Current date: 2026-03-26
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Datestamp limit: 2026-03-26 (0 days ago)
Created/updated limit: 2026-03-19 (7 days ago)
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Suggested sets: physics, physics:astro-ph, physics:gr-qc, physics:physics
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Scoring abstracts
Number of records retrieved: 694
Keyword score statistics
score 13 -- 1 abstracts
score 9 -- 2 abstracts
score 8 -- 1 abstracts
score 5 -- 4 abstracts
score 4 -- 2 abstracts
score 3 -- 7 abstracts
score 2 -- 18 abstracts
in total -- 35 abstracts
Articles that appeared on 2026-03-26
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[abstract 1 / 35] Wow! (score: 13)
- Title: VHE gamma-ray intranight variability from BL Lacertae during the extreme flaring state of 2022Authors: K. Abe, S. Abe, A. Abhishek, F. Acero, A. Aguasca-Cabot, I. Agudo, C. Alispach, D. Ambrosino, F. Ambrosino, L. A. Antonelli, C. Aramo, A. Arbet-Engels, C. Arcaro, T. T. H. Arnesen, P. Aubert, A. Baktash, M. Balbo, A. Bamba, A. Baquero Larriva, U. Barres de Almeida, J. A. Barrio, L. Barrios Jiménez, I. Batkovic, J. Baxter, J. Becerra González, J. Bernete, A. Berti, E. Bissaldi, O. Blanch, G. Bonnoli, P. Bordas, A. Briscioli, G. Brunelli, J. Buces, A. Bulgarelli, I. Burelli, L. Burmistrov, M. Cardillo, S. Caroff, A. Carosi, R. Carraro, F. Cassol, D. Cerasole, A. Cerviño Cortínez, Y. Chai, G. Chon, L. Chytka, G. M. Cicciari, J. L. Contreras, J. Cortina, H. Costantini, M. Croisonnier, M. Dalchenko, G. D'Amico, P. Da Vela, F. Dazzi, A. De Angelis, M. de Bony de Lavergne, R. Del Burgo, C. Delgado, J. Delgado Mengual, D. della Volpe, B. De Lotto, L. Del Peral, R. de Menezes, G. De Palma, V. de Souza, C. Díaz, L. Di Bella, A. Di Piano, F. Di Pierro, R. Di Tria, L. Di Venere, D. Dominis Prester, A. Donini, D. Dorner, L. Eisenberger, D. Elsässer, G. Emery, L. Feligioni, F. Ferrarotto, A. Fiasson, L. Foffano, Y. Fukazawa, S. Gallozzi, R. Garcia López, S. Garcia Soto, C. Gasbarra, D. Gasparrini, J. Giesbrecht Paiva, N. Giglietto, F. Giordano, N. Godinovic, T. Gradetzke, R. Grau, J. Green, G. Grolleron, S. Gunji, P. Günther, J. Hackfeld, D. Hadasch, M. Hashizume, T. Hassan, K. Hayashi, L. Heckmann, M. Heller, J. Herrera Llorente, N. Hiroshima, D. Hoffmann, D. Horns, J. Houles, D. Hrupec, R. Imazawa, T. Inada, S. Inoue, K. Ioka, M. Iori, T. Itokawa, A. Iuliano, J. Jahanvi, I. Jimenez Martinez, J. Jimenez Quiles, I. Jorge Rodrigo, J. Jurysek, M. Kagaya, V. Karas, H. Katagiri, D. Kerszberg, T. Kiyomoto, Y. Kobayashi, K. Kohri, P. Kornecki, H. Kubo, J. Kushida, B. Lacave, M. Lainez, A. Lamastra, L. Lemoigne, M. Linhoff, S. Lombardi, F. Longo, R. López-Coto, A. López-Oramas, S. Loporchio, J. Lozano Bahilo, F. Lucarelli, H. Luciani, P. L. Luque-Escamilla, M. Makariev, M. Mallamaci, D. Mandat, K. Mannheim, F. Marini, M. Mariotti, P. Marquez, G. Marsella, J. Martí, O. Martinez, G. Martínez, M. Martínez, M. Massa, D. Mazin, J. Méndez-Gallego, S. Menon, E. Mestre Guillen, D. Miceli, T. Miener, J. M. Miranda, M. Molero Gonzalez, E. Molina, T. Montaruli, A. Moralejo, A. Morselli, V. Moya, A. L. Müller, H. Muraishi, S. Nagataki, T. Nakamori, A. Neronov, D. Nieto Castaño, M. Nievas Rosillo, L. Nikolic, K. Noda, V. Novotny, S. Nozaki, M. Ohishi, Y. Ohtani, A. Okumura, R. Orito, L. Orsini, J. Otero-Santos, P. Ottanelli, M. Palatiello, G. Panebianco, D. Paneque, R. Paoletti, J. M. Paredes, M. Pech, M. Pecimotika, M. Peresano, F. Perrotta, F. Pfeifle, M. Pihet, G. Pirola, C. Plard, F. Podobnik, M. Polo, C. Pozo-Gonzaléz, E. Prandini, S. Rainò, R. Rando, W. Rhode, M. Ribó, G. Rodriguez Fernandez, M. D. Rodríguez Frías, A. Roy, A. Ruina, E. Ruiz-Velasco, T. Saito, S. Sakurai, D. A. Sanchez, H. Sano, E. Santos Moura, T. Šarić, Y. Sato, F. G. Saturni, V. Savchenko, F. Schiavone, F. Schussler, T. Schweizer, M. Seglar Arroyo, G. Silvestri, A. Simongini, J. Sitarek, V. Sliusar, I. Sofia, J. Strišković, M. Strzys, Y. Suda, A. Sunny, H. Tajima, M. Takahashi, R. Takeishi, S. J. Tanaka, D. Tateishi, T. Tavernier, P. Temnikov, Y. Terada, K. Terauchi, T. Terzic, M. Teshima, M. Tluczykont, T. Tomura, D. F. Torres, F. Tramonti, P. Travnicek, G. Tripodo, A. Tutone, M. Vacula, M. Vázquez Acosta, G. Verna, I. Viale, A. Viana, A. Vigliano, C. F. Vigorito, E. Visentin, V. Vitale, G. Voutsinas, I. Vovk, T. Vuillaume, R. Walter, T. Yamamoto, R. Yamazaki, Y. Yao, T. Yoshida, T. Yoshikoshi, W. Zhang, N. Zywucka, the CTAO-LST collaboration, F. Aceituno, J. A. Acosta-Pulido, V. Casanova, J. Escudero Pedrosa, V. Fallah Ramazani, J. Jormanainen, S. Jorstad, G. Keating, P. M. Kouch, M. Gurwell, A. Lähteenmäki, E. Lindfors, A. Marscher, D. Morcuende, I. Myserlis, K. Nilsson, C. A. Ortega Hunter, R. Rao, A. Sota, M. Tornikoski, H. Zhang,Comments: Accepted for publication in A&A. 13 pages + 8 pages of AppendixSubjects: astro-ph.HE astro-ph.GACreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
BL Lacertae (BL Lac), the archetype BLAZAR of its subclass and one of the most studied BLAZARs in the last decades, has gone through a series of major multi-wavelength outbursts since 2020, resulting in its highest recorded $γ$-ray flare up to date between September and November 2022 together with those from August 2021 and October 2024. We characterise the $γ$-ray and multi-wavelength emission and spectral energy distribution (SED) of BL Lac, as well as their evolution during the major and extended $γ$-ray and multi-wavelength flare occurring between September and November 2022. We evaluate the variability of the flare, with focus on the nights of October 20 and November 13, when clear intranight very-high-energy (VHE, $E>100$ GeV) $γ$-ray variability is observed. We model the $γ$-ray and broadband SEDs during periods of stable emission identified with a Bayesian block analysis, interpreting their evolution of the flare from the variability of the RELATIVISTIC particles and physical parameters of the JET. The VHE emission shows an average flux of 0.23 Crab Units (C.U.) above 200 GeV during this flare and a variability amplitude of more than a factor 10. Intranight doubling-flux variations as fast as $\sim$8 minutes are observed during the nights of October 20 and November 13, when maximum fluxes of 4.4 C.U. above 100 GeV and 2.8 C.U. above 200 GeV are reached. The spectral analysis reveals a transition of the X-ray emission from the high- to the low-energy SED peak, and a shift of the $γ$-ray peak towards higher energies. The broadband emission was interpreted within a leptonic two-zone model in which intranight variability is explained as MAGNETic RECONNECTion in a compact region closely oriented with the line of sight while weekly-scale variations can be explained as variations of the electron distributions and the injection of accelerated particles.
[abstract 2 / 35] Wow! (score: 9) - Title: Jet-environment interaction after delayed collapse in binary neutron star mergersAuthors: Jay V. Kalinani, Riccardo Ciolfi, Manuela Campanelli, Bruno Giacomazzo, Andrea Pavan, Allen Wen, Yosef Zlochower,Comments: 11 pages, 11 figures; matches published version on ApJLSubjects: astro-ph.HE astro-ph.SR gr-qcCreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
We present general RELATIVISTIC MAGNETohydrodynamic simulations of binary neutron star (BNS) mergers, where the collapse of the metastable massive neutron star (MNS) remnant leads to the production of an incipient JET having terminal Lorentz factor and Poynting-flux luminosity compatible with a short GAMMA-RAY BURST (GRB). We consider different MNS lifetimes of about 25 and 50 ms, long enough for massive polar outflows to emerge before BLACK HOLE (BH) formation. The interaction of the following BH-driven JET with such polar outflows, responsible for shock heating and possible electroMAGNETic signatures, is self-consistently captured for the first time. Exploiting an unprecedentedly low numerical density floor scaling as r^-6, we explore the JET propagation up to distances of ~10^4 km. Comparing the outcome of different MNS lifetimes, we find that the latter, by strongly affecting the propagation environment, plays a major role in determining the final properties of the escaping JET. Finally, we consider a non-collapsing case, where the MNS-driven outflow is found to exhibit a much higher density and lower velocity compared to the BH-driven JET.
[abstract 3 / 35] Wow! (score: 9) - Title: Simultaneous Multi-band Optical Follow-up Observations of a Gamma-Ray Flare in BL LacertaeAuthors: X. Chang, D. R. Xiong, Chenxu Liu, J. R. Xu, G. Bhatta, T. F. Yi, J. Zhang, Y. Pan, X. Z. Zou, X. L. Chen, Y. P. Yang, J. H. Zhang, X. K. Liu, Y. Fang, G. W. Du, T. Wang, X. F. Zhu, Y. L. Gong, Z. X. Wang, X. W. Liu,Comments:Subjects: astro-ph.HE astro-ph.GACreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
On $2024$ October $5$, BL Lacertae ($2200+420$) experienced one of its brightest gamma-ray flares. We conducted simultaneous follow-up observations in the $u$, $v$, $g$, $r$, $i$, and $z$ bands from $2024$ October $17$ to November $21$ using the Mephisto telescope and its two $50$ cm twin auxiliary photometric telescopes of Yunnan University. Intraday variability (IDV) was detected in the $g$, $r$, $i$, and $z$ bands. The IDV duty cycle increased with observing frequency across these bands. The shortest variability time-scale, derived from auto-correlation analysis, constrains the upper limit of the BLACK HOLE mass to be $M_{\bullet} \lesssim 10^{8.29} M_{\odot}$ assuming a Kerr BLACK HOLE, and $M_{\bullet} \lesssim 10^{8.77} M_{\odot}$ assuming a Schwarzschild BLACK HOLE. The emission region responsible for the observed variability has a size of $R \le 3.51 \times 10^{14}$ cm and is located at a distance of $R_H \le 2.83 \times 10^{15}$ cm from the central supermassive BLACK HOLE. This distance is approximately three orders of magnitude smaller than the typical radius of the broad-line region, indicating that the emission region lies well within it. A general bluer-when-brighter (BWB) trend was detected on intraday time-scales, suggesting that shock-accelerated RELATIVISTIC electrons enhance the high-energy particle population, leading to spectral hardening. A potential quasi-periodic oscillation (QPO) with a period of $\sim 100.77$ minutes was detected with $>99.99$ per cent confidence, consistent with predictions from the MAGNETic RECONNECTion model. These observed optical intraday variabilities and colour variations of BL Lacertae can be well explained by the turbulent JET model.
[abstract 4 / 35] Wow! (score: 8) - Title: The shortest detected intra-day variability of ACTIVE GALACTIC NUCLEi in TESS surveyAuthors: Heechan Yuk, Xinyu Dai, Natalie Kovacevic,Comments: 10 pages, 8 figures, accepted for publication in A&ASubjects: astro-ph.GACreated: 2026-03-24; Updated: 2026-03-26; Datestamp: 2026-03-26
AGNs are known to be variable in almost all wavelengths and timescales. The shortest variability timescale of AGNs can be used to probe the smallest scale structures within AGNs. We aim to measure the shortest detected variability timescale, $t_{min,ul}$, of type 1 radio-quiet Seyfert galaxies and analyse their characteristics. We extracted TESS light curves of 47 Seyfert 1 galaxies. We measured the PSDs of the sample, modelled by a power law model plus a constant noise, and constrained the shortest detected AGN variability timescale as the power law component exceeds the constant noise and systematic uncertainties indicated by the upper limits of non-variable quiescent galaxies' PSDs. We measured the upper limits of the shortest variability timescale to be $\log(t_{min,ul}/hrs)=0.85\pm0.55$. We compared these upper limits to a range of theoretical AGN variability timescales, and the natural interpretation of our measured $t_{min,ul}$ is the light crossing scale from a coherently varying region, where the measured $t_{min,ul}$ corresponds to the range from a few to thousands of gravitational radii. A significant fraction of these light crossing scales is smaller than the accretion disk emission sizes measured by QUASAR microlensing, reverberation mapping, or theoretical accretion disk models. Since we only measure the upper limits, the true physical shortest variability timescales are even shorter. We measure the power law index to be $2.0\pm0.2$, and find weak anticorrelations with the BLACK HOLE mass and luminosity. Our analysis suggests that the shortest optical variability is driven by a compact region smaller than the accretion disk size, potentially by X-ray reprocessing. Alternatively, this shortest timescale variability suggests that the accretion disk can be inhomogeneous potentially caused by turbulence from MAGNETorotational instability or MAGNETic RECONNECTions. (abridged)
[abstract 5 / 35] Yes (score: 5) - Title: Do plasmoids induce fast MAGNETic RECONNECTion in well-resolved current sheets in 2D MHD simulations?Authors: G. H. Vicentin, G. Kowal, E. M. de Gouveia Dal Pino, A. Lazarian,Comments: Accepted for publication in ApJ. 25 pages, 17 figures, 1 tableSubjects: physics.plasm-ph astro-ph.HE hep-thCreated: 2026-03-24; Updated: 2026-03-26; Datestamp: 2026-03-26
We investigate the development of tearing-mode instability using the highest-resolution two-dimensional MAGNETohydrodynamic simulations of RECONNECTing current sheets performed on a uniform grid, for Lundquist numbers of $10^3 \le S \le 5 \times 10^5$ , reaching up to $65,536^2$ grid cells. We demonstrate a Sweet--Parker scaling of the RECONNECTion rate $V_{\text{rec}} \sim S^{-1/2}$ up to Lundquist numbers $S \sim 10^4$. For larger values of Lundquist number, between $2\times 10^4\le S \le 2 \times 10^5$, plasmoid formation sets in, leading to a slight enhancement of the RECONNECTion rate, $V_{\text{rec}} \sim S^{-1/3}$, consistent with the prediction from linear tearing mode induced RECONNECTion, indicating that RECONNECTion remains resistivity-dependent and therefore slow. In this range of $S$-values, the plasmoids do not undergo a merger cascade, as they are rapidly advected out of the RECONNECTion layer. Only for $S > 2 \times 10^5$, we observe the nonlinear development of the tearing-mode instability, with plasmoid coalescence and a saturation of the RECONNECTion rate at $V_\text{rec} / V_A \sim 0.01$. At such high $S$, however, the corresponding Reynolds number is large, reaching $\text{Re} > 2000$ even on scales comparable to the current-sheet thickness. We therefore conclude that, in astrophysical systems, it is essential to account for the dominant influence of turbulence and three-dimensional effects in the RECONNECTion process.
[abstract 6 / 35] Yes (score: 5) - Title: A large population of over-massive BLACK HOLE QUASARs at z=0.3-0.8 revealed by eROSITAAuthors: Johannes Buchner, Isabelle Gauger, Qiaoya Wu, Hattie Starck, Catarina Aydar, Yue Shen, Vardha N. Bennert, Kirpal Nandra, Sophia G. H. Waddell, Andrea Merloni, Mara Salvato, Roberto J. Assef, Zsofi Igo, Franz E. Bauer, Dong-Woo Kim, Anton M. Koekemoer, Donald P. Schneider,Comments: Resubmitted to A&A after a positive referee reportSubjects: astro-ph.HECreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
In most galaxies, the central BLACK HOLE accounts for no more than a percent of the total mass in stars. Recently, however, extremely over-massive BLACK HOLEs with ratios of 10% have been reported in dwarf galaxies at z<1 and at cosmic dawn (z>5.5) by JWST. Both findings have been interpreted as signatures of the still mysterious origins of super-massive BLACK HOLEs, such that most of the BLACK HOLE mass was built at birth rather than through BLACK HOLE accretion. Here we show that among evolved galaxies over-massive BLACK HOLEs are also present, indicating that overmassive BHs are not a signature unique to BLACK HOLE formation channels. The first large-area sky survey of the eROSITA X-ray telescope on board SpectrRG identified 200 QUASARs by their luminous hard X-ray radiation. These signpost rapidly growing BLACK HOLEs. Complementary optical spectroscopy from the Sloan Digital Sky Survey and archival UV to IR photometric data combined with galaxy-QUASAR decomposition techniques allow us unbiased estimates of cosmological distances, BLACK HOLE masses and host galaxy stellar masses. We securely identify a sample of over-massive BLACK HOLEs with BH-to-host ratios of more than 5%, which may have undergone exponential accretion spurts lasting about a billion years. Our survey identified a high space density of at least 4/Gpc^3 of overmassive BLACK HOLEs near cosmic noon. This indicates an accretion channel disconnected from the stellar population that cause strong deviations from galaxy scaling relations. This channel is currently not part of galaxy evolution models. The identified channel, if applicable also for the first billion years of cosmic time, can explain JWST AGN without requiring them to signify imprints of BLACK HOLE seeding mechanism.
[abstract 7 / 35] Yes (score: 5) - Title: Unifying the X-ray coronae and ultra-fast outflows: a PBI-enhanced outflow-based corona model for the inner accretion discAuthors: Haichao Xu,Comments: accepted by MNRAS, 14 pages, 7 figuresSubjects: astro-ph.HECreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
The fact that luminous X-ray coronae and Ultra-Fast Outflows (UFOs) are both inferred to originate from the innermost regions of ACTIVE GALACTIC NUCLEi (AGNs) suggests a deep physical connection between them. However, standard MAGNETic buoyancy models struggle to transport sufficient energy through the radiation-pressure-dominated inner disc to sustain both the phenomena, creating a theoretical energy deficit. In this work, we propose an outflow-based model with energy transport enhanced by the Photon Bubble Instability (PBI) in the inner region. By coupling this enhanced energy supply with the MHD turbulence-driven mass-loading mechanism appropriate for weakly MAGNETized standard discs, we solve the dynamical and thermodynamic structure of the corona. We find that the model can successfully launch high speed winds matching observed UFO kinematics provided the mechanical acceleration efficiency is high ($f_{\rm acc}\gtrsim 0.5$). Furthermore, the model naturally reproduces the observed spectral evolution found in AGN coronae: as the accretion rate increases, the corona becomes optically thicker and cooler and produces a softer spectrum. Our results support an extended slab-like coronal geometry and suggest that UFOs and X-ray coronae in the inner discs are manifestations of the same MAGNETic activity.
[abstract 8 / 35] Yes (score: 5) - Title: Multi-mission Investigation of X-ray Superorbital Modulation in the Supergiant High Mass X-ray Binary 4U 1538-52Authors: H. I. Cohen, N. Islam, R. H. D. Corbet, A. Lange, K. Pottschmidt, E. Bozzo, P. Romano, R. Ballhausen, C. Malacaria, J. B. Coley,Comments: 21 pages, 9 figures, 2 tables, accepted for publication in ApJSubjects: astro-ph.HECreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
Superorbital modulations has been detected in the supergiant High-Mass X-ray binary 4U 1538-52 using long-term monitoring with the Neil Gehrels SWIFT Observatory Burst Alert Telescope (BAT). The source also exhibits a long-term pulse period evolution as seen with Rossi X-ray Timing Explorer (RXTE), INTEGRAL, and FERMI Gamma-Ray Burst Monitor (GBM) that appears uncorrelated with changes in its X-ray flux. To investigate the mechanisms causing these superorbital modulations and its possible dependence on pulse period changes, we analyzed long-term monitoring with SWIFT-BAT and Monitor of All Sky X-ray Image Gas Slit Camera (MAXI-GSC) to construct dynamic power spectra and superorbital intensity profiles. In addition, we used pointed X-ray observations from Nuclear Spectroscopic Telescope Array (NUSTAR) and Neutron Star Interior Composition Explorer mission (NICER) to investigate the pulsation and spectral properties across different superorbital and orbital phase intervals. We find the presence of superorbital modulations in the MAXI-GSC 2-20 keV lightcurves, consistent with the periodicity observed with the SWIFT-BAT lightcurves. However, no significant changes are detected in the pulse profiles or spectral parameters across different superorbital, orbital, or pulse-change intervals. This lack of spectral or timing variations with orbital and superorbital phases suggests that the mechanisms driving the observed superorbital modulation and pulse period changes are likely associated with large-scale stellar wind structures, such as Co-Rotating Interaction regions, within the stellar wind of the supergiant companion.
[abstract 9 / 35] Yes (score: 4) - Title: The annular gap model under a rotating dipole field approximation: simulating gamma-ray light curveAuthors: Jie Tian, Xin Xu, Qijun Zhi, Jiguang Lu, Shijun Dang, Ke Yang, Xiao Wei, Guojun Qiao,Comments: 12 pages, 7 figures, 1 Tables, Accept by ApJSubjects: astro-ph.HECreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
A more realistic description of the MAGNETosphere is crucial for understanding the radiation emitted by pulsars. In this paper, we revisit the annular gap model by employing a rotating dipole field, which is more realistic than the static dipole field, as an approximation of the MAGNETic structure of the pulsar MAGNETosphere. Compared with the static dipole field approximation, the open field-line region, including both the core and annular gaps, is significantly enlarged, and the two regions become asymmetric with respect to the fiducial plane. We apply this model to three young gamma-ray pulsars with distinct light-curve morphologies, PSRs J0631$+$1036 (single peak), J1709$-$4429 (double peaks), and J1048$-$5832 (three peaks). Using viewing geometries constrained by radio POLARIZATION measurements, the annular gap model within the rotating dipole field successfully reproduces the main morphological features of their gamma-ray light curves above 0.1 GeV. Our model provides a framework for interpreting pulsar high-energy emission, which can be used to analyze the emission properties of high-energy pulsars.
[abstract 10 / 35] Yes (score: 4) - Title: Derivation of the injection spectrum of positrons and electrons from Geminga and MonogemAuthors: Qian Zhong,Comments: 16 pages, 3 figuresSubjects: astro-ph.HECreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
Extended $γ$-ray emission has been observed around several nearby pulsars and interpreted as inverse Compton radiation from RELATIVISTIC electrons and positrons diffusing in the surrounding interstellar medium. In this work, we present a unified analysis of the TeV halos associated with the Geminga and Monogem pulsars, combining GeV--TeV $γ$-ray observations within a common physical framework. Assuming continuous injection of $e^\pm$ pairs from pulsar wind nebulae, we model the resulting $γ$-ray emission by accounting for particle diffusion and radiative energy losses. We find that the observed spectra of both Geminga and Monogem are well reproduced by the model, provided that particle transport in the vicinity of the pulsars is significantly suppressed with respect to the average Galactic diffusion. The injection spectra require cutoff energies of several tens of TeV, consistent with efficient acceleration in pulsar wind nebulae. Using the best-fit models inferred from the $γ$-ray data, we also evaluate the contribution of Geminga and Monogem to the local cosmic-ray positron flux measured by AMS-02. We find that the suppressed diffusion around the sources strongly limits the positron flux reaching the Earth, resulting in a subdominant contribution over the entire energy range probed by the experiment excect for the highest energy at around 1 TeV. Our results support an interpretation in which TeV halos trace regions of inhibited particle diffusion around pulsars, without implying a significant impact on the local cosmic-ray positron spectrum. This combined analysis highlights the importance of extended $γ$-ray observations for constraining particle transport in the vicinity of Galactic cosmic-ray sources.
[abstract 11 / 35] (score: 3) - Title: Investigating MAXI J1752-457 with NUSTAR in the aftermath of a superburstAuthors: Sean N. Pike, Hitoshi Negoro, Douglas Buisson, Benjamin Coughenour, Julian Gerber, Aarran W. Shaw, Mutsumi Sugizaki, John A. Tomsick,Comments: 12 pages, 5 figures, 3 tables; accepted for publication in ApJSubjects: astro-ph.HECreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
We present two NUSTAR observations of the X-ray transient, MAXI J1752-457, following a superburst which was observed by MAXI/GSC in November, 2024. NUSTAR follow-up confirmed that MAXI J1752-457 is coincident with the previously observed Einstein Probe source, EP240809a. We performed a spectral analysis of the source during both NUSTAR observations, and we find that the hard X-ray spectra are consistent with the inclusion of a spherical blackbody component and a steep, non-thermal, power law component. At about 79 hours after the onset of the superburst, we find a blackbody temperature of $kT_\mathrm{bb}=0.60\pm0.1$ keV and $R_\mathrm{bb}/D_{8}=6.0^{+0.4}_{-0.3}$ km (not including corrections for scattering in the neutron star atmosphere), where $D_{8}$ is the source distance, which is not yet known, in units of 8 kpc. We found that the blackbody temperature did not change significantly in the one day interval between successive NUSTAR observations, and we performed an energy-resolved timing analysis which showed that the source variability was dominated by red noise in the power law component, suggesting coupling with an accretion disk. We infer that the source had entered an accretion-powered flux state. Furthermore, we measure a photon index of $Γ\approx4$, much steeper than those typically observed during accretion onto neutron stars at similar luminosities. This is suggestive of ongoing evolution of the electron energy distribution responsible for the power law component several days after the superburst, but the lack of hard X-ray observations prior to and throughout the superburst make it difficult to present a conclusive physical interpretation of this result.
[abstract 12 / 35] (score: 3) - Title: Magnetic flux systems involved in the May 2024 solar energetic events from AR 13664 inferred through coronal dimmingsAuthors: Amaia Razquin, Karin Dissauer, Astrid M. Veronig, Graham Barnes,Comments:Subjects: astro-ph.SRCreated: 2026-03-24; Updated: 2026-03-26; Datestamp: 2026-03-26
Coronal dimmings are transient depletions of coronal plasma observed in extreme ultraviolet and soft X-rays, interpreted as low-corona signatures of coronal mass ejections (CMEs). Their evolution is closely linked to CME dynamics, flare RECONNECTion, and large-scale coronal MAGNETic restructuring. In May 2024, active region (AR) 13664 produced 66 > M-class flares and multiple fast CMEs that caused the strongest geoMAGNETic storm since 2003. We analysed 16 on-disc dimmings observed in SDO/AIA 211Ådata between May 1-14, 2024. We extracted dimmings using logarithmic base-ratio thresholding, and derived MAGNETic properties from SDO/HMI line-of-sight MAGNETograms. We identified flare ribbons in AIA 1600Ådata via adaptive thresholding, and computed RECONNECTion fluxes from radial MAGNETic field maps. We examined the MAGNETic flux systems involved in the eruptions using PFSS and NLFF extrapolations. We found correlations between dimming and flare ribbon properties stronger than previously reported. The dimming morphology evolved systematically, with southward expansion before May 9 and northward afterward, coinciding with a shift in flare ribbon locations between two mayor east-west polarity inversion lines (PILs). These changes imply the presence of two distinct MAGNETic domains. The PFSS extrapolations showed that southward (northward) dimmings are mainly strapping flux dimmings with MAGNETic field lines vaulting above the southern (northern) PIL. The final extent of the dimmings was then given by the exterior flux involved in the eruption via stretching and RECONNECTion. One event revealed an extended quiet-Sun dimming likely triggered by EUV wave-induced field opening.
[abstract 13 / 35] (score: 3) - Title: Radiation-ionization hydrodynamic simulations of AGN line-driven winds lead to transient shielding and BAL/UFO signaturesAuthors: Nicolas Scepi, Christian Knigge, Amin Mosallanezhad, Knox S. Long, James H. Matthews, Stuart A. Sim, Austen Wallis,Comments: Accepted for publication in MNRAS, 17 pages, 12 figures and 7 videos as supplementary material on MNRAS websiteSubjects: astro-ph.HE astro-ph.GA astro-ph.SRCreated: 2026-03-24; Updated: 2026-03-26; Datestamp: 2026-03-26
Disc winds from ACTIVE GALACTIC NUCLEi (AGN) can be launched by radiation pressure acting on spectral lines. However, launching a line-driven wind in the X-ray rich environment of AGN is challenging, as the wind easily gets over-ionized. Previous simulations suggested that X-ray self-shielding could enable line driving, though it remained unclear whether this relied on simplified treatments of radiation and ionization. Here, we revisit the X-ray shielding scenario using the first multi-frequency, multi-directional Monte-Carlo radiative photo-ionization hydrodynamical simulations of AGN line-driven winds. We find that sustaining a steady wind with mass-loss rates of $\approx20\%$ of the accretion rate requires an unrealistically weak X-ray flux ($α_{\rm OX}<-3$). For stronger X-ray emission ($-3<α_{\rm OX}<-1$), self-shielding is only transient, leading to episodic ejections with mass-loss rates approaching the accretion rate. Our steady winds naturally produce FeLoBAL, HiBAL, and broad emission line signatures, depending on the disc spectral energy distribution and the observer's inclination. At moderate X-ray luminosities ($α_{\rm OX}\sim-3$), transient winds can generate short-lived BAL and ultra-fast outflow (UFO) features. At the highest X-ray luminosities ($α_{\rm OX}\sim-1$), the winds are too ionized to form BALs, but still produce UFOs. These results imply that additional physics is required to explain BAL outflows at realistic X-ray levels and to drive winds strong enough for AGN feedback. Nonetheless, our simulations provide a new framework for interpreting the observed diversity of AGN outflow signatures with fully coupled radiation and dynamics.
[abstract 14 / 35] (score: 3) - Title: MICONIC: JWST/MIRI-MRS reveals heavily reprocessed PAH emission in the circum-nuclear disc of Centaurus AAuthors: L. Pantoni, M. Baes, L. Decin, P. Guillard, A. Alonso Herrero, L. Evangelista, L. Hermosa Muñoz, I. García-Bernete, F. Donnan, V. Buiten, S. Garcia-Burillo, G. Wright, L. Colina, T. Böker, G. Östlin, D. Dicken, A. Labiano, D. Rouan, P. van der Werf, A. Eckart, M. García-Marín, M. Güdel, Th. Henning, P. -O. Lagage, F. Walter, M. J. Ward,Comments: Accepted for publication in A&A. 14 pages, 10 figures; plus 5 pages and 4 figures in the appendicesSubjects: astro-ph.GACreated: 2026-03-24; Updated: 2026-03-26; Datestamp: 2026-03-26
Polycyclic aromatic hydrocarbons (PAHs) are key dust components in galaxies and play a fundamental role in the physics of the interstellar medium (ISM), yet their response to AGN feedback remains debated. We present a spatially resolved analysis of PAHs in the central $7^{\prime\prime}\times12^{\prime\prime}$ ($\sim100\times200$ pc$^2$) of Centaurus A. We use JWST/MIRI-MRS observations at 5-28 $μ$m from the MIRI European consortium GTO program MICONIC, with angular resolution of $0.35^{\prime\prime}-1^{\prime\prime}$ (about 6-17 pc). We derive PAH moment-0 maps via local continuum subtraction and extract one-dimensional spectra from five regions of interest, including the nucleus, the circumnuclear disc, and a PAH-deficient region. The spectra are decomposed into continuum, emission lines, and PAHs to measure feature intensities and equivalent widths (EWs). PAH emission is primarily distributed in a ring-like structure with localized enhancements at $\sim40$ pc from the nucleus. A distinct PAH-deficient region is observed to the north-west, roughly perpendicular to the JET axis, and coincident with enhanced ionized-gas velocity dispersion and inflowing molecular streamers. The 11.3/7.7 $μ$m and 6.2/7.7 $μ$m ratios exceed model predictions for pericondensed PAHs, indicating processed populations with more open structures. The 11.3/12.7 $μ$m ratio suggests a dominance of solo hydrogen sites and partial dehydrogenation, particularly in the PAH-deficient region, where shocks likely drive erosion. The largest EWs are found in the ring, while reduced values in the deficient region point to partial destruction; in the nucleus, low EWs are mainly due to continuum dilution.
[abstract 15 / 35] (score: 3) - Title: The Role of Reconnection at Magnetic Separators in Complex Solar Flare RibbonsAuthors: Graham Barnes, Karin Dissauer,Comments: 15 pages, 9 figures, Astrophysical Journal in pressSubjects: astro-ph.SRCreated: 2026-03-24; Updated: 2026-03-26; Datestamp: 2026-03-26
Solar flare ribbons, manifesting as transient brightenings in the chromosphere, are believed to trace out the footpoints of MAGNETic field lines that are RECONNECTing higher in the solar atmosphere. These field lines lie in a separatrix or quasi-separatrix layer that separates domains of different MAGNETic connectivity and hence forms a natural location for RECONNECTion. Solar flares are typically characterized as being circular ribbon flares, two-ribbon flares, or complex ribbon flares based on the number and shape of the ribbons. There are relatively well-developed models to explain the first two types of flares based on the location of the RECONNECTion powering the flare. The case of complex ribbons is less well understood, but is often posited to be a result of RECONNECTion at multiple locations. We demonstrate here that RECONNECTion at a MAGNETic separator connecting two coronal null points can naturally explain the complex ribbons observed for two events, an M2.9 class flare from NOAA AR 11112 (SOL2010-10-16T19:12), and an X2.2 class flare from NOAA AR 11158 (SOL2011-02-15T01:56).
[abstract 16 / 35] (score: 3) - Title: IXPE view of the Crab pulsar following the 17 July and 6 August 2025 glitchesAuthors: Paolo Soffitta, Niccolò Bucciantini, Josephine Wong, Denis Gonzalez Caniulef, Matteo Bachetti, Riccardo Ferrazzoli, Fei Xie, Enrico Costa, Maura Pilia, Nicolò Cibrario, Jack T. Dinsmore, Niccolò Di Lalla, Philip Kaaret, Kuan Liu, Tsunefumi Mizuno, Michela Negro, C. -Y. Ng, Nicola Omodei, Simone Pagliarella, Stefano Silvestri, Yi-Jung Yang, Martin C. Weisskopf,Comments: 15 pages, 5 tables, 7 figures accepted for publication in Astrophysical Journal on 24 March 2026Subjects: astro-ph.HE astro-ph.IMCreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
The Crab pulsar experienced two relatively small glitches separated by only 20 days in September and October 2025. IXPE observed the source twice, with delay times since the glitch epoch ranging between 35 and 75 days, depending on the observation. We carried out a multi-method analysis to investigate whether there is evidence for significant changes in the POLARIZATION properties of the pulsar, underlying possible variations in the pulsar MAGNETosphere itself following the glitches. Specifically, we performed: (1) phase-averaged polarimetry of the Crab pulsar before and after the glitches, following an approach similar to that adopted in 2019 by PolarLight, a non-imaging CubeSat-class photoelectric polarimeter which observed a change in the X-ray POLARIZATION within 100 days after a stronger glitch in July 2019; (2) a comparison, before and after the glitch, of phase-resolved X-ray polarimetry with IXPE, not possible with PolarLight. Furthermore, we investigated, by means of phase-resolved optical (OPTIMA) polarimetry, whether a significant change in the X-to-optical lag was present in the data before and after the glitch. We find no evidence of a change in the POLARIZATION for the pulsar emission before and after the glitch, We use the upper limits obtained to estimate the maximum change in MAGNETic obliquity allowed by the data, using the standard rotating vector model and assuming that the glitch is due to a neutron-star quake. We constrain this maximum change to be no greater than $\pm4^{o}$ at the 95\% confidence level.
[abstract 17 / 35] (score: 3) - Title: RRAT J1541+4703: A Rotating Radio Transient Exhibiting Normal Pulsar StatesAuthors: Xin Xu, Qijun Zhi, Jie Tian, Jiguang Lu, Peng Jiang, Shijun Dang, Renxin Xu, Juntao Bai, Ke Yang,Comments: 15 pages, 11 figures, 2 Tables, Accept by ApJSubjects: astro-ph.HECreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
Rotating Radio Transients (RRATs) are a class of pulsar-like objects characterized by intermittent radio emissions. Among them, RRATs that exhibit both RRAT and normal pulsar (NP) states may represent a key evolutionary stage from nulling pulsars to RRATs. We performed a detailed analysis of RRAT J1574+4703 using the Five-hundred-meter Aperture Spherical Radio Telescope (FAST) at a frequency of 1250 MHz. Our findings indicate that this RRAT spends approximately 98% of its time in the RRAT state, with the remainder spent in an NP state exhibiting nulling behavior. Additionally, we observed distinct integral pulse profiles and POLARIZATION properties between the two states, suggesting that they originate from different emission heights and MAGNETospheric structures. Furthermore, it was observed that the NP states of this RRAT exhibit mode switching, with ~44% of the time spent in the normal mode and ~39% in the abnormal mode. Notably, abnormal modes are predominantly detected at the onset and termination of the NP states. This discrepancy between the modes indicates potential instability in the MAGNETospheric processes that govern the NP states.
[abstract 18 / 35] (score: 2) - Title: The Duality of Whittaker Potential Theory: Fundamental Representations of ElectroMAGNETism and Gravity, and Their OrthogonalityAuthors: Mark Titleman,Comments:Subjects: physics.hist-ph physics.class-phCreated: 2026-03-24; Updated: 2026-03-26; Datestamp: 2026-03-26
E. T. Whittaker produced two papers in 1903 and 1904 that, although sometimes considered mere mathematical statements (Barrett, 1993), held important implications for physical theory. The Whittaker 1903 paper united electrostatic and gravitational attraction as resulting from longitudinal waves - waves whose wavefronts propagate parallel to their direction. The Whittaker 1904 paper showed that electroMAGNETic waves resulted from the interference of two such longitudinal waves or scalar potential functions. Although unexplored, the implications of these papers are profound: gravitational lensing, gravitational waves, the Aharonov-Bohm effect, the existence of a hyperspace above or behind normal space, the elimination of gravitational and point charge singularities, MOND, and the expansion of the universe. This last implication can be related to the recent finding that BLACK HOLEs with posited vacuum energy interior solutions alongside cosmological boundaries have a cosmological coupling constant of k=3, meaning that BLACK HOLEs gain mass-proportional to a3 in a parameterization equation within a Robertson-Walker cosmology and are a cosmological accelerated expansion species (Farrah et al., 2023). This expansion and many features of General Relativity can be explained by the mass-proportionality and preferred direction of the longitudinal waves within the two underlying non-local Whittaker potentials (Titleman, 2022). Expansion of the universe is produced as longitudinal motion within the Whittaker potentials only when dynamic electroMAGNETism is separate from time-static gravity in intergalactic space.
[abstract 19 / 35] (score: 2) - Title: Symplectic particle-in-cell methods for hybrid plasma models with Boltzmann electrons and space-charge effectsAuthors: Yingzhe Li,Comments: 22 pages, 6 figuresSubjects: math.NA cs.NA physics.plasm-phCreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
We study the geometric particle-in-cell methods for an electrostatic hybrid plasma model. In this model, ions are described by the fully kinetic equations, electron density is determined by the Boltzmann relation, and space-charge effects are incorporated through the Poisson equation. By discretizing the action integral or the Poisson bracket of the hybrid model, we obtain a finite dimensional Hamiltonian system, for which the Hamiltonian splitting methods or the discrete gradient methods can be used to preserve the geometric structure or energy. The global neutrality condition is conserved under suitable boundary conditions. Moreover, the results are further developed for an electroMAGNETic hybrid model proposed in [Vu H X. J Comput Phys, 124(2):417-430]. Numerical experiments of finite grid instability, Landau damping, and resonantly excited nonlinear ion waves illustrate the behaviour of the proposed numerical methods.
[abstract 20 / 35] (score: 2) - Title: Refining Galactic primordial BLACK HOLE evaporation constraintsAuthors: Pedro De la Torre Luque, Jordan Koechler, Shyam Balaji,Comments: 13 pages, 9 figures, erratum version at the endSubjects: astro-ph.HE astro-ph.CO hep-phCreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
We revisit the role of primordial BLACK HOLEs (PBHs) as potential DARK MATTER (DM) candidates, particularly focusing on light asteroid-mass PBHs. These PBHs are expected to emit particles through Hawking evaporation that can generate COSMIC RAYs (CRs), eventually producing other secondary radiations through their propagation in the Milky Way, in addition to prompt emissions. Here, we perform a comprehensive analysis of CR signals resulting from PBH evaporation, incorporating the full CR transport to account for reacceleration and diffusion effects within the Milky Way. In particular, we revisit the $e^\pm$ flux produced by PBHs, using Voyager 1, and study for the first time the diffuse X-ray emission from the up-scattering of Galactic ambient photons due to PBH-produced $e^\pm$ via the inverse Compton effect using XMM-Newton data, as well as the morphological information of the diffuse 511 keV line measured by INTEGRAL/SPI. In doing so, we provide leading constraints on the fraction of DM that can be in form of PBHs in a conservative way, whilst also testing how different assumptions on spin and mass distributions affect our conclusions.
[abstract 21 / 35] (score: 2) - Title: Search for spatial coincidence between MAGNETars and IceCube detected neutrinosAuthors: Fathima Shifa M., Shantanu Desai,Comments: 8 pages, 2 figures. published in Phys. Dark. UnivSubjects: astro-ph.HECreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
We implement a search for spatial coincidence between high energy neutrinos detected by the IceCube neutrino detector (using the publicly available 10-year muon track data) and 37 MAGNETars, including six extragalactic sources. We use the unbinned maximum likelihood method for our analysis. We do not find any such spatial association between any of the known MAGNETars and IceCube-detected neutrinos. Therefore, we conclude that none of the known galactic or extragalactic MAGNETars contribute to the diffuse neutrino flux observed in IceCube. A stacked analysis also does not show a statistically significant excess.
[abstract 22 / 35] (score: 2) - Title: JWST observes the assembly of a massive galaxy at z~4Authors: Aayush Saxena, Roderik A. Overzier, Catarina Aydar, Jianwei Lyu, George H. Rieke, Victoria Reynaldi, Montserrat Villar-Martín, Krisztina Éva Gabányi, Kenneth J. Duncan, Sándor Frey, Andrew Humphrey, George Miley, Laura Pentericci, Krisztina Perger, Huub Röttgering, Philip Best, Sarah E. I. Bosman, Gyorgy Mező, Masafusa Onoue, Zsolt Paragi, Bram Venemans,Comments: 15 pages, 9 figures; Published in the Open Journal of Astrophysics; Based on JWST programs GO 1964 and GTO 1205Subjects: astro-ph.GACreated: 2026-03-23; Updated: 2026-03-26; Datestamp: 2026-03-26
We present JWST observations of the RADIO GALAXy TGSSJ1530+1049, spectroscopically confirmed at $z=4.0$. NIRCam images and NIRSpec/IFU spectroscopy (R=2700) show that TGSSJ1530+1049 is part of one of the densest-known structures of continuum and line-emitting objects found at these redshifts. NIRCam images show a number of distinct continuum objects and evidence of interactions traced by diffuse emission, and the NIRSpec IFU cube reveals further strong line emitting regions. We identify six continuum and four additional strong H$α$ emitting sources with weaker or no underlying continuum within the 3x3 arcsec IFU field. From spatial alignment with high-resolution radio data and emission line profiles, the radio AGN host galaxy is clearly identified. The bright H$α$ emission (but not the optical components) is distributed remarkably linearly along the radio axis, suggestive of a biconical illumination zone by a central obscured AGN. The emission line kinematics indicate JET-gas interactions on scales of a few kpc. However, due to large relative velocities and presence of underlying continuum, the alignment with the radio structure appears to be, at least partly, caused by a particular configuration of interacting galaxies. At least four objects within a 10x10 (projected) kpc$^2$ area which includes the radio source have high stellar masses ($\log(M_\star/M_\odot)>10.3$) and STAR FORMATION rates in the range $70-163\,M_\odot$ yr$^{-1}$. Using a stellar mass-based analysis, we predict a total DARK MATTER halo mass of $\approx10^{13} M_\odot$. Based on the physical separations and velocity differences between the galaxies, it is expected that these galaxies will merge to form a massive galaxy within a few Gyr. The system qualitatively resembles the forming brightest cluster galaxies in cosmological simulations that form early through a rapid succession of mergers.
[abstract 23 / 35] (score: 2) - Title: Waveforms and Fluxes of Generic Extreme-Mass-Ratio Inspirals with a Spinning SecondaryAuthors: Qiuxin Cui, Wen-Biao Han,Comments:Subjects: astro-ph.HE gr-qcCreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
Extreme mass-ratio inspirals (EMRIs), comprising a stellar-mass compact object (CO) orbiting a supermassive BLACK HOLE (BH), are key targets for future space-based gravitational-wave (GW) observatories. Incorporating the spin of the secondary body into waveform models not only enhances measurement precision but also offers insight into the spin distribution of stellar-mass objects. In this work, we construct the flux and waveform for an EMRI with a spinning secondary in a Kerr background under the linear-spin approximation. Using the radiative prescription (half-retarded minus half-advanced field), we derive orbit-averaged evolution equations for the fundamental constants of motion, including the energy, angular momentum, Carter-like constant, and the parallel spin component. This framework provides a tractable route to generating waveforms that incorporate the secondary spin, with the potential for further simplification in future work.
[abstract 24 / 35] (score: 2) - Title: Constraints on the $^{12}$C$(α, γ)^{16}$O and $^{16}$O+$^{16}$O Reaction Rates from Binary Black Holes Detected via Gravitational Wave SignalsAuthors: Wenyu Xin, Xiaokun Hou, Xianfei Zhang, Shaolan Bi, Gang Zhao,Comments:Subjects: astro-ph.SR astro-ph.HECreated: 2026-03-20; Updated: 2026-03-26; Datestamp: 2026-03-26
Gravitational-wave observations of binary BLACK HOLE (BH) mergers provide a novel avenue for testing massive-star evolution and the resulting BH mass spectrum. Recent population analyses under the hierarchical-merger hypothesis have offered evidence for the BH mass gap and inferred its lower edge to $\sim 44 - 68$ M$_\odot$. Motivated by these findings, we compute low-metallicity ($Z=10^{-5}$) helium star models with MESA and systematically explore the effect of uncertainties in the $^{12}$C$(α, γ)^{16}$O and $^{16}$O+$^{16}$O reaction rates on the final fate. Varying the $^{12}$C$(α, γ)^{16}$O reaction rate by $-3 σ$ to $+3σ$, we find that the predicted BH mass gap shifts from $\sim104 - 184$ M$_\odot$ to $\sim45 - 135$ M$_\odot$. In contrast, scaling the $^{16}$O+$^{16}$O reaction rate by global factors of 0.1, 1, and 10 has only a modest effect on the lower edge of the BH mass gap (less than 5 M$_\odot$), and shifts the upper edge by more than 10 M$_\odot$. Using the predictions of our models together with the literature estimates for the lower edge of the BH mass gap, we constrain the astrophysical S factor of $^{12}$C$(α, γ)^{16}$O reaction at 300 keV of $S_{300} \simeq$ 137.6 - 263.4 keV barn.
[abstract 25 / 35] (score: 2) - Title: Investigating the radio emission in the Perseus cluster with LOFAR sub-80 MHz LBAAuthors: C. Groeneveld, R. J. van Weeren, M. -L. Gendron-Marsolais, E. Osinga, A. Botteon, F. de Gasperin, M. Cianfaglione, G. di Gennaro, G. Brunetti, R. Cassano,Comments: Accepted for publication in A&A. 16 pages, 2 tables, 16 figuresSubjects: astro-ph.CO astro-ph.GACreated: 2026-03-24; Updated: 2026-03-26; Datestamp: 2026-03-26
The Perseus cluster is a nearby cool-core galaxy cluster that hosts an archetypal radio mini-halo. Recent Low Frequency Array (LOFAR) High Band Antenna (HBA) observations at 120 - 168 MHz have revealed the presence of a giant radio halo within the cluster with a size of 1.1 Mpc enveloping the mini-halo. By exploring the spectral properties of the radio emission at low frequencies, we can gain deeper insights into the nature of this emission and improve our understanding of its origin. Here we present LOFAR Low Band Antenna (LBA) images of the cluster between 30.0 - 57.7 MHz, with a resolution of 19.2'' x 15.0'' and a r.m.s. noise of 3.7 mJy/beam . In our images, we detect both the mini-halo and giant radio halo. We measured the spectral indices between 44 and 144 MHz of the mini-halo and giant radio halo to be -1.34 +- 0.10, and -1.01 +- 0.11, respectively. An alternative and more direct measurement of the spectrum of the giant radio halo results in a spectral index of -1.28 +- 0.15. The discrepancy between both values is caused by the poor ionospheric conditions. In addition, we study two X-ray 'ghost cavities' in the cluster. These cavities are thought to have been produced by an older outburst from the central AGN 3C 84. We measure a spectral index between 44 and 144 MHz for the radio plasma in these cavities of -1.86 +- 0.12 and -1.90 +- 0.12 for the northwest and southern ghost cavities, respectively. Furthermore, by including VLA 352 MHz data, we find that the spectrum steepens at higher frequencies. These results are consistent with the ghost cavities being filled with old and aged radio plasma. We also detect the tailed RADIO GALAXies NGC 1265 and IC 310. In our analysis, these sources show signs of spectral steepening along their tails.
[abstract 26 / 35] (score: 2) - Title: Reducing cosmological degeneracies by combining multiple classes of LISA gravitational-wave standard sirensAuthors: Danny Laghi, Nicola Tamanini, Alberto Sesana, Jonathan Gair, Enrico Barausse, Chiara Caprini, Walter Del Pozzo, Alberto Mangiagli, Sylvain Marsat,Comments: 7+2 pages, 3 figuresSubjects: astro-ph.CO gr-qcCreated: 2026-03-24; Updated: 2026-03-26; Datestamp: 2026-03-26
We present the first joint gravitational-wave cosmological inference with LISA extreme mass-ratio inspirals at $z\lesssim1$ (galaxy redshifts) and massive BLACK HOLE binaries at $z\gtrsim1$ (electroMAGNETic counterparts). Combining these standard sirens reduces cosmological degeneracies and yields competitive constraints on the Hubble constant $H_0$ and the dark-energy equation-of-state parameter $w_0$. This highlights LISA's potential for late-time cosmology across a broad redshift range with systematics distinct from electroMAGNETic distance indicators.
[abstract 27 / 35] (score: 2) - Title: $B$-JET fragmentation with $B^{\pm} \to J/ψK^{\pm}$ decays in $\sqrt{s} = 13$ TeV $pp$ collisions at LHCbAuthors: LHCb collaboration, R. Aaij, A. S. W. Abdelmotteleb, C. Abellan Beteta, F. Abudinén, T. Ackernley, A. A. Adefisoye, B. Adeva, M. Adinolfi, P. Adlarson, C. Agapopoulou, C. A. Aidala, Z. Ajaltouni, S. Akar, K. Akiba, P. Albicocco, J. Albrecht, R. Aleksiejunas, F. Alessio, P. Alvarez Cartelle, R. Amalric, S. Amato, J. L. Amey, Y. Amhis, L. An, L. Anderlini, M. Andersson, P. Andreola, M. Andreotti, S. Andres Estrada, A. Anelli, D. Ao, C. Arata, F. Archilli, Z. Areg, M. Argenton, S. Arguedas Cuendis, M. Arias, L. Arnone, A. Artamonov, M. Artuso, E. Aslanides, R. Ataíde Da Silva, M. Atzeni, B. Audurier, J. A. Authier, D. Bacher, I. Bachiller Perea, S. Bachmann, M. Bachmayer, J. J. Back, Z. B. Bai, P. Baladron Rodriguez, V. Balagura, A. Balboni, W. Baldini, Z. Baldwin, L. Balzani, H. Bao, J. Baptista de Souza Leite, C. Barbero Pretel, M. Barbetti, I. R. Barbosa, R. J. Barlow, M. Barnyakov, S. Barsuk, W. Barter, J. Bartz, S. Bashir, B. Batsukh, P. B. Battista, A. Bavarchee, A. Bay, A. Beck, M. Becker, F. Bedeschi, I. B. Bediaga, N. A. Behling, S. Belin, A. Bellavista, K. Belous, I. Belov, I. Belyaev, G. Benane, G. Bencivenni, E. Ben-Haim, A. Berezhnoy, R. Bernet, A. Bertolin, F. Betti, J. Bex, O. Bezshyyko, S. Bhattacharya, M. S. Bieker, N. V. Biesuz, A. Biolchini, M. Birch, F. C. R. Bishop, A. Bitadze, A. Bizzeti, T. Blake, F. Blanc, J. E. Blank, S. Blusk, V. Bocharnikov, J. A. Boelhauve, O. Boente Garcia, T. Boettcher, A. Bohare, A. Boldyrev, C. Bolognani, R. Bolzonella, R. B. Bonacci, N. Bondar, A. Bordelius, F. Borgato, S. Borghi, M. Borsato, J. T. Borsuk, E. Bottalico, S. A. Bouchiba, M. Bovill, T. J. V. Bowcock, A. Boyer, C. Bozzi, J. D. Brandenburg, A. Brea Rodriguez, N. Breer, J. Brodzicka, J. Brown, D. Brundu, E. Buchanan, M. Burgos Marcos, C. Burr, C. Buti, J. S. Butter, J. Buytaert, W. Byczynski, S. Cadeddu, H. Cai, Y. Cai, A. Caillet, R. Calabrese, L. Calefice, M. Calvi, M. Calvo Gomez, P. Camargo Magalhaes, J. I. Cambon Bouzas, P. Campana, A. C. Campos, A. F. Campoverde Quezada, Y. Cao, S. Capelli, M. Caporale, L. Capriotti, R. Caravaca-Mora, A. Carbone, L. Carcedo Salgado, R. Cardinale, A. Cardini, P. Carniti, L. Carus, A. Casais Vidal, R. Caspary, G. Casse, M. Cattaneo, G. Cavallero, V. Cavallini, S. Celani, I. Celestino, S. Cesare, A. J. Chadwick, I. Chahrour, H. Chang, M. Charles, Ph. Charpentier, E. Chatzianagnostou, R. Cheaib, M. Chefdeville, C. Chen, J. Chen, S. Chen, Z. Chen, A. Chen Hu, M. Cherif, A. Chernov, S. Chernyshenko, X. Chiotopoulos, G. Chizhik, V. Chobanova, M. Chrzaszcz, A. Chubykin, V. Chulikov, P. Ciambrone, X. Cid Vidal, G. Ciezarek, P. Cifra, P. E. L. Clarke, M. Clemencic, H. V. Cliff, J. Closier, C. Cocha Toapaxi, V. Coco, J. Cogan, E. Cogneras, L. Cojocariu, S. Collaviti, P. Collins, T. Colombo, M. Colonna, A. Comerma-Montells, L. Congedo, J. Connaughton, A. Contu, N. Cooke, G. Cordova, C. Coronel, I. Corredoira, A. Correia, G. Corti, J. Cottee Meldrum, B. Couturier, D. C. Craik, M. Cruz Torres, M. Cubero Campos, E. Curras Rivera, R. Currie, C. L. Da Silva, X. Dai, E. Dall'Occo, J. Dalseno, C. D'Ambrosio, J. Daniel, G. Darze, A. Davidson, J. E. Davies, O. De Aguiar Francisco, C. De Angelis, F. De Benedetti, J. de Boer, K. De Bruyn, S. De Capua, M. De Cian, U. De Freitas Carneiro Da Graca, E. De Lucia, J. M. De Miranda, L. De Paula, M. De Serio, P. De Simone, F. De Vellis, J. A. de Vries, F. Debernardis, D. Decamp, S. Dekkers, L. Del Buono, B. Delaney, J. Deng, V. Denysenko, O. Deschamps, F. Dettori, B. Dey, P. Di Nezza, I. Diachkov, S. Ding, Y. Ding, L. Dittmann, A. D. Docheva, A. Doheny, C. Dong, F. Dordei, A. C. dos Reis, A. D. Dowling, L. Dreyfus, W. Duan, P. Duda, L. Dufour, V. Duk, P. Durante, M. M. Duras, J. M. Durham, O. D. Durmus, A. Dziurda, A. Dzyuba, S. Easo, E. Eckstein, U. Egede, A. Egorychev, V. Egorychev, S. Eisenhardt, E. Ejopu, L. Eklund, M. Elashri, D. Elizondo Blanco, J. Ellbracht, S. Ely, A. Ene, J. Eschle, T. Evans, F. Fabiano, S. Faghih, L. N. Falcao, B. Fang, R. Fantechi, L. Fantini, M. Faria, K. Farmer, F. Fassin, D. Fazzini, L. Felkowski, C. Feng, M. Feng, A. Fernandez Casani, M. Fernandez Gomez, A. D. Fernez, F. Ferrari, F. Ferreira Rodrigues, M. Ferrillo, M. Ferro-Luzzi, S. Filippov, R. A. Fini, M. Fiorini, M. Firlej, K. L. Fischer, D. S. Fitzgerald, C. Fitzpatrick, T. Fiutowski, F. Fleuret, A. Fomin, M. Fontana, L. A. Foreman, R. Forty, D. Foulds-Holt, V. Franco Lima, M. Franco Sevilla, M. Frank, E. Franzoso, G. Frau, C. Frei, D. A. Friday, J. Fu, Q. Führing, T. Fulghesu, G. Galati, M. D. Galati, A. Gallas Torreira, D. Galli, S. Gambetta, M. Gandelman, P. Gandini, B. Ganie, H. Gao, R. Gao, T. Q. Gao, Y. Gao, Y. Gao, Y. Gao, L. M. Garcia Martin, P. Garcia Moreno, J. García Pardiñas, P. Gardner, L. Garrido, C. Gaspar, A. Gavrikov, L. L. Gerken, E. Gersabeck, M. Gersabeck, T. Gershon, S. Ghizzo, Z. Ghorbanimoghaddam, F. I. Giasemis, V. Gibson, H. K. Giemza, A. L. Gilman, M. Giovannetti, A. Gioventù, L. Girardey, M. A. Giza, F. C. Glaser, V. V. Gligorov, C. Göbel, L. Golinka-Bezshyyko, E. Golobardes, D. Golubkov, A. Golutvin, S. Gomez Fernandez, W. Gomulka, F. Goncalves Abrantes, I. Gonçales Vaz, M. Goncerz, G. Gong, J. A. Gooding, I. V. Gorelov, C. Gotti, E. Govorkova, J. P. Grabowski, L. A. Granado Cardoso, E. Graugés, E. Graverini, L. Grazette, G. Graziani, A. T. Grecu, N. A. Grieser, L. Grillo, C. Gu, M. Guarise, L. Guerry, A. -K. Guseinov, E. Gushchin, Y. Guz, T. Gys, K. Habermann, T. Hadavizadeh, C. Hadjivasiliou, G. Haefeli, C. Haen, S. Haken, G. Hallett, P. M. Hamilton, J. Hammerich, Q. Han, X. Han, S. Hansmann-Menzemer, L. Hao, N. Harnew, T. J. Harris, M. Hartmann, S. Hashmi, J. He, N. Heatley, A. Hedes, F. Hemmer, C. Henderson, R. Henderson, R. D. L. Henderson, A. M. Hennequin, K. Hennessy, J. Herd, P. Herrero Gascon, J. Heuel, A. Heyn, A. Hicheur, G. Hijano Mendizabal, J. Horswill, R. Hou, Y. Hou, D. C. Houston, N. Howarth, W. Hu, X. Hu, W. Hulsbergen, R. J. Hunter, M. Hushchyn, D. Hutchcroft, M. Idzik, D. Ilin, P. Ilten, A. Iohner, A. Ishteev, H. Jage, S. J. Jaimes Elles, S. Jakobsen, T. Jakoubek, E. Jans, B. K. Jashal, A. Jawahery, C. Jayaweera, A. Jelavic, V. Jevtic, Z. Jia, E. Jiang, X. Jiang, Y. Jiang, Y. J. Jiang, E. Jimenez Moya, N. Jindal, M. John, A. John Rubesh Rajan, D. Johnson, C. R. Jones, S. Joshi, B. Jost, J. Juan Castella, N. Jurik, I. Juszczak, K. Kalecinska, D. Kaminaris, S. Kandybei, M. Kane, Y. Kang, C. Kar, M. Karacson, A. Kauniskangas, J. W. Kautz, M. K. Kazanecki, F. Keizer, M. Kenzie, T. Ketel, B. Khanji, S. Kholodenko, G. Khreich, F. Kiraz, T. Kirn, V. S. Kirsebom, S. Klaver, N. Kleijne, A. Kleimenova, D. K. Klekots, K. Klimaszewski, M. R. Kmiec, T. Knospe, R. Kolb, S. Koliiev, L. Kolk, A. Konoplyannikov, P. Kopciewicz, P. Koppenburg, A. Korchin, I. Kostiuk, O. Kot, S. Kotriakhova, E. Kowalczyk, A. Kozachuk, P. Kravchenko, L. Kravchuk, O. Kravcov, M. Kreps, P. Krokovny, W. Krupa, W. Krzemien, O. Kshyvanskyi, S. Kubis, M. Kucharczyk, V. Kudryavtsev, E. Kulikova, A. Kupsc, V. Kushnir, B. Kutsenko, J. Kvapil, I. Kyryllin, D. Lacarrere, P. Laguarta Gonzalez, A. Lai, A. Lampis, D. Lancierini, C. Landesa Gomez, J. J. Lane, G. Lanfranchi, C. Langenbruch, J. Langer, T. Latham, F. Lazzari, C. Lazzeroni, R. Le Gac, H. Lee, R. Lefèvre, A. Leflat, M. Lehuraux, E. Lemos Cid, O. Leroy, T. Lesiak, E. D. Lesser, B. Leverington, A. Li, C. Li, C. Li, H. Li, J. Li, K. Li, L. Li, P. Li, P. -R. Li, Q. Li, T. Li, T. Li, Y. Li, Y. Li, Y. Li, Z. Lian, Q. Liang, X. Liang, Z. Liang, S. Libralon, A. Lightbody, C. Lin, T. Lin, R. Lindner, H. Linton, R. Litvinov, D. Liu, F. L. Liu, G. Liu, K. Liu, S. Liu, W. Liu, Y. Liu, Y. Liu, Y. L. Liu, G. Loachamin Ordonez, I. Lobo, A. Lobo Salvia, A. Loi, T. Long, F. C. L. Lopes, J. H. Lopes, A. Lopez Huertas, C. Lopez Iribarnegaray, S. López Soliño, Q. Lu, C. Lucarelli, D. Lucchesi, M. Lucio Martinez, Y. Luo, A. Lupato, E. Luppi, K. Lynch, S. Lyu, X. -R. Lyu, G. M. Ma, H. Ma, S. Maccolini, F. Machefert, F. Maciuc, B. Mack, I. Mackay, L. M. Mackey, L. R. Madhan Mohan, M. J. Madurai, D. Magdalinski, D. Maisuzenko, J. J. Malczewski, S. Malde, L. Malentacca, A. Malinin, T. Maltsev, G. Manca, G. Mancinelli, C. Mancuso, R. Manera Escalero, F. M. Manganella, D. Manuzzi, D. Marangotto, J. F. Marchand, R. Marchevski, U. Marconi, E. Mariani, S. Mariani, C. Marin Benito, J. Marks, A. M. Marshall, L. Martel, G. Martelli, G. Martellotti, L. Martinazzoli, M. Martinelli, D. Martinez Gomez, D. Martinez Santos, F. Martinez Vidal, A. Martorell i Granollers, A. Massafferri, R. Matev, A. Mathad, V. Matiunin, C. Matteuzzi, K. R. Mattioli, A. Mauri, E. Maurice, J. Mauricio, P. Mayencourt, J. Mazorra de Cos, M. Mazurek, D. Mazzanti Tarancon, M. McCann, N. T. McHugh, A. McNab, R. McNulty, B. Meadows, D. Melnychuk, D. Mendoza Granada, P. Menendez Valdes Perez, F. M. Meng, M. Merk, A. Merli, L. Meyer Garcia, D. Miao, H. Miao, M. Mikhasenko, D. A. Milanes, A. Minotti, E. Minucci, T. Miralles, B. Mitreska, D. S. Mitzel, R. Mocanu, A. Modak, L. Moeser, R. D. Moise, E. F. Molina Cardenas, T. Mombächer, M. Monk, T. Monnard, S. Monteil, A. Morcillo Gomez, G. Morello, M. J. Morello, M. P. Morgenthaler, A. Moro, J. Moron, W. Morren, A. B. Morris, A. G. Morris, R. Mountain, Z. Mu, E. Muhammad, F. Muheim, M. Mulder, K. Müller, F. Muñoz-Rojas, V. Mytrochenko, P. Naik, T. Nakada, R. Nandakumar, G. Napoletano, I. Nasteva, M. Needham, E. Nekrasova, N. Neri, S. Neubert, N. Neufeld, P. Neustroev, J. Nicolini, D. Nicotra, E. M. Niel, N. Nikitin, L. Nisi, Q. Niu, B. K. Njoki, P. Nogarolli, P. Nogga, C. Normand, J. Novoa Fernandez, G. Nowak, C. Nunez, H. N. Nur, A. Oblakowska-Mucha, V. Obraztsov, T. Oeser, A. Okhotnikov, O. Okhrimenko, R. Oldeman, F. Oliva, E. Olivart Pino, M. Olocco, R. H. O'Neil, J. S. Ordonez Soto, D. Osthues, J. M. Otalora Goicochea, P. Owen, A. Oyanguren, O. Ozcelik, F. Paciolla, A. Padee, K. O. Padeken, B. Pagare, T. Pajero, A. Palano, L. Palini, M. Palutan, C. Pan, X. Pan, S. Panebianco, S. Paniskaki, L. Paolucci, A. Papanestis, M. Pappagallo, L. L. Pappalardo, C. Pappenheimer, C. Parkes, D. Parmar, G. Passaleva, D. Passaro, A. Pastore, M. Patel, J. Patoc, C. Patrignani, A. Paul, C. J. Pawley, A. Pellegrino, J. Peng, X. Peng, M. Pepe Altarelli, S. Perazzini, D. Pereima, H. Pereira Da Costa, M. Pereira Martinez, A. Pereiro Castro, C. Perez, P. Perret, A. Perrevoort, A. Perro, M. J. Peters, K. Petridis, A. Petrolini, S. Pezzulo, J. P. Pfaller, H. Pham, L. Pica, M. Piccini, L. Piccolo, B. Pietrzyk, R. N. Pilato, D. Pinci, F. Pisani, M. Pizzichemi, V. M. Placinta, M. Plo Casasus, T. Poeschl, F. Polci, M. Poli Lener, A. Poluektov, N. Polukhina, I. Polyakov, E. Polycarpo, S. Ponce, D. Popov, K. Popp, S. Poslavskii, K. Prasanth, C. Prouve, D. Provenzano, V. Pugatch, A. Puicercus Gomez, G. Punzi, J. R. Pybus, Q. Qian, W. Qian, N. Qin, R. Quagliani, R. I. Rabadan Trejo, R. Racz, J. H. Rademacker, M. Rama, M. Ramírez García, V. Ramos De Oliveira, M. Ramos Pernas, M. S. Rangel, F. Ratnikov, G. Raven, M. Rebollo De Miguel, F. Redi, J. Reich, F. Reiss, Z. Ren, P. K. Resmi, M. Ribalda Galvez, R. Ribatti, G. Ricart, D. Riccardi, S. Ricciardi, K. Richardson, M. Richardson-Slipper, F. Riehn, K. Rinnert, P. Robbe, G. Robertson, E. Rodrigues, A. Rodriguez Alvarez, E. Rodriguez Fernandez, J. A. Rodriguez Lopez, E. Rodriguez Rodriguez, J. Roensch, A. Rogachev, A. Rogovskiy, D. L. Rolf, P. Roloff, V. Romanovskiy, A. Romero Vidal, G. Romolini, F. Ronchetti, T. Rong, M. Rotondo, M. S. Rudolph, M. Ruiz Diaz, R. A. Ruiz Fernandez, J. Ruiz Vidal, J. J. Saavedra-Arias, J. J. Saborido Silva, S. E. R. Sacha Emile R., N. Sagidova, D. Sahoo, N. Sahoo, B. Saitta, M. Salomoni, I. Sanderswood, R. Santacesaria, C. Santamarina Rios, M. Santimaria, L. Santoro, E. Santovetti, A. Saputi, D. Saranin, A. Sarnatskiy, G. Sarpis, M. Sarpis, C. Satriano, A. Satta, M. Saur, D. Savrina, H. Sazak, F. Sborzacchi, A. Scarabotto, S. Schael, S. Scherl, M. Schiller, H. Schindler, M. Schmelling, B. Schmidt, N. Schmidt, S. Schmitt, H. Schmitz, O. Schneider, A. Schopper, N. Schulte, M. H. Schune, G. Schwering, B. Sciascia, A. Sciuccati, G. Scriven, I. Segal, S. Sellam, A. Semennikov, T. Senger, M. Senghi Soares, A. Sergi, N. Serra, L. Sestini, B. Sevilla Sanjuan, Y. Shang, D. M. Shangase, M. Shapkin, R. S. Sharma, L. Shchutska, T. Shears, J. Shen, Z. Shen, S. Sheng, V. Shevchenko, B. Shi, J. Shi, Q. Shi, W. S. Shi, E. Shmanin, R. Shorkin, R. Silva Coutinho, G. Simi, S. Simone, M. Singha, I. Siral, N. Skidmore, T. Skwarnicki, M. W. Slater, E. Smith, M. Smith, L. Soares Lavra, M. D. Sokoloff, F. J. P. Soler, A. Solomin, A. Solovev, K. Solovieva, N. S. Sommerfeld, R. Song, Y. Song, Y. Song, Y. S. Song, F. L. Souza De Almeida, B. Souza De Paula, K. M. Sowa, E. Spadaro Norella, E. Spedicato, J. G. Speer, P. Spradlin, F. Stagni, M. Stahl, S. Stahl, S. Stanislaus, M. Stefaniak, O. Steinkamp, D. Strekalina, Y. Su, F. Suljik, J. Sun, J. Sun, L. Sun, D. Sundfeld, W. Sutcliffe, P. Svihra, V. Svintozelskyi, K. Swientek, F. Swystun, A. Szabelski, T. Szumlak, Y. Tan, Y. Tang, Y. T. Tang, M. D. Tat, J. A. Teijeiro Jimenez, A. Terentev, F. Terzuoli, F. Teubert, E. Thomas, D. J. D. Thompson, A. R. Thomson-Strong, H. Tilquin, V. Tisserand, S. T'Jampens, M. Tobin, T. T. Todorov, L. Tomassetti, G. Tonani, X. Tong, T. Tork, L. Toscano, D. Y. Tou, C. Trippl, G. Tuci, N. Tuning, L. H. Uecker, A. Ukleja, D. J. Unverzagt, A. Upadhyay, B. Urbach, A. Usachov, A. Ustyuzhanin, U. Uwer, V. Vagnoni, A. Vaitkevicius, V. Valcarce Cadenas, G. Valenti, N. Valls Canudas, J. van Eldik, H. Van Hecke, E. van Herwijnen, C. B. Van Hulse, R. Van Laak, M. van Veghel, G. Vasquez, R. Vazquez Gomez, P. Vazquez Regueiro, C. Vázquez Sierra, S. Vecchi, J. Velilla Serna, J. J. Velthuis, M. Veltri, A. Venkateswaran, M. Verdoglia, M. Vesterinen, W. Vetens, D. Vico Benet, P. Vidrier Villalba, M. Vieites Diaz, X. Vilasis-Cardona, E. Vilella Figueras, A. Villa, P. Vincent, B. Vivacqua, F. C. Volle, D. vom Bruch, N. Voropaev, K. Vos, C. Vrahas, J. Wagner, J. Walsh, E. J. Walton, G. Wan, A. Wang, B. Wang, C. Wang, G. Wang, H. Wang, J. Wang, J. Wang, J. Wang, J. Wang, M. Wang, N. W. Wang, R. Wang, X. Wang, X. Wang, X. W. Wang, Y. Wang, Y. Wang, Y. H. Wang, Z. Wang, Z. Wang, J. A. Ward, M. Waterlaat, N. K. Watson, D. Websdale, Y. Wei, Z. Weida, J. Wendel, B. D. C. Westhenry, C. White, M. Whitehead, E. Whiter, A. R. Wiederhold, D. Wiedner, M. A. Wiegertjes, C. Wild, G. Wilkinson, M. K. Wilkinson, M. Williams, M. J. Williams, M. R. J. Williams, R. Williams, S. Williams, Z. Williams, F. F. Wilson, M. Winn, W. Wislicki, M. Witek, L. Witola, T. Wolf, E. Wood, G. Wormser, S. A. Wotton, H. Wu, J. Wu, X. Wu, Y. Wu, Z. Wu, K. Wyllie, S. Xian, Z. Xiang, Y. Xie, T. X. Xing, A. Xu, L. Xu, M. Xu, R. Xu, Z. Xu, Z. Xu, Z. Xu, S. Yadav, K. Yang, X. Yang, Y. Yang, Y. Yang, Z. Yang, Z. Yang, H. Yeung, H. Yin, X. Yin, C. Y. Yu, J. Yu, X. Yuan, Y Yuan, J. A. Zamora Saa, M. Zavertyaev, M. Zdybal, F. Zenesini, C. Zeng, M. Zeng, S. H Zeng, C. Zhang, D. Zhang, J. Zhang, L. Zhang, R. Zhang, S. Zhang, S. L. Zhang, Y. Zhang, Y. Z. Zhang, Z. Zhang, Y. Zhao, A. Zhelezov, S. Z. Zheng, X. Z. Zheng, Y. Zheng, T. Zhou, X. Zhou, V. Zhovkovska, L. Z. Zhu, X. Zhu, X. Zhu, Y. Zhu, V. Zhukov, J. Zhuo, D. Zuliani, G. Zunica,Comments: All figures and tables, along with any supplementary material and additional information, are available at https://lbfence.cern.ch/alcm/public/analysis/full-details/5692 (LHCb public pages)Subjects: hep-exCreated: 2026-03-24; Updated: 2026-03-26; Datestamp: 2026-03-26
The collinear and transverse-momentum-dependent JET fragmentation function and the radial profile for $B^{\pm}$ mesons in JETs are measured. The $B^{\pm}$ mesons are reconstructed through the $J/ψ(\to μ^{+} μ^{-}) K^{\pm}$ decay channel using proton-proton collision data collected during 2016-2018 with the LHCb detector at a center-of-mass energy of $\sqrt{s}=13$ TeV, corresponding to an integrated luminosity of $5.4$ fb$^{-1}$. The results complement recent measurements of JET fragmentation functions for heavy-flavor hadrons and suggest a growing contribution of gluon fragmentation to $B^{\pm}$ mesons as the JET transverse momentum increases.
[abstract 28 / 35] (score: 2) - Title: A rotating GUP BLACK HOLE: metric, shadow, and bounds on quantum parametersAuthors: Federica Fragomeno, Samantha Hergott, Saeed Rastgoo, Evan Vienneau,Comments: 26 pages, 6 figuresSubjects: gr-qc astro-ph.HECreated: 2026-03-24; Updated: 2026-03-26; Datestamp: 2026-03-26
Recently, for the first time, a metric of a static spherically symmetric generalized uncertainty inspired quantum BLACK HOLE was derived. We apply the modified Newman-Janis algorithm to this metric and derive its rotating counterpart. We show that this metric has all the correct limits, while due to Newman-Janis side effects, the singularity which was resolved in the static case, is introduced back into the model. However, the slowly-rotating limit of this BLACK HOLE is singularity-free. Furthermore, we show that the presence of quantum parameters modifies the location of the horizons, temperature, and entropy of the BLACK HOLE, and allows the existence of naked singularities even if the ratio of the spin parameter to mass of the BLACK HOLE is less than unity. Finally, by computing the shadow parameters of this BLACK HOLE and comparing them with data from the Event Horizon Telescope for both M87* and Sgr A*, we set bounds on one of the quantum parameters of the model, and show that there is a limit on the angular momentum of M87* if this model is valid.
[abstract 29 / 35] (score: 2) - Title: Microtearing Thresholds and Second-Stable Ballooning in the DIII-D Pedestal: Reduced Modeling and Core-Edge ImplicationsAuthors: David R. Hatch, Leonhard A. Leppin, Mike T. Kotschenreuther, Saeid Houshmandyar, Swadesh M. Mahajan, Joseph Schmidt, Ping-Yu Li,Comments:Subjects: physics.plasm-phCreated: 2026-03-24; Updated: 2026-03-26; Datestamp: 2026-03-26
Global and local linear gyrokinetic simulations of 42 pedestal equilibria from three DIII-D discharges are used to investigate pedestal stability and its impact on pedestal structure and confinement. Microtearing modes (MTMs) and kinetic ballooning modes (KBMs) represent the main ion scale instabilities. For all three discharges, MTMs lie near a stability boundary in the mid-pedestal and exhibit threshold behavior, with growth rates increasing at and beyond pre-ELM pressure gradients. Pedestal MTMs retain conventional signatures but also show enhanced particle transport and partial density-gradient drive, indicating they can constrain pedestal {\it pressure} rather than electron temperature alone. KBMs are typically second-stable in this region due to low MAGNETic shear and large pressure gradients, though they can become active near the pedestal foot where MAGNETic shear is higher. These findings suggest MTMs play the role of inter-ELM pressure limit in the mid-pedestal when KBM is second stable. A preliminary quasilinear mixing-length transport model, with properly tuned free parameters, reproduces experimental temperature and density profiles when coupled to ASTRA. When applied to a case with doubled separatrix density, the model predicts reduced pedestal pressure consistent with ITPA H-mode confinement trends, attributable to increased MTM and ETG transport. These results clarify pedestal-limiting mechanisms and establish a physics-based link between separatrix conditions, pedestal structure, and global confinement. This work lays the foundation for new predictive modeling capabilities for core-edge integration in burning plasma regimes.
[abstract 30 / 35] (score: 2) - Title: Jet-edge interaction: linear and non-linear frequency-selection mechanismsAuthors: Michael N. Stavropoulos, André V. G. Cavalieri, Lutz Lesshafft, Peter Jordan,Comments:Subjects: physics.flu-dynCreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
We consider a round turbulent JET grazing a rectangular plate angled at $45^\circ$. Through sound pressure measurements, the tonal dynamics associated with JET-edge interaction are explored in a parameter space comprising JET Mach number, $M_j$, and plate radial position, $R/D$. A variety of spectral signatures are observed and classified. The classification - based on analysis of power-spectral density and bicoherence, and on the resonance model proposed by Jordan et al. (2018) - comprises: broadband spectra; tonal spectra associated with purely linear frequency-selection mechanisms; tonal spectra associated with both linear and non-linear frequency selection. The classification identifies regions in the parameter space ($M_j$, $R/D$); and clarifies mechanisms underpinning regime changes. The linear frequency selection (LFS) regime comprises multiple tones, with no evidence of triad interaction. A regime involving non-linear frequency selection emerges from this state, with the strong amplification of one LFS tone, which then generates multiple harmonics. Intermediate regimes are identified involving weaker, non-harmonic triadic interactions where two LFS tones interact to generate a third tone. In addition to these mechanisms a mode-switching mechanism is identified at $M_j$ = 0.84 and shown to result from the cut-on of a new upstream-travelling wave at that Mach number. The mode-switch is found to be remarkably robust, occurring in a repeatable manner over a Mach-number increment of 0.01 regardless of whether the Mach number is increased or decreased (no hysteresis is observed).
[abstract 31 / 35] (score: 2) - Title: Machine Learning-Based Classification of Active Galaxies and Estimation of Supermassive Black Hole MassesAuthors: Farideh Mazoochi, Reihaneh Karimi, Mohammad Hossein Zhoolideh Haghighi, Fatemeh Tabatabaei,Comments: 9 Pages, 7 Figures, Accepted for publication in Monthly Notices of the Royal Astronomical SocietySubjects: astro-ph.GACreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
Distinguishing active galaxies from star-forming galaxies is essential for understanding galaxy evolution. Diagnostic methods like the BPT (Baldwin, Phillips, and Terlevich) diagram use optical emission-line ratios to separate galaxies. However, with growing availability of large surveys and high-resolution instruments, manually identifying galaxy types has become increasingly challenging. In this study, we investigate machine learning to classify active and star-forming galaxies using properties like stellar mass, stellar velocity dispersion, colour, redshift, and [O III] luminosity. These new approaches enable faster AGN/star-forming galaxy classification than the BPT diagram and provide a flexible, scalable alternative that can complement traditional diagnostics, particularly for large surveys or low-quality data. We employ four classification algorithms -- Decision Tree, Random Forest, Support Vector Classifier (SVC), and k-Nearest Neighbours (KNN) -- using the Galaxy Zoo 1 dataset derived from the SDSS sample. The dataset contains 47,675 galaxies within the redshift range 0.02--0.05, including 17,002 pure star-forming and 2,254 active galaxies, labeled using the BPT diagram. These labels train and evaluate our models through confusion matrices, learning curves, and receiver operating characteristic (ROC) curves. Among the four algorithms, the SVC and Random Forest models achieve the highest accuracy of approximately 93\%, while KNN shows the lowest at 88\%. Furthermore, we estimate supermassive BLACK HOLE masses using stellar velocity dispersion ($σ$) and the $M_{\rm BH}-σ$ relation. We apply four regression models -- Random Forest Regressor, Support Vector Regressor (SVR), KNN Regressor, and Polynomial Regression. All four models produce similar results, with $R^2$ values from 0.75 to 0.77, indicating consistent performance.
[abstract 32 / 35] (score: 2) - Title: Study of Low-Frequency Core-Edge Coupling in a Tokamak: II. Spatial Channeling & Focusing In Antenna-Driven MHDAuthors: Andreas Bierwage, Wonjun Lee, Young-chul Ghim, Panith Adulsiriswad, Nobuyuki Aiba, Seungmin Bong, Gyungjin Choi, Matteo Falessi, Philipp W. Lauber, Masatoshi Yagi,Comments: 36 pages (23 main + Appendices), 30 figures (17 main + Appendices)Subjects: physics.plasm-phCreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
Motivated by evidence for core-edge coupling in the form of double-peaked fishbone-like low-frequency modes ($\lesssim 20\,{\rm kHz}$) in KSTAR, which exhibit synchronized Alfvénic activity both in the central core and near the plasma edge [1], we study the nonlocal response of a tokamak plasma in a visco-resistive full MHD simulation model using the code MEGA. The waves are driven by an internal "antenna" that is localized both radially and azimuthally in the poloidal $(R,z)$ plane and has a sinusoidal form $\exp(inζ- iωt)$ with Fourier mode number $n=\pm 1$ in the toroidal angle $ζ$ and fixed angular frequency $ω$ in time $t$. By flattening the safety factor profile $q(r)$ at suitable locations in the minor radius $r$, we created plateaus in the low-frequency Alfvén continua that act as wave "receivers". First, we confirm that such continuum plateaus respond with a coherent quasi-mode even when the driving antenna is located at a distant radius. Second, by varying the antenna location, we confirm the expectation of inward drive being more efficient than outward drive, which we attribute to volumetric focusing. Third, we find that the central core also responds well at frequencies below the central Alfvénic continuum plateau, which could facilitate chirping. Our results show that a core-localized low-frequency response does not necessarily require core-localized drive nor an exactly matching continuum, but may be driven from the edge and sub-resonantly. It remains to be seen to what extent the examined effects play a role in double-peaked fishbone-like activity. Other possible contributing mechanisms are discussed to motivate further study. Our analyses also elucidate the mode structure formation process, from transients to quasi- or eigenmodes, here in the realm of MHD, and to be followed by a verification study against kinetic models.
[abstract 33 / 35] (score: 2) - Title: A generalization of the Froissart-Stora formula to piecewise-linear spin-orbit resonance crossingsAuthors: Joseph P. Devlin, Georg H. Hoffstaetter, Desmond P. Barber,Comments: 12 pages, 7 figuresSubjects: physics.acc-phCreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
Spin-polarized beams are important for some nuclear and high-energy physics experiments, such as those planned for the future Electron-Ion Collider (EIC). However, maintaining POLARIZATION during the acceleration of a charged-particle beam is difficult because the periodic nature of circular accelerators leads to spin-orbit resonances where the spin-precession frequency is a sum of integer multiples of the orbital frequencies. Usually, the dominant dePOLARIZATION mechanisms are first-order spin-orbit resonances and the dePOLARIZATION associated with crossing such a resonance can be computed using the Froissart-Stora formula. However, accelerating polarized hadron beams to high energy requires special MAGNET structures called Siberian snakes. When these are implemented to maintain a spin-precession frequency of one-half the revolution frequency, there will be no first-order spin-orbit resonance crossings. The dominant dePOLARIZATION mechanisms are then higher-order spin-orbit resonances. The Froissart-Stora formula can be applied to higher-order resonances when the slope of the amplitude-dependent spin tune is constant. However, the slope of the amplitude-dependent spin tune often changes at the moment of resonance crossing. This work introduces a generalization of the Froissart-Stora formula which is applicable when the slope changes in this manner. The applicability of this formula is demonstrated through tracking simulations of a higher-order resonance crossing in both a toy model and the Relativistic Heavy Ion Collider (RHIC). It is additionally shown that the Froissart-Stora formula is mathematically equivalent to the Landau-Zener formula for the diabatic transition probability in two-level systems with a linearly increasing energy gap and constant coupling. This work therefore also extends the Landau-Zener formula to the case of changing slope.
[abstract 34 / 35] (score: 2) - Title: Experimental Evidence for Increased Particle Fluxes Due to a Change in Transport at the Separatrix near Density Limits on Alcator C-ModAuthors: M. A. Miller, J. W. Hughes, T. Eich, G. R. Tynan, P. Manz, A. E. Hubbard, B. LaBombard, J. Dunsmore,Comments:Subjects: physics.plasm-phCreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
Experimental inferences of cross-field particle flux at the separatrix, $Γ_{\perp}^\mathrm{sep}$, show rapid growth near H-mode and L-mode density limits at high MAGNETic field on Alcator C-Mod. Increases in $Γ_{\perp}^\mathrm{sep}$ correlate well with proximity to high density operational boundaries as proposed by the separatrix operational space model. $Γ_{\perp}^\mathrm{sep}$ grows as the L-mode density limit and the H-L-mode back transition boundaries are approached, consistent with expectations of plasma instability-driven turbulence suggested by theory, confirming the power dependence of density limits. $Γ_{\perp}^\mathrm{sep}$ is well-organized by the characteristic wavenumber for resistive ballooning mode turbulence, $k_\mathrm{RBM}$, from interchange-drift-Alfvén fluid turbulence theory, with additional dependence on the cylindrical safety factor, $\hat{q}_\mathrm{cyl}$, yielding an empirical limit to plasma operation of $k_\mathrm{RBM}^{2}\hat{q}_\mathrm{cyl} = 1$. This limit corresponds to the point where the perpendicular heat flux, $Q_{\perp}$, reaches the level of the parallel heat flux, $Q_{\parallel}$, i.e. $Q_{\perp} \approx Q_{\parallel}$, beyond which point thermal equilibrium is not satisfied, resulting in a fold catastrophe.
[abstract 35 / 35] (score: 2) - Title: Study of Low-Frequency Core-Edge Coupling in a Tokamak: I. Experimental Observation in KSTARAuthors: Wonjun Lee, Andreas Bierwage, Seungmin Bong, Jaewook Kim, K. D. Lee, J. G. Bak, G. J. Choi, C. Sung, Y. -c. Ghim,Comments: 16 pages, 16 figuresSubjects: physics.plasm-phCreated: 2026-03-25; Updated: 2026-03-26; Datestamp: 2026-03-26
Double-peaked fishbone events across multiple KSTAR discharges are investigated. The normalized beta $β_{\mathrm{N}}$ and the edge safety factor $q_{\mathrm{95}}$ under which the fishbones appear vary depending on the presence and form of external MAGNETic perturbations. The fishbone strength is closely related to $β_{\mathrm{N}}$ and $q_{\mathrm{95}}$: as $β_{\mathrm{N}}$ increases and $q_{\mathrm{95}}$ decreases, the fishbone strength increases. Measured fishbone-relevant signals are decomposed into amplitude envelope and phase components in the temporal domain, which are analyzed separately. In terms of the amplitude envelope component, the edge electron temperature fluctuation $\tilde T_\mathrm{e}^{\mathrm{Edge}}$ becomes more correlated with the poloidal MAGNETic fluctuation $\dot{B}_\mathrmθ$ compared to the core electron temperature fluctuation $\tilde T_\mathrm{e}^{\mathrm{Core}}$ as fishbone strength increases. In terms of the phase component, the phase of $\tilde T_\mathrm{e}^{\mathrm{Edge}}$ precedes the phase of $\tilde T_\mathrm{e}^{\mathrm{Core}}$ except in the case of very weak fishbones where the phase relations are inconclusive due to weak fishbone activity at the edge plasma, which is comparable to background fluctuations. The investigation suggests the possibility that the edge activity is not a mere side effect of the core activity, but could play an active role.
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