Current date: 2026-06-30
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Scoring abstracts
Number of records retrieved: 1175
Keyword score statistics
score 10 -- 1 abstracts
score 8 -- 1 abstracts
score 7 -- 5 abstracts
score 6 -- 2 abstracts
score 5 -- 8 abstracts
score 4 -- 11 abstracts
score 3 -- 7 abstracts
score 2 -- 35 abstracts
in total -- 70 abstracts
Articles that appeared on 2026-06-30
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[abstract 1 / 70] Wow! (score: 10)
- Title: SKA-VLBI Probes of High-energy Emission Processes in Relativistic JetsAuthors: M. Kadler, E. K. Bempong-Manful, P. G. Edwards, F. Eppel, C. M. Fromm, M. Giroletti, J. Heßdörfer, T. Hovatta, Y. Y. Kovalev, K. Mannheim, R. Ojha, F. Rösch, E. Ros,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Kadler01Subjects: astro-ph.HE astro-ph.GACreated: 2026-06-28; Updated: 2026-06-30; Datestamp: 2026-06-30
Relativistic JETs in the nuclei of active galaxies are ubiquitous sources of high-energy emission. In particular, BLAZARs represent the most luminous persistent X-ray and gamma-ray sources, whose defining characteristics are small JET inclination angles to the line of sight. Blazars can be detected in many cases up to TeV energies and the largest class of TeV emitting extragalactic AGN is represented by high-SYNCHROTRON peaked (HSP) BL Lac objects, which are generally comparably faint radio sources. Moreover, evidence has also been accumulated that high-energy cosmic neutrinos detected by IceCube can be associated with BLAZARs. There is an increasing number of suggested BLAZAR-neutrino associations, along with many cases of coincident flaring radio emission, but in a majority of cases, faint BLAZARs on the level of millijanskies or below have to be considered. These high-energy photon and neutrino emission processes hold many unanswered questions including the unknown source of seed-photons for photo-pion production and the infamous Doppler crisis of TeV-emitting BL Lac objects. SKA-VLBI offers the opportunity to achieve superior sensitivity at milliarcsecond resolutions, provided by the combination of the phased SKA-Mid and global VLBI arrays. This opens the possibility to perform high-sensitivity and high-angular resolution imaging and polarimetric probes of faint BLAZARs. The resulting high-fidelity spatially resolved parameterizations of structured JETs in bright sources will yield key insights to constrain physical models of high-energy photon and particle emission in AGN JETs.
[abstract 2 / 70] Wow! (score: 8) - Title: Correlation Between Hard X-Ray and Cosmic Neutrino Sources: From Obscured AGN to BlazarsAuthors: Emma Kun, Imre Bartos, Claudio Ricci, Santiago del Palacio, Francis Halzen, Julia Becker Tjus, Peter L. Biermann, Anna Franckowiak,Comments: 21 pages, 7 figures, 5 tables. Accepted for publication in PASPSubjects: astro-ph.HECreated: 2026-06-28; Updated: 2026-06-30; Datestamp: 2026-06-30
The origin of high-energy astrophysical neutrinos remains a key open question in multimessenger astrophysics. A correlation between unabsorbed hard X-ray and high-energy neutrino luminosity has been reported in six ACTIVE GALACTIC NUCLEi with the highest individual IceCube significances, linking neutrino production to compact, photon-rich environments near supermassive BLACK HOLEs. We study whether the threshold-near IceCube excesses associated with seven NUSTAR-observed BLAZARs are statistically consistent with that relation. Calibrating the $L_\mathrm{hX}$-$L_ν$ relation on the six published sources via a Bayesian regression with errors on both axes, the slope is consistent with $β= 1$ and the intrinsic scatter is $\sim 0.6$\,dex. All seven new BLAZARs are posterior-predictively consistent with this calibration ($χ^2_7 = 1.58$, $p = 0.98$) under the working hypothesis that the published IceCube $\hat{n}_s$ values reflect the signal. A null-injection test confirms that, at the present calibration sample size, the consistency test does not by itself adjudicate between signal and selected-background origins. A distance-free $L_\mathrm{hX}/L_ν$ ratio diagnostic places both populations within the photohadronic prediction band, statistically indistinguishable. Two diagnostics that control the common $d_L^{\,2}$ distance bias, a redshift-partial rank correlation ($τ|z = 0.69$, $\sim\!2.7\,σ$) and a flux-space permutation test on the 13-source joint sample ($p = 6.3\times10^{-4}$, $3.23\,σ$), indicate a residual $L_\mathrm{hX}$-$L_ν$ association beyond the distance-induced trend. We interpret these results as a conditional consistency check; a detection-level statement requires either an enlarged calibration set or an X-ray-weighted IceCube stacking likelihood with internal data.
[abstract 3 / 70] Wow! (score: 7) - Title: Testing the Correlations between X-ray Spectral Properties and Polarization for High Synchrotron Peaked BlazarsAuthors: M. Lynne Saade, Steven Ehlert, Ioannis Liodakis, Philip Kaaret, Fabrizio Tavecchio, Sara Capecchiacci, Riccardo Middei,Comments: Revised, submitted to MNRASSubjects: astro-ph.HECreated: 2026-06-26; Updated: 2026-06-30; Datestamp: 2026-06-30
IXPE has enabled the X-ray POLARIZATIONs of many BLAZARs to be measured. We perform the first population study for high SYNCHROTRON peaked BLAZARs observed using IXPE using a uniform X-ray data analysis. We find a potential statistically significant correlation between the X-ray spectral curvature and the X-ray POLARIZATION degree. More data is needed to determine whether this correlation is robust. The lack of any other correlations may imply that there is little connection between the energy distribution of the X-ray emitting electrons and the uniformity of the MAGNETic field in the X-ray emitting regions of these BLAZARs. These results will inform future theoretical work and potentially help narrow down the acceleration process of the SYNCHROTRON electrons.
[abstract 4 / 70] Wow! (score: 7) - Title: Modelling the delayed shock-breakout emission following JET-launching binary neutron star mergers via RELATIVISTIC MHD simulationsAuthors: Matteo Pais, Riccardo Ciolfi, Andrea Pavan,Comments: 17 pages, 14 figures, submittedSubjects: astro-ph.HE astro-ph.SR gr-qcCreated: 2026-06-28; Updated: 2026-06-30; Datestamp: 2026-06-30
In binary neutron star (BNS) mergers launching a RELATIVISTIC JET, an electroMAGNETic (EM) signal is produced when the JET-driven shock breaks out of the merger ejecta. The observed time delay of this shock-breakout (SBO) emission with respect to the gravitational-wave (GW) signal from the merger provides a powerful probe of the physical conditions governing JET launching and early-time JET propagation. Considering different models of JET propagation in realistic post-merger environments, we investigate the SBO emission and corresponding GW-EM delay that would be observed depending on the viewing angle and the assumed ejecta opacity. We perform RELATIVISTIC MHD simulations of JETs propagating through a post-merger environment directly imported from the outcome of a previous BNS merger simulation. We also introduce a specific procedure to faithfully reconstruct the early dynamical ejecta up to their natural front. The evolution is followed in 3D up to 0.6 s and then continued imposing axisymmetry and higher resolution. Varying JET launching time and luminosity, we identify three representative models spanning regimes from early breakout to extended JET choking. For each case, we track the JET-driven forward shock up to the photosphere and compute the angle-dependent bolometric SBO luminosity, assuming full conversion of the thermal energy within the shocked material into radiation, and taking into account non-radial photon propagation, RELATIVISTIC Doppler shifts, and light-travel-time effects. We consider two opacity values spanning a factor of 10. We find that the GW-EM delay depends weakly on both viewing angle and ejecta opacity, making it a robust diagnostic for constraining models. Comparing with GRB 170817A, the model resulting in a substantially choked JET provides the most plausible peak bolometric luminosity and the closest match to the observed GW-EM delay and signal duration.
[abstract 5 / 70] Wow! (score: 7) - Title: General Relativistic Shock Wave Solutions with Black Hole Formation: The Singular Isothermal Sphere CaseAuthors: Chien-Ting J. Chen, Michael J. Cai, Fabio Pacucci,Comments: 16 pages, 6 figures, 1 table. Submitted to ApJ. Comments welcomeSubjects: astro-ph.HE astro-ph.CO astro-ph.GA gr-qcCreated: 2026-06-28; Updated: 2026-06-30; Datestamp: 2026-06-30
The rapid emergence at $z\gtrsim 6$ of ubiquitous populations of supermassive BLACK HOLEs (SMBHs) revealed by JWST and of QUASARs with estimated masses $M_\bullet > 10^{10} M_\odot$ demands efficient pathways for early growth. The smooth collapse of a singular isothermal sphere (SIS) has been solved analytically in full general relativity, but the shock waves that inevitably accompany such collapse have not. Here, we derive general-RELATIVISTIC self-similar shock-wave solutions for the collapse of an SIS to a BLACK HOLE, extending the framework of Cai \& Shu (2005) to discontinuous flows. We obtain the general RELATIVISTIC jump conditions for an isothermal fluid and show that they connect interior collapse solutions to exterior envelopes that may be static, expanding, or collapsing, yielding a rich family of shocks propagating at up to $\sim$40\% the speed of light; the available exterior types narrow with increasing sound speed. A coordinate-matching technique that uses the zero-velocity surface uniquely bridges the Schwarzschild and comoving self-similar descriptions, completing the characterization of the growing BLACK HOLE. The central accretion rate is set by the interior collapse alone and is suppressed by a factor of $\sim$5--7 relative to the smooth expansion-wave solution, while the energy released at the shock reaches $\sim$10\% of the enclosed rest mass -- nearly twice the 5.7\% radiative efficiency of Schwarzschild accretion. These results provide an analytical energy budget for direct-collapse BLACK HOLE formation, with implications for SMBH seed assembly, the dense cocoons around nascent high-redshift BLACK HOLEs, the recently discovered JWST's Little Red Dots, and RELATIVISTIC transients such as GAMMA-RAY BURSTs.
[abstract 6 / 70] Wow! (score: 7) - Title: Magnetic Reconnection in Galaxy ClustersAuthors: Takuya Akahori, Kohei Kurahara, Shin-ya Nitta, Haruka Sakemi, Hiroki Akamatsu, Mami Machida, Motokazu Takizawa,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Akahori01. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.GACreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
Galaxy clusters contain an intra-cluster medium (ICM) with temperatures of tens of millions of Kelvin. Cosmological structure formation simulations show that this diffuse gas is heated not only by adiabatic gravitational compression but also by shock waves and turbulence generated during mergers of galaxy groups and clusters. These processes are expected to produce MAGNETic fields and COSMIC RAYs, observed through SYNCHROTRON POLARIZATION. One structure formed during cluster evolution is the cold front, a contact discontinuity created when colder gas moves transonically through hotter gas. Using MeerKAT, GMRT, and ATCA, we recently discovered radio emission along cold fronts in two galaxy clusters, with spectra indicating re-acceleration at the discontinuity. This presents a new puzzle because the standard mechanism in galaxy clusters, FERMI acceleration, is not naturally expected there. We propose MAGNETic RECONNECTion as the re-acceleration mechanism. Compression and stretching of MAGNETized plasma at the discontinuity can generate current sheets that trigger RECONNECTion, as also suggested by simulations. With AA*, we will probe broadband radio spectra at high spatial resolution to constrain where re-acceleration occurs. Polarization measurements will reveal MAGNETic-field structures and clarify the conditions required for MAGNETic RECONNECTion.
[abstract 7 / 70] Wow! (score: 7) - Title: Lighting Up the CGM: Strong, Jet-Aligned $Hα$ Emission around Radio GalaxiesAuthors: Namrata Roy, Sanchayeeta Borthakur, Timothy Heckman, Tanmay Singh,Comments: 10 pages (excluding Appendix), 5 figures, under review in ApJLSubjects: astro-ph.GACreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
A primary question within galaxy evolution is how ACTIVE GALACTIC NUCLEi (AGN) feedback modifies the circumgalactic medium (CGM). We present a search for faint H$α$ emission from the cool ionized CGM ($T\sim 10^4$ K) around RADIO GALAXies by stacking background-QUASAR spectra from DESI sightlines. We take into account the projected distance and position angle of each QUASAR sightline relative to the radio JET axis, and test whether JET--CGM coupling is anisotropic. We detect a strong H$α$ excess at $>5σ$ along the collimated radio JET axis ($θ<20^\circ$) with a mean integrated flux of $1.19\times10^{-17}\ {\rm erg\ cm^{-2}\ s^{-1}}$. In contrast, the azimuthally averaged stack over all 324 sightline angles yields no detection ($<2σ$), indicating that this excess emission is very localized along the radio JET. We also find that the JET-aligned H$α$ signal is radially structured, where the strongest emission occurs near the host galaxy just outside the optical half-light radius, and rising again near the projected radio-lobe region. The JET-aligned stacks reveal H$α$ signal that is roughly 100 times brighter than normal halos. In the same sightlines however, Mg II absorption shows no difference in incidence between JET-aligned and off-axis directions, with broadly similar equivalent widths, column densities, and line widths. This striking contrast shows that while Mg II traces the ambient, clumpy cool CGM reservoir, the H$α$ emission directly captures localized, low-covering-fraction clouds whose density, pressure, or ionization level has been dramatically boosted by the propagating JET. These results deliver clear evidence of localized JET-CGM interaction in radio-JETted AGNs.
[abstract 8 / 70] Yes (score: 6) - Title: Dual AGN and Multiple SMBH Systems in the Era of SKAOAuthors: Q. D'Amato, L. Cui, R. Deane, S. Komossa, C. Pillay, A. Tripathi, P. Kharb, H. Guo, S. Nandi, K. Rubinur, S. Anton, T. An, S. Bonoli, N. Chang, R. Dave, A. De Rosa, M. Habouzit, F. Mannucci, I. Prandoni, P. Severgnini, M. Scialpi, C. Spingola, C. Vignali, W. Xu, X. Yan, Y. Zhang,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-No: AASKAII/DAmato01. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.HE astro-ph.GACreated: 2026-06-26; Updated: 2026-06-30; Datestamp: 2026-06-30
We present a radio-oriented review of current strategies for the detection and characterization of dual ACTIVE GALACTIC NUCLEi (DAGN) and supermassive BLACK HOLE binaries (SMBHBs), emphasizing the crucial role of radio interferometry in advancing this field. We discuss how high-resolution radio imaging - particularly through very long baseline interferometry (VLBI) - provides a unique, dust-unbiased tool to identify multiple accreting SMBHs, disentangle AGN-related emission from STAR FORMATION, and trace components from tens of kpc to sub-parsec scales. We summarize current observational limitations, such as insufficient sensitivity-resolution combination and area coverage. We then outline how the SKAO will overcome these constraints through its unprecedented combination of sensitivity, survey speed, imaging fidelity and angular resolution, enabling the discovery and characterization of dual and binary SMBHs from the nearby Universe to the epoch of reionization. Several science cases are presented, including radio follow-ups of optical/infrared-selected DAGN, direct blind radio selection of DAGN, studies of compact bound SMBHBs, and the link between SMBHB orbital evolution and low-frequency gravitational wave emission. We further emphasize the synergy between SKAO observations and modern and upcoming facilities such as the James Webb and Euclid space telescopes, Rubin Observatory, and gravitational wave detectors including the Laser Interferometer Space Antenna and pulsar timing arrays. These combined capabilities will allow SKAO to enable the first comprehensive radio census of dual and binary SMBH systems, bridge the gap between electroMAGNETic and gravitational wave observations, and provide a statistically significant view of SMBH pairing, accretion, and merger-driven feedback throughout cosmic history.
[abstract 9 / 70] Yes (score: 6) - Title: Identifying Observational Signatures of Flux Eruption Events in Supermassive Black Hole Accretion Flows with Machine LearningAuthors: Angelo Ricarte, Erandi Chavez, Franc O, Pavlos Protopapas,Comments: Submitted to ApJ, 18 pages, 11 figures, 4 tablesSubjects: astro-ph.HECreated: 2026-06-26; Updated: 2026-06-30; Datestamp: 2026-06-30
Simulated BLACK HOLE accretion flows with strong MAGNETic fields often exhibit "flux eruption events" (FEEs), transient and localized expulsions of matter near the event horizon due to MAGNETic RECONNECTion. It may now be possible to image them with the Event Horizon Telescope (EHT), a global network of millimeter-wave observatories that images BLACK HOLEs. Here we use machine learning as an interpretable inference tool to identify observational signatures of FEEs that could be accessible to the EHT. First, we train a convolutional neural network to learn task-relevant representations of FEEs in uncorrupted simulated images. After using this network to label a larger set of images, we then train interpretable models (random forest and logistic regression) to determine observational signatures. We find that during a FEE, images in the millimeter tend toward more diffuse emission, higher linear POLARIZATION, and lower total fluxes, but these signatures are weak for most FEEs compared to the usual time variability of these features. Moreover, the Q-U loop rotation rate decreases during FEEs, contrary to a picture in which FEEs could jointly cause both millimeter Q-U loops and flares. Our random forest trained on observable summary statistics achieves ~80% class-weighted accuracy, suggesting that the CNN learns FEE structure not fully mapped onto these traditional summary statistics. Our results imply that image size and POLARIZATION fraction can be used to flag candidate FEEs, but high-resolution, high-dynamic range images will still be important to confirm FEEs and test accretion flows for this phenomenon.
[abstract 10 / 70] Yes (score: 5) - Title: GWTC-4.0: Methods for Identifying and Characterizing Gravitational-wave TransientsAuthors: The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration, A. G. Abac, I. Abouelfettouh, F. Acernese, K. Ackley, S. Adhicary, D. Adhikari, N. Adhikari, R. X. Adhikari, V. K. Adkins, S. Afroz, D. Agarwal, M. Agathos, M. Aghaei Abchouyeh, O. D. Aguiar, S. Ahmadzadeh, L. Aiello, A. Ain, P. Ajith, S. Akcay, T. Akutsu, S. Albanesi, R. A. Alfaidi, A. Al-Jodah, C. Alléné, A. Allocca, S. Al-Shammari, P. A. Altin, S. Alvarez-Lopez, O. Amarasinghe, A. Amato, C. Amra, A. Ananyeva, S. B. Anderson, W. G. Anderson, M. Andia, M. Ando, T. Andrade, M. Andrés-Carcasona, T. Andrić, J. Anglin, 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, J. S. Areeda, L. Argianas, N. Aritomi, F. Armato, S. Armstrong, N. Arnaud, M. Arogeti, S. M. Aronson, G. Ashton, Y. Aso, M. Assiduo, S. Assis de Souza Melo, S. M. Aston, P. Astone, F. Attadio, F. Aubin, K. AultONeal, G. Avallone, S. Babak, F. Badaracco, C. Badger, S. Bae, S. Bagnasco, E. Bagui, L. Baiotti, R. Bajpai, T. Baka, T. Baker, M. Ball, G. Ballardin, S. W. Ballmer, S. Banagiri, B. Banerjee, D. Bankar, T. M. Baptiste, P. Baral, J. C. Barayoga, B. C. Barish, D. Barker, N. Barman, P. Barneo, F. Barone, B. Barr, L. Barsotti, M. Barsuglia, D. Barta, A. M. Bartoletti, M. A. Barton, I. Bartos, S. Basak, A. Basalaev, R. Bassiri, A. Basti, D. E. Bates, 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, D. S. Bellie, L. Bellizzi, W. Benoit, I. Bentara, J. D. Bentley, M. Ben Yaala, S. Bera, F. Bergamin, B. K. Berger, S. Bernuzzi, M. Beroiz, C. P. L. Berry, D. Bersanetti, A. Bertolini, J. Betzwieser, D. Beveridge, G. Bevilacqua, N. Bevins, R. Bhandare, S. A. Bhat, R. Bhatt, D. Bhattacharjee, S. Bhaumik, S. Bhowmick, V. Biancalana, A. Bianchi, I. A. Bilenko, G. Billingsley, A. Binetti, S. Bini, C. Binu, 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, F. Bobba, N. Bode, G. Boileau, M. Boldrini, G. N. Bolingbroke, A. Bolliand, L. D. Bonavena, R. Bondarescu, F. Bondu, E. Bonilla, M. S. Bonilla, A. Bonino, R. Bonnand, P. Booker, A. Borchers, S. Borhanian, V. Boschi, S. Bose, V. Bossilkov, A. Boudon, A. Bozzi, C. Bradaschia, P. R. Brady, A. Branch, M. Branchesi, I. Braun, 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, G. S. Cabourn Davies, G. Cabras, R. Cabrita, V. Cáceres-Barbosa, L. Cadonati, G. Cagnoli, C. Cahillane, A. Calafat, J. Calderón Bustillo, T. A. Callister, E. Calloni, G. Caneva Santoro, K. C. Cannon, H. Cao, L. A. Capistran, E. Capocasa, E. Capote, G. Capurri, G. Carapella, F. Carbognani, M. Carlassara, J. B. Carlin, T. K. Carlson, M. F. Carney, M. Carpinelli, G. Carrillo, J. J. Carter, G. Carullo, J. Casanueva Diaz, C. Casentini, S. Y. Castro-Lucas, S. Caudill, M. Cavaglià, R. Cavalieri, G. Cella, P. Cerdá-Durán, E. Cesarini, W. Chaibi, P. Chakraborty, S. Chakraborty, S. Chalathadka Subrahmanya, J. C. L. Chan, M. Chan, R. -J. Chang, S. Chao, E. L. Charlton, P. Charlton, E. Chassande-Mottin, C. Chatterjee, Debarati Chatterjee, Deep Chatterjee, M. Chaturvedi, S. Chaty, K. Chatziioannou, C. Checchia, A. Chen, A. H. -Y. Chen, D. Chen, H. Chen, H. Y. Chen, S. Chen, Y. Chen, Yanbei Chen, Yitian Chen, H. P. Cheng, P. Chessa, H. T. Cheung, S. Y. Cheung, F. Chiadini, G. Chiarini, R. Chierici, A. Chincarini, M. L. Chiofalo, A. Chiummo, C. Chou, S. Choudhary, N. Christensen, S. S. Y. Chua, P. Chugh, G. Ciani, P. Ciecielag, M. Cieślar, M. Cifaldi, R. Ciolfi, F. Clara, J. A. Clark, J. Clarke, T. A. Clarke, P. Clearwater, S. Clesse, S. M. Clyne, E. Coccia, E. Codazzo, P. -F. Cohadon, S. Colace, E. Colangeli, 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, A. Corsi, S. Cortese, R. Cottingham, M. W. Coughlin, A. Couineaux, J. -P. Coulon, J. -F. Coupechoux, P. Couvares, D. M. Coward, R. Coyne, K. Craig, J. D. E. Creighton, T. D. Creighton, P. Cremonese, A. W. Criswell, S. Crook, R. Crouch, J. Csizmazia, J. R. Cudell, T. J. Cullen, A. Cumming, E. Cuoco, M. Cusinato, P. Dabadie, L. V. Da Conceição, T. Dal Canton, S. Dall'Osso, S. Dal Pra, G. Dálya, B. D'Angelo, S. Danilishin, S. D'Antonio, K. Danzmann, K. E. Darroch, L. P. Dartez, A. Dasgupta, S. Datta, V. Dattilo, A. Daumas, N. Davari, I. Dave, A. Davenport, M. Davier, T. F. Davies, D. Davis, L. Davis, M. C. Davis, P. Davis, M. Dax, J. De Bolle, M. Deenadayalan, J. Degallaix, U. Deka, M. De Laurentis, S. Deléglise, F. De Lillo, D. Dell'Aquila, F. Della Valle, W. Del Pozzo, F. De Marco, G. Demasi, F. De Matteis, V. D'Emilio, N. Demos, T. Dent, A. Depasse, N. DePergola, R. De Pietri, R. De Rosa, C. De Rossi, M. Desai, R. DeSalvo, A. DeSimone, R. De Simone, A. Dhani, R. Diab, M. C. Díaz, M. Di Cesare, G. Dideron, N. A. Didio, T. Dietrich, L. Di Fiore, C. Di Fronzo, M. Di Giovanni, T. Di Girolamo, D. Diksha, A. Di Michele, J. Ding, S. Di Pace, I. Di Palma, F. Di Renzo, Divyajyoti, A. Dmitriev, Z. Doctor, N. Doerksen, E. Dohmen, D. Dominguez, L. D'Onofrio, F. Donovan, K. L. Dooley, T. Dooney, S. Doravari, O. Dorosh, M. Drago, J. C. Driggers, J. -G. Ducoin, L. Dunn, U. Dupletsa, D. D'Urso, H. Duval, S. E. Dwyer, C. Eassa, M. Ebersold, T. Eckhardt, G. Eddolls, B. Edelman, T. B. Edo, O. Edy, A. Effler, J. Eichholz, H. Einsle, M. Eisenmann, R. A. Eisenstein, A. Ejlli, M. Emma, K. Endo, R. Enficiaud, A. J. Engl, 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, F. Faedi, V. Fafone, S. Fairhurst, A. M. Farah, B. Farr, W. M. Farr, G. Favaro, M. Favata, M. Fays, M. Fazio, J. Feicht, M. M. Fejer, R. Felicetti, E. Fenyvesi, D. L. Ferguson, T. Fernandes, D. Fernando, S. Ferraiuolo, I. Ferrante, T. A. Ferreira, 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, C. Foo, B. Fornal, P. W. F. Forsyth, K. Franceschetti, N. Franchini, S. Frasca, F. Frasconi, A. Frattale Mascioli, Z. Frei, A. Freise, O. Freitas, R. Frey, W. Frischhertz, P. Fritschel, V. V. Frolov, G. G. Fronzé, M. Fuentes-Garcia, S. Fujii, T. Fujimori, P. Fulda, M. Fyffe, B. Gadre, J. R. Gair, S. Galaudage, V. Galdi, H. Gallagher, B. Gallego, R. Gamba, A. Gamboa, D. Ganapathy, A. Ganguly, B. Garaventa, J. García-Bellido, C. García Núñez, C. García-Quirós, J. W. Gardner, K. A. Gardner, J. Gargiulo, 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, D. T. Gibson, C. Gier, S. Gkaitatzis, J. Glanzer, F. Glotin, J. Godfrey, P. Godwin, A. S. Goettel, E. Goetz, J. Golomb, S. Gomez Lopez, B. Goncharov, Y. Gong, G. González, P. Goodarzi, S. Goode, A. W. Goodwin-Jones, M. Gosselin, R. Gouaty, D. W. Gould, K. Govorkova, S. Goyal, B. Grace, A. Grado, V. Graham, A. E. Granados, M. Granata, V. Granata, S. Gras, P. Grassia, A. Gray, C. Gray, R. Gray, G. Greco, A. C. Green, S. M. Green, S. R. Green, A. M. Gretarsson, E. M. Gretarsson, D. Griffith, W. L. Griffiths, H. L. Griggs, G. Grignani, C. Grimaud, H. Grote, S. Grunewald, D. Guerra, D. Guetta, G. M. Guidi, A. R. Guimaraes, H. K. Gulati, F. Gulminelli, A. M. Gunny, H. Guo, W. Guo, Y. Guo, Anchal Gupta, Anuradha Gupta, I. Gupta, N. C. Gupta, P. Gupta, S. K. Gupta, T. Gupta, V. Gupta, N. Gupte, J. Gurs, N. Gutierrez, F. Guzman, D. Haba, M. Haberland, S. Haino, E. D. Hall, R. Hamburg, E. Z. Hamilton, G. Hammond, W. -B. Han, M. Haney, J. Hanks, C. Hanna, M. D. Hannam, O. A. Hannuksela, A. G. Hanselman, H. Hansen, J. Hanson, R. Harada, A. R. Hardison, S. Harikumar, K. Haris, T. Harmark, J. Harms, G. M. Harry, I. W. Harry, J. Hart, B. Haskell, C. -J. Haster, K. Haughian, H. Hayakawa, K. Hayama, R. Hayes, M. C. Heintze, J. Heinze, J. Heinzel, H. Heitmann, A. Heffernan, F. Hellman, A. F. Helmling-Cornell, G. Hemming, O. Henderson-Sapir, M. Hendry, I. S. Heng, M. H. Hennig, C. Henshaw, M. Heurs, A. L. Hewitt, J. Heyns, S. Higginbotham, S. Hild, S. Hill, Y. Himemoto, N. Hirata, C. Hirose, S. Hochheim, D. Hofman, N. A. Holland, D. E. Holz, L. Honet, C. Hong, S. Hoshino, J. Hough, S. Hourihane, N. T. Howard, E. J. Howell, C. G. Hoy, C. A. Hrishikesh, H. -F. Hsieh, H. -Y. Hsieh, C. Hsiung, W. -F. Hsu, Q. Hu, H. Y. Huang, Y. Huang, Y. T. Huang, A. D. Huddart, B. Hughey, D. C. Y. Hui, V. Hui, S. Husa, R. Huxford, L. Iampieri, G. A. Iandolo, M. Ianni, A. Ierardi, A. Iess, H. Imafuku, K. Inayoshi, Y. Inoue, G. Iorio, P. Iosif, M. H. Iqbal, J. Irwin, R. Ishikawa, M. Isi, Y. Itoh, H. Iwanaga, M. Iwaya, B. R. Iyer, C. Jacquet, P. -E. Jacquet, S. J. Jadhav, S. P. Jadhav, T. Jain, A. L. James, P. A. James, R. Jamshidi, A. Jan, K. Jani, J. Janquart, K. Janssens, N. N. Janthalur, S. Jaraba, P. Jaranowski, R. Jaume, W. Javed, A. Jennings, W. Jia, J. Jiang, S. J. Jin, C. Johanson, G. R. Johns, N. A. Johnson, N. K. Johnson-McDaniel, M. C. Johnston, R. Johnston, N. Johny, D. H. Jones, D. I. Jones, E. J. Jones, R. Jones, S. Jose, P. Joshi, S. K. Joshi, J. Ju, L. Ju, K. Jung, J. Junker, V. Juste, H. B. Kabagoz, T. Kajita, I. Kaku, V. Kalogera, M. Kalomenopoulos, M. Kamiizumi, N. Kanda, S. Kandhasamy, G. Kang, N. C. Kannachel, J. B. Kanner, S. J. Kapadia, D. P. Kapasi, S. Karat, R. Kashyap, M. Kasprzack, W. Kastaun, T. Kato, E. Katsavounidis, W. Katzman, R. Kaushik, K. Kawabe, R. Kawamoto, A. Kazemi, D. Keitel, J. Kennington, R. Kesharwani, J. S. Key, R. Khadela, S. Khadka, F. Y. Khalili, F. Khan, I. Khan, T. Khanam, M. Khursheed, N. M. Khusid, W. Kiendrebeogo, N. Kijbunchoo, C. Kim, J. C. Kim, K. Kim, M. H. Kim, S. Kim, Y. -M. Kim, C. Kimball, M. Kinley-Hanlon, M. Kinnear, J. S. Kissel, S. Klimenko, A. M. Knee, N. Knust, K. Kobayashi, P. Koch, S. M. Koehlenbeck, G. Koekoek, K. Kohri, K. Kokeyama, S. Koley, P. Kolitsidou, K. Komori, A. K. H. Kong, A. Kontos, M. Korobko, R. V. Kossak, X. Kou, A. Koushik, N. Kouvatsos, M. Kovalam, D. B. Kozak, S. L. Kranzhoff, V. Kringel, N. V. Krishnendu, A. Królak, K. Kruska, J. Kubisz, G. Kuehn, S. Kulkarni, A. Kulur Ramamohan, A. Kumar, Praveen Kumar, Prayush Kumar, Rahul Kumar, Rakesh Kumar, J. Kume, K. Kuns, N. Kuntimaddi, S. Kuroyanagi, S. Kuwahara, K. Kwak, K. Kwan, J. Kwok, G. Lacaille, P. Lagabbe, D. Laghi, S. Lai, E. Lalande, M. Lalleman, P. C. Lalremruati, M. Landry, B. B. Lane, R. N. Lang, J. Lange, R. Langgin, B. Lantz, A. La Rana, I. La Rosa, J. Larsen, A. Lartaux-Vollard, P. D. Lasky, J. Lawrence, M. N. Lawrence, M. Laxen, C. Lazarte, A. Lazzarini, C. Lazzaro, P. Leaci, L. Leali, Y. K. Lecoeuche, H. M. Lee, H. W. Lee, J. Lee, K. Lee, R. -K. Lee, R. Lee, Sungho Lee, Sunjae Lee, Y. Lee, I. N. Legred, J. Lehmann, L. Lehner, M. Le Jean, A. Lemaî, M. Lenti, M. Leonardi, M. Lequime, N. Leroy, M. Lesovsky, N. Letendre, M. Lethuillier, Y. Levin, K. Leyde, A. K. Y. Li, K. L. Li, T. G. F. Li, X. Li, Y. Li, Z. Li, A. Lihos, C-Y. Lin, E. T. Lin, L. C. -C. Lin, Y. -C. Lin, C. Lindsay, S. D. Linker, T. B. Littenberg, A. Liu, G. C. Liu, Jian Liu, F. Llamas Villarreal, J. Llobera-Querol, R. K. L. Lo, J. -P. Locquet, M. R. Loizou, L. T. London, A. Longo, D. Lopez, M. Lopez Portilla, A. Lorenzo-Medina, V. Loriette, M. Lormand, G. Losurdo, E. Lotti, T. P. Lott, J. D. Lough, H. A. Loughlin, C. O. Lousto, N. Low, M. J. Lowry, N. Lu, L. Lucchesi, H. Lück, D. Lumaca, A. P. Lundgren, A. W. Lussier, L. -T. Ma, S. Ma, R. Macas, A. Macedo, M. MacInnis, R. R. Maciy, D. M. Macleod, I. A. O. MacMillan, A. Macquet, D. Macri, K. Maeda, S. Maenaut, S. S. Magare, R. M. Magee, E. Maggio, R. Maggiore, M. Magnozzi, M. Mahesh, M. Maini, S. Majhi, E. Majorana, C. N. Makarem, D. Malakar, J. A. Malaquias-Reis, U. Mali, S. Maliakal, A. Malik, L. Mallick, A. Malz, N. Man, V. Mandic, V. Mangano, B. Mannix, G. L. Mansell, G. Mansingh, M. Manske, M. Mantovani, M. Mapelli, F. Marchesoni, C. Marinelli, D. Marín Pina, F. Marion, S. Márka, Z. Márka, A. S. Markosyan, A. Markowitz, E. Maros, S. Marsat, F. Martelli, I. W. Martin, R. M. Martin, B. B. Martinez, M. Martinez, V. Martinez, A. Martini, J. C. Martins, D. V. Martynov, E. J. Marx, L. Massaro, A. Masserot, M. Masso-Reid, M. Mastrodicasa, S. Mastrogiovanni, T. Matcovich, M. Matiushechkina, M. Matsuyama, N. Mavalvala, N. Maxwell, G. McCarrol, R. McCarthy, D. E. McClelland, S. McCormick, L. McCuller, S. McEachin, C. McElhenny, G. I. McGhee, J. McGinn, K. B. M. McGowan, J. McIver, A. McLeod, T. McRae, D. Meacher, Q. Meijer, A. Melatos, M. Melching, S. Mellaerts, C. S. Menoni, F. Mera, R. A. Mercer, L. Mereni, K. Merfeld, E. L. Merilh, J. R. Mérou, J. D. Merritt, M. Merzougui, C. Messenger, C. Messick, B. Mestichelli, M. Meyer-Conde, F. Meylahn, A. Mhaske, A. Miani, H. Miao, I. Michaloliakos, C. Michel, Y. Michimura, H. Middleton, S. J. Miller, M. Millhouse, E. Milotti, V. Milotti, Y. Minenkov, N. Mio, Ll. M. Mir, L. Mirasola, M. Miravet-Tenés, C. -A. Miritescu, A. K. Mishra, A. Mishra, C. Mishra, T. Mishra, A. L. Mitchell, J. G. Mitchell, S. Mitra, V. P. Mitrofanov, R. Mittleman, O. Miyakawa, S. Miyamoto, S. Miyoki, G. Mo, L. Mobilia, S. R. P. Mohapatra, S. R. Mohite, M. Molina-Ruiz, C. Mondal, M. Mondin, M. Montani, C. J. Moore, D. Moraru, A. More, S. More, E. A. Moreno, G. Moreno, S. Morisaki, Y. Moriwaki, G. Morras, A. Moscatello, M. Mould, P. Mourier, B. Mours, C. M. Mow-Lowry, F. Muciaccia, D. Mukherjee, Samanwaya Mukherjee, Soma Mukherjee, Subroto Mukherjee, Suvodip Mukherjee, N. Mukund, A. Mullavey, H. Mullock, J. Munch, J. Mundi, C. L. Mungioli, Y. Murakami, M. Murakoshi, P. G. Murray, S. Muusse, D. Nabari, S. L. Nadji, A. Nagar, N. Nagarajan, K. Nakagaki, K. Nakamura, H. Nakano, M. Nakano, D. Nanadoumgar-Lacroze, D. Nandi, V. Napolano, P. Narayan, I. Nardecchia, T. Narikawa, H. Narola, L. Naticchioni, R. K. Nayak, A. Nela, A. Nelson, T. J. N. Nelson, M. Nery, A. Neunzert, S. Ng, L. Nguyen Quynh, S. A. Nichols, A. B. Nielsen, G. Nieradka, Y. Nishino, A. Nishizawa, S. Nissanke, E. Nitoglia, W. Niu, F. Nocera, M. Norman, C. North, J. Novak, J. F. Nuño Siles, L. K. Nuttall, K. Obayashi, J. Oberling, J. O'Dell, M. Oertel, A. Offermans, G. Oganesyan, J. J. Oh, K. Oh, T. O'Hanlon, M. Ohashi, M. Ohkawa, F. Ohme, R. Oliveri, R. Omer, B. O'Neal, K. Oohara, B. O'Reilly, R. Oram, N. D. Ormsby, M. Orselli, R. O'Shaughnessy, S. O'Shea, Y. Oshima, S. Oshino, C. Osthelder, I. Ota, D. J. Ottaway, A. Ouzriat, H. Overmier, B. J. Owen, A. E. Pace, R. Pagano, M. A. Page, A. Pai, L. Paiella, A. Pal, S. Pal, M. A. Palaia, M. Pálfi, P. P. Palma, C. Palomba, P. Palud, J. Pan, K. C. Pan, R. Panai, P. K. Panda, Shiksha Pandey, Swadha Pandey, P. T. H. Pang, F. Pannarale, K. A. Pannone, B. C. Pant, F. H. Panther, F. Paoletti, A. Paolone, A. Papadopoulos, E. E. Papalexakis, L. Papalini, G. Papigkiotis, A. Paquis, A. Parisi, B. -J. Park, J. Park, W. Parker, G. Pascale, D. Pascucci, A. Pasqualetti, R. Passaquieti, L. Passenger, D. Passuello, O. Patane, D. Pathak, L. Pathak, A. Patra, B. Patricelli, A. S. Patron, B. G. Patterson, K. Paul, S. Paul, E. Payne, T. Pearce, M. Pedraza, A. Pele, F. E. Peña Arellano, S. Penn, M. D. Penuliar, A. Perego, Z. Pereira, J. J. Perez, C. Périgois, G. Perna, A. Perreca, J. Perret, S. Perriès, J. W. Perry, D. Pesios, S. Petracca, C. Petrillo, H. P. Pfeiffer, H. Pham, K. A. Pham, K. S. Phukon, H. Phurailatpam, M. Piarulli, L. Piccari, O. J. Piccinni, M. Pichot, M. Piendibene, F. Piergiovanni, L. Pierini, G. Pierra, V. Pierro, M. Pietrzak, M. Pillas, F. Pilo, L. Pinard, I. M. Pinto, M. Pinto, B. J. Piotrzkowski, M. Pirello, M. D. Pitkin, A. Placidi, E. Placidi, M. L. Planas, W. Plastino, C. Plunkett, R. Poggiani, E. Polini, L. Pompili, J. Poon, E. Porcelli, E. K. Porter, C. Posnansky, R. Poulton, J. Powell, M. Pracchia, B. K. Pradhan, T. Pradier, A. K. Prajapati, K. Prasai, R. Prasanna, P. Prasia, G. Pratten, G. Principe, M. Principe, G. A. Prodi, L. Prokhorov, P. Prosperi, P. Prosposito, A. C. Providence, A. Puecher, J. Pullin, M. Punturo, P. Puppo, M. Pürrer, H. Qi, J. Qin, G. Quéméner, V. Quetschke, P. J. Quinonez, F. J. Raab, I. Rainho, S. Raja, C. Rajan, B. Rajbhandari, K. E. Ramirez, F. A. Ramis Vidal, A. Ramos-Buades, D. Rana, S. Ranjan, K. Ransom, P. Rapagnani, B. Ratto, A. Ray, V. Raymond, M. Razzano, J. Read, M. Recaman Payo, T. Regimbau, L. Rei, S. Reid, D. H. Reitze, P. Relton, A. I. Renzini, A. Renzini, B. Revenu, R. Reyes, A. S. Rezaei, F. Ricci, M. Ricci, A. Ricciardone, J. W. Richardson, M. Richardson, A. Rijal, K. Riles, H. K. Riley, S. Rinaldi, J. Rittmeyer, C. Robertson, F. Robinet, M. Robinson, A. Rocchi, L. Rolland, J. G. Rollins, A. E. Romano, R. Romano, A. Romero, I. M. Romero-Shaw, J. H. Romie, S. Ronchini, T. J. Roocke, L. Rosa, T. J. Rosauer, C. A. Rose, D. Rosińska, M. P. Ross, M. Rossello-Sastre, S. Rowan, S. Roy, S. K. Roy, D. Rozza, P. Ruggi, N. Ruhama, E. Ruiz Morales, K. Ruiz-Rocha, S. Sachdev, T. Sadecki, J. Sadiq, P. Saffarieh, S. Safi-Harb, M. R. Sah, S. Saha, T. Sainrat, S. Sajith Menon, K. Sakai, M. Sakellariadou, S. Sakon, O. S. Salafia, F. Salces-Carcoba, L. Salconi, M. Saleem, F. Salemi, M. Sallé, S. U. Salunkhe, S. Salvador, A. Samajdar, A. Sanchez, E. J. Sanchez, J. H. Sanchez, L. E. Sanchez, N. Sanchis-Gual, J. R. Sanders, E. M. Sänger, F. Santoliquido, F. Sarandrea, T. R. Saravanan, N. Sarin, P. Sarkar, S. Sasaoka, A. Sasli, P. Sassi, B. Sassolas, B. S. Sathyaprakash, R. Sato, Y. Sato, O. Sauter, R. L. Savage, T. Sawada, H. L. Sawant, S. Sayah, V. Scacco, D. Schaetzl, M. Scheel, A. Schiebelbein, M. G. Schiworski, P. Schmidt, S. Schmidt, R. Schnabel, M. Schneewind, R. M. S. Schofield, K. Schouteden, B. W. Schulte, B. F. Schutz, E. Schwartz, M. Scialpi, J. Scott, S. M. Scott, R. M. Sedas, T. C. Seetharamu, M. Seglar-Arroyo, Y. Sekiguchi, D. Sellers, A. S. Sengupta, D. Sentenac, E. G. Seo, J. W. Seo, V. Sequino, M. Serra, G. Servignat, A. Sevrin, T. Shaffer, U. S. Shah, M. S. Shahriar, M. A. Shaikh, L. Shao, A. Sharma, A. K. Sharma, P. Sharma, S. Sharma Chaudhary, M. R. Shaw, P. Shawhan, N. S. Shcheblanov, Y. Shikano, M. Shikauchi, K. Shimode, H. Shinkai, J. Shiota, S. Shirke, D. H. Shoemaker, D. M. Shoemaker, R. W. Short, S. ShyamSundar, A. Sider, H. Siegel, D. Sigg, L. Silenzi, M. Simmonds, L. P. Singer, A. Singh, D. Singh, M. K. Singh, N. Singh, S. Singh, A. Singha, A. M. Sintes, V. Sipala, V. Skliris, B. J. J. Slagmolen, D. A. Slater, T. J. Slaven-Blair, J. Smetana, J. R. Smith, L. Smith, R. J. E. Smith, W. J. Smith, K. Somiya, I. Song, K. Soni, S. Soni, V. Sordini, F. Sorrentino, H. Sotani, A. Southgate, F. Spada, V. Spagnuolo, A. P. Spencer, M. Spera, P. Spinicelli, C. A. Sprague, A. K. Srivastava, F. Stachurski, D. A. Steer, N. Steinle, J. Steinlechner, S. Steinlechner, N. Stergioulas, P. Stevens, S. P. Stevenson, F. Stolzi, M. StPierre, G. Stratta, M. D. Strong, A. Strunk, R. Sturani, A. L. Stuver, M. Suchenek, S. Sudhagar, N. Sueltmann, L. Suleiman, J. M. Sullivan, K. D. Sullivan, J. Sun, L. Sun, S. Sunil, J. Suresh, B. J. Sutton, P. J. Sutton, T. Suzuki, Y. Suzuki, B. L. Swinkels, A. Syx, M. J. Szczepańczyk, P. Szewczyk, M. Tacca, H. Tagoshi, S. C. Tait, H. Takahashi, R. Takahashi, A. Takamori, T. Takase, K. Takatani, H. Takeda, K. Takeshita, C. Talbot, M. Tamaki, N. Tamanini, D. Tanabe, K. Tanaka, S. J. Tanaka, T. Tanaka, D. Tang, S. Tanioka, D. B. Tanner, W. Tanner, L. Tao, R. D. Tapia, E. N. Tapia San Martín, R. Tarafder, C. Taranto, A. Taruya, J. D. Tasson, J. G. Tau, R. Tenorio, H. Themann, A. Theodoropoulos, M. P. Thirugnanasambandam, L. M. Thomas, M. Thomas, P. Thomas, J. E. Thompson, S. R. Thondapu, K. A. Thorne, E. Thrane, S. Tibrewal, J. Tissino, A. Tiwari, P. Tiwari, S. Tiwari, V. Tiwari, M. R. Todd, A. M. Toivonen, K. Toland, A. E. Tolley, T. Tomaru, K. Tomita, V. Tommasini, T. Tomura, H. Tong, C. Tong-Yu, A. Toriyama, N. Toropov, A. Torres-Forné, C. I. Torrie, M. Toscani, I. Tosta e Melo, E. Tournefier, M. Trad Nery, A. Trapananti, F. Travasso, G. Traylor, C. Trejo, M. Trevor, M. C. Tringali, A. Tripathee, G. Troian, A. Trovato, L. Trozzo, R. J. Trudeau, T. T. L. Tsang, S. Tsuchida, L. Tsukada, K. Turbang, M. Turconi, C. Turski, H. Ubach, N. Uchikata, T. Uchiyama, R. P. Udall, T. Uehara, M. Uematsu, S. Ueno, V. Undheim, T. Ushiba, M. Vacatello, H. Vahlbruch, G. Vajente, A. Vajpeyi, G. Valdes, J. Valencia, A. F. Valentini, M. Valentini, S. A. Vallejo-Peña, S. Vallero, V. Valsan, N. van Bakel, M. van Beuzekom, M. van Dael, J. F. J. van den Brand, C. Van Den Broeck, D. C. Vander-Hyde, M. van der Sluys, A. Van de Walle, J. van Dongen, K. Vandra, H. van Haevermaet, J. V. van Heijningen, P. Van Hove, J. Vanier, M. VanKeuren, J. Vanosky, M. H. P. M. van Putten, Z. Van Ranst, N. van Remortel, M. Vardaro, A. F. Vargas, J. J. Varghese, V. Varma, A. N. Vazquez, A. Vecchio, G. Vedovato, J. Veitch, P. J. Veitch, S. Venikoudis, J. Venneberg, P. Verdier, M. Vereecken, D. Verkindt, B. Verma, P. Verma, Y. Verma, S. M. Vermeulen, F. Vetrano, A. Veutro, A. M. Vibhute, A. Viceré, S. Vidyant, A. D. Viets, A. Vijaykumar, A. Vilkha, V. Villa-Ortega, E. T. Vincent, J. -Y. Vinet, S. Viret, A. Virtuoso, S. Vitale, A. Vives, H. Vocca, D. Voigt, E. R. G. von Reis, J. S. A. von Wrangel, L. Vujeva, S. P. Vyatchanin, J. Wack, L. E. Wade, M. Wade, K. J. Wagner, A. Wajid, M. Walker, G. S. Wallace, L. Wallace, E. J. Wang, H. Wang, J. Z. Wang, W. H. Wang, Y. F. Wang, Z. Wang, G. Waratkar, J. Warner, M. Was, T. Washimi, N. Y. Washington, D. Watarai, K. E. Wayt, B. R. Weaver, B. Weaver, C. R. Weaving, S. A. Webster, N. L. Weickhardt, M. Weinert, A. J. Weinstein, R. Weiss, F. Wellmann, L. Wen, P. Weßels, K. Wette, J. T. Whelan, B. F. Whiting, C. Whittle, E. G. Wickens, J. B. Wildberger, D. Wilken, D. J. Willadsen, K. Willetts, D. Williams, M. J. Williams, N. S. Williams, J. L. Willis, B. Willke, M. Wils, C. W. Winborn, J. Winterflood, C. C. Wipf, G. Woan, J. Woehler, N. E. Wolfe, H. T. Wong, I. C. F. Wong, J. L. Wright, M. Wright, C. Wu, D. S. Wu, H. Wu, E. Wuchner, D. M. Wysocki, V. A. Xu, Y. Xu, N. Yadav, H. Yamamoto, K. Yamamoto, T. S. Yamamoto, T. Yamamoto, S. Yamamura, R. Yamazaki, T. Yan, F. W. Yang, F. Yang, K. Z. Yang, Y. Yang, Z. Yarbrough, H. Yasui, S. -W. Yeh, A. B. Yelikar, X. Yin, J. Yokoyama, T. Yokozawa, J. Yoo, H. Yu, S. Yuan, H. Yuzurihara, A. Zadrożny, M. Zanolin, M. Zeeshan, T. Zelenova, J. -P. Zendri, M. Zeoli, M. Zerrad, M. Zevin, A. C. Zhang, L. Zhang, R. Zhang, T. Zhang, Y. Zhang, C. Zhao, Yue Zhao, Yuhang Zhao, Y. Zheng, H. Zhong, R. Zhou, X. -J. Zhu, Z. -H. Zhu, A. B. Zimmerman, M. E. Zucker, J. Zweizig,Comments: As part of the Astrophysical Journal Letters Focus Issue on the Gravitational Wave Transient Catalog. Published versionSubjects: gr-qc astro-ph.HECreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
The Gravitational-Wave Transient Catalog (GWTC) is a collection of candidate gravitational-wave transient signals identified and characterized by the LIGO-Virgo-KAGRA Collaboration. Producing the contents of the GWTC from detector data requires complex analysis methods. These comprise techniques to model the signal; identify the transients in the data; evaluate the quality of the data and mitigate possible instrumental issues; infer the parameters of each transient; compare the data with the waveform models for compact binary coalescences; and handle the large amount of results associated with all these different analyses. In this paper, we describe the methods employed to produce the catalog's fourth release, GWTC-4.0, focusing on the analysis of the first part of the fourth observing run of Advanced LIGO, Advanced Virgo and KAGRA.
[abstract 11 / 70] Yes (score: 5) - Title: Known changing-look AGN located within Rubin Deep Drilling FieldsAuthors: Mariangella Camus, Swayamtrupta Panda,Comments: 4 pages, 1 figure, submitted to Research Notes in AASSubjects: astro-ph.GA astro-ph.HECreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
Changing-look ACTIVE GALACTIC NUCLEi (CL-AGN) exhibit spectroscopic and photometric changes on timescales of months to years, making them powerful laboratories for studying accretion variability onto supermassive BLACK HOLEs. Motivated by the growing relevance of large spectro-photometric time-domain surveys, especially the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST), we compiled a master catalog of known CL-AGN from the literature and evaluated its spatial overlap with the Rubin survey footprint. Using a geometric cross-match based on sky coordinates, we identify 79 sources located in high-cadence regions of the main survey footprint (Wide-Fast-Deep, or WFD), including 5 particularly favorable targets lying within the Deep Drilling Fields (DDFs) of COSMOS and XMM-LSS. These sources represent especially promising candidates for future variability studies in the Rubin era. This Research Note presents a first proof of concept for connecting known CL-AGN with Rubin observing fields, while the full catalog and a more comprehensive analysis will be presented in a forthcoming paper.
[abstract 12 / 70] Yes (score: 5) - Title: EP260321a/SN 2026gzf: The Faintest Shock Breakout Associated with a Broad-Lined SupernovaAuthors: Brendan O'Connor, Xander J. Hall, Malte Busmann, Daniel Gruen, Alberto Floris, Tomas Cabrera, Ziyuan Zhu, Antonella Palmese, Dylan Green, John Banovetz, Julius Gassert, Christopher L. Fryer, Roberto Ricci, Eleonora Troja, Surya Shivaprasad, Gregory R. Zeimann, Ariel J. Amsellem, Stephen Bailey, Segev BenZvi, Simone Dichiara, Hendrik van Eerten, Jeremy Hare, Lei Hu, Christopher M. Irwin, Keerthi Kunnumkai, Konstantin Malanchev, Mitra Maleki, Michael J. Moss, Adam D. Myers, Dheeraj Pasham, Christoph Ries, Geoffrey Ryan, David Schlegel, Michael Schmidt, Silona Wilke, Yu-Han Yang,Comments: Accepted for publication in ApJL on June 26, 2026Subjects: astro-ph.HECreated: 2026-06-26; Updated: 2026-06-30; Datestamp: 2026-06-30
The explosion of a star is first marked by the shock wave breaking out of the stellar surface, producing a burst of ultraviolet and X-ray radiation. These events are observationally rare, despite likely accompanying the majority of SUPERNOVAe. Here, we report on our multi-wavelength observing campaign of the closest Einstein Probe fast X-ray transient EP260321a at $z=0.0344$. The thermal ($kT=130$ eV) X-ray emission with peak luminosity $1.0\times10^{45}$ erg s$^{-1}$ points to a shock breakout origin. We demonstrate that EP260321a is accompanied by a broad-lined Type Ic SUPERNOVA, SN 2026gzf. The SUPERNOVA properties, including its spectral evolution, lightcurve evolution, and expansion velocities, are all typical of the energetic stripped-envelope SUPERNOVAe associated with GAMMA-RAY BURSTs. However, deep X-ray upper limits obtained with the \textit{Chandra X-ray Observatory} do not detect an X-ray afterglow, and instead exclude the afterglow of known GAMMA-RAY BURSTs or fast X-ray transients. If the stellar explosion launched a successful RELATIVISTIC JET, we require that it had both a low Lorentz factor $Γ_0$\,$<$\,$30$ and a kinetic energy $E_\textrm{kin}$\,$<$\,$10^{49}$ erg for a stellar wind density of $A_*$\,$\gtrsim$\,$1$. We propose that EP260321a originated from a mildly RELATIVISTIC, weak outflow that was choked by the progenitor star. This scenario is capable of naturally explaining its low X-ray luminosity and lack of prompt gamma-ray emission. EP260321a bridges the gap between SN 2008D and low-luminosity GRBs, suggesting a greater diversity in the physical parameters of stripped stars as they undergo terminal collapse.
[abstract 13 / 70] Yes (score: 5) - Title: Stochastic Variability of Binary AccretionAuthors: Akhil Nair, Jonathan Zrake,Comments: 15 pages, 9 figuresSubjects: astro-ph.HE astro-ph.GACreated: 2026-06-26; Updated: 2026-06-30; Datestamp: 2026-06-30
We measure the power spectral density (PSD) of the accretion rate time series in an unequal mass (q = 0.2) binary surrounded by a circumbinary gas disk, using very high-resolution 2D hydrodynamics simulations. Our aim is to identify new signposts of supermassive BLACK HOLE (SMBH) binaries in ACTIVE GALACTIC NUCLEi (AGN), based on the shape of the continuum PSD, to complement well-studied line features in the PSD (periodicities). We find that the continuum PSD is a broken power-law, transitioning from flat (white noise) to a slope of -4 at a break frequency generically ~5 times the binary orbital frequency. This form is expected when (a) delivery of gas from the circumbinary disk to the individual "minidisks" is a damped random walk with correlation time equal to binary orbital period and (b) the minidisks function as low-pass filters acting at the Kepler frequency of the outer edge of the smaller BLACK HOLE's minidisk; we show numerical evidence for both. The broken power-law PSD is attained in a limit where the secondary BLACK HOLE is much smaller than its minidisk, realized numerically by a sufficiently small "sink" region; larger sinks lead to excess high-frequency noise seen as accretion rate spikes, and we argue these should be regarded as artificial when the BLACK HOLEs themselves are smaller than the sink regions. The broken power-law PSD is reminiscent of stochastic variability in ordinary AGN, inviting the conjecture that canonical AGN variability could result from widespread binarity, however pulsar timing experiments may exclude this possibility.
[abstract 14 / 70] Yes (score: 5) - Title: Radio Galaxies and Jet Duty CyclesAuthors: M. J. Hardcastle, C. Konar, S. Dutta, D. V. Lal, R. D. Baldi, M. Brienza, A. Hota, M. Kunert-Bajraszewska, B. Mingo, M. Pandey-Pommier, K. Rubinur, S. Shabala, E. Vardoulaki,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no: AASKAII/Hardcastle01Subjects: astro-ph.GA astro-ph.HECreated: 2026-06-27; Updated: 2026-06-30; Datestamp: 2026-06-30
Radio-luminous ACTIVE GALACTIC NUCLEi, or RADIO GALAXies, are the brightest population of objects in the extragalactic radio sky and will be seen in large numbers in essentially every SKA observation. Despite having been studied for more than seventy years, some aspects of RADIO GALAXy physics are still poorly understood, and the SKA will shed light on this by enabling the generation of very large samples of high-resolution, sensitive, broad-band images of RADIO GALAXies, allowing us to probe, for example, regions of particle acceleration, spectral ageing, and the MAGNETic field structures both internal and external to the radio lobes. A key feature of the RADIO GALAXy population is that observations of extended sources probe the past history, and thus the duty cycles, of accretion onto the central supermassive BLACK HOLE, and we discuss ways in which the SKA will improve our understanding of episodic and dying RADIO GALAXies in particular.}
[abstract 15 / 70] Yes (score: 5) - Title: Constraints on Hadronic Emission from MicroQUASARs Detected by LHAASOAuthors: V. Vecchiotti, E. Amato, G. Giacinti, G. Morlino, G. Peron,Comments:Subjects: astro-ph.HECreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
Recently, the LHAASO collaboration reported ultra-high-energy (UHE) gamma rays from six microQUASARs. For five of these sources, the emission extends beyond $100$ TeV, making microQUASARs promising candidates for Galactic PeVatrons. We investigate whether gamma-rays around $100$ TeV originate from hadronic interactions of accelerated COSMIC RAYs (CRs) with the ambient medium, and we estimate the contribution of these sources to the measured CR spectrum around the knee. We also place upper limits on six LHAASO microQUASARs with no detected UHE emission. We assume diffusion-dominated propagation of CR, with a diffusion coefficient suppressed compared to the average Galactic value near the source and equal to the Galactic value at large distances. We assume continuous injection over timescales of $t_{\rm age}=0.1-1$ Myrs. Using available measurements of the gas density, we find that hadronic interactions alone cannot fully account for the observed emission for any of the detected sources. However, in the case of GRS 1915+105 and MAXI J1820+070, the hadronic scenario may still be valid when considering acceleration efficiency higher than $10\%$. We then derive upper limits on the hadronic contribution to the observed gamma-ray flux. We estimate that the detected sources contribute at most $\sim4\%$ of the Galactic CR spectrum at $1$ PeV for an injection timescales of $0.1$ Myrs and a CR acceleration efficiency of $10 \%$. When adopting the maximum acceleration efficiency allowed by the gamma-ray observations the contribution rises to $37\%$. Longer injection timescales ($\sim 1$ Myrs) lead to contributions exceeding the observational constraints. For sources not detected at UHE, we obtained a maximum contribution of $\sim 17\%$, achieved assuming continuous injection over $1$ Myr.
[abstract 16 / 70] Yes (score: 5) - Title: No evolution in the number density of little red dots from cosmic dawn to cosmic noonAuthors: Federica Loiacono, Roberto Gilli, Marco Mignoli, Marcella Brusa, Francesco Calura, Marco Chiaberge, Andrea Comastri, Quirino D'Amato, Roberto Decarli, Ivan Delvecchio, Kazushi Iwasawa, Ignas Juodžbalis, Giorgio Lanzuisi, Roberto Maiolino, Stefano Marchesi, Giovanni Mazzolari, Colin Norman, Alessandro Peca, Isabella Prandoni, Matteo Sapori, Matilde Signorini, Paolo Tozzi, Eros Vanzella, Cristian Vignali, Fabio Vito, Gianni Zamorani, Anita Zanella,Comments: 19 pages, 10 figures. Submitted to A&ASubjects: astro-ph.GA astro-ph.COCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
We present our search for little red dots (LRDs) in the "J1030 field", a region of the sky around the $z\sim 6.3$ QUASAR SDSS J1030+0524, observed by the JWST EIGER program. Over 154 point-like sources selected in a JWST-based photometric catalog, we find five broad line emitters (with $FWHM \gtrsim 1000\ \rm km s^{-1}$) that are red ($F200W - F356W > 0$) and are undetected in the X-rays. We use these sources to derive the bolometric luminosity function (LF) of LRDs at $z = 2.4$ and $z = 4.5$. At $z = 2.4$, the space density of LRDs is only a factor of $\sim 2$ lower than that of all pre-JWST ACTIVE GALACTIC NUCLEi (AGNs) with bolometric luminosity $L_{\rm bol} \gtrsim 3 \times 10^{44}\ \rm erg\ s^{-1}$. At $z = 4.5$, our estimate is consistent with those derived for LRDs based on larger areas of the sky. A similar behaviour is observed in the BLACK HOLE mass function. More importantly, we study the number density of LRDs from cosmic dawn to cosmic noon. We find that there is no significant evolution in the abundance of LRDs with $L_{\rm bol} \gtrsim 3 \times 10^{44}\ \rm erg\ s^{-1}$ at $z > 2$. We speculate that the drop at $z < 4$ seen by other studies is due to their sampling of only the bright-end of the LRDs LF. At cosmic noon, the abundance of LRDs is $n = 3.4^{+5.6}_{-2.4} \times 10^{-5}\ \rm Mpc^{-3}$, which is a factor of $\sim 350$ larger than recent model predictions and is comparable with that of X-ray selected AGNs with similar bolometric luminosity. Our result may imply that, if LRDs are the early, rapid stages of supermassive BLACK HOLE growth, as suggested by some models, then the formation of BLACK HOLE seeds can be efficient down to epochs as recent as cosmic noon. Alternatively, LRDs may simply be a high-accretion phase in already mature BLACK HOLEs.
[abstract 17 / 70] Yes (score: 5) - Title: The SKA-VLBI Perspective on Radio-Quiet AGNAuthors: Francesca Panessa, Tao An, James Petley, Ailing Wang, Ranieri Diego Baldi, Ehud Behar, Emmanuel Bempong-Manful, Gabriele Bruni, Ning Chang, Sina Chen, Lang Cui, Filippo D'Ammando, Marcello Giroletti, Magdalena Kunert-Bajraszewska, Sibasish Laha, Ari Laor, Ian McHardy, Eileen Meyer, Monica Orienti, Miguel Pérez-Torres, Isabella Prandoni, Claudio Ricci, David R. A. Williams-Baldwin, Zsolt Paragi,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no: AASKAII/Panessa01. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.GACreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
The accretion-ejection mechanism in Active Galactic Nuclei (AGN) remains a central open problem in astrophysics, tied to the role of AGN feedback in galaxy formation and evolution. Radio-quiet AGN dominate the observed AGN population. Lacking luminous JETs, their radio emission traces a rich set of processes spanning the host galaxy kpc scales down to the vicinity of the supermassive BLACK HOLE: STAR FORMATION, AGN-driven winds and shocks, free-free emission from photo-ionized gas, low-power JETs, and coronal activity close to the inner accretion disk. The Square Kilometre Array (SKA) will probe these processes across a wide frequency range with unprecedented sensitivity, wide-field survey capability, and, critically, high-resolution VLBI imaging. Flux, spectral, and POLARIZATION monitoring will constrain dynamics and environmental coupling, while mapping nuclear regions on sub-pc to kpc scales will disentangle compact cores from host emission, resolving the diversity of radio activity across accretion regimes and JET powers from the local Universe to the cosmic dawn. At the full AA4 deployment, the SKA-MID phased into global VLBI arrays will deliver sub-milliarcsecond imaging and $μ$Jy sensitivity over 0.35--15\,GHz, enabling the first population-level census of radio-quiet AGN nuclei. Earlier AA$\ast$ operations will support pilot studies of the brightest nearby systems.
[abstract 18 / 70] Yes (score: 4) - Title: Kerr BLACK HOLE in presence of force-free MAGNETic fieldAuthors: Haidar Sheikhahmadi,Comments: 35 pages, 6 figures, 2 appendices; typos correctedSubjects: gr-qc astro-ph.CO hep-th math-ph math.MPCreated: 2026-06-27; Updated: 2026-06-30; Datestamp: 2026-06-30
We extend the study of force-free MAGNETospheres from non-rotating to rotating BLACK HOLEs \cite{Sheikhahmadi} and investigate the influence of a force-free MAGNETic field on the geometry around a Kerr BLACK HOLE. Using the Newman-Penrose formalism, we explicitly construct the electroMAGNETic field strength tensor in the Kerr background and compute the corresponding stress-energy tensor. The resulting metric perturbation is then obtained by solving the linearised Einstein equations. In this modified geometry, we analyse key observables of thin accretion disks, including the innermost stable circular orbit (ISCO), effective potential, energy flux, temperature, and efficiency parameter. Our results demonstrate that MAGNETic backreaction significantly alters the spacetime near the BLACK HOLE, with important consequences for accretion physics and JET-launching mechanisms such as the Blandford-Znajek process. This work underlines the essential role of MAGNETic fields in shaping RELATIVISTIC astrophysical environments.
[abstract 19 / 70] Yes (score: 4) - Title: Mass Transfer in Tidally Heated Stars Orbiting Massive Black Holes and Implications for Repeating Nuclear TransientsAuthors: Philippe Z. Yao, Eliot Quataert,Comments: 12 pages, 6 figures, Published in the Open Journal of AstrophysicsSubjects: astro-ph.HE astro-ph.GA astro-ph.SRCreated: 2026-06-24; Updated: 2026-06-30; Datestamp: 2026-06-30
The structure of stars orbiting close to supermassive BLACK HOLEs (SMBHs) can be dramatically modified by tidal heating, which can in principle dissipate an energy much larger than the stellar binding energy. We use analytic models and MESA to explore the coupled dynamics of tidal heating, stellar structural evolution, orbital decay due to gravitational waves and tides, and mass transfer. In contrast to more equal mass stellar binaries, the stable mass transfer rate for stars orbiting SMBHs is typically set by the tidal heating timescale (the timescale for tides to increase the stellar radius), not by the gravitational wave orbital decay timescale. The resulting stable mass transfer rate is sensitive to the tidal heating model but is plausibly $\sim 10^{-5}-10^{-3} M_\odot {\, \rm yr^{-1}}$ (and perhaps larger), sufficient to produce low-luminosity ACTIVE GALACTIC NUCLEi in many galaxies. The stability of mass transfer is sensitive to where in the stellar interior the tidal energy is dissipated. MESA models confirm the expected result that mass transfer is unstable (stable) if tidal heating increases (decreases) the fraction of the star that is convective. More detailed conclusions about the stability of mass-transfer will require self-consistently calculating how the tidal heating of stars changes in response to internal structural changes produced by the tidal heating itself. Stars with tidal heating-induced mass transfer can produce a large population of low-luminosity ACTIVE GALACTIC NUCLEi; they may also be the progenitors of some partial tidal disruption candidates (e.g., ASASSN-14ko) as well as short-period quasi-periodic eruptions (e.g., eRO-QPE2 and GSN 069). However, many repeating nuclear transients produced by tidal heating-induced mass loss are likely fainter than those detected thus far, and remain to be discovered.
[abstract 20 / 70] Yes (score: 4) - Title: Analysis and implications of the spatio-spectral morphology of the FERMI BubblesAuthors: Ami Tank, Roland Crocker, Mark R. Krumholz,Comments: 12 pages, 11 figures, Published in the Open Journal of Astrophysics, Data available at https://doi.org/10.5281/zenodo.19675422Subjects: astro-ph.HE astro-ph.GACreated: 2026-06-26; Updated: 2026-06-30; Datestamp: 2026-06-30
The FERMI Bubbles are gamma-ray structures extending from the center of the Milky Way to +/-50 degree Galactic latitude that were discovered in data obtained by the FERMI/LAT instrument. Their origin and power source remain uncertain. To help address this uncertainty, here we use a template-free reconstruction of ten years of all-sky FERMI/LAT data provided by Platz et al. (2023) to carry out a pixel-by-pixel spectral analysis of the Bubbles. We recover the position-dependent spectral shape and normalization that would be required for parent proton or electron COSMIC RAY populations to produce the Bubbles' observed gamma-ray spectra. We find that models in which the gamma-ray emission is driven by either hadronic or leptonic processes can explain the data equally well. The COSMIC RAY population driving the emission must have either broken power-law or exponentially cut-off spectra, with break or cutoff energies that are almost constant with latitude but spectral indices below the break that harden towards the Bubbles' southern tip. For the leptonic channel, reproducing the observed position-dependent gamma-ray spectrum also requires a COSMIC RAY electron energy density that grows with distance from the Galactic plane and increases towards the edges of the Bubbles. This finding disfavors scenarios for the origin of the Bubbles where a population of COSMIC RAY electrons is accelerated near the Milky Way center and subsequently advected out to the extremities of the Bubbles.
[abstract 21 / 70] Yes (score: 4) - Title: Towards direct imaging and orbital parameter estimation of supermassive BLACK HOLE binaries with spaceborne VLBIAuthors: B. Hudson, L. I. Gurvits, E. Mooij, A. Ricarte, D. Palumbo,Comments: Accepted for publication in Astronomy & Astrophysics. 19 pages, 14 figuresSubjects: astro-ph.IM astro-ph.HECreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
Direct observation of the orbital motion of a sub-parsec supermassive BLACK HOLE binary (SMBHB) would provide the first conclusive electroMAGNETic proof of such systems existing. Widely considered to be the source of gravitational waves, binaries are expected to form as a natural consequence of galactic mergers, and determining the processes that drive their evolution is essential to understanding cosmological evolution. In this work, we evaluate the prospects of using ground and spaceborne Very Long Baseline Interferometry (VLBI) to observe SMBHBs and estimate their orbital parameters. The Black Hole Explorer (BHEX) is considered the primary case study. Achieving unprecedented resolution, BHEX will provide access to a new volume of binary parameter space, potentially enabling the first confident detection of an SMBHB. We present an orbit-fitting approach that uses relative astrometry and Bayesian dynamic nested sampling, and demonstrate its efficacy on a set of example binary systems. For simulating observations, we use a binary image model based on post-Newtonian orbit propagation and find that for BHEX, binary detection requires a total flux density of 40 mJy and a minimum separation of $\sim$2 $μ$as. With three annual observations, BHEX could constrain the semi-major axis and the eccentricity of binaries with orbital periods of $\leq$10 years to within 0.06 dex of the true values under specific noise assumptions. We have also evaluated the benefits provided by BHEX for binary detection compared to ground-only observations by arrays such as the next generation Event Horizon Telescope (ngEHT). Finally, we constrained the requirements of a future spaceborne VLBI system capable of performing a statistically significant survey of SMBHBs.
[abstract 22 / 70] Yes (score: 4) - Title: VLBI-Enabled Localization of Continuous GW SourcesAuthors: Keitaro Takahashi, Takuya Akahori, Kenta Fujisawa, Hiroshi Imai, Hajime Kita, Hideyuki Kobayashi, Hiroaki Misawa, Kotaro Niinuma, Tomoaki Oyama, Kazuhiro Takefuji, Fuminori Tsuchiya,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Takahashi01. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.IM astro-ph.HECreated: 2026-06-27; Updated: 2026-06-30; Datestamp: 2026-06-30
Pulsar timing arrays (PTAs) are opening the nanohertz gravitational-wave (GW) band by timing millisecond pulsars (MSPs) to target signals from supermassive BLACK HOLE binaries (SMBHBs). Beyond evidence for a stochastic background, a central SKA-era objective is detecting individual continuous-wave (CW) sources. The scientific payoff hinges on localization: conventional PTA searches yield uncertainties of tens-hundreds of deg$^2$, too large to identify a unique host, obtain a redshift, infer intrinsic masses, or pursue electroMAGNETic counterparts. This limitation is chiefly geometric: the CW response includes Earth and pulsar terms, and poorly known pulsar distances make the pulsar-term phase a free parameter that degrades triangulation. If distances to a few MSPs are known to better than a GW wavelength ($\sim$ 1 pc), these phases are fixed and localization improves by orders of magnitude. Simulations indicate that with sub-parsec distances for a handful of nearby MSPs, the uncertainty can shrink to $\sim 10^{-3}$ deg$^2$ (arcminute scale), enabling unique host association and multi-messenger follow-up. Achieving such distances requires $\sim$ 10 $μ$arcsec parallaxes for MSPs within a few hundred parsecs, a precision now approached with Very Long Baseline Interferometry (VLBI) and expected to become practical with phased-array SKA1-Mid operating as a sensitive VLBI element. SKA1's multi-beam, multi-calibrator astrometry will provide the independent distance priors needed for PTAs to localize nanohertz GW sources and measure SMBHB parameters and environments. We assess VLBI's role in PTA CW searches and propose a concrete SKA1-Mid observing strategy for nearby MSPs to deliver the required sub-parsec distances.
[abstract 23 / 70] Yes (score: 4) - Title: Radio Diagnostics of Particle Acceleration in Solar Flares with SKAO ObservationsAuthors: Rohit Sharma, Marina Battaglia, Sijie Yu, Hamish Reid, Eduard Kontar, Bin Chen,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366) Report-no: AASKAII/Sharma01 Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.SRCreated: 2026-06-27; Updated: 2026-06-30; Datestamp: 2026-06-30
Particle acceleration is a fundamental astrophysical process occurring across diverse systems and scales, producing electroMAGNETic emission across all wavelengths. Radio bursts from astrophysical systems like active galaxy JETs, solar flares, pulsars, etc., provide a probe into the emission mechanism and particle acceleration processes. Among all astrophysical phenomena, MAGNETically driven solar flares provide unique diagnostics of nonthermal particles due to the advantage of multiple spatial-temporal and spectral measurements. The subsequent emitted radiation spans various sections of the radio spectrum. Based on brightness temperature and spectrum, one can distinguish between bright plasma emission or 'nonthermal' emission. Nonthermal radio bursts in meter and microwave bands arise from suprathermal particles, while the surrounding plasma produces fainter thermal emission. High spatial-temporal studies along with polarimetry will enable tracking of electron beams in evolving MAGNETic fields and constrain coronal properties such as MAGNETic strength, density, and temperature. Fine spectral structures from gyroSYNCHROTRON bursts allow mapping of MAGNETic fields along acceleration tracks. However, emissions from the more numerous, weaker particle populations remain difficult to observe. Particles in solar flares follow a power-law energy distribution, with weaker populations being more common. The Square Kilometre Array Observatory (SKAO) will provide high-fidelity data that will enable detailed characterisation of these populations, statistical studies of particle beams, and insights into their interaction with MAGNETic topologies. Its high-resolution (especially SKA-Mid) and multi-wavelength synergy (EUV, X-rays) will refine diagnostics of coronal and acceleration-region properties. This chapter reviews particle acceleration models and expected advances from SKAO.
[abstract 24 / 70] Yes (score: 4) - Title: Insights into Jet-Induced Cloud Disruption in NGC 1316: ALMA Reveals a Spatially Extended Molecular GasAuthors: Kana Morokuma-Matsui, Alexander Y. Wagner, Filippo M. Maccagni, Lauranne Lanz, Fumiya Maeda, Jin Koda, Akihiko Hirota, Yutaka Fujita, Kotaro Kohno, Tomoki Morokuma, Tsutomu T. Takeuchi, Kouichiro Nakanishi, Fumi Egusa, Kenji Bekki, Daniel Espada, Bärbel Koribalski, Jing Wang,Comments: 47 pages, 20 figures, accepted for publication in ApJSubjects: astro-ph.GACreated: 2026-06-27; Updated: 2026-06-30; Datestamp: 2026-06-30
We present ALMA CO($J=1-0$) observations of a nearby RADIO GALAXy NGC1316 at a 100-pc resolution to investigate the impact of AGN JETs on the molecular gas. The molecular gas exhibits complex spatial and kinematic distributions, with broad CO line widths ($>50$ km s$^{-1}$) observed in several regions. The interferometric CO flux is only 34%-38% compared to single-dish data, indicating a large fraction of spatially extended molecular gas, especially in the central regions. We identified 24 Giant Molecular Clouds Associations (GMAs) primarily within the ``NW Shell'' and the ``SE Blob''; these GMAs show velocity dispersions approximately twice as high as those in typical star-forming galaxies for their sizes. Analysis of archival ALMA CO($J=2-1$) and CO($J=3-2$) data reveals elevated line ratios ($R_{21} \sim 1$ and $R_{31} \sim 1$) in gas near the JET, whereas, away from the JET, typical values ($R_{21} \sim 0.7$, $R_{31} \sim 0.3$). A multi-wavelength comparison reveals a $\sim$5 kpc warm ionized gas shell that encompasses the molecular NW Shell. The observed energetics and bubble morphology are consistent with an expanding bubble model driven by the JET assuming a JET power of $1.6\times10^{43}$~erg~s$^{-1}$. We propose that the high extended gas fraction results from the destruction of molecular clouds due to interactions with the JET plasma. NGC1316 may be a good example of JET-induced negative feedback through the ablation, dispersal, and rarification of dense molecular clouds through JET-ISM interactions.
[abstract 25 / 70] Yes (score: 4) - Title: Citizen Science Research with the Square Kilometre Array Observatory (SKAO)Authors: Ananda Hota, Pratik Dabhade, M. J. Hardcastle, Stephen Serjeant, C. Konar, Hugh Dickinson, Sabyasachi Pal, Sravani Vaddi, Sagar Sethi, Shubhrangshu Ghosh, Arundhati Purohit,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Hota01. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.GACreated: 2026-06-28; Updated: 2026-06-30; Datestamp: 2026-06-30
Over the past two decades, internet-enabled citizen science research (CSR) has contributed to significant discoveries while involving millions of people in the research process. Our review highlights CSR in extragalactic radio astronomy and emphasises that such approaches will become increasingly relevant across radio astronomy in the era of the Square Kilometre Array (SKA). As astronomical data volumes grow, CSR is converging with Artificial Intelligence and Machine Learning (AI/ML), creating hybrid human-machine frameworks suited to big-data challenges. Two CSR platforms, Radio Galaxy Zoo and RAD@home, demonstrate success: the former excels in large-scale, web-based catalogue creation, while the latter combines structured training with collaborative discovery. Following this, we propose CSR with the SKA, namely SKA@home, with two modes: one purely web-based and the other in collaboratory mode with national training programmes. We argue that CSR can complement, and at times surpass, automated AI/ML pipelines, particularly in identifying rare, intricate, or unexpected features. Illustrative CSR discoveries include an episodic wide-angle-tailed RADIO GALAXy, a JET-galaxy interaction, a collimated SYNCHROTRON thread, a twin-ring odd radio circle, and a large-scale shock ahead of a cluster-infalling galaxy. Consistent with the IAU's recognition of CSR as a driver of Astronomy for Development and the United Nations' affirmation of participation in science as a universal human right, both the SKA construction proposal and outreach strategies show commitment to enabling CSR with SKA. The proposed SKA@home would not only enhance the early discovery potential of SKA data but also initiate a deeper and more meaningful connection with society at large.
[abstract 26 / 70] Yes (score: 4) - Title: Distribution of energy release events due to MAGNETic braidingAuthors: David I. Pontin, Klaus Galsgaard, James A. Klimchuk,Comments: Accepted for publication in ApJ. 18 pages, 10 figuresSubjects: astro-ph.SRCreated: 2026-06-28; Updated: 2026-06-30; Datestamp: 2026-06-30
Energy conversion by RECONNECTion-powered nanoflare heating is one of the leading explanations for the heating of the solar chromosphere and corona. The aim of this paper is to shed light on this mechanism by exploring the MAGNETic Reynolds number dependence of the energy conversion process. To do this we employ boundary-driven, MAGNETohydrodynamic, flux-braiding simulations at different MAGNETic Reynolds numbers ($R_m$), and explore in detail the properties of the individual MAGNETic energy release events. The properties of the RECONNECTing current sheets that mediate the energy release are shown to depend on $R_m$. For increasing $R_m$, the current sheets become thinner, more intense, and more numerous. For sufficiently large $R_m$, the current sheets fragment along their length, leading to a sharp cutoff in the current sheet length distribution. The cutoff is consistent with the threshold for non-linear tearing/plasmoid instability. For increasing $R_m$ the MAGNETic field lines become increasingly tangled, the mean and peak values of the MAGNETic field strength increase, and the Poynting flux into the domain increases, implying that the heating rate also increases. The global RECONNECTion rate is essentially independent of $R_m$. These results support the braiding mechanism as a viable way to effectively heat the internal portions of coherent flux tubes in the corona.
[abstract 27 / 70] Yes (score: 4) - Title: Pulsed Infrared Emission from Magnetar 4U 0142+61 Detected by JWSTAuthors: Jeremy Hare, George G. Pavlov, Bettina Posselt, George Younes, Oleg Kargaltsev,Comments: Submitted to ApJSubjects: astro-ph.HECreated: 2026-06-28; Updated: 2026-06-30; Datestamp: 2026-06-30
We report on a JWST observation of the MAGNETar 4U 0142+61 on 2024 August 18 with the Near-Infrared Camera (NIRCam). NIRCam observed the MAGNETar for 33~min in timing mode, providing a time resolution of 2.5~s. In the F410M filter (pivot wavelength 4.08 $μ$m), we measured the flux density $f_ν= 22.9\pm0.6$ $μ$Jy and detected pulsations at a frequency of $115.059\pm0.035$ mHz, in agreement with the MAGNETar's spin period at the epoch of the JWST observation. The observed pulse profile has one peak per period (although this may be due to the poor time resolution), with a lower limit on the pulsed fraction of about 10\%. We compare the IR pulse profile to the NICER and NUSTAR X-ray pulse profiles and find that the IR peak overlaps with the hard X-ray peak, suggesting a MAGNETospheric origin for the pulsed IR emission.
[abstract 28 / 70] Yes (score: 4) - Title: Non-thermal Sources from Stereoscopic Hard X-ray and Earth-based Microwave Observations in a Data-Constrained Magnetohydrodynamic SimulationAuthors: Keitarou Matsumoto, Satoshi Inoue, Meiqi Wang, Bin Chen, Muriel Zoë Stiefel, Säm Krucker, Satoshi Masuda, Haimin Wang,Comments: It has been accepted by ApJSubjects: astro-ph.SRCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
We analyze the X7.1 flare on 2024 October 1 from NOAA AR 13842 using hard X-ray (HXR) imaging, microwave observations by the Expanded Owens Valley Solar Array (EOVSA), and a three-dimensional Magnetohydrodynamic (MHD) simulation. The flare was observed from two vantage points, with Solar Orbiter/Spectrometer Telescope for Imaging X-rays viewing the flare near the limb and Advanced Space-based Solar Observatory/Hard X-ray Imager and EOVSA observing it on the disk. We carried out a data-constrained MHD simulation using a nonlinear force-free field extrapolation as the initial condition and constrained the height of the non-thermal looptop source from stereoscopic HXR and microwave observations. The height is consistent between the stereoscopic analysis and the MHD simulation. A secondary non-thermal microwave source aligned with a southward plasma ejection corresponds to an elongated current sheet. Although the current sheet grows in multiple directions, the secondary microwave emission is observed only from the southern segment. This localization suggests RECONNECTion in regions with different MAGNETic field strengths. Reconnection in strong-field regions produces flare arcades with dominant looptop emission, whereas RECONNECTion in weaker southern regions gives rise to secondary microwave emission at higher altitudes. The height of the secondary source is consistent between the stereoscopic analysis and the MHD simulation. Microwave spectral fitting suggests a higher low-energy cutoff for non-thermal electrons in the secondary microwave source than in the main looptop source. This may reflect the transport of electrons pre-accelerated near the looptop source by the southward plasma ejection.
[abstract 29 / 70] (score: 3) - Title: Electron penetration heating in turbulent MAGNETic loops driven by nonRELATIVISTIC LASER-plasma interactionAuthors: Zheng Gong, Sida Cao, Caleb Redshaw, Matthew R. Edwards,Comments:Subjects: physics.plasm-ph astro-ph.HECreated: 2026-06-27; Updated: 2026-06-30; Datestamp: 2026-06-30
Using particle-in-cell simulations to study nonRELATIVISTIC LASER pulse propagation in a under-critical plasma, we identify a novel mechanism that occurs during the growth of turbulent MAGNETic loops: electron penetration heating. The loops have an electroMAGNETic left-hand chirality distinct from that of well-known quasistatic MAGNETic islands. The fast electrons penetrate through the loops and thus are accelerated to unexpected RELATIVISTIC energies due to the symmetry breaking induced by the coupling between the loop field and the non-RELATIVISTIC electroMAGNETic wave. The identified features of penetration heating and MAGNETic loops might provide an alternative perspective for understanding superponderomotive electron heating in under-critical plasmas irradiated by nonRELATIVISTIC LASER pulses. This is a potential explanation for anomalous hot electron generation in scenarios of LASER-driven inertial confinement fusion.
[abstract 30 / 70] (score: 3) - Title: Flavor physics at the EIC with b-JET taggingAuthors: Shaouly Bar-Shalom, Jose Wudka,Comments: 12 pages, 6 figures. Final version as published in PRDSubjects: hep-ph hep-exCreated: 2026-06-28; Updated: 2026-06-30; Datestamp: 2026-06-30
We employ an approximate conserved quantum number (defined as "$b$-Parity" in [1]) of the Standard Model (SM): $b_P=(-1)^n$, where $n$ is the number of produced $b$-JETs in the reaction $e + p/A \to n \cdot j_b +X$, to explore new TeV-scale flavor-changing interactions involving the 3rd generation QUARKs at the EIC; simply by counting the number of $b$-JETs in the final state. In particular, the SM single and di-JET production at the EIC which occur through charge current interactions, $e + p/A \to j + \!\not\!E_T$ and $e + p/A \to 2\cdot j + \!\not\!E_T$, are $b_P$-even since the $b_P$-violating (i.e, $b_P=-1$) SM signals for these processes are necessarily CKM suppressed and, therefore, have a vanishingly small production rate. In contrast, new flavor physics can generate $b_P=-1$ signals at the EIC whose only significant SM background is due to $b$-JET misidentification. We thus show that $b_P$ can be used as a simple and sensitive probe of new flavor violating physics; specifically, we find that counting single $b$-JET events in $e + p/A \to j + \!\not\!E_T$ at the EIC with a center-of-mass (CM) energy of $\sqrt{s} \sim 140$ GeV, can probe scales of new physics up to $Λ\sim {\cal O}(5)$ TeV for a certain type of new chiral flavor-changing physics in 3rd generation interactions. This is remarkably more than 30 times larger than the assumed EIC CM energy and it critically depends on the $b$-tagging efficiency and purity as well as the feasibility of electron-beam POLARIZATION. The sensitivity of the di-JET process, $e + p/A \to 2j + \!\not\!E_T$, to these type of new physics is reduced compared to the single-JET channel.
[abstract 31 / 70] (score: 3) - Title: Pulsational mass loss from supermassive stars creates the compact shells of Little Red DotsAuthors: Devesh Nandal, Igor Chilingarian, Chris Nagele, John Chisholm, Franz E. Bauer, Abraham Loeb,Comments: 20 pages, 6 figures. Accepted by ApJL !Subjects: astro-ph.HE astro-ph.GA astro-ph.SRCreated: 2026-06-27; Updated: 2026-06-30; Datestamp: 2026-06-30
Little Red Dots (LRDs) have emerged as one of the central puzzles of the JWST era. Their spectra increasingly require dense gas close to the source, yet the physical origin of that cocoon-like structure remains unclear. We examine whether late pulsational mass loss from supermassive stars (SMS)leads to dense gas cocoons. We analyze five accreting GENEC models at different metallicities with characteristic masses of order $10^5\,M_\odot$, following them through post-accretion evolution with radial pulsation calculations and general RELATIVISTIC (GR) stability diagnostics. Mass loss during the final stages of evolution occurs not as a steady wind, but through discrete strange-mode ejection episodes. In the $Z=10^{-2}\,Z_\odot$ model, which provides the clearest LRD analogue, four late episodes last $41$--$282$ yr and eject $10$--$348\,M_\odot$ each, for a total loss of $(4.8-10)\times10^2\,M_\odot$; the final episode alone contributes $\simeq 73\%$ of that budget. Since the last episode dominates the mass-loss, it is the only event sufficiently massive enough to leave behind a compact, optically thick shell extending out to 0.4 pc that reproduces the LRD dense gas cocoon. The final ejecta are H/He dominated but chemically distinctive, with a robust nitrogen-rich composition, $\log(\mathrm{N/O})\simeq0.13$ and $\log(\mathrm{C/O})\simeq-0.23$. The SMS reaches GR instability at an age of $\sim 1$ Myr and collapses in $\sim10^4$ s, retaining $\sim 99\%$ all of its mass. Across the full metallicity range from Pop III to $10^{-2}\,Z_\odot$, this shell-ejection channel persists. Pulsational mass-loss from SMSs therefore provides a physically motivated origin for the compact cocoon-like structure implied by LRDs, while remaining the natural progenitors of the massive BLACK HOLE seeds invoked in direct collapse scenario.
[abstract 32 / 70] (score: 3) - Title: Semi-Implicit Stellarator Magnetohydrodynamics with Nodal Spectral ElementsAuthors: C. R. Sovinec, S. A. Patil, J. V. Cauilan,Comments:Subjects: physics.plasm-ph physics.comp-phCreated: 2026-06-26; Updated: 2026-06-30; Datestamp: 2026-06-30
Nonlinear time-dependent computation of macroscale dynamics in stellarators is motivated by laboratory results showing the possibility of robust operation in conditions where MAGNETohydrodynamic (MHD) modes are linearly unstable. A new formulation of semi-implicit MHD computation for toroidally shaped MAGNETic confinement systems uses 2D nodal spectral elements over the poloidal plane and Fourier representation over a generalized toroidal angle. Geometric mappings and steady-state (equilibrium) fields are expanded in the same 3D representation as the time-evolved fields to model non-axisymmetric configurations. For accuracy at large timestep, the semi-implicit operator is based on the ideal-MHD energy integral using 3D pressure and MAGNETic fields. The nodal spectral elements allow numerical convergence through either h-refinement or p- refinement. Our implementation (NIMSTELL) with the continuous H1 expansion of MAGNETic-field components and diUusive divergence control is a generalization of the NIMROD code [JCOMP 195, 355]. The NIMSTELL implementation is verified linearly and nonlinearly on resonant ideal interchange, where convergence from the stable side results from the stabilization method used in NIMROD [JCOMP 319, 61]. Optionally, NIMSTELL may use an H(curl) representation for vector potential, and both MAGNETic representations are verified with respect to results from JOREK [Phys. Plasmas 29, 063901] on linear and nonlinear MAGNETic tearing in the W7-A rotating-ellipse configuration. Application of the existing vector-potential implementation to interchange shows that it needs a minimum level of electrical resistivity to avoid numerical noise for a given level of spatial resolution. Solving the algebraic systems from the implicit parts of the time advance is facilitated by including the Fourier components of stellarator mode families in each preconditioning operation.
[abstract 33 / 70] (score: 3) - Title: The Lockman-SpReSO Project: A Deep X-ray Spectral View of a FIR-selected AGN PopulationAuthors: Mauricio Elías-Chávez, Takamitsu Miyaji, Martín Herrera-Endoqui, Irene Cruz-González, Yair Krongold, Héctor Hernández-Toledo, Mirjana Povic, Bereket Assefa, Mauro González-Otero, Castalia Alenka Negrete, Miguel Cerviño, J. Antonio de Diego, Miguel Sánchez-Portal, Erika Benítez, Jordi Cepa, José Antonio Vázquez Mata, Monica I. Rodriguez, Emilio J. Alfaro, J. Jesús González, Carmen P. Padilla-Torres, J. Ignacio González-Serrano, Vladimir Ávila-Reese, Ángel Bongiovanni, A. M. Perez Garcia,Comments: 24 pages, 16 figures, accepted for publication in MNRASSubjects: astro-ph.GACreated: 2026-06-28; Updated: 2026-06-30; Datestamp: 2026-06-30
We present a detailed X-ray spectral analysis of the ACTIVE GALACTIC NUCLEus (AGN) population in the Lockman-SpReSO project, a multiwavelength campaign of FIR sources in the Lockman Hole field. Using deep XMM-Newton observations cross-matched with FIR-selected galaxies, we characterize 94 AGNs based on their X-ray spectral properties. The sample is distributed over a large redshift range of $z = 0.07-5$, and reaches a flux limit of $5 \times 10^{-16}\, \mathrm{erg\, s^{-1}\, cm^{-2}}$ in the $0.3-10\, \mathrm{keV}$ band. We model the X-ray spectra using absorbed power-law, reflection, and soft excess components to estimate intrinsic column densities ($N_{\mathrm{H}}$), rest-frame $2-10\, \mathrm{keV}$ luminosities, and iron line equivalent widths $(EW)$. Additionally, we included an advanced model fitting for Compton-thick AGNs (CT-AGNs) using the XCLUMPY model. Our results show an increase in the fraction of obscured AGNs toward higher redshifts, including the identification of one strong and two borderline CT-AGN candidates with $N_{\mathrm{H}} \gtrsim 10^{24}\, \mathrm{cm^{-2}}$. Soft excess emission is detected in 10 AGNs, with an average blackbody temperature of $0.12 \pm 0.02\, \mathrm{keV}$. We also detect the X-ray Baldwin effect in both obscured and unobscured populations, and we found a strong correlation between the torus angular width $(σ_\mathrm{tor})$, dust covering factor $(f_{\mathrm{cov}})$, and X-ray luminosity, described by $f_{\mathrm{cov}} = (-0.1 \pm 0.01) \times \log(L_{2-10\, \mathrm{keV}}/(10^{44}\, \mathrm{erg\, s^{-1}})) + (0.65 \pm 0.01)$, supporting the receding torus scenario. While consistent with deep X-ray surveys, the FIR selection favours the identification of dusty star-forming host galaxies and heavily obscured AGNs.
[abstract 34 / 70] (score: 3) - Title: Projection Is All You Need: Interpreting Polarization Measurements in the Orion Clouds with Sub-Alfvénic MHD SimulationsAuthors: Feiyu Quan, Yitao Xu, Keping Qiu, Xiaodan Fan, Hua-bai Li,Comments: 21 pages, 13 figures, accepted to ApJ. Interactive version of Figure 1 can be also found at https://doi.org/10.5281/zenodo.20923459Subjects: astro-ph.GACreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
Dust POLARIZATION observations are widely used to diagnose the relative importance of MAGNETic fields and turbulence in star forming molecular clouds, often through summary statistics such as the mean POLARIZATION direction $μ$ and dispersion $σ$. Recent multi-scale POLARIZATION observations of the Orion Integral-Shaped Filament (ISF) reveal substantial diversity in POLARIZATION morphology among its dense cores, raising questions about the underlying Alfvénic nature of the cloud. In this work, we develop a statistical framework to compare POLARIZATION-based summary statistics from observations with those derived from projected three dimensional MHD simulations, explicitly accounting for projection effects. Using globally sub-Alfvénic simulations that naturally produce slightly super-Alfvénic dense cores, we show that modest deviations of core-scale MAGNETic fields from the parent cloud field, when combined with projection, can generate a wide range of plane-of-sky POLARIZATION dispersions. Applying hypothesis testing, we find that the observed $(μ, σ)$ values in the Orion ISF are statistically consistent with sub-Alfvénic cloud models over a broad range of viewing angles. This broad degeneracy implies that $μ$ and $σ$ alone cannot provide precise information about the three-dimensional MAGNETic-field distribution, and hence the Alfvén Mach number, of an individual cloud. While the observations can provide evidence against certain projection geometries, we demonstrate that POLARIZATION statistics based solely on $(μ, σ)$ are insufficient to provide evidence against sub-Alfvénic cloud models. Our results highlight the necessity of explicitly incorporating projection effects when interpreting POLARIZATION observations of molecular clouds.
[abstract 35 / 70] (score: 3) - Title: Enabling population studies on wind-driven Galactic binary systemsAuthors: B. Marcote, P. Benaglia, V. Bosch-Ramon, M. De Becker, S. del Palacio, P. Atri, J. Moldón, J. M. Paredes, M. Ribó, G. E. Romero, A. Tej,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Marcote01Subjects: astro-ph.HE astro-ph.GA astro-ph.SRCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
Galactic binaries driven by stellar wind shocks, such as colliding wind binaries (CWBs) and gamma-ray binaries (gBs), harbor one of the most efficient particle acceleration engines known in the Universe. Despite their potential, these sources remain relatively unexplored, particularly in the domains of low radio frequencies and very high resolution. As a result, we lack comprehensive population studies and well-characterized individual systems. Only a few of these binaries, such as the iconic gB PSR B1259$-$63 or the massive CWB WR 140, have been studied in enough detail to probe their wind dynamics and shock physics. Current observations lack the sensitivity to detect weak non-thermal SYNCHROTRON emission from low-energy particle populations and the angular resolution to resolve shock structures on sub-au scales. The Square Kilometre Array Observatory (SKAO) will mark a significant improvement in both sensitivity and resolution with its SKA-low and SKA-mid telescopes, solving these challenges. This will enable systematic studies of the winds and shock interactions in these binary systems. Additionally, SKA-VLBI will facilitate the observation of changes in shock geometry at different orbital phases, linking particle acceleration processes to the binary's orbital characteristics and stellar wind properties. SKAO will pave the way for comprehensive population studies of these energetic binary systems.
[abstract 36 / 70] (score: 2) - Title: On the effective spin-mass ratio relation of binary BLACK HOLE mergers that evolved in isolationAuthors: Sambaran Banerjee, Aleksandra Olejak,Comments: 36 pages, 28 figures. Minor figure rearrangement for improved readability. Published in the Open Journal of AstrophysicsSubjects: astro-ph.HE astro-ph.SR gr-qcCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
The ground-based measurement of gravitational waves (GW) from merging binary BLACK HOLEs (BBH) allows independent determination of spins of stellar-remnant BLACK HOLEs (BH). The observed population of BBH mergers exhibits two intriguing peculiarities related to BH spins, namely, a positively biased distribution of the effective spin parameter, $χ_{\rm eff}$, and an apparent anti-correlation between merger mass ratio, $q$, and $χ_{\rm eff}$. Here we investigate the potential mechanisms for such observed properties, in BBH mergers via isolated binary evolution. We synthesise BBH mergers with the fast binary evolution code BSE. The role of various physical assumptions is explored, including tidal spin-up, compact remnant mass, and mass transfer physics. We compare the properties of BBHs that form through stable mass transfer (SMT) and common envelope evolution (CE). We find that both the asymmetry in the $χ_{\rm eff}$ distribution and the $χ_{\rm eff}$ anti-correlation can be natural outcomes of isolated-binary BBH formation. The anti-correlation is especially pronounced for SMT-channel BBH mergers that experience a mass-ratio reversal, i.e., those where the second-born BH is the more massive one. The anti-correlation arises from the dependence of orbital shrinking during mass transfer and the Roche lobe size on the system's mass ratio. This characteristic $χ_{\rm eff}-q$ trend diminishes with increasing metallicity and when the isolated-binary BBH merger population is mixed with a significant contribution of dynamically formed BBH mergers or the newly formed BH's spin is misaligned relative to the parent star's spin. Our results demonstrate that isolated massive binary evolution via the SMT sub-channel can reproduce trends in the observable BBH merger population, with the characteristic signatures in mass, mass ratio, and spin distributions.
[abstract 37 / 70] (score: 2) - Title: Idealized Global Models of Accretion Disks with Strong Toroidal Magnetic FieldsAuthors: Minghao Guo, Eliot Quataert, Jonathan Squire, Philip F. Hopkins, James M. Stone,Comments: Published in the Open Journal of AstrophysicsSubjects: astro-ph.HE astro-ph.GACreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
We present global MAGNETohydrodynamic (MHD) simulations of idealized accretion disks with a strong toroidal MAGNETic field using an equation of state that fixes the gas thermal scale height. The disk forms from the inflow of a rotating MAGNETized gas cloud with a toroidal MAGNETic field. We find that the system maintains a moderately strong mean azimuthal field in the midplane, with plasma-$β\sim1$, trans-Alfvénic fluctuations, and large accretion stresses $α\sim0.1$. The azimuthal field in the disk is continuously escaping along the vertical direction but is also replenished via a local dynamo. The inflowing gas initially forms a strongly MAGNETized Keplerian disk with $β\ll1$ and $α\gg 1$. The disk gradually collapses from the inside out over $\sim 50-80$ orbits to form a moderately MAGNETized disk with $β\sim1$ and $α\sim0.1$. Radial advection of azimuthal MAGNETic field can maintain $β\lesssim1$ exterior to the circularization radius but not inside of it. Inclusion of a net initial vertical MAGNETic field can lead to an even more strongly MAGNETized disk midplane, consistent with previous work. When the gas thermal scale is not resolved ($\lesssim 4$ cells per thermal scale height), however, the disk remains highly MAGNETized with $β\ll 1 $. We discuss our results in the context of related shearing box simulations and other global disk simulations. The level of angular momentum transport found here is consistent with that inferred observationally in DWARF NOVAe and X-ray transient outbursts, unlike simulations of weakly MAGNETized accretion disks.
[abstract 38 / 70] (score: 2) - Title: Guided Unconditional and Conditional Generative Models for Super-Resolution and Inference of Quasi-Geostrophic TurbulenceAuthors: Anantha Narayanan Suresh Babu, Akhil Sadam, Pierre F. J. Lermusiaux,Comments: 47 pages, 16 figures, 5 tablesSubjects: physics.flu-dyn cs.LG physics.ao-ph physics.geo-phCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
Typically, numerical simulations of Earth systems are coarse, and Earth observations are sparse and gappy. We apply four generative diffusion modeling approaches to super-resolution and inference of forced two-dimensional quasi-geostrophic turbulence on the beta-plane from coarse, sparse, and gappy observations. Two guided approaches minimally adapt a pre-trained unconditional model: SDEdit modifies the initial condition, and Diffusion Posterior Sampling (DPS) modifies the reverse diffusion process score. Two conditional approaches, a vanilla variant and classifier-free guidance, require training with paired high-resolution and observation data. We consider multiple test cases spanning: two regimes, eddy and anisotropic-JET turbulence; two Reynolds numbers, 10^3 and 10^4; and two observation types, 4x coarse-resolution fields and coarse, sparse and gappy observations. Our comprehensive skill metrics include norms of the reconstructed vorticity fields, turbulence statistical quantities, and quantifications of the super-resolved probabilistic ensembles and their errors. We also study the sensitivity to tuning parameters such as guidance strength. Results show that the generated super-resolution fields of SDEdit are unphysical, while those of DPS are reasonable but with smoothed fine-scale features; however, neither of these lower-cost models propagates observational information effectively to unobserved regions. The two conditional models require re-training, but reconstruct missing fine-scale features, are cycle-consistent with observations, and predict correct turbulence statistics, including the tails. Further, their mean errors are highly correlated with and predictable from their ensemble standard deviations. Results highlight the tradeoffs between ease of implementation, fidelity (sharpness), and cycle-consistency of the diffusion models, and offer practical guidance for deployment.
[abstract 39 / 70] (score: 2) - Title: Gamma-ray burst light curve reconstruction with predictive modelsAuthors: Zhunuskanov A., Sakan A., Akhmetali A., Zaidyn M., Ussipov N,Comments: Published versionSubjects: astro-ph.HE astro-ph.IMCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
Gamma-ray bursts represent some of the most energetic and complex phenomena in the universe, characterized by highly variable light curves that often contain observational gaps. Reconstructing these light curves is essential for gaining deeper insight into the physical processes driving such events. This study proposes a machine learning-based framework for the reconstruction of GAMMA-RAY BURST light curves, focusing specifically on the plateau phase observed in X-ray data. The analysis compares the performance of three sequential modeling approaches: a bidirectional recurrent neural network, a gated recurrent architecture, and a convolutional model designed for temporal data. The findings of this study indicate that the Bidirectional Gated Recurrent Unit model showed the best predictive accuracy among the evaluated models across all GRB types, as measured by Mean Absolute Error, Root Mean Square Error, and Coefficient of Determination. Notably, Bidirectional Gated Recurrent Unit exhibited enhanced capability in modeling both gradual plateau phases and abrupt transient features, including flares and breaks, particularly in complex light-curve scenarios.
[abstract 40 / 70] (score: 2) - Title: Revisit of the electroMAGNETic correction to $τ\toππν_τ$ and its implication for muon $g-2$ based on $τ$ dataAuthors: Zhi-Xin Li, Ao Li, Jin Hao, Chun-Gui Duan, Zhi-Hui Guo,Comments: 20 pages, 3 figures. To match the published versionSubjects: hep-phCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
In this work we focus on the evaluation of the leading-order hadronic vacuum POLARIZATION contribution from the $ππ$ channel to the muon anomalous MAGNETic moment $a_μ$ by using the experimental $τ\toππν_τ$ data. The isospin breaking corrections play the decisive role in this approach of computing $a_μ$. One of such important isospin breaking sources is the long-distance electroMAGNETic correction factor $G_{\rm EM}$ of the $τ\toππν_τ$ process from the real photon radiation. The latter effect can be calculated from the $τ\toππν_τγ$ amplitude, which is revised in this work within the resonance chiral theory by simultaneously including the even-intrinsic-parity and odd-intrinsic-parity resonance operators. We update the determination of the only unknown resonance coupling through the $ω\toπ^0π^0γ$ decay by including contributions from both the vector and scalar resonances. By taking other remaining contributions from the muon $g-2$ White Paper 2025, we further revise the complete value of $a_μ$, which turns out to deviate from the newest world average result after FERMIlab's measurement at the level of 2.7 $σ$.
[abstract 41 / 70] (score: 2) - Title: Comprehensive study of solar type II radio bursts and the properties of the associated shock wavesAuthors: K. Bhandari, D. E. Morosan, S. Normo,Comments: 13 pages (9 page main body, 4 page appendix), 13 figuresSubjects: astro-ph.SRCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
Type II radio bursts are solar radio emissions generated by electrons accelerated by coronal shocks. These bursts are typically found close to expanding coronal mass ejections (CMEs), making them valuable for studying the properties and dynamics of CME-driven shocks in the solar corona. Here, we aim to determine the regions in the solar corona where shock waves accelerate electrons and determine their characteristic properties. To do this, we combine radio observations of type II solar radio bursts with MAGNETo-hydrodynamic (MHD) simulations of the solar corona. We analyse ten type II radio bursts from Solar Cycle 25 exhibiting emissions. The novelty of this study lies in using radio imaging data for all type II bursts to examine the positions of the radio sources. The radio source positions, combined with a geometrical fitting of the CME shock and the MHD simulations, are used to determine essential shock parameters at the acceleration region, such as the Alfvén Mach number $(M_{\rm A}$ and $θ_{\rm BN}$. The shock parameters are then combined with the properties of the radio emission and the associated eruption in a comprehensive study. We found that for all events, the type II bursts are located near or inside coronal streamers. The estimated shock speeds are high, resulting in the formation of super-critical shocks ($3.8~\leq~M_{\rm A}~\leq~7.7$) at the type II locations. In most events, type II bursts are located at oblique shocks rather than near-perpendicular geometries, suggesting that the shock structure is more complex at local scales than the simple spherical shock models usually applied to CME shocks. Our results suggest that CME-streamer interaction regions are necessary for the generation of type II bursts, as they provide ideal plasma conditions for the formation of super-critical shocks and the subsequent acceleration of electrons.
[abstract 42 / 70] (score: 2) - Title: A positivity preserving and entropy stable nodal discontinuous Galerkin scheme for ideal MHDAuthors: Yue Wu, Chi-Wang Shu,Comments: 24 pages, 8 figuresSubjects: math.NA cs.NA physics.comp-phCreated: 2026-06-27; Updated: 2026-06-30; Datestamp: 2026-06-30
Numerically solving MAGNETohydrodynamic (MHD) equations faces many challenges: avoiding divergence error, maintaining positivity, and satisfying entropy conditions. Among discontinuous Galerkin (DG) schemes, there has been a modal version that is locally divergence-free and positivity preserving and a nodal version that is semi-discretely entropy stable. In this work, we develop a DG scheme that combines the advantages of these two and solves all the three challenges. The key ingredients that bring these two schemes together are an HLL numerical flux with entropy stable signal speed estimates and a locally divergence-free projection. To handle problems with strong shocks, the essentially oscillation-free damping is applied. Various numerical experiments verify the accuracy and robustness of our method.
[abstract 43 / 70] (score: 2) - Title: Nonradial oscillations of realistic anisotropic neutron stars: Axial modesAuthors: Jose F. Rodriguez-Ruiz, L. M. Becerra, F. D. Lora-Clavijo,Comments: 12 pages, 5 figures. Accepted for publication in Phys. Rev. D. Revised version to match the journal versionSubjects: gr-qc astro-ph.HECreated: 2026-06-27; Updated: 2026-06-30; Datestamp: 2026-06-30
Non-radial oscillation modes of neutron stars serve as diagnostics of their internal composition and RELATIVISTIC structure. In this work, we investigate the perturbations of static and spherically symmetric neutron stars characterized by an anisotropic pressure. Given the background symmetry, perturbations decouple into polar and axial modes. To date, axial modes have remained less explored, primarily because matter and metric perturbations decouple in the isotropic limit. In this work, we provide a consistent treatment of axial modes and demonstrate that pressure anisotropy induces a direct coupling between matter and metric perturbations. We employ parameterized anisotropy models that ensure consistency with the treatment of matter perturbations. We numerically integrate the linearized Einstein field equations for the axial modes, employing a diverse set of realistic equations of state. Our results indicate that as the stellar mass grows, the frequency of the base $w$-mode generally decreases, while its damping time increases. Softer equation of states typically yield slightly higher oscillation frequencies. Furthermore, larger anisotropy (i. e., when the tangential pressure exceeds the radial pressure) allows for more massive equilibrium configurations, which correspondingly leads to lower oscillation frequencies and prolonged damping times. Finally, we demonstrate that the frequency and damping time, both scaled by the stellar mass, exhibit a nearly universal quadratic dependence on the stellar compactness, remaining largely insensitive to the underlying equation of state, but slightly dependent to the specific anisotropy model.
[abstract 44 / 70] (score: 2) - Title: $Ab$ $initio$ modeling of Galactic dust polarized CMB foregroundAuthors: Alexei G. Kritsuk, Ka Wai Ho, Ka Ho Yuen, Raphael Flauger,Comments: 4 pages, 3 figures, contribution to the 2026 Cosmology session of the 60th Rencontres de MoriondSubjects: astro-ph.GA astro-ph.COCreated: 2026-06-26; Updated: 2026-06-30; Datestamp: 2026-06-30
We present the analysis of high-resolution synthetic dust POLARIZATION maps derived from large-scale simulations of MAGNETized multiphase interstellar turbulence carried out with the AthenaK code on the $Frontier$ exascale supercomputer at the Oak Ridge National Laboratory. Our turbulence model accurately captures spectral properties of the $E$- and $B$-modes measured by $Planck$ at 353 GHz. The simulations provide new insights into the physical origins of the observed $E/B$ asymmetry and positive $TE$ signal, facilitating the development of advanced models of Galactic foreground emission for current and future CMB experiments.
[abstract 45 / 70] (score: 2) - Title: Dynamical Casimir Effect and Vacuum Friction in the Near-Horizon Geometry of a Black HoleAuthors: Hamed Hadi, Amin Rezaei Akbarieh, Goksel Daylan Esmer,Comments: 12 pagesSubjects: gr-qcCreated: 2026-06-26; Updated: 2026-06-30; Datestamp: 2026-06-30
We investigate the Dynamical Casimir Effect (DCE) for a RELATIVISTIC scalar field confined within a cavity possessing moving boundaries in the (1+1)-dimensional near-horizon geometry of a BLACK HOLE. By applying a coordinate transformation, we map the moving-boundary problem to an equivalent acoustic metric with static boundaries, allowing for an exact canonical Hamiltonian formulation. We find that the local gravitational redshift fundamentally alters the vacuum structure, and the dynamical boundary motion induces time-dependent mode-mixing. When a boundary moves, it scatters the fluctuations of the ambient Hartle-Hawking state, generating a flux of created particles. Crucially, because the coordinate speed of light relative to the Killing time $t$ vanishes as one approaches the event horizon, we establish that maintaining physical, subluminal boundary motion requires the mechanical oscillation amplitude to scale proportionally with the proper distance to the horizon. Consequently, the effective Mach number of the moving mirror approaches zero in the near-horizon limit. Using a rigorous small-amplitude perturbative expansion and proper canonical operator normalization, we demonstrate that the transition probability into the field is heavily suppressed by a conformal geometric factor. Furthermore, we account for the Bose-enhancement caused by the thermal Hawking bath. While the thermal presence introduces infrared density-of-states enhancement, it remains insufficient to overcome the kinematic damping. Finally, we conclude that the extreme spacetime curvature acts to protect the near-horizon vacuum; the transition probability vanishes as the boundary approaches the event horizon, indicating a geometric and kinematic suppression of particle creation in the strong-gravity limit.
[abstract 46 / 70] (score: 2) - Title: ElectroMAGNETic duality degeneracy in dynamical BLACK HOLE mergersAuthors: José Ferreira, Gabriele Bozzola, Carlos A. R. Herdeiro, Vasileios Paschalidis, Miguel Zilhão,Comments: 11 pages, 9 figuresSubjects: gr-qc hep-thCreated: 2026-06-27; Updated: 2026-06-30; Datestamp: 2026-06-30
ElectroMAGNETic duality is a symmetry of the source-free Einstein-Maxwell equations that rotates electric and MAGNETic fields while leaving the stress-energy tensor invariant. We present the first fully nonlinear realization of this symmetry in dynamical strong-gravity regimes by performing numerical relativity simulations of charged BLACK HOLE mergers across a continuous duality family. Starting from electrically charged binaries, we generate dyonic and MAGNETically charged configurations via duality rotations and evolve them within a common numerical framework. We find that all dual configurations exhibit identical spacetime dynamics, while the emitted electroMAGNETic radiation is related by a rotation of its POLARIZATION equal to the duality angle. Our results demonstrate a degeneracy of gravitational observables under electroMAGNETic duality and provide a concrete mapping between dual configurations at the level of radiation, establishing electroMAGNETic duality as an organizing principle for dynamical Einstein-Maxwell solutions.
[abstract 47 / 70] (score: 2) - Title: JWST observations support the jittering-JETs explosion mechanism (JJEM) for the core-collapse SUPERNOVA remnant SNR 0540-69.3Authors: Dmitry Shishkin, Noam Soker,Comments: Will be submitted in two days to allow for commentsSubjects: astro-ph.HECreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
We examine published JWST observations of the core-collapse SUPERNOVA (CCSN) remnant SNR 0540-69.3 and identify a point-symmetric morphology in its inner ejecta. Within the framework of the jittering JETs explosion mechanism (JJEM), we interpret this morphology as evidence that the ejecta were shaped by two, and likely three or more, pairs of JETs during the explosion process. Both visual inspection and a recently developed quantitative symmetry-identification method for astrophysical imaging reveal an approximate rotational symmetry between the northeastern redshifted ejecta and the southwestern blueshifted ejecta. Each side contains clumps (knots) surrounding a previously identified cavity, with the best quantitative correspondence obtained for a rotation of 189°. We further identify a symmetry center that is offset from the current pulsar position, strengthening an earlier claim for a pulsar kick. We interpret the pair of cavities and their surrounding clumpy structures as having been shaped by multiple JET-launching episodes. In addition, we identify a pair of opposing nozzles at a large angle to the cavities, which we attribute to another JET pair. Guided by the similarities to point-symmetric planetary nebulae shaped by JETs and by recent three-dimensional hydrodynamical simulations of the JJEM, we conclude that the inner ejecta were shaped by at least three JET pairs launched by the neutron star after it acquired its kick velocity, consistent with the JJEM.
[abstract 48 / 70] (score: 2) - Title: Twin Peaks: Resolving Features in the Binary Black Hole Mass Function with COSMIC-METISSEAuthors: Duncan B. Maclean, Poojan Agrawal, Katelyn Breivik, and Alexandra G. Guerrero, Michael Zevin, Mathieu Renzo, Carl L. Rodriguez,Comments: 22 pages, 12 figures. Submitted to ApJSubjects: astro-ph.HECreated: 2026-06-26; Updated: 2026-06-30; Datestamp: 2026-06-30
Gravitational waves from inspiraling binary BLACK HOLEs (BBHs) provide insights into the lives and deaths of massive stars. Population synthesis allows us to model these binaries through isolated binary evolution, but its predictive power is limited by difficulties in varying the stellar models and their associated uncertainties. We present a new grid of stellar tracks computed with the open-source stellar evolution code MESA, spanning metallicities $10^{-3} \le Z/Z_{\odot} \le 7$. We vary two stellar physics parameters: wind-driven mass loss and the convective boundary mixing (CBM) mechanism. We pair these models with the Method of Interpolation for Single Stellar Evolution (METISSE) and binary population synthesis code COSMIC to obtain synthetic populations of merging BBHs in the local Universe. We find a maximum in the primary mass spectrum near $10M_\odot$ which in most model variations is composed of two sub-populations at $\approx8M_{\odot}$ and $\approx13 M_\odot$, with the higher-mass population dominated by BBHs whose progenitors underwent a mass ratio reversal (MRR). This population also suggests an anticorrelation between higher primary masses and mass ratio, as BBHs with $m_1\gtrapprox10M_\odot$ preferentially undergo MRR and prefer a final mass ratio of $q\approx0.7$. However, the location and relative strength of these two sub-populations is sensitive to our assumed stellar physics: varying both the wind and CBM treatments can merge the MRR and non-MRR populations into a single peak near $9M_\odot$. Variations in our stellar tracks, especially CBM, lead to a factor of $\approx6$ difference in the rate, primarily due to modulation of the common envelope formation channel.
[abstract 49 / 70] (score: 2) - Title: The NANOGrav 15 yr Data Set: Impacts of Customized Chromatic Noise Models on Gravitational Wave AnalysesAuthors: Nikita Agarwal, Gabriella Agazie, Alessandra Amosso, Akash Anumarlapudi, Anne M. Archibald, Zaven Arzoumanian, Anjana Ashok, Jeremy G. Baier, Paul T. Baker, Bence Becsy, Laura Blecha, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Rand Burnette, Robin Case, J. Andrew Casey-Clyde, Yu-Ting Chang, Maria Charisi, Shami Chatterjee, Tyler Cohen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Kathryn Crowter, Megan E. DeCesar, Paul B. Demorest, Heling Deng, Lankeswar Dey, Timothy Dolch, Graham M. Doskoch, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Emiko C. Gardiner, Nate Garver-Daniels, Peter A. Gentile, Kyle A. Gersbach, Joseph Glaser, Deborah C. Good, Kayhan Gultekin, Aiden Gundersen, C. J. Harris, Doa Hashemi Asl, Jeffrey S. Hazboun, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, David L. Kaplan, Anala K. Sreekumar, Luke Zoltan Kelley, Matthew Kerr, Joey S. Key, Nima Laal, Michael T. Lam, William G. Lamb, Bjorn Larsen, T. Joseph W. Lazio, Natalia Lewandowska, Tingting Liu, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Chung-Pei Ma, Dustin R. Madison, Ashley Martsen, Cayenne Matt, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Patrick M. Meyers, Matthew T. Miles, Chiara M. F. Mingarelli, Andrea Mitridate, Cherry Ng, David J. Nice, Shania Nichols, Stella K. Ocker, Daniel J. Oliver, Ken D. Olum, Timothy T. Pennucci, Benetge B. P. Perera, Polina Petrov, Nihan S. Pol, Henri A. Radovan, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Jessie C. Runnoe, Alexander Saffer, Shashwat C. Sardesai, Ann Schmiedekamp, Carl Schmiedekamp, Kai Schmitz, Levi Schult, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Sophia V. Sosa Fiscella, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Robin Strahler, Abhimanyu Susobhanan, Joseph K. Swiggum, Jacob Taylor, Stephen R. Taylor, Mercedes S. Thompson, Jacob E. Turner, Michele Vallisneri, Rutger van Haasteren, Joris P. W. Verbiest, Sarah J. Vigeland, Haley M. Wahl, Kalista Wayt, Kevin P. Wilson, Caitlin A. Witt, David Wright, Olivia Young,Comments: 28 pages, 17 figures, Submitted to Astrophysical Journal Letters. For questions or comments, please email jeremy.baier@nanograv.org or bjorn.larsen@nanograv.orgSubjects: astro-ph.CO astro-ph.HECreated: 2026-06-26; Updated: 2026-06-30; Datestamp: 2026-06-30
We report updated nHz gravitational wave (GW) significance, characterization, and interpretations using the customized chromatic-noise models (CNMs) developed in Larsen, Baier et al. (2026). for the NANOGrav 15-year data set. We find increased evidence for the Hellings-Downs (HD) correlation signature of the stochastic gravitational wave background (GWB), with a Bayes factor of $1571\pm14$ for HD-correlations over a common uncorrelated red-noise process using a power-law model with $14$ Fourier modes. We find this $\sim8\times$ increase in Bayes factor from Agazie et al. (2023a) is a result of improved noise mitigation. Assuming an analytic null distribution for the frequentist interpulsar correlation statistic, this corresponds to a slightly more significant measurement from $3.16σ$ to $3.32σ$ against the no-correlation scenario. Spectral inference with CNMs brings the power-law GWB amplitude down to $A_{\rm GWB} = 2.1^{+0.6}_{-0.5}\times10^{-15}$ at fixed $γ_{\rm GWB} = 13/3$. In a varied-$γ$ analysis, the spectral index increases to $γ_{\rm GWB}=3.5^{+0.7}_{-0.6}$. We report updates on an all-sky continuous gravitational wave (CW) search as well as select targeted searches and calculate a $3.2\times$ larger detection volume for the NANOGrav detector. With CNMs, we find reduced evidence for a non-Einsteinian, scalar-transverse mode of gravity. Finally, we reinterpret the GWB first with the assumption of an astrophysical background sourced by SMBHBs and then assuming the more exotic origins of cosmic inflation, a first-order cosmological phase transition, and stable cosmic strings. Under both the SMBHB hypothesis and the cosmological hypotheses, we see only marginal shifts in model parameter posteriors which are consistent with the slightly quieter and steeper power-law GWB spectrum.
[abstract 50 / 70] (score: 2) - Title: Confinement-Induced Suppression of Jet Drop Size by Bubble Bursting in Shallow LiquidsAuthors: Zhengyu Yang, Vatsal Sanjay, C. Ricardo Constante-Amores, Jie Feng,Comments: 7 pages, 4 figuresSubjects: physics.flu-dynCreated: 2026-06-26; Updated: 2026-06-30; Datestamp: 2026-06-30
Bubble bursting is a major source of aerosol generation in a wide range of natural and industrial systems. While the resulting JET dynamics have been extensively studied in deep liquid pools, bubble bursting often occurs in shallow liquid layers where the influence of the nearby solid boundary remains poorly understood. Here, we show numerically that a shallow liquid layer produces smaller and more numerous JET drops, even when the initial bubble shape is unchanged. We identify a wall-induced viscous sticking effect that suppresses the upward motion of the cavity bottom, leading to a steeper cavity geometry during capillary-wave focusing. We further develop a semi-empirical scaling law that predicts the JET drop radius as a function of the Ohnesorge number and the initial bubble-wall distance. Our results establish geometric confinement as a governing factor in bubble bursting and provide a framework for predicting and controlling aerosol generation in shallow liquid environments.
[abstract 51 / 70] (score: 2) - Title: Wave Activity at MHD-ion Scales Associated with SwitchbacksAuthors: Kyung-Eun Choi, Oleksiy V. Agapitov, Forrest Mozer, Seung-Ju Yang, Dae-Young Lee, Richard D. Sydora, Lucas Colomban, Liudmyla Kozak, Mingzhe Liu, Marc Pulupa, Jia Huang, Shaosui Xu,Comments: Submitted to The Astrophysical JournalSubjects: physics.space-ph astro-ph.SRCreated: 2026-06-26; Updated: 2026-06-30; Datestamp: 2026-06-30
Magnetic switchbacks (SB) -- the localized MAGNETic structures with MAGNETic field direction inclined at an angle $θ$ relative to the background $B_0$ -- in the young solar wind have been associated with enhanced ion-scale wave activity and local plasma heating. It remains debated whether the apparent wave-power increase is intrinsic or mainly caused by sampling geometry. In this work, we analyze MAGNETic and electric field fluctuations measured by Parker Solar Probe, focusing on the 0.1--3~\(f_{cp}\) frequency band that spans the transition from the MHD inertial range to ion-kinetic scales. By decomposing MAGNETic fluctuations into field-aligned and transverse components and comparing SB and non-SB intervals at the same local MAGNETic field angle, we test whether SBs sample an anisotropic cascade from different viewing angles or host intrinsically amplified wave activity. We find that the transverse MAGNETic power $δB_{\perp}$ is systematically enhanced inside switchbacks across a wide range of MAGNETic field rotation angles $θ$. The enhancement persists even at small and intermediate deflections, where geometric projection alone predicts weak power, indicating an intrinsic origin beyond sampling geometry. The inertial-range spectral indices also remain similar between SB and non-SB intervals despite the enhanced wave power inside SBs, suggesting that the underlying turbulence cascade is largely preserved. This excess $δB_{\perp}$ coincides with elevated proton temperatures and enhanced electric-field fluctuations, supporting the interpretation that SBs act as localized sites of cross-scale energy transfer and ion-scale dissipation in the near-Sun solar wind.
[abstract 52 / 70] (score: 2) - Title: Enhancing VLBI Capability with the SKA-Mid and the Jingdong 120-m Radio TelescopeAuthors: Wen Chen, Jun Yang, Zhixuan Li, Yingjie Li, Niu Liu,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Chen01Subjects: astro-ph.IM astro-ph.GACreated: 2026-06-27; Updated: 2026-06-30; Datestamp: 2026-06-30
The Jingdong Radio Telescope (JRT) is a 120-meter fully steerable radio telescope currently under construction in Jingdong County, Yunnan Province, China. Located at a relatively low latitude (24.5 degree), the JRT will enable observations of nearly 90% of the sky. Equipped with two broadband single-pixel receivers covering 1-8 GHz and 6-18 GHz, and a powerful digital backend, the telescope will support single-dish studies of various radio sources-particularly millisecond pulsars for enhancing the detection of nanohertz gravitational waves. In addition to single-dish capabilities, the JRT is expected to contribute approximately 800 hours annually to international Very Long Baseline Interferometry (VLBI) observations via a standard VLBI backend. When operating in conjunction with the phased-up SKA-Mid, the JRT will significantly enhance the technical and scientific capabilities of existing VLBI networks. This paper presents a comprehensive overview of the JRT's VLBI module and explores its potential to improve joint VLBI observations with current VLBI networks. Our analysis suggests that coordinated VLBI observations involving both the SKA-Mid and the JRT have the potential to significantly advance the field. For early sciences, we also highlight a few highly promising scientific cases, e.g. measuring the distance to PSR J0437-4715 with <1 ly accuracy and exploring JET formation with an event-horizon-scale resolution in M60*.
[abstract 53 / 70] (score: 2) - Title: Cosmological inference from the eBOSS QSO full-shape analysis with optimal redshift weightsAuthors: Xiaoyong Mu, Zhuo-Heng Li, Wentao Luo, Yuting Wang, Gong-Bo Zhao,Comments: 12 pages, 9 figures, comments welcomeSubjects: astro-ph.COCreated: 2026-06-27; Updated: 2026-06-30; Datestamp: 2026-06-30
We present a full-shape power-spectrum analysis of the eBOSS DR16 QUASAR sample with optimal redshift weights. The DR16 QSO catalog contains 343,708 QUASARs over $0.8
[abstract 54 / 70] (score: 2) - Title: Quadrupole and quadratic-in-spin effects in quasicircular, spinning, asymmetric binariesAuthors: Mostafizur Rahman, Misbah Shahzadi, Adam Pound, Josh Mathews,Comments: 24 pages, 7 figures, 3 tablesSubjects: gr-qcCreated: 2026-06-27; Updated: 2026-06-30; Datestamp: 2026-06-30
Next-generation gravitational-wave detectors will require significant improvements in current theoretical waveform models, particularly in the case of asymmetric-mass binaries. Here we provide one such improvement by calculating fully RELATIVISTIC finite-size effects for small mass ratios -- primarily, fluxes of energy -- including quadratic-in-secondary-spin terms, spin-induced quadrupole terms, and tidally induced quadrupole terms, for quasicircular inspirals of a small companion into a Kerr BLACK HOLE. We formulate these calculations within a multiscale waveform-generation framework in self-force theory, which could be used, with an energy-balance law we derive, to develop self-contained waveform models for asymmetric binaries involving stars orbiting BLACK HOLEs. Our results could additionally be used to improve other families of waveform models across all mass ratios. We present results both as complete numerical data sets on a Chebyshev grid and as analytical post-Newtonian expansions (to sixth PN order relative to the leading term in each contribution to the flux).
[abstract 55 / 70] (score: 2) - Title: Tracking Entanglement Transfer: Emergence of Thermodynamics from Quantum InformationAuthors: Debraj Debata, Abhirup Mukherjee, Siddhartha Lal,Comments: 15 pages, 15 figures with captionSubjects: quant-phCreated: 2026-06-27; Updated: 2026-06-30; Datestamp: 2026-06-30
We study entanglement transfer in a minimal model of two qubits that are coupled with one another through an antiferroMAGNETic Heisenberg exchange ($\tilde{J}$), and where one of them is additionally coupled to a fermionic environment through another antiferroMAGNETic Heisenberg exchange ($J_{K}$). By tuning the coupling ratio $J_{K}/\tilde{J}$, the system undergoes a quantum phase transition at $T=0$, accompanied by a redistribution of entanglement from the $d'-d$ qubit-subsystem to the environment. Remarkably, the resulting physics exhibits properties that bear analogy with a quantum-information theoretic perspective of the physics of BLACK HOLE thermodynamics. Carefully selected bipartite and tripartite mutual information measures displays behaviour analogous to the dynamical evolution of BLACK HOLE entropy, Hawking entropy, and the Page curve expected during the process of evaporation. An effective temperature scale is obtained from the variation of the ground state energy with respect to changes in the bipartite mutual information between the subsystem and the bath. A steady growth of this temperature with the coupling ratio resembles that of the Hawking temperature with the inverse mass of the BLACK HOLE. Concomitantly, the emergence of non-FERMI liquid behaviour observed near the quantum critical point and in the strong-coupling phase resembles strange-metal-like physics expected near the event horizon from a holographic duality perspective. Our results establish the minimal model as a platform for studying entanglement transfer and information scrambling within a fully unitary quantum framework, and offer new insights into a resolution of the BLACK HOLE information paradox.
[abstract 56 / 70] (score: 2) - Title: Detecting Quantum Stochastic Effects in Radiation Reaction via Laser-Produced Surface QED PlasmasAuthors: Junhua Zhang, Xianshu Wu, Luyao Zhang, Yao Meng, Longqing Yi,Comments: 7 pages,5 figuresSubjects: physics.plasm-phCreated: 2026-06-28; Updated: 2026-06-30; Datestamp: 2026-06-30
We propose a method to detect quantum stochastic effects in radiation reaction by irradiating a V-shaped plasma cavity with an ultra-intense LASER pulse. The pulse accelerates GeV electrons along the inner surface and simultaneously drives strong-field surface wave near the cavity apex. The accelerated electron bunches then collide with the surface wave, the latter acts as an effective counter-propagating ultra-intense electroMAGNETic wave, triggering significant radiation reaction. Importantly, because the surface wave is confined to an ultra-thin QED plasma layer (on the scale of the skin depth) where the expected number of hard photon emissions per electron is of order unity, stochastic effects are expected. Three-dimensional particle-in-cell simulations with different QED models show that radiation reaction strongly reshapes the angular distribution of high-energy electrons. In particular, electrons deflected by the surface wave experience strong radiation loss. However, compared with the semi-classical model, the stochastic QED model preserves a higher-energy component in the deflected beam, producing a clear angular-spectral signature, which potentially opens a pathway for experimental study of quantum stochastic effects in radiation reaction.
[abstract 57 / 70] (score: 2) - Title: Saturation Equations of State in Critical Gravitational Collapse: The Primordial Black Hole ThresholdAuthors: Benaoumeur Bakhti,Comments:Subjects: gr-qcCreated: 2026-06-28; Updated: 2026-06-30; Datestamp: 2026-06-30
The threshold and scaling laws of gravitational critical collapse depend sensitively on the matter equation of state. We investigate how these quantities are modified by a generic feature of dense matter that is absent from the radiation fluid commonly assumed in primordial BLACK HOLE (PBH) studies: pressure stiffening as a maximum density is approached. As an analytically tractable proxy, we adopt the closed-form equation of state of a single-occupancy lattice gas, \(p=-T\ln(1-ρ)\), which exhibits a density-dependent sound speed and a saturation density. Using general-RELATIVISTIC simulations of spherically symmetric collapse, we show that this nonlinear pressure feedback increases the PBH formation threshold by \(0.50\pm0.02\%\) relative to the radiation equation of state within the causal regime of the model. At the same time, the critical mass-scaling exponent remains \(γ=0.357\pm0.001\), consistent with the radiation-fluid value to within our numerical precision. This agreement reflects the fact that the lattice equation of state approaches the radiation fluid at low density and remains only a mild perturbation over the near-critical regime, rather than indicating a universal critical exponent. Our results provide a proof of principle that saturation-induced stiffening can stabilize gravitational collapse and shift the PBH threshold, while introducing a linear-response framework for assessing the impact of more realistic equations of state on primordial BLACK HOLE formation.
[abstract 58 / 70] (score: 2) - Title: Bidirectional Autoregressive Latent Diffusion for Forward and Inverse MagnetohydrodynamicsAuthors: Alexander Scheinker,Comments:Subjects: stat.ML cs.LG nlin.AO physics.plasm-phCreated: 2026-06-28; Updated: 2026-06-30; Datestamp: 2026-06-30
This work presents a new bidirectional autoregressive latent diffusion approach for predicting the evolution of multiple fields (mass density, pressure, velocity, and MAGNETic field components) for MAGNETohydrodynamics. We show that this bidirectional flow can be used as a self-supervised consistency metric for uncertainty and error estimation, which enables the model to estimate test-time uncertainty and error without access to ground truth, by comparing how closely flowing forwards and backwards in time returns to the same predicted fields. We also demonstrate this methods's potential to serve as a non-invasive plasma diagnostic, and show how adaptive feedback can be used to make the model more robust based on sparse diagnostics or limited views/measurements.
[abstract 59 / 70] (score: 2) - Title: VLBI Astrometry of MagnetarsAuthors: Takuya Akahori, Sujin Eie, Kei Amada, Sangita Kumari, Kohei Kurahara, Hiroto Masaoka, Hao Ding, Teruaki Enoto, Shota Kisaka, Keiichi Maeda, Kotaro Niinuma,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Akahori02Subjects: astro-ph.HE astro-ph.SRCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
The origin of the strongest MAGNETic fields in the Universe, i.e., the origin of MAGNETars, is a longstanding question. An enhanced dynamo effect in an irregular SUPERNOVA explosion is a possible origin, which implies a stronger kick velocity and a higher proper motion of the MAGNETar compared to those of ordinary pulsars as well as an irregular morphology of the host SUPERNOVA remnant (SNR). However, this hypothesis is not well studied yet, because there is a lack of precise measurement of the proper motion of MAGNETar and of identification of the host SNR. VLBI astrometry of MAGNETars is a unique tool to examine the hypothesis. In this chapter, we introduce the MONSTER (Monitoring Observations of the Neutron Stars That Evolve Rapidly) Project. SKA-VLBI's unprecedented sensitivity and the highest angular resolution will allow us to dramatically expand the survey volume in which we can measure the proper motion of MAGNETars within a radio outburst period of a few months.
[abstract 60 / 70] (score: 2) - Title: Verified residual-specific explicit derivative kernels for physics-informed learning and discretized PDE adjointsAuthors: Wenbo Cao, Zhe Lu, Weiwei Zhang,Comments:Subjects: physics.comp-phCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
Derivative computation is central to scientific computing, from space-time derivatives in physics-informed neural networks (PINNs) to residual Jacobian actions and discrete-adjoint operators in computational fluid dynamics (CFD). General-purpose automatic differentiation (AD) reduces implementation effort, but can incur substantial runtime and memory overhead for high-order residuals and complex discretized operators. Explicit derivative kernels can exploit problem-specific structure and provide efficient, controllable evaluations, but their use has been limited by derivation and implementation costs. This work revisits explicit differentiation (ED) as a residual-specific and verifiable route enabled by agent-assisted implementation and stringent numerical verification. For PINNs, we propose residual-specific partial-JET propagation, which makes the derivative-state closure of the target PDE residual explicit and realizes it through specialized layerwise kernels, rather than relying only on nested AD or a generic Taylor-mode transform. Relative to nested AD, the resulting ED kernels achieve floating-point-level agreement in residual and parameter-gradient evaluations and accelerate complete PINN training, often reaching 2-4x speedups while reducing peak GPU memory in most cases. For discretized PDE adjoints, we apply the same verification-driven strategy to a finite-volume CFD residual. The generated tangent-action and transpose-action kernels pass Taylor-remainder, inner-product, and reduced-gradient consistency checks, and are embedded into a GPU-resident discrete-adjoint workflow for freestream Mach-number and angle-of-attack inversion. These results suggest that verified explicit derivative kernels, supported by agent-assisted implementation, can serve as a practical, structure-aware complement to general-purpose AD for derivative-intensive scientific computing.
[abstract 61 / 70] (score: 2) - Title: Photon Motion and Shadows of Rotating Black Holes with Nonlinear ElectroMAGNETic and Anisotropic Matter FieldsAuthors: Mou Xu, Jianbo Lu, Yu Liu, Shumin Wu,Comments: 20 pages, 5 figuresSubjects: gr-qcCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
This paper investigates the effects of the nonlinear electroMAGNETic field and the anisotropic matter field on photon motion, shadow structures, and the energy emission rate of a rotating BLACK HOLE (BH). Using the Hamilton-Jacobi formalism, we derive the photon motion equations and analyze the distribution and stability of photon regions. The results show that the anisotropic matter field parameters affect the size and shape of the photon region outside the event horizon more significantly than the nonlinear electroMAGNETic field parameter. As the anisotropic matter field parameter $K$ decreases, the unstable photon region outside the BH gradually expands and becomes increasingly flattened. Furthermore, we construct the BH shadow in terms of the celestial coordinates and obtain the corresponding shadow images by backward ray tracing. Several shadow observables, including the shadow radius, distortion parameter, shadow area, and oblateness, are also analyzed. The results indicate that the anisotropic matter field affects the shadow size more strongly than the shadow shape. Specifically, the shadow radius and area both decrease significantly as the parameter $K$ decreases, but increase markedly as the anisotropic matter state parameter $ω$ increases. In addition, we analyze the energy emission rate of the BH and find that decreasing $K$ or increasing MAGNETic charge $Q$ suppresses its peak value, while the influence of $ω$ remains comparatively mild. These results provide a useful reference for understanding the effects of nonlinear electroMAGNETic and anisotropic matter fields on rotating BH shadows and related observational signatures.
[abstract 62 / 70] (score: 2) - Title: Kinematics of Weak Cool-Core Cluster A3571 Observed with XRISM: Low Cooling Rate Balanced by Low Heating RateAuthors: Hannah McCall, Irina Zhuravleva, Kyoko Matsushita, Annie Heinrich, Congyao Zhang, Eugene Churazov, William Forman, Ildar Khabibullin, Kotaro Fukushima, Daniele Rogantini, Itsuki Aihara, Christine Jones, Kazunori Suda,Comments: 14 pages, 8 figures. Submitted to The Open Journal of AstrophysicsSubjects: astro-ph.GA astro-ph.HECreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
Most XRISM galaxy cluster observations to date have focused on AGN feedback or actively merging systems. The weak cool-core cluster A3571 was observed in four XRISM Cycle 1 pointings, enabling the study of gas kinematics in a relaxed, AGN-feedback-free system. We present measurements of the velocity dispersion and bulk velocity in the core regions of A3571, out to $120$ kpc. The velocity dispersion is relatively uniform across all regions ($\sim100-120 ~\mathrm{km~s^{-1}}$), except in the northern gas sloshing elongation, where a $68\%$ upper limit of $68~\mathrm{km~s^{-1}}$ is obtained. The core Mach number and non-thermal pressure fraction of A3571 are lower than in the extremely relaxed cluster A2029 and below predictions from cosmological simulation suites. Despite relatively low velocity dispersion values, the derived turbulent heating rate is sufficient to offset cooling losses in all studied regions. This suggests that sloshing motions contribute significantly to the heating budget. Comparing XRISM observations of merging and relaxed clusters, we find that mergers exhibit an average Mach number of $0.29\pm0.07$, nearly twice that of the relaxed sample, which is consistent with predictions from non-radiative cosmological simulations. A3571 is a promising target for resonant scattering studies; however, simulations indicate that deeper observations are required to obtain reliable turbulent velocities via the $z/w$ line ratio.
[abstract 63 / 70] (score: 2) - Title: Multi-height Identification of Sausage and Fluting Eigenmodes in a Solar PoreAuthors: Shahin Jafarzadeh, David B. Jess, Marco Stangalini, Luiz A. C. A. Schiavo, Timothy J. Duckenfield, Suzana S. A. Silva, Gary Verth, Viktor Fedun, Sami K. Solanki, H. N. Smitha, Andreas Lagg, Achim Gandorfer, Alex Feller, Francisco A. Iglesias, Tino L. Riethmüller, Bianca Grauf, Johannes Hoelken, Yukio Katsukawa, Pietro Bernasconi, Thomas Berkefeld, Alberto Álvarez-Herrero, Masahito Kubo, David Orozco Suárez, Michael Carpenter, Alexander Bell, Valentín Martínez Pillet, Francisco Javier Bailén, Julian Blanco Rodríguez, Juan Sebastián Castellanos Durán, Edvarda Harnes, Ryohtaroh T. Ishikawa, Yusuke Kawabata, Takuma Matsumoto, Takayoshi Oba, Azaymi L. Siu-Tapia, Hanna Strecker, Dušan Vukadinović,Comments: Accepted for publication in The Astrophysical Journal LettersSubjects: astro-ph.SRCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
Magnetic pores are compact, strongly MAGNETised waveguides in the lower solar atmosphere and therefore provide favourable conditions for identifying MAGNETohydrodynamic (MHD) wave modes. Earlier seeing-free observations revealed concurrent sausage, kink, and fluting modes in photospheric pores, but only at a single sampled layer. In this Letter, we exploit the dense spectral sampling of the near-ultraviolet 327-329 nm window observed by the Sunrise-III UV Spectropolarimeter and Imager (SUSI) to investigate how pore wave modes behave across multiple photospheric and low-chromospheric heights spanning roughly 500 km. We analyse ~75 min of a Sunrise-III/SUSI time series containing a small solar pore. From eight selected spectral lines sampling different estimated formation heights, we identify the pore boundary at each line and time step and apply proper orthogonal decomposition (POD) to the boundary oscillations. In all eight lines, the first POD mode is consistently identified as an axisymmetric sausage mode, with dominant power at ~1-2 mHz, and carries the dominant normalised eigenvalue fraction, typically about 66-86%, while the second mode is a fluting mode with azimuthal wave number m = 2, dominant at ~2-3.5 mHz, and contributes about 4-10%. Cross-line wavelet phase analysis of the temporal coefficients shows that the sausage mode remains close to zero phase difference across the sampled heights, consistent with standing or near-standing behaviour, whereas the fluting mode displays a modest but systematic increase in phase with height, reaching about 50 degrees, indicative of an upward-propagating component. These observations provide the first multi-height identification and phase characterisation of sausage and fluting modes inferred from pore-boundary oscillations.
[abstract 64 / 70] (score: 2) - Title: Probing Magnetic Fields In and Around Galaxies Near and FarAuthors: S. A. Mao, Rainer Beck, Aritra Basu, Lerato Baidoo, Andrea Bracco, Ralf-Jürgen Dettmar, Volker Heesen, Cathy Horellou, Timea O. Kovacs, Kohei Kurahara, Yu-Qing Lou, Yik Ki Ma, Rikuto Omae, Rosita Paladino, Amit Seta, Fatemeh Tabatabaei, Theresa Wiegert,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Mao01Subjects: astro-ph.GACreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
In order to understand the MAGNETization of galaxies and the role of MAGNETic fields in feedback processes that govern STAR FORMATION and galaxy evolution, it is essential to have a comprehensive census of MAGNETic fields in and around galaxies from the nearby Universe to high redshifts. In this chapter, we outline the science goals, strategies, techniques, and observational requirements with SKA AA4 for (1) a homogeneous polarimetric survey of nearby galaxies - mapping both the diffuse polarized emission as well as producing a dense RM grid within the virial radius; (2) a survey of the interstellar MAGNETic fields in distant galaxies targeting strong lensing systems with polarized lensed QUASARs, as well as a general statistical back-illumination survey to probe the redshift evolution of MAGNETic fields in the CGM. These proposed observations will serve as a major step towards understanding the co-evolution of galaxies and their MAGNETic fields over cosmic time and provide constraints on galactic dynamo theories.
[abstract 65 / 70] (score: 2) - Title: Fusion-power amplification by compressive hydrodynamic fluctuationsAuthors: Henry Fetsch, Nathaniel J. Fisch,Comments: 54 pages, 18 figures, 1 tableSubjects: physics.plasm-phCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
Compressive fluctuations in hot plasma, including acoustic waves and compressible turbulence, increase the rate of fusion reactions. This power amplification comprises hydrodynamic, ``two-temperature,'' and kinetic components, the first resulting from the clumping of hot ions in the peaks of the fluctuations, the second from the unequal heating of ions and electrons as fluctuations dissipate, and the third from the long mean free paths of fast ions near the Gamow peak, which allow these ions to stream across gradients in fluctuating hydrodynamic fields before colliding. In many cases, the increase in fusion power produced by waves exceeds that produced if the wave energy were instead used for heating. Response functions describing the modification to fusion power by compressive fluctuations are obtained in MAGNETized and unMAGNETized fusion plasmas. Comparison to the related shear flow reactivity enhancement effect, a kinetic mechanism that increases fusion power in some divergence-free flows, illustrates a fundamental distinction between compressible and solenoidal turbulence in fusion plasmas.
[abstract 66 / 70] (score: 2) - Title: Sudden expansion stability thresholds modified by lateral flowsAuthors: T. Salamon, R. Debuysschère, A. Chafaï, B. Scheid, F. Gallaire,Comments: 15 pages, 9 figuresSubjects: physics.flu-dynCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
We study the flow in a symmetric three-dimensional confined sudden expansion with lateral inflow at Reynolds number below 300 and varying lateral-to-central flow rate ratio, using experiments, linear stability analysis, weakly nonlinear theory, and direct numerical simulations. Three distinct flow regimes are identified. Outside an intermediate band of lateral-to-central flow rate ratio, the flow undergoes a steady symmetry-breaking bifurcation above a critical Reynolds number, deflecting the central JET toward one side wall; weakly nonlinear analysis shows this bifurcation to be supercritical, excepting a very narrow parametric range. Within the intermediate band, no such critical Reynolds number exists and direct numerical simulations confirm that residual velocity asymmetries reflect the imposed geometric imperfections rather than intrinsic amplification. Fluctuations observed experimentally in the intermediate band of lateral-to-central flow rate ratio remain unexplained and warrant further investigation.
[abstract 67 / 70] (score: 2) - Title: Differential Invariants of Carrollian SpacetimesAuthors: Boris Kruglikov, Eivind Schneider, Wijnand Steneker,Comments: 24 pagesSubjects: math.DG gr-qcCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
We compute invariants of Carrollian spacetimes, deriving them from the geometry of the screen bundle. For generic Carrollian structures we specify how to generate the entire algebra of differential invariants, with emphasis on dimension 3, which has special physical relevance. Then, in the framework of JET-spaces, we compute the numerology behind these invariants: the Hilbert and Poincaré functions that govern their numbers according to order. Finally, we compute the Spencer cohomology behind the Carrollian geometry that, in particular, contains the spaces of intrinsic torsion and intrinsic curvature, which are fundamental invariants, important in the equivalence problem and symmetry analysis. Thus, we also discuss symmetry sizes of Carrollian spacetimes.
[abstract 68 / 70] (score: 2) - Title: Sloshing Motions in Abell 3571 Revealed by XRISM/Resolve Velocity MappingAuthors: Itsuki Aihara, Congyao Zhang, Sora Nakajima, Kyoko Matsushita, Hannah McCall, Irina Zhuravleva, Shogo B. Kobayashi, Kotaro Fukushima, William R. Forman, Christine Jones, Annie Heinrich, Daniele Rogantini, Kosuke Sato, Kazunori Suda, Ildar Khabibullin,Comments: Submitted to AAS Journal. 10 pages, 4 figuresSubjects: astro-ph.HECreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
Minor mergers can induce sloshing motions in the intracluster medium, leaving characteristic signatures in the thermodynamic structure and gas kinematics of cluster cores. Abell 3571 is an X-ray-bright, apparently relaxed cluster at $z \sim 0.04$. We observed the central $\sim 300$ kpc region of Abell 3571 with four partially overlapping XRISM Resolve pointings, covering three contiguous Resolve fields to the north, south and east with a total exposure time of approximately 575 ks. The velocity dispersions are subsonic and are at the level of $\sim 100$--$150 \, \mathrm{km~ \, s^{-1}}$ across most regions. The cooler region associated with the northern surface-brightness excess is blueshifted by up to $\sim -60 \, \mathrm{km \, s^{-1}}$ relative to the brightest cluster galaxy (BCG), while the hotter region in the southern and eastern surface-brightness deficit regions is redshifted by up to $\sim 170 \, \mathrm{km \, s^{-1}}$. Numerical simulations suggest that this large-scale thermodynamic and kinematic asymmetry is broadly consistent with early-phase sloshing induced by an off-axis minor merger. Abell 3572, an X-ray-faint gas-poor cluster located 1.6 Mpc to the south, is a promising candidate for the perturber. Given the lack of clear signatures of prominent AGN feedback in Abell 3571, these results suggest that sloshing-driven gas redistribution may contribute to delaying the re-establishment of a strong cool core in Abell 3571.
[abstract 69 / 70] (score: 2) - Title: Comment on the "New Rotating Black Hole in ElectroMAGNETic Fields: Cosmological Horizon without Cosmological Constant''Authors: Hryhorii Ovcharenko,Comments: 8 pages. Comment on arXiv:2606.23782Subjects: gr-qcCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
In this comment we discuss some properties of the novel spacetime, recently found in [L. Ma, H. Lü, arXiv:2606.23782]. In particular, we draw attention to the background of this solution that the authors claim to be a new spacetime. We show that this is not the case because this background belongs to the special class of electrovacuum Kundt spacetimes of type D with either electric or MAGNETic charge. We show this by first analyzing the algebraic properties of this spacetime, and then by finding the explicit coordinate transformations. We hope that this analysis of the background allows for a better understanding of the structure of the general class of this type, namely as the Kerr-like BLACK HOLEs in the background generated by an accelerating electric or MAGNETic charge.
[abstract 70 / 70] (score: 2) - Title: Primordial Black Holes in a Radiation-Dominated UniverseAuthors: Thomas W. Baumgarte, Katy Clough, Mary Gerhardinger, John T. Giblin, Amanda Miller,Comments: 16 pages, 6 figuresSubjects: astro-ph.CO gr-qcCreated: 2026-06-29; Updated: 2026-06-30; Datestamp: 2026-06-30
Primordial fluctuations frozen out during inflation re-enter the cosmological horizon and can collapse, leading to the formation of primordial BLACK HOLEs. We perform simulations of the direct collapse of over-dense regions re-entering the horizon during a radiation-dominated epoch, using full 3+1 general RELATIVISTIC simulations with the BSSN formalism. Building on previous studies, we impose periodic boundary conditions and allow the matter content of the Universe to self-consistently drive its dynamics. We analyze the evolution of over-densities in both the collapse and dispersal regimes and find a threshold, $0.77<δ_c<0.83$, above which over-densities collapse and form primordial BLACK HOLEs. Our findings are consistent with previous analytic predictions as well as numerical studies that use different formalisms and computational approaches, and hence provide independent validation of those results.
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