Current date: 2026-08-06
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Scoring abstracts
Number of records retrieved: 615
Keyword score statistics
score 12 -- 1 abstracts
score 9 -- 1 abstracts
score 8 -- 2 abstracts
score 7 -- 1 abstracts
score 6 -- 2 abstracts
score 5 -- 3 abstracts
score 4 -- 5 abstracts
score 3 -- 5 abstracts
score 2 -- 11 abstracts
in total -- 31 abstracts
Articles that appeared on 2026-08-06
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[abstract 1 / 31] Wow! (score: 12)
- Title: A precessing JET from a supermassive BLACK HOLE: multi-wavelength observations of S5 1044+71Authors: M. Cerruti, P. A. Duverne, G. Ganesaratnam, P. Goswami, H. X. Ren, N. Sahakyan,Comments: In press in JHEAP. Abstract abridgedSubjects: astro-ph.HECreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
The bright gamma-ray BLAZAR S5 1044+71 has been identified as showing very significant quasi-periodic oscillations in the FERMI-LAT data in recent studies, with a periodicity of about 3 years. With the completion of a new gamma-ray cycle, we aim to revisit the periodicity in FERMI-LAT data, and analyze all available multi-wavelength (MWL) data to search for possible correlations and time-lags. These observations will be used to test for the compatibility of the observed periodicity with a precessing JET from the supermassive BLACK HOLE. We analyze data from FERMI-LAT, NUSTAR, SWIFT, AstroSat, ASAS-SN, ZTF, Pan-STARRS, and NEOWISE. In addition we present an analysis from historical observations from Palomar and Pulkovo. Single-band spectral variability, MWL correlations, and cross-correlations are computed. We then model the FERMI-LAT light curve with a precessing JET model, providing constraints on the geometry of the system and the evolution of the Doppler factor. The latter is used as a geometrical constraint in the modeling of the spectral energy distributions. We confirm previous claims on the existence of a periodic gamma-ray signal. We detect significant spectral variability in gamma-ray, X-rays, and optical/UV data. We detect significant correlation between low-energy (infrared/optical/ultraviolet) data and gamma-rays, with a correlation index of about 1; the correlation between X-rays and gamma-ray is milder, with a correlation index of about 0.3. We do not detect any significant time-lag between bands. The FERMI-LAT light curve is successfully fit by a precessing JET model. The fit to the spectral energy distributions indicate that S5 1044+71 is a typical BLAZAR, in which the gamma-ray emission is located beyond the broad-line region. All MWL observations we present in this work are consistent with the existence of a precessing RELATIVISTIC JET from the supermassive BLACK HOLE.
[abstract 2 / 31] Wow! (score: 9) - Title: Modeling the imprints of large-scale MAGNETized structures on $γ$-rays from extragalactic transientsAuthors: Saikat Das, Soebur Razzaque, Nestor Mirabal, Nicola Omodei, Kohta Murase, Israel Martinez-Castellanos,Comments: 15 pages, 7 figures, accepted for publication in ApJSubjects: astro-ph.HECreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
In the multimessenger era, the association of high-energy transients with their $γ$-ray counterparts can be obscured by MAGNETized large-scale structure surrounding the source. We analyze models for delayed off-axis $γ$-rays, arising from the injection of ultrahigh-energy COSMIC RAYs ($E\gtrsim 10^{18}$ eV) and $γ$-rays ($\varepsilon_γ\gtrsim10^{18}$ eV), and very-high-energy $γ$-rays ($\varepsilon_γ\gtrsim 100$ GeV) from the transient. As a representative case, we consider the brightest GAMMA-RAY BURST, GRB~221009A, embedded in a MAGNETized structure. We examine charged-particle deflection in electroMAGNETic cascades, followed by propagation of secondaries through the intergalactic medium, and derive the time delays and angular offsets of the resulting $γ$-rays. To test the models, we analyze 1.25 years of post-event \textit{FERMI} Large Area Telescope (LAT) data and construct a 1 GeV -- 1 TeV test statistic (TS) map within $10^\circ$ of the burst localization. We find two sub-threshold peaks with TS$\geq9$. The more significant peak, J1911.8+2044, shows $γ$-ray emission in pre-burst LAT data, while J1913.2+1901 coincides with a 664.6 GeV $γ$-ray recorded $\sim191.9$ days after the trigger at $\approx 0^{\circ}.75$ from the GRB. The corresponding flux upper limit provides a fiducial value for constraining the parameter space in our models and estimating the source energy requirement for delayed off-axis signals. Although a MAGNETized structure can reproduce the angular offset of this sub-threshold feature, the resulting time delay disfavors an origin in this GRB.
[abstract 3 / 31] Wow! (score: 8) - Title: Different Jet Dissipation Mechanisms Underlying the Variability in BlazarsAuthors: Hong-bin Tan, Ruo-yu Liu,Comments: 18 pages, 9 figuresSubjects: astro-ph.HECreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
Blazars are among the most extreme classes of ACTIVE GALACTIC NUCLEi. They are powered by RELATIVISTIC JETs, but the way in which the JET energy is dissipated is still unclear. The flat radio spectrum and the core-shift effect trace the distributions of MAGNETic fields and RELATIVISTIC particles along the JET, while variability carries information about time-dependent dissipation. However, a unified framework connecting these observables to the underlying JET physics has been lacking. Here we present a multi-frequency analysis of the prototypical BLAZAR Mrk~501. We model its core-shift measurements, spectral energy distributions (SEDs), and power spectral densities (PSDs) with a conical JET model that conserves MAGNETic power. The core-shift data localize the radio emitting regions and constrain the electron-density and dissipation-rate profiles along the JET. With a single radial distribution of JET parameters, the model reproduces the core-shift relation and SED, but it underpredicts the observed variability at high radio frequencies and in the optical to $γ$-ray bands. We therefore introduce different blob distributions for the inner ($\lesssim$~0.1\,pc) and outer ($\gtrsim$~0.1\,pc) JET regions. With this extended model, the simulated PSDs are consistent with the multiwavelength observations of Mrk~501 during its 2017--2019 low state. This result points to different dissipation behavior in the inner and outer JET. Our study demonstrates that spectro--timing--astrometric JET modeling, which combines SEDs, multiwavelength PSDs, and radio core-shift measurements, can constrain JET stratification and scale-dependent dissipation in BLAZARs.
[abstract 4 / 31] Wow! (score: 8) - Title: The most extreme high-z radio QUASARs in the eRASS:1 X-ray surveyAuthors: L. Ighina, L. Palmieri, L. N. Martínez-Ramírez, A. Caccianiga, T. Connor, A. Moretti, B. Arsioli, Y. Beletsky, E. Marini, A. Rossi,Comments: Accepted for pubblication on MNRAS 2026 August 04, Submitted 2026 May 25Subjects: astro-ph.GA astro-ph.HECreated: 2026-08-04; Updated: 2026-08-06; Datestamp: 2026-08-06
We present the selection and identification of high-z radio QUASARs from a combination of X-ray (eROSITA All-Sky Survey), optical/NIR (DECam Local Volume Exploration), and radio (Rapid ASKAP Continuum Survey) surveys. After building a sample of 68 new high-z QUASAR candidates, we performed follow-up spectroscopic observations on 46 sources, confirming 39 to have redshifts z>3.5. For the subset of radio QUASARs at z>4, the 14 new sources identified here represent an increase of $\sim$65% in the known population of objects above the same flux limits in the same area. Using X-ray-to-optical relative intensity, we identified BLAZARs in our sample, which we then used to compare the total number of z>4, X-ray selected BLAZARs to the predictions of a fractional IC/CMB model previously proposed in the literature. Overall we find a relatively good agreement, even considering the potential biases in the redshift distribution from the incompleteness of the spectroscopic follow-up and the BLAZAR classification criteria. The sources presented in this work represent a sample well suited for investigating the evolution of the most extreme systems in the early Universe, including their RELATIVISTIC JETs and accretion properties
[abstract 5 / 31] Wow! (score: 7) - Title: Spherically Polarized Alfvén Waves and the Gosling BoostAuthors: Yuliang Ding, Marco Velli, Zesen Huang, Chen Shi, Lorenzo Matteini, Nikos Sioulas, Stuart D. Bale, Anna Tenerani, Mingzhe Liu,Comments: 12 pages, 6 figuresSubjects: astro-ph.SR physics.plasm-phCreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
Alfvén waves are thought to play critical roles in solar wind acceleration and plasma heating in the solar corona and inner heliosphere. Parker Solar Probe (PSP) has highlighted the role of large amplitude Spherically Polarized Alfvén Waves (SPAWs), where the locally constant MAGNETic field magnitude $|\mathbf{B}|$ together with outward propagation explains the observed one sided radial velocity enhancement - the Gosling boost. Starting from the MHD equations, we derive the modified wave pressure and Poynting flux under the SPAW condition, and demonstrate both are governed solely by the transverse MAGNETic fluctuations. Using PSP data from Encounters 6--25, we define an unperturbed velocity baseline from the lower 10th-percentile running average and statistically characterize the radial evolution of Alfvénic fluctuations. The background solar wind velocity shows clear radial acceleration, while the velocity perturbation amplitude $δv$ decreases with heliocentric distance. This decay is anisotropic between the radial and perpendicular directions, which is a direct consequence of the growing MAGNETic deflection angle related to the spherical POLARIZATION. Our results demonstrate that radial velocity enhancements in the young solar wind arise naturally from SPAWs rather than from localized velocity JETs, and provide direct observational evidence for the anisotropic radial evolution of SPAWs in the inner heliosphere.
[abstract 6 / 31] Yes (score: 6) - Title: Insights on the Gamma-Ray Bursts variability in their cosmological rest frameAuthors: Giovanni Della Casa, Fabrizio Fiore, Giuseppe Dilillo, Simonetta Puccetti, Andrea Vacchi,Comments: 12 pages, 18 figures Submitted to A&A. Revised versionSubjects: astro-ph.HECreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
Gamma-ray bursts temporal profile can be extremely variable, going from a single pulse of a few seconds duration to multiple superimposed pulses occurring over tens or even hundreds of seconds. The variability displayed in the lightcurve of each GAMMA-RAY BURST can be the result of the activity taking place in the central engine that generates these violent phenomena, as well as due to MAGNETic RECONNECTion activities at larger distances. The objective of this work is to find the shortest variability hidden in the lightcurves of the GRBs, with particular focus for the ones with measured redshift, on timescales as short as few milliseconds. This variability will then be related to physical characteristics of the central engine, and evidences of its relation with the spectral parameters of the burst, such as the isotropic energy and peak energy, will be presented. This research is even more relevant in view of the future generation of satellites with improved timing resolution, that will allow us to explore the possible variability in the microsecond region.
[abstract 7 / 31] Yes (score: 6) - Title: A Real-Time Jet Laboratory in SWIFT J1727.8-1613Authors: Callan M. Wood, James C. A. Miller-Jones, Arash Bahramian, Steven J. Tingay, Sara E. Motta, Hongmin Cao, Thomas D. Russell, Francesco Carotenuto, Pikky Atri, Diego Altamirano, Alexandra J. Tetarenko, Rob Fender, Elmar Körding, Dipankar Maitra, Sera Markoff, David M. Russell, Gregory R. Sivakoff, Roberto Soria, Valeriu Tudose,Comments: 26 pages, 19 figures, 5 tables. Accepted for publication by PASASubjects: astro-ph.HECreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
We present the results of our intensive VLBI campaign on the black-hole low-mass X-ray binary (LMXB) SWIFT J1727.8-1613 during its 2023-2024 outburst. We observed the repeated quenching and re establishment of the highly-extended continuous JET during several transitions between hard-intermediate and soft-intermediate states, and the repeated ejection of transient JETs. Using time-dependent visibility model fitting, we tracked the motion of nine discrete JET knots, obtaining some of the most precise measurements of transient JET proper motions and ejection dates in an LMXB. These ejecta were only detectable for a short time with VLBI, and some showed rapid intra-observation flux density variability that was not captured in image reconstructions. For the first time, we use time-dependent visibility modelling to fit a piecewise model for the JET knot flux densities, allowing us to create complex, non-parametric light curves of their intra-observation variability. We observed the launching of multiple ejecta across several state transitions, however, we could not identify a consistent signature of JET ejection in the available X-ray intensity or hardness data. We constrained the intrinsic speeds and bulk Lorentz factors of the JET knots, finding that SWIFT J1727.8-1613 launched both mildly RELATIVISTIC and highly RELATIVISTIC ejecta throughout its outburst. We used their proper motions to constrain a posterior distribution for the maximum inclination angle of the JET axis, which had 50th, 84th, and 99th percentiles of 40°, 50°, and 66°, respectively. These unique observations of the repeated ejection of transient JETs by a single LMXB reveal that fixed parameters such as black-hole mass, black-hole spin, and spin-orbit misalignment do not uniquely determine the varying properties of transient JETs, particularly their speeds and Lorentz factors.
[abstract 8 / 31] Yes (score: 5) - Title: GWTC-5.0: Constraints on the Cosmic Expansion Rate and Modified Gravitational-wave PropagationAuthors: The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration, A. G. Abac, A. Abe, I. Abouelfettouh, F. Acernese, K. Ackley, A. Adam, S. Adhicary, D. 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, L. Albers, W. Ali, S. Al-Kershi, C. Allene, A. Allocca, S. Al-Shammari, J. A. Alvarez, S. Alvarez-Lopez, W. Amar, O. Amarasinghe, A. Amato, F. Amicucci, C. Amra, A. B. Anand, C. Anand, A. Ananyeva, S. B. Anderson, W. G. Anderson, M. Andia, M. Ando, F. Andrade-Oliveira, M. Andrés-Carcasona, J. L. Andrey, T. Andrić, J. Anglin, J. Anna, J. M. Antelis, S. Antier, T. Aoki, M. Aoumi, E. Z. Appavuravther, E. A. Appelt, 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, P. S. Aswathi, F. Attadio, F. Aubin, K. AultONeal, G. Avallone, N. Avdeev, E. A. Avila, S. Babak, C. Badger, S. Bae, S. Bagnasco, S. Baimukhametova, L. Baiotti, T. Baka, K. A. Baker, T. Baker, G. Balbi, G. Baldi, N. Baldicchi, M. Ball, G. Ballardin, M. Ballelli, 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, 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, J. C. Bayley, A. C. Baylor, P. A. Baynard, M. Bazzan, V. M. Bedakihale, F. Beirnaert, M. Bejger, A. S. Bell, C. Bellani, D. S. Bellie, D. Beltran-Martinez, E. Benedetti, W. Benoit, I. Bentara, M. Ben Yaala, S. Bera, F. Bergamin, B. K. Berger, M. Beroiz, C. P. L. Berry, I. Berry, D. Bersanetti, T. Bertheas, A. Bertolini, J. Betzwieser, D. Beveridge, N. Bevins, J. Bezerra-Sobrinho, R. Bhandare, R. Bhatt, A. Bhattacharjee, D. Bhattacharjee, S. Bhattacharyya, S. Bhaumik, V. Biancalana, F. Bianchi, I. A. Bilenko, M. Bilicki, G. Billingsley, A. Binetti, S. Bini, 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, M. Bloch, N. Bode, N. Boettner, P. Bogdan, G. Boileau, M. Boldrini, G. N. Bolingbroke, L. D. Bonavena, 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, T. D. Boybeyi, 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, D. D. Brown, M. L. Brozzetti, S. Brunett, G. Bruno, R. Bruntz, J. Bryant, Y. Bu, F. Bucci, A. Buchicchio, A. Buggiani, O. Bulashenko, T. Bulik, H. J. Bulten, A. Buonanno, K. Burtnyk, R. Buscicchio, N. Busdon, D. Buskulic, R. L. Byer, R. Cabrita, V. A. Cáceres-Barbosa, L. Cadonati, G. Cagnoli, C. Cahillane, A. Calafat, J. Calderón Bustillo, J. D. Callaghan, T. A. Callister, E. Calloni, S. R. Callos, K. Cannon, V. Cantory, H. Cao, L. A. Capistran, E. Capocasa, G. Capoccia, E. Capote, C. Capuano, G. Capurri, F. Carbognani, K. J. Cardona-Martínez, M. Carlassara, M. Carpinelli, G. Carrillo, G. Carullo, A. Casallas-Lagos, J. Casanueva Diaz, C. Casentini, S. Caudill, M. Cavaglià, R. Cavalieri, A. Ceja, G. Cella, P. Cerdá-Durán, E. Cesarini, N. Chabbra, W. Chaibi, A. Chakraborty, P. Chakraborty, S. Chakraborty, S. Chalathadka Subrahmanya, C. Chan, J. C. L. Chan, M. Chan, C. -Y. Chang, K. Chang, S. Chao, C. Chapman-Bird, P. Charlton, E. Chassande-Mottin, C. Chatterjee, Debarati Chatterjee, Deep Chatterjee, M. Chaturvedi, S. Chaty, K. Chatziioannou, A. Chen, A. H. -Y. Chen, D. Chen, H. Chen, H. Y. Chen, S. Chen, Yanbei Chen, Yiwen 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, A. Chiummo, A. Chopra, C. Chou, S. Choudhary, N. Christensen, Y. K. Chu, S. S. Y. Chua, G. Ciani, P. Ciecielag, M. Cieślar, M. Cifaldi, B. Cirok, F. Clara, J. A. Clark, T. A. Clarke, A. Claveus, M. R. Claypool, S. Clesse, F. Cleva, S. M. Clyne, E. Coccia, E. Codazzo, P. -F. Cohadon, D. E. Cohen, E. Colangeli, O. Cole, M. Colleoni, C. G. Collette, J. Collins, S. Colloms, A. Colombo, G. Compère, C. M. Compton, G. Connolly, L. Conti, T. R. Corbitt, I. Cordero-Carrión, S. Corezzi, N. J. Cornish, A. Corsi, S. Cortese, L. A. Corubolo, L. Cotnoir, R. Cottingham, J. A. Cotturone, M. W. Coughlin, P. Couvares, R. Coyne, A. Cozzumbo, J. D. E. Creighton, T. D. Creighton, S. Crook, R. Crouch, J. Csizmazia, K. Csukás, T. J. Cullen, A. Cumming, E. Cuoco, M. Cusinato, R. R. Cuzinatto, L. V. da Conceição, T. Dal Canton, S. Dall'Osso, S. Dal Pra, G. Dálya, Y. Dang, B. D'Angelo, S. Danilishin, O. Danner, S. D'Antonio, K. Danzmann, K. E. Darroch, L. P. Dartez, R. Das, S. Das, A. Dasgupta, L. Datrier, V. Dattilo, A. Daumas, I. Dave, A. Davenport, T. F. Davies, D. Davis, M. C. Davis, P. Davis, E. J. Daw, M. Dax, J. De Bolle, E. deBruin, 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, C. de Melo, N. Demos, T. Dent, A. Depasse, N. DePergola, R. De Pietri, R. De Rosa, C. De Rossi, E. K. Derrick, M. Desai, D. DeSantis, S. Deshmukh, V. Deshmukh, R. De Simone, S. Determan, S. Dhage, A. Dhani, R. Dhatri, R. Dhurkunde, R. Diab, C. Diaz, M. C. Díaz, F. Diaz Guerra, M. Di Cesare, M. A. Dicorato, T. Dietrich, C. Di Fronzo, M. Di Giovanni, 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, S. Doravari, O. Dorosh, F. Dosopoulou, M. Drago, J. C. Driggers, M. Dubois, R. S. Dumbreck, U. Dupletsa, D. D'Urso, P. Dutta Roy, H. Duval, S. Dwivedi, S. E. Dwyer, C. Eassa, M. Eberhardt, M. Ebersold, M. Ebiri, G. Eddolls, A. Effler, J. Eichholz, H. Einsle, M. Eisenmann, M. Emma, K. Endo, R. Enficiaud, V. Ernst, L. Errico, R. Espinosa, M. Esposito, R. C. Essick, H. Estellés, T. Etzel, M. Evans, T. Evstafyeva, 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, A. Feo, J. Fernandes, T. Fernandes, G. Fernández Rodríguez, D. Fernando, S. Ferraiuolo, T. A. Ferreira, M. Ferrer-Martinez, F. Fidecaro, P. Figura, I. Fiori, M. Fishbach, R. P. Fisher, S. K. Fitzgerald, V. Fiumara, R. Flaminio, B. Flanagan, S. M. Fleischer, L. S. Fleming, F. Flocco, E. Floden, H. Fong, J. A. Font, F. 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Goode, A. Goodwin-Jones, M. Gosselin, S. M. Goss-Grubbs, C. Gostiaux, R. Gouaty, D. W. Gould, D. Goupilliere, K. Govorkova, A. Grado, V. Graham, A. E. Granados, M. Granata, V. Granata, S. Gras, P. Grassia, C. Gray, R. Gray, G. Greco, A. C. Green, L. Green, S. R. Green, A. M. Gretarsson, E. M. Gretarsson, D. Griffith, C. Grimaud, H. Grote, S. Grunewald, A. G. Guerrero, G. M. Guidi, T. Guidry, H. K. Gulati, F. Gulminelli, H. Guo, W. Guo, Y. Guo, A. Gupta, I. Gupta, N. C. Gupta, S. K. Gupta, V. Gupta, N. Gupte, N. Guttman, F. Guzman, M. Haberland, S. Haino, E. D. Hall, E. Z. Hamilton, G. Hammond, W. -B. Han, M. Haney, J. Hanks, C. Hanna, M. D. Hannam, O. A. Hannuksela, H. Hansen, J. Hanson, R. Harada, A. R. Hardison, S. Harikumar, K. Haris, I. Harley-Trochimczyk, J. Harms, G. M. Harry, I. W. Harry, M. T. Hartman, B. Haskell, C. -J. Haster, K. Haughian, H. Hayakawa, K. Hayama, J. Hedberg, A. Heffernan, D. Hegde, M. C. Heintze, J. Heinzel, H. Heitmann, F. Hellman, A. F. 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Villanueva Espinosa, E. T. Vincent, J. -Y. Vinet, S. Viret, S. Vitale, A. Vives, L. Vizmeg, B. Vizzone, 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, R. -Z. Wan, H. Wang, P. Wang, W. H. Wang, Y. F. Wang, Z. Wang, R. L. Ward, J. Warner, M. Was, T. Washimi, N. Y. Washington, D. Watarai, 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. Wimmer, C. W. Winborn, A. Wingfield, J. Winterflood, C. C. Wipf, G. Woan, N. E. Wolfe, H. T. Wong, I. C. F. Wong, T. Wouters, J. L. Wright, M. Wright, B. Wu, C. Wu, D. S. Wu, H. Wu, K. 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. Yébana Carrilero, A. B. Yelikar, X. Yin, J. Yokoyama, T. Yokozawa, M. Yoshihara, S. Yuan, H. Yuzurihara, M. Zanatta, M. Zanolin, M. Zeeshan, T. Zelenova, J. -P. Zendri, M. Zeoli, M. Zerrad, M. Zevin, H. Zhang, J. Zhang, L. Zhang, N. Zhang, R. Zhang, T. Zhang, C. Zhao, J. Zhao, Yue Zhao, Yuhang Zhao, L. -M. Zheng, Y. Zheng, L. Zhizhong, H. Zhong, H. Zhou, H. O. Zhu, X. -J. Zhu, Z. -H. Zhu, Z. Zhu, D. Z. Zieba, A. B. Zimmerman, L. Zimmermann, M. E. Zucker,Comments: main paper: 20 pages and 7 figures; total with appendices: 51 pages and 13 figures. This article draws heavily from the corresponding GWTC-4 article, arXiv:2509.04348Subjects: astro-ph.CO gr-qcCreated: 2026-08-04; Updated: 2026-08-06; Datestamp: 2026-08-06
We employ 236 gravitational-wave (GW) sources in the fifth LIGO--Virgo--KAGRA Collaboration (LVK) Gravitational-Wave Transient Catalog (GWTC-5.0) to estimate the Hubble constant $H_0$. We compare the luminosity distance measured from GWs to the redshift inferred i) using features in the mass spectrum, and ii) using statistical host galaxy association. Probing the relationship between source luminosity distances and redshifts obtained in this way yields constraints on cosmological parameters. We estimate $H_0 = {71.7}_{-7.5}^{+9.4}\,{\text{km}\,\text{s}^{-1}\,\text{Mpc}^{-1}}$ (median with $68\%$ symmetric credible interval). This combines information from the source-frame mass distribution with the $H_0$ measurement from GW170817 and its electroMAGNETic counterpart as well as galaxy catalog information from Dark Energy Survey Year 6 (DES-Y6). We improve over the GWTC-4.0 measurement by using more GW sources, some with significantly smaller sky localization volumes, which leads to a reduction by $22.0\%$ of the $H_0$ uncertainty and a reconstructed mass distribution with lower uncertainties. We also constrain deviations from general relativity (GR) which affect GW propagation, specifically that modify the luminosity distance inferred from the GW signal. We find no departures from GR in parameterized tests of GW propagation.
[abstract 9 / 31] Yes (score: 5) - Title: Comparative properties of X-Ray Flashes and Gamma-Ray Bursts from BeppoSAX observations of Fast X-ray TransientsAuthors: L. Piro, G. Gianfagna, J. J. M. in't Zand, B. Gendre, C. Guidorzi, L. Amati, F. Frontera, E. Kuulkers,Comments: 17 pages, 18 figures. Accepted in A&ASubjects: astro-ph.HECreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
We present the homogeneous and complete sample of 96 bona-fide Gamma Ray Bursts (GRBs) detected by the Wide Field Cameras and Gamma Ray Burst Monitor of BeppoSAX. We derive the spectral and temporal properties of the prompt emission, and assess the properties of the soft population of GRB, namely X-ray flashes (XRFs) in comparison with normal GRBs. We find that 36 events are XRFs, 40 X-ray rich events (XRR), and 20 normal GRBs. We analyze the distribution of the spectral parameters of the Band function, finding that the spectral indexes of the three classes are broadly similar. On the contrary the peak energy is the parameter driving the spectra shape, from 8.5 keV for XRF keV to 83 keV for GRBs. For the 67 events that are detected in both instruments we find that 9 events exhibit a soft X-ray precursor taking place from 14 to 105 s before the onset of the GAMMA-RAY BURST. About 90\% of the events that were identified in real time exhibit an X-ray afterglow, with a similar fraction for the three classes. In the optical and radio the the corresponding fractions are 35% and 33%. All the similarities in the spectrum, duration and afterglow properties suggest common progenitors for the three classes, where the differences are likely a combination of the effect of different baryon loading, energy, structure and orientation of the JET with respect to the observer. A comparison with Einstein Probe shows that the latter, thanks to its sensitivity, reaches out to a population of fainter and more numerous events, whose presence was firstly hinted at by the unique very low luminosity BeppoSAX GRB980425.
[abstract 10 / 31] Yes (score: 5) - Title: Magnetic Reconnection and Energy Extraction from a Rotating Black Hole in a Four-dimensional Einstein-Gauss-Bonnet GravityAuthors: Abdul Malik Sultan, Muhammad Israr Aslam, Muhammad Nawaz, Rubab Manzoor, Ke Wang, Hamood Ur Rehman, Yakup Yildirim,Comments:Subjects: gr-qcCreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
Recently, Comisso and Asenjo proposed a new mechanism for energy extraction based on MAGNETic RECONNECTion of plasma within the ergosphere. In this paper, we analyze the power and efficiency of energy extraction through MAGNETic RECONNECTion in a rotating four-dimensional Einstein-Gauss-Bonnet gravity BLACK HOLE. Firstly, we analyze the background properties of this spacetime and its physical quantities, including the event horizon, the boundary of the ergosphere, and the size of the ergosphere. We analyze the MAGNETic RECONNECTion in circular orbits and investigate the energy extraction region, as well as the power and efficiency of energy extraction. Our results indicate that energy extraction remains feasible even for a low spin parameter of $0.4$, which is well below the previously reported threshold. We also find that the energy extraction power exceeds that of the Blandford-Znajek mechanism. The Gauss-Bonnet coupling parameters $α$ lower the spin threshold for energy extraction. Similarly, we analyze the energy extraction region in the plunging regime, together with the corresponding power and efficiency. We find that energy extraction is possible even for a low spin parameter as $0.22$. We also observe that the Gauss-Bonnet coupling parameter $α$ further lowers the spin threshold. This behavior is consistent with that observed in the circular orbit case. Finally, we compare the energy extraction power in the plunging and circular orbit regimes and find that the plunging regime yields a higher energy extraction power than the circular orbit case.
[abstract 11 / 31] Yes (score: 4) - Title: Short GAMMA-RAY BURST progenitors have short delay timesAuthors: Matteo Pracchia, Om Sharan Salafia,Comments:Subjects: astro-ph.HECreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
Short GAMMA-RAY BURSTs (SGRBs) are thought to be primarily associated with binary neutron star (BNS) mergers. The SGRB population can therefore be scrutinized for signatures of the delay time between the formation of the progenitor massive star binary and the eventual merger, which could produce an evolution of the cosmic rate density of such events whose shape departs from that of the cosmic STAR FORMATION history. We therefore studied a large sample of SGRBs within a hierarchical Bayesian framework, with a particular focus on the delay time distribution (DTD) of the population. Following previous studies, we modelled the DTD either as a power-law with a minimum time delay or as a log-normal function. We considered two models for the intrinsic SGRB luminosity distribution: an empirical luminosity function with a doubly broken power-law shape and another based on a quasi-universal structured JET model. Regardless of the chosen parametrization, we found average time delays of $10\lesssim \langle τ_\mathrm{d}\mathrm\rangle/\mathrm{Myr}\lesssim 900$ and a minimum delay time of $τ_\mathrm{d,min}\lesssim 350\,\mathrm{Myr}$, in contrast with previous studies that found long delay times of a few gigayears. We demonstrate that the cause of the longer inferred time delays in past studies most likely resides in an incorrect treatment of selection effects
[abstract 12 / 31] Yes (score: 4) - Title: From Coils to Surface Recession: Multiphysics Simulation of Ablation in ICP Wind TunnelsAuthors: Sanjeev Kumar, Alessandro Munafo, Blaine Vollmer, Massimo Franco, Kelly A. Stephani, Daniel J. Bodony, Marco Panesi,Comments: 44 pages, 24 figuresSubjects: physics.plasm-phCreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
This work presents a multi-solver, coupled computational framework for predicting the thermo-chemical material response of thermal protection systems in inductively coupled plasma (ICP) wind tunnels. The framework integrates a high-fidelity Navier-Stokes plasma solver, an electroMAGNETic field solver, and a discontinuous-Galerkin material response solver using a partitioned coupling strategy. This enables an ab initio, end-to-end simulation of the 350 kW Plasmatron X facility at the University of Illinois Urbana-Champaign (UIUC), including plasma generation, electroMAGNETic heating, near-wall thermochemistry, and time-accurate material ablation. The model captures key ICP physics such as vortex-mode recirculation, Joule-heating-driven plasma formation, and Lorentz-force-induced flow confinement, and accurately predicts the transition from subsonic to supersonic JET behavior at low pressures. Validation against cold-wall calorimetry shows that predicted stagnation-point cold-wall heat fluxes fall well within experimental uncertainty, while coupled ablation simulations accurately reproduce measured stagnation temperature histories and recession rates with errors below 12% and 10%, respectively. Remaining discrepancies are attributed to uncertainties in power-coupling efficiency, equilibrium ablation modeling, and material property datasets. Sensitivity analyses reveal that a 10% variation in system efficiency can induce changes of up to 11% in steady- state surface temperature and 17% in recession rate, whereas an equivalent variation in material thermal conductivity results in comparatively minor deviations of about 1.5% and 0.5%, respectively. Overall, the framework demonstrates strong predictive capability for ICP wind tunnel environments and provides a foundation for improved design, interpretation, and planning of hypersonic material testing campaigns.
[abstract 13 / 31] Yes (score: 4) - Title: Testing the theory of colliding winds: The periastron passage of 9 Sagittarii. II. Radio monitoringAuthors: R. Blomme, G. Rauw, D. Volpi, Y. Nazé, R. Prinja,Comments: 8 pages, 4 figures, language-edited version, accepted for publication in A&ASubjects: astro-ph.SR astro-ph.HECreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
Colliding winds in massive-star binaries generate non-thermal radio emission and an increased X-ray emission. We study the radio emission of the non-thermal emitter 9 Sgr, which is a long-period and highly eccentric binary. We conducted a monitoring campaign of 9 Sgr around its 2013 - 2014 periastron passage, obtaining radio, X-ray and optical spectroscopy data. In this paper, we analyse the radio data. The radio data at 3.6, 6 and 20 cm show a maximum near periastron. Other non-thermal radio emitters among O-type binaries have a minimum flux near periastron, because the SYNCHROTRON emission is absorbed by the free-free absorption in the two stellar winds. This is not the case for 9 Sgr, because even at periastron the orbital separation is sufficient to maintain the wind-wind collision and its associated SYNCHROTRON emission outside the effective free-free radius of both stars. Our standard modelling with a local MAGNETic field that decreases inversely proportional to the distance from the stars (1/r) fails to explain the observed fluxes. Instead, we need to adopt a local MAGNETic field that decreases faster than 1/r. While our model provides an acceptably good fit to the data, there is clearly still room for improvement. More advanced modelling should include MAGNETohydrodynamics and more detailed physics of the injection, acceleration and cooling of the RELATIVISTIC electrons. Radio observations at orbital phases away from periastron can put further constraints on the models.
[abstract 14 / 31] Yes (score: 4) - Title: X-ray Reflection as Diagnostic of Supermassive Black Hole Binary PropertiesAuthors: Julie Malewicz, Tamara Bogdanović, David R. Ballantyne, Laura Brenneman, Thomas Dauser,Comments: 19 pages, 9 figures. Submitted to ApJ. Comments are welcome!Subjects: astro-ph.HECreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
We investigate correlations between prominent features in the RELATIVISTIC X-ray reflection spectrum emitted by an accreting supermassive BLACK HOLE (SMBH) binary with the underlying properties of the binary system. Model-independent measurements of the RELATIVISTIC Fe K$α$ line ($\sim$6.4 keV) and the Compton reflection hump ($\sim$20-30 keV) are shown to be useful in constraining binary parameters. We compute 24,570 X-ray reflection spectra from two mini-disks attached to SMBHs at a fixed separation of 100 $GM/c^2$ on circular orbits, by varying its mass ratio, spin parameters, inclination, orbital phase and total mass accretion rate. We find that the location of the blue peak in the RELATIVISTIC Fe K$α$ is a relatively robust diagnostic of the binary inclination, which could be obtained from a single-epoch X-ray spectrum. Given a few epochs of spectra, one may be able to determine the orbital phase of the binary and place constraints on its mass ratio by monitoring the Fe K$α$ centroid. Of all parameters, SMBH spin efects are most subtle and prone to measurement degeneracies. Some markers of high SMBH spin may nevertheless surface in the composite spectrum due to increased radiative efficiency. The approach developed here can be used to place preliminary constraints on binary parameters before a full parametrized X-ray spectral fitting method is available. It complements gravitational wave measurements by the Pulsar Timing Arrays (PTAs) and the Laser Interferometer Space Antenna by providing independent constraints on binary parameters that may be prone to degeneracy (inclination), or otherwise inaccessible (spin for PTAs).
[abstract 15 / 31] Yes (score: 4) - Title: Dissecting the Nuclear Structure of NGC 5548 with XRISM. I. Physical Properties of the Highly Ionized OutflowsAuthors: Missagh Mehdipour, Jon M. Miller, Jelle S. Kaastra, Gerard A. Kriss, Keigo Fukumura, Liyi Gu, Doyee Byun, Xin Xiang, Ehud Behar, Laura W. Brenneman, Elisa Costantini, Maryam Dehghanian, Jacobo Ebrero, Massimo Gaspari, Anna Juráňová, Erin Kara, Chen Li, Junjie Mao, Hirofumi Noda, Anna Ogorzalek, Ioanna Psaradaki, Daniele Rogantini, Sascha T. Zeegers, Keqin Zhao,Comments: Accepted for publication in ApJ, 14 pagesSubjects: astro-ph.HE astro-ph.GACreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
We present a detailed spectral analysis of an X-Ray Imaging and Spectroscopy Mission (XRISM) observation of the prototypical Seyfert 1 galaxy NGC 5548. XRISM's Resolve microcalorimeter reveals, for the first time, highly ionized outflows in this ACTIVE GALACTIC NUCLEus (AGN) through the detection of Fe XXV and Fe XXVI absorption lines in the Fe K band. Modeling the XRISM/Resolve spectrum alongside XMM-Newton Reflection Grating Spectrometer (RGS) data allows us to probe the ionization and kinematic structure of the outflows in this AGN. We identify four distinct ionization components, with ionization parameters log $ξ$ ranging from 0.9 to 3.4. Three of these components are further resolved into two velocity sub-components, demonstrating the multiphase structure of the outflows. The measured outflow velocities span 240 to 2730 km/s. We find a trend of increasing column density with ionization parameter ($ξ$), along with a general pattern of increasing outflow velocity with $ξ$. The XRISM/Resolve spectrum provides a far more detailed absorption measure distribution (AMD) than was previously possible, revealing two distinct slopes above and below $\logξ\sim 2.6$. A comparison of the Fe XXV absorption line profile with UV absorption lines (C IV and Ly$α$) observed with the Hubble Space Telescope reveals both overlaps and deviations. The XRISM/Resolve results suggest a multiphase, clumpy outflow in NGC 5548, consistent with a "hybrid wind" scenario in which the observed parameter trends arise from multiple origins and driving mechanisms.
[abstract 16 / 31] (score: 3) - Title: Transition of Magnetic Reconnection Regimes in Partially Ionized PlasmasAuthors: Liang Wang, Chuanfei Dong, Yi-Min Huang, Yue Yuan, Xinmin Li, Yang Zhang,Comments: 9 pages, 5 figuresSubjects: physics.plasm-ph astro-ph.SR physics.space-phCreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
Magnetic RECONNECTion in partially ionized plasmas plays a crucial role in a wide range of solar, astrophysical, and laboratory environments. While RECONNECTion in such plasmas is commonly characterized by the ion-neutral coupling strength and the ionization fraction $χ=n_{i}/(n_{i}+n_{n})$, most previous studies have focused primarily on the former. A systematic exploration of the ionization fraction, particularly in combination with ion-neutral coupling, is still lacking. This study presents the first systematic scan of the two-dimensional parameter space defined by ion-neutral collisionality and ionization fraction, enabling investigation of the transition from strongly coupled RECONNECTion to faster, decoupled RECONNECTion. To achieve this, we employ a new three-fluid, five-moment numerical model that treats electrons, ions, and neutrals as separate species on an equal footing. We find that in the strongly coupled regime, the RECONNECTion rate is consistent with a $χ^{1/4}$ scaling. As collisionality decreases, the system transitions to a fast, ionization-independent regime. On the other hand, in the weakly coupled and fast-RECONNECTion regimes, the current sheet approaches an ion-inertial-scale thickness rather than the expanded hybrid scale $d_{i}χ^{-1/2}$ predicted by fully coupled analytic fluid theories. The identified critical thickness and the resulting onset of fast RECONNECTion agree reasonably well with recent fully kinetic simulations and laboratory experiments. In addition, we show that, over a wide range of coupling strengths, the ion outflow velocities remain Alfvénic, scaling with the appropriate ion or hybrid Alfvén speed, while the hybrid outflow velocity scales as $χ^{1/2}$ when normalized by ion Alfvén speed.
[abstract 17 / 31] (score: 3) - Title: Bayesian Geometrical Modeling of IXPE Polarization Angle Curves of the Magnetars 1E 2259+586 and 1E 1547.0-5408Authors: Biao-Peng Li, Zhi-Fu Gao, Wen-Qi Ma, Wei-Feng Zhang, L. C. Garcia de Andrade,Comments: 17 pages, 6 figures, Accepted by ApJSubjects: astro-ph.HECreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
X-ray polarimetry directly probes the radiation geometry and large-scale MAGNETic configuration of MAGNETars. We present a uniform Bayesian comparison between a dipole-dominated classical rotating vector model (CRVM) and a modified rotating vector model (MRVM) including a first-order MAGNETospheric twist correction. The models are applied to the phase-resolved IXPE POLARIZATION position angle (PA) curves of 1E~2259+586 and 1E~1547.0$-$5408. Parameters are inferred with a PA-level likelihood, and the models are compared using $χ^2$, AIC, BIC, and Bayesian evidence. For 1E~1547.0$-$5408, we also test radio-derived geometrical constraints using radio-informed priors and radio-fixed fits. The current IXPE PA data for both sources are consistent with a dipole-dominated geometry and do not require a significant global twist. The MRVM gives only a marginal improvement for 1E~2259+586, with a Bayes factor of $\simeq3.3$, and no meaningful improvement for 1E~1547.0$-$5408, with a Bayes factor of $\simeq1.29$. We confirm that for 1E 1547, the nearly aligned radio geometry is not ruled out, but the radio RVM central geometry is not preferred by the X-ray PA data alone. The two sources show different impact angles, suggesting that MAGNETar X-ray POLARIZATION diversity reflects both viewing geometry and source-dependent emission physics. This work provides a framework for future Stokes-level and multi-epoch polarimetric studies with missions such as eXTP.
[abstract 18 / 31] (score: 3) - Title: Gravitational wave detectability range informed by external messengersAuthors: S. Ronchini, A. Chopra, T. Dal Canton, B. Banerjee, A. L. De Santis, M. Branchesi,Comments:Subjects: astro-ph.HE gr-qcCreated: 2026-08-04; Updated: 2026-08-06; Datestamp: 2026-08-06
A rapid estimate of gravitational-wave (GW) detectability associated with astronomical transients is crucial for optimizing multi-messenger follow-up strategies and for constraining the physical origin of the transient itself. We introduce here the Targeted Detectability Range (TDR), designed to evaluate, with minimal computational effort, the detectability of compact binary coalescences under the hypothesis of association with an external messenger, such as an electroMAGNETic or neutrino signal. Unlike the standard GW range, which is based on averaged source parameters, the TDR incorporates prior information from observations of the external messenger, including sky localization, inclination constraints, and physically motivated bounds on component masses. We report the TDR of all short- and long-duration GAMMA-RAY BURSTs, observed during the first three observing runs of Advanced LIGO and Advanced Virgo. The method is validated by performing a systematic comparison with the 90$\%$ exclusion distances provided by modeled targeted GW searches. In the absence of a coincident detection by all-sky, all-time GW searches, the TDR provides a rapid and quantitative constraint on a possible merger origin of the astrophysical source. Its low-latency implementation and public availability would enable timely prioritization of follow-up observations and optimized allocation of observational resources, with direct impact on the physical interpretation of astronomical transients.
[abstract 19 / 31] (score: 3) - Title: Computational Methods and GPU Acceleration in Plasma Physics: A Empirical Analysis of arXiv Publications and Research TrendsAuthors: Jeremy J. Williams, Anders Brostrom, Stefano Markidis,Comments: Quantitative research study prepared in the standardized Springer LNCS format and consists of 13 pages, which includes the main text, references, and figuresSubjects: physics.plasm-ph physics.comp-phCreated: 2026-08-04; Updated: 2026-08-06; Datestamp: 2026-08-06
Computational plasma physics increasingly relies on high-performance computing (HPC) methods, including particle-in-cell (PIC), gyrokinetic, and MAGNETohydrodynamic (MHD) simulations, yet field-wide evidence on how method choice, team size, and GPU adoption shape research outputs remains limited. We analyze 5,522 computational plasma physics papers published on arXiv between 2010 and 2025 using large-scale text mining, employing abstract length as a proxy for methodological and algorithmic complexity. Using ordinary least squares (OLS), tobit, and logistic regression models, we examine how abstract length and GPU mentions vary with computational method, number of authors, and publication year. Controlling for collaboration size and temporal trends, results show that MHD studies have longer abstracts than PIC and gyrokinetic papers, indicating more extensive methodological and physical exposition. Abstract length increases modestly with team size, while temporal effects suggest gradual changes in abstract conciseness over time. At the same time, PIC and gyrokinetic methods have grown substantially in relative prevalence over the past decade and are strongly linked to GPU adoption, reflecting their higher computational intensity and suitability for accelerator-based architectures. Together, these findings highlight a decoupling between methodological verbosity and method prevalence, offering a new bibliometric perspective on the evolution of HPC-driven plasma physics research.
[abstract 20 / 31] (score: 3) - Title: Observation of the Moon and Sun shadows with COSMIC RAYs at an average energy of $\text{7}{\times}\text{10}^\text{17}\,$eVAuthors: The Pierre Auger Collaboration, A. Abdul Halim, P. Abreu, M. Aglietta, M. Ahmed, I. Allekotte, K. Almeida Cheminant, R. Aloisio, J. Alvarez-Muñiz, A. Ambrosone, J. Ammerman Yebra, L. Anchordoqui, B. Andrada, L. Andrade Dourado, L. Apollonio, C. Aramo, J. C. Arteaga Velázquez, P. Assis, G. Avila, E. Avocone, A. Bakalova, Y. Balibrea, A. Baluta, F. Barbato, A. Bartz Mocellin, O. Batalla Cruz, J. P. Behler, C. Berat, M. E. Bertaina, M. Bianciotto, P. L. Biermann, V. Binet, K. Bismark, T. Bister, J. Biteau, J. Blazek, J. Blümer, M. Boháčová, D. Boncioli, C. Bonifazi, N. Borodai, J. Brack, P. G. Brichetto Orquera, S. Buitink, A. Bwembya, T. R. Caba Pineda, K. S. Caballero-Mora, S. Cabana-Freire, L. Caccianiga, J. Caraça-Valente, R. Caruso, A. Castellina, F. Catalani, G. Cataldi, L. Cazon, M. Cerda, B. Čermáková, A. Cermenati, K. Cerny, J. A. Chinellato, J. Chudoba, L. Chytka, R. W. Clay, A. C. Cobos Cerutti, R. Colalillo, R. Conceição, G. Consolati, M. Conte, F. Convenga, D. Correia dos Santos, P. J. Costa, C. E. Covault, M. Cristinziani, C. S. Cruz Sanchez, S. Dasso, K. Daumiller, B. R. Dawson, R. M. de Almeida, E. -T. de Boone, B. de Errico, J. de Jesús, S. J. de Jong, J. R. T. de Mello Neto, I. De Mitri, D. de Oliveira Franco, F. de Palma, V. de Souza, E. De Vito, A. Del Popolo, O. Deligny, N. Denner, K. Denner Syrokvas, L. Deval, A. di Matteo, C. Dobrigkeit, J. C. D'Olivo, L. M. Domingues Mendes, T. Dominguez, Y. Dominguez Ballesteros, Q. Dorosti, R. C. dos Anjos, J. Ebr, F. Ellwanger, R. Engel, M. Erdmann, A. Etchegoyen, C. Evoli, H. Falcke, G. Farrar, A. C. Fauth, T. Fehler, F. Feldbusch, A. Fernandes, M. Fernández Alonso, B. Fick, J. M. Figueira, P. Filip, A. Filipčič, B. Flaggs, A. Franco, M. Freitas, T. Fujii, A. Fuster, C. Galea, B. García, C. Gaudu, P. L. Ghia, U. Giaccari, M. Giammarco, C. Glaser, F. Gobbi, F. Gollan, G. Golup, P. F. Gómez Vitale, J. P. Gongora, N. González, D. Góra, A. Gorgi, M. Gottowik, F. Guarino, G. P. Guedes, Y. C. Guerra, L. Gülzow, S. Hahn, P. Hamal, M. R. Hampel, P. Hansen, A. Haungs, M. Havelka, T. Hebbeker, C. Hojvat, J. R. Hörandel, P. Horvath, M. Hrabovský, T. Huege, A. Insolia, P. G. Isar, M. Ismaiel, P. Janecek, V. Jilek, K. -H. Kampert, B. Keilhauer, V. V. Kizakke Covilakam, H. O. Klages, M. Kleifges, A. Klingel, J. Köhler, F. Krieger, M. Kubatova, N. Kunka, B. L. Lago, N. Langner, N. Leal, M. A. Leigui de Oliveira, Y. Lema-Capeans, A. Letessier-Selvon, I. Lhenry-Yvon, L. Lopes, M. Mallamaci, S. Mancuso, D. Mandat, P. Mantsch, A. G. Mariazzi, C. Marinelli, I. C. Mariş, G. Marsella, D. Martello, S. Martinelli, O. Martínez Bravo, A. Martínez-Mendez, M. A. Martins, H. -J. Mathes, J. Matthews, G. Matthiae, E. Mayotte, S. Mayotte, P. O. Mazur, G. Medina-Tanco, D. Melo, A. Menshikov, C. Merx, S. Michal, M. I. Micheletti, L. Miramonti, M. Mogarkar, S. Mollerach, F. Montanet, L. Morejon, K. Mulrey, R. Mussa, W. M. Namasaka, S. Negi, L. Nellen, K. Nguyen, G. Nicora, M. Niechciol, D. Nitz, D. Nosek, A. Novikov, V. Novotny, L. Nožka, A. Nucita, L. A. Núñez, S. E. Nuza, J. Ochoa, M. Olegario, C. Oliveira, L. Östman, M. Palatka, J. Pallotta, G. Parente, T. Paulsen, M. Pech, J. Pękala, R. Pelayo, C. Pérez Bertolli, L. Perrone, S. Petrera, T. Pierog, M. Pimenta, M. Platino, P. Privitera, C. Priyadarshi, M. Prouza, K. Pytel, S. Querchfeld, J. Rautenberg, D. Ravignani, J. V. Reginatto Akim, M. Z. Rennó, A. Reuzki, J. Ridky, F. Riehn, M. Risse, V. Rizi, B. Rocha Moldes, E. Rodriguez, G. Rodriguez Fernandez, J. Rodriguez Rojo, S. Rossoni, M. Roth, E. Roulet, A. C. Rovero, A. Saftoiu, M. Saharan, F. Salamida, H. Salazar, G. Salina, P. Sampathkumar, N. San Martin, J. D. Sanabria Gomez, F. Sánchez, F. M. Sánchez Rodriguez, E. Santos, F. Sarazin, R. Sarmento, R. Sato, P. Savina, V. Scherini, H. Schieler, M. Schimp, D. Schmidt, O. Scholten, H. Schoorlemmer, P. Schovánek, F. G. Schröder, J. Schulte, T. Schulz, S. J. Sciutto, M. Scornavacche, A. Sedoski, S. Sehgal, S. U. Shivashankara, G. Sigl, K. Simkova, F. Simon, R. Šmída, S. Soares Sippert, P. Sommers, S. Stanič, J. Stasielak, P. Stassi, S. Strähnz, M. Straub, T. Suomijärvi, A. D. Supanitsky, Z. Svozilikova, Z. Szadkowski, F. Tairli, A. Tapia, C. Taricco, C. Timmermans, O. Tkachenko, P. Tobiska, C. J. Todero Peixoto, B. Tomé, A. Travaini, P. Travnicek, C. Trimarelli, M. Tueros, M. Unger, R. Uzeiroska-Geyik, L. Vaclavek, M. Vacula, I. Vaiman, J. F. Valdés Galicia, L. Valore, P. van Dillen, E. Varela, V. Vašíčková, A. Vásquez-Ramírez, D. Veberič, I. D. Vergara Quispe, S. Verpoest, V. Verzi, J. Vicha, S. Vorobiov, J. B. Vuta, A. A. Watson, A. Weindl, M. Weitz, L. Wiencke, H. Wilczyński, B. Wundheiler, B. Yue, A. Yushkov, E. Zas, D. Zavrtanik, M. Zavrtanik,Comments: submitted for reviewSubjects: astro-ph.HECreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
Interactions of COSMIC RAYs with the Moon and the Sun produce deficits in their arrival-direction distributions relative to an isotropic flux. Such shadows have been observed previously at energies between $10^{12}\,$eV and $10^{16}\,$eV. We report the first observation of the Moon and Sun shadows at cosmic-ray energies larger than about $10^{16}\,$eV (average energy of $7\times10^{17}\,$eV), using data collected by the Pierre Auger Observatory. We employ data from three detector arrays covering $3000\,\text{km}^2$, $27\,\text{km}^2$, and $2\,\text{km}^2$, with spacings of $1500\,\text{m}$, $750\,\text{m}$, and $433\,\text{m}$, respectively. The data amount to over 10.6 million events. The Moon and Sun shadows are detected with a combined significance of approximately $3σ$. These observations confirm the pointing accuracy of the Surface Detector of the Pierre Auger Observatory using celestial bodies. From the combined Sun and Moon shadows, we infer an overall angular resolution of $(0.59^{+0.15}_{-0.11})^\circ$.
[abstract 21 / 31] (score: 2) - Title: A New Approach to Compute Linear Landau DampingAuthors: M. Pelkner, K. Hallatschek, M. Raeth,Comments:Subjects: physics.plasm-phCreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
We present a semi-analytical method for calculating exact time-domain solutions to linear Landau-damping problems. Unlike traditional residue-based approaches, our framework avoids the need to compute complex zeros of the dielectric function. We illustrate the method for an electrostatic, unMAGNETized plasma with kinetic ions and adiabatic electrons by deriving the response of both the ion density and the ion distribution function to an initial density perturbation. We further show that the construction can be formally extended to linear Vlasov-Maxwell problems with a uniform background MAGNETic field and a Maxwellian equilibrium distribution.
[abstract 22 / 31] (score: 2) - Title: Gravitational Waves from Strongly Magnetized Eccentric Neutron Star BinariesAuthors: R. Prasad, Anushka Doke, Prayush Kumar,Comments:Subjects: astro-ph.HE gr-qcCreated: 2026-08-04; Updated: 2026-08-06; Datestamp: 2026-08-06
We explore the dynamics of neutron star binaries that approach their final inspiral stages with residual eccentricity and strong MAGNETic fields, features that can arise in systems formed through dynamical capture of relatively young neutron stars. Our analysis focuses on identifying MAGNETic-field imprints on the gravitational wave signal arising from two mechanisms: MAGNETic interaction between the neutron stars and electroMAGNETic radiation from the system's effective dipole. Using a perturbative approach, we obtain the associated gravitational wave energy loss rate and phase evolution, and quantify detectability through cumulative dephasing, horizon distances, and Fisher-matrix analyses. While MAGNETic effects are intrinsically small, entering at 2 post-Newtonian (PN) order, their cumulative influence over extended inspirals will become distinguishable in future detectors owing to enhanced low-frequency sensitivity. For binaries with comparable MAGNETic fields, we show that $10^{14}\,\mathrm{G}$ systems will be detectable up to $\sim10$ Mpc with DECIGO and the Einstein Telescope, while $10^{15}\,\mathrm{G}$ fields will be discernible out to several hundred Mpc. For extreme fields of $10^{16}\,\mathrm{G}$, third-generation detectors could probe out to Gpc scales. These findings suggest that MAGNETic effects in compact binaries can indeed become observable with next-generation detectors, offering a potential probe of MAGNETar-level fields and binary formation pathways.
[abstract 23 / 31] (score: 2) - Title: The SOFIA Massive (SOMA) Radio Survey. III. Radio Emission from Intermediate-Mass ProtostarsAuthors: Francisco Sequeira-Murillo, Viviana Rosero, Joshua Marvil, Jonathan C. Tan, Ruben Fedriani, Yichen Zhang, Prasanta Gorai, James M. De Buizer, Maria T. Beltrán,Comments: Accepted to ApJSubjects: astro-ph.SR astro-ph.GACreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
We present results from Very Large Array (VLA) radio continuum observations of twelve intermediate-mass (IM) protostars, as part of the SOFIA Massive Star Formation Survey. Using these observations, we studied their morphology, multiplicity and radio spectral energy distributions (SEDs). Across our target regions, we resolve multiple compact sources and report eight new detections, four of which are entirely new and four that have counterparts at other wavelengths, but are detected here for the first time at radio frequencies. Based on radio morphologies and spectral indices, we assess the nature of the detected sources, highlighting seven that display JET-like structures and spectral indices consistent with ionized JETs. Combining our results with the SOMA Radio I and II results, we expand the overall sample to 29 protostars, covering a bolometric luminosity range from $L_{\rm bol}\sim 10^2$ to $10^6\:L_\odot$. These sources help define a potential evolutionary sequence in the radio versus bolometric luminosity diagram. IM protostars have radio luminosities that are lower than expected from a simple power law extrapolation from low-mass protostars. However, this result is consistent with theoretical expectations from protostellar evolution models, which show low levels of photoionization and reduced shock ionization emission due to expanded stellar radii during this phase. Overall our expanded SOMA Radio sample provides new constraints on theoretical models of massive protostellar evolution, especially the connection to ionized gas structures.
[abstract 24 / 31] (score: 2) - Title: Systematic study of lepton-flavor-violating DARK MATTER interactions via indirect detection in effective field theoriesAuthors: Sahabub Jahedi, Jin-Han Liang, Yi Liao, Xiao-Dong Ma, Yoshiki Uchida,Comments: v1: 17pages, 10 figures; v2: version accepted for publication in PRDSubjects: hep-phCreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
Lepton-flavor-violating (LFV) interactions involving DARK MATTER (DM) particles remain a largely unexplored area. In this study, we systematically investigate LFV DM interactions within the framework of effective field theories by analyzing astrophysical photons and positrons produced from DM annihilation. Employing the astrophysical photon and positron data collected by FERMI-LAT, INTEGRAL, XMM-Newton, and AMS-02, we place meaningful constraints on all leading-order effective operators involving a DM pair and a flavor-violating charged lepton pair. Our analysis covers the three well-known DM candidates: a scalar, a fermion, and a vector particle. For the photon flux, we consider contributions from final-state radiation, radiative decay, and inverse Compton scattering and examine their respective sensitivity regions across different DM masses and photon energies. We find that, for DM masses below $\mathcal{O}(20\,\rm GeV)$, INTEGRAL provides the most stringent constraints on annihilation cross sections and effective operators in all three LFV channels, whereas AMS-02 offers the strongest constraints above $\mathcal{O}(20~\rm GeV)$.
[abstract 25 / 31] (score: 2) - Title: General RELATIVISTIC limit of f(R) gravity in the horizon scale of BLACK HOLEAuthors: Pranjali Bhattacharjee, Sanjeev Kalita, Debojit Paul, Rajibul Shaikh,Comments: 20 pages, 19 figures. Corrected version. Comments are welcomeSubjects: gr-qcCreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
The environment of the Galactic Centre (GC) BLACK HOLE, Sgr A* gives us new opportunities to test BLACK HOLE physics and deviation from General Relativity. In this analytical study we calculate null geodesics around the GC BLACK HOLE for the recently developed stationary, axisymmetric and vacuum metric of f(R) gravity theory. We study the impact of scalaron degree of freedom of f(R) gravity theory on size and shape of the BLACK HOLE shadow. A minimum bound of $10^{-17}$ eV for scalaron mass has been obtained by using $1 σ$ upper bounds on deviation parameter measured by the Keck telescope and the VLT. Scalarons lighter than this bound are found to increase shadow size beyond that measured by the Event Horizon Telescope. We calculate shadow displacement and asymmetry and infer that $10^{-16}$ eV scalarons which produce exact Kerr sized shadow yield 6\% departure from Kerr quadrupole. From asymmetry we infer preservation of BLACK HOLE no-hair theorem for such scalaron mass and further examine possibility of violation of the theorem. The same mass scale is found to reproduce the PPN parameter ($γ$) constrained in the weak field limit of the solar system. Gravitational identifiers, the Kretschmann scalar ($κ$) and gravitational potential ($ϕ$) have been used to infer scalaron masses in the regime of S-stars near Sgr A* which are found to be consistent with the limits obtained by using shadow scales. We ensure existence of an appropriate general RELATIVISTIC limit of f(R) gravity scalaron mass in the horizon scale of the BLACK HOLE.
[abstract 26 / 31] (score: 2) - Title: Infrared Line Diagnostics Fail to Constrain Sgr A*'s UV OutputAuthors: Mayura Balakrishnan, Sebastiano D. von Fellenberg, Daryl Haggard, Joseph M. Michail, Nicole M. Ford, Joseph L. Hora, Laurent Loinard, Sera Markoff, Joey Neilsen, Giacomo Principe, Nadeen B. Sabha, Howard A. Smith, Zach Sumners, Shuo Zhang,Comments: 19 pages, 5 figures, 3 tables. Accepted by ApJ for publicationSubjects: astro-ph.HE astro-ph.GACreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
Sgr A*, the 4 x $10^6 M_{sun}$ supermassive BLACK HOLE at the Galactic Center, exhibits frequent flaring with X-ray luminosities of $L_X \sim 10^{35}-10^{36}$ erg s$^{-1}$, while its ultraviolet (UV) emission remains unconstrained due to extreme extinction ($A_V \sim 30$ mag). We use JWST/MIRI time-resolved spectroscopy of the central 0.3" region to search for mid-infrared emission line variability driven by Sgr A* flares, comparing the results to CLOUDY photoionization models spanning flare luminosities of $L_{UV} = 10^{32}$-$10^{39}$ erg s$^{-1}$. We detect no continuum-correlated variability in any mid-infrared line, including [Fe II] (5.34 $μ$m), [Ne II] (12.813 $μ$m), [Fe II] (17.936 $μ$m), and [S III] (18.713 $μ$m) over lags of $\sim1$-8~hr. Despite expectations of a flare-driven response, we show that the lack of variability is consistent with the physical conditions in the spatially extended line-emitting gas, where light-crossing timescales of $\sim0.1$-$10$ days and recombination and cooling timescales much longer than the variability timescales suppress any observable response to individual flares. We further find that the modeled infrared spectra are dominated by continuum emission rather than isolated line emission. The brightest predicted lines are intrinsically weak (lower than 10$^{-5}$ mJy), and their detectability is further reduced by the large kinematic broadening expected at the CLOUDY-predicted emitting radii, reducing their contrast against the continuum. Extending the analysis to higher-ionization mid-infrared and near-infrared lines does not improve sensitivity. These results demonstrate that infrared emission lines trace a steady-state radiation field rather than individual flaring events, and therefore infrared line diagnostics cannot be used to constrain the instantaneous UV flux of Sgr A*.
[abstract 27 / 31] (score: 2) - Title: Pfirsch-Schlüter CurrentAuthors: Allen H Boozer,Comments:Subjects: physics.plasm-phCreated: 2026-08-04; Updated: 2026-08-06; Datestamp: 2026-08-06
The Pfirsch-Schlüter current is a current that flows along the MAGNETic field lines in a toroidal plasma equilibrium that is required to make the plasma current density divergence free in the presence of a plasma-pressure gradient. A distortion in the plasma shape is caused by the Pfirsch-Schlüter current, and it is desirable to minimize both the strength and the distance this current flows along the MAGNETic field lines. The Pfirsch-Schlüter current is localized within a half period of a stellarator when $d\ell/B$ integrated over the half period is the same for all lines in the MAGNETic surface. It is shown that within parts in a thousand this is the same condition as the distance $\ell_{s}$ required for a field line to cross the half period being the same for all lines in the surface. To make the $\ell_{s}$'s the same, the lines started on the small major radius side of the plasma must undergo wiggles to make their $\ell_{s}$ as long as those started on the outboard side. This is generally achieved using modular coils with a large helical component on the small major radius side but could be achieved with a central column carrying a helical current.
[abstract 28 / 31] (score: 2) - Title: Time-dependent cosmic-ray escape from wind bubbles: hard spectra formationAuthors: Lukas Merten, Sophie Aerdker, Enrico Peretti,Comments:Subjects: astro-ph.HECreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
Overview: Wind-driven bubbles are dynamic systems that can accelerate COSMIC RAYs, depending on their physical properties, up to very high energies. We investigate how a time-dependent description of the particle transport may impact the escaping cosmic-ray flux. Model: The wind bubble system is modeled as spherically symmetric. Cosmic rays are continuously injected at the position of the termination shock and propagate through advection and diffusion until the escape at the time-dependent position of the forward shock, which is treated as a free escape boundary. Methods: The one-dimensional spherical time-dependent transport equation is solved by transforming it into the corresponding set of stochastic differential equations, and integrated with a modified version of the open source cosmic-ray propagation framework CRPropa. Results: We find that, during the wind driven phase, the downstream escaping spectra from wind bubbles can be harder than $\sim E^{-2}$, the conventional expectation from diffusive shock acceleration. Depending on the turbulence model the initial energy spectrum can be significantly suppressed at lowest energies, which could be an observable feature to distinguish between different turbulence realizations. This effect could lead to an efficient confinement of low energy particles, potentially leading to observable implication in terms of multi-messenger radiation and cosmic-ray accumulated grammage within the bubble.
[abstract 29 / 31] (score: 2) - Title: Implications of Broad [O III] 4364 and UV Line Emission in Two Little Red Dots at z ~ 7 - 8Authors: Casey Papovich, Kaila Ronayne, Weida Hu, Dale D. Kocevski, Pablo Arrabal Haro, Taylor A. Hutchison, Steven L. Finkelstein, Erini Lambrides, Rebecca L. Larson, Bren E. Backhaus, Micaela B. Bagley, Nikko J. Cleri, Mark Dickinson, Ray Garner, Jeyhan Kartaltepe, Vasily Kokorev, Grace M. Olivier, Anthony J. Taylor, Jonathan R. Trump, Jiayang Yang,Comments: Submitted to ApJ; 24 pages, 14 figures. Comments welcomeSubjects: astro-ph.GACreated: 2026-08-04; Updated: 2026-08-06; Datestamp: 2026-08-06
We present deep, NIRSpec G140M and G395M spectroscopy of Little Red Dots (LRDs) at z = 6.68 and z = 8.35. Both LRDs show broad Balmer and [O III] $λ$4364 emission. The broad [O III] $λ$4364 lines have FWHM ~1000 km/s, about 1/3 that of the H$β$ lines. Assuming gas temperatures T ~ 15,000 - 25,000 K, the [O III] $λ$4364/[O III] $λ$5008 ratios of the broad lines yield high gas densities, log n/cm^-3 = 6.3 to 7.9, 3-10$\times$ higher than those in broad-line regions of low-redshift QUASARs. If the broad-lines trace virial motions, it is evidence for metal-enhanced gas clouds, ~1-10~pc from the LRD engine. Both LRDs show narrow [C III] $λ$1907 + C III] $λ$1909, and O III] $λλ$1661,1666. The C III] ratios yield narrow-line gas densities, log n/cm^-3 = 4.2-5.2, similar to those in other star-forming galaxies. The line equivalent widths, EW(O III]), EW(C III]), are at, or exceed, limits expected for stellar populations, likely requiring an additional ionizing source. The LRDs also have [O III] $λ$4364/H$γ$ ratios that favor ionization from an accretion disk, possibly combined with stars. Both LRDs show nitrogen enhancement based on detections of N III] $λ$1746 or N IV] $λ$1486, which may imply rapid, recent star-formation. These results favor a scenario where the LRD gas envelopes are highly stratified, having high-density clouds with a non-unity covering factors and a complex geometry, such that ionizing radiation from the LRD accretion disk, combined with that from star-forming regions, produce the nebular emission features.
[abstract 30 / 31] (score: 2) - Title: The Constant Evolution of the Neil Gehrels SWIFT Observatory: Two Decades of Operational Innovation for Time-Domain and Multi-Messenger AstrophysicsAuthors: Jamie A. Kennea,Comments: 12 pages, 6 figures, submitted to SPIESubjects: astro-ph.IMCreated: 2026-08-04; Updated: 2026-08-06; Datestamp: 2026-08-06
The Neil Gehrels SWIFT Observatory has, for more than twenty years, served as NASA's premier rapid-response, multi-wavelength facility for the study of GAMMA-RAY BURSTs (GRBs) and the transient sky. While SWIFT's hardware has remained essentially unchanged since its 2004 launch, its operational capabilities have evolved continuously, driven by a philosophy of ``always be developing.'' Hosted entirely at The Pennsylvania State University, with co-located flight and science operations, SWIFT has repeatedly reinvented how a NASA mission can be commanded, transforming itself from a GRB-chasing autonomous robotic telescope into a flexible, automated platform for time-domain and multi-messenger astrophysics (TDAMM). We review the key operational innovations that have enabled this evolution: the development of automated target-of-opportunity (TOO) uploads in response to the early loss of active X-ray Telescope cooling; onboard tiling of large error regions; the ManyPoint flight-software capability for executing hundreds of pointings; the Gamma-ray Urgent Archiver for Novel Opportunities (GUANO); and the ``Urgency 0'' continuous-commanding mode that has reduced TOO response latencies from hours to seconds. We illustrate the scientific impact of these capabilities through SWIFT's gravitational-wave and neutrino follow-up campaigns, including GW170817/AT2017gfo and IceCube-170922A, and through real-time ``early-warning'' slewing toward predicted compact-binary mergers. Finally, we discuss the heritage SWIFT is creating for future TDAMM missions, and the ongoing efforts to extend SWIFT's life, both through attitude-based scheduling that minimizes the spacecraft's atmospheric drag cross-section and through a commercial orbit-boost mission.
[abstract 31 / 31] (score: 2) - Title: Constraining Lorentz invariance violation from the depth of air-shower maximumAuthors: Nickolay S. Martynenko, Grigory I. Rubtsov, Petr S. Satunin, Andrey K. Sharofeev, Sergey V. Troitsky,Comments: 16 pages, 4 figures. To be submitted to Phys. Rev. DSubjects: astro-ph.HE hep-phCreated: 2026-08-05; Updated: 2026-08-06; Datestamp: 2026-08-06
Hypothetical Lorentz invariance violation (LIV) remains strongly constrained but has not been excluded as a possible manifestation of new high-energy physics. In subluminal photon-sector LIV, suppressed Bethe$\unicode{x2013}$Heitler pair production modifies the electroMAGNETic component of extensive air showers. We present a simulation-based toy analysis of this effect using published Pierre Auger fluorescence-detector distributions of the reconstructed depth of air-shower maximum. The modified distributions of the depth of the shower maximum are folded with the Auger detector-response parametrizations and compared with the data using free composition fractions in each reconstructed-energy bin. Within this approach, the comparison gives a sensitivity to LIV compatible with that expected from ultra-high-energy photon-induced showers. We obtain $M_{\rm LIV}>1.5\times 10^{21}\,\text{GeV}$ ($95\%$ confidence level). This result should not be interpreted as a detector-level experimental limit because the detector response and reconstruction are simplified, and the result remains composition dependent. However, the approach presented here opens the way for constraining LIV in hadronic air showers with more detailed analyses.
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