Current date: 2026-10-12
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Number of records retrieved: 703
Keyword score statistics
score 7 -- 1 abstracts
score 6 -- 2 abstracts
score 5 -- 2 abstracts
score 4 -- 1 abstracts
score 3 -- 8 abstracts
score 2 -- 15 abstracts
in total -- 29 abstracts
Articles that appeared on 2026-10-12
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[abstract 1 / 29] Wow! (score: 7)
- Title: Formation Dynamics of a Rotating Solar Spicule-like Event and Associated Energy-Mass TransportAuthors: Liufan Gong, Lei Ni, Guanchong Cheng, Jiajia Liu, Quan Xie, Robert Erdélyi,Comments: 13 pages, 10 figuresSubjects: astro-ph.SRCreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
We performed three-dimensional radiative MAGNETohydrodynamic(3D RMHD) simulations in an upward-directed (positive-polarity) open MAGNETic field with an initial background strength of 10 G. We identified vortex-associated spicule-like events and carried out a detailed analysis of one representative event. Prior to the formation of this spicule-like event, a photospheric vortex appears and twists the MAGNETic field lines, then develops upward into higher atmospheric layers, forming a MAGNETic tornado system. This event is generated during this process. At the periphery of this MAGNETic tornado, twisted MAGNETic field lines with negative vertical components RECONNECT with both external positive-polarity background fields and central positive-polarity fields. The MAGNETic RECONNECTion sites rise and rotate together with the developed MAGNETic tornado, and many JET-like substructures in this event are closely associated with plasma upward ejections from these RECONNECTion regions. A vertical force analysis shows that, for this event, plasma uplift in the photosphere and lower chromosphere is dominated by the pressure-gradient force, whereas in the upper chromosphere, the Lorentz force gradually becomes dominant. At a height of about 4 Mm above the solar surface, this event produces a mean upward mass flux density on the order of $10^{-7}~{\rm kg~m^{-2}~s^{-1}}$ and a mean upward Poynting flux density of approximately $525~{\rm W~m^{-2}}$. The wave-mode decomposition results show that the energy transport associated with the rotational spicule-like event is dominated by the Alfvén mode. Alfvén waves, fast-mode waves, and slow-mode waves carry energy into the lower corona in an approximate ratio of $10:7:3$.
[abstract 2 / 29] Yes (score: 6) - Title: Radio streaks in the Lighthouse Nebula discovered with MeerKAT -- Particles escaping from the tail and illuminating the ambient MAGNETic fieldAuthors: Pierrick Martin, Mickael Coriat, Barbara Olmi, Elena Amato, Niccolò Bucciantini, Sanja Lazarević, Miroslav D. Filipović, Alexandre Marcowith, Sarah Recchia,Comments: 10 pages, 7 figures, Accepted for publication in A&A. Revised version including ASKAP observations and two additional co-authorsSubjects: astro-ph.HECreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
Bow-shock pulsar wind nebulae are valuable sources for investigating the dynamics of RELATIVISTIC pulsar winds and the mechanisms by which they produce cosmic-ray leptons at the highest energies. The Lighthouse Nebula is one such object, famous for the high velocity of its pulsar and its long, misaligned X-ray JET, which may provide a specific escape channel for the most energetic particles. We aim to understand how the bulk of non-thermal particles is released into the ISM. We focus on GHz radio observations, which probe lower-energy particles that are dominant in number and long-lived, thus providing a picture of how escape proceeds over long timescales. We analysed MeerKAT and ASKAP observations at 1.28GHz and 0.94GHz, respectively. MeerKAT observations reveal a highly structured SYNCHROTRON nebula downstream of the pulsar PSRJ1101-6101. A cometary tail extends beyond 5pc from the pulsar, while we detect multiple two-sided transverse emission streaks for the first time. We detect no radio counterpart of the misaligned X-ray JET, but the spectral index map shows an apparent asymmetry, with the steepest values near the base of the JET. We interpret the radio streaks as the occasional, charge-independent release of energetic leptons from the tail into the surrounding medium, resulting from dynamical instabilities and reconfiguration in the downstream flow. Most of the particle content of the nebula is discharged into the ambient medium within several pc. Escaped particles light up the ambient MAGNETic field, which appears to have a coherence length of at least a few pc. The length and persistence of the streaks indicate a low level of MAGNETic turbulence, possibly slightly enhanced with respect to average cosmic-ray transport conditions in the Galaxy. This may result from self-generated turbulence caused by a resonant streaming instability or from past activity of the progenitor star.
[abstract 3 / 29] Yes (score: 6) - Title: Resistive alignment of a black-hole MAGNETosphereAuthors: Ruben Lier, Oliver Porth,Comments:Subjects: astro-ph.HE hep-th physics.plasm-phCreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
Recent numerical simulations have shown that black-hole MAGNETospheres evolve rapidly toward alignment between the MAGNETic axis and spin axis but the physical origin of this process has remained unclear. We develop an analytic theory of this alignment within resistive RELATIVISTIC MAGNETohydrodynamics. Taking the slow-spin Blandford-Znajek monopole solution as the exterior MAGNETic field, we reduce the induction equation to a relaxation equation for the current-sheet inclination angle. Our analysis shows that alignment results from second-order spin effects in the Blandford-Znajek solution combined with explicit resistive dissipation. We test this prediction using resistive-GRMHD simulations at several spins and resistivities and find a regime in which the measured late-time secular decay agrees quantitatively with the analytic prediction.
[abstract 4 / 29] Yes (score: 5) - Title: Search for Gamma-ray emission from Abell 119 galaxy cluster using INTEGRAL/ISGRI, COMPTEL, and DAMPE dataAuthors: Siddhant Manna, Shantanu Desai,Comments: 11 pages, 4 figures. Published in the Open Journal of AstrophysicsSubjects: astro-ph.HE astro-ph.COCreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
We present a comprehensive search for non-thermal high-energy $γ$-ray emission from the nearby merging galaxy cluster Abell~119 ($z=0.044$) using archival observations spanning over seven decades in photon energy. Our analysis combines hard X-ray data from INTEGRAL/ISGRI (30--100~keV), MeV $γ$-ray observations from COMPTEL (0.75--30~MeV), and GeV--TeV data from the DArk Matter Particle Explorer (DAMPE; 3~GeV--1~TeV). No statistically significant emission is detected at the cluster position in any energy band. In the hard X-ray regime, we derive a $3σ$ upper limit of $F_{30-100\,\mathrm{keV}} \lesssim 8.5 \times 10^{-11}$~erg~cm$^{-2}$~s$^{-1}$ from ISGRI mosaic imaging. Reanalysis of archival COMPTEL data yields 95\% confidence-level upper limits ranging from $\sim 9 \times 10^{-11}$ to $\sim 8 \times 10^{-10}$~erg~cm$^{-2}$~s$^{-1}$ across 0.75--30~MeV. In the GeV--TeV range, DAMPE \rthis{places upper limits on the} differential energy flux to $\sim 10^{-12}$--$10^{-10}$~erg~cm$^{-2}$~s$^{-1}$ (95\% confidence level). These results provide independent multi-band constraints on the reported GeV excess from recent FERMI-LAT studies. While our DAMPE limits do not exclude the flux levels claimed in those analyses, the absence of confirmation across keV--MeV--GeV bands indicates that any non-thermal emission from Abell~119 remains tentative.
[abstract 5 / 29] Yes (score: 5) - Title: HAMCOR: A physics-driven Hamiltonian framework for inferring AGN coronal geometry from X-ray reverberation lagsAuthors: Fabio Buffoli,Comments: 17 pages, 9 figures, 8 tablesSubjects: astro-ph.HECreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
We present HAMCOR (Hamiltonian-based AGN Multi-constraint CORonal inference framework), a geometry-agnostic method for inferring the X-ray coronal structure of accreting BLACK HOLEs using reverberation-lag measurements. Unlike conventional template-fitting approaches, HAMCOR reframes coronal geometry inference as the ground-state selection of a physical Hamiltonian. The corona is represented as a discrete emissivity distribution over a cylindrical grid, and its geometry emerges from five competing physical constraints: MAGNETic coherence, lag consistency, illumination consistency, pair-production stability, and energy budget feasibility. Minimisation is performed via projected gradient descent with Armijo backtracking line search on the probability simplex. We validate HAMCOR on three synthetic geometries (lamppost, column, ring) using the same grid as the real-data fits, recovering spatial correlations rho = 0.24, 0.50, 0.12 and fractional lag errors below 24 per cent. A hyperparameter sensitivity analysis confirms robustness over more than one order of magnitude in the coupling constants. We apply HAMCOR to five sources spanning seven orders of magnitude in BLACK HOLE mass: four AGN observed with XMM-Newton (Mrk 335, 1H 0707-495, IRAS 13224-3809, MCG-6-30-15) and the stellar-mass BLACK HOLE binary Cyg X-1 (M_bh = 14.8 M_sun), recovering consistent extended disc-corona geometries across the full mass range. We further present a multi-epoch analysis of Mrk 335 across five XMM-Newton observations (2006-2019), revealing that the coronal centroid remains stable at (R_c, z_c) ~ (6.3, 0.5) r_g across flux states spanning a factor of ~15 in reverberation lag amplitude, arguing against a collapsing or expanding lamppost. Schwarzschild-Shapiro delay corrections amount to ~79 per cent of the flat-spacetime lag on average; the recovered spatial morphology is robust to this correction.
[abstract 6 / 29] Yes (score: 4) - Title: TeV Gamma-Ray Emission in the DA 495 Region from HAWC Observations of J1952+2924, J1954+2837, and J1958+2848Authors: R. Alfaro, C. Alvarez, E. Anita-Rangel, M. Araya, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, P. Bangale, A. Bernal, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, N. Di Lalla, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, C. Espinoza, N. Fraija, S. Fraija, A. Galván-Gámez, J. A. García-González, F. Garfias, N. Ghosh, A. Gonzalez Muñoz, M. M. González, J. A. González, J. A. Goodman, J. Gyeong, J. P. Harding, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, S. Kaufmann, D. Kieda, K. Leavitt, W. H. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, P. E. Mirón-Enriquez, J. A. Morales-Soto, E. Moreno, M. Mostafá, M. Najafi, L. Nellen, M. U. Nisa, R. Noriega-Papaqui, M. Osorio-Archila, E. Ponce, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, M. Roth, A. Sandoval, J. Serna-Franco, M. Shin, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, I. Torres, R. Torres-Escobedo, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, H. Wu, S. Yu, S. Yun-Cárcamo, X. Zhang, H. Zhou, C. de León,Comments:Subjects: astro-ph.HECreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
Previous observations of the DA 495 region, which contains the pulsar wind nebula (PWN) DA 495 and other very-high-energy (VHE; $>100~\textrm{GeV}$) gamma-ray emitters, showed inconsistent results across different VHE experiments, including differences in the measured flux of DA 495 and in the number of reported sources. Our new dedicated analysis using 3071 days of HAWC data resolves these discrepancies. We identify three extended sources, HAWC J1952+2924 (DA 495), HAWC J1954+2837, and HAWC J1958+2848, all with curved spectra, and find a hint of a fourth source. For DA 495, a multi-wavelength analysis, including our results, radio, X-ray, and other gamma-ray data, reveals that its extended emission is best described by leptonic interactions with an inferred MAGNETic field of $B\sim10~μ\textrm{G}$ and that hadronic components are not required. On the other hand, we interpret the other two sources, which have no confirmed counterparts, as TeV halos associated with nearby pulsars, PSR J1954+2836 and PSR J1958+2846, respectively. These results reinforce the interpretation of DA 495 as a leptonic-dominated PWN and add two candidates to the growing population of TeV halos.
[abstract 7 / 29] (score: 3) - Title: Cosmic rays density fluctuations with turbulence universal spectrum -8/3Authors: Artem S. Chefranov, Sergey G. Chefranov, Georgy S. Golitsyn,Comments: 10 pages, 2 figureSubjects: astro-ph.HE physics.flu-dynCreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
An exact turbulence universal scaling law-8/3 for the density fluctuations of COSMIC RAY (CR) is obtained on the basis of a new analytical compressible turbulence theory and known two-fluid model of the CR dynamics. It is shown that the origin of this scaling law may be due to the breaking of the nonlinear simple waves in CR medium near the scale of their Larmor radii as for the space plasma of solar wind and MAGNETosheath.
[abstract 8 / 29] (score: 3) - Title: On the ideal MAGNETohydrodynamic stability of the sheared-flow Z pinchAuthors: Daniel W. Crews, Jackson C. Turner,Comments: 21 pages, 16 figures. Accepted for publication in Physics of PlasmasSubjects: physics.plasm-ph physics.flu-dynCreated: 2026-10-08; Updated: 2026-10-12; Datestamp: 2026-10-12
Sheared-flow Z-pinch stability has previously been studied within ideal MHD primarily through growth rate calculations, which find that even trans-Alfvénic sheared flows apparently fail to suppress the kink instability. Here, trans-Alfvénic sheared flow is shown to stabilize the MHD kink but also to excite shear-driven instabilities characteristic of high-Reynolds-number supersonic flow. This distinction is evident from the dispersion relations underlying the growth rates, computed as the analytic dispersion function in the complex-frequency plane. Regularization splits this function into adiabatic and resonant parts describing how discrete modes emerge from and interact with the continuous spectrum. The Doppler-shifted flow continuum is then seen to interact with the interchange and kink instabilities in distinct ways. For interchange, the continuum overlaps the instability branch at all wavenumbers, so even sub-Alfvénic sheared flow stabilizes profiles modestly beyond the interchange threshold. The kink, by contrast, is shielded from the continuum by a frequency gap, and trans-Alfvénic flow is required to Doppler-shift the continuum into resonance with it, giving a geometric picture of the stabilization threshold. But shear-driven instabilities arise at this same threshold, including reflection modes and an acoustic kink. It is these shear-driven modes, not the original MHD instabilities, that dominate the ideal-MHD spectrum in trans-Alfvénic conditions. The ideal analysis thus describes the stabilization mechanism while showing that the stability of the sheared-flow Z pinch ultimately rests on non-ideal physics, such as finite orbit width and dissipation.
[abstract 9 / 29] (score: 3) - Title: Investigating the nature of MAGNETic turbulence in Tycho's SNR using X-ray observationAuthors: Ashwin Aravindaraj, Hui Zhu, Adrien Picquenot, Hsiang-Kuang Chang,Comments: Accepted for publication in MNRASSubjects: astro-ph.HECreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
Supernova remnants (SNRs) are widely regarded as the primary sources of Galactic COSMIC RAY acceleration and the particles are energized at the shock front of SNRs through the diffusive shock acceleration (DSA) mechanism, gaining energy by repeatedly crossing the shock. Magnetic turbulence plays a crucial role in scattering these particles back and forth, making the investigation of turbulence essential to understanding the acceleration process. In this study, we apply the two-point correlation method to derive the MAGNETic energy spectrum from the non-thermal X-ray flux image of Tycho's SNR. This image was obtained using Poissonian-based Generalized Morphological Component Analysis (pGMCA). The turbulence length scale observed in the resulting spectrum is shorter than the turbulence scale derived from previous studies of radio observations of Tycho's SNR. Additionally, we use the X-ray rim thickness measured across Tycho which is an indicator of MAGNETic field strength to estimate the MAGNETic energy spectrum. The turbulence scale inferred from this method is consistent with that obtained from the non-thermal X-ray flux analysis.
[abstract 10 / 29] (score: 3) - Title: Quasi-periodic oscillations in Letelier BLACK HOLEs within Kalb-Ramond gravity embedded in a uniform external MAGNETic fieldAuthors: Ahmad Al-Badawi, Shokhzod Jumaniyozov,Comments: 17 pages, 14 figuresSubjects: gr-qcCreated: 2026-10-08; Updated: 2026-10-12; Datestamp: 2026-10-12
We investigate the dynamics of charged test particles around a Letelier BLACK HOLE, i.e. a BLACK HOLE surrounded by a cloud of strings (CoS), in Kalb-Ramond (KR) gravity, immersed in an external, asymptotically uniform MAGNETic field aligned with the symmetry axis. The geometry depends on the CoS parameter and on the Lorentz-violating KR parameter only through a single combination of the two, so that the two effects can compensate each other and the Schwarzschild metric is recovered when both parameters are equal. Because the spacetime is not Ricci flat, the Wald potential is not a solution of the Maxwell equations; we show that the regular source-free MAGNETic test field is given in closed form by a Gauss hypergeometric function of the radial coordinate, which reduces to the Wald solution in the Schwarzschild limit. Using this exact field we derive the equations of motion, the effective potential, the circular orbits, the innermost stable circular orbit (ISCO), representative escaping, captured and curled trajectories, and the orbital, radial and vertical epicyclic frequencies in closed form; all frequency expressions are cross-checked against direct numerical integration of the full equations of motion. Within the RELATIVISTIC precession model, we perform a Markov chain Monte Carlo (MCMC) analysis of the twin-peak high-frequency quasi-periodic oscillations (QPOs) of GRO J1655-40, XTE J1550-564 and GRS 1915+105 for four nested models, complemented by nested sampling to compute Bayesian evidences and to weight the two (Larmor and anti-Larmor) MAGNETic modes of the posterior. The Schwarzschild model is excluded for GRO J1655-40 and XTE J1550-564, with a difference in the Akaike information criterion of about 110.
[abstract 11 / 29] (score: 3) - Title: The Population of Type~1 Active Galactic Nuclei in Dark Energy Spectroscopic Instrument. I. Profile-dependent Measurements of the Low-redshift SampleAuthors: Zhu-Heng Yao, Wei-Jian Guo, Shuo Zhai, Yu-Chang Li, Cheng Cheng, Jun-Rong Liu, Shuang Jin, Antonios Katsianis, Jing Wang, Da-Wei Xu, Jian-Yan Wei,Comments: 24 pages, 14 figures; Accepted for publication in ApJSSubjects: astro-ph.GACreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
We present a spectral analysis of a large sample of low-redshift type 1 ACTIVE GALACTIC NUCLEi (AGNs) selected from the first data release of the Dark Energy Spectroscopic Instrument (DESI DR1). For objects at $z\le0.9$, we perform spectral fitting and ML-assisted refinement, yielding 114,754 type 1 AGNs. We use two fitting schemes that differ only in the broad-line model: the broad Balmer components are fitted with either a Lorentzian function or a sum of Gaussians. The continuum and [O III] luminosity measurements agree closely between the two schemes, whereas the Gaussians scheme generally yields larger broad-H$β$ full width at half maximum (FWHM) values, larger virial BLACK HOLE masses, and lower accretion rates. The adopted broad-Balmer profile also changes the decomposition of narrow Balmer emission. Specifically, the anti-correlation between [O III]$\lambda5007$/narrow H$β$ and accretion rate is stronger under the Gaussians scheme with a Spearman rank correlation coefficient $r_{\rm s}=-0.412$, than under the Lorentzian scheme with $r_{\rm s}=-0.206$; the same tendency is observed in the narrow-line Seyfert 1 galaxies (NLS1s) subset ($r_{\rm s}=-0.435$ and $-0.259$ for the Gaussians and Lorentzian schemes, respectively), suggesting that the Gaussians scheme may provide a more self-consistent separation of the broad and narrow H$β$ components. Moreover, the consistent correlations recovered under both profile prescriptions favor a continuous type 1 accretion-state sequence, with NLS1s occupying its high-accretion end rather than constituting a distinct population.
[abstract 12 / 29] (score: 3) - Title: Extreme mass ratio inspirals from the Hills mechanism, The eccentricity distribution of Hills EMRIs in LISAAuthors: Biancamaria Sersante, Davide Mancieri, Kevin Leopoldo Muñoz Zavala, Luca Broggi, Zephyr Penoyre, Elena Maria Rossi, Alberto Sesana,Comments: 18 pages, 12 figuresSubjects: astro-ph.HECreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
Extreme mass ratio inspirals (EMRIs) are promising sources for future space-based gravitational-wave detectors. We investigate EMRIs produced through the Hills mechanism, in which a stellar-mass black-hole binary (BBH) is tidally separated by a massive BLACK HOLE (MBH), leaving one component bound to it. We present the first self-consistent modelling of this channel, combining an orbit-averaged Fokker-Planck treatment of the nuclear star cluster (NSC), three-body modelling of the binary-MBH encounter, Monte Carlo evolution of captured BLACK HOLEs (BHs), and fully RELATIVISTIC EMRI trajectories to follow the evolution from binary supply down to final plunge. We find that Hills EMRIs are substantially more circular than classical EMRIs formed through two-body relaxation. For an MBH of $4 \times 10^6 M_\odot$ and circular, equal-mass BBHs of $20 M_\odot$ with initial separation of $0.1$ AU, EMRI mean eccentricities are approximately $0.097$ at our adopted LISA-band entry threshold and $0.034$ at plunge, compared with $0.478$ and $0.228$, respectively, for classical EMRIs. Of the initial BBHs, approximately $0.4$ per cent become EMRIs, whereas approximately $60$ per cent of captured BHs do. For comparable NSC initial compact-object mass, we find approximately $1.6 \times 10^{-8}$ Hills EMRIs per year per galaxy, approximately $12$ per cent of the classical EMRI yield. The Hills channel contribution to the overall eccentricity distribution depends strongly on the binary mass fraction in NSCs. We discuss implications for identifying EMRI formation channels with LISA and for quasi-periodic eruptions.
[abstract 13 / 29] (score: 3) - Title: Implementation and verification of a new free boundary module for Resistive Wall Modes simulations with the nonlinear 3D full MHD code SpeCylAuthors: Francesco Galeazzi, Daniele Bonfiglio, Luca Spinicci, Susanna Cappello,Comments: 39 pages, 10 figures, 3 appendixesSubjects: physics.plasm-ph physics.comp-phCreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
Self-consistent numerical simulations of free boundary instabilities, such as resistive wall modes (RWMs) and external kink modes, require special attention given their relevance on the path towards MAGNETic fusion based nuclear reactors. In this work, a new implementation and a verification benchmark are presented for the nonlinear three-dimensional (3D) full MAGNETo-hydrodynamics (MHD) code SpeCyl, which self-consistently combines a free flow 3D treatment for the edge plasma velocity with double resistive wall thin shell MAGNETic boundary conditions, capable of capturing the essential features of common setups in experimental devices. Two coaxial resistive shells surround the plasma. Vacuum conditions are assumed between and outside the resistive shells, whose relative positions and time constants can be varied on purpose. The implementation is extensively verified against Shafranov's analytic theory, valid for a circular cross section large aspect ratio tokamak and assuming a flat current profile. The correctness of newly implemented Boundary Conditions (BCs) is confirmed by the good agreement obtained for the linear growth rates of (m=2,n=1) RWM and external kink, over a wide range of wall positions, resistive shell time constants, and for different initial reference equilibria. The (m=2,n=1) RWM growth rates are also benchmarked against previous different RWMs modelling and successful validation studies for RFX-mod tokamak plasmas. The new BCs make SpeCyl a flexible and robust tool to investigate free boundary MHD modes in large aspect ratio MAGNETic confinement configurations, such as those achieved with the RFX-mod machine and expected in RFX-mod2.
[abstract 14 / 29] (score: 3) - Title: Perpendicular transport in isotropic MAGNETic turbulence. The role of stochastic driftsAuthors: F. Pucci, P. Blasi, O. Pezzi, C. Evoli, F. Malara,Comments:Subjects: astro-ph.HECreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
In COSMIC RAY propagation through turbulent MAGNETic fields, transport perpendicular to the mean field plays an important role in various astrophysical environments. Numerical simulations have shown that parallel and perpendicular diffusion coefficients exhibit different energy scalings, causing their ratio to increase with energy, but a comprehensive theoretical explanation remains elusive. Here, we investigate perpendicular diffusion using test particle simulations in synthetic isotropic turbulence spanning 6-7 orders of magnitude in wavenumber, together with a theoretical extension of nonlinear guiding center theory that incorporates stochastic drifts. Our approach combines field line random walk and random guiding center drifts to describe perpendicular transport. We find that parallel and perpendicular diffusion coefficients exhibit the same energy scaling only for $r_L \lesssim 10^{-2} L_c$, where $r_L$ is the particle Larmor radius and $L_c$ is the turbulence coherence length. At higher energies, perpendicular diffusion develops a stronger energy dependence, consistently across different turbulence levels. Our theoretical model suggests that this behavior arises from stochastic drifts induced by turbulent MAGNETic field components parallel to the mean field.
[abstract 15 / 29] (score: 2) - Title: A Star's Death by a Thousand Cuts: The Runaway Periodic Eruptions of AT2023uqmAuthors: Yibo Wang, Tingui Wang, Shifeng Huang, Jiazheng Zhu, Ning Jiang, Wenbin Lu, Rongfeng Shen, Shiyan Zhong, Dong Lai, Yi Yang, Xinwen Shu, Tianyu Xia, Di Luo, Jianwei Lyu, Thomas Brink, Alex Filippenko, Weikang Zheng, Minxuan Cai, Zelin Xu, Mingxin Wu, Xiaer Zhang, Weiyu Wu, Lulu Fan, Ji-an Jiang, Xu Kong, Bin Li, Feng Lin, Ming Liang, Wentao Luo, Jinlong Tang, Zhen Wan, Hairen Wang, Jian Wang, Yongquan Xue, Dazhi Yao, Hongfei Zhang, Wen Zhao, Xianzhong Zheng, Qingfeng Zhu, Yingxi Zuo,Comments: Published in Science BulletinSubjects: astro-ph.HECreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
Stars on bound orbits around a supermassive BLACK HOLE may undergo repeated partial tidal disruption events (rpTDEs), producing periodic flares. While several candidates have been suggested, definitive confirmation of these events remains elusive. We report the discovery of AT2023uqm, a nuclear transient that has exhibited at least five periodic optical flares, making it only the second confirmed case of periodicity after ASASSN-14ko. Uniquely, the flares from AT2023uqm show a nearly exponential increase in energy--a "runaway" phenomenon signaling the star's progressive destruction. This behavior is consistent with rpTDEs of low-mass, main-sequence stars or evolved giant stars. Multiwavelength observations and spectroscopic analysis of the two most recent flares reinforce its interpretation as an rpTDE. Intriguingly, each flare displays a similar double-peaked structure, potentially originating from a double-peaked mass fallback rate or two discrete collisions per orbit. The extreme ratio of peak separation to orbital period draws attention to the possibility of a giant star being disrupted, which could be distinguished from a low-mass main-sequence star by its future mass-loss evolution. Our analysis demonstrates the power of rpTDEs to probe the properties of disrupted stars and the physical processes of tidal disruption, though it is currently limited by our knowledge of these events. AT2023uqm emerges as the most compelling rpTDE thus far, serving as a crucial framework for modeling and understanding these phenomena.
[abstract 16 / 29] (score: 2) - Title: New Signs Pointing Toward a Correlation Between Astrophysical Neutrinos and Radio FlaresAuthors: Yjan A. Gordon, Peter S. Ferguson, Eric J. Hooper, Michael N. Martinez,Comments: 15 pages, 11 figures, 5 tables. Published in OJAp. Supplementary data available at https://zenodo.org/records/23223067Subjects: astro-ph.GA astro-ph.HECreated: 2026-10-08; Updated: 2026-10-12; Datestamp: 2026-10-12
We use data from the first two epochs of the Very Large Array Sky Survey (VLASS) and the IceCube Neutrino Observatory to search for evidence of a correlation between radio variability and the detection of astrophysical neutrinos. Our work probes the radio population down to $S_{3\,\text{GHz}}\gtrsim$ a few mJy, more than an order of magnitude fainter than previous analyses that aim to cross correlate radio variability with neutrino detections. We find an excess number of associations between flaring radio sources and neutrinos that were detected between the first and second VLASS observations at $>2σ$ confidence. This excess is consistent with radio flares contributing $\sim13\,\%$ of the astrophysical neutrinos observed by IceCube. Notably, $\sim90\,\%$ of the radio flares associated with neutrinos are not detected at either $γ$-ray or X-ray wavelengths, highlighting the importance of deep radio observations for identifying potential electroMAGNETic counterparts to astrophysical neutrinos. No excess in the number of associations between the wider radio-variable population and the IceCube neutrinos is seen when no time constraint is placed on the neutrino detection. We predict that data from future VLASS epochs will see an excess number of associations between radio flares and neutrinos at the $>3σ$ level, and expected improvements to the positional constraints on the neutrinos may increase that confidence to $>5σ$, should our results be representative.
[abstract 17 / 29] (score: 2) - Title: Far-infrared Polarization Properties of Nearby Star-forming Regions: A New Compendium of SOFIA/HAWC+ ObservationsAuthors: Kaitlyn Karpovich, Susan E. Clark, Enrique Lopez-Rodriguez,Comments: 26 pages, 17 figures, 2 tables, Accepted to ApJSubjects: astro-ph.GACreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
We present a comprehensive polarimetric study of 26 nearby molecular clouds in four far-infrared bands (53 $μ$m~to 214~$μ$m) using 52 archival SOFIA/HAWC+ datasets{, over half of which are unpublished}. Far-infrared dust POLARIZATION observations probe the plane-of-sky MAGNETic field. To investigate scale-dependent trends, we group the molecular clouds by distance and analyze the data at common angular ($25''$) and common physical (0.052 pc and 0.32 pc) resolutions. The two shorter wavelengths are more impacted by smoothing, exhibiting a larger decrease in percent POLARIZATION. We analyze the POLARIZATION spectrum --- the POLARIZATION fraction as a function of wavelength --- and find that it depends more strongly on column density than dust temperature. We find a ``falling" spectrum at the 0.052 pc resolution, but find a ``flat" spectrum at the 0.32 pc resolution, suggesting that resolution plays an important role in the observed POLARIZATION spectra. We propose that warm dust grain emission in small-scale structures ($\lesssim$~0.1 pc) traces different MAGNETic field geometries only resolved in our {near} regime data. There is no preferred MAGNETic field orientation across our data, which suggests that the MAGNETic field in our $\sim$~parsec scale regions is decoupled from the large-scale field that is primarily parallel to the Galactic plane. The relationship between percent POLARIZATION and column density varies between clouds, but the correlation between percent POLARIZATION and {POLARIZATION angle} dispersion is consistent across regions. This compendium highlights the value of observing at multiple far-infrared wavelengths and enables additional population-level studies of MAGNETic fields and dust across star-forming environments.
[abstract 18 / 29] (score: 2) - Title: On the MAGNETic counterpart of the Uehling correctionAuthors: T. Azevedo, F. A. Barone, C. Farina, R. de Melo e Souza, G. Zarpelon,Comments: 11 pages + appendices, 3 figures; v2: added section on applications, updated reference listSubjects: hep-ph hep-thCreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
In this work, we investigate the MAGNETic properties of the quantum vacuum in the context of QED. We calculate the quantum RELATIVISTIC correction of virtual particle-anti-particle pair creation to the field of a classical point-like idealized MAGNET. Using such correction, we find the induced currents stemming from the effect of the POLARIZATION of the vacuum, which behaves like a paraMAGNETic medium. We also calculate the correction to the electric dipole potential and show that the well-known symmetry between the classical fields of point electric and MAGNETic dipoles is broken at the quantum level. Lastly, to illustrate possible applications of our findings, we briefly discuss the effect of the corrections obtained here in the context of neutron-neutron scattering and the hyperfine splitting for hydrogen-like atoms.
[abstract 19 / 29] (score: 2) - Title: Dynamics of fast MAGNETosonic wave turbulenceAuthors: Nicolás Pablo Müller, Sébastien Galtier,Comments:Subjects: physics.plasm-ph physics.flu-dynCreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
Fast MAGNETosonic waves are among the fundamental oscillation modes of astrophysical plasmas. To study their dynamics, we carry out numerical simulations of the wave turbulence kinetic equation, which describes the evolution of the energy spectrum of a set of weakly nonlinear fast MAGNETosonic waves. This kinetic equation, which involves three-wave interactions, has recently been derived from compressible MAGNETohydrodynamics in the low-$β$ limit (Galtier 2023). It has an exact stationary solution, the Kolmogorov-Zakharov spectrum, corresponding to a direct energy cascade. Here we perform free decay simulations of the kinetic equation for which we propose a Kolmogorov-type phenomenology to explain the temporal decay laws of energy and integral length scale. In the forced simulations, we show that the cascade is in fact composed of a mixture of a forward cascade for counter-propagating waves, and a backward cascade for co-propagating waves, with the former being stronger than the latter. The Kolmogorov-Zakharov energy spectrum in $k^{-3/2}$ is found in the radial direction with an anisotropy due to the amplitude that depends on the angle relative to the strong mean MAGNETic field. We give the analytical expression of the Kolmogorov-Zakharov constant, which is numerically verified in the high Reynolds number limit. Our study provides a theoretical explanation for certain observations in the solar wind plasma (Zhao et al. 2022), where a regime of weak turbulence has been identified for fast MAGNETosonic waves, alongside a critical balance regime for strong Alfvén wave turbulence.
[abstract 20 / 29] (score: 2) - Title: Observing the Peculiar Acceleration of our Solar System with Quasar Proper MotionsAuthors: Phu Huy Nguyen, Calum Murray,Comments: 18 pages, 17 figures, 1 table, updated figures and table, accepted for publication in Astronomy & Astrophysics (abstract shortened for ArXiv)Subjects: astro-ph.GA astro-ph.COCreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
We measured the proper motion dipole of QUASARs observed by \textit{Gaia} to determine the acceleration of the Solar System with respect to the QUASAR rest frame. We characterised the full angular power spectrum of the proper motion field using the pseudo-$C_\ell$ formalism and employed simulation-based inference to jointly constrain the dipole and higher multipole power. Cross-correlation with the \textit{Gaia} scanning strategy, stellar density and stellar proper motion maps was used to diagnose the origin of systematic power beyond the dipole. We applied this framework to both the \textit{Gaia} EDR3 QUASAR catalogue and the Quaia catalogue. The inferred acceleration is consistent with the previous determination, but the credible intervals widen by factors of 1.5 to 5 when higher-multipole degeneracies are properly marginalised, indicating that previous uncertainty estimates were optimistic. Our best estimate, based on the Quaia catalogue, is ($g_x,\,g_y,\,g_z$) = $\left(1.01^{+0.72}_{-0.72}, \,-4.94^{+0.54}_{-0.55},\,-2.13^{+0.58}_{-0.58}\right) \;\rm μas \,yr^{-1}$. This corresponds to an amplitude of $5.55_{-0.53}^{+0.54}\,\rm \;μas\,yr^{-1}$, where $\mathbf{g} = \mathbf{a}/c$ is the Solar System acceleration expressed as a proper motion drift in equatorial coordinates. The inferred acceleration is directed towards $(l,\, b) = \left(11.71^{+7.0}_{-6.8},\, -9.01^{+7.0}_{-6.9}\right)^\circ$, equivalently $(α,\, δ) = \left(281.39^{+7.8}_{-8.0},\, -22.93^{+6.5}_{-6.2}\right)^\circ$. This is in good agreement with a Galactic centre--dominated acceleration. The acceleration components show no significant dependence on source redshift, providing further evidence of the acceleration's kinematic origin.
[abstract 21 / 29] (score: 2) - Title: Breaking the Blend: A multi-tracer kinematic decomposition method for IFS data applied to disentangling the AGN outflow and circumnuclear ring in NGC 5728 with JWSTAuthors: Oscar Veenema, Niranjan Thatte, Dimitra Rigopoulou, Richard I. Davies, Miguel Pereira-Santaella, Ismael García-Bernete, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew J. Bunker, Françoise Combes, Tanio Díaz Santos, Fergus R. Donnan, Donaji Esparza-Arredondo, Federico Esposito, Santiago García-Burillo, Begoña García-Lorenzo, Omaira Gonzalez Martin, Laura Hermosa Muñoz, Erin K. S. Hicks, Sebastian F. Hönig, Masatoshi Imanishi, Alvaro Labiano, Nancy A. Levenson, Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Claudio Ricci, Rogemar A. Riffel, Marko Stalevski,Comments: 7 pages, 2 figures, MNRAS Letters accepted, Supplementary material available as an ancillary fileSubjects: astro-ph.GACreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
Integral field spectroscopy (IFS) of the central kiloparsecs of ACTIVE GALACTIC NUCLEi (AGN) reveals a mixture of spatially coincident emission from star-formation and AGN feedback exciting the interstellar medium. Disentangling these components remains a challenge, as most spectral tracers are affected by both processes, limiting robust interpretation of kinematics and energetics. We present a new framework for decomposing IFS data into distinct components on a spaxel-by-spaxel basis using a multi-tracer, stacked kinematics approach. This method combines kinematic modelling with imposed flux decomposition per spaxel, quantifying the contribution of each component across the field of view. We apply this method to JWST IFS observations of the Seyfert galaxy NGC 5728 from the Galaxy Activity, Torus, and Outflow Survey (GATOS), analysing twelve mid-infrared fine-structure lines (4.49 < $λ$ < 25.89 $μ$m, 7.9 < IP < 126.2 eV). We find that the circumnuclear emission can be decomposed into two dominant components: a star-forming ring and an AGN-driven biconical outflow. Our method separates these structures and recovers their detailed spatial morphology. This framework provides a general and scalable method for physically motivated component separation in IFS data, applicable across many wavelength ranges and targets, enabling reliable interpretation of complex emission line structures (or morphologies) in active galaxies and beyond.
[abstract 22 / 29] (score: 2) - Title: On the notion of kinetic energy in a spacetime of maximal proper accelerationAuthors: Ricardo Gallego Torromé,Comments: 19 pagesSubjects: physics.gen-ph gr-qcCreated: 2026-10-07; Updated: 2026-10-12; Datestamp: 2026-10-12
It is shown in this work that in spacetimes of maximal proper acceleration there are situations where a particle decelerates and simultaneously increases its kinetic energy. To illustrate the effect, a classical $1$-dimensional electric cavity-like scheme is discussed. The gain in kinetic energy by deceleration suggests an equivalence between velocity and acceleration from the energetic point of view. Such an equivalence is stated in a form resembling Born reciprocity principle but formulated in the framework of higher order JET spacetime geometry. We also show the existence in the theory of a dynamical superluminal sector for point particles with positive mass and characterized by superluminal speed and a proper acceleration larger than the maximal proper acceleration. Therefore, the speed of light and the maximal proper acceleration become only {\it separation conditions} at the classical level of the two dynamical sectors.
[abstract 23 / 29] (score: 2) - Title: A Burst of Reionization in the Dark AgesAuthors: Neal Weiner, Soubhik Kumar, Wenzer Qin, Zilu Zhou, Yacine Ali-Haïmoud, Hector Afonso G. Cruz,Comments: 17 pages, 13 figuresSubjects: astro-ph.COCreated: 2026-10-08; Updated: 2026-10-12; Datestamp: 2026-10-12
Primordial overdensities at small scales can be significantly larger than those observed at large scales. As a result, they can collapse much earlier, at redshifts $z \sim 100$. In these collapsed halos, stars and BLACK HOLEs can form, where they can then contribute to an early reionization of the universe. If this epoch is temporary, the free electrons will recombine yielding a low level of ionization leading into cosmic dawn. This contributes to the optical depth of the universe, and adds more weakly to low-$\ell$ POLARIZATION signals of ionization compared to later sources. We study the effects of a redshift-localized source of reionization $Δτ_{burst}$ in the context of a broad suite of cosmological data to constrain this scenario, finding a preference of approximately $\sim 2-2.5σ$ for a new contribution. Regardless of Planck reprocessing used (PR3 - SRoll2+plik or PR4 - LoLLiPoP+CamSpec/HiLLiPoP), the results are consistent, favoring a new contribution $Δτ_{burst} \sim 0.012$ ($0.001 < Δτ_{burst} < 0.022$ at 95\%) and a similar total optical depth $τ\sim 0.073$. The precise era of reionization is somewhat discrepant depending on the higher-$\ell$ reprocessing used, with HiLLiPoP favoring $z\sim 45$, CamSpec $z\sim 100$ and plik $z\sim 165$. If such a source is present at $40\lesssim z\lesssim150$, LiteBIRD should be able to detect it, while Simons Observatory should also constrain it.
[abstract 24 / 29] (score: 2) - Title: Flux Evolution of PSR B0540--69 and the Spectral Energy Distribution of its Pulsar Wind NebulaAuthors: Juan Zhang, Xuezhi Liu, Junyang Zhang, Hanlong Peng, Mingyu Ge, Songzhan Chen, Shanshan Weng, Shijie Zheng, Shumei Jia, Chengkui Li, Haisheng Zhao, Ju Guan, Yong Chen, Liming Song, Fangjun Lu,Comments: 11 pages, 5 figures, 5 tables, submittedSubjects: astro-ph.HECreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
The young Crab-like pulsar PSR B0540--69, located in the Large Magellanic Cloud, underwent a spin-down rate transition (SRT) in 2011 December, after which its pulsar wind nebula (PWN) was reported to brighten up to 2018. In this work, we extend the study of its X-ray and $γ$-ray flux evolution through 2026 by combining observations from multiple X-ray instruments with data from the FERMI Large Area Telescope, thereby constructing a flux history of the PSR$+$PWN system spanning more than two decades. We find that the enhanced X-ray luminosity of the PSR$+$PWN system has persisted for more than 14 yr after the SRT, up to early 2026, whereas the pulsed X-ray flux remains unchanged across all epochs. This confirms that the brightening originates from the PWN. In the $γ$-ray band, neither the pulsed nor the non-pulsed flux shows any detectable long-term variation between 2008 and 2025. Together, these results imply that the additional spin-down energy released at the SRT has been continuously injected into the PWN over decades, placing strong constraints on the energy budget and physical mechanism of the transition. Combining the non-pulsed X-ray and $γ$-ray fluxes measured here with previously published radio-to-UV data, we further construct a broadband spectral energy distribution of the PWN, which shows properties markedly different from those of the Crab Nebula.
[abstract 25 / 29] (score: 2) - Title: Energy-dependent trapping of backscattered helium during MAGNETron sputtering growth: A molecular dynamics studyAuthors: Pascal Brault, Anne-Lise Thomann, Alejandro Borroto,Comments:Subjects: physics.comp-ph physics.plasm-phCreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
Helium incorporation during MAGNETron sputtering can strongly affect thin film growth and lead to the formation of gas/solid nanocomposites and nanoporous structures. Here, molecular dynamics (MD) simulations are used to investigate the trapping mechanism of helium atoms (He) and the subsequent formation of He bubbles during the sputter deposition of aluminum (Al) and titanium (Ti) thin films. The simulations account for the kinetic energy distributions of sputtered metal atoms and backscattered gas species. Results indicate that He is efficiently incorporated into the growing films, leading to the formation of high-pressure, dense He bubbles, with a much higher He-to-metal atomic ratio in Ti ($\sim$ 60%) than in Al ($\sim$ 12%). More importantly, the simulations reveal a clear energy dependence of He trapping in Ti: background He atoms at thermal energies are essentially not incorporated, whereas efficient trapping starts at an incident energy of approximately 20 eV and increases up to a saturation regime near 100 eV. Simulated thermal desorption spectroscopy (TDS) further reveals distinct release mechanisms in the two investigated metals: He desorption from Al occurs at higher temperatures and is preceded by the removal of surface Al atoms, whereas He and Ti atom desorption starts continuously around 950 K, leading to a porous structure. Comparative simulations with argon (Ar) demonstrate negligible trapping even at comparable kinetic energy or momentum, showing that neither parameter alone accounts for the strong He incorporation observed in Ti. The above results are in very good agreement with what is reported in literature for low-kinetic energy He ion implantation in metal surfaces, suggesting similar insertion mechanisms. They clarify the atomistic conditions governing noble gas trapping during film growth and provide a basis for controlling He incorporation and porosity in films synthesized by MAGNETron sputtering.
[abstract 26 / 29] (score: 2) - Title: Magnetic connectivity from the Sun to the Earth with MHD models II. Impact of input MAGNETic mapsAuthors: Barbara Perri, Silke Kennis, Brigitte Schmieder, Stefaan Poedts,Comments: 9 pages, 4 figures, accepted in A&ASubjects: astro-ph.SR physics.space-phCreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
Connectivity estimation needs to be fast and thus usually relies on semi-empirical models. We previously established that optimised MAGNETohydrodynamics (MHD) models can also be used to derive MAGNETic connectivity, yielding good results, especially for complex configurations. However, the modelling is not the only factor that can impact the connectivity estimation. Models' results, both semi-empirical and MHD, depend heavily on the input data used to drive the simulation. In order to quantify this impact on our connectivity estimation, we used 20 different maps by four providers. We selected the period of July 2019, which corresponds to Carrington rotation (CR) number 2219, because it had already been studied in a previous paper. It corresponds to a period of minimum activity, meaning minimal interference from transient structures, but with a high-speed stream and several polarity switches. We have compared our results with in situ data from ACE and developed several visualisation techniques to validate connectivity not only for a specific date but also for a full CR. The choice of the input MAGNETic map drastically affects the connectivity estimates, with global scores going from 28% global agreement to 63% in the most extreme case. The HMI and GONG maps consistently gave the best connectivity estimations, with more than 50% correct results of the full CR. For this specific period, the GONG-ADAPT maps yielded the least reliable results, with a score below 35%. This is not surprising, as we have shown before that COCONUT required parameter adjustments for these maps. However, WSO maps which showed poor coronal agreement actually provided good connectivity estimates, showing that the Heliospheric Current Sheet (HCS) location is in the end the most crucial parameter for connectivity. Consistent data over a full Carrington rotation are to be favored compared to daily.
[abstract 27 / 29] (score: 2) - Title: High Resolution Spectro-Polarimetric Observations of the Optical Filaments surrounding NGC 1275 with ESPaDOnSAuthors: Benjamin Vigneron, Julie Hlavacek-Larrondo, Luca Fabiani, Lison Malo, Carter Lee Rhea, Megan Donahue, Jorge Karolt Barrera Ballesteros, Hyunseop Choi, Nadine Manset,Comments: 19 pages, 7 figures, 3 tables, accepted for publication in ApJSubjects: astro-ph.GACreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
We analyze archival high spectral resolution ESPaDOnS spectropolarimetric observations (R = $λ/Δλ$ = 68000) of three targeted locations within the filamentary nebula surrounding NGC 1275. We present here the analysis of the main filaments emission lines, namely: [NII]$\lambda6584$, H$α$, and [NII]$\lambda6548$, across our three pointings displaying clear detectable emission, with one also showing additional [SII]$\lambda6716$ and [SII]$\lambda6731$ emission line doublet. Using a Markov Chain Monte-Carlo (MCMC) algorithm and thanks to the exceptionally high spectral resolution of the observations, we resolve for the first time each of the emission lines within one of the pointings into a set of three emission components with a remarkable velocity dispersion contrast ($σ_1 \sim 25$ km/s, $σ_2 \sim 90$ km/s and $σ_3 \sim 208$ km/s). We also perform flux ratios of the three detected emission components, which reveal differences in electron density and ionization sources. Consequently, the ESPaDOnS observations appear to reveal for the first time the overlap of an outer quiescent filament and a central turbulent filament likely affected by the AGN activity at a distance of $\sim 6.8''$ ($\sim 2.5$ kpc) from the central BCG. Finally, ESPaDOnS polarimetric data of one of the pointing allows us to confirm an average linear POLARIZATION degree of $\sim 0.15-0.14\%$ and an angle of POLARIZATION of $5.3\pm25.7^\circ$ for the optical emission of the filaments, as well as POLARIZATION dips associated with the H$α$ emission line and its multiple emission components. We interpret these features and measurements as tentative POLARIZATION due to dust scattering.
[abstract 28 / 29] (score: 2) - Title: A strategy for astrometric QUASAR selection with Gaia DR3 and its application to discover new luminous $z>2$ QUASARsAuthors: J. Li, J. P. U. Fynbo,Comments: Submitted to A&A. 12 pages, 31 figuresSubjects: astro-ph.GACreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
We aim to provide a cookbook for purely astrometric selection of QUASARs with Gaia DR3 and to provide an example of its use for the identification of very luminous $z>2$ QUASARs. We analyse the Gaia DR3 astrometry of confirmed QUASARs and stationary sources. We show that the proper motion signal to noise $μ/σ_μ$ follows a Rayleigh-like distribution. We also show the importance of properly taking into account the correlation between proper motions in right ascension and declination, as well as the non-linear error propagation. We adopt the Mahalanobis distance to the null proper-motion hypothesis. A scaled $χ^2$ distribution with $k=2$ and scale $s=1.1485$ is fitted to Gaia-CRF3; the corresponding $\pm2σ$ Gaussian-equivalent threshold is $D^2_{M(μ)}<7.097$. The final criteria combine this with the parallax condition and $\mathrm{ruwe}<1.4$. Applying the new criteria to the SDSS DR16Q confirmed QUASARs, the recovery rate is $90.25\%$. The suggested purely astrometric selection significantly improves both completeness and purity compared to other strategies used in the literature, reaching a QUASAR purity of approximately $95\%$ ($\sim2σ$ Gaussian-equivalent). It can be used to improve the selection purity and completeness for future QUASAR surveys. As an example, we use the suggested strategi to locate 24 very bright $z>2$ QUASARs without redshifts in the literature. Our proposed astrometric selection strategy recovers 95\% of known QUASARs. Its potential use for new discoveries is demonstrated by the identification of 24 very luminous $z>2$ QUASARs. Ten of these are new discoveries and for an additional seven we correct the redshifts determined by other methods.}
[abstract 29 / 29] (score: 2) - Title: A dust-reddened QUASAR in a [C II]-luminous host at z=6.55Authors: Daming Yang, Joseph F. Hennawi, Rychard Bouwens, Timo Kist, Eduardo Bañados, Hiddo S. B. Algera, Aaron J. Barth, Sarah E. I. Bosman, Frederick B. Davies, Anna-Christina Eilers, Xiaohui Fan, Victoria A. Fawcett, Yuming Fu, Anniek J. Gloudemans, Francesco Guarneri, Bin Jia, Elia Pizzati, Huub Röttgering, Jan-Torge Schindler, Feige Wang, Jinyi Yang,Comments: 11 figures, 2 tables, including appendicesSubjects: astro-ph.GACreated: 2026-10-09; Updated: 2026-10-12; Datestamp: 2026-10-12
Most known QUASARs at $z>6$ were selected through their rest-frame UV emission. Only a small number of reddened QUASARs have been identified at these redshifts, leaving their nuclear and host-galaxy properties poorly constrained. We present JWST/NIRSpec spectroscopy and ALMA band 6 observations of the QUASAR J1440+0019 at $z=6.5488$, revealing its dust-reddened nature and jointly characterizing its nucleus and host galaxy. The continuum is best described by an SMC-like extinction law with $E(B-V)=0.20\pm0.03$. Three absorption systems detected in N V, Si IV, and C IV are blueshifted by approximately $900$--$3600$ km s$^{-1}$ and likely trace an ionized nuclear outflow. The broad Mg II line and extinction-corrected continuum yield a black-hole mass of $\log(M_{\rm BH}/M_\odot)=9.04\pm0.42$, a bolometric luminosity of $L_{\rm bol}\simeq1.1\times10^{47}$ erg s$^{-1}$, and an Eddington ratio of $λ_{\rm Edd}\simeq0.8$. ALMA observations further reveal its host galaxy to be among the most [C II]-luminous known at $z>6$, with $L_{\mathrm{[C II]}}=(7.21\pm0.25)\times10^9 L_\odot$. For a fiducial dust temperature of 47 K and emissivity index $β=1.6$, the dust continuum implies $L_{\rm TIR}=8.9\times10^{12} L_\odot$ and $M_{\rm dust}=4.0\times10^8 M_\odot$. The inferred dynamical mass places J1440+0019 in the region of the $M_{\rm BH}$--$M_{\rm dyn}$ plane occupied by high-redshift blue QUASARs. These observations reveal a moderately reddened, rapidly accreting QUASAR in a luminous, dust-rich host during reionization. Its measured nuclear and host-galaxy properties provide an observational reference for identifying and characterizing similar systems in future systematic searches with wide-area infrared surveys.
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