00:00:00Z date_updated: 2026-05-11T06:48:33Z day: '10' ddc: - '520' department: - _id: ZoHa - _id: JoMa doi: 10.3847/2041-8213/ae58a5 external_id: arxiv: - '2602.02702' file: - access_level: open_access checksum: 8c31d8603cd6ad39c772a72d136dc3f8 content_type: application/pdf creator: dernst date_created: 2026-05-11T06:44:37Z date_updated: 2026-05-11T06:44:37Z file_id: '21851' file_name: 2026_AstrophysicalJourLetters_Baggen.pdf file_size: 13359642 relation: main_file success: 1 file_date_updated: 2026-05-11T06:44:37Z fulldoi: https://doi.org/10.3847/2041-8213/ae58a5 has_accepted_license: '1' intvolume: ' 1002' issue: '1' language: - iso: eng month: '04' oa: 1 oa_version: Published Version project: - _id: bd9b2118-d553-11ed-ba76-db24564edfea grant_number: '101076224' name: Young galaxies as tracers and agents of cosmic reionization 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: 'Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation' 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: 1002 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '22362' abstract: - lang: eng text: "We present a systematic study of the environments of 25 luminous quasars at z > 6.5 from the ASPIRE program.\r\nUsing JWST/NIRCam wide-field slitless spectroscopy data, we identified 487 galaxies at 5.3 ≲ z ≲ 7.0 exhibiting\r\n[O III] emission. Among these, 122 [O III] emitters lie within |Δvlos| < 1000 km s\r\n−1 of the quasars, corresponding\r\nto a ∼9.4-fold enhancement relative to the average galaxy density at other redshifts. Furthermore, we identified 16\r\n[C II]-emitting galaxies at the quasar redshifts from Atacama Large Millimeter/submillimeter Array (ALMA) mosaic observations. A cross-correlation function analysis between quasars and [O III]+[C II] emitters yields a\r\ncross-correlation length of r 8.68 h cMpc 0\r\nQG\r\n0.55 = +0.51 1\r\nand an autocorrelation of r 15.76 h cMpc 0\r\nQQ\r\n2.70 = +2.48 1 ,\r\nindicating that z ∼ 7 quasars reside in dark matter halos with\r\nMhalo 1012.27 0.26 M 0.21\r\n= +\r\nand have a quasar lifetime of\r\ntQ 10 yr 7.05 1.01\r\n0.95\r\n= +\r\n. Notably, the number of [O III]-emitting galaxies at quasar redshifts varies significantly from\r\nfield to field, ranging from 0 to 20, highlighting a diverse quasar environment. Remarkably, seven quasars trace\r\nsignificant galaxy overdensities (i.e., protoclusters), with δgal > 5 within a volume of V ∼ 500 cMpc3\r\n. We also\r\nfind that |Δvlos| increases rapidly toward smaller galaxy–quasar separations in protocluster fields, consistent with\r\ngalaxy kinematics around extremely massive halos in cosmological simulations. By combining JWST and ALMA\r\ndata, we reveal the complex and diverse environments of these early quasars, providing robust evidence that the\r\nearliest luminous quasars are effective tracers of galaxy overdensities, albeit with substantial field-to-field\r\nvariation." acknowledgement: "F.W. acknowledges support from NSF award AST-2513040. J.B.C. acknowledges funding from the JWST Arizona/Steward Postdoc in Early galaxies and Reionization (JASPER) Scholar contract at the University of Arizona. M.H. acknowledges support from the Swiss SNSF Starting Grant (grant no. 218032). S.E.I.B. is supported by the Deutsche Forschungsgemeinschaft (DFG) under Emmy Noether grant No. BO 5771/1-1. J.-T.S. is supported by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)—project No. 518006966. A.L. acknowledges support from PRIN MUR 2022935STW. C.M. acknowledges support from Fondecyt Iniciacion grant 11240336 and the ANID BASAL project FB210003. R.A.M. acknowledges support from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. B.T. acknowledges support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 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. M.V. gratefully acknowledges financial support from the Independent Research Fund Denmark via grant Nos. DFF 8021-00130 and 3103-00146 and from the Carlsberg Foundation (grant CF23-0417).\r\n\r\nThis work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program #2078 and can be accessed via doi:10.17909/vt74-kd84. Support for program #2078 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. We acknowledge the strong support provided by the program coordinator Weston Eck and instrument reviewers Norbert Pirzkal and Stephanie La Massa." article_number: '39' article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: Feige full_name: Wang, Feige last_name: Wang - first_name: Jaclyn B. full_name: Champagne, Jaclyn B. last_name: Champagne - first_name: Jiamu full_name: Huang, Jiamu last_name: Huang - first_name: Jinyi full_name: Yang, Jinyi last_name: Yang - first_name: Joseph F. full_name: Hennawi, Joseph F. last_name: Hennawi - first_name: Xiaohui full_name: Fan, Xiaohui last_name: Fan - first_name: Haowen full_name: Zhang, Haowen last_name: Zhang - first_name: Tiago full_name: Costa, Tiago last_name: Costa - first_name: Roberto full_name: Decarli, Roberto last_name: Decarli - first_name: Melanie full_name: Habouzit, Melanie last_name: Habouzit - first_name: Fengwu full_name: Sun, Fengwu last_name: Sun - first_name: Eduardo full_name: Bañados, Eduardo last_name: Bañados - first_name: Xiangyu full_name: Jin, Xiangyu last_name: Jin - first_name: Koki full_name: Kakiichi, Koki last_name: Kakiichi - first_name: Romain A. full_name: Meyer, Romain A. last_name: Meyer - first_name: Yunjing full_name: Wu, Yunjing last_name: Wu - first_name: Silvia full_name: Belladitta, Silvia last_name: Belladitta - first_name: Laura full_name: Blecha, Laura last_name: Blecha - 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: Thomas full_name: Connor, Thomas last_name: Connor - first_name: Frederick B. full_name: Davies, Frederick B. last_name: Davies - first_name: Anna Christina full_name: Eilers, Anna Christina last_name: Eilers - 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: Mingyu full_name: Li, Mingyu last_name: Li - first_name: Zihao full_name: Li, Zihao last_name: Li - first_name: Weizhe full_name: Liu, Weizhe last_name: Liu - first_name: Alessandro full_name: Lupi, Alessandro last_name: Lupi - first_name: Jianwei full_name: Lyu, Jianwei last_name: Lyu - first_name: Chiara full_name: Mazzucchelli, Chiara last_name: Mazzucchelli - first_name: Masafusa full_name: Onoue, Masafusa last_name: Onoue - first_name: Elia full_name: Pizzati, Elia last_name: Pizzati - first_name: Maria full_name: Pudoka, Maria last_name: Pudoka - first_name: Sofía full_name: Rojas-Ruiz, Sofía last_name: Rojas-Ruiz - first_name: Jan Torge full_name: Schindler, Jan Torge last_name: Schindler - first_name: Yue full_name: Shen, Yue last_name: Shen - first_name: Wei Leong full_name: Tee, Wei Leong last_name: Tee - first_name: Benny full_name: Trakhtenbrot, Benny last_name: Trakhtenbrot - first_name: Maxime full_name: Trebitsch, Maxime last_name: Trebitsch - 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: Huanian full_name: Zhang, Huanian last_name: Zhang - first_name: Siwei full_name: Zou, Siwei last_name: Zou citation: ama: 'Wang F, Champagne JB, Huang J, et al. ASPIRE: The environments and dark matter halos of luminous quasars in the epoch of reionization. Astrophysical Journal. 2026;1006(1). doi:10.3847/1538-4357/ae7bfa' apa: 'Wang, F., Champagne, J. B., Huang, J., Yang, J., Hennawi, J. F., Fan, X., … Zou, S. (2026). ASPIRE: The environments and dark matter halos of luminous quasars in the epoch of reionization. Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae7bfa' chicago: 'Wang, Feige, Jaclyn B. Champagne, Jiamu Huang, Jinyi Yang, Joseph F. Hennawi, Xiaohui Fan, Haowen Zhang, et al. “ASPIRE: The Environments and Dark Matter Halos of Luminous Quasars in the Epoch of Reionization.” Astrophysical Journal. IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae7bfa.' ieee: 'F. Wang et al., “ASPIRE: The environments and dark matter halos of luminous quasars in the epoch of reionization,” Astrophysical Journal, vol. 1006, no. 1. IOP Publishing, 2026.' ista: 'Wang F, Champagne JB, Huang J, Yang J, Hennawi JF, Fan X, Zhang H, Costa T, Decarli R, Habouzit M, Sun F, Bañados E, Jin X, Kakiichi K, Meyer RA, Wu Y, Belladitta S, Blecha L, Bosman SEI, Cai Z, Connor T, Davies FB, Eilers AC, Haiman Z, Jun HD, Li M, Li Z, Liu W, Lupi A, Lyu J, Mazzucchelli C, Onoue M, Pizzati E, Pudoka M, Rojas-Ruiz S, Schindler JT, Shen Y, Tee WL, Trakhtenbrot B, Trebitsch M, Vestergaard M, Volonteri M, Walter F, Zhang H, Zou S. 2026. ASPIRE: The environments and dark matter halos of luminous quasars in the epoch of reionization. Astrophysical Journal. 1006(1), 39.' mla: 'Wang, Feige, et al. “ASPIRE: The Environments and Dark Matter Halos of Luminous Quasars in the Epoch of Reionization.” Astrophysical Journal, vol. 1006, no. 1, 39, IOP Publishing, 2026, doi:10.3847/1538-4357/ae7bfa.' short: F. Wang, J.B. Champagne, J. Huang, J. Yang, J.F. Hennawi, X. Fan, H. Zhang, T. Costa, R. Decarli, M. Habouzit, F. Sun, E. Bañados, X. Jin, K. Kakiichi, R.A. Meyer, Y. Wu, S. Belladitta, L. Blecha, S.E.I. Bosman, Z. Cai, T. Connor, F.B. Davies, A.C. Eilers, Z. Haiman, H.D. Jun, M. Li, Z. Li, W. Liu, A. Lupi, J. Lyu, C. Mazzucchelli, M. Onoue, E. Pizzati, M. Pudoka, S. Rojas-Ruiz, J.T. Schindler, Y. Shen, W.L. Tee, B. Trakhtenbrot, M. Trebitsch, M. Vestergaard, M. Volonteri, F. Walter, H. Zhang, S. Zou, Astrophysical Journal 1006 (2026). das_tickbox: '1' dataavailabilitystatement: "This paper makes use of the following ALMA data: ADS/JAO.ALMA#2022.1.01077.L. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\r\n\r\nFacility: JWST - James Webb Space Telescope (NIRCam).\r\n\r\nSoftware: astropy (Astropy Collaboration et al. 2018), Matplotlib (J. D. Hunter 2007), Numpy (C. R. Harris et al. 2020), Photutils (L. Bradley et al. 2022), Scipy (P. Virtanen et al. 2020), Source Extractor (E. Bertin & S. Arnouts 1996)." date_created: 2026-07-19T22:01:46Z date_published: 2026-07-20T00:00:00Z date_updated: 2026-07-20T13:31:18Z day: '20' ddc: - '520' department: - _id: ZoHa doi: 10.3847/1538-4357/ae7bfa external_id: arxiv: - '2602.04979' file: - access_level: open_access checksum: dd561fc00841217c227687e42d499ff0 content_type: application/pdf creator: dernst date_created: 2026-07-20T13:19:42Z date_updated: 2026-07-20T13:19:42Z file_id: '22377' file_name: 2026_AstrophysicalJour_Wang.pdf file_size: 6884305 relation: main_file success: 1 file_date_updated: 2026-07-20T13:19:42Z fulldoi: https://doi.org/10.3847/1538-4357/ae7bfa has_accepted_license: '1' intvolume: ' 1006' issue: '1' language: - iso: eng month: '07' oa: 1 oa_version: Published Version publication: Astrophysical Journal publication_identifier: eissn: - '15384357' issn: - 0004637X publication_status: published publisher: IOP Publishing quality_controlled: '1' researchdata_availability: no scopus_import: '1' status: public supplementarymaterial: no title: 'ASPIRE: The environments and dark matter halos of luminous quasars in the epoch of reionization' 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: 1006 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '22616' abstract: - lang: eng text: Accretion disks in active galactic nuclei (AGN) are promising sites for mergers of stellar-mass black holes (BHs) detectable via gravitational waves (GWs). These environments facilitate both in situ formation and dynamical capture of compact objects and their subsequent mergers. The uncertain origin of GW events detected by LIGO, Virgo, and KAGRA motivates searching for accompanying electromagnetic (EM) signatures. Here, we investigate postmerger EM flares associated with jets launched from merger remnants, as well as from the shocked ambient gas as the jet breaks out of the disk. We find that jet breakout produces luminous gamma-ray emission, detectable with MeV-band telescopes. Cooling emission from a shocked circum-BH minidisk, winds, and background AGN disk peaks in the UV and optical, with durations ranging from about an hour to a month, and can be identified through year-long monitoring of ∼103 AGNs with luminosities ranging from ∼1044 to ∼1045 erg s−1. With a single set of parameters, this postmerger jet model produces gamma-ray, hard X-ray, and optical flares similar to those claimed to be associated with GW events. Furthermore, by incorporating a transition from a high- to low-angular-momentum accretion state after the merger, the model avoids excessive BH growth, alleviating tensions with hyper-Eddington accretion scenarios. acknowledgement: We thank Wen-Biao Han for fruitful discussions on possible scenarios. H.T. is supported by The National Key R&D Program of China (grant No. 2024YFC2207700). S.S.K. was supported by Japan Society for the Promotion of Science (JSPS) KAKENHI grant numbers 22K14028, 21H04487, and 23H04899 and the Tohoku Initiative for Fostering Global Researchers for Interdisciplinary Sciences (TI-FRIS) of MEXT’s Strategic Professional Development Program for Young Researchers. Z.H. was supported by NASA grant 80NSSC22K0822 and NSF grant AST-2006176. article_number: '121' article_processing_charge: Yes article_type: original author: - 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: Shigeo S. full_name: Kimura, Shigeo S. last_name: Kimura - first_name: Hassen M. full_name: Yesuf, Hassen M. last_name: Yesuf - first_name: Hengxiao full_name: Guo, Hengxiao last_name: Guo citation: ama: 'Tagawa H, Haiman Z, Kimura SS, Yesuf HM, Guo H. Electromagnetic flares from compact-object mergers in active galactic nucleus disks: Signatures and predictions. The Astrophysical Journal. 2026;1006(2). doi:10.3847/1538-4357/ae7d29' apa: 'Tagawa, H., Haiman, Z., Kimura, S. S., Yesuf, H. M., & Guo, H. (2026). Electromagnetic flares from compact-object mergers in active galactic nucleus disks: Signatures and predictions. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae7d29' chicago: 'Tagawa, Hiromichi, Zoltán Haiman, Shigeo S. Kimura, Hassen M. Yesuf, and Hengxiao Guo. “Electromagnetic Flares from Compact-Object Mergers in Active Galactic Nucleus Disks: Signatures and Predictions.” The Astrophysical Journal. IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae7d29.' ieee: 'H. Tagawa, Z. Haiman, S. S. Kimura, H. M. Yesuf, and H. Guo, “Electromagnetic flares from compact-object mergers in active galactic nucleus disks: Signatures and predictions,” The Astrophysical Journal, vol. 1006, no. 2. IOP Publishing, 2026.' ista: 'Tagawa H, Haiman Z, Kimura SS, Yesuf HM, Guo H. 2026. Electromagnetic flares from compact-object mergers in active galactic nucleus disks: Signatures and predictions. The Astrophysical Journal. 1006(2), 121.' mla: 'Tagawa, Hiromichi, et al. “Electromagnetic Flares from Compact-Object Mergers in Active Galactic Nucleus Disks: Signatures and Predictions.” The Astrophysical Journal, vol. 1006, no. 2, 121, IOP Publishing, 2026, doi:10.3847/1538-4357/ae7d29.' short: H. Tagawa, Z. Haiman, S.S. Kimura, H.M. Yesuf, H. Guo, The Astrophysical Journal 1006 (2026). das_tickbox: '0' date_created: 2026-08-02T22:01:52Z date_published: 2026-08-01T00:00:00Z date_updated: 2026-08-03T08:00:54Z day: '01' ddc: - '520' department: - _id: ZoHa doi: 10.3847/1538-4357/ae7d29 file: - access_level: open_access checksum: 767660c73eb8b0a8bf39f54afe240bc6 content_type: application/pdf creator: dernst date_created: 2026-08-03T07:58:25Z date_updated: 2026-08-03T07:58:25Z file_id: '22630' file_name: 2026_AstrophysicalJournal_Tagawa.pdf file_size: 2873666 relation: main_file success: 1 file_date_updated: 2026-08-03T07:58:25Z fulldoi: https://doi.org/10.3847/1538-4357/ae7d29 has_accepted_license: '1' intvolume: ' 1006' issue: '2' language: - iso: eng month: '08' 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' researchdata_availability: no scopus_import: '1' status: public supplementarymaterial: yes title: 'Electromagnetic flares from compact-object mergers in active galactic nucleus disks: Signatures and predictions' 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: 1006 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '22676' abstract: - lang: eng text: 'We search for a population-level signature of gravitational-wave recoiling supermassive black holes: a positive correlation between dust obscuration and the magnitude of the line-of-sight velocity offset of broad emission lines relative to the host. Using the SDSS DR16 quasar catalogue, we estimate the velocity offset, $\Delta v$, as the difference between the broad H$\beta$ redshift and a noise-weighted redshift from narrow lines ([O iii] 5007, [O ii] 3728, and Ca ii 3934). We adopt the redshift-relative colour excess $\Delta (g-i)$ as a proxy for dust column density. Analysing $\sim 10^{5}$ quasars that meet basic spectral quality requirements, we find a modest but highly significant positive correlation between $|\Delta v|$ and $\Delta (g-i)$ (Spearman $r\simeq 0.12$ and Pearson $r\simeq 0.13$, with $p\ll 10^{-10}$ in both cases). The fraction of highly obscured quasars increases with $|\Delta v|$, indicating that the correlation is driven by a dust-reddened subpopulation. The result is robust to the choice of minimum $|\Delta v|$ threshold and to the line redshift estimator (peak vs. centroid). As expected, the correlation is largely absent when velocity offsets are computed between narrow emission lines. We find systematic differences between redshifted and blueshifted subsamples, which may point to residual velocity biases or additional physical effects (e.g. winds, inflows, orientation-dependent obscuration, or asymmetric broad-line regions). Recoiling massive black holes provide a natural explanation for the observed correlation, but alternative scenarios should be explored. If confirmed, this would enable population-level constraints on massive black hole merger rates, recoil dynamics, and active galactic nuclei disc properties.' acknowledgement: We thank Paul Hewett for useful discussions, and Qiaoya Wu for guidance on the data presented in Q. Wu & Y. Shen (2022). ZH acknowledges financial support from NASA grants 80NSSC24K0440 and 80NSSC22K0822. PR and ZF have received funding from the HUN-REN Hungarian Research Network and were supported by the NKFIH excellence grant TKP2021-NKTA-64. article_number: stag1367 article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: Bence full_name: Bécsy, Bence last_name: Bécsy - first_name: Peter full_name: Raffai, Peter last_name: Raffai - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman orcid: 0000-0003-3633-5403 - first_name: Andor full_name: Budai, Andor last_name: Budai - first_name: Zsolt full_name: Frei, Zsolt last_name: Frei citation: ama: Bécsy B, Raffai P, Haiman Z, Budai A, Frei Z. Statistical evidence for massive black hole recoils in active galactic nuclei. Monthly Notices of the Royal Astronomical Society. 2026;550(4). doi:10.1093/mnras/stag1367 apa: Bécsy, B., Raffai, P., Haiman, Z., Budai, A., & Frei, Z. (2026). Statistical evidence for massive black hole recoils in active galactic nuclei. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stag1367 chicago: Bécsy, Bence, Peter Raffai, Zoltán Haiman, Andor Budai, and Zsolt Frei. “Statistical Evidence for Massive Black Hole Recoils in Active Galactic Nuclei.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2026. https://doi.org/10.1093/mnras/stag1367. ieee: B. Bécsy, P. Raffai, Z. Haiman, A. Budai, and Z. Frei, “Statistical evidence for massive black hole recoils in active galactic nuclei,” Monthly Notices of the Royal Astronomical Society, vol. 550, no. 4. Oxford University Press, 2026. ista: Bécsy B, Raffai P, Haiman Z, Budai A, Frei Z. 2026. Statistical evidence for massive black hole recoils in active galactic nuclei. Monthly Notices of the Royal Astronomical Society. 550(4), stag1367. mla: Bécsy, Bence, et al. “Statistical Evidence for Massive Black Hole Recoils in Active Galactic Nuclei.” Monthly Notices of the Royal Astronomical Society, vol. 550, no. 4, stag1367, Oxford University Press, 2026, doi:10.1093/mnras/stag1367. short: B. Bécsy, P. Raffai, Z. Haiman, A. Budai, Z. Frei, Monthly Notices of the Royal Astronomical Society 550 (2026). das_tickbox: '1' dataavailabilitystatement: The data and software that support the findings of this study are openly available. The processed data sets, analysis outputs, and software are archived on Zenodo (B. Bécsy et al. 2026a), and are also available on GitHub (B. Bécsy et al. 2026b). date_created: 2026-08-11T06:19:34Z date_published: 2026-08-01T00:00:00Z date_updated: 2026-08-11T06:55:10Z day: '01' ddc: - '520' department: - _id: ZoHa doi: 10.1093/mnras/stag1367 external_id: arxiv: - '2605.04781' file: - access_level: open_access checksum: 85a01a4e163e4d2eccebe2472cdb453f content_type: application/pdf creator: dernst date_created: 2026-08-11T06:53:09Z date_updated: 2026-08-11T06:53:09Z file_id: '22681' file_name: 2026_MNRAS_Becsy.pdf file_size: 3792460 relation: main_file success: 1 file_date_updated: 2026-08-11T06:53:09Z fulldoi: https://doi.org/10.1093/mnras/stag1367 has_accepted_license: '1' intvolume: ' 550' issue: '4' language: - iso: eng month: '08' 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' researchdata_availability: yes scopus_import: '1' status: public supplementarymaterial: no title: Statistical evidence for massive black hole recoils in active galactic nuclei 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: 550 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '22713' abstract: - lang: eng text: Ground-based gravitational-wave (GW) observatories have detected approximately 200 binary black hole (BH) mergers. The astrophysical origin of these events is debated, with evidence suggesting that at least a subset originated from dynamic environments characterized by frequent close encounters. Accretion disks in active galactic nuclei (AGNs) are of particular interest, as certain observed features could be more readily produced within such environments. In this paper, we investigate the expected properties of mergers in these environments, and their dependence on various parameters, using 1D N-body simulations combined with a comprehensive semianalytical model. In our fiducial model, the distributions of masses (m1 and m2) and mass ratios (q ≡ m2/m1 ≤ 1) are similar to those observed. However, they depend strongly on the lifetime and density of the AGN disk and on the number and accretion efficiency of BHs, with higher masses predicted as these quantities increase. The most massive mergers, such as GW231123, can be produced either by efficient gas accretion or by hierarchical mergers among ≥3 generations of BHs. The observed negative correlation between q and the average effective spin (χeff), along with the positive correlation between χeff and the chirp mass (Mchirp), can be explained by a combination of efficient gas accretion, which promotes spin alignment, and hierarchical mergers, which produce high-∣χeff∣ and low-q binaries. Hierarchical mergers can also explain the negative correlation between q and the dispersion of χeff, as well as the positive correlation between ∣χeff∣and Mchirp. We present a comprehensive study on how the expected distribution of each of these quantities depends on model parameters and assumptions, which will aid the interpretation of observed GW population properties. acknowledgement: H.T. is supported by the National Science and Technology Major Project of China (No. 2024ZD1100601) and the National Key R&D Program of China (grant No.2024YFC2207700). Z.H. was supported by NASA grants 80NSSC22K0822 and 80NSSC24K0440. B.K. is supported by the Science and Technology Facilities Council grant No. ST/W000903/1. Simulations were carried out on Cray XD2000 at the Center for Computational Astrophysics, National Astronomical Observatory of Japan. article_number: '67' article_processing_charge: Yes article_type: original arxiv: 1 author: - 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: Bence full_name: Kocsis, Bence last_name: Kocsis citation: ama: Tagawa H, Haiman Z, Kocsis B. Properties of black hole mergers in disks of active galactic nuclei. The Astrophysical Journal. 2026;1007(1). doi:10.3847/1538-4357/ae8760 apa: Tagawa, H., Haiman, Z., & Kocsis, B. (2026). Properties of black hole mergers in disks of active galactic nuclei. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae8760 chicago: Tagawa, Hiromichi, Zoltán Haiman, and Bence Kocsis. “Properties of Black Hole Mergers in Disks of Active Galactic Nuclei.” The Astrophysical Journal. IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae8760. ieee: H. Tagawa, Z. Haiman, and B. Kocsis, “Properties of black hole mergers in disks of active galactic nuclei,” The Astrophysical Journal, vol. 1007, no. 1. IOP Publishing, 2026. ista: Tagawa H, Haiman Z, Kocsis B. 2026. Properties of black hole mergers in disks of active galactic nuclei. The Astrophysical Journal. 1007(1), 67. mla: Tagawa, Hiromichi, et al. “Properties of Black Hole Mergers in Disks of Active Galactic Nuclei.” The Astrophysical Journal, vol. 1007, no. 1, 67, IOP Publishing, 2026, doi:10.3847/1538-4357/ae8760. short: H. Tagawa, Z. Haiman, B. Kocsis, The Astrophysical Journal 1007 (2026). das_tickbox: '0' date_created: 2026-08-16T22:01:43Z date_published: 2026-08-10T00:00:00Z date_updated: 2026-08-18T09:05:25Z day: '10' ddc: - '520' department: - _id: ZoHa doi: 10.3847/1538-4357/ae8760 external_id: arxiv: - '2604.25994' file: - access_level: open_access checksum: 1531fd5997b054d26e99d44ccc7f8ff5 content_type: application/pdf creator: dernst date_created: 2026-08-18T09:01:50Z date_updated: 2026-08-18T09:01:50Z file_id: '22731' file_name: 2026_AstrophysicalJour_Tagawa.pdf file_size: 2246236 relation: main_file success: 1 file_date_updated: 2026-08-18T09:01:50Z fulldoi: https://doi.org/10.3847/1538-4357/ae8760 has_accepted_license: '1' intvolume: ' 1007' issue: '1' language: - iso: eng month: '08' oa: 1 oa_version: Published Version publication: The Astrophysical Journal publication_identifier: eissn: - 1538-4357 issn: - 000-4637X publication_status: published publisher: IOP Publishing quality_controlled: '1' researchdata_availability: no scopus_import: '1' status: public supplementarymaterial: no title: Properties of black hole mergers in disks of active galactic nuclei 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: 1007 year: '2026' ... --- OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '22381' abstract: - lang: eng text: "Context. X-ray binaries exhibit complex variability patterns studied in the power spectrum. These include the broadband noise (BBN)\r\ncomponents and various types of narrow components called quasi-periodic oscillations (QPOs). There is currently no consensus about\r\nwhat determines the presence or absence of the BBN or what generates the QPOs. Many believe that QPO generation is due to framedragging effects caused by Lense–Thirring torques.\r\nAims. We investigated the potential impact of frame-dragging effects on the accretion disk itself. In particular, we focused on its\r\nimpact on the observed variability and on the presence (and types) of associated QPOs.\r\nMethods. We made analytical estimates to assess the potential presence of a geometric warp in the inner accretion disk during state\r\ntransitions.\r\nResults. We show that the presence of a warp can modify the spectral-timing properties in a way that matches the observed transition\r\nbetween QPO types during outbursts. We also discuss the peculiar case of Cyg X-1, as well as how the hard-to-soft transition could\r\nbe driven by the warp itself.\r\nConclusions. The (expected) emergence of a warp provides a consistent explanation for the evolution of both the BBN and the QPO\r\nproperties during state transitions. This offers a first path toward unifying the variability of black hole X-ray binaries." acknowledgement: "GM acknowledges support from the Polish National Science Center grant 2023/48/Q/ST9/00138 and the Academy of Finland grant 355672. The authors thank the Editor for their insightful comments and effective stewardship of the review process. SGDT acknowledges support under\r\nSTFC Grant ST/X001113/1. This work made use of the python packages\r\nMatplotlib (Hunter 2007), NumPy (Harris et al. 2020), and Stingray v2.2\r\n(Huppenkothen et al. 2019; Bachetti et al. 2024b,a)." article_number: A387 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: G. full_name: Marcel, G. last_name: Marcel - first_name: S. G. D. full_name: Turner, S. G. D. last_name: Turner - first_name: B. J. full_name: Ricketts, B. J. last_name: Ricketts - first_name: V. full_name: López-Barquero, V. last_name: López-Barquero - first_name: D. J. K. full_name: Buisson, D. J. K. last_name: Buisson - first_name: F. full_name: Vincentelli, F. last_name: Vincentelli - first_name: M. full_name: Middleton, M. last_name: Middleton - first_name: C.S. full_name: Reynolds, C.S. last_name: Reynolds - first_name: Mark full_name: Avara, Mark id: 24edc561-7790-11f0-acf5-82cd0823fe7e last_name: Avara citation: ama: 'Marcel G, Turner SGD, Ricketts BJ, et al. Disk warping and black hole X-ray binaries: I. Tentative unification of low-frequency quasi-periodic oscillations. Astronomy & Astrophysics. 2026;710. doi:10.1051/0004-6361/202558103' apa: 'Marcel, G., Turner, S. G. D., Ricketts, B. J., López-Barquero, V., Buisson, D. J. K., Vincentelli, F., … Avara, M. (2026). Disk warping and black hole X-ray binaries: I. Tentative unification of low-frequency quasi-periodic oscillations. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202558103' chicago: 'Marcel, G., S. G. D. Turner, B. J. Ricketts, V. López-Barquero, D. J. K. Buisson, F. Vincentelli, M. Middleton, C.S. Reynolds, and Mark Avara. “Disk Warping and Black Hole X-Ray Binaries: I. Tentative Unification of Low-Frequency Quasi-Periodic Oscillations.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202558103.' ieee: 'G. Marcel et al., “Disk warping and black hole X-ray binaries: I. Tentative unification of low-frequency quasi-periodic oscillations,” Astronomy & Astrophysics, vol. 710. EDP Sciences, 2026.' ista: 'Marcel G, Turner SGD, Ricketts BJ, López-Barquero V, Buisson DJK, Vincentelli F, Middleton M, Reynolds CS, Avara M. 2026. Disk warping and black hole X-ray binaries: I. Tentative unification of low-frequency quasi-periodic oscillations. Astronomy & Astrophysics. 710, A387.' mla: 'Marcel, G., et al. “Disk Warping and Black Hole X-Ray Binaries: I. Tentative Unification of Low-Frequency Quasi-Periodic Oscillations.” Astronomy & Astrophysics, vol. 710, A387, EDP Sciences, 2026, doi:10.1051/0004-6361/202558103.' short: G. Marcel, S.G.D. Turner, B.J. Ricketts, V. López-Barquero, D.J.K. Buisson, F. Vincentelli, M. Middleton, C.S. Reynolds, M. Avara, Astronomy & Astrophysics 710 (2026). das_tickbox: '0' date_created: 2026-07-21T10:29:36Z date_published: 2026-06-01T00:00:00Z date_updated: 2026-09-09T08:38:49Z day: '01' ddc: - '520' department: - _id: ZoHa doi: 10.1051/0004-6361/202558103 external_id: arxiv: - '2511.10474' file: - access_level: open_access checksum: 95c1695f3c7183b2ad9d58167500b18d content_type: application/pdf creator: dernst date_created: 2026-07-21T12:20:49Z date_updated: 2026-07-21T12:20:49Z file_id: '22382' file_name: 2026_AstronomyAstrophysics_Marcel.pdf file_size: 3286905 relation: main_file success: 1 file_date_updated: 2026-07-21T12:20:49Z fulldoi: https://doi.org/10.1051/0004-6361/202558103 has_accepted_license: '1' intvolume: ' 710' language: - iso: eng month: '06' 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' researchdata_availability: no scopus_import: '1' status: public supplementarymaterial: yes title: 'Disk warping and black hole X-ray binaries: I. Tentative unification of low-frequency quasi-periodic oscillations' 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: 710 year: '2026' ... --- 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 fulldoi: https://doi.org/10.3847/2041-8213/ae279c 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 fulldoi: https://doi.org/10.1093/mnras/staf1583 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 fulldoi: https://doi.org/10.3847/1538-4357/ae0ca8 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 fulldoi: https://doi.org/10.3847/1538-4357/ae045b 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 fulldoi: https://doi.org/10.3847/1538-4357/ae1ca7 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' ... --- 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' fulldoi: https://doi.org/10.1088/1361-6382/adbda6 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 fulldoi: https://doi.org/10.3847/2041-8213/adc680 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 fulldoi: https://doi.org/10.3847/1538-4357/adc727 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' ... --- 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' fulldoi: https://doi.org/10.1038/s41550-025-02628-1 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 fulldoi: https://doi.org/10.1093/mnras/staf1269 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' ...