Current date: 2026-06-26
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Scoring abstracts
Number of records retrieved: 733
Keyword score statistics
score 12 -- 1 abstracts
score 11 -- 1 abstracts
score 10 -- 1 abstracts
score 9 -- 2 abstracts
score 8 -- 3 abstracts
score 7 -- 1 abstracts
score 6 -- 1 abstracts
score 5 -- 3 abstracts
score 4 -- 10 abstracts
score 3 -- 9 abstracts
score 2 -- 32 abstracts
in total -- 64 abstracts
Articles that appeared on 2026-06-26
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[abstract 1 / 64] Wow! (score: 12)
- Title: The Emerging Population of High-energy Emitting Radio GalaxiesAuthors: G. Bruni, V. S. Paliya, D. J. Saikia, L. Bassani, R. D. Baldi, E. Bronzini, F. D'Ammando, S. del Palacio, M. Kadler, Y. Y. Kovalev, D. V. Lal, G. Migliori, B. Mingo, J. Moldon, L. Ostorero, F. Panessa, M. Persic, I. Prandoni, L. Ricci, T. Savolainen, F. Shankar, F. Tavecchio, E. Traianou, F. Ubertosi, T. Venturi,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no: AASKAII/Bruni01. 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: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
High-energy emission from RADIO GALAXies provides a unique laboratory to study the connection between accretion, JET formation, and particle acceleration in ACTIVE GALACTIC NUCLEi (AGN). The recent detection of $γ$-ray emission from misaligned RADIO GALAXies - including Compact Symmetric Objects (CSOs), FR0, FRI/II, and even Giant Radio Galaxies (GRGs) - has shown that efficient particle acceleration is not limited to BLAZARs, but occurs throughout the full radio-loud AGN population. This finding supports a unifying framework where leptonic SYNCHROTRON, SYNCHROTRON self-Compton (SSC), and external inverse-Compton (EIC) processes coexist across multiple spatial scales, from the inner JET and corona to the extended lobes, possibly with a hadronic contribution in dense environments. The Square Kilometre Array (SKA) will be pivotal in advancing this field. SKA1-Low will detect and characterize diffuse, low-surface-brightness emission tracing aged plasma and JET duty cycles. SKA1-Mid will enable high-resolution spectral and polarimetric studies of compact JETs and nuclear regions, while SKA-VLBI will connect parsec- to kiloparsec-scale structures, identifying the exact sites of high-energy dissipation. In synergy with forthcoming high-energy missions such as NewAthena and CTAO, SKA will provide the first spatially resolved, multi-scale view of particle acceleration and energy release in misaligned AGN, unveiling the physical link between the central engine and its large-scale feedback on the host galaxy evolution.
[abstract 2 / 64] Wow! (score: 11) - Title: Broad-band Spectral Modeling of Large-Scale X-ray Jets in High-Redshift Quasars: An MHD-Informed ApproachAuthors: Patryk Liniewicz, Łukasz Stawarz, C. C. Cheung, Giulia Migliori, Aneta Siemiginowska,Comments: Submitted to ApJSubjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
We present a systematic spectral analysis of kiloparsec-scale JETs in high-redshift QUASARs, modeling their radio-to-X-ray emission as SYNCHROTRON radiation and inverse-COMPTONization of CMB by RELATIVISTIC electrons. In contrast to the homogeneous one-zone approximation commonly adopted in the literature, we describe the JET as a current-carrying, axially symmetric outflow with a purely toroidal MAGNETic field in MAGNETohydrostatic equilibrium and with radial velocity shear. In this framework, the pressure, MAGNETic-field, and bulk-velocity profiles are linked self-consistently, capturing the radial stratification of the emitting region without introducing additional free parameters. For any individual source, the model effectively retains only a small number of free parameters, including the total JET power, $L_{\rm j}$, and the on-axis bulk Lorentz factor, $Γ_0$. We consider two prescriptions for the radial distribution of the radiating electrons -- proportional either to the gas pressure or to the rest-frame MAGNETic energy density -- and two toroidal-field profiles, yielding four model variants. Applying the model to a sample of ten QUASAR JETs at $z \geq 2.5$ with X-ray features resolved by \textit{Chandra}, we perform Bayesian parameter inference and model comparison. The Bayesian evidence systematically favors electron distributions that follow the gas pressure rather than the MAGNETic energy density, while the data discriminate only weakly between the assumed field profiles. The inferred JET powers, reaching $L_{\rm j} \sim 10^{49}\,\mathrm{erg\,s^{-1}}$, are systematically larger than those obtained from one-zone models, and the corresponding global JET MAGNETization parameters are low. None of the derived quantities, including $Γ_0 \sim \mathcal{O}(10)$, shows a significant monotonic trend with redshift.
[abstract 3 / 64] Wow! (score: 10) - Title: Extreme PeV accelerator associated with GRS 1915+105Authors: Zhen Cao, F. Aharonian, Y. X. Bai, Y. W. Bao, D. Bastieri, X. J. Bi, Y. J. Bi, W. Bian, J. Blunier, A. V. Bukevich, C. M. Cai, Y. Y. Cai, W. Y. Cao, Zhe Cao, J. Chang, J. F. Chang, E. S. Chen, G. H. Chen, H. K. Chen, L. F. Chen, Liang Chen, Long Chen, M. J. Chen, M. L. Chen, Q. H. Chen, S. Chen, S. H. Chen, S. Z. Chen, T. L. Chen, X. B. Chen, X. J. Chen, X. P. Chen, Y. Chen, N. Cheng, Q. Y. Cheng, Y. D. Cheng, M. Y. Cui, S. W. Cui, X. H. Cui, Y. D. Cui, B. Z. Dai, H. L. Dai, Z. G. Dai, Danzengluobu, Y. X. Diao, A. J. Dong, X. Q. Dong, K. K. Duan, J. H. Fan, Y. Z. Fan, J. Fang, J. H. Fang, K. Fang, C. F. Feng, H. Feng, L. Feng, S. H. Feng, X. T. Feng, Y. Feng, Y. L. Feng, S. Gabici, B. Gao, Q. Gao, W. Gao, W. K. Gao, M. M. Ge, T. T. Ge, L. S. Geng, G. Giacinti, G. H. Gong, Q. B. Gou, M. H. Gu, F. L. Guo, J. Guo, K. J. Guo, X. L. Guo, Y. Q. Guo, Y. Y. Guo, R. P. Han, O. A. Hannuksela, M. Hasan, H. H. He, H. N. He, J. Y. He, X. Y. He, Y. He, S. Hernández-Cadena, B. W. Hou, C. Hou, X. Hou, H. B. Hu, S. C. Hu, C. Huang, D. H. Huang, J. J. Huang, X. L. Huang, X. T. Huang, X. Y. Huang, Y. Huang, Y. Y. Huang, A. Inventar, X. L. Ji, H. Y. Jia, K. Jia, H. B. Jiang, K. Jiang, X. W. Jiang, Z. J. Jiang, M. Jin, S. Kaci, M. M. Kang, I. Karpikov, D. Khangulyan, D. Kuleshov, K. Kurinov, Cheng Li, Cong Li, D. Li, F. Li, H. B. Li, H. C. Li, Jian Li, Jie Li, K. Li, L. Li, R. L. Li, S. D. Li, T. Y. Li, W. L. Li, X. R. Li, Xin Li, Y. Li, Zhe Li, Zhuo Li, E. W. Liang, Y. F. Liang, S. J. Lin, B. Liu, C. Liu, D. Liu, D. B. Liu, H. Liu, J. Liu, J. L. Liu, J. R. Liu, M. Y. Liu, R. Y. Liu, S. M. Liu, W. Liu, X. Liu, Y. Liu, Y. Liu, Y. N. Liu, Y. Q. Lou, Q. Luo, Y. Luo, H. K. Lv, B. Q. Ma, L. L. Ma, X. H. Ma, I. O. Maliy, J. R. Mao, Z. Min, W. Mitthumsiri, Y. Mizuno, G. B. Mou, A. Neronov, K. C. Y. Ng, M. Y. Ni, L. Nie, L. J. Ou, Z. W. Ou, P. Pattarakijwanich, Z. Y. Pei, D. Y. Peng, J. C. Qi, M. Y. Qi, J. J. Qin, D. Qu, A. Raza, C. Y. Ren, D. Ruffolo, A. Sáiz, D. Savchenko, D. Semikoz, L. Shao, O. Shchegolev, Y. Z. Shen, X. D. Sheng, Z. D. Shi, F. W. Shu, H. C. Song, Yu. V. Stenkin, V. Stepanov, Y. Su, D. X. Sun, H. Sun, J. X. Sun, Q. N. Sun, X. N. Sun, Z. B. Sun, N. H. Tabasam, J. Takata, P. H. T. Tam, H. B. Tan, Q. W. Tang, R. Tang, Z. B. Tang, W. W. Tian, C. N. Tong, L. H. Wan, C. Wang, D. H. Wang, G. W. Wang, H. G. Wang, J. C. Wang, K. Wang, Kai Wang, Kai Wang, L. P. Wang, L. Y. Wang, L. Y. Wang, R. Wang, W. Wang, X. G. Wang, X. J. Wang, X. Y. Wang, Y. Wang, Y. D. Wang, Z. H. Wang, Z. X. Wang, Zheng Wang, D. M. Wei, J. J. Wei, Y. J. Wei, T. Wen, S. S. Weng, C. Y. Wu, H. R. Wu, Q. W. Wu, S. Wu, X. F. Wu, Y. S. Wu, S. Q. Xi, J. Xia, J. J. Xia, G. M. Xiang, D. X. Xiao, G. Xiao, Y. F. Xiao, Y. L. Xin, H. D. Xing, Y. Xing, D. R. Xiong, B. N. Xu, C. Y. Xu, D. L. Xu, R. F. Xu, R. X. Xu, S. S. Xu, W. L. Xu, L. Xue, D. H. Yan, T. Yan, C. W. Yang, C. Y. Yang, F. F. Yang, L. L. Yang, M. J. Yang, R. Z. Yang, W. X. Yang, Z. H. Yang, Z. G. Yao, X. A. Ye, L. Q. Yin, N. Yin, X. H. You, Z. Y. You, Q. Yuan, H. Yue, H. D. Zeng, T. X. Zeng, W. Zeng, X. T. Zeng, M. Zha, B. B. Zhang, B. T. Zhang, C. Zhang, H. Zhang, H. M. Zhang, H. Y. Zhang, J. L. Zhang, J. Y. Zhang, Li Zhang, P. F. Zhang, R. Zhang, S. R. Zhang, S. S. Zhang, S. Y. Zhang, W. Zhang, W. Y. Zhang, X. Zhang, X. P. Zhang, Yi Zhang, Yong Zhang, Z. P. Zhang, J. Zhao, L. Zhao, L. Z. Zhao, S. P. Zhao, X. H. Zhao, Z. H. Zhao, F. Zheng, T. C. Zheng, B. Zhou, H. Zhou, J. N. Zhou, M. Zhou, P. Zhou, R. Zhou, X. X. Zhou, X. X. Zhou, B. Y. Zhu, C. G. Zhu, F. R. Zhu, H. Zhu, K. J. Zhu, Y. C. Zou, X. Zuo,Comments: 10 pages, 4 figures, with supplementary material. Corrected a typo in the y-axis units of Fig. 2Subjects: astro-ph.HE hep-exCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
MicroQUASARs, binary systems featuring RELATIVISTIC JETs, have emerged as sources for particle acceleration beyond PeV energies. We present a study of the broadband $γ$-ray emission from one of the most prominent Galactic microQUASARs GRS 1915+105 based on data accumulated by LHAASO and FERMI-LAT over 4 and 17 years, respectively. A joint analysis of LHAASO-WCDA and LHAASO-KM2A data reveals extended $γ$-ray emission whose centroid appears significantly shifted, by ~ 0.13°, from the binary system and its JETs. The spectral energy distribution is well described by a curved spectrum with progressive steepening that can be described by a log-parabola function with no evidence for a sharp cutoff, consistent with parent particles reaching multi-PeV energies and an extreme acceleration efficiency approaching the limit set by the available potential drop across the source. Several features, most notably the shift of the emission and single-power-law spectrum down to GeV band, favor radiation by COSMIC RAYs accelerated in the source interacting with the dense ambient medium. Our spectral modeling implies that at least a few percent of the JET mechanical power is transferred to protons, whose maximum energy reaches beyond 5 PeV. These results strengthen the case for microQUASARs as exceptionally efficient accelerators in our Galaxy.
[abstract 4 / 64] Wow! (score: 9) - Title: Revision of conservative lower bound on the intergalactic MAGNETic field from FERMI and Cherenkov telescope observations of extreme BLAZARsAuthors: J. Blunier, A. Neronov, D. Semikoz,Comments: 12 pages, 6 figures, 3 tablesSubjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Joint observations of extreme BLAZARs with FERMI Large Area Telescope (LAT) and Imaging Atmospheric Cherenkov telescopes (IACT) have been previously used to derive lower bounds on intergalactic MAGNETic field (IGMF). We update these previous bounds using a set of extreme BLAZARs that are detected in the Very-High-Energy (VHE, photon energies above 100 GeV) band by both FERMI/LAT and IACTs. We measure IGMF-dependent suppression of secondary delayed gamma-ray flux from electron-positron pairs deposited in the intergalactic medium by VHE gamma-rays interacting with Extragalactic Background Light. From overall 22 extreme BLAZARs detected by FERMI/LAT and IACTs in the VHE band, seven have their spectral characteristics inconsistent with the possibility of zero MAGNETic field along their lines of sight, even under the most restrictive assumption that the sources have only switched on at the start of VHE band observations. Adopting this assumption, we derive a "conservative" lower bound on the IGMF strength at the level of 2e-17 G. The tightest bound is imposed by the signal of 1ES 0502+675, a source that has not been considered in the IGMF analysis before. Our bound is comparable to the bound derived by MAGIC collaboration, but is weaker than that previously derived from analysis of FERMI/LAT and HESS telescope data, even though our dataset includes that data. We clarify the origin of this discrepancy.
[abstract 5 / 64] Wow! (score: 9) - Title: Gamma-ray Bursts and Kilonovae from Gravitational Wave EventsAuthors: Alberto Colombo, Marcello Giroletti, Susanna D. Vergani, Lauren Rhodes,Comments: Published in Advancing Astrophysics with the SKAII (AASKAII), 2026 (arXiv:2606.20366). Report-no: AASKAII/Colombo01Subjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
The detection of gravitational waves (GWs) from binary BLACK HOLEs in 2015 and the joint GW-electroMAGNETic (EM) observation of the binary neutron star merger GW170817 set a milestone in the multimessenger era in astrophysics. After four observing runs by the LIGO, Virgo, and KAGRA interferometers, a new cycle is planned for 2028, paving the way for next-generation detectors in the 2030s -- such as the Einstein Telescope, Cosmic Explorer, and LISA. The prospects for joint GW-EM studies, including kilonova searches in wide optical surveys, are vast but demanding. In the radio domain, connected interferometers and VLBI arrays have already proven essential in constraining the ejecta properties of GW170817. Radio emission from GAMMA-RAY BURST (GRB) afterglows, whether on- or off-axis, remains detectable for very long time, making radio observations the most effective method for identifying and tracking GW merger counterparts. These observations enable precise characterization of system evolution, detailed probing of GRB JET structures, and possible detection of misaligned JETs once their velocity becomes non-RELATIVISTIC. Even in its initial configuration (AA*), the SKAO will provide the sensitivity and field of view needed to complement GW counterpart searches during O5 and beyond, offering unmatched capabilities for long-term monitoring. Furthermore, independent of the GW detections, SKAO will enable population studies of the properties of both long (produced by the collapse of massive stars) and short (produced by the merger of neutron stars) GRBs, of their JETs and of their environment. We present an overview of this evolving observational landscape and of the key scientific questions SKAO will address.
[abstract 6 / 64] Wow! (score: 8) - Title: Magnetic monopole plasma oscillations and implications for TeV BLAZARsAuthors: Mariia Khelashvili, Takeshi Kobayashi, Andrew J. Long,Comments: 13+12 pages, 7+8 figuresSubjects: hep-ph astro-ph.CO astro-ph.HECreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
Magnetic monopoles arise in many beyond Standard Model scenarios, symmetrize Maxwell's equations, and their existence would be tied to the quantization of electric charge. It has been argued that, when placed in an astrophysical MAGNETic field, monopoles can induce a MAGNETic version of plasma oscillations. In this work, we explore monopole-induced oscillations of the intergalactic MAGNETic field (IGMF). We show that monopole-induced oscillations of the MAGNETic field lead to collimation of electrically charged particle trajectories, reducing the usual deflection by the MAGNETic field. The collimation effect impacts the deflection angle in the electroMAGNETic cascades of TeV BLAZARs and leads to a decrease in the angular size of BLAZAR secondary GeV halos. Therefore, the constraints on the secondary halo angular size from combined H.E.S.S. and FERMI-LAT observations translate into bounds on the MAGNETic monopole abundance. The bounds on the MAGNETic monopole flux obtained in this work from BLAZAR 1ES 0229+200, depending on the IGMF strength, can be as strong as $F \lesssim 6 \times 10^{-23}\, \text{cm}^{-2} \text{s}^{-1} \text{str}^{-1}$ for low-mass monopoles $m \lesssim 10^6\, \text{GeV}$, stronger than existing laboratory and astrophysical bounds. The bound becomes subdominant to current constraints if the present-day IGMF value is stronger than $B \gtrsim 10^{-12}\, \text{G}$. At the same time, in the case of non-zero monopole abundance, the IGMF lower bound from TeV observations itself should be revised, resulting in a stronger lower bound at higher monopole number density.
[abstract 7 / 64] Wow! (score: 8) - Title: Hunting for extreme high-energy-peaked BL Lacs: Rare to find and difficult to classifyAuthors: Loredana Bassani, Raffaella Landi, Nicola Masetti,Comments: 14 pages, 9 figures, 2 tables; accepted for publication in Journal of High Energy AstrophysicsSubjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
We explore the possible existence of a new population of BL Lacs, called ultra extreme high-energy-peaked BL Lacs (UEHBLs), whose SYNCHROTRON emission component peaks in the MeV band. In particular, we analysed SWIFT/XRT follow-up observations of a set of 10 hard X-ray sources from the SWIFT/BAT catalogues which were suggested to represent the first observational hints of this new BLAZAR population on the basis of their spectral properties. We find that 6 of these candidate UEHBLs can be classified as line-emitting ACTIVE GALACTIC NUCLEi (AGNs), 4 of which are of type 2 and X-ray absorbed objects, while 2 are type 1 AGN and X-ray unabsorbed sources. In one more case, we find that the hard X-ray emission is probably the contribution of two line-emitting AGN, i.e. a Seyfert of type 1.9 and another of type 2. All these 7 classifications exclude the possibility that these hard X-ray sources are extreme BL Lacs. Of the remaining 3 UEHBL candidates, only 2 objects are found to have a spectral energy distribution (SED) compatible with those expected by MeV-peaked BL Lacs: however, in one of these 2 cases, an alternative Galactic association is also possible. The third source is instead likely associated with a more classical quasi-stellar object. Overall, we find that UEHBLs are extremely rare to find and probably very difficult to classify. Nevertheless, they represent a viable alternative classification for hard X-ray sources displaying no obvious or very weak counterparts.
[abstract 8 / 64] Wow! (score: 8) - Title: Exploring Tidal Disruption Events with SKA and VLBI: Unveiling the Mystery of Black Hole Feeding and OutflowsAuthors: Xinwen Shu, Guobin Mou, Tao An, S. Komossa, Miguel Perez-Torres, Weihua Lei, Luming Sun, Ning Jiang, Tinggui Wang, Chichuan Jin, Jun Yang,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Shu01. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Tidal disruption events (TDEs) probe the birth and evolution of BLACK HOLE accretion flows and JETs on human timescales. Radio emission traces shocks and outflows from thermal TDEs and powerful RELATIVISTIC JETs in the rare JETted class. SKA Mid, phased for VLBI and used together with global networks, will deliver milliarcsecond imaging, tens of microarcsecond astrometry, and microJy sensitivity, enabling: (i) proper motion measurements that discriminate off axis RELATIVISTIC JETs from subRELATIVISTIC winds; (ii) resolved morphologies and MAGNETic field diagnostics via polarimetry; and (iii) precise nuclear localization to distinguish SMBH vs. IMBH and to reveal recoiling or binary systems. SKA's wide frequency coverage (0.35 to 15.4 GHz) and 1h continuum sensitivities of 3 to 10 microJy per beam, together with multibeam tiedarray VLBI and a transient buffer for rapid triggers, are transformational. LSST, Einstein Probe, and SVOM will increase TDE alerts to hundreds per year, and late time radio flares appear common, ensuring rich SKA VLBI samples. We provide observing strategies, detection forecasts, and predictions, e.g., about 5 proper motion detections of JETted (or off axis) TDEs per year and routine core shift constraints at the microarcsecond level. This program will establish TDEs as laboratories for exploring JET launching, particle acceleration (including neutrinos), BLACK HOLE accretion history and demographics, and properties of circumnuclear medium.
[abstract 9 / 64] Wow! (score: 7) - Title: Transforming X-ray Binary Astrophysics with SKA+VLBIAuthors: Tao An, Ailing Wang, James C. A. Miller-Jones, Valeriu Tudose, Pikky Atri, Lang Cui, Hua Feng, Benito Marcote, Sara E. Motta,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/TaoAn01Subjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
X-ray binaries (XRBs) are unique laboratories where accretion, JETs, strong gravity and MAGNETic fields can be probed on humanly tractable timescales. The phased SKA-Mid operating as a single, ultra-sensitive Very Long Baseline Interferometry (VLBI) element will transform radio studies of XRBs primarily through its time-domain capabilities: substantially improved sensitivity on VLBI baselines that include SKA-Mid in Bands 2 and 5, together with connected-element SKA-Mid imaging extending down to 0.35--1 GHz (Band 1), microarcsecond-precision astrometry for bright systems, high-fidelity polarimetry for the most strongly polarized sources, and rapid target-of-opportunity response. In synergy with global VLBI networks, SKA+VLBI will track the evolution of compact ejecta and compact JETs on astronomical unit (AU) scales, measure frequency-dependent core shifts to infer MAGNETic field strengths and gradients, resolve disk--JET coupling during state transitions in real time, and determine precise distances and natal kicks via parallaxes and proper motions. Joint campaigns with future X-ray and optical telescopes will enable strictly simultaneous, multi-band constraints on accretion--ejection physics and on JET composition. We outline a quantitative program for \aastar\ and AA4, including cadenced, multi-frequency VLBI ``movies'' of JETs over the first days of outbursts, an XRB astrometric census, and a core-shift survey, and we provide representative detection rates, MAGNETic field measurements and distance accuracies. These outcomes will set the microphysical foundation for JET physics across the mass scale from stellar-mass BLACK HOLEs and neutron stars to ACTIVE GALACTIC NUCLEi, and will establish SKA+VLBI as the definitive facility for time-domain, high-resolution XRB astrophysics.
[abstract 10 / 64] Yes (score: 6) - Title: Feeding and Feedback in Dwarf Galaxies (FeeD) -- I. Evidence of nuclear ultra-fast and galaxy-scale outflows in the dwarf galaxy Arp 151Authors: Santanu Mondal, Ankit Patel, Mar Mezcua, Ravi Joshi, Yerong Xu, K. Aditya, Smitha Subramanian, Victor Rodriguez Morales,Comments: 4 pages, 3 figures, Accepted for publication in A&A LettersSubjects: astro-ph.GA astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Feeding and feedback regulated by supermassive BLACK HOLEs (SMBHs) play a central role in galaxy growth and evolution, yet these processes remain poorly understood in low-mass galaxies. In particular, the presence, properties, and role of ultra-fast nuclear outflows (UFOs) in low-mass galaxy systems are largely unexplored. We analyze available NUSTAR X-ray observations of Arp 151 and find a possible evidence ($\sim 2σ$ confidence) for a fast outflow with a velocity of $\sim0.18c$ from the central BH. Furthermore, we have also detected an optical galaxy-scale outflow in MaNGA Integral Field Unit data. The estimated nuclear and galaxy-scale mass outflow rates are $\sim0.015$ $M_\odot$/yr from {\it NUSTAR} and $\sim0.43$ $M_\odot$/yr from MaNGA, respectively. Our estimates suggest that such outflows may significantly regulate the feedback process in the galaxy. Comparing the kinetics of the UFO and the galaxy-scale outflow indicates that they are in the momentum-conserving phase. This tentative detection implies that dwarf galaxies are also able to generate UFOs, which so far have been detected in massive galaxies. Thus, the AGN feedback may also be important for the evolution of the dwarf galaxies.
[abstract 11 / 64] Yes (score: 5) - Title: Radiation Reaction effects on Coherent Emission in Relativistic Magnetized ShocksAuthors: Yu Zhang, Yuanpei Yang, Liangliang Ji,Comments: 6 pages, 4 figuresSubjects: astro-ph.HE physics.plasm-phCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Relativistic MAGNETized shocks are natural sources of coherent radiation, representing a promising framework for fast radio bursts (FRBs). This study explores how the radiation reaction (RR) effect, triggered by high-energy photon emissions during shock radiation, significantly alters particle dynamics and coherent radiation properties. Using kinetic particle simulations, we demonstrate that RR severely suppresses electron energies from shock acceleration, resulting in multiple coherent gyration cycles at the shock front. It amplifies the intensity of coherent radiation and boosts energy efficiency by several fold, as compared to the single gyration cycle in the standard model of RELATIVISTIC MAGNETized shocks. We further find that the coherent radiation spectrum from RR-mediated shocks is characterized by upshift peak frequency, broaden bandwidth, and narrow spectral peak. These RR-induced radiation changes may be related with several observed FRB phenomena, including the statistically positive correlation between luminosity and bandwidth in repeating and one-off FRBs, the narrow spectra seen in some FRB events, and the bimodal energy distribution reported in FRB 20121102A.
[abstract 12 / 64] Yes (score: 5) - Title: A Minimal Interpretation of the Galactic Cosmic-Ray Proton and Helium Spectra from GeV to PeV EnergiesAuthors: Felix Aharonian, Bing Theodore Zhang,Comments: Accepted for publication in The Astrophysical JournalSubjects: astro-ph.HE astro-ph.SRCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
High-precision measurements of the cosmic-ray (CR) proton and helium spectra have revealed significant deviations from a simple power law, characterized by multiple spectral features, including a hardening above $\sim$100~GeV, a broad excess in the multi-TeV range, and a pronounced structure at PeV energies. We propose a minimal phenomenological two-cosmic-ray-population framework that consistently accounts for the observed spectra of protons and helium across six decades in energy, with agreement at the level of $\sim 10 \%$ or better over most of the explored energy range. In this scenario, the spectral complexity arises from a transition between two Galactic CR populations in the 10~TeV-1~PeV energy range. The low-energy proton population exhibits a sharp cutoff at tens of TeV, while a second, higher-energy population emerges and dominates above 100~TeV, terminating with a smooth exponential cutoff at $\sim$6.5~PeV. The same two-component model applied to CR helium, with a slightly harder first component extending effectively to several hundred TeV and a second component that scales with the proton spectrum in MAGNETic rigidity, provides a consistent description of both the helium spectrum and the p/He ratio. This framework reproduces the main observed spectral features of CR protons and helium without invoking contributions from nearby sources or non-standard assumptions about CR acceleration or propagation. Recent gamma-ray observations of SUPERNOVA remnants, star-forming regions, and microQUASARs offer plausible astrophysical sites for these two CR components.
[abstract 13 / 64] Yes (score: 5) - Title: Pulsar based modeling of point spread function of FERMI Large Area TelescopeAuthors: J. Blunier, A. Neronov, D. Semikoz,Comments: 10 pages, 11 figures, 1 tableSubjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Sensitivity of searches for extended emission around gamma-ray sources is naturally limited by the precision of the knowledge of the Point Spread Function (PSF) of gamma-ray telescopes. Inaccuracies in the PSF models of the FERMI Large Area Telescope (LAT) can potentially lead to false positive detections of source extension. We explore uncertainties in the FERMI/LAT PSF by comparing the PSF models provided by the FERMI/LAT Instrument Response Functions (IRFs) with signals of bright pulsars. We compare the analytical PSF models of FERMI/LAT IRFs with pulsar data and fit the pulsar data with the same analytical model as in the FERMI/LAT IRFs to derive an improved set of PSF parameters. We then apply this revised PSF parameterisation to the search of extended emission around a BLAZAR, Mrk 501. We find that the parameters of the analytical PSF models of FERMI/LAT IRFs are inconsistent with the pulsar data. We obtain an improved set of PSF parameters from the fits to pulsar data that is consistent with observations. We find no evidence of the previously reported extended signal around Mrk 501 if the revised PSF consistent with pulsar data is used in data analysis.
[abstract 14 / 64] Yes (score: 4) - Title: LITMUS: Bayesian Lag Recovery in Reverberation Mapping with Fast Differentiable ModelsAuthors: Hugh McDougall, Tamara M. Davis, Benjamin J. S. Pope,Comments: 17 Pages, 10 FiguresSubjects: astro-ph.GA astro-ph.CO astro-ph.IMCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Reverberation mapping is a technique in which the mass of a Seyfert I galaxy's central supermassive BLACK HOLE is estimated, along with the system's physical scale, from the timescale at which variations in brightness propagate through the galactic nucleus. This mapping allows for a long baseline of time measurements to extract spatial information beyond the angular resolution of our telescopes, and is the main means of constraining supermassive BLACK HOLE masses at high redshift. The most recent generation of multi-year reverberation mapping campaigns for large numbers of ACTIVE GALACTIC NUCLEi (e.g. OzDES) have had to deal with persistent complications of identifying false positives, such as those arising from aliasing due to seasonal gaps in time-series data. We introduce LITMUS (Lag Inference Through the Mixed Use of Samplers), a modern lag recovery tool built on the "damped random walk" model of QUASAR variability, built in the autodiff framework JAX. LITMUS is purpose built to handle the multimodal aliasing of seasonal observation windows and provides evidence integrals for model comparison, a more quantified alternative to existing methods of lag validation. LITMUS also offers a flexible modular framework for extending modelling of AGN variability, and includes JAX-enabled implementations of other popular lag recovery methods like nested sampling and the interpolated cross correlation function. We test LITMUS on a number of mock light curves modelled after the OzDES sample and find that it recovers their lags with high precision and a successfully identifies spurious lag recoveries, reducing its false positive rate to drastically outperform the state of the art program JAVELIN. LITMUS's high performance is accomplished by an algorithm for mapping the Bayesian posterior density which both constrains the lag and offers a Bayesian framework for model null hypothesis testing.
[abstract 15 / 64] 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: 2026-06-26; Datestamp: 2026-06-26
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 16 / 64] Yes (score: 4) - Title: Relativistic Tidal Dissipation and the Gravitational-wave Signal of a White Dwarf Orbiting an Intermediate-Mass Black HoleAuthors: Yang Yang, Leif Lui, Alejandro Torres-Orjuela, Xian Chen,Comments: 14 pages, 9 figuresSubjects: astro-ph.HE gr-qcCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Finding intermediate-mass BLACK HOLEs (IMBHs) and measuring their masses and spins are key to understanding massive BLACK HOLE formation. White dwarf (WD)-IMBH binaries provide a unique probe because they emit both electroMAGNETic radiation and gravitational waves (GWs), thereby conveying richer information. However, such multi-messenger sources often enter the regime of strong gravity, where existing models fail to capture their RELATIVISTIC dynamics. Here, we develop a fully RELATIVISTIC model for the tidal response of a WD close to an IMBH and use it to study the secular orbital evolution as well as the GW signal. We find that for IMBHs more massive than 10^5 solar masses, tidal interaction becomes RELATIVISTIC and sensitive to IMBH spin. The interaction generally dissipates binary orbital energy and angular momentum, but due to RELATIVISTIC frame rotation, which reduces phase coherence across pericenter passages, the orbit-averaged tidal dissipation rate can be suppressed by up to about 50% relative to Newtonian predictions. Including tidal dissipation leads to more rapid damping of the orbital eccentricity, to the extent that the pericenter distance may even increase over time, potentially explaining quasi-periodic eruptions and secular orbital period growth. Such tidal effects accumulate into measurable phase and amplitude deviations in the GW signal. For typical space-based observations, the GW waveform mismatch can reach values of order 0.1 within 6 months. Our results indicate that RELATIVISTIC tidal dissipation is both dynamically important and observationally essential for reliably predicting the multi-messenger signals of WD-IMBH systems.
[abstract 17 / 64] Yes (score: 4) - Title: A JET formation model for astrophysical objectsAuthors: Chun Xu,Comments: 7 pages,1 figure; Accepted for publication in MNRASSubjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
We propose a unified model for JET formation applicable to ACTIVE GALACTIC NUCLEi, young stellar objects, and X-ray binaries. In this model, the binding energy released from the accretion disk is primarily stored as turbulence rather than being radiated away, leading to the formation of advection-dominated accretion flows. Near the central object, a thick accretion disk with funnel-like structures develops. Within the turbulent flows, the smallest stable blobs can be accelerated beyond the escape velocity through the combination of two mechanisms - the Gaussian-like velocity distribution within the turbulence and a mechanism involving the combined effects of inward pressure force and angular momentum conservation.These rapidly moving blobs may exit through the funnels, collectively forming two opposing JETs. This model predicts that JETs originate from the innermost region of the thick disk surrounding the central object. The formation of JET is directly related a parameter ηthat describes the energy fraction stored in turbulence in units of the binding energy of local Keplerian energy. η> 0.5 is a minimal condition for JET to form. This model can be extended to account for JET formation in ACTIVE GALACTIC NUCLEi, young stellar objects, X-ray binaries, and other analogous astronomical systems.
[abstract 18 / 64] Yes (score: 4) - Title: A Census of Variable and Transient Radio Sources Within High-Energy Neutrino FieldsAuthors: Florian Rösch, Matthias Kadler, Roger P. Deane, Philip G. Edwards, Karl Mannheim, Jack F. Radcliffe,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no: AASKAII/Rosch01. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.HECreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
The origin of high-energy cosmic neutrinos detected by the IceCube observatory is a hotly debated topic in astroparticle physics. Neutrinos can be produced via interactions of high-energy protons with photons. There are multiple candidate source classes which can accelerate cosmic particles to the energies required to emit high-energy cosmic neutrinos and which have in common that they lead to variable/transient radio emissions. However, so far only a few ACTIVE GALACTIC NUCLEi (AGNs) could be associated with high confidence with IceCube neutrinos. The bulk of the diffuse neutrino flux might be emitted from a rather faint and numerous source population. The sub-mJy low-frequency radio sky may harbor these neutrino emitters that have gone unnoticed in previous searches. SKA-Mid continuum observations of high-energy neutrino fields will yield the most complete census of coincident transient and variable radio sources that might be associated with the neutrino emission. In previous MeerKAT observations of the IceCube gold alert IC240929A at 815 MHz, we detect about 550 faint radio sources inside the 90% uncertainty region of this neutrino field with flux densities between $169\,\mathrm{μJy}$ and $140\,\mathrm{mJy}$. In its AA4 configuration, SKA-Mid will achieve about four times the sensitivity of MeerKAT, allowing for the detection of even fainter radio sources within such neutrino fields. By adding wide-field VLBI analysis of the fields under consideration, all neutrino-candidate radio sources can be tested for high brightness-temperature compact emission (indicative of an AGN classification) and milliarcsecond-scale resolved structures.
[abstract 19 / 64] Yes (score: 4) - Title: Long-Period Transients as a new frontier in time-domain astronomyAuthors: Manisha Caleb, Dougal Dobie, Natasha Hurley-Walker, Yogesh Maan, Yuan Mao, Hao Qiu, Nanda Rea, Kovi Rose, Iris de Ruiter, Ben Stappers, Ziteng Wang,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366) Report-no: AASKAII/Qiu01 On behalf of the SKA Transients Science Working GroupSubjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Long-period radio transients (LPTs) are relatively new astrophysical objects occupying the observational gap between canonical pulsars and slowly varying radio variables. They emit coherent, highly polarised radio bursts with periods from minutes to hours, often exhibiting millisecond- to minute-scale substructure, short duty cycles, and broadband emission. Their radio luminosities typically exceed what rotational energy alone can power, necessitating alternative energy sources such as MAGNETic field decay, MAGNETospheric RECONNECTion, or binary interactions. As multiwavelength counterparts in X-ray, optical, and infrared bands provide key constraints on progenitors and emission mechanisms, observational evidence points to a diverse progenitor population including ultra-long period MAGNETars and MAGNETic white dwarf binaries. Fast imaging surveys with SKAO and its precursors are opening a new discovery space, enabling systematic detection, high-cadence monitoring, and detailed follow-up. Despite the challenges of high extinction, intermittent emission, and computational demands for discovery, the expanding LPT population provides a new laboratory for studying coherent radio emission in a range of compact-object systems, from pulsars to white dwarf binaries. This diversity allows us to test how the emission processes depend on MAGNETic field strength, rotation, and binary interaction.
[abstract 20 / 64] Yes (score: 4) - Title: A Boundary-Consistent Two-Zone Electron Kernel for Distant Pulsar Contributions to Positron Flux and AnisotropyAuthors: Yiwei Bao, Jie-Shuang Wang, Hao Zhou,Comments: submittedSubjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
We present a semi-analytical series solution for electron and positron propagation in a spherical two-zone diffusion model. The solution treats slow diffusion inside a near-source region and standard interstellar diffusion outside it, while SYNCHROTRON and Klein--Nishina inverse-Compton cooling are included through energy characteristics. The formulation avoids the oscillatory cancellations of direct two-zone integral evaluations and preserves the sharp radiative cooling boundary seen in finite-volume checks. We apply the kernel to pulsar contributions to the local cosmic-ray lepton flux. Nearby pulsars remain natural candidates near the TeV cutoff, but at tens to hundreds of GeV the larger source volume allows more distant pulsars to contribute collectively: for a disk half-thickness of $0.2\,{\rm kpc}$, sources beyond $1\,{\rm kpc}$ can still provide $37$--$47\%$ of the $10$--$100\,{\rm GeV}$ flux. Comparing with AMS-02 positron data and all-electron anisotropy limits, and imposing an inner $100\,{\rm pc}$ cavity motivated by the Local Bubble and pulsar proper motions, we find that Geminga-scale slow-diffusion halos remain compatible with current data. The fitted pulsar component is dominated by sources beyond $0.3\,{\rm kpc}$, but flux and anisotropy data alone do not uniquely determine the halo size; external information such as TeV halo morphology is still required.
[abstract 21 / 64] Yes (score: 4) - Title: Unraveling the mysteries of SUPERNOVAe with SKA+VLBIAuthors: Tao An, Zhengwei Liu, Ailing Wang, Miguel Pérez-Torres, Javier Moldon, Liangduan Liu, Peter Lundqvist, Xuefei Chen, Xiangcun Meng,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/TaoAn02Subjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Supernovae (SNe) drive cosmic chemical enrichment and shape galactic feedback, yet the link between progenitors and explosion outcomes remains poorly constrained because the earliest phases are rarely resolved. Radio emission traces SYNCHROTRON radiation where the fastest ejecta interact with the circumstellar medium (CSM), providing a uniquely penetrating probe of these phases. SKA-Mid phased into global VLBI will move from simple detections to routine interferometric imaging of nearby extragalactic SNe. Sub-$μ$Jy sensitivity and mas-scale SKA+VLBI imaging, complemented by visibility-domain model fitting for sub-beam radius measurements at 5-15 GHz will allow us to follow the expanding shocks of stripped-envelope SNe out to $\sim$25 Mpc, measure deceleration indices ($m$) and axial ratios to $\approx 5-10\%$, and directly test JET-assisted versus neutrino-driven explosion mechanisms. For interacting SNe (Type IIn/Ibn), SKA+VLBI will resolve clumpy and toroidal CSM on progenitor scales, constraining the timing and geometry of eruptive pre-explosion mass loss. Deep limits on Type Ia SNe will tightly restrict the allowed single-degenerate parameter space, while late-time imaging will search for nascent compact remnants and pulsar wind nebulae. In synergy with optical, X-ray and gravitational wave facilities, SKA+VLBI will turn nearby SNe into laboratories for time-resolved shock physics and progenitor mapping.
[abstract 22 / 64] Yes (score: 4) - Title: Optical observations of candidate host galaxies of eight fast X-ray transientsAuthors: Agnes P. C. van Hoof, Peter G. Jonker, Lieke Tommel, Jonathan A. Quirola-Vásquez, Daniel Mata Sánchez, Joyce N. D. van Dalen, Andrew J. Levan, Morgan Fraser, Ann Zabludoff, Manuel A. P. Torres, Javi Sánchez-Sierras, Antonio Martin-Carrillo, Thomas Wevers, Marco Berton, Minghao Yue, Vik S. Dhillon, Franz E. Bauer, Stuart P. Littlefair,Comments: 17 pages, 9 figures and 5 tables. Version accepted by A&ASubjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Fast X-ray transients (FXTs) are extragalactic flashes of X-rays with a typical duration of minutes to hours for which a variety of origins has been proposed and observed. To decipher the origin of FXTs, particularly those lacking multi-wavelength counterparts, we aim to understand their energetics and environments. We present deep optical ground-based observations of the positions of eight FXTs in order to try and identify and characterize candidate host galaxies. We use their properties to discriminate between possible progenitor scenarios. We identify candidate host galaxies for SWIFT~J050400.2+673405, XRT140507, XRT040610, XRT151121, XRT191127 and EP240708a. For each candidate, we infer the spectroscopic or photometric redshift, stellar mass, STAR FORMATION rate, metallicity and stellar population age by fitting our data with the spectral energy distribution fitting code BAGPIPES. We re-identify XRT191223 as a Galactic stellar flare. For several FXTs, there are multiple candidate host galaxies, which complicates deriving constraints on the origin of the FXT. Assuming association with (one of) those candidates, all are consistent with a (non-)RELATIVISTIC white dwarf - intermediate mass BLACK HOLE tidal disruption event (WD-IMBH TDE) and a binary neutron star (BNS) merger. Two are consistent with a SUPERNOVA shock breakout and only EP240708a with cocoon emission from a long GAMMA-RAY BURST. We also discuss the possibility that the host galaxies remain undetected in our observations. We conclude that FXTs detected by Chandra and XMM-Newton are likely to arise from a variety of origins, and we discuss that part of this population differs from FXTs detected by Einstein Probe many of which appear consistent with a collapsar scenario.
[abstract 23 / 64] Yes (score: 4) - Title: HALO II: Constraining Hubble constant $H_{0}$ through continuum delay fitting of Fairall 9Authors: Amit Kumar Mandal, Francisco Pozo Nuñez, Vikram Kumar Jaiswal, Mohammad Hassan Naddaf, Bożena Czerny, Swayamtrupta Panda, Paulina Karczmarek, Grzegorz Pietrzyński, Shivangi Pandey, R. Edelson, B. M. Peterson, Michal Zajaček, Alberto Floris, Mary Loli Martínez-Aldama, Michal Dovčiak, Vladimir Karas, Weronika Narloch, Mirosław Kicia, Marek Górski, Mikołaj Kałuszyński, Gergely Hajdu, Piotr Wielgórski, Bartłomiej Zgirski, Cezary Gałan, Wojciech Pych, Radosław Smolec, Ricardo Salinas, Henryka Netzel-Iłkiewicz, Karolina Bąkowska, Wolfgang Gieren, Pierre Kervella,Comments: Submitted to A&A, 19 pages, 11 figures, and 2 tablesSubjects: astro-ph.GA astro-ph.CO gr-qc hep-ph hep-thCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
The Hubble tension remains one of the most significant unresolved problems in modern cosmology. A key question is whether it may arise from underestimated systematic uncertainties in the different measurement techniques. In this context, new independent methods are of exceptional importance. We therefore pursue a novel approach to determining the Hubble constant, $H_{0}$ based on continuum time delay and spectral energy distribution (SED) modeling in ACTIVE GALACTIC NUCLEi (AGNs). Unlike conventional techniques, this method is entirely independent of the cosmic distance ladder and does not require cross-calibration against other distance indicators. As a result, it enables a direct determination of $H_{0}$, free from the arbitrary normalizations that often affect indirect measurements. We conducted a dedicated monitoring campaign of the Seyfert galaxy Fairall 9 and further developed the {\tt H0RIZON-AGN} model to interpret the resulting observations. The model incorporates the effects of radiation reprocessing in the surrounding cold accretion disk, enabling a more realistic description of the observed continuum delays. Through the simultaneous modeling of the continuum lag-spectrum and the broadband SED of Fairall 9, we derived a Hubble constant of $H_{0}=72.4_{-3.7}^{+3.4} \, \rm km \, s^{-1} \, Mpc^{-1}$. Achieving a measurement precision of approximately 5% from a single source demonstrates the considerable potential of this method for independent determinations of the Hubble constant. Our determination of $H_{0}$ is broadly consistent, within the current uncertainties, with both early- and late-Universe measurements. Future applications of the method to larger datasets, particularly those provided by the Vera Rubin Observatory, are expected to reduce the uncertainty to below 1%, thereby establishing this approach as a powerful independent probe of the Hubble tension.
[abstract 24 / 64] (score: 3) - Title: A pipeline to search for signatures of line-of-sight acceleration in gravitational wave signals produced by compact binary coalescencesAuthors: Avinash Tiwari, Aditya Vijaykumar, Shasvath J. Kapadia, Shrobana Ghosh, Alex B. Nielsen,Comments:Subjects: astro-ph.HE gr-qcCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Compact binary coalescences (CBCs), such as merging binary BLACK HOLEs (BBHs), binary neutron stars (BNSs), or neutron star BLACK HOLEs (NSBHs), hosted by dense stellar environments, could produce gravitational waves (GWs) that contain signatures of line-of-sight acceleration (LOSA) imparted by the environment's gravitational potential. We calculate the Post-Newtonian (PN) corrections to the $(2,\,2)$ mode GW phase due to a finite LOSA, starting from the leading order at -4 PN below the quadrupole order, up to 3.5 PN above the leading order correction. We do so for binaries whose component spins are aligned with the orbital angular momentum, as well as for binaries with non-zero tidal deformation. We implement these corrections into the LIGO-Virgo-Kagra (LVK) collaboration's flagship parameter estimation (PE) software Bilby_tgr. We study the systematics associated with recovering LOSAs. We find that, when the injection and recovery waveform models are identical, LOSAs are recovered as expected. We test the robustness of the pipeline against waveforms with strong higher-mode signatures or signatures of beyond-general-RELATIVISTIC (beyond-GR) effects, to delimit the range of applicability of our GR-consistent quasi-circular LOSA-corrected waveforms.
[abstract 25 / 64] (score: 3) - Title: Solitary Alfvén WavesAuthors: Zesen Huang, Marco Velli, Chen Shi, Yuliang Ding,Comments: Accepted by ApJLSubjects: astro-ph.SR astro-ph.HE physics.plasm-ph physics.space-phCreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
We present the solitary Alfvén wave as an ideal nonlinear Alfvénic solution in the solitary far-field limit and construct a three-dimensional numerical model -- an \emph{Alfvénon}. The model is characterized by an unperturbed far field, quasi-constant $|\boldsymbol{B}|$, and open field-line topology. Direct MHD simulations of the Alfvénon show coherent finite-time propagation, confirming that it behaves as a nonlinear solitary Alfvénic solution under ideal MHD evolution.
[abstract 26 / 64] (score: 3) - Title: Evaluation of the beam-induced dePOLARIZATION of the HJET target at the EICAuthors: A. A. Poblaguev,Comments: 18 pages, 11 figures, 5 tablesSubjects: physics.ins-det physics.acc-phCreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
The Polarized Atomic Hydrogen Gas Jet Target (HJET) has played a central role in the absolute calibration of proton beam POLARIZATION at RHIC and is foreseen as a key component of the hadron polarimetry program at the future Electron--Ion Collider (EIC). The substantially higher beam current, reduced bunch spacing, and shorter bunch length planned for EIC operation motivate a careful reassessment of possible beam-induced dePOLARIZATION of the JET target. In this paper, the dePOLARIZATION of ground-state hydrogen atoms caused by the time-dependent MAGNETic field of the circulating polarized proton beam is quantitatively evaluated. The hydrogen atom is treated as a four-level hyperfine system in a holding MAGNETic field, and transitions driven by harmonic components of the bunch-induced MAGNETic field are analyzed using time-dependent quantum-mechanical evolution along atomic trajectories. Numerical tracking of hydrogen atoms through the beam region is performed using nominal EIC beam parameters. It is shown that, for a holding field of $120 \mathrm{mT}$ (as used at RHIC), the resulting dePOLARIZATION of the JET target at the EIC is negligibly small, $\lesssim 0.01\%$, and well below the level relevant for EIC POLARIZATION accuracy requirements. The stability of this result with respect to plausible variations of the EIC proton beam parameters is also evaluated. In addition, possible effects under alternative experimental conditions are also examined.
[abstract 27 / 64] (score: 3) - Title: 3D Kinematic Reconstruction of the Crab Nebula That Includes the Northern Ejecta `Jet'Authors: Ziwei Ding, Dan Milisavljevic, Thomas Martin, Tea Temim, John C. Raymond, Soham Mandal, Laurent Drissen,Comments: 23 pages, 15 figures. Submitted to ApJ. Animations available at https://doi.org/10.5281/zenodo.20822317Subjects: astro-ph.HECreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
We present new detailed three-dimensional kinematic reconstructions of the Crab Nebula created from hyperspectral cubes obtained with the SITELLE instrument mounted on the Canada--France--Hawaii Telescope. Our data cubes span a wavelength range from 3600Å to 7000Å, covering major emission lines including [O II] $λλ$3726, 3729, H$β$, [O III] $λλ$4959, 5007, [N II] $λ$5755, He I $λ$5876, [N II] $λλ$6548, 6584, [S II] $λλ$6717, 6731, and H$α$. The field of view encompasses the ``chimney" or ``JET," a 45-arcsec-wide funnel-shaped structure that extends 100 arcsec beyond the northern limb of the nebula. Our 3D reconstructions confirm and geometrically resolve a cavity at the JET's base that was suggested by earlier kinematic studies, establishing a direct physical connection between the filamentary network and the JET funnel. The morphology and kinematics indicate that the early pulsar wind nebula (PWN) played a central role in forming the JET. Several formation scenarios, which are not necessarily mutually exclusive, remain viable, including a bipolar outflow shaped by a circumstellar disk, a breach or underdensity in the ejecta shell, and a pre-existing progenitor mass-loss trail acting as a low-density channel. Collectively, these scenarios exhibit differing abilities to account for the JET's pronounced collimation, the absence of a southern counterpart, and its near-ballistic motion. Discriminating among them will require fully three-dimensional hydrodynamic simulations that trace the remnant's evolution from the progenitor phase through late-time PWN expansion.
[abstract 28 / 64] (score: 3) - Title: Wind Acceleration as a Driver of Detached Blueshifted Absorption in Quasar Disk WindsAuthors: Randall C. Dannen, Daniel Proga, Paola Rodríguez Hidalgo, Kara Smith, Anna Ritchie, Liliana Flores, Morrigan Kalet,Comments: 1 Table, 4 FiguresSubjects: astro-ph.GACreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
Active galactic nuclei (AGN) unification models often emphasize the viewing angle, $i$, but $i$ alone does not determine QUASAR properties. This is crucial for QUASAR outflows: UV absorption in Extremely High Velocity Outflow (EHVO) QUASARs can reach blueshifted velocities of $\sim0.2~c$. In disk-wind models, both $i$ and internal wind structure shape the emergent spectrum. We test their interplay using biconical QUASAR disk-wind models with different acceleration lengths, $R_v$, and generate synthetic spectra over a range of $i$. We use Monte Carlo radiative transfer to account for finite continuum sources, wind attenuation, scattering, reprocessing, and emission. Changing $R_v$ greatly alters the ionization structure, continuum shape, and absorption-line profiles. At intermediate viewing angles, sightlines pass through the fastest wind. Even there, highly detached and blueshifted \CIV\ absorption like that observed in EHVO QUASARs appears only in models with small $R_v$. In these models, the gas reaches high velocity before attaining the ionization and density conditions favorable for \CIV. Models with larger $R_v$ instead produce broader, less detached troughs, even when the terminal velocity is very high. Thus, highly detached and blueshifted absorption requires both a high terminal velocity and small $R_v$, making such features diagnostics of disk-wind acceleration and structure. EHVO QUASARs provide a clear example, but the same principle applies more broadly to highly detached and blueshifted absorption in QUASAR outflows. Our results support an extended disk-wind view of AGN unification: $i$ selects the observed wind region, while $R_v$ shapes the emergent spectrum and absorption morphology.
[abstract 29 / 64] (score: 3) - Title: Integrating Gyrokinetic Flux Predictions with Ideal MHD Stability BoundariesAuthors: J. McClenaghan, K. E. Thome, T. F. Neiser, J. Candy, F. D. Halpern, T. H. Osborne, S. Saarelma, the MAST-U team,Comments:Subjects: physics.plasm-phCreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
Accurate prediction of pedestal height and width in tokamaks remains a critical issue as it strongly influences the predicted plasma performance of all future reactors. We present an integrated pedestal-stability workflow that combines equilibrium scans with MAGNETohydrodynamic (MHD) stability analysis using ELITE and GATO and gyrokinetic transport predictions using CGYRO/QLGYRO. The workflow reproduces the characteristic KBM first- and second-stability structure previously identified in gyrokinetic pedestal studies. Applied to spherical tokamaks (STs), the workflow shows good agreement with past studies when low-n peeling stability is included, emphasizing the importance of resolving low-n physics in ST pedestals. Extending the analysis to SPARC-like, high toroidal field plasmas, kinetic ballooning mode (KBM) and microtearing mode (MTM) heat fluxes are found to increase strongly with toroidal field, suggesting that access to the KBM second-stability region may become significantly more difficult in high toroidal field devices. Comparison with global ELITE finite-n analysis at SPARC parameters suggests that the H-mode pedestal lies in an intermediate regime bounded by local KBM second stability on one side and global finite-n ballooning instability on the other, consistent with the EPED picture once global effects are included
[abstract 30 / 64] (score: 3) - Title: Identification of MHD equilibrium $β$ limits for CFQS plasmasAuthors: Jian Zhang, Ping Zhu, Haifeng Liu, Yasuhiro Suzuki, Chris C. Hegna, Yuhong Xu,Comments: 32 pages, 18 figuresSubjects: physics.plasm-phCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
The MAGNETohydrodynamic (MHD) equilibrium $β$ limits in the Chinese First QuasiAxisymmetric Stellarator (CFQS) are investigated using the NTEC code, for both the standard and the MAGNETic island configurations. The equilibrium $β$ limit is identified upon the onset of the rapid destruction of nested flux surfaces by evaluating several numerical metrics, including the fractal dimension, weighted Birkhoff average, and effective volume of parallel diffusion. In the standard configuration, the net-current-free and the bootstrap-current-carrying equilibria can sustain well-ordered MAGNETic surfaces up to $\langleβ\rangle\approx1.5\%$. The proliferation of stochastic field lines starts after the critical overlap between the internal major islands and the high-order island chains. Two types of divertor island configurations are studied based on net-current-free equilibria. It is found that the edge islands may transition into open field lines at low $\langleβ\rangle$ values and lead to a drastic shrinkage of the last closed flux surface. Meanwhile, the threshold $\langleβ\rangle$ value of the degradation of inner flux surfaces is similar to the standard configuration.
[abstract 31 / 64] (score: 3) - Title: Supernova remnants in the new radio astronomy eraAuthors: A. Ingallinera, M. Arias, G. Castelletti, C. Bordiu, F. Bufano, G. Cosentino, M. D. Filipović, D. Liu, S. Loru, S. Orlando, O. Petruk, Z. Smeaton, A. Traficante, C. Trigilio, G. Umana, G. Anderson, F. Bocchino, C. Buemi, F. Cavallaro, E. Egron, N. Hurley-Walker, R. Kothes, P. Leto, S. Mantovanini, M. Miceli, G. Morlino, A. Pellizoni, M. Sasaki,Comments: Published in Advancing Astrophysics with the SKAII (AASKAII), 2026(arXiv:2606.20366). Report-no: AASKAII/Ingallinera01Subjects: astro-ph.HE astro-ph.GA astro-ph.SRCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Supernova remnants (SNRs) are what is left after stellar explosions, when the stellar ejecta, the explosion shock and the circumstellar medium interact. Despite being among the first objects studied in radio astronomy, observational difficulties have so far prevented a definitive characterisation, which would help answer open questions related to these sources. It is debated which is the contribution of SNRs to Galactic COSMIC RAYs, or how the interaction with the surrounding environments influences the particle energetics. The SKA precursors are providing valuable and unexpected discoveries on SNRs, thanks to their unique capabilities to probe spatial scales from a few arcseconds to a few degrees with a sensitivity of tens of microjansky. Accurate integrated flux density measurements and arcsecond-scale spectral-index maps are now possible for tens of SNRs, substantially expanding the small subset of remnants traditionally studied in great detail. SKA will markedly enhance current observations by providing: higher sensitivity, enabling the detection of fainter SNRs also in polarisation, revealing diffuse structures and the underlying MAGNETic field configuration; higher angular resolution, allowing detailed mapping of compact remnants and reducing depolarisation in fine structures, tracing filaments and shocks fronts; wider frequency coverage to probe unexplored spectral windows, where spectral turnovers and breaks or cut-off may occur, establishing a direct connection to X-ray and γ-ray emission that constrains the electron population, and enabling accurate modelling of the non-thermal emission across the electroMAGNETic spectrum; improved image fidelity for more reliable cross-matching with other wavelengths, leading to a better understanding of the SNR-interstellar medium interplay.
[abstract 32 / 64] (score: 3) - Title: Clustering of high-redshift QUASARs with DESI DR2Authors: M. Charles, P. Martini, A. J. Ross, D. H. Weinberg, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, C. Hahn, H. K. Herrera-Alcantar, K. Honscheid, C. Howlett, M. Ishak, R. Joyce, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, A. D. Myers, S. Nadathur, N. Palanque-Delabrouille, W. J. Percival, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou,Comments: 44 pages, 15 figuresSubjects: astro-ph.COCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
We present clustering measurements for high-redshift QUASARs using data from the Dark Energy Spectroscopic Instrument Data Release 2. Our sample consists of QUASARs with $2.0 < z < 3.5$ in the luminosity range $M_{1450} \leq -19.94$\,mag. We measure the mean QUASAR bias $b_Q(\bar{z} = 2.48) = 3.61 \pm 0.01$ for the full sample of $\sim 715,000$ QUASARs and quantify the redshift evolution of QUASAR bias by dividing the sample into four equal redshift bins. There is strong evolution of the QUASAR bias with redshift that is well fit by the function $b_Q(z) = a [(1 + z)^2 - 6.565] + b$ with $a=0.230 \pm 0.007$ and $b=2.394 \pm 0.035$, and this fit is also a good match to lower redshift measurements in the literature. This bias evolution is consistent with a characteristic halo mass of $\bar{M}_{\mathrm{h}} \sim 10^{12}\,\mathrm{M_\odot}$ that does not vary significantly with redshift. The inferred duty cycles for QUASARs in our sample are $f_{\mathrm{duty}} \sim 10^{-2}$, staying mostly constant over redshifts. We investigate the luminosity dependence of QUASAR clustering by dividing each of our four redshift bins into three luminosity bins. The size of our QUASAR sample permits the first statistically significant measurement of the luminosity dependence of QUASAR bias at these redshifts. We measure weak dependence of QUASAR bias on luminosity at fixed redshift, inconsistent with no dependence, but weaker than predicted by a model in which QUASAR luminosity is tightly correlated with halo mass. These clustering measurements provide a stringent test for models of active BLACK HOLE light curves and the BLACK HOLE-halo connection at high redshift.
[abstract 33 / 64] (score: 2) - Title: EMU: Cross-correlating EMU Pilot Survey 1 with Dark Energy Survey to validate the RADIO GALAXy bias and redshift distributionAuthors: Chandra Shekhar Saraf, David Parkinson, Jacobo Asorey, Catherine L. Hale, Benedict Bahr-Kalus, Maciej Bilicki, Stefano Camera, Andrew M. Hopkins, Konstantinos Tanidis,Comments: 18 pages, 8 figures, 5 tables. Prepared for submission to PASASubjects: astro-ph.CO astro-ph.GACreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Radio continuum galaxy surveys can provide a relatively fast map of the projected distribution of structure in the Universe, at the cost of lacking information about the radial distribution. We can use these surveys to learn about the growth of structure and the fundamental physics of the Universe, but doing so requires extra information to be provided in the modelling of the redshift distribution, $dN/dz$. In this work, we show how the cross-correlation of the two-dimensional radio continuum map with another galaxy map (in this case a photometric optical extragalactic survey), with a known redshift distribution, can be used to determine the redshift distribution through statistical inference. We use data from the Evolutionary Map of the Universe (EMU) Pilot Survey 1 and cross-correlate it with optical data from the Dark Energy Survey to fit the parameters of our $dN/dz$ model. We show that the recovered distribution has a similar shape to the distribution predicted by the current state-of-the-art simulation, and can fit the angular power spectrum data from cross-correlations very well, validating this model. These results will have significance for future cosmological analyses with large-scale radio continuum surveys such as the full EMU, or with the SKAO.
[abstract 34 / 64] (score: 2) - Title: Constraints on the MAGNETic field evolution in tokamak power plantsAuthors: Allen H Boozer,Comments:Subjects: physics.plasm-phCreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
Forty-five years ago a coordinate system was shown to exist that gave simple but exact expressions whenever and wherever a toroidal plasma equilibrium $\vec{\nabla}p=\vec{j}\times\vec{B}$ exists. These coordinates, now called Boozer coordinates, which revolutionized the stellarator program, are also applicable to tokamaks. Here expressions for Faraday's Law, the safety factor, and the internal inductance are derived. Their constraints should be useful in the design of tokamak power plants and for the thoughtful allocation of resources to minimize the time and the cost to the achievement of practical fusion power. Simple explanations are obtained for (1) why disruptions in tokamaks are so common, (2) why current-profile control though difficult may be required, especially during plasma shutdowns, and (3) why only pulsed tokamaks seem possible. Lack of familiarity with Boozer coordinates can make simple but exact expressions appear naive. Complicated derivations with dubious assumptions have been interpreted as ``more rigorous.''
[abstract 35 / 64] (score: 2) - Title: Testing the nature of GW200105 by probing the frequency evolution of eccentricityAuthors: Avinash Tiwari, Sajad A. Bhat, Md Arif Shaikh, Shasvath J. Kapadia,Comments:Subjects: astro-ph.HE gr-qcCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
GW200105 is a compact binary coalescence (CBC) event, consisting of a neutron star and a BLACK HOLE, observed in LIGO-Virgo-KAGRA's (LVK's) third observing run (O3). Recent reanalyses of the event using state-of-the-art waveform models have claimed observation of signatures of an eccentric orbit. It has nevertheless been pointed out in the literature that certain physical or modified gravity effects could mimic eccentricity by producing a spurious non-zero eccentricity value, at a given reference frequency, when recovered with an eccentric waveform model. We recently developed a waveform-model-independent Eccentricity Evolution Consistency Test (EECT, S. A. Bhat et al. 2025) to identify such mimickers, by comparing the measured frequency $\textit{evolution}$ of eccentricity, $e(f)$, with that expected from General Relativity (GR). In this $\textit{paper}$, we apply EECT to GW200105 and find that it satisfies EECT within 68% confidence. Our analysis therefore lends complementary support in favour of the eccentricity hypothesis, while also providing a novel test of the consistency of $e(f)$ with GR.
[abstract 36 / 64] (score: 2) - Title: Search for Diffuse Supernova Neutrino Background with 956.2 days of Super-Kamiokande Gadolinium DatasetAuthors: K. Abe, S. Abe, Y. Asaoka, M. Harada, Y. Hayato, K. Hiraide, K. Hosokawa, T. H. Hung, K. Ieki, M. Ikeda, J. Kameda, Y. Kanemura, Y. Kataoka, S. Miki, S. Mine, M. Miura, S. Moriyama, M. Nakahata, S. Nakayama, Y. Noguchi, G. Pronost, K. Sato, H. Sekiya, R. Shinoda, M. Shiozawa, Y. Suzuki, A. Takeda, Y. Takemoto, H. Tanaka, T. Yano, Y. Itow, T. Kajita, R. Nishijima, K. Okumura, T. Tashiro, T. Tomiya, X. Wang, P. Fernandez, L. Labarga, D. Samudio, B. Zaldivar, C. Yanagisawa, E. Kearns, L. Wan, T. Wester, B. W. Pointon, J. Bian, B. Cortez, N. J. Griskevich, Y. Jiang, M. B. Smy, H. W. Sobel, V. Takhistov, A. Yankelevich, J. Hill, M. C. Jang, S. H. Lee, D. H. Moon, R. G. Park, B. S. Yang, B. Bodur, K. Scholberg, C. W. Walter, A. Beauch'ene, E. Le Bl'evec, O. Drapier, A. Ershova, M. Ferey, Th. A. Mueller, A. D. Santos, P. Paganini, C. Quach, R. Rogly, T. Nakamura, J. S. Jang, R. P. Litchfield, L. N. Machado, F. J. P. Soler, J. G. Learned, K. Choi, S. Cao, L. H. V. Anthony, N. W. Prouse, M. Scott, Y. Uchida, V. Berardi, N. F. Calabria, M. G. Catanesi, N. Ospina, E. Radicioni, A. Langella, G. De Rosa, G. Collazuol, M. Feltre, M. Mattiazzi, L. Ludovici, M. Gonin, L. P'eriss'e, B. Quilain, S. Horiuchi, A. Kawabata, M. Kobayashi, Y. M. Liu, Y. Maekawa, Y. Nishimura, R. Akutsu, M. Friend, T. Hasegawa, Y. Hino, T. Ishida, T. Kobayashi, M. Jakkapu, T. Matsubara, T. Nakadaira, Y. Oyama, A. Portocarrero Yrey, K. Sakashita, T. Sekiguchi, T. Tsukamoto, N. Bhuiyan, G. T. Burton, F. Di Lodovico, J. Gao, T. Katori, R. Kralik, N. Latham, R. M. Ramsden, H. Ito, T. Sone, A. T. Suzuki, Y. Takeuchi, S. Wada, H. Zhong, J. Feng, L. Feng, S. Han, J. Hikida, J. R. Hu, Z. Hu, M. Kawaue, T. Kikawa, T. Nakaya, T. V. Ngoc, R. A. Wendell, S. J. Jenkins, N. McCauley, A. Tarrant, M. Fan`i, M. J. Wilking, Z. Xie, Y. Fukuda, H. Menjo, Y. Yoshioka, J. Lagoda, M. Mandal, J. Zalipska, M. Mori, J. Jiang, K. Hamaguchi, H. Ishino, Y. Koshio, F. Nakanishi, T. Tada, T. Ishizuka, G. Barr, D. Barrow, L. Cook, S. Samani, D. Wark, A. Holin, F. Nova, S. Jung, J. Yoo, J. E. P. Fannon, L. Kneale, M. Malek, J. M. McElwee, T. Peacock, P. Stowell, M. D. Thiesse, L. F. Thompson, H. Okazawa, S. M. Lakshmi, E. Kwon, M. W. Lee, J. W. Seo, I. Yu, Y. Ashida, A. K. Ichikawa, K. D. Nakamura, S. Goto, H. Hayasaki, S. Kodama, Y. Kong, Y. Masaki, Y. Mizuno, T. Muro, K. Nakagiri, Y. Nakajima, N. Taniuchi, M. Yokoyama, P. de Perio, S. Fujita, C. Jes'us-Valls, K. Martens, Ll. Marti, K. M. Tsui, M. R. Vagins, J. Xia, M. Kuze, S. Izumiyama, R. Matsumoto, R. Asaka, M. Ishitsuka, M. Sugo, M. Wako, K. Yamauchi, Y. Nakano, F. Cormier, R. Gaur, M. Hartz, A. Konaka, X. Li, B. R. Smithers, S. Chen, Y. Wu, B. D. Xu, A. Q. Zhang, B. Zhang, H. Adhikary, M. Girgus, P. Govindaraj, M. Posiadala-Zezula, Y. S. Prabhu, S. B. Boyd, R. Edwards, D. Hadley, M. Nicholson, M. O'Flaherty, B. Richards, A. Ali, B. Jamieson, C. Bronner, D. Horiguchi, A. Minamino, Y. Sasaki, R. Shibayama, R. Shimamura,Comments: ApJ acceptedSubjects: astro-ph.HECreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
We report the search result for the Diffuse Supernova Neutrino Background (DSNB) in neutrino energies beyond 9.3~MeV in the gadolinium-loaded Super-Kamiokande (SK) detector with $22,500\times956.2$$~\rm m^3\cdot day$ exposure. %$22.5{\rm k}\times956.2$$~\rm m^3\cdot day$ exposure. Starting in the summer of 2020, SK introduced 0.01\% gadolinium (Gd) by mass into its ultra-pure water to enhance the neutron capture signal, termed the SK-VI phase. This was followed by a 0.03\% Gd-loading in 2022, a phase referred to as SK-VII. We then conducted a DSNB search using 552.2~days of SK-VI data and 404.0~days of SK-VII data through September 2023. This analysis includes several new features, such as two new machine-learning neutron detection algorithms with Gd, an improved atmospheric background reduction technique, and two parallel statistical approaches. No significant excess over background predictions was found in a DSNB spectrum-independent analysis, and 90\% C.L. upper limits on the astrophysical electron anti-neutrino flux were set. Additionally, a spectral fitting result exhibited a $\sim1.2σ$ disagreement with a null DSNB hypothesis, comparable to a previous result from 5823~days of all SK pure water phases.
[abstract 37 / 64] (score: 2) - Title: OzDES Reverberation Mapping of Active Galactic Nuclei: Final Data Release, Black-Hole Mass Results, & Scaling RelationsAuthors: H. McDougall, T. M. Davis, Z. Yu, P. Martini, C. Lidman, U. Malik, A. Penton, G. F. Lewis, B. E. Tucker, B. J. S. Pope, S. Allam, F. Andrade-Oliveira, J. Asorey, D. Bacon, S. Bocquet, D. Brooks, A. Carnero Rosell, D. Carollo, A. Carr, J. Carretero, T. Y. Cheng, L. N. da Costa, M. E. da Silva Pereira, J. De Vicente, H. T. Diehl, P. Doel, S. Everett, J. García-Bellido, K. Glazebrook, D. Gruen, G. Gutierrez, K. Herner, S. R. Hinton, D. L. Hollowood, D. J. James, A. G. Kim, K. Kuehn, S. Lee, M. March, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, J. Myles, R. L. C. Ogando, A. Porredon, E. Sanchez, D. Sanchez Cid, R. Sharp, M. Smith, E. Suchyta, M. E. C. Swanson, C. To, D. L. Tucker, A. R. Walker, N. Weaverdyck,Comments: 36 Pages, 15 Figures; see also companion paper Penton et. al. 2025Subjects: astro-ph.GA astro-ph.COCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Over the last decade, the Australian Dark Energy (OzDES) collaboration has used Reverberation Mapping to measure the masses of high redshift supermassive BLACK HOLEs. Here we present the final review and analysis of this OzDES reverberation mapping campaign. These observations use 6-7 years of photometric and spectroscopic observations of 735 Active Galactic Nuclei (AGN) in the redshift range 0.13-3.85 and bolometric luminosity range 44.3 - 47.5 erg/s. Both photometry and spectra are observed in visible wavelengths, allowing for the physical scale of the AGN broad line region to be estimated from reverberations of the H\b{eta}, MgII and CIV emission lines. We successfully use reverberation mapping to constrain the masses of 62 super-massive BLACK HOLEs, and combine with existing data to fit a power law to the lag-luminosity relation for the H\b{eta} and MgII lines with a scatter of ~0.25 dex, the tightest yet identified, fit specifically for consistency with high redshift AGN. We fit a similarly constrained relation for CIV, resolving a tension with the low luminosity literature AGN by accounting for selection effects arising from finite survey length. We also examine the impact of emission line width and luminosity (related to accretion rate) in reducing the scatter of these scaling relationships and find no significant improvement over the lag-only approach for any of the three lines. Using these relations, we further estimate the masses and accretion rates of 246 AGN with single epoch methods. We also use these relations to estimate the relative sizes of the H\b{eta}, MgII and CIV emitting regions. In short, we provide a comprehensive benchmark of high redshift AGN reverberation mapping at the close of this most recent generation of surveys, including light curves, time-delays, and a set of significantly improved radius-luminosity relations for use with high-redshift populations.
[abstract 38 / 64] (score: 2) - Title: Pseudo Little Red Dot: an Active Black Hole Embedded in a Dense and Dusty, Metal-Poor Starburst Galaxy at z=5.96Authors: Karina I. Caputi, Ryan A. Cooper, Pierluigi Rinaldi, Rafael Navarro-Carrera, Edoardo Iani, Abigail A. Tumborang,Comments: 16 pages, including 9 figures and 2 tables. Accepted for publication at the ApJSubjects: astro-ph.GA astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
We present a study of Pseudo-LRD-NOM (Pseudo little red dot with no metal lines), a highly magnified low-mass galaxy behind the lensing cluster Abell 370 at z=5.96. We classify this object as a pseudo-LRD because its red rest-frame optical colour is contaminated by a prominent Halpha line (with EW0 >~ 800 Angstroms) present in its JWST NIRSpec spectrum. Halpha is dominated by a narrow component and also has a minor broad component indicative of an active BLACK HOLE with M_BH = 5.6x10^6 Msun. A narrow Hbeta emission line is also detected (with S/N = 8), producing a Balmer decrement (narrow) Halpha/Hbeta = 11. The rest-frame UV spectral slope is beta_UVspec = -1.20 +/-0.28. All these features can be ascribed to high dust attenuation. However, no [OIII]5007 or any other metal lines are detected in the spectrum, so [OIII]5007/Hbeta < 0.25, at odds with a simple dust-attenuation explanation. Accounting for all the spectral properties requires the model of a starburst with moderate colour excess E(B-V)=0.2-0.5, high gas density (n_H >~ 10^6 cm^{-3}) and low to extremely low gas/stellar metallicities (Z = 0.01-0.1 Zsun). The demagnified stellar mass is 2.25^{+1.30}_{-0.83} x10^7 Msun and the stellar-mass surface density is Sigma* = 418^{+725}_{-310} Msun/pc^2, similar to that of massive/nuclear star clusters. Pseudo-LRD-NOM provides evidence of massive black-hole growth occurring in a high-density, dusty starburst which is at the early stages of its chemical enrichment, and is likely a precursor to a real LRD.
[abstract 39 / 64] (score: 2) - Title: Plasma effects on gravitational lensing and shadow observables of a Kerr-like BLACK HOLE in a DARK MATTER haloAuthors: Connor McMillin, Zhichen Guan, Owen Gartlan, Lotus Liu, Leo Rodriguez, Shanshan Rodriguez,Comments: 16 pages, 13 figures. Version to appear in PRDSubjects: gr-qc astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Plasma surrounding a BLACK HOLE modifies light propagation and can alter the observed shadow, potentially affecting the interpretation of Event Horizon Telescope data. We study the effects of DARK MATTER and nonMAGNETized pressureless plasma on the shadow of a Kerr-like BLACK HOLE by analyzing null geodesics in both homogeneous and inhomogeneous plasma distributions. For the homogeneous plasma profile, the asymptotic Bardeen coordinates acquire a refractive normalization factor arising from the leading-order coupling between the metric function $Δ(r)$ and the radial plasma function $f_r(r)\propto r^2$. We show that increasing the BLACK HOLE spin generally enlarges the shadow radius and increases its deformation, while moving the observer away from the equatorial plane decreases both quantities. For the parameter ranges considered, astrophysically reasonable DARK MATTER densities in this model do not produce appreciable changes in the photon trajectories. Plasma effects, however, are significant: increasing the plasma density increases the shadow radius and deformation for homogeneous plasma, but decreases them for inhomogeneous plasma. The energy emission rate likewise depends strongly on the plasma model, with homogeneous plasma producing a substantially larger rate as the plasma strength increases. As an illustrative benchmark, we compare the resulting geometric critical-curve sizes with EHT-inferred shadow-size intervals for M87* and Sgr A*.
[abstract 40 / 64] (score: 2) - Title: Cosmological Constraints from GW-FRB Associations without Redshift Measurements for LIGO-Virgo and Cosmic ExplorerAuthors: Jiaming Zhuge, Marios Kalomenopoulos, Carl-Johan Haster, Bing Zhang,Comments: Accepted for publication in ApJSubjects: astro-ph.CO astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
The potential association between gravitational waves (GWs) and fast radio bursts (FRBs) offers a unique multi-messenger probe for cosmology. In this paper, we develop a redshift-independent framework to constrain cosmological parameters using the luminosity distance - dispersion measure relation, accounting for realistic astrophysical uncertainties. We perform a comprehensive comparative analysis across different GWs detector sensitivities and modeling assumptions. Specifically, we investigate the performance of the current LIGO-Virgo (LV) network (at $z < 0.2$) versus the future Cosmic Explorer (CE). Our study further evaluates the impact of different dispersion measure (DM) distributions -- specifically the corrected Macquart's PDF (Zhuge+2025) and the log-normal distribution -- and explores the influence of including or excluding host galaxy DM contributions. Using realistic simulated observations, we find that while the current LV network lacks the precision to provide meaningful constraints, CE will enable high-precision cosmology. Even without spectroscopic redshifts, CE observations can effectively break parameter degeneracies and robustly constrain both cosmology and host galaxy parameters. These results highlight the necessity of next-generation detectors.
[abstract 41 / 64] (score: 2) - Title: Self-Reconstructing Codazzi Defects, $\mathbb{CP}^1$ Quantization, and the Minimal Standard-Model CarrierAuthors: Piotr Ogonowski,Comments:Subjects: physics.gen-phCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
A filtered local reconstruction scheme is formulated for codimension-three Codazzi defects in four-dimensional Lorentzian branches. The closure defect of the self-reconstruction loop is organized as a lexicographic residual whose entries fix, in order, the projective link, Gauss-local charges, Toeplitz support, determinant carrier, finite shadow, torsor response, and Schur completion. For a worldline defect with resolved link $\mathbb{CP}^1_Γ$, the scalar two-JET leaves two principal non-scalar types, $V_1$ and $V_2$. Faithful reconstruction of these Gauss-local charges, together with $\mathbb{CP}^1$ Toeplitz visibility, selects the separated support $E_3\oplus E_2$; reduced finite visibility fixes the degree-one line. After this carrier has been selected, the split top-form condition gives the familiar $S(U(3)\times U(2))/\mathbb Z_6$ global form and the standard one-generation exterior package, with the usual hypercharge normalization and anomaly checks. This determinant package is used as the structural comparison layer for the reconstructed carrier. The remaining construction keeps the full $\mathbb Z_6$ finite shadow, realizes its projective-color projection as a boundary torsor, and organizes the locked low sector by a $B-L$-filtered Schur-Kuranishi completion. Yukawa, neutrino, mixing, running, and contact coefficients are thereby treated as completed-branch data rather than as inputs to the carrier selection. A scale-free charged-lepton balance residual is recorded as a Schur-layer diagnostic; its zero-correction form gives the Koide-type singlet-torsor balance, while the observed deviation is left as a finite Schur-tensor datum.
[abstract 42 / 64] (score: 2) - Title: The properties of tidal disruption event infrared counterparts produced by dust rings and inference of the observing angleAuthors: Rob A. J. Eyles-Ferris,Comments: 8 pages, 7 figures, 2 tables. Accepted to MNRAS. Revision to correct typo in Table 1Subjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
A substantial fraction of tidal disruption events (TDEs), resulting from a BLACK HOLEs's disruption and accretion of a star, exhibit infrared (IR) counterparts thought to arise from spherical shells of dust reprocessing the TDE emission. Some modelling of TDEs also predicts an angular dependence in their observed properties with more X-ray emission on-axis and more optical emission at higher angles. However, there is growing evidence that X-ray rich TDEs are more likely to exhibit IR counterparts, contradicting the spherical shell model that predicts no significant variation in IR luminosity with angle. Here, I demonstrate that this result naturally follows for dust arranged in a ring instead of a spherical shell. I present a toy model of this scenario and show that on-axis angles result in a brighter counterpart. I also show that on-axis angles result in a delay in the initial rise and off-axis angles may display a double-peaked structure. Crucially, this model also allows the observing angle of the TDE to be constrained. Finally, I demonstrate that this model reproduces the properties of two IR counterparts, including constraining their observing angles and independently inferring an optical plateau, and briefly comment on its application to quasi-periodic eruption counterparts.
[abstract 43 / 64] (score: 2) - Title: Dust destruction signals shock-accelerated outflows in the nearby active galaxy NGC 1068Authors: Luke R. Holden, Clive N. Tadhunter, Daniel J. B. Smith, Martin A. Bourne, Marina I. Arnaudova, Isaac M. Mutie,Comments: 15 pages, 12 figures, 2 tables; accepted for publication in MNRASSubjects: astro-ph.GA astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Massive gas outflows driven by ACTIVE GALACTIC NUCLEi (AGN) are a key ingredient in models of galaxy evolution, in which they are required to regulate STAR FORMATION and thus explain the observed properties of the galaxy population. However, it remains uncertain how such outflows are accelerated. Here, we use deep spectroscopic observations of the nearby active galaxy NGC 1068 to directly address this issue. Based on the flux ratios of high-ionisation [NeV]$λ$3425 and [FeVII]$λ$6087 coronal forbidden lines, we show that the non-outflowing gas in the disk of the galaxy is characterised by high levels of depletion of refractory elements onto dust grains, but the outflowing gas just above the disk is largely dust-free. Consistent results are also found for the ratios of lower-ionisation forbidden lines of refractory and non-refractory elements. Moreover, a range of diagnostic ratios demonstrate that the density of outflowing gas is a factor 19-110 times higher than that of the non-outflowing gas. Together, these results imply that the outflows in NGC 1068 are accelerated by fast shocks that both compress the gas and destroy much of the dust. Consistent with the idea that AGN-driven shocks play an important role in heating and accelerating the near-nuclear gas in galaxies, this study demonstrates that coronal emission lines are a key diagnostic of the destructive impact of AGN activity.
[abstract 44 / 64] (score: 2) - Title: Using SKA-Low to Detect PeV Gamma-rays from Galactic SourcesAuthors: Anna Nelles, Philipp Laub, Haoning He, Felix Schlüter, Sjoerd Bouma, Justin Bray, Stijn Buitink, Arthur Corstanje, Vital De Henau, Edwin Dickinson, Brian Hare, Jörg Hörandel, Tim Huege, Clancy James, Xingyu Li, Hermann-Josef Mathes, Katharine Mulrey, Subhadip Saha, Olaf Scholten, Ralph Spencer, Christopher Sterpka, Karen Terveer, Satyendra Thoudam, Gia Trinh, Paulina Turekova, Darko Veberic, Keito Watanabe, Hiroaki Yamamoto, Chao Zhang, Pengfei Zhang, Yi Zhang,Comments: Published in Advancing Astrophysics with the SKAII(AASKAII), 2026(arXiv:2606.20366). Report-no:AASKAII/Nelles01Subjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Detecting so called PeVatrons is considered one of the prime goals of $γ$-ray astronomy. PeVatrons are astrophysical objects in the Galaxy that are sources of COSMIC RAYs exceeding PeV ($10^{15}$ eV) energies, the highest in our Galaxy. Their nature is unknown as of now, with some candidates reaching barely above PeV energies just having been identified. Serendipitously, the energy threshold of air shower detection using radio emission, has been proven at 50 PeV. There is a case to be made that SKA-Low with its unprecedented number of antennas, can reach lower in energy, while the size of the core is sufficiently large provide a significant effective area to measure PeV fluxes. While this promises a novel angle towards understanding the COSMIC RAY accelerators in our Galaxy, it also would be the first detection of $γ$-ray air showers using radio emission.
[abstract 45 / 64] (score: 2) - Title: Images of Braneworld BLACK HOLEs with radiatively inefficient accretion flowsAuthors: Chengjia Chen, Yin Hao, Zelin Zhang, Qiyuan Pan, Jiliang Jing,Comments: 16 pages,8 figures,Subjects: gr-qc astro-ph.HE hep-thCreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
Horizon-scale imaging acts as a transformative tool for probing spacetime geometry, enabling stringent tests of gravitational theories in the strong-field regime. The Casadio-Fabbri-Mazzacurati(CFM) BLACK HOLE in braneworld contains an extra parameter that characterizes the tidal effects from the bulk geometry, making it highly valuable for this task. We perform general RELATIVISTIC radiative transfer (GRRT) simulations and generate synthetic images consistent with Event Horizon Telescope observations of M87*. We find that the tidal parameter imprints nonmonotonic changes on the image morphology, underscoring the intricate coupling between spacetime geometry and the observable radiation from the accreting plasma. We also analyze the image-comparison metric using normalized cross-correlation coefficients and the DSSIM index and find that the magnitudes of these mismatches are on the order of 10^3, which implies that identifying braneworld BLACK HOLEs through BLACK HOLE images remains challenging even with future ngEHT and BHEX observations.
[abstract 46 / 64] (score: 2) - Title: Electrically Charged Distorted Black Holes: Thermodynamics, Particle Dynamics, and Quasinormal SignaturesAuthors: Gamal G. L. Nashed, Salvatore Capozziello,Comments: 22 pages, 3 figuresSubjects: gr-qc astro-ph.HE hep-thCreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
We construct an exact solution for the electrically charged extension of a distorted BLACK HOLE spacetime within Einstein-Maxwell theory using the Harrison transformation. The resulting solution represents a charged deformation of a static distorted vacuum geometry in which the electroMAGNETic field is introduced through a nonlinear transformation preserving the radial structure of the seed spacetime. Consequently, the Killing horizon remains determined solely by the seed metric and it is not shifted by the electric charge. We analyze the thermodynamic properties of the solution and show that the horizon area, entropy, and temperature are governed by the geometric sector, while the electric charge enlarges the thermodynamic phase space through the electroMAGNETic potential. The motion of charged test particles is studied using the effective potential formalism, where the distortion parameter modifies circular orbits and shifts the location of the innermost stable circular orbit. We also investigate the BLACK HOLE shadow for a static observer at finite distance and show that the distortion parameter displaces the photon sphere outward, increasing the apparent shadow size. A geometric correspondence between the photon orbit, determining the shadow and the leading eikonal quasinormal-mode frequency, is discussed, linking optical and perturbative observables. Finally, we study charged scalar perturbations and show that the vanishing horizon electric potential prevents a charged superradiant amplification. In the weak-coupling regime, the quasinormal-mode spectrum is estimated using the WKB method, where the electroMAGNETic interaction enters through the gauge-invariant combination $(ω- q_s ξ_t)$ and shifts the oscillation frequencies of the perturbations.
[abstract 47 / 64] (score: 2) - Title: Gravitational Wave Signatures from Periodic Orbits around a Non--commutative Schwarzschild Black HoleAuthors: N. Heidari, A. A. Araújo Filho, I. P. Lobo, V. B. Bezerra,Comments:Subjects: gr-qcCreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
In this work, we investigate massive particle motion and the gravitational wave emission generated by periodic trajectories around a non--commutative \textit{Schwarzschild} BLACK HOLE sourced by a Lorentzian matter distribution. We analyze the effective potential, the marginally bound orbit, and the innermost stable circular orbit, showing that non--commutative corrections shift these characteristic orbits toward smaller radii and reduce their corresponding angular momenta. The allowed region in the $(E, L)$ plane is also displaced toward lower values, favoring more tightly bound configurations. Periodic trajectories are classified through the rational parameter $q$, which relates the radial and azimuthal frequencies. For a fixed orbital topology, increasing the non--commutative parameter lowers the energy required to produce the orbit and results in more compact zoom--whirl configurations. Small deviations from the periodic energies are also shown to generate precessional drift. From the periastron advance of the S2 star around Sgr~A$^*$, we obtain the preliminary bound $Θ/M^{2}<0.014$. Finally, using the adiabatic and numerical kludge approximations, we compute the gravitational wave POLARIZATIONs and find phase shifts and an overall enhancement of the amplitude.
[abstract 48 / 64] (score: 2) - Title: Fast Simultaneous Surveys with On-the-Fly MappingAuthors: Suman Chatterjee, Sarvesh Mangla, Sourabh Paul, Keith Grainge, Matthias Hoeft, Tamera Kassie, Joseph J. Mohr, Yvette Perrott, Kristof Rozgonyi, Mario G. Santos, Oleg M. Smirnov, Cyril Tasse, Laura Wolz,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Chatterjee01. 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.CO astro-ph.GACreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
The SKAO is a next-generation radio telescope that will transform our understanding of the formation and evolution of RADIO GALAXies, QUASARs, transients, and other cosmic sources. Surveys conducted on precursor telescopes can inform us about the capabilities and challenges to be overcome in preparation for SKAO science. The MeerKAT Large Area Synoptic Survey (MeerKLASS), is a pathfinder large area survey to probe cosmology using the single-dish ${\rm H\hspace{0.5mm}}{\scriptsize {\rm I}}$~intensity mapping (IM). MeerKLASS provides an additional wide, high angular-resolution commensal survey by utilizing the ``On-the-Fly'' (OTF) imaging technique. The survey target is to cover 10,000 sq. degrees in the Southern sky avoiding the Galactic plane, using the UHF-band (544-1088 MHz). The survey aims to achieve an r.m.s. of 25 $μ$Jy/beam and $14''$ resolution. In this chapter we discuss the survey strategy, observational status, the development of the MeerKLASS OTF imaging pipeline and the science prospects of the data products. OTF imaging, which relies upon constant elevation fast scanning, comes with its own set of challenges, such as smearing. Here we detail how we have mitigated them and the current scientific impact. Significantly fast survey speed ($\sim 3.5$ sq. deg per min), commensality with ${\rm H\hspace{0.5mm}}{\scriptsize {\rm I}}$~IM survey, deep and large area continuum images make MeerKLASS OTF an economic survey technique. Lessons from this technique will be valuable for the upcoming SKA-Mid, where we expect a better resolution $(< 2'')$ and sensitivity $(\sim 7μ{\rm Jy/beam})$ of the OTF images with the AA4 configuration. Furthermore, improvements in the correlator will result in negligible smearing effects in the imaging.
[abstract 49 / 64] (score: 2) - Title: Latent thermal instabilityAuthors: Prakriti Pal Choudhury, Archie F. A. Bott,Comments: 10 pages, 4 figures, 1 table. To be submitted, comments are welcomeSubjects: astro-ph.GA physics.plasm-phCreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
Multiscale temperature fluctuations are abundant in the intracluster medium (ICM) outside of galaxy cluster cores ($\sim 100~{\rm kpc}$). Their origin is often attributed to turbulent stirring by subhalos or accreting baryons crossing the virial radius. However, their apparent resistance to mixing and thermal conduction in a collisional medium has not been explained. We propose a new mechanism by which steady-state temperature fluctuations can form and persist outside the cluster core. Local thermal instability, or Field instability, is used to explain filamentary condensates in cluster cores but is usually dismissed outside them because thermal conduction should suppress instability. In weakly collisional or collisionless plasmas, however, thermal conduction can be anomalously suppressed by heat-flux-driven plasma instabilities triggered in presence of a local MAGNETic field, leading to two effects: (i) condensates form in a new parameter regime that overlaps with conditions outside the core, and (ii) condensates reach a steady state as in the hydrodynamic limit. This extends the regime of instability-driven fluctuations to over $\gtrsim50\%$ (depending on hot plasma temperature) of the cluster. We use one-dimensional hydrodynamic simulations of condensates to test our analytical ideas.
[abstract 50 / 64] (score: 2) - Title: Prediction for IMAP: Revealing the Role of the Solar Magnetic Field in the HeliotailAuthors: M. Kornbleuth, M. Opher,Comments: Submitted to ApJLSubjects: astro-ph.SRCreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
The classic paradigm of the heliosphere considered the solar MAGNETic field as having a passive role in the heliosheath, yet recent work has suggested that the solar MAGNETic field plays an active role by collimating the solar wind plasma. Previous work has suggested that high-latitude lobes observed by IBEX-Hi energetic neutral atom (ENA) maps are solely due to the fast/slow solar wind profile, yet other works have found that the solar MAGNETic field may play a role in organizing the lobes as well. Here, using an MHD solution with and without the solar MAGNETic field, we find that the fast/slow wind profile largely dictates the ENA profile up to 10 keV. Beyond this energy, the collimation effects are more prominent and the fast/slow solar wind profile no longer organizes the maps. The collimation creates two high latitude lobes. At 80 keV, the split-tail heliosphere yields an enhancement of ENAs of the high-latitude tail lobes compared to the low-latitude region by a factor of $\sim$2, IMAP should be able to see whether the solar MAGNETic field collimates the solar wind, as well as probe the shape of the deep heliotail.
[abstract 51 / 64] (score: 2) - Title: A Stellar Role Reversal: Multiple Features in the Mass and Mass Ratio Distributions of Merging Binary Black Holes from Stable Mass TransferAuthors: Gina Chen, Katelyn Breivik, Lieke A. C. van Son,Comments: 16 pages, 6 figures, to be submitted to AAS Journals, comments welcomeSubjects: astro-ph.SR astro-ph.HECreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
Observations of gravitational wave events have enabled the measurement of the merging binary BLACK HOLE (BBH) mass function. This mass function encodes the physical interactions which shape the formation and evolution of BBHs. In this work we investigate how the stable mass transfer (SMT) channel of BBH formation imprints onto the BBH primary mass and mass ratio distributions. We use both an analytic framework and binary population synthesis to show how assumptions about mass transfer accretion efficiency and mass transfer stability affect the BBH mass distribution. Under the assumption of conservative mass transfer, we find that the SMT channel produces two observationally distinct subpopulations: a high primary mass, near equal mass ratio population formed through mass ratio reversal (MRR), and a low primary mass non-MRR subpopulation. The mass range where MRR occurs is determined by assumptions about binary SMT. In particular, we find that the stability criteria for mass transfer at different stellar evolutionary stages carve out complementary regions in the primary-mass--mass-ratio plane, separating the MRR and non-MRR populations into distinct peaks at high and low primary mass respectively. Our results imply that the physics of SMT creates distinct features in gravitational wave populations which current and near future gravitational wave detectors may be able to resolve.
[abstract 52 / 64] (score: 2) - Title: A nonRELATIVISTIC radiative transfer module for IdefixAuthors: Nicolas Scepi, Geoffroy Lesur,Comments: Accepted for publication in A&A. 12 pages and 12 FiguresSubjects: astro-ph.IM astro-ph.EP astro-ph.GA astro-ph.HE astro-ph.SRCreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
Radiation MAGNETohydrodynamic (RMHD) simulations are essential for comparisons with observations, particularly in the regime where fluids and radiation are dynamically coupled. Although computationally expensive, RMHD is becoming increasingly accessible with the advent of exascale computing. However, only a few public RMHD codes are currently able to fully exploit the diversity of modern accelerated architectures. We present a nonRELATIVISTIC radiative transfer module for the public MAGNETohydrodynamic code IDEFIX; it is built on the Kokkos library to ensure performance portability. Our goal is to provide a user-friendly RMHD code capable of running efficiently on current and future exascale supercomputers. The radiative transfer module is based on the M1 approximation and implemented using a split explicit-implicit scheme. A reduced speed of light approximation is employed to alleviate the timestep constraint imposed by radiation. The module supports several radiation Riemann solvers and Cartesian, cylindrical, and spherical geometries in one, two, and three dimensions. The implicit step relies on a simple matrix inversion, ensuring both robustness and high performance. Users can choose between built-in opacity models or supply tabulated opacities and custom user-defined functions. The radiative module of IDEFIX demonstrates excellent performance on accelerated architectures, including the AMD MI250X and MI300 partitions of the AdAstra supercomputer. On MI250X nodes, it achieves up to $7.\times 10^8$ cell updates per second per node, at a computational cost only 1.6 times higher than a pure MAGNETohydrodynamic simulation. These results establish IDEFIX as a fast, robust, and portable RMHD code suitable for the wider community.
[abstract 53 / 64] (score: 2) - Title: The 10-15 GHz radio continuum survey of the Galactic Plane with SKAOAuthors: A. Traficante, C. Mininni, F. Cavallaro, G. Umana, C. Trigilio, S. Molinari, L. D. Anderson, M. Audard, C. Bordiu, C. S. Buemi, C. Carrasco-Gonzalez, L. Cerrigone, E. J. Chung, J. Dey, A. Ingallinera, I. Jimenez-Serra, P. Klaassen, S. Loru, K. Mallick, A. Nucara, M. Padovani, J. D. Pandian, K. L. J. Rygl, T. M. Rodríguez, G. Sabatini, S. Reissl, P. Suin, M. A. Thompson, T. L. Bourke, J. S. Urquhart, M. Valeille-Manet, F. Xu, A. Zavagno, M. Benedettini, E. Bianchi, A. Bracco, F. Bufano, C. Codella, N. Cunningham, J. Dawson, D. Galli, M. G. Guarcello, A. Karska, W. -J. Kim, P. Leto, B. Liu, B. Mookerjea, F. Motte, T. Nony, R. Paladini, A. Patel, L. Podio, A. J. T. Ramaila, B. Riaz, S. Riggi, D. A. Roshi, A. Ruggeri, Á. Sánchez-Monge, R. Schödel, O. M. Smirnov, J. D. Soler, S. Sottie, R. Unnikrishnan, A. Y. Yang, K. Wang, T. Wilson,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:26.06.20366). Report-no:AASKAII/Traficante01. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.GACreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
Star formation emerges from the complex interplay between gravity, turbulence, MAGNETic fields, and stellar feedback, all of which vary across spatial scales and Galactic environments. Over the past decades, extensive multiwavelength surveys of the Galactic Plane have progressively unveiled this complexity. Far-infrared and sub-millimetre surveys have identified and characterized tens of thousands of star-forming regions, revealing their mass, temperature, and evolutionary stage. Complementary molecular-line surveys, spanning several CO transitions and isotopologues, have mapped the gas kinematics from giant molecular clouds down to sub-parsec structures. The advent of interferometers such as ALMA has revolutionized this field, enabling systematic studies of gas dynamics, fragmentation, and collapse in dense clumps at scales of a few thousand astronomical units. At the same time, mid-infrared and radio surveys at frequencies 0.8 <= nu <= 5 GHz have traced ionised gas associated with the earliest and latest phases of massive-star evolution, including thermal radio JETs, hypercompact and ultracompact HII regions, SUPERNOVA remnants, planetary nebulae, and evolved massive stars. Yet, a uniform, Galaxy-wide census of ionised structures and feedback processes remains elusive. A transformational leap forward requires a sensitive, high-resolution radio survey of the Galactic Plane at 10-15 GHz, capable of resolving physical scales smaller than 0.05 pc at distances up to 20 kpc. This is precisely the goal of the SKA-Mid Galactic Plane survey, which will, with its unprecedented sensitivity, angular resolution, and mapping speed, provide the first panoptic view of ionised gas and stellar feedback across the Milky Way.
[abstract 54 / 64] (score: 2) - Title: Constraints on Binarity for the Extreme Oe Variable Star AzV 493Authors: M. S. Oey, Irene Vargas-Salazar, Edmund Hodges-Kluck, Norberto Castro, Michal K. Szymanski, Mario Mateo, Mathieu Renzo, Mark W. Suffak, Maxwell Moe,Comments: 13 pages, 4 figures, 2 tables. Accepted to PASPSubjects: astro-ph.SR astro-ph.HECreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
The extreme Oe star AzV 493 is known to show unusual photometric and spectroscopic variability that suggest the presence of an unseen companion in a highly eccentric and long-period (7.3 or 14.6-year) orbit. We obtained a Chandra/ACIS observation near the putative periastron for the 7.3-year orbit to test for transient X-ray emission that would confirm its binary nature. Our data only place an upper limit to the X-ray luminosity of L_X < 2.5 x 10^33 erg/s based on the 0.5 - 8 keV flux limit. Additionally, we obtained 4 new spectroscopic observations with the M2FS spectrograph at Magellan and 20 archive FLAMES/GIRAFFE and X-Shooter spectra from ESO/VLT to further constrain the possibility of radial velocity (RV) variation. Statistical analysis of the RV measurements yields inconclusive results regarding the existence of variations. We discuss possible mass limits for a potential companion, which may be a BLACK HOLE, in the event that the variations are real. The violet-to-red (V/R) Balmer ratio has also recently inverted, which may be a further indication of a companion.
[abstract 55 / 64] (score: 2) - Title: Debiasing the Observed Fast Radio Burst Population with the CHIME/FRB Selection FunctionAuthors: Kyle McGregor, Jason W. T. Hessels, Victoria M. Kaspi, Kaitlyn Shin, Fengqiu A. Dong, Naman Jain, Robert A. Main, Mawson W. Sammons, Michele Woodland, Daniel Amouyal, Derek Bingham, Charanjot Brar, Amanda M. Cook, Radu Craiu, Alice P. Curtin, Gwendolyn Eadie, Bryan M. Gaensler, Jeff Huang, Afrokk Khan, Calvin Leung, Kiyoshi W. Masui, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Sachin Pradeep E. T., Paul Scholz, Seth R. Siegel, Kendrick Smith, David C. Stenning,Comments: 25 pages, 10 figures, submitted to ApJSubjects: astro-ph.HECreated: 2026-06-24; Updated: 2026-06-26; Datestamp: 2026-06-26
The recent release of CHIME/FRB Catalog~2 provides the largest sample to date with which to investigate the intrinsic distributions of fast radio bursts (FRBs). Leveraging an expanded campaign of 587,367 synethetic bursts injected into the live CHIME/FRB search pipeline, we perform a population analysis of the fluence, scattering timescale, pulse width, and dispersion measure distributions of Catalog~2 FRBs. We first infer the intrinsic population using a resampling-based framework that accounts for instrumental selection effects following previous CHIME/FRB population studies. A central goal of this work is to constrain the intrinsic distribution of scattering timescales, that remained weakly constrained in Catalog~1 owing to limited statistics at moderate and large scattering times ($τ\gtrsim 10\,\mathrm{ms}$ at 600~MHz) and sparse injection coverage in this regime. Second, we construct an explicit multidimensional selection function by training a logistic regression model on the injected events. This model estimates the detection probability as a function of FRB observable properties, including higher-order interaction terms. We incorporate this selection function into a simulation-based inference framework to refine the inferred intrinsic scattering-timescale distribution. We find evidence for a slight downturn in the intrinsic FRB scattering timescale distribution, though a flat or slightly rising distribution cannot be ruled out, that is further supported through a comparison with the higher-frequency scattering timescale distribution observed by Commensal Real-time ASKAP Fast Transients (CRAFT) survey.
[abstract 56 / 64] (score: 2) - Title: Search for Seeds of The Cradle of Stars: Study of The Evolution From Atomic to Molecular Hydrogen Clouds with 1000 AU Scale ResolutionAuthors: Hiroaki Yamamoto, Yamato Matsuzuki, Kengo Tachihara,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Yamamoto01. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.GACreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
The aim of this science case for SKA1-Mid is to elucidate the spatial and velocity structure of the Cold Neutral Medium (CNM) on scales below the Field length, thereby elucidating the physical processes that govern CNM structure formation and its role in the earliest stages of molecular cloud formation. This goal will be achieved through a unique observational combination of several-arcsecond angular resolution, high velocity resolution, and unprecedented surface-brightness sensitivity. These observations will reveal the characteristic size, morphology, velocity structure, and internal dynamics of CNM clumps, and will directly connect such structures to the earliest phases of the atomic to molecular transition. Full-POLARIZATION observations with SKA1-Mid will also enable emission-based Zeeman measurements of the CNM, allowing the MAGNETic field strength to be mapped and opening a new window on the role of MAGNETic fields in CNM formation and evolution. In particular, this will make it possible to determine whether MAGNETic fields primarily inhibit fragmentation by supporting the gas against compression, or instead guide anisotropic condensation and promote the development of small-scale CNM structure through thermal instability. In combination with interferometric spatial filtering and high spectral resolution, SKA1-Mid will selectively trace the CNM and robustly identify individual clumps in both position and velocity space. These capabilities will provide decisive tests of thermal instability and the two-phase turbulence model, and will establish a new observational foundation for understanding how molecular clouds emerge from the multi-phase atomic interstellar medium.
[abstract 57 / 64] (score: 2) - Title: From Holst to Carroll Gravity, a Hamiltonian point of viewAuthors: J. Fernando Barbero G, Juan Margalef-Bentabol, Valle Varo, Eduardo J. S. Villaseñor,Comments: 21 pages, no figuresSubjects: gr-qcCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
The Carrollian regime of gravity provides a useful ultraRELATIVISTIC framework for studying asymptotically flat spacetimes, horizon dynamics, and condensed matter systems. In this paper, we present a comprehensive Hamiltonian analysis of the most general Carroll-invariant Lagrangian that can be derived from the Holst action. To guide the analysis, Cartan geometry tools are used. We identify the full constraint structure of the theory, characterize its gauge symmetries, obtain the explicit form of the Hamiltonian vector fields and introduce Ashtekar-like variables for the MAGNETic Carrollian regime. We also discuss in detail an analog of the time gauge employed in the Hamiltonian analysis of the Holst action for general relativity.
[abstract 58 / 64] (score: 2) - Title: A geometric multimessenger consistency test of radiative and near-zone gravity with LISA and SKAAuthors: Bhooshan Gadre,Comments: 14 pages, 5 figuresSubjects: gr-qc astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Compact binary pulsars observed both through precision radio timing and low-frequency gravitational waves offer a direct way to compare the same binary geometry with two independent messengers. We propose a multimessenger consistency test based on the orbital inclination, measured from the Shapiro-delay shape parameter in radio timing and from the tensor POLARIZATION amplitude ratio in the gravitational-wave signal. Defining the common-epoch residual $\eps(t_0)=s_{\rm Shapiro}(t_0)-s_{\rm GW}(t_0)$, general relativity predicts $\eps=0$, while a nonzero value would indicate either an unmodeled systematic or a mismatch between the near-zone and radiative descriptions of gravity. We estimate the attainable precision on this quantity for representative LISA--SKA compact binary pulsars using a seven-parameter timing Fisher matrix and a sky-averaged LISA sensitivity curve including the Galactic foreground. We adopt a conservative radio baseline, $σ_{\rm TOA}=1\,μ{\rm s}$ and $N_{\rm eff}=10^4$, intended to summarize radiometer noise, jitter, residual dispersion-measure and scattering effects, profile evolution, and cadence losses after wideband timing. For systems at $d=5\,{\rm kpc}$ observed for four years, we find $σ_\eps\simeq4\times10^{-3}$ for a favorable double neutron star and $σ_\eps\simeq9\times10^{-4}$ for a hypothetical pulsar--black-hole system. The former is the more robust astrophysical benchmark; the latter illustrates the reach if such a high-SNR chirping source is discovered. The useful cases remain limited mainly by gravitational-wave polarimetry, while radio timing supplies the near-zone reference measurement of the inclination. These results define a quantitative target for future joint Bayesian analyses of compact binary pulsars observed in both radio and gravitational waves.
[abstract 59 / 64] (score: 2) - Title: A possible approach to overcome the saturation of the neutron yield in a Plasma Focus and to achieve breakevenAuthors: Andrea Di Vita,Comments: 34 pages; 3 figuresSubjects: physics.plasm-phCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Saturation of the neutron yield with increasing energy of the condenser bank in a Plasma Focus led to the shutdown of PF research focussed on controlled nuclear fusion in the past. We review available models of saturation and develop further the model of Lee S., Applied Phys. Lett. 95, 151503, 2009. This model relies on the well-known and generally accepted model of Lee S., J. Fusion Energy 2014, 33, 319 of Plasma Focus discharges and describes saturation in terms of the dynamic resistance, i.e. the rate of change of PF inductance due to the motion of the plasma sheath during rundown. A model of this sheath discussed in Di Vita A., J. Plasma Physics, 1993, 50, 1 shows that its spontaneous filamentation rules the dynamic resistance, spoiling the power supply from the condenser bank to the plasma at the values of condenser bank energy above 0.5 MJ values which are relevant to a fusion reactor. Together, these two models lead to the conclusion that suppression of such filamentation prevents saturation, multiplies the PF drive parameter by a factor 3 at least and allows breakeven in a 224 kV, 10 MJ Plasma Focus working with DT. We can suppress filamentation by superimposing a radial MAGNETic field to the interelectrode region of the Plasma Focus where rundown occurs. A conservative estimate shows that a 1.4 T radial MAGNETic field is enough to suppress many known filamentation instabilities. Suitably located MAGNETs can generate this field. Their layout resembles the layout of the sources of radial MAGNETic field in the cylindrical geometry of a Hall thruster for space propulsion. For high temperature superconducting MAGNETs, the required current density is too small to trigger quenching.
[abstract 60 / 64] (score: 2) - Title: Probing Anomalous Microwave Emission with the Square Kilometre ArrayAuthors: Matías Vidal, Simón Casassus, Roke Cepeda-Arroita, Miguel Cárcamo, Stuart E. Harper, Thiem Hoang, J. A. Rubiño-Martín, Kieran A. Cleary, Clive Dickinson, R. T. Génova-Santos, Gabriel A. Hoerning, Melis O. Irfan, A. Lazarian, Hauyu Baobab Liu, Eric J. Murphy, M. W. Peel, Nathalie Ysard, Zheng Zhang,Comments: Published in Advancing Astrophysics with the SKAII(AASKAII), 2026 (arXiv:2606.20366). Report-no: AASKAII/Vidal01Subjects: astro-ph.GA astro-ph.IMCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Anomalous microwave emission (AME) represents an excess of radiation in the 10-60 GHz range, distinct from SYNCHROTRON, free-free, or thermal dust emission. Although most commonly attributed to electric dipole radiation from rapidly rotating small dust grains (spinning dust), alternative mechanisms such as MAGNETic dipole emission (MDE) remain plausible. The detection of AME across diverse environments, from diffuse interstellar clouds to protoplanetary disks and external galaxies, suggests that multiple physical processes or carriers may contribute to its origin. Understanding AME is essential for both Galactic astrophysics and cosmology, as it constitutes a significant foreground for cosmic microwave background (CMB) studies, potentially biasing measurements. This chapter reviews current theoretical frameworks and observational evidence for AME, highlighting the key outstanding questions concerning its emission mechanisms, carriers, and POLARIZATION properties. We discuss how the Square Kilometre Array Observatory (SKAO), through its unprecedented sensitivity, angular resolution, and frequency coverage, will transform AME studies. SKA observations will enable detailed mapping of AME morphology, precise characterisation of its spectral energy distribution, and the identification of its carriers in Galactic and extragalactic environments. By combining SKA-mid data with higher-frequency observations from ALMA and other facilities such as SPHEREx, it will be possible to disentangle competing models and exploit AME as a diagnostic probe of interstellar grain physics and the small-scale structure of the interstellar medium.
[abstract 61 / 64] (score: 2) - Title: Redshift-Dependent Intrinsic Dispersion in the Quasar UV/X-ray Luminosity RelationAuthors: Jiaze Gao, Jianping Hu, Yun Chen, Bowen Zhao, Lixin Xu,Comments: 11 pages, 4 figures, 2 tablesSubjects: astro-ph.COCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Accurate modeling of the intrinsic dispersion in the QUASAR UV/X-ray luminosity relation is essential for reliable cosmological inference. We investigate its redshift dependence using luminosity distances reconstructed from cosmic chronometer and baryon acoustic oscillation measurements through Gaussian-process (GP) regression. Bayesian model comparison and posterior constraints show that the intrinsic dispersion is not well described by a single redshift-independent constant over $0.7
[abstract 62 / 64] (score: 2) - Title: A search for Fast Radio Bursts from globular clusters in M49 with FASTAuthors: Simon C. -C. Ho, Chris Flynn, Matthew Bailes, Emma Carli, Lei Zhang, Manisha Caleb, Kenneth C. Freeman, Tetsuya Hashimoto, Tomotsugu Goto, James O. Chibueze,Comments: 11 pages, 5 figures, accepted for publication in MNRASSubjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
The origins of fast radio bursts (FRBs) remain uncertain, although MAGNETars are a leading progenitor candidate. Because MAGNETars are thought to form primarily through core-collapse SUPERNOVAe in young stellar populations, the discovery of FRB 20200120E in a globular cluster (GC) in the nearby galaxy M81 was unexpected given the ancient stellar populations of GCs. Expanding the sample of FRBs localised to nearby galaxies is therefore essential for testing FRB formation channels in old stellar environments. M49 (NGC 4472) is a nearby (~17 Mpc), radio-quiet giant elliptical galaxy in the Virgo cluster hosting about 7000 GCs, making it an ideal target for GC FRB searches. We conducted a 9-hour SnapShotCal observation of M49 using the Five-hundred-meter Aperture Spherical Telescope (FAST) 19-beam receiver, covering approximately 4230 GCs (2.1 hr per GC), and performed a comprehensive single-pulse search over a dispersion measure range of 0-5000 pc cm^-3. No unambiguous astrophysical FRBs were detected. The most significant trigger reached a post-processed signal-to-noise ratio of 8.6 sigma at a dispersion measure of 412.2 pc cm^-3, but is statistically consistent with thermal noise after accounting for the false-alarm rate. We derive a beam-averaged peak flux-density sensitivity of about 16.5 mJy (corresponding to a fluence limit of about 16.5 mJy ms for a 1 ms burst) and place an upper limit on the FRB occurrence rate of 4.7 x 10^-4 FRB GC^-1 hr^-1. Our non-detection constrains only bright bursts above this fluence threshold during the observing window.
[abstract 63 / 64] (score: 2) - Title: Ion firehose and ion cyclotron instability with subtracted-Kappa distributionsAuthors: Luiz F. Ziebell, Rudi Gaelzer, Danny Summers,Comments: 15 pages, 8 figuresSubjects: physics.plasm-phCreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
In the present paper we discuss numerical solutions of the dispersion relation for electroMAGNETic waves propagating along the lines of an ambient MAGNETic field, considering parameters representative of space plasma environments, and considering the ion population described by a subtracted-Kappa distribution. We consider situations in which the ion thermal anisotropy is such that $T_{i\perp}
[abstract 64 / 64] (score: 2) - Title: Origins of Cosmic Rays in the Galactic-extragalactic Transition Energy RangeAuthors: A. Corstanje, S. Saha, S. Bouma, J. Bray, S. Buitink, V. de Henau, E. Dickinson, B. Hare, A. Haungs, H. He, J. Hörandel, T. Huege, C. James, P. Laub, X. Li, H-J. Mathes, K. Mulrey, A. Nelles, F. Schlüter, O. Scholten, R. Spencer, C. Sterpka, K. Terveer, S. Thoudam, G. Trinh, P. Turekova, D. Veberic, K. Watanabe, C. Zhang, P. Zhang, Y. Zhang,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Corstanje01Subjects: astro-ph.HECreated: 2026-06-25; Updated: 2026-06-26; Datestamp: 2026-06-26
Cosmic rays arrive at Earth with energies ranging from $10^9$ to over $10^{20}$ eV. One of the open questions in high-energy COSMIC RAY science concerns the origin of the highest-energy COSMIC RAYs that can be accelerated by Galactic sources, and the transition energy beyond which only extragalactic sources can provide. Measuring the mass composition gives essential information for comparing measurements to source and propagation models, both from the abundances at the source and from the maximum attainable energy which is proportional to the particle charge (and hence its mass). The highest-energy COSMIC RAYs from the Galaxy are found in a range of $10^{16}$ to $10^{18}$ eV which is well suited for radio detection. Building on a decade of experience in measuring COSMIC RAYs at LOFAR, we show that SKA-Low, augmented with an array of small particle detectors, is well suited to advance the field by measuring the mass composition of COSMIC RAYs across this energy range.
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