Current date: 2026-07-10
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Datestamp limit: 2026-07-10 (0 days ago)
Created/updated limit: 2026-07-03 (7 days ago)
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Scoring abstracts
Number of records retrieved: 744
Keyword score statistics
score 11 -- 1 abstracts
score 8 -- 1 abstracts
score 6 -- 4 abstracts
score 5 -- 3 abstracts
score 4 -- 5 abstracts
score 3 -- 10 abstracts
score 2 -- 18 abstracts
in total -- 42 abstracts
Articles that appeared on 2026-07-10
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[abstract 1 / 42] Wow! (score: 11)
- Title: Broad-band Spectral Modeling of Large-Scale X-ray Jets in High-Redshift Quasars: An MHD-Informed ApproachAuthors: Patryk Liniewicz, Łukasz Stawarz, C. C. Cheung, Giulia Migliori, Aneta Siemiginowska,Comments: Accepted for publication in ApJSubjects: astro-ph.HECreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
We present a systematic spectral analysis of kiloparsec-scale JETs in high-redshift QUASARs, modeling their radio-to-X-ray emission as SYNCHROTRON radiation and inverse-COMPTONization of CMB by RELATIVISTIC electrons. In contrast to the homogeneous one-zone approximation commonly adopted in the literature, we describe the JET as a current-carrying, axially symmetric outflow with a purely toroidal MAGNETic field in MAGNETohydrostatic equilibrium and with radial velocity shear. In this framework, the pressure, MAGNETic-field, and bulk-velocity profiles are linked self-consistently, capturing the radial stratification of the emitting region without introducing additional free parameters. For any individual source, the model effectively retains only a small number of free parameters, including the total JET power, $L_{\rm j}$, and the on-axis bulk Lorentz factor, $Γ_0$. We consider two prescriptions for the radial distribution of the radiating electrons -- proportional either to the gas pressure or to the rest-frame MAGNETic energy density -- and two toroidal-field profiles, yielding four model variants. Applying the model to a sample of ten QUASAR JETs at $z \geq 2.5$ with X-ray features resolved by \textit{Chandra}, we perform Bayesian parameter inference and model comparison. The Bayesian evidence systematically favors electron distributions that follow the gas pressure rather than the MAGNETic energy density, while the data discriminate only weakly between the assumed field profiles. The inferred JET powers, reaching $L_{\rm j} \sim 10^{49}\,\mathrm{erg\,s^{-1}}$, are systematically larger than those obtained from one-zone models, and the corresponding global JET MAGNETization parameters are low. None of the derived quantities, including $Γ_0 \sim \mathcal{O}(10)$, shows a significant monotonic trend with redshift.
[abstract 2 / 42] Wow! (score: 8) - Title: VAPOLA -- A multi-year, multi-band POLARIZATION survey of AGN and Sgr A* at mm wavelengths with ALMA I. Survey Overview and Science-Ready Archival ProductsAuthors: Alejandro Mus, Ciriaco Goddi, Douglas Carlos, Vincenzo Galluzzi, Ezequiel Albentosa-Ruiz, Ivan Martí-Vidal, Hugo Messias, Kazi L. J. Rygl, Geoffrey B. Crew, Lynn D. Matthews, Elisabetta Liuzzo, Nicola Marchili, Raphael P. Rolim, Mariafelicia De Laurentis, Rocco Lico, Cristiano Urban,Comments: Accepted in A&A, 07/06/2026Subjects: astro-ph.GA astro-ph.IMCreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
The Atacama Large Millimeter/submillimeter Array (ALMA) is the most sensitive interferometric array at millimeter and submillimeter wavelengths. Through the ALMA Phasing System (APS), it can participate in global Very Long Baseline Interferometry (VLBI) arrays, enhancing their sensitivity and resolution. However, processing and analzing the ALMA data obtained in APS mode during VLBI observations remains a complex task, requiring specialized expertise and time-consuming calibration and imaging procedures. In this paper, we present VAPOLA-the first online, multi-epoch, multi-band repository of high-level data products from ALMA observations of ACTIVE GALACTIC NUCLEi (AGN) and Sgr A* during global VLBI campaigns. Built on an automated pipeline that processes fully calibrated ALMA (QA2) data, generates science-ready products with minimal user intervention. The repository includes fully calibrated interferometric visibilities, full-Stokes images across individual and combined spectral windows, polarimetric and spectral index maps, as well as tabulated polarimetric parameters from visibility-domain POLARIZATION fitting. By offering ready-to-use data through a user-friendly web portal, VAPOLA enables non-expert users to perform advanced science analyses without needing in-depth knowledge of ALMA procedures. This resource will facilitate a broad range of scientific investigations, including the characterization of MAGNETic field properties in accretion flows and RELATIVISTIC JETs, the structure and kinematics of dusty and molecular tori in AGN, and absorption studies of the interstellar medium toward the Galactic Center. In addition, the dataset provides source-integrated parameters and calibration metadata essential for refining VLBI calibration and imaging workflows as well as for placing robust observational constraints on theoretical models of supermassive BLACK HOLEs and their environments.
[abstract 3 / 42] Yes (score: 6) - Title: Global Magnetohydrodynamic Simulations of Monster Shocks in Neutron Star MagnetospheresAuthors: Michael P. Grehan, Bart Ripperda, Andrei M. Beloborodov, Christopher Thompson, Elias R. Most,Comments: 24 pages, 18 figures. Published in the Astrophysical JournalSubjects: astro-ph.HE physics.plasm-phCreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
Waves launched from the neutron star surface or inner MAGNETosphere propagate through the MAGNETosphere as small perturbations, but can grow relative to the background MAGNETic field and steepen into ``monster shocks'' -- ultra-RELATIVISTIC MAGNETized shocks which can power high-energy emission. Such shocks can develop around isolated MAGNETars, merging binaries, and collapsing neutron stars. They occur in MAGNETically dominated plasma and are described by RELATIVISTIC MAGNETohydrodynamics (MHD). We present global RELATIVISTIC MHD simulations of monster shocks in unperturbed and perturbed (``wrinkled'') backgrounds with a global dipolar geometry. Our simulations confirm analytical predictions for equatorial shocks and provide new insight into the behavior of oblique shocks off the equator. Simulations where the shock is formed through Alfvén mode to fast mode conversion are also presented, demonstrating the generic nature of the monster shock mechanism. We explore how the presence of additional modes in the MAGNETosphere modifies the shock behavior. Modes of comparable amplitude can fragment the shock front, substantially reduce the MAGNETization, produce localized enhancements in the Lorentz factor relative to an unperturbed dipole background, and intermittently generate additional shocks along a line of sight.
[abstract 4 / 42] Yes (score: 6) - Title: Universal behaviour of $α$-viscosity in BLACK HOLE accretion discsAuthors: Marek A. Abramowicz, Axel Brandenburg, Jiří Horák, Debora Lančová, John C. Miller, Ewa Szuszkiewicz, Maciek Wielgus,Comments: 9 pages, 3 figures, accepted for publication in Astronomy&AstrophysicsSubjects: astro-ph.HECreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
The Shakura-Sunyaev $α$-viscosity coefficient, defined as the ratio of total stress to total pressure, $α= \mathbb{T}/p$, began to play an important role in the development of accretion disc theory in the early 1970s. The origin of the turbulence that causes the stress $\mathbb{T}$ was unknown at that time; Shakura and Sunyaev assumed $α=$ const. Today we know that this was not quite realistic - modern general RELATIVISTIC MAGNETo-hydrodynamic simulations (GRMHD) of BLACK HOLE accretion discs have revealed that $α$ changes by about an order of magnitude within the disc, being smaller far away from the BLACK HOLE and larger in the plunging region close in, and it has been found that the behaviour of $α$ reflects some underlying, fundamental properties of the stress $\mathbb{T}$. In particular, it has been argued by several authors, that $\mathbb{T}$ must be zero at the BLACK HOLE horizon. We note that the stress calculated in three independent GRMHD simulations of accretion discs around non-rotating BLACK HOLEs, made by a variety of authors (including ourselves), each has its prominent maximum close to the location of the circular photon orbit. We propose a formula that accurately describes this 'universal' behaviour of $α$ in terms of the 'gyration radius', a physical characteristic of rotation well known in Newtonian dynamics and in the BLACK HOLE case uniquely defined by the Kerr space-time geometry. Analytic and semi-analytic models of BLACK HOLE accretion discs provide an invaluable insight into fundamental physics, and the GRMHD simulations do not aspire to replace them. Rather, simulations could help to improve analytic models by making them more realistic. For example, our $α$-formula, deduced from the GRMHD simulations, may be useful in the construction of improved versions of thin and slim disc models.
[abstract 5 / 42] Yes (score: 6) - Title: Radiative GRMHD simulations of puffy accretion discs: Numerical versus analytical models of sub-Eddington accretionAuthors: Debora Lančová, Maciek Wielgus, Marek Abramowicz, Agata Różańska, Włodek Kluźniak, Jiří Horák, David Abarca, Aleksander Sądowski, Gabriel Török,Comments: 13 pages, 9 figures, accepted for publication in MNRASSubjects: astro-ph.HECreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
A widely accepted picture of an accretion flow in the luminous soft spectral state of X-ray binary systems is a geometrically thin disc structure much like the classic analytic solution of Shakura& Sunyaev. Although the analytic models are troubled by instabilities and miss important aspects of physics, such as MAGNETic fields, they are successfully used as a framework for interpreting observational data. Here, we compare the results of general RELATIVISTIC radiative MAGNETohydrodynamic (GRRMHD) simulations of optically thick, mildly sub-Eddington accretion on a stellar-mass BLACK HOLE (the puffy disc) with established analytic and semi-analytic accretion models in the same regime. From the simulations, we find that the accretion flow is stabilised by the MAGNETic field, with a puffed-up, optically thick region resembling a warm corona surrounding a denser and cooler disc core. However, the stratified vertical structure of the disc significantly influences the observational picture of such a system. We analyse the inner disc structure, flow properties, effective viscosity, and inner edge position, and compare them to the predictions of standard models. We find that the simulated discs share some similarities with the models; however, they differ in several important aspects, most notably: the photosphere is geometrically thick, the inner edge is located closer to the central BLACK HOLE than the analytic models assume, the surface density is significantly lower than analytically predicted, and the effective viscosity parameter is not constant but rises steeply in the innermost region.
[abstract 6 / 42] Yes (score: 6) - Title: The SANE, the MAD, and the ChimeraAuthors: George N. Wong, James M. Stone,Comments: 22 pages, 13 figuresSubjects: astro-ph.HECreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
Non-radiative BLACK HOLE accretion flows are commonly classified by their MAGNETic flux state, with standard and normal evolution (SANE) disks and MAGNETically arrested disks (MADs) marking the usual weak- and strong-flux regimes. We compare three-dimensional general RELATIVISTIC MAGNETohydrodynamics simulations of a weakly MAGNETized SANE flow, a standard MAD, and a Chimera flow fed by a different reservoir of mass, angular momentum, and coherent MAGNETic flux. The Chimera reaches a MAD-level horizon MAGNETic flux and launches a powerful electroMAGNETic JET during an extended non-eruptive interval, showing that a flow can maintain large horizon flux and JET power without sharing the standard MAD's bursty horizon-flux variability, mass-flow distribution, or inner-flow morphology. In the SANE flow, we show that radial support is primarily hydrodynamic and provided by gas pressure gradients, whereas in MAD flows, MAGNETic pressure and tension enter the radial force budget at comparable order and help regulate the inner flow dynamics. The Chimera remains distinct from the standard MAD in its density structure, funnel-wall geometry, mass-flow channels, radial force budget, and angular-momentum transport throughout the analyzed evolution. We therefore argue that MAD-like behavior is not captured by any single diagnostic, but by a dynamical coupling among horizon flux, JET power, MAGNETic support, Maxwell transport, surface-layer flow, disk morphology, and eruption activity. The Chimera shows that these outcomes can be separated by accretion history and MAGNETic-flux supply.
[abstract 7 / 42] Yes (score: 5) - Title: Searching For Fast Radio Transients And Radio Pulsars Using SPOTLIGHTAuthors: Kenil Ajudiya,Comments: 46 pages, 23 figuresSubjects: astro-ph.HECreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
Our initial impressions of astronomical objects was that they are inherently "static" over the course of any reasonably long observation. However, with the discovery of QUASARs and their scintillation in 1963-64, we learnt that there are transient phenomena even at the astronomical scales. The world of known transients has been expanding ever since then. Objects and phenomena like QUASARs, gamma ray bursts (GRBs), pulsars, rotating radio transients (RRATs), fast radio bursts (FRBs) and ultra long period transients (ULPTs) have answered several unanswered questions about the end states of stellar collapse, i.e, the formation and properties of back holes, neutron stars and white dwarfs. Even more interestingly, they have made us better realise how little we know about the universe. Even after more than 5 decades of research, many lurking questions about neutron stars await answers. In the current work, I explored the arena of FRB and radio pulsar astronomy by joining and contributing to the efforts of the SPOTLIGHT collaboration. The recent decades have witnessed huge leaps in radio instrumentation and high performance computing (HPC) technologies driven by the development of high throughput Graphics Processing Units (GPUs). These major technological advancements are conducive to probing extremely small time scales (up to microseconds) of astronomical events. Modern and next generation radio transients surveys at existing and upcoming radio telescopes worldwide are designed to make optimal use of the available resources to push the research frontiers with the sheer volume of data they produce (hence the terminology, data-driven astronomy). There is an urgent need to upgrade the existing time-domain radio astronomy software to keep up with the pace of the technological revolution on the hardware side. Although pulsar phenomena has been studied in great detail...
[abstract 8 / 42] Yes (score: 5) - Title: Classification of IGR J20084+3221 as an Intermediate Polar using X-ray and Optical ObservationsAuthors: Julian Gerber, Jeremy Hare, John A. Tomsick, Daniel Stern, Aarran W. Shaw,Comments: 9 pages, 5 figures, accepted to MNRASSubjects: astro-ph.HECreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
IGR J20084+3221 is a previously unclassified Galactic source first detected by INTEGRAL. Chandra observations led to possible classifications of either a MAGNETic Cataclysmic Variable (mCV) or high mass X-ray binary (HMXB) based on the hardness of its spectrum. Here, we report follow-up observations taken by XMM-Newton, NUSTAR, and the Hale Telescope at Palomar Observatory. Based on these observations, we conclude that IGR J20084+3221 is most likely an Intermediate Polar (IP) type mCV. Timing analysis of the X-ray data found a significant peak period of $P=635.0\pm0.4$ s, which we interpret to be the spin period of the white dwarf (WD). The X-ray spectrum is well fit to an absorbed Bremsstrahlung model with components accounting for partial covering, reflection, and a fluorescent Fe-line, all typical for an IP. The optical spectrum shows clear emission lines, consistent with emission dominated by an accretion disk. We find counterparts to the source across the optical and infrared (IR) bands, and, despite uncertainties in the distance and extinction, we estimate that the source is too faint in the IR to be an HMXB. Given the evidence pointing towards an IP classification, we fit the X-ray spectrum to a post-shock region model where we find a WD mass of $M=1.09^{+0.12}_{-0.11}\mathrm{M}_{\odot}$, larger than the average mass for a WD in an mCV.
[abstract 9 / 42] Yes (score: 5) - Title: Sub-Torque-Balance Upper Limits on Continuous Gravitational Waves from Scorpius X-1Authors: The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration, the Precision Ephemerides for Gravitational-Wave Searches, Project, :, A. G. Abac, I. Abouelfettouh, F. Acernese, K. Ackley, A. Adam, C. Adamcewicz, S. Adhicary, D. Adhikari, N. Adhikari, R. X. Adhikari, V. K. Adkins, S. Afroz, A. Agapito, D. Agarwal, M. Agathos, N. Aggarwal, S. Aggarwal, O. D. Aguiar, I. -L. Ahrend, L. Aiello, A. Ain, P. Ajith, T. Akutsu, S. Albanesi, L. Albers, W. Ali, S. Al-Kershi, C. Alléné, A. Allocca, S. Al-Shammari, P. A. Altin, S. Alvarez-Lopez, W. Amar, O. Amarasinghe, A. Amato, F. Amicucci, C. Amra, C. Anand, A. Ananyeva, S. B. Anderson, W. G. Anderson, M. Andia, M. Ando, M. Andrés-Carcasona, J. L. Andrey, T. Andrić, J. Anglin, J. Anna, S. Ansoldi, J. M. Antelis, S. Antier, M. Aoumi, E. Z. Appavuravther, S. Appert, S. K. Apple, K. Arai, A. Araya, M. C. Araya, M. Arca Sedda, F. Arciprete, J. S. Areeda, N. Aritomi, F. Armato, S. Armstrong, N. Arnaud, M. Arogeti, S. M. Aronson, G. Ashton, Y. Aso, L. Asprea, M. Assiduo, S. Assis de Souza Melo, S. M. Aston, P. Astone, F. Attadio, F. Aubin, K. AultONeal, G. Avallone, E. A. Avila, S. Babak, C. Badger, S. Bae, S. Bagnasco, L. Baiotti, R. Bajpai, T. Baka, K. A. Baker, T. Baker, G. Balbi, G. Baldi, N. Baldicchi, M. Ball, G. Ballardin, S. W. Ballmer, S. Banagiri, B. Banerjee, D. Bankar, T. M. Baptiste, P. Baral, M. Baratti, J. C. Barayoga, K. Baric, B. C. Barish, D. Barker, N. Barman, P. Barneo, F. Barone, B. Barr, M. Barrios, L. Barsotti, M. Barsuglia, D. Barta, M. A. Barton, I. Bartos, A. Basalaev, R. Bassiri, A. Basti, M. Bawaj, P. Baxi, J. C. Bayley, A. C. Baylor, P. A. Baynard, M. Bazzan, V. M. Bedakihale, F. Beirnaert, M. Bejger, D. Belardinelli, A. S. Bell, C. Bellani, L. Bellizzi, D. Beltran-Martinez, W. Benoit, I. Bentara, M. Ben Yaala, S. Bera, F. Bergamin, B. K. Berger, S. Bernuzzi, M. Beroiz, I. Berry, D. Bersanetti, T. Bertheas, A. Bertolini, J. Betzwieser, D. Beveridge, G. Bevilacqua, N. Bevins, R. Bhandare, R. Bhatt, A. Bhattacharjee, D. Bhattacharjee, S. Bhattacharyya, S. Bhaumik, V. Biancalana, A. Bianchi, F. Bianchi, I. A. Bilenko, G. Billingsley, A. Binetti, S. Bini, C. Binu, S. Biot, O. Birnholtz, S. Biscoveanu, A. Bisht, M. Bitossi, M. -A. Bizouard, S. Blaber, J. K. Blackburn, L. A. Blagg, C. D. Blair, D. G. Blair, N. Bode, N. Boettner, P. Bogdan, G. Boileau, M. Boldrini, G. N. Bolingbroke, A. Bolliand, L. D. Bonavena, R. Bondarescu, F. Bondu, V. A. Bonhomme, E. Bonilla, M. S. Bonilla, A. Bonino, R. Bonnand, A. Borchers, N. Borghi, V. Boschi, S. Bose, V. Bossilkov, Y. Bothra, A. Boudon, M. Boyle, A. Bozzi, C. Bradaschia, M. J. Brady, P. R. Brady, A. Branch, M. Branchesi, T. Briant, A. Brillet, M. Brinkmann, P. Brockill, E. Brockmueller, A. F. Brooks, B. C. Brown, D. D. Brown, M. L. Brozzetti, S. Brunett, G. Bruno, R. Bruntz, J. Bryant, Y. Bu, F. Bucci, J. Buchanan, O. Bulashenko, T. Bulik, H. J. Bulten, A. Buonanno, K. Burtnyk, R. Buscicchio, D. Buskulic, C. Buy, R. L. Byer, R. Cabrita, V. Cáceres-Barbosa, L. Cadonati, G. Cagnoli, C. Cahillane, A. Calafat, T. A. Callister, E. Calloni, S. R. Callos, M. Canepa, G. Caneva Santoro, K. C. Cannon, H. Cao, L. A. Capistran, E. Capocasa, G. Capoccia, E. Capote, G. Capurri, G. Carapella, F. Carbognani, K. J. Cardona-Martínez, M. Carlassara, J. B. Carlin, T. K. Carlson, M. F. Carney, M. Carpinelli, G. Carrillo, J. J. Carter, G. Carullo, A. Casallas-Lagos, J. Casanueva Diaz, C. Casentini, S. Caudill, M. Cavaglià, R. Cavalieri, G. Cella, S. Cepic, P. Cerdá-Durán, E. Cesarini, N. Chabbra, W. Chaibi, A. Chakraborty, P. Chakraborty, S. Chakraborty, S. Chalathadka Subrahmanya, R. Chalmers, C. Chan, J. C. L. Chan, M. Chan, K. Chang, P. Charlton, E. Chassande-Mottin, C. Chatterjee, Debarati Chatterjee, Deep Chatterjee, M. Chaturvedi, S. Chaty, A. Chen, A. H. -Y. Chen, D. Chen, H. Chen, H. Y. Chen, S. Chen, Y. Chen, G. Cheng, H. P. Cheng, P. Chessa, T. Cheunchitra, H. T. Cheung, S. Y. Cheung, F. Chiadini, G. Chiarini, A. Chiba, A. Chincarini, D. Chintala, M. L. Chiofalo, A. Chiummo, C. Chou, S. Choudhary, N. Christensen, S. S. Y. Chua, G. Ciani, P. Ciecielag, M. Cieślar, M. Cifaldi, B. Cirok, F. Clara, J. A. Clark, T. A. Clarke, P. Clearwater, S. Clesse, F. Cleva, S. M. Clyne, E. Coccia, E. Codazzo, P. -F. Cohadon, D. E. Cohen, S. Colace, E. Colangeli, O. Cole, M. Colleoni, C. G. Collette, J. Collins, S. Colloms, A. Colombo, C. M. Compton, G. Connolly, L. Conti, T. R. Corbitt, I. Cordero-Carrión, S. Corezzi, N. J. Cornish, I. Coronado, A. Corsi, L. A. Corubolo, L. Cotnoir, R. Cottingham, M. W. Coughlin, P. Couvares, D. M. Coward, D. C. Coyne, R. Coyne, A. Cozzumbo, J. D. E. Creighton, T. D. Creighton, S. Crook, R. Crouch, J. Csizmazia, J. R. Cudell, T. J. Cullen, A. Cumming, E. Cuoco, M. Cusinato, L. V. Da Conceição, T. Dal Canton, S. Dall'Osso, S. Dal Pra, G. Dálya, O. Dan, Y. Dang, B. D'Angelo, S. Danilishin, S. D'Antonio, K. Danzmann, K. E. Darroch, L. P. Dartez, R. Das, A. Dasgupta, V. Dattilo, A. Daumas, I. Dave, A. Davenport, M. Davier, T. F. Davies, D. Davis, L. Davis, M. C. Davis, P. Davis, E. J. Daw, M. Dax, J. De Bolle, M. Deenadayalan, J. Degallaix, M. De Laurentis, C. J. Delgado Mendez, F. De Lillo, S. Della Torre, W. Del Pozzo, O. M. del Rio, A. Demagny, F. De Marco, G. Demasi, F. De Matteis, N. Demos, T. Dent, A. Depasse, N. DePergola, R. De Pietri, R. De Rosa, C. De Rossi, M. Desai, V. Deshmukh, R. De Simone, S. Determan, A. Dhani, R. Dhurkunde, R. Diab, C. Diaz, M. C. Díaz, M. Di Cesare, G. Dideron, T. Dietrich, L. Di Fiore, C. Di Fronzo, M. Di Giovanni, T. Di Girolamo, D. Diksha, J. Ding, S. Di Pace, I. Di Palma, D. Di Piero, F. Di Renzo, Divyajyoti, A. Dmitriev, J. P. Docherty, Z. Doctor, N. Doerksen, E. Dohmen, A. Doke, A. Domiciano De Souza, L. D'Onofrio, F. Donovan, K. L. Dooley, T. Dooney, S. Doravari, O. Dorosh, F. Dosopoulou, W. J. D. Doyle, M. Drago, J. C. Driggers, M. Dubois, R. R. Dumbreck, L. Dunn, U. Dupletsa, D. D'Urso, P. Dutta Roy, H. Duval, P. -A. Duverne, S. E. Dwyer, C. Eassa, M. Eberhardt, M. Ebersold, T. Eckhardt, G. Eddolls, A. Effler, J. Eichholz, H. Einsle, M. Eisenmann, R. A. Eisenstein, M. Emma, K. Endo, R. Enficiaud, L. Errico, R. Espinosa, M. Esposito, R. C. Essick, H. Estellés, T. Etzel, M. Evans, T. Evstafyeva, B. E. Ewing, J. M. Ezquiaga, F. Fabrizi, V. Fafone, S. Fairhurst, X. Fan, A. M. Farah, B. Farr, W. M. Farr, M. Favata, M. Fays, M. Fazio, J. Feicht, M. M. Fejer, J. -N. Feldhusen, E. Fenyvesi, J. Fernandes, T. Fernandes, D. Fernando, S. Ferraiuolo, T. A. Ferreira, M. Ferrer, F. Fidecaro, P. Figura, A. Fiori, I. Fiori, M. Fishbach, R. P. Fisher, R. Fittipaldi, V. Fiumara, R. Flaminio, S. M. Fleischer, L. S. Fleming, E. Floden, H. Fong, J. A. Font, F. Fontinele-Nunes, C. Foo, B. Fornal, P. W. F. Forsyth, K. Franceschetti, A. Franco-Ordovas, F. Frappez, S. Frasca, F. Frasconi, J. P. Freed, Z. Frei, A. Freise, O. Freitas, R. Frey, W. Frischhertz, P. Fritschel, V. V. Frolov, M. Fuentes-Garcia, S. Fujii, T. Fujimori, P. Fulda, M. Fyffe, B. Gadre, J. R. Gair, S. Galaudage, V. Galdi, R. Gamba, A. Gamboa, S. Gamoji, A. Ganguly, B. Garaventa, P. García Abia, J. García-Bellido, C. García-Quirós, J. W. Gardner, S. Garg, J. Gargiulo, X. Garrido, A. Garron, F. Garufi, P. A. Garver, C. Gasbarra, B. Gateley, F. Gautier, V. Gayathri, T. Gayer, G. Gemme, A. Gennai, V. Gennari, J. George, R. George, O. Gerberding, L. Gergely, Archisman Ghosh, Sayantan Ghosh, Shaon Ghosh, Shrobana Ghosh, Suprovo Ghosh, Tathagata Ghosh, J. A. Giaime, K. D. Giardina, D. R. Gibson, C. Gier, S. Gkaitatzis, J. Glanzer, F. Glotin, J. Godfrey, R. V. Godley, O. Godwin, A. S. Goettel, E. Goetz, J. Golomb, S. Gomez Lopez, G. González, P. Goodarzi, S. Goode, A. Goodwin-Jones, M. Gosselin, C. Gostiaux, R. Gouaty, D. W. Gould, K. Govorkova, A. Grado, A. E. Granados, M. Granata, V. 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Thorne, E. Thrane, J. Tissino, A. Tiwari, Pawan Tiwari, Praveer Tiwari, S. Tiwari, V. Tiwari, M. R. Todd, E. Tofani, M. Toffano, A. M. Toivonen, K. Toland, A. E. Tolley, T. Tomaru, V. Tommasini, T. Tomura, H. Tong, C. Tong-Yu, A. Torres-Forné, C. I. Torrie, I. Tosta e Melo, E. Tournefier, M. Trad Nery, A. Trapananti, R. Travaglini, F. Travasso, G. Traylor, M. Trevor, M. C. Tringali, A. Tripathee, G. Troian, A. Trovato, L. Trozzo, R. J. Trudeau, T. Tsang, S. Tsuchida, K. Tsuji, L. Tsukada, K. Turbang, M. Turconi, C. Turski, H. Ubach, A. S. Ubhi, T. Uchiyama, R. P. Udall, T. Uehara, K. Ueno, V. Undheim, L. E. Uronen, T. Ushiba, M. Vacatello, H. Vahlbruch, G. Vajente, J. Valencia, M. Valentini, E. Vallejo-Pagès, S. A. Vallejo-Peña, S. Vallero, M. van Dael, E. Van den Bossche, J. F. J. van den Brand, C. Van Den Broeck, M. van der Kolk, M. van der Sluys, A. Van de Walle, J. van Dongen, K. Vandra, M. VanDyke, H. van Haevermaet, J. V. van Heijningen, P. Van Hove, J. Vanier, J. Vanosky, N. van Remortel, M. Vardaro, A. F. Vargas, V. Varma, A. Vecchio, G. Vedovato, J. Veitch, P. J. Veitch, S. Venikoudis, J. Venneberg, R. C. Venterea, P. Verdier, M. Vereecken, D. Verkindt, B. Verma, Y. Verma, S. M. Vermeulen, F. Vetrano, A. Veutro, A. Viceré, S. Vidyant, A. D. Viets, A. Vijaykumar, A. Vilkha, N. Villanueva Espinosa, V. Villa-Ortega, E. T. Vincent, J. -Y. Vinet, S. Viret, S. Vitale, A. Vives, L. Vizmeg, H. Vocca, D. Voigt, E. R. G. von Reis, J. S. A. von Wrangel, W. E. Vossius, L. Vujeva, S. P. Vyatchanin, J. Wack, L. E. Wade, M. Wade, K. J. Wagner, L. Wallace, E. J. Wang, H. Wang, W. H. Wang, Y. F. Wang, Z. Wang, G. Waratkar, R. L. Ward, J. Warner, M. Was, T. Washimi, N. Y. Washington, B. Weaver, S. A. Webster, N. L. Weickhardt, M. Weinert, A. J. Weinstein, R. Weiss, L. Wen, K. Wette, C. Wheeler, J. T. Whelan, B. F. Whiting, E. G. Wickens, D. Wilken, B. M. Williams, D. Williams, M. J. Williams, N. S. Williams, J. L. Willis, B. Willke, M. Wils, L. Wilson, C. W. Winborn, J. Winterflood, C. C. Wipf, G. Woan, J. Woehler, N. E. Wolfe, H. T. Wong, I. C. F. Wong, K. Wong, T. Wouters, J. L. Wright, M. Wright, B. Wu, C. Wu, D. S. Wu, H. Wu, K. Wu, Q. Wu, Z. Wu, E. Wuchner, D. M. Wysocki, V. A. Xu, Y. Xu, N. Yadav, H. Yamamoto, K. Yamamoto, T. S. Yamamoto, T. Yamamoto, R. Yamazaki, T. Yan, H. Yang, K. Z. Yang, Y. Yang, Z. Yarbrough, J. Yebana, S. -W. Yeh, A. B. Yelikar, X. Yin, J. Yokoyama, T. Yokozawa, S. Yuan, H. Yuzurihara, M. Zanolin, M. Zeeshan, T. Zelenova, J. -P. Zendri, M. Zeoli, M. Zerrad, M. Zevin, H. Zhang, L. Zhang, N. Zhang, R. Zhang, T. Zhang, C. Zhao, Yue Zhao, Yuhang Zhao, Z. -C. Zhao, Y. Zheng, H. Zhong, H. Zhou, H. O. Zhu, Z. -H. Zhu, Z. Zhu, A. B. Zimmerman, L. Zimmermann, M. E. Zucker, T. L. Killestein, D. Steeghs, J. Casares, D. K. Galloway,Comments: 30 pages, 7 figuresSubjects: astro-ph.HE gr-qcCreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
We present the results of a search for continuous gravitational waves from the low-mass X-ray binary Scorpius X-1 using LIGO data from the first part of the fourth LIGO-Virgo-KAGRA observing run. By applying the resampling version of the cross-correlation pipeline to search for signal frequencies $f_0$ between $25$ and $200\un{Hz}$ (corresponding to neutron star spin frequencies of $12.5$ to $100\un{Hz}$ for GW due to triaxiality, or $\sim15-20$ to $\sim120-150\un{Hz}$ for GW due to $r$-modes), we set upper limits below the standard torque balance level, independent of neutron star spin inclination, for $50\un{Hz}\lesssim f_0\lesssim200\un{Hz}$. While uncertainties in the modelling of torque and equation of state limit the strength of our inference, our results nonetheless argue against torque balance in this spin range for a neutron star described by a hadronic equation of state. The most sensitive upper limits on the gravitational wave amplitude $h_0$, at the upper end of the frequency band searched, approach $5\times10^{-26}$ marginalized over inclination angle and $2\times10^{-26}$ assuming the most favorable inclination. The marginalized upper limits correspond to a sensitivity depth of $70-75\un{Hz}^{-1/2}$, improving sensitivity considerably over previous searches. Expressed as constraints on the triaxial deformation of the neutron star, the limits correspond to an ellipticity of $3\times10^{-5}$ if the GW frequency $f_0$ is $75\un{Hz}$ and $3\times10^{-6}$ if $f_0=200\un{Hz}$, approaching deformations which could be supported by ordinary nuclear matter. Outliers from the search were ruled out as potential signals by a combination of hierarchical followup and analysis of additional data from later in the observing run.
[abstract 10 / 42] Yes (score: 4) - Title: Luminous Fast Blue Optical Transients as "Failed" Gravitational-wave Sources: Helium Core$-$Black Hole Mergers Following Delayed Dynamical InstabilityAuthors: Jakub Klencki, Brian D. Metzger,Comments: 18 pages, 11 figures + Appendix, published in ApJSubjects: astro-ph.HE astro-ph.SR gr-qcCreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
Binaries in which a massive donor star undergoes an extended ($\gtrsim$ kyr) phase of stable mass transfer onto a BLACK HOLE (BH) accretor offer a promising channel for creating LIGO gravitational wave sources. However, in many systems the mass transfer terminates prematurely in a dynamical instability at orbital periods of a few days, culminating in the BH plunging into the donor and potentially disrupting and accreting its helium core at highly super-Eddington rates. Combining a suite of binary evolution models with analytic estimates and population synthesis, we predict the population of luminous transients from delayed dynamical instability (DDI) and attribute them to the "luminous" class of fast blue optical transients (LFBOTs). The initial plunge of the BH into the partially stripped envelope typically ejects $\sim 10M_{\odot}$ of H/He-enriched material at speeds $\sim 10^{2}-10^{3}$ km s$^{-1}$, generating a compact circumstellar medium (CSM) of radius $\lesssim 1000R_{\odot}$ by the time the BH meets and tidally disrupts the HeC. Rapid BH accretion generates a highly aspherical wind-driven explosion into the environment, powering UV/optical emission via CSM interaction and X-ray reprocessing that rises over a few days to a luminosity $\sim 10^{44}-10^{45}$ erg s$^{-1}$ before fading as the disk spreads outwards and accretion rate drops. Luminous radio/sub-mm emission is generated over several months as the JET collides with the slow quasi-spherical binary outflow, generated by the stable mass transfer preceding DDI, extending to radii $\sim 10^{17}$ cm, in agreement with the inferred CSM environments of LFBOTs. We estimate local rates of DDI merger transients $5-300$ Gpc$^{-3}$ yr$^{-1}$, with a preference for low-metallicities, in agreement with LFBOT demographics. Taken together, our results support LFBOTs as being luminous signposts of "failed" gravitational wave sources.
[abstract 11 / 42] Yes (score: 4) - Title: No Measurable Changes in Radio and X-ray Emission Surrounding Glitches in the Young Pulsar PSR J2229+6114Authors: Wenke Xia, Robert A. Main, Mason Ng, Victoria M. Kaspi, Jason W. Hessels, Alyssa Cassity, Abigail K. Denney, Emmanuel Fonseca, Deborah C. Good, Ajay Kumar, Lars Kunkel, Bradley W. Meyers, Aaron B. Pearlman, Ingrid Stairs,Comments: 14 pages, 8 figures. Submitted to ApJ, comments welcomeSubjects: astro-ph.HECreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
We present our first result from an ongoing pulsar glitch monitoring campaign at the Canadian Hydrogen Intensity Mapping Experiment (CHIME), in which we analyzed the radio and X-ray emission surrounding four glitches in PSR J2229+6114. Using daily CHIME observations, we detected a glitch in PSR J2229+6114 in near-real time and triggered an X-ray follow-up with NUSTAR two days after the glitch. We identified three additional glitch events in archival CHIME/Pulsar observations that coincided with an independent X-ray observing campaign with NICER. Our data show there is no measurable change in the source's X-ray and radio emission during the four glitch events, in stark contrast to the post-glitch activity in high-MAGNETic-field, rotation-powered pulsars (RPPs), which have been observed to exhibit MAGNETar-like X-ray outbursts immediately after large glitches. Those high-MAGNETic-field (high-B) RPPs are considered transitional objects between ordinary RPPs and MAGNETars, thereby leading to a unifying neutron star model in which the inferred dipolar surface MAGNETic field strength serves as a unifying parameter. However, such a model remains challenged, in part, by the lack of constraints near the low-B end of the high-B regime, and our result provides additional evidence that MAGNETar-like post-glitch activity is likely more common among high-B RPPs.
[abstract 12 / 42] Yes (score: 4) - Title: Photon Acceleration in Magnetized Plasma: A Mechanism for Fast Radio BurstsAuthors: Sergei V. Bulanov, Gabriele Maria Grittani, Marcel Lamac, Petr Valenta, Stepan S. Bulanov, Timur Zh. Esirkepov, Gianluca Gregori, Brandon K. Russell, Alexander G. R. Thomas, Arno Vanthieghem,Comments: 25 pages, 6 figuresSubjects: physics.space-ph astro-ph.HE physics.plasm-phCreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
We propose a mechanism for fast radio bursts based on photon acceleration by RELATIVISTIC shocks propagating through highly MAGNETized electron--positron plasmas, as expected in MAGNETar MAGNETospheres. Density modulations at the shock front create RELATIVISTICally moving refractive-index perturbations that transform low-frequency electroMAGNETic precursors into amplified high-frequency radiation. We show that the predicted frequencies, durations, and energetics of the resulting fast radio bursts are consistent with the MAGNETic-field strengths, shock Lorentz factors, and characteristic spatial scales expected in MAGNETar MAGNETospheres.
[abstract 13 / 42] Yes (score: 4) - Title: FAST Discovery of $μ$Jy Radio Pulsations from PSR J2238+5903, Providing a DM Distance Anchor for the Candidate TeV Halo 1LHAASO J2238+5900Authors: Jianli Zhang, Hui Zhu, Guanhong Lin, Dejia Zhou, Yuting Chu, Songzhan Chen, Min Zha, WenJun Huang, ZiWei Ou, P. H. Thomas Tam, Sha Wu, Qiang Yuan, Yi Zhang, Ran Duan,Comments: 8 pages, 2 figures, comments welcomeSubjects: astro-ph.HECreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
We report the first detection of radio pulsations from PSR J2238+5903, a gamma-ray pulsar spatially coincident with the extended TeV source 1LHAASO J2238+5900. Our 3000 s FAST L-band observation reveals a weak periodic signal at the known FERMI-LAT spin period, with $P=162.76568$ ms and $\mathrm{DM}=247.5\pm3.0~\mathrm{pc~cm^{-3}}$. The signal is independently confirmed by both FFT-based and Fast Folding Algorithm searches. The radiometer equation gives a flux density of $S_{1250}\simeq3\,μ$Jy, placing PSR J2238+5903 among the faintest radio-detected FERMI pulsars. Interpreting the DM with Galactic electron-density models gives $d_{\rm DM}=7.4\pm3.9$ kpc. At this distance, the LHAASO WCDA 39\% containment radius corresponds to a characteristic diameter of $\sim132$ pc, and the $>1$ TeV luminosity is $L_{\rm TeV}\simeq7.1\times10^{34}$ erg s$^{-1}$, about 8\% of the pulsar's spin-down power. The radio DM thus provides the first pulsar-specific distance constraint for assessing whether 1LHAASO J2238+5900 is a young relic-PWN / TeV-halo transition system.
[abstract 14 / 42] Yes (score: 4) - Title: Tilted thin accretion disks in the full Kerr spacetime and their implicationsAuthors: K. S. Sruthy, Chandrachur Chakraborty, Sudip Bhattacharyya,Comments: 25 pages, 17 figures, 2 tables, accepted for publication in Phys. Rev. DSubjects: astro-ph.HE gr-qcCreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
We derive a steady-state warped-disk equation in the full Kerr spacetime to study the tilt dynamics of a thin, viscous accretion disk around a spinning collapsed object. The formulation, based on Pringle's framework, remains valid for all values of the Kerr parameter $a$, thereby encompassing both Kerr BLACK HOLEs (BHs; $0 < a \le 1$) and Kerr naked singularities ($a > 1$). By incorporating the exact Keplerian and Lense-Thirring precession frequencies, we analytically obtain the radial tilt profiles of the disk without invoking slow-spin or weak-field approximations. Numerical solutions of the resulting equations, obtained under realistic boundary conditions, reveal significant deviations from slow-spin approximations, particularly in the inner disk where the RELATIVISTIC effects dominate. In the diffusive regime, we find that for Kerr naked singularities the tilt profile exhibits distinct inner hump(s) near the radius where the specific angular momentum vanishes -- a feature absent for Kerr BHs. Consideration of a tilt in the inner disk could significantly influence the interpretations from observed X-ray spectral, timing, and POLARIZATION features, which are crucial to probe the strong gravity regime and to infer the spin of the central object. While such a distinct hump feature alone does not uniquely distinguish Kerr BHs from Kerr naked singularities, their interpretation in conjunction with constraints on the disk regime may provide a potential observational handle on the nature of the accreting collapsed object.
[abstract 15 / 42] (score: 3) - Title: Multiphase gas in Circumgalactic cloud complexes: Insights from kiloparsec-scale Magnetohydrodynamic Turbulence SimulationsAuthors: Rajsekhar Mohapatra, Alankar Dutta, Prateek Sharma,Comments: Published in the Open Journal of AstrophysicsSubjects: astro-ph.GACreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
The circumgalactic medium (CGM) is the diffuse gas surrounding a galaxy's halo, and it plays a vital role in the galactic baryon cycle. However, its mass distribution across the virial phase and the cooler, denser atomic phase, remains uncertain. To investigate this, we perform high-resolution MAGNETohydrodynamic simulations of 0.125--8 kpc-scale representative patches of the CGM, with parameters informed by QUASAR absorption line observations. Our simulations resolve the cooling length (the minimum across all temperatures of $c_s t_{\rm cool}$, where $c_s$ is the sound speed and $t_{\rm cool}$ is the cooling time in isobaric conditions), allowing us to track the evolution of cold gas more accurately. We find that low-density CGM gas ($3\times10^{-4}$ cm$^{-3}$) cannot sustain cold gas below $10^4$ K for long, due to a large value of the ratio between the cooling to mixing time ($t_{\rm cool}/t_{\rm mix}$). In contrast, higher-density environments ($3\times10^{-3}~{\rm cm}^{-3}$) reach a turbulent multiphase steady state, with up to $50\%$ of the mass in the cold phase, occupying only about $1\%$ of the volume. To connect with large-volume cosmological simulations and small ${\rm pc}$-scale idealized simulations, we explore different box sizes (0.125--8 kpc) and identify a key scaling relation: simulations with similar $t_{\rm cool}/t_{\rm mix}$ exhibit comparable cold gas mass fractions and lifetimes. Importantly, we find that simply sub-sampling (reducing box-size) a small region from a large-volume simulation while maintaining a constant turbulent energy density injection rate from larger to smaller scales artificially shortens $t_\mathrm{mix}$, leading to inaccurate predictions for cold gas survival. This means that cold gas at small $\lesssim 10$ kpc scales arises in relatively dense, quiescent regions of the CGM rather than the turbulent ones undergoing cascade from large scales.
[abstract 16 / 42] (score: 3) - Title: Residual energy in weakly compressible turbulence with a mean guide fieldAuthors: R. Skalidis, A. Tritsis, J. R. Beattie, P. F. Hopkins,Comments: Accepted for publication in A&ASubjects: astro-ph.SR physics.flu-dyn physics.plasm-phCreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
The energy distribution is a fundamental property of MAGNETohydrodynamic (MHD) turbulence. In strongly MAGNETized turbulence energy imbalances arise and are quantified by the residual energy: $E_r~=~(E_{kin}~ - ~E_{mag})$; $E_{kin}$ and $E_{mag}$ stand for the volume-averaged kinetic and MAGNETic energy, respectively. We explore the properties of $E_r$ in weakly compressible MHD turbulence in the presence of an initially strong (guide) MAGNETic field, investigating how the driving mechanism and the MAGNETic field strength affect the cascade of $E_r$. We run a suite of direct numerical simulations with the PENCIL code. The sonic Mach number is approximately equal to 0.1 in all simulations, whereas the plasma beta varies. We drive turbulence by either injecting velocity or MAGNETic fluctuations at large scales and study the power spectra of kinetic, MAGNETic, density, and $E_r$. Magnetically driven simulations show locally imbalanced Alfvénic fluctuations and a $\propto k^{-3/2}$ cascade, consistent with the dynamic alignment theory. In the inertial range, $E_r \approx$ 0. Kinetically driven simulations give rise to a $\propto k^{-1}$ scaling, consistent with weakly interacting modes that preserve a high level of coherence throughout the inertial range. Residual energy is positive at all scales of the inertial range. The spectral slope of the $E_r$ cascade steepens systematically with increasing MAGNETization, varying from approximately -1 at $β= 0.3$ to between -2.0 and -5/3 at $β= 4.0$. The energy partition in weakly compressible turbulence is strongly influenced by the forcing mechanism, even when the global sonic and Alfvénic Mach numbers are comparable across simulations.
[abstract 17 / 42] (score: 3) - Title: The measurable impact of the 2pN spin-dependent accelerations on the JET precession of M87$^\ast$Authors: Lorenzo Iorio,Comments: LaTex2e, 28 pages, no tables, 3 figures. Accepted for publication in Classical and Quantum GravitySubjects: gr-qc astro-ph.GACreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
Motivated by recent accurate measurements of disk/JET coprecessions around some galactic supermassive BLACK HOLEs, the accelerations experienced by an uncharged, spinless object in the Kerr metric, written in harmonic coordinates, are analytically calculated up to the formal second post-Newtonian order. To such a level, some new accelerations make their appearance. They are proportional to even and odd powers of the hole's angular momentum. Their counterparts are not known where the primary is a material body. After expressing them in a coordinate-independent, vector form valid for any orientations of the hole's spin axis in space, their orbital effects are perturbatively worked out in terms of the particle's Keplerian orbital elements. The resulting expressions, averaged over one orbital revolution, are valid for generic shapes and inclinations of the orbit. The orbital plane's precession proportional to the first power of the hole's angular momentum and to the reciprocal of the fourth power of the speed of light amounts to about twenty per cent of the corresponding Lense-Thirring effect. The latter is believed to be the cause of the accurately measured disk/JET precessional phenomenology, currently measured to a few per cent accuracy. Although at a lesser extent, also the precession proportional to the second power of the hole's spin and to the reciprocal of the fourth power of the speed of light is measurable. Allowed domains in the parameter space of the JET precession around M87$^\ast$ are displayed.
[abstract 18 / 42] (score: 3) - Title: The incidence of eROSITA X-ray AGN in the local Universe: from dwarf to massive galaxiesAuthors: Z. Igo, A. Merloni, A. Georgakakis, J. Buchner, R. Arcodia, M. Salvato, J. Aird, K. Nandra, B. Trakhtenbrot, P. G. Boorman, J. Comparat, G. Lamer, B. Laloux, M. Kluge, W. Roster, E. Bulbul, F. Balzer, T. Dwelly, W. N. Brandt, R. Seppi, S. Morrison, E. Kyritsis, J. Gelfand, S. F. Anderson, D. P. Schneider,Comments: 27 pages, 20 figures; accepted for publication in A&ASubjects: astro-ph.GA astro-ph.HECreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
Combining deep, wide-area X-ray surveys with multi-wavelength catalogues provides insights into rare, highly-accreting AGN and low-mass galaxies at low redshift, the latter potentially representing local analogues of the first galaxies in the early Universe. We use the four-pass eROSITA All Sky Survey to select the largest catalogue of X-ray AGN in a highly complete sample of low-redshift galaxies, including low-mass (logM*/Msol<10) ones. We probe their distribution of specific accretion rates, $λ$_SAR, and the cumulative AGN fraction above varying $λ$_SAR thresholds. Our parent sample consists of ~5.35 million galaxies selected from the Legacy Survey DR10 with z-band fluxes brighter than 20 mag and redshifts 0.03
[abstract 19 / 42] (score: 3) - Title: Intensity fluctuations of radio halo in galaxy cluster: Insights from power spectrum estimationAuthors: Srijita Pal, Nirupam Roy, Sameer Salunkhe, Surajit Paul, Tanu Sharma, Samir Choudhuri,Comments: Accepted for publication in ApJSubjects: astro-ph.COCreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
Non-thermal SYNCHROTRON emissions from radio halo allow us to study mechanisms of particle (re)acceleration, MAGNETic field distribution, merger history, and turbulence in the intra-cluster medium. We propose power spectrum estimation as a novel and complementary method to study galaxy clusters. We use 610 MHz observations of MACSJ0014.3-302 and MACSJ0152.5-2852 to estimate the angular power spectrum (C_l) from the central halo regions. The C_l shows excess emission only for MACSJ0014.3-302. Using simulations, we find that a halo model with power-law fluctuations, in addition to the smooth exponential radial profile, is required to explain the observed C_l. We compare the observed power-law with existing models of MHD turbulence. The method may be useful for large data from SKA, finding megahalos in other sources, or detecting faint cluster emissions beyond the visible extent.
[abstract 20 / 42] (score: 3) - Title: TeV Electron Beams from Plasma Acceleration via Regenerative CascadingAuthors: Chaojie Zhang, Chan Joshi,Comments: 8 pages, 5 figuresSubjects: physics.acc-ph physics.plasm-phCreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
Plasma accelerators sustain gradients orders of magnitude higher than conventional radiofrequency machines, but most proposed paths to TeV energies still require tens of stages, each demanding sub-micrometer alignment, femtosecond synchronization, and precise matching of the accelerating trailing bunch. Here we introduce plasma wakefield acceleration via regenerative cascading, in which each stage self-injects a fresh trailing electron bunch and the accelerated trailing bunch becomes the driver for the next stage. This approach has several advantages: energy multiplication instead of addition; automatic alignment, synchronization, and matching of the trailing bunch to the wake; and trailing bunch brightness reset in each stage. Particle-in-cell simulations show the generation of a 1.1 TeV electron beam with ~0.3% rms energy spread and 0.12 nC charge from a two-stage, sub-kilometer plasma accelerator driven by a 45 GeV, 100 nC beam. The low energy spread is achieved via dynamic beam loading in the evolving wake of the post-depletion driver that acts as a built-in energy dechirper.
[abstract 21 / 42] (score: 3) - Title: A Transport Theory of Turbulent Coronal Heating in General GeometryAuthors: Jonathan Squire, Benjamin D. G. Chandran, Toby Adkins, William A. Clarke, Romain Meyrand, Matthew W. Kunz,Comments:Subjects: astro-ph.SR astro-ph.HE physics.plasm-ph physics.space-phCreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
Magnetic geometry shapes how turbulence transports and dissipates energy in strongly MAGNETized plasmas. The solar corona, a maze of open and closed flux tubes with sharp transverse gradients, is a prominent example, yet most wave-turbulence models of coronal heating assume symmetric flux tubes or add geometric effects in ad hoc ways. Here we develop a geometry-complete multiscale transport theory for reduced-MAGNETohydrodynamic turbulence in an arbitrary background field, retaining squashing (MAGNETic shear), transverse gradients, curvature, and gravity at the same order as standard expansion-driven reflection, and coupling fast, anisotropic fluctuations to slow background evolution through conservation laws. Applied to the corona, it recovers the standard reflection-driven turbulent cascade in smooth regions such as coronal-hole interiors, but predicts that in structured regions geometry-driven channels can dominate: squashing drives reflection even when parallel Alfvén-speed gradients are weak; curvature and non-radial geometry drive compressive heating channels; and waves catalyze the relaxation of velocity shear into heat. The same dynamics drive cross-field transport of mass, composition, momentum, and heat across open-closed interfaces, at rates rivaling the field-parallel supply from the base. These effects bias heating to low altitudes in structured regions, giving a physical basis for the coronal-hole--boundary corrections used in empirical wind-speed predictors. Additionally, the framework's slow-timescale transport equations could be evolved in time, providing a route to a global, geometry-aware model of a structured wave-driven corona and wind. More broadly, the theory provides an energy-consistent account of turbulence, geometry, and transport effects relevant to various astrophysical and terrestrial settings, from MAGNETospheres and accretion flows to fusion experiments.
[abstract 22 / 42] (score: 3) - Title: Multi-wavelength Constraints on the Transient EP250905aAuthors: J. Quirola-Vasquez, P. G. Jonker, A. Levan, D. B. Malesani, F. E. Bauer, A. Martin-Carrillo, G. Corcoran, D. Mata Sanchez, R. A. J. Eyles-Ferris, F. Carotenuto, M. Ravasio, J. Sanchez-Sierras, J. Bright, J. A. Chacon, L. Cotter, F. J. Cowie, N. Sarin, M. A. P. Torres, J. N. D. van Dalen, A. P. C. van Hoof, V. D'Elia, P. Jakobsson, N. Habeeb, S. Kobayashi, A. Saccardi, M. De Pasquale, D. Xu, Y. H. Cheng, R. D. Liang, H. Sun, Y. Wang, W. Yuan, W. D. Zhang,Comments: Accepted for publication in A&ASubjects: astro-ph.HECreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
Fast X-ray transients (FXTs) are a diverse class of high-energy suggested origins, ranging from stellar explosions to compact object mergers. The Einstein Probe (EP) satellite discovers approximately 100 FXTs per year. We aim to constrain the physical origin of EP250905a. We analyze X-ray, optical, near-infrared (NIR), and radio temporal and spectral properties of EP250905a. In addition, we assess the possible role of weak gravitational lensing in shaping its observed characteristics. EP250905a fades rapidly in X-rays, and we detect no NIR or radio emission, but we detect early optical emission that rapidly fades beyond the detection limits. Two nearby galaxies are identified for which we derive spectroscopic redshifts of $z=0.374$ (G1) and $z=2.714$ (G2). Our analysis favors G2 as the host of the FXT EP250905a. The angular separation of 2.56\arcsec\, between the FXT's optical counterpart and the center of the G1 galaxy suggests the emission of the FXT might be moderately magnified by lensing effects ($μ\approx3.9$) given the inferred Einstein radius of G1 ($θ_E\approx1.9$ arcsec). The data are best explained as an afterglow from a mildly off-axis structured JET at $z=2.714$, providing a consistent broadband interpretation that also allows for weakly lensed emission of EP250905a.
[abstract 23 / 42] (score: 3) - Title: Successive Coronal Jets as Novel Facilitators for Filament Oscillation and EruptionAuthors: Chengrui Zhou, Chun Xia, Wentai Fu, Hechao Chen, Qiaoling Li,Comments:Subjects: astro-ph.SRCreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
Solar filament eruptions are central to coronal mass ejections and space weather, yet their triggering mechanisms remain a fundamental open question. In particular, the early-stage that drives a MAGNETic flux rope toward instability and its observable signatures are poorly understood. Here, combining multi-instrument observations, we report successive coronal JETs impacting a filament, causing its gradual rise and oscillations with growing amplitude and period. When the filament reaches the height where the decay index exceeds the torus instability threshold, the rapid filament eruption commences. This filament eruption is reproduced by MAGNETohydrodynamic simulations, in which successive thermal JETs disturb a stable filament in a MAGNETic flux rope and excite oscillations together with the eruption of the filament. As the filament rises to erupt, the restoring forces for the oscillation progressively weaken, which naturally leads to an increase of the oscillation amplitude and period. Our results demonstrate the growing oscillations as one of the observable precursors for filament eruptions, enhancing our ability to predict solar eruptions.
[abstract 24 / 42] (score: 3) - Title: The 20 GeV Galactic Halo Excess: Pixel-Level Confirmation and Consistency with Sub-TeV WIMP AnnihilationAuthors: Trinity Rosebud Stenhouse, Chamkaur Ghag, Frank F. Deppisch,Comments: 14 pages, 7 figuresSubjects: astro-ph.HE hep-exCreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
A recent analysis of 15 years of FERMI-LAT data reported a spherically symmetric, halo-like component of the Galactic diffuse emission that peaks near 20GeV. We independently reproduce this cell-aggregated analysis, then extend it to a pixel-level likelihood on the native $0.125^\circ$ maps, adding energy-dependent point-spread-function forward folding and masking bright sources. Both methods replicate the 20GeV halo spectrum, with the pixel-level normalisation ${\sim}20\%$ above the cellwise fit across NFW emissivity scalings $ρ^p$, $p \in 1,2,2.5$. This 20GeV halo is a high-latitude feature, distinct from the inner-Galaxy excess, and consistent with sub-TeV DARK MATTER (WIMP) annihilation. It is centrally concentrated, strongly disfavouring extragalactic emission. Fitting prompt $s$-wave annihilation spectra, best-fit masses are $m_χ\simeq 0.55$TeV ($W^+W^-$) and $0.72$TeV ($b\bar{b}$) with $\langleσv\rangle \simeq 1\times10^{-24}~\mathrm{cm^3\,s^{-1}}$, in $\sim\!4$-$5\times$ tension with dwarf spheroidal galaxy limits. However, accounting for foreground modelling and $J$-factor systematic uncertainties widens the tension window to $R\simeq1.6$-$9.3$, leaving the $s$-wave interpretation viable. To close the tension, we consider alternative particle DARK MATTER models. $p$-wave annihilation misses relic abundance constraints by $\sim\!7$ orders of magnitude. A decay interpretation evades dwarf limits but is disfavoured by the isotropic gamma-ray background. The only viable velocity structure consistent with dwarf limits, present-day halo rates, and relic density is low-velocity-enhanced annihilation (resonant Sommerfeld or Breit-Wigner). This supplies the required $\approx\!45\times$ boost from a thermal relic. Fully resolving the dwarf tension requires a fine-tuned resonance peaking at the halo velocity and falling for colder systems.
[abstract 25 / 42] (score: 2) - Title: Braginskii Viscosity in Cosmological Simulations of Galaxy Clusters: Implementation, Validation, and First ApplicationAuthors: Tirso Marin-Gilabert, Ulrich P. Steinwandel, Milena Valentini, John A. ZuHone, Klaus Dolag,Comments: 19 pages, 17 figures, accepted for publication in MNRASSubjects: astro-ph.IM astro-ph.CO astro-ph.GA physics.plasm-phCreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
We present the implementation of an anisotropic viscosity solver within the MAGNETohydrodynamics (MHD) framework of the TreeSPH code OpenGadget3. The solver models anisotropic viscous transport along MAGNETic field lines following the Braginskii formulation and includes physically motivated limiters based on the mirror and firehose instability thresholds, which constrain the viscous stress in weakly collisional plasmas. To validate the implementation, we performed a suite of standard test problems -- including two variants of the sound wave test, circularly and linearly polarized Alfven waves, fast MAGNETosonic wave, and the Kelvin-Helmholtz instability -- both with and without the plasma-instability limiters. The results show excellent agreement with the AREPO implementation of a similar anisotropic viscosity model, confirming the accuracy and robustness of our method. Our formulation integrates seamlessly within the individual adaptive timestepping framework of OpenGadget3, avoiding the need for subcycling. This provides efficient and stable time integration while maintaining physical consistency. Finally, we applied the new solver to a cosmological zoom-in simulation of a galaxy cluster as a proof-of-concept application, demonstrating its capability to model anisotropic transport and plasma microphysics in realistic large-scale environments. Our implementation offers a versatile and computationally efficient tool for studying anisotropic viscosity in MAGNETized astrophysical systems.
[abstract 26 / 42] (score: 2) - Title: Characterizing Binary Black Hole Subpopulations in GWTC-4 with Binned Gaussian Processes: On the Origins of the $35M_{\odot}$ PeakAuthors: Omkar Sridhar, Anarya Ray, Vicky Kalogera,Comments: Journal Accepted Version, 20 pages, 11 figuresSubjects: astro-ph.HE astro-ph.GACreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
Understanding the astrophysical origins of binary BLACK HOLEs requires accurate and flexible modeling of multi-dimensional population properties. In this \textit{Letter}, using a data-driven framework based on binned Gaussian processes, we characterize the joint distribution of BBH primary masses, mass ratios, and effective inspiral spins. We identify three distinct subpopulations in the GWTC-4 sample of observations and investigate their astrophysical origins. We find that only one of the three subpopulations exhibits the $35M_{\odot}$ peak, which is characterized by a strong preference for equal mass systems and isotropic spin orientations. Our inferred distributions are consistent with a predominantly dynamical origin of this feature. By comparing with theoretical simulations, we further show that the subpopulation that exhibits the $35M_{\sun}$ peak can exclusively comprise dynamically assembled systems in globular clusters, specifically if BLACK HOLE birth spins are in the range~$(0.1-0.2)$, whereas the other two subpopulations require substantial contributions from alternative formation channels. We constrain the \textit{lower bound} on the merger rate of BBHs in globular clusters to be $0.69^{+0.23}_{-0.33} \rm{Gpc}^{-3}\rm{yr}^{-1}$, which is consistent with most theoretical predictions(that can range from $0.2-57\rm{Gpc}^{-3}\rm{yr}^{-1}$ depending on modeling assumptions). We conclude that dynamical formation in globular clusters remains a strong candidate for the origin of this excess near $30-40M_{\odot}$ and that more data and targeted parametric models are necessary to rigorously establish this interpretation.
[abstract 27 / 42] (score: 2) - Title: Could the high-mass BLACK HOLEs from gravitational-wave observations be explained by lensing?Authors: Ritesh Harshe, R. Prasad, Parameswaran Ajith,Comments: 11 pages, 12 figuresSubjects: astro-ph.GA astro-ph.HE gr-qcCreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
The high-mass ($M \gtrsim 30 M_\odot$) BLACK HOLEs (BHs) from the gravitational-wave (GW) observations of LIGO and Virgo came as a surprise to many astronomers. While the collapse of metal-poor massive stars could produce such BHs, gravitational lensing has been invoked to explain their high masses. Broadhurst, Diego, and Smoot (henceforth BDS) argued that the mass distribution of BHs in coalescing binaries is very similar to that of the galactic BHs, and the inferred high masses are the result of neglecting the lensing magnification. They also proposed a redshift distribution of binary BH (BBH) mergers to explain the observed LIGO-Virgo mass distribution. We ask whether such a model is consistent with different aspects of the GW observations: 1) the observed number of BBH mergers, 2) the distribution of their redshifted total mass and apparent luminosity distance, 3) the non-detection of strongly lensed events, and 4) the non-observation of the stochastic GW background. By simulating lensed BBH mergers with the BDS model and comparing them with observations, we conclude that no choice of BDS model parameters is consistent with all aspects of the observations. Lensing magnification is not a viable explanation for the high-mass BHs discovered by LIGO and Virgo.
[abstract 28 / 42] (score: 2) - Title: Parameter-estimation bias induced by transient orbital resonances in extreme-mass-ratio inspiralsAuthors: Edoardo Levati, Alejandro Cárdenas-Avendaño,Comments: 10 pages, 4 figures, 1 table. Minor modifications to match journal versionSubjects: gr-qc astro-ph.HECreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
Given the multifrequency nature of RELATIVISTIC orbits, transient orbital resonances are expected to be ubiquitous during an extreme-mass-ratio inspiral (EMRI). At a resonance, the orbital dynamics is modified in a nontrivial way, imprinting an overall dephasing in the emitted gravitational waves and potentially impacting both the detection and parameter estimation of these sources. In this work, using a Fisher-matrix approach, we investigate the bias induced by transient orbital resonances in EMRI parameter estimation. We focus on the most dynamically significant low-order resonances, 3 : 2 and 2 : 1, as well as on the high-order, subdominant resonances 3 : 1 and 4 : 3. We find that, for most of the orbits considered, neglecting the effect of a resonance crossing leads to significant losses in signal-to-noise ratio and induces bias in parameter recovery. Furthermore, both the sign and the amplitude of the resonance-induced modifications to the integrals of motion play a crucial role and must be modeled accurately. Our results provide further evidence that failing to model transient orbital resonances accurately can hinder EMRI detection and parameter estimation, thereby limiting their scientific potential.
[abstract 29 / 42] (score: 2) - Title: Multi-Wavelength Signatures of a Giant Cometary Radio Halo in MACSJ0417-1154Authors: Ramananda Santra, Marco Balboni, Ruta Kale,Comments: 24 pages (total), 24 figures, 6 tables, 3 appendix (6 figures). Accepted for publication in ApJSubjects: astro-ph.HE astro-ph.CO astro-ph.GACreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
Galaxy clusters hosting diffuse non-thermal radio emission offer direct insight into plasma processes of the intracluster medium (ICM). We present the first multi-frequency study of the radio halo in MACSJ0417 (z = 0.445) using uGMRT (300-850 MHz), MeerKAT (900-1670 MHz), and archival \textit{XMM-Newton} data. The halo extends to $\sim$1.75 Mpc at 400 MHz, while two candidate relics (R1 and R2) are detected at 2.9 Mpc. The integrated spectra follow single power-laws with spectral indices $α\simeq -1.3$ for the halo and $α\simeq -1.6$ for the relics. Sensitive uGMRT imaging reveals a radio surface brightness edge $\sim$43$''$ SE of the cluster centre, which coincides with an X-ray discontinuity. Resolved spectral maps (400--1280 MHz) show significant fluctuations and a clear radial steepening of the spectral index. X-ray analysis reveals an elongated SE-NW morphology and high-temperature regions ($\sim$11 keV) along this axis. A strong radio and X-ray surface brightness correlation is found (correlation coefficient $\sim$ 0.85), with the correlation slope evolving from sublinear at 400 MHz to linear at 1280 MHz. These results, together with the spectral properties, support the turbulent re-acceleration model and point to inhomogeneous ICM conditions. The pure hadronic model is excluded owing to unrealistic energy requirements for cosmic-ray protons. We propose that MACSJ0417 is undergoing a minor off-axis dissociative merger (mass ratio $\sim$6:1) along the SE-NW axis, which has preserved its cool core while driving turbulence that powers the giant radio halo.
[abstract 30 / 42] (score: 2) - Title: Tracing BLACK HOLE and galaxy growth across environments since cosmic noonAuthors: Emma Jane Weller, Priyamvada Natarajan, Colin J. Burke, Shashank Dattathri,Comments: 16 pages, 11 figures. Under review at ApJSubjects: astro-ph.GACreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
The distribution of systems in the BLACK HOLE mass-stellar mass ($M_\mathrm{BH}-M_\star$) plane encodes not only the integrated growth of galaxies and their central BLACK HOLEs (BHs), but also the processes that shape their evolution. Using the ASTRID and TNG300 cosmological simulations, we track massive BHs from cosmic noon ($z=2$) to $z=0.5$, spanning 5.3 Gyr of assembly. Unlike most previous studies, we follow the BHs themselves rather than their original host galaxies, thereby capturing central BHs, BHs in satellites, and off-nuclear wandering BHs. We find that central BHs in both simulations evolve along a relatively tight, nearly redshift-invariant $M_\mathrm{BH}-M_\star$ relation that is broadly consistent with local empirical constraints and with measurements from variable ACTIVE GALACTIC NUCLEi (AGN) at comparable redshifts. Departures from this relation trace distinct evolutionary channels. High-mass central BHs grow substantially through mergers and subsequently quench their hosts through AGN kinetic feedback. Tidal stripping moves satellites to lower $M_\star$ at nearly fixed $M_\mathrm{BH}$, producing weakly accreting, overmassive central BHs in gas-poor systems. In ASTRID, satellite accretion and inefficient dynamical friction generate wandering BHs that are undermassive relative to their new hosts and experience minimal accretion or merger-driven growth. These populations occupy characteristic regions in both the $M_\mathrm{BH}-M_\star$ and the specific BH accretion rate-specific STAR FORMATION rate planes, demonstrating that a BH's location in these planes is a fossil record of its dynamical, accretion, and feedback history.
[abstract 31 / 42] (score: 2) - Title: The DESI View of the Faint Radio Source Population in LoTSS DR2Authors: M. I. Arnaudova, L. R. Holden, D. J. B. Smith, P. N. Best, R. Kondapally, K. J. Duncan, A. Bushi, S. Das, S. R. Flury, C. L. Hale, M. J. Hardcastle, H. J. A. Rottgering, S. Shenoy,Comments: 20 pages, 15 figures, accepted for publication in MNRASSubjects: astro-ph.GACreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
The faint radio-source population includes galaxies dominated by both STAR FORMATION (SF) and ACTIVE GALACTIC NUCLEi (AGN), which are two key processes shaping galaxy evolution. To investigate this population, we probabilistically classified 251,413 radio sources from the second data release of the LOFAR Two-metre Sky Survey (LoTSS DR2) using spectroscopic data from the first release of the Dark Energy Spectroscopic Instrument (DESI DR1). Our classification method includes: (i) the identification of radio excess relative to SF, (ii) the Baldwin, Philips & Terlevich (BPT) diagram, (iii) a modified Mass Excitation (MEx) diagram, and (iv) the [OIII]5007 equivalent width. These are combined with Monte Carlo methods to estimate the probability that each source is a star-forming galaxy (SFG), a radio-quiet AGN (RQ AGN), or a low- or high-excitation RADIO GALAXy (LERG or HERG), allowing various thresholds to be applied depending on science goals. Considering classifications above a 90 per cent probability threshold, we identify 68,820 SFGs, 32,288 RQ AGN, 35,210 LERGs and 3,085 HERGs, representing the largest radio sample to date with high-confidence spectroscopic classifications. Using this sample, we show with higher statistical power than previous studies that LERGs typically accrete below 1 per cent of the Eddington limit and HERGs above it. We also identify a small subset of high-accreting LERGs whose stacked spectra reveal prominent star-forming features, highlighting difficulties in interpreting their accretion properties. Our results demonstrate the power of large spectroscopic samples to characterise the radio-source population, providing a foundation for studies in the SKA era.
[abstract 32 / 42] (score: 2) - Title: Compact Objects Merging with Stars as an Origin of Ultra-Long Gamma-Ray Bursts and Luminous Fast Blue Optical TransientsAuthors: V. Ashley Villar, Anya E. Nugent, Eric Burns, Brian D. Metzger, Tarraneh Eftekhari, Jakub Klencki, Christopher L. Fryer,Comments: submitted to ApJL; comments welcomeSubjects: astro-ph.HECreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
Ultra-long GAMMA-RAY BURSTs (ULGRBs) and luminous fast blue optical transients (LFBOTs) are two rare classes of engine-driven transients whose physical connection remains unknown. It has been suggested that both may arise from the mergers of a massive helium core with a compact object. We investigate this common origin by reanalyzing the optical counterpart of the highly unusual GRB 111209A/SN 2011kl associated with an ULGRB in the context of a recently developed, analytical LFBOT model. We find that SN 2011kl is broadly consistent with an LFBOT origin, exhibiting a rapid, luminous and blue early emission. However, compared to the LFBOT population, SN~2011kl features a longer "plateau" of emission ~2 weeks post-merger, suggesting an extended pre-merger mass-loss history, as well as stronger UV suppression. We additionally compare the host galaxy environments of five ULGRBs to those of LFBOTs and classical LGRBs. We find that ULGRBs, similar to LFBOTs and long GRBs, tend to occur in lower mass (<10^10 solar masses) galaxies with higher amounts of active STAR FORMATION than observed for field galaxy populations at similar redshifts. Together, these results support a shared progenitor for at least a subset of ULGRBs and LFBOTs.
[abstract 33 / 42] (score: 2) - Title: Analysis of collisional and facility effects in a MAGNETic nozzle plasma expansionAuthors: Manuel Cortés-Hernán, Mario Merino, Diego García-Lahuerta, Eduardo Ahedo,Comments: 36 pages, 10 figuresSubjects: physics.plasm-phCreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
An axisymmetric, quasineutral three-fluid model is proposed to study the plasma expansion in a MAGNETic nozzle under the presence of neutrals coming either from the plasma source or as an homogeneous background. As a difference with other models, electron cooling in the plume is achieved by treating the electron energy flux as mainly convective and without the need to postulate any anomalous resistivity. Solutions are presented for the electron high-MAGNETization limit, in which the electron main magnitudes can be integrated along MAGNETic lines. Ionization, elastic and charge-exchange collisions with neutrals do not change the main qualitative features of the plasma expansion, known from previous collisionless models. Ionization enhances the plasma flow in the nozzle, and leads to additional electron cooling, which decreases the electric potential fall along the nozzle. The efficiency of the nozzle is quantified in terms of the gain of MAGNETic thrust and the plume divergence angle. Two types of boundary conditions are discussed for the electron flow: local current ambipolarity conditions at the nozzle throat and global current-free conditions at the outer boundary (i.e., metallic vacuum chamber walls). These last ones are shown to be physically more reliable: they introduce the influence of the chamber walls on the plasma expansion by shaping the ambipolar electric field; they permit the extrapolation to undisturbed free space conditions; and they approximate better experimental trends with the background pressure.
[abstract 34 / 42] (score: 2) - Title: Alcock-Paczynski Blinding Scheme for the Ly-$α$ Forest AnalysisAuthors: G. Perez-Sanchez, S. F. Beltran, G. Niz, S. Brieden, L. Verde, A. Font-Ribera, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. Cuceu, A. de la Macorra, B. Dey, P. Doel, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, D. Huterer, M. Ishak, R. Joyce, A. Kremin, O. Lahav, A. Lambert, M. Landriau, L. Le Guillou, M. Manera, P. Martini, R. Miquel, S. Nadathur, N. Palanque-Delabrouille, W. J. Percival, F. Prada, I. Pérez-Ràfols, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver,Comments: 30 pages, 15 figuresSubjects: astro-ph.COCreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
We present and validate a blinding method for the Lyman-$α$ (Ly$α$) forest analysis based on a modification of the Alcock-Paczynski test. In order to hide the background expansion history, the method employs a geometrical shift of each QUASAR (QSO) forest in wavelength space, once the QUASAR continuum has been fitted and the fluctuation field is extracted. The redshift positions for the QSO sample are also changed in a consistent manner. We show that the method remains effective when applied to real data, where contamination from metals and Lyman-$β$ is intrinsically mixed with the Lyman-$α$ forest. This limitation is primarily visible in the 1D correlation function, where other blinding strategies can mitigate the effect. To assess its effectiveness, the prescription is tested against a series of datasets of increasing complexity: from idealized low-noise mocks, to realistic DESI year one synthetic datasets, and finally to data from DESI first data release (DR1), using both the auto (Ly$α\times$Ly$α$) and cross (Ly$α\times$ QSO) correlations. We find that the method robustly shifts the BAO peak position from the 3D correlation functions to the expected value for cosmology changes of around 5\% in the matter content, without altering the shape of the posteriors in the model parameters. In conclusion, this catalog-level blinding strategy is a viable method for cosmological inference with the Lyman-$α$ forest, particularly if a cross-analysis with other tracers using the same blinding strategy is pursued.
[abstract 35 / 42] (score: 2) - Title: Nonlinear hydrodynamics in spinning neutron stars: Theoretical universal relations and equilibrium solutionsAuthors: Hang Yu, Giorgio Nicolini, Shu Yan Lau, K. J. Kwon, Tejaswi Venumadhav, Nils Andersson, Pantelis Pnigouras, Fabian Gittins, Amlan Nanda,Comments: 37 pages, 11 figures, to be submittedSubjects: gr-qc astro-ph.HECreated: 2026-07-08; Updated: 2026-07-10; Datestamp: 2026-07-10
We study tides during the inspiral of a binary neutron star (BNS) system, including nonlinear hydrodynamical interactions. Using an affine approximation that treats the perturbed NS as an ellipsoid, we analytically derive coupling coefficients among the f-modes and the radial mode to the four-wave order (i.e., next-to-next-to-leading order) in the Hamiltonian, allowing for arbitrary rotation of the background star. Our model reveals a series of universal relations from first-principles arguments. Besides the well-known relations, we show that the three-wave (next-to-leading-order) interaction coefficients are fully determined by the properties of the linear tide. Therefore, they do not probe new physics of the NS. Nonetheless, not including the three-wave nonlinear tides can lead to significant systematic errors in the gravitational waveform. We support this claim via a hybrid approach that simultaneously captures mode resonances expected in Newtonian hydrodynamics and is consistent with RELATIVISTIC calculations in the low-frequency expansion. The nonlinear tide in a single NS can cause a phase shift of around 1.7 radians accumulated up to merger compared to the linear tide model; for a binary of similar masses, the phase shift is approximately doubled. Our calculation extends to four-wave interactions, which, for a slowly spinning NS, provide only small corrections and are subdominant compared to the tidal back-reaction on the orbit. For a rapidly rotating NS, the nonlinear centrifugal drive of the f-mode and the four-wave anharmonicity provides a window to study the adiabatic exponent related to internal buoyancy that cannot be probed by the linear and three-wave tides in slowly spinning systems. The anharmonicity cannot lead to resonance locking of the f-mode.
[abstract 36 / 42] (score: 2) - Title: Spectroscopic structure of Non-Hermitian $\mathcal{PT}$-Symmetric Klein--Gordon Fields in a Magnetized Cosmic String SpacetimeAuthors: Omar Mustafa, Abdullah Guvendi,Comments: 7 pages, 1 FigureSubjects: gr-qcCreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
We investigate non-Hermitian $\mathcal{PT}$-symmetric Klein--Gordon (KG) fields in a MAGNETized cosmic string spacetime. A complex non-minimal scalar interaction, $\mathcal{F}_μ=(0,\mathcal{F}_{r},0,0)$ with $\mathcal{F}_{r}=ωr+ib\in\mathbb{C}$, indulged with a MAGNETic charge $q=ie$, is shown to introduce an effective $\mathcal{PT}$-symmetric Klein--Gordon oscillator supplemented by complex Coulombic and linear interactions. The resulting radial equation is shown to be conditionally exactly solvable using a biconfluent Heun series-to-polynomial approach. To observe non-Hermitian \(\mathcal{PT}\) symmetrization, we compare with the Hermitian counterpart by mapping $e=-i\tilde e \Rightarrow q\in \mathbb R$ and $b=-i\tilde b \Rightarrow \mathcal F_r\in \mathbb R$. In the limiting case $ω=0$, the system is shown to reduce to an exactly solvable non-Hermitian \(\mathcal{PT}\) symmetric Coulomb-type KG equation using confluent hypergeometric series/polynomials. Hereby, for both \(\mathcal{PT}\) symmetric models considered, we show that non-Hermitian \(\mathcal{PT}\) symmetrization introduces an upper limit for the allowed energies, unlike the corresponding Hermitian cases. These results provide an analytically tractable framework for exploring non-Hermitian RELATIVISTIC quantum fields in curved spacetimes and demonstrate the role of $\mathcal{PT}$-symmetry in regulating the allowed spectrum.
[abstract 37 / 42] (score: 2) - Title: A Magnetar Engine and Circumstellar Medium Interaction: Synergistic Effects in Producing Superluminous SupernovaeAuthors: Guang-Lei Wu, Yun-Wei Yu, Liang-Duan Liu,Comments: 18 pages, 9 figures, 2 tables, accepted for publication in ApJSubjects: astro-ph.HECreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
Superluminous SUPERNOVAe (SLSNe) are often modeled as being powered either by a central engine or by strong interaction with dense circumstellar material (CSM). These two mechanisms may be dynamically coupled if the ejecta interact with dense CSM while being energized by a newborn MAGNETar. We develop a semi-analytical hybrid model that follows the coupled dynamics, energy conversion, and radiative output of such systems. A rapidly rotating MAGNETar injects energy through a RELATIVISTIC wind, inflating a hot bubble inside the expanding ejecta. Part of the injected energy is stored as radiation, while the rest is converted into bulk kinetic energy of the swept-up ejecta. At the same time, the outer ejecta collide with the surrounding CSM and form a circumstellar interaction (CSI) region. As the shock driven by the MAGNETar accelerates through the ejecta, it can catch up with the CSI region and take over the subsequent interaction with the unshocked CSM. The emergent light curves are therefore governed by the coupled effects of MAGNETar energy injection, shock heating, and radiative diffusion. We show that this hybrid model can produce diverse SLSN light-curve morphologies, including luminous interaction-powered peaks, asymmetric post-peak declines, and late-time emission sustained by delayed leakage of MAGNETar-powered radiation. The model provides a plausible way to reduce the extreme nickel-mass or initial explosion-energy requirements often encountered in purely radioactive or purely interaction-powered interpretations.
[abstract 38 / 42] (score: 2) - Title: Sensitivity of a low-shear heliotron configuration to localised ferrite perturbationsAuthors: A. Matsuyama, Y. Nakamura, S. Inagaki, F. Tanji, Yusuke Yamashita, Akihisa Yamamoto, S. Kobayashi, F. Kin, S. Kado, S. I. Inagaki, S. Konoshima, T. Mizuuchi, K. Nagasaki,Comments: 18 pages, 13 figuresSubjects: physics.plasm-phCreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
The influence of ferritic steel on low-shear stellarator/heliotron MAGNETic configurations is investigated for the Heliotron J device using a point dipole MAGNETisation model. By numerically evaluating ferritic steel plates assumed at several locations inside the Heliotron J vacuum vessel, the changes in the rotational transform and MAGNETic island width are shown to be sensitive to the installation location. This sensitivity arises from the coupling between the background nonaxisymmetric field and ferrite perturbation, rather than being determined solely by the perturbation amplitude. Ferritic steel plates placed on the outer side of a straight section produce the most significant changes in the MAGNETic topology and exhibit the highest sensitivity to violations of the $M = 4$ toroidal periodicity. Additionally, we show that appropriate arrangements of passive MAGNETic dipoles can reduce the effective helical ripple while preserving the vacuum MAGNETic well depth in Heliotron J, and can induce stellaratorasymmetric boundary perturbation in low-field experiments near the ferrite saturation threshold.
[abstract 39 / 42] (score: 2) - Title: Precision three-Dimensional Atmospheric Neutrino Flux Calculation Based on Honda Flux ModelAuthors: Jie Cheng, Yu-Feng Li, Liang-Jian Wen,Comments: 47 pages, including an appendix, with 22 figures. The flux model data is available at https://github.com/JIECheng2021/atm_nu_flux_dataSubjects: hep-ph astro-ph.HE hep-exCreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
We present a comprehensive three-dimensional atmospheric neutrino flux calculation based on the well-recognized simulation framework develeped by Honda and his collaborators, incorporating for the first time the muon propagation inside the Earth and its subsequent decay or nuclear capture. Other updates of essential input models include: the AMS02-based primary COSMIC RAY model, IGRF2020 geoMAGNETic field, and muon-recalibrated hadronic interaction model. The calculation covers seven detector sites across diverse geoMAGNETic environments, spanning 10~MeV to $10^4$~GeV. Significant site-dependent differences appear at $E_ν< 10$~GeV, with $ν_μ$ flux at IceCube approximately twice that at JUNO below 1~GeV. Compared to HKKMS15, deviations of 2\%--10\% are attributed to the updated input models. Below 100~MeV, we present precise flux results, revealing that muon propagation contributes a globally significant component to the low-energy neutrino flux at all sites, with an approximately site-independent absolute increment. The hadronic uncertainty is re-estimated across the energy range using the updated hadronic interaction model, with significant reduction of the systematic error compared to previous calculations. These results provide essential inputs for neutrino oscillation and rare-event search experiments including JUNO, Super-Kamiokande/Hyper-Kamiokande, DUNE, KM3NeT/ORCA, and IceCube, as well as direct DARK MATTER detection experiments facing the neutrino fog.
[abstract 40 / 42] (score: 2) - Title: Classification of BLAZARs based on data-driven approachesAuthors: Simone Vaccaro, Maria Isabel Carnerero, Claudia M. Raiteri, Massimo Brescia, Ylenia Maruccia, Natale De Bonis, Giuseppe Riccio, Stefano Cavuoti,Comments: 11 pages, 7 figures. Published online on Astronomy and Astrophysics on 03/07/2026Subjects: astro-ph.GA astro-ph.IMCreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
Active galactic nuclei (AGNs), including BLAZARs, exhibit distinctive variability in their optical light curves, making them ideal for classification studies. This work uses data from the latest GAIA and Pan-STARRS data releases to analyze these patterns. The goal of this work is to classify AGNs into two categories: "BLAZARs" and "non-BLAZARs'' using only optical light curves. This strategy differs from most existing works, as it relies exclusively on optical variability without employing any other multiwavelength information. We processed optical light curves from GAIA and Pan-STARRS using the FATS library to extract standard time-series features. We computed additional features with custom algorithms based on literature methods. A Light Gradient-Boosting Machine (LightGBM) model was trained to classify AGNs into BLAZARs and non-BLAZARs based on these features. We then used this knowledge base to carry out a self-learning experiment with AGN candidates of an unknown nature. The LightGBM model achieved an accuracy of $86\%$, with precision, recall, and F1 score above $80-85\%$ for classifying BLAZARs and non-BLAZAR AGNs using optical data. The application of a BoostBoruta algorithm for feature selection reduced the feature space from 70 to 13. while maintaining comparable performance. A self-training classifier yielded similar results $85\%$, confirming the robustness of the model and the reliability of pseudo-labeling for unknown objects.
[abstract 41 / 42] (score: 2) - Title: Active galactic nuclei are not responsible for systematics in the empirical properties of type Ia SUPERNOVAeAuthors: Peter Clark,Comments: Published in RNAAS - This is an author compiled version. 3 Pages, 1 FigureSubjects: astro-ph.HECreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
Despite being key cosmological anchors, the empirical properties of Type Ia SUPERNOVAe (SNe Ia) remain subject to significant systematic uncertainties, the largest of which being their astrophysics and how this is linked to their environment. The relative importance of these uncertainties will grow as larger observational samples reduce statistical uncertainties. Here I explore if the presence of an ACTIVE GALACTIC NUCLEus (AGN) within a portion of SN Ia host galaxies could be one such systematic uncertainty. With the ZTF SNe Ia DR2 sample I find that, in the low redshift regime (z < 0.15), the presence of AGNs in some SN Ia hosts does not produce a significant systematic effect on their measured Hubble residuals.
[abstract 42 / 42] (score: 2) - Title: SACRA-K: A Performance-Portable Numerical Relativity Code with KokkosAuthors: Ming-Zhe Han, Kenta Kiuchi, Masaru Shibata,Comments: 15 pages, 8 figuresSubjects: astro-ph.HE astro-ph.IM gr-qcCreated: 2026-07-09; Updated: 2026-07-10; Datestamp: 2026-07-10
We present SACRA-K (SimulAtor for Compact objects in Relativistic Astrophysics with Kokkos), a performance-portable numerical relativity code ported from the Fortran code SACRA-MPI to C++ with the Kokkos library. SACRA-K retains the physics and numerical methods of SACRA-MPI, namely a Baumgarte-Shapiro-Shibata-Nakamura (BSSN) spacetime evolution with Z4c constraint propagation and a box-in-box Berger-Oliger adaptive mesh refinement, together with the high resolution shock capturing scheme for the general RELATIVISTIC hydrodynamics from NANASI, while gaining cross vendor portability. We validate the port against SACRA-MPI across binary BLACK HOLE, BLACK HOLE neutron star, and binary neutron star configurations. Across these tests, the waveform discrepancies are well below both the scatter among independent numerical relativity codes and the resolution dependent variation within a given code, and remain at or below the distinguishability threshold of current gravitational-wave detectors; the $π$ symmetry is preserved exactly at the bitwise level; and the gravitational wave phase of the binary neutron star merger exhibits second order convergence. In the smallest test configuration, SACRA-K runs about an order of magnitude faster on the NVIDIA A100 GPU cluster or the AMD MI300A APU cluster than the Fortran SACRA-MPI on the CPU cluster, and we measure its scaling up to 256 accelerator devices.
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