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Physics Astrophysics

astro-ph Watch Astrophysics

Saturday 13 June

Earth and Planetary Astrophysics

Tracking low-velocity ejecta from the DART impact on Dimorphos

Isabel Herreros and Sébastien Charnoz

The DART impact on Dimorphos produced a large population of low-velocity ejecta (v < vesc), likely containing most of the excavated mass, whose early fate remains poorly constrained. We investigate the first 22 h evolution of ejecta launched at 1-9 cm/s and assess how orbital dynamics and surface transport after first contact shape the surface distribution of the re-accreted ejecta blanket. We use RAVEL, a model that couples three-dimensional orbital dynamics in the Didymos-Dimorphos system with surface transport on a digital terrain model, including detachment, re-impact, rebound, and frictional sliding. Re-accretion is rapid and asymmetric: more than 99% of the re-accreted mass returns to Dimorphos within 5 h. The slowest ejecta remain concentrated near the DART crater and dominate the primary ejecta blanket, whereas faster particles undergo orbital transport and preferentially populate antipodal and trailing regions. Surface motion strongly modifies the first-contact pattern, and the DART-derived rough terrain model produces elongated, topographically channelled depositional streaks dominated by the slowest ejecta, giving rise to a ray-like pattern. These results provide testable predictions for ESA's Hera mission and link ejecta-blanket morphology to orbital dynamics, re-accretion, and surface topography.
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Earth and Planetary Astrophysics

Comprehensive Statistical Validation of TOI-7701.01: A Sub-Saturn Companion at the Giant Planet Boundary

Biel Escolà-Rodrigo

We present the formal statistical validation of TOI-7701.01 (TIC 122522333), a sub-Saturn transiting companion candidate orbiting a bright F-type subgiant host star ($V=11.09$). Initially detected via an automated machine-learning transit survey by Salinas et al. (2025), the planetary nature of this signal remained unclear. We implement an independent vetting and statistical pipeline leveraging multi-sector space kinematics and the triceratops Bayesian framework to compute false positive scenarios. A key methodological finding is the structural convergence of the companion's physical scale; despite utilizing un-detrended Simple Aperture Photometry (SAP) with a raw depth of $2417$ ppm to preserve field dilution metrics, the triceratops MCMC engine naturally converges on a physical radius of $7.86\,R_\oplus$ under the dominant Target Planet scenario ($\mathcal{P}_{\rm TP} = 78.1\%$). This independent statistical derivation matches the geometric radius of $8.07\,R_\oplus$ inferred directly from the instrumentally corrected Pre-Search Data Conditioning (PDCSAP) data. By aggregating our multi-iteration ensemble to suppress MCMC stochasticity, we derive a robust global False Positive Probability ($\mathrm{FPP} = 0.00191$) and a Nearby False Positive Probability ($\mathrm{NFPP} < 10^{-6}$), firmly validating the companion well below the rigorous $1.5\%$ threshold established for this Bayesian framework. While the derived $7.8\text{--}8.1\,R_\oplus$ radius places the object at the boundary between giant planets and low-mass brown dwarfs, such a radius is highly atypical for a brown dwarf, pointing to a planetary nature. We report TOI-7701.01 as a validated companion and encourage prompt radial velocity characterization.
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Astrophysics of Galaxies

Consistency between X-ray and UV-Optical reverberation measurements in NGC 5548

Amit Kumar Mandal, Bożena Czerny, Michal Dovčiak et al. (+2 more)

The hard X-ray$-$emitting hot corona is a key component of active galaxies. Constraints on the hot corona height can be derived from reverberation studies in both the X-ray and optical bands. X-ray reverberation (X-ray$-$RM) studies often imply a very low corona height, whereas UV/optical reverberation mapping (photometrcic continuum$-$RM) typically points to a much larger one. To reconcile this discrepancy, we examine the constraints provided by both methods for the same source. We adopt a uniform methodology using the KYNSED and KYNXiltr codes within a consistent modeling framework for reverberation mapping, applicable across both the X-ray and UV-optical spectral and time domains. We select the source NGC 5548, for which the necessary observational data are available in the literature. We carry out our analysis for NGC 5548, a source with extensive reverberation mapping data obtained independently in the X-ray and UV-optical bands across different epochs. Our results hint for a substantial discrepancy between the global parameters required to reproduce the X-ray and those needed to fit the UV-optical reverberation signals. In particular, the mismatch in the inferred black hole mass and accretion rate presents a significant challenge for interpreting the observed time delays within a unified reflection-based framework. Our unified reflection-based modeling sheds light on X-ray and UV-optical variability of NGC 5548, but discrepancies in black hole mass, accretion rate, and corona properties might imply fundamental challenges to a self-consistent model. However, future analyses leveraging extended X-ray dataset with improved treatment of absorption and variability coherence are crucial to obtaining more robust constraints.
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All authors Amit Kumar Mandal, Bożena Czerny, Michal Dovčiak, Elias Kammoun, Iossif Papadakis

High Energy Astrophysical Phenomena

Constraining hydrodynamic model of nearby type IIP SN 2023ixf

V. P. Utrobin and N. N. Chugai

Despite proximity of SN 2023ixf and a wealth of observational data, the released hydrodynamic models leave too broad range of the derived explosion energy and the ejected mass. We revisit the hydrodynamic modeling based on a broader set of observables than have been previously used. Among those of top priority is the early maximum ejecta velocity that is crucial in removing parameter degeneracy. The inferred parameters of SN 2023ixf are the explosion energy of 2.8x10^{51} erg, ejecta mass of 13.2 Msun, presupernova radius of 1540 Rsun, and Ni-56 mass of 0.07 Msun. The circumstellar matter is composed by the dense circumstellar shell with the mass of 0.01 Msun and radius of 5x10^{14} cm, as well as the external rarefied wind. Both circumstellar components are consistent with the early H-alpha broad wings caused by the Thomson scattering and the intrinsic column density provided by X-ray data. Based on the radiation hydrodynamics we, for the first time, simulate the SN 2023ixf phenomenon from the explosion to the emergence of the hard X-ray radiation.
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High Energy Astrophysical Phenomena

Comparison of X-ray Emission Properties of TDEs and Soft Flares from AGNs

Samaresh Mondal, K. Decker French and Jason T. Hinkle

X-ray flaring activity from active galactic nuclei (AGNs) may mimic the expected emission from tidal disruption events (TDEs), thus contaminating TDE searches. To compare X-ray emission properties between TDEs and AGNs, we cross-match publicly available XMM-Newton and Swift-XRT point source catalogs with the Million Quasars Catalog and optically selected TDEs. We find that AGNs tend to become softer with a similar hardness ratio (HR) value as TDEs during their flaring events. The soft HRs during flaring events in these AGNs are driven by the emergence of a blackbody-like component below $\sim$2 keV, likely associated with the soft X-ray excess, as well as the continuum emission becoming steeper with the increase of accretion rate. We find 2.5% in XMM-Newton (23 out of 920) and 4.4% in Swift-XRT (179 out of 4089) AGNs display flares with peak count rate $>$$2\sigma$ from the median count rate and peak HR$<$$-0.75$. The rate of such flares in XMM-Newton and Swift-XRT is (1.1-2.5)$\times10^{-3}\rm\ galaxy^{-1}\ yr^{-1}$ and (0.9-2.0)$\times10^{-3}\rm\ galaxy^{-1}\ yr^{-1}$, respectively. We also estimate the rate of flares with a maximum flux change (peak/min) of $>20\times$ over on a rest-frame time scale of two years or more with a HR$<$$-0.75$ at peak to be (4.7-11.0)$\times10^{-5}\rm\ galaxy^{-1}\ yr^{-1}$ and (3.1-7.1)$\times10^{-5}\rm\ galaxy^{-1}\ yr^{-1}$ in XMM-Newton and Swift-XRT, respectively. Finding an optical or infrared counterpart may help to identify these flaring AGNs. We confirm 61% and 79% of flaring sources from XMM-Newton and Swift-XRT, respectively, as AGNs through variability in ZTF light curves or a WISE $W1$$-$$W2$$>$0.8 mag color cut.
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High Energy Astrophysical Phenomena

Mapping Domain-Wall Bayesian Reconstruction with LISA

Satyabrata Datta and Rome Samanta

We study the Bayesian reconstruction of peaked domain-wall gravitational-wave signals at LISA and construct reconstruction maps over the signal-parameter plane. These maps identify the regions in which the signal can be probed with minimal posterior uncertainty and parameter degeneracy. Our analysis employs a two-parameter domain-wall spectral template and includes isotropic, unmodulated astrophysical foregrounds from Galactic double white-dwarf binaries and extra-galactic compact binaries, together with LISA instrumental noise. The inference is performed for 64 injection points distributed on an equidistant grid using nested sampling, and the resulting posterior quantities are interpolated with the Clough–Tocher method to generate smooth maps over the full parameter plane. We find that LISA reconstructs domain-wall signals most effectively when the annihilation temperature lies approximately in the range $10^3\text{--}10^6\,\mathrm{GeV}$. In this regime, the posterior becomes both tighter and less degenerate, enabling genuine two-parameter reconstruction. The most favorable region corresponds to signals with ${\rm SNR}\gtrsim 50$, while signals with ${\rm SNR}\sim 10$ can still be reconstructed effectively only in a narrower part of parameter space concentrated near $T_*\lesssim 10^5\,\mathrm{GeV}$. In terms of the observable spectrum, this weaker-signal region corresponds approximately to peak amplitudes $\Omega_{\rm GW}^{\rm peak}h^2 \gtrsim 4\times10^{-11}$ and peak frequencies typically satisfying $f_p\lesssim 10\text{--}20\,{\rm mHz}$. Our results provide a quantitative reconstruction forecast for peaked domain-wall signals in the LISA band and a useful guide for particle-physics realizations of domain walls that predict peaked gravitational-wave spectra in the milli-Hz range.
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Astrophysics of Galaxies

PEARLS: NuSTAR and XMM-Newton Extragalactic Survey of the JWST North Ecliptic Pole Time Domain Field VI: Multiwavelength SED Analysis

Rafael Ortiz III, Francesca Civano, Rogier A. Windhorst et al. (+27 more)

We model spectral energy distributions of 261 X-ray sources to $z \sim 5$ in the North Ecliptic Pole Time Domain Field, extending prior XMM-Newton and NuSTAR analyses. Using the star-forming main sequence (SFMS) and black hole accretion rate (BHAR) frameworks, we find that SFRs generally lie below the SFMS while most BHARs exceed the population average, as expected for X-ray-selected samples. There is a strong correlation ($\rho=+0.73$) between SFR relative to the SFMS and specific AGN luminosity, $L_{AGN}/M_*$; galaxies with the highest $L_{AGN}/M_*$ exist at or above the SFMS. X-ray luminosity correlates with SFR ($\rho=+0.80$), revealing a star-forming and X-ray luminous "cold quasar" population consistent with dramatic, short-timescale accretion episodes. Low-mass galaxies show BHARs well above the population averaged value for their mass whereas high-mass galaxies' SMBHs accrete at the population averaged BHAR, suggesting "growth spurt" and "maintenance-mode" accretion, respectively. Traditional AGN classifications (obscured, unobscured, or radio-loud) do not reveal these distinctions, demonstrating the X-ray perspective's unique ability to identify rare AGN phases that are critical for the instantaneous link between galaxies and their SMBHs.
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All authors Rafael Ortiz III, Francesca Civano, Rogier A. Windhorst, S. P. Willner, Gibson B. Bowling, Timothy Carleton, Seth H. Cohen, Samantha Creech, Vicente Estrada-Carpenter, Brenda L. Frye, Norman A. Grogin, Heidi B. Hammel, Timothy Heckman, Rachel Honor, Rolf A. Jansen, Satoshi Kikuta, Anton M. Koekemoer, Madeline A. Marshall, Sylvia Mesicek, Mar Mezcua, Stefanie N. Milam, Simon D. Mork, Rosalia O'Brien, Payaswini Saikia, Ross M. Silver, Brent M. Smith, Hyewon Suh, Christopher N. A. Willmer, Haojing Yan, Xiurui Zhao

Instrumentation and Methods for Astrophysics

Spiking Neural Dedispersion: A Neuromorphic Fast Radio Burst Detection Pipeline

Alessio Magro

Real-time FRB detection at next-generation radio telescopes is increasingly dominated in cost and footprint by the real-time dedispersion backend. We present a complete neuromorphic FRB detection pipeline built on the Spiking Neural Dedispersion (SND) algorithm, a hierarchical delay-and-add tree that performs incoherent dedispersion on spike-encoded filterbank data, supporting arbitrary trial-DM grids and configurable branching factors. Three operating modes are evaluated, spanning a resource-sensitivity trade-off from binary thresholded accumulation to full float32 precision. Validated against Heimdall on synthetic Northern Cross filterbanks, float SND matches Heimdall at 99.3% detection completeness (244 mW per beam), graded mode achieves 89.3% at 61 mW, and binary mode reaches 59.4% overall (1.75 mW), retaining 91% sensitivity for bright, narrow events. The full pipeline fits on a single SpiNNaker 2 chip across all three modes; binary mode fits entirely within on-chip SRAM, while graded and float require external DRAM for the history buffer. On a deployed 48-chip system, total power projects to approximately 100-112 W, a reduction of order 10-40x over an equivalent GPU deployment, with 48 simultaneous beams per board.
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Instrumentation and Methods for Astrophysics

GridFire: A new, open source, nuclear network for stellar structure and evolution

Emily M. Boudreaux and Aaron Dotter

We present a novel nuclear network implementation, GridFire, which has been developed with a focus on efficiency, ease of use, and automatic physical extension. In this first paper we provide a detailed overview of GridFire's numerics, performance characteristics, and a comparison to pre-existing nuclear network implementations pynucastro and MESA's net module. We find that generally GridFire performs similarly to and requires significantly less user input and setup than these current generation nuclear network codes. Further, GridFire has been developed with a flexible "view" based physics engine that allowing researchers to implement domain specific physics without modifying the underlying source code. GridFire has been released under an open-source license, GPL v3.0, and will eventually be incorporated into the forthcoming 4D-STAR stellar structure evolution code.
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Cosmology and Nongalactic Astrophysics · Cross-listed from hep-ph

Particle and Gravitational Wave Probes of Minimal Seesaw Neutrinos

Sanjoy Mandal, Rishav Roshan and Jose W. F. Valle

Observable gravitational waves (GWs) from first-order phase transitions (FOPTs) can coexist with distinct particle physics signatures. These include same-sign dilepton plus four~jet events at colliders, such as $e^+ e^-/\mu^+\mu^- \to \ell^\pm \ell^\pm 4j$, neutrinoless double beta decay, as well as charged lepton flavor violating (cLFV) processes such as $\mu \to e \gamma$. We explore this synergy within the minimal low-scale linear seesaw model. This framework successfully reproduces neutrino oscillation data, providing a direct avenue to probe the neutrino mass ordering and Majorana nature at colliders. Crucially, the FOPT responsible for the GW background is driven by a leptophilic Higgs doublet, establishing a direct link between early-universe cosmology and terrestrial laboratory experiments.
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High Energy Astrophysical Phenomena · Cross-listed from hep-ph

Line-of-sight magnetic-field propagation effects on axion-like particle constraints from GRB 221009A

Chengcheng Han, Zhanhong Lei, Jiajie Yang et al. (+1 more)

High-energy photons from GRB 221009A provide a powerful opportunity to probe axion-like particles (ALPs) through photon-ALP oscillations in cosmic magnetic fields. We revisit the ALP constraints implied by the LHAASO observation of this burst, with particular emphasis on the magnetic-field environments encountered along the line of sight. We include the host-galaxy, intergalactic, and Milky-Way magnetic fields and assess their respective impacts on the photon survival probability and on the exclusion limits in the ALP mass-coupling plane. We show that the constraints are only mildly affected by the choice of host-galaxy and Galactic magnetic-field models, but can change significantly once the intergalactic magnetic field is varied. Its field strength, coherence scale, and stochastic properties can all leave visible imprints on the derived exclusion contours, and in some cases generate pronounced oscillatory features. This demonstrates that the intergalactic magnetic field constitutes the dominant astrophysical uncertainty in extracting ALP limits from GRB 221009A. Our analysis highlights the importance of realistic propagation modeling in future gamma-ray searches for ALPs.
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All authors Chengcheng Han, Zhanhong Lei, Jiajie Yang, Shutong Zhao

Solar and Stellar Astrophysics

Polarity Reversal of the Polar Magnetic Fields in Solar Cycle 25

Yin Li, Shuhong Yang, Yuzong Zhang et al. (+4 more)

The polar magnetic field polarity reversal is a key signature of solar cycle evolution, and precise determination of its timing is crucial for dynamo theory validation and solar cycle prediction. We investigate the polar polarity reversal of solar cycle 25 using the vector magnetic field data from the spectropolarimeter on board the Hinode satellite. We constructed polar top-down composite maps from Hinode-view magnetograms. These maps show the year-to-year polar polarity variations, with the northern polar region gradually changing from positive to negative and the southern polar region exhibiting the reverse behavior. The polarity reversals of the northern and southern polar caps (above 70 deg latitude) likely occurred in November 2024 and October 2024, respectively. The northern polarity reversal lagged the northern hemispheric sunspot number maximum by approximately 19 months, while the southern reversal possibly coincided with the southern maximum. Moreover, polarity reversal times calculated at 5 deg latitude intervals above 70 deg reveal a trend of earlier reversal in lower latitudes consistent with that of solar cycle 24. These results offer observational references for modeling polar polarity reversal in solar cycles.
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All authors Yin Li, Shuhong Yang, Yuzong Zhang, Qiao Song, Guiping Zhou, Yuanyong Deng, Jingxiu Wang

Astrophysics of Galaxies

TODDLERS 2.0: Stellar feedback and observables across diverse IMFs, binary populations, and cloud environments

Anand Utsav Kapoor, Andrea Gebek, Maarten Baes et al. (+4 more)

Modeling the feedback-driven evolution of star-forming regions and their multi-wavelength emission is essential for interpreting galaxy observations across cosmic time. TODDLERS couples 1D shell dynamics with Cloudy photoionization to predict UV-to-mm observables. The original framework assumed instantaneous star formation, uniform cloud density, a fixed IMF with single-star evolution, and fixed dust properties. We present TODDLERS 2.0, extending the framework to broader stellar populations, birth-cloud conditions, and dust physics. Stellar feedback and input spectra are modeled using pySTARBURST99 (arbitrary IMFs, upper mass limits up to 500 M$\odot$) and BPASS (binary evolution, upper mass limits up to 300 M$\odot$), including stochastic IMF sampling for low-mass clusters (M$* \lesssim 10^4$ M$\odot$) and constant star formation. The 1D evolution includes non-uniform cloud density profiles and dynamic cloud density evolution driven by escaping ionizing radiation. Cloudy post-processing includes modified grain size distributions and diffuse ionized gas. Cloud density profile and star formation mode regulate fragmentation timescales and shell extent: centrally concentrated profiles fragment earlier, while constant star formation delays fragmentation relative to bursts. Top-heavy IMFs generate stronger feedback and earlier fragmentation than a Kroupa IMF. Dynamic cloud density evolution introduces an additional feedback channel, strongest at low metallicity where unswept cloud density decreases by up to three orders of magnitude. For low-mass clusters, stochastic sampling produces order-of-magnitude feedback variations, demonstrating breakdown of the fully sampled IMF approximation. TODDLERS 2.0 models diverse stellar populations, cloud structures, and star formation modes as a standalone tool or sub-grid emission model for galaxy simulations.
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All authors Anand Utsav Kapoor, Andrea Gebek, Maarten Baes, Sven De Rijcke, Arjen van der Wel, Sébastien Vicens-Mouret, Carmelle Robert

High Energy Astrophysical Phenomena · Cross-listed from gr-qc

Eccentricity in Disguise? Insights from GW231123 and Numerically Simulated Binary Black Hole Merger Signals

Koustav Chandra, Johann Fernandes, Akshita Mittal et al. (+1 more)

GW231123 is a gravitational-wave signal originating from the merger of a black hole binary with total mass $\sim 250 M_{\odot}$, the largest ever detected by the LIGO-Virgo-Kagra Collaboration. Remarkably, under standard priors, the system features among the fastest-spinning binary components confidently measured in binary mergers, $ \chi_{1,2} \gtrsim 0.7$ at $90\%$ one-dimensional credibility, according to the most accurate model employed. As typical binary mergers result in remnants with $\chi \sim 0.7$, such spin values are challenging to obtain even from previous (hierarchical) mergers. These inferred properties rely on waveform models lacking eccentric corrections in the merger-ringdown stage. Here, we show that binaries retaining significant eccentricity up to merger can be misinterpreted as near-extremally spinning when non-circular corrections are neglected. Binary-agnostic ringdown analysis instead provides unbiased estimates of the remnant properties, provided that a robust estimate of the signal peak can be obtained. We re-analyse GW231123 using available eccentric numerical-relativity catalogues, finding that although eccentric templates can provide a good fit to the data, quasi-spherical templates are still favoured. Ringdown analyses confirm a secondary likelihood peak correlated with large eccentricity values, but improved eccentric models will be required to assess the reliability of this interpretation. Finally, analysing GW231123 under population-informed parametric priors confirms the exceptional nature of this event within the current black hole binary population.
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All authors Koustav Chandra, Johann Fernandes, Akshita Mittal, Gregorio Carullo

High Energy Astrophysical Phenomena

Relativistic Accretion Flow in a Generic Class of Spherically Symmetric Static Spacetime

Pradeepkumar Yadav, Sayan Chakrabarti and Santabrata Das

We investigate the properties of low angular momentum, inviscid, advective accretion flows in a generic static and spherically symmetric spacetime that incorporates higher-order corrections up to the fourth order in $1/r$. Employing this metric, we self-consistently solve the relativistic hydrodynamical equations and obtain the family of global transonic accretion solutions ($O$, $A$, $W$ and $I$-types) by means of the spacetime parameters ($\delta$, $\eta$, $\beta$) and the flow parameters (specific energy $\mathscr{E}$ and angular momentum $\lambda$). Our analysis reveals that the accretion flow possesses either single or multiple critical points depending on these input parameters. We delineate the regions of the $\delta-\lambda$ and $\lambda-\mathscr{E}$ parameter spaces that admits solutions with multiple critical points and demonstrate how these regions evolve with increasing spacetime parameter $\delta$. Furthermore, while connecting the spacetime geometry with observable signatures, we compute the spectral energy distribution (SED) from thermal bremsstrahlung emission and observe that increasing $\delta$ enhances the SED relative to the Schwarzschild case. Finally, we find that global transonic solutions harbouring inner critical points ($I$-types) yields more luminous power than those with only outer critical points ($O$ and $A$ types).
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Solar and Stellar Astrophysics

Comparative Analysis of Ellerman and Quiet Sun Ellerman Bombs in the Solar Atmosphere

Ravi Chaurasiya, Ankala Raja Bayanna and Jayant Joshi

Ellerman Bombs (EBs) and Quiet-Sun Ellerman Bombs (QSEBs) are small-scale signatures of magnetic reconnection in the lower solar atmosphere, observed in active regions and quiet-Sun areas, respectively. We investigate and compare some of their properties using coordinated multiwavelength observations from the Swedish 1-m Solar Telescope, the Interface Region Imaging Spectrograph, and the Solar Dynamics Observatory. We employ k-means clustering to identify EBs and QSEBs and perform a detailed analysis of a subset of these events. Our results show that EBs are frequently associated with opposite magnetic polarities, whereas QSEBs generally lack clear polarity signatures, likely due to limited spatial resolution. Spectral inversions using the STiC code reveal temperature enhancements of up to 1700 K in the lower chromosphere for EBs. In contrast, no clear temperature enhancement is detected for QSEBs, which may be attributed to the limited spatial resolution or insufficient wavelength sampling of the Ca II 8542 A. We further find that some EBs exhibit signatures extending to transition-region temperatures. An analysis of EBs temporal evolution reveals episodic heating, with a range of periodicities, most commonly around 6-7 minutes. In addition, we identify spatial associations between the footpoints of some spicules and EBs/QSEBs, suggesting that reconnection in these events may contribute to spicule formation. These results demonstrate similarities and differences between EBs and QSEBs and support the interpretation that small-scale magnetic reconnection contributes to heating and dynamics in EBs, while the underlying mechanism of QSEBs requires further investigation.
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High Energy Astrophysical Phenomena

Short Spike, Long Story: Episode-Dependent Shifts of Long-Duration Type-I GRBs on $E_{\rm p,z}$–$E_{\rm iso}$ Plane

Ya-Hui Jiang, Run-Chao Chen, Zhen-Yu Yan et al. (+3 more)

Observations of peculiar GRBs have challenged the traditional $T_{90}$-based classification, demonstrating that duration does not map uniquely onto progenitor type. A striking class is long-duration Type~I GRBs – merger-origin events whose prompt emission lasts far longer than the canonical 2 s boundary, typically comprising an initial short hard spike followed by softer extended emission. Identifying the physical origin of such bursts requires diagnostics beyond duration alone, among which the Amati relation, linking rest-frame spectral peak energy $E_{\rm p,z}$ and isotropic-equivalent energy $E_{\rm iso}$, is widely used as a complementary classification tool. We analyze a sample of eight long-duration Type~I GRBs and merger candidates by separating the initial spike from the extended emission and examining their episode-dependent locations on the $E_{\rm p,z}$–$E_{\rm iso}$ plane. We find that the initial spike generally lies within, or close to, the empirical Type~I region, consistent with a compact-merger-like prompt-emission component. In contrast, the extended-emission episode systematically occupies a region closer to Type~II GRBs, and could be misidentified as collapsar-like if analyzed in isolation. This episode-dependent Type~I-to-Type~II transition is further supported by time-resolved spectral analysis, although its magnitude and trajectory vary among bursts, suggesting diversity in central-engine evolution or outflow properties between the two phases. Our results caution that the Amati relation alone can lead to misleading empirical classification when the initial hard spike is weak, outside the instrumental bandpass, or missed entirely, leaving only the extended emission to be analyzed. Broad temporal and spectral coverage, and independent multi-wavelength diagnostics, is therefore essential for identifying the physical origin of these events.
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All authors Ya-Hui Jiang, Run-Chao Chen, Zhen-Yu Yan, Kamil Nadaf, Xiao-Hong Zhao, Bin-Bin Zhang

Friday 12 June

Astrophysics of Galaxies

Seeing through the dust: Unraveling near-infrared variability in type 2 active galactic nuclei

J. Cerón-Meneses, P. Arévalo, P. Sánchez-Sáez et al. (+3 more)

Near-infrared (NIR) variability studies of active galactic nuclei (AGNs) are still limited, as long-term multiepoch monitoring in the NIR is observationally challenging. The depth, wavelength coverage, and 14-year temporal baseline of UltraVISTA make it one of the few surveys capable of providing a detailed characterization of AGN variability in this regime. We aim to quantify the NIR variability of known AGNs in the COSMOS field and to investigate the physical origin of variability in type 2 AGNs. In particular, we examine how NIR variability can help clarify the discrepancies between optical and X-ray classifications. Using the 14-year multiepoch UltraVISTA DR6 dataset in the YJHKs bands, we constructed calibrated NIR light curves and quantified their variability through a set of metrics. AGN-like stochastic variability was identified by modeling the light curves with a damped random walk (DRW) process. We find that about 7-17% of the 533 type 2 AGNs are variable in the NIR, with variability fractions increasing toward Ks, where the dusty torus dominates the emission. Based on the wavelength dependence of the DRW variability amplitude, we classify variable type 2 AGNs into disk-dominated, torus-dominated, and highly obscured groups. About one third of the X-ray unobscured (XR I) type 2 AGNs are variable in the NIR, consistent with misclassified weak type 1 or true type 2 AGNs. On the other hand, 21.4% (30/140) of the X-ray obscured (XR II) type 2 AGNs show detectable variability in the NIR, most of them only in H or Ks, consistent with obscuration of the bluer (accretion disk) bands. Type 2 AGNs without X-ray counterparts (165) show the smallest fraction (3.6%) of variable objects. NIR variability provides an effective and independent diagnostic for confirming optical classifications and for identifying weak or misclassified type 1 AGNs in deep extragalactic surveys.
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All authors J. Cerón-Meneses, P. Arévalo, P. Sánchez-Sáez, W. Yu, P. Lira, B. Milvang-Jensen

Cosmology and Nongalactic Astrophysics · Cross-listed from hep-ph

Domain walls and magnetic monopoles in Grand Unified Models

Harish Hemming, Tanmay Vachaspati and Anja Wachowitz

Motivated by Grand Unification, we study the formation of magnetic monopoles in an SU(3) non-Abelian gauge theory. We find that the number density of magnetic monopoles depends critically on a parameter, $\epsilon$, that controls the abundance and subsequent decay of biased domain walls. For sufficiently small but non-vanishing values of $\epsilon$, very few monopoles and walls survive in our simulations, potentially solving the cosmological monopole over-abundance problem. In addition, the scenario predicts a stochastic gravitational background from biased domain walls and the possibility of magnetically charged black holes.
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Earth and Planetary Astrophysics

Thermally Regulated Viscoelastic Tidal Migration of Eccentric Planets

Cristobal Petrovich and Hareesh Gautham Bhaskar

A growing population of short-period Neptune-like planets has nonzero eccentricities and, in some cases, large stellar obliquities, suggestive of high-eccentricity migration. Modeling this evolution requires a prescription for tidal dissipation, which in Neptune-like planets may be dominated by rocky or icy cores rather than by extended gaseous envelopes as often assumed for gas giants. We study the coupled orbital and thermal evolution of eccentric Neptune-like planets whose tidal dissipation is controlled by a viscoelastic Maxwell core. We compute the full harmonic tidal response, follow the equilibrium spin state, and evolve the core temperature; the changing thermal state feeds back on the orbit by modifying the viscosity and hence the frequency-dependent tidal response. We find that the coupled evolution is self-regulated: tidal heating initially drives cold, weakly dissipative cores toward efficient dissipation, but the resulting temperature increase lowers the viscosity, shifts the tidal response toward the fluid-like side of the Maxwell peak, and slows the subsequent migration. This feedback drives the system toward a quasi-steady heating-cooling balance, produces long-lived eccentric phases, and weakens the otherwise steep dependence of circularization time on final orbital distance. Thermally regulated tides therefore offer a natural explanation for how observed hot Neptunes can remain eccentric across a broad range of orbital distances, where a single fixed tidal efficiency would either erase eccentricity too efficiently close in or fail to damp it farther out.
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Astrophysics of Galaxies

The Milky Way as a distant galaxy: an IFU and panchromatic view

Sergey Khoperskov, Alina Boecker, Nikolay Kacharov et al. (+4 more)

Understanding the structure and evolution of galaxies increasingly benefits from placing the Milky Way (MW), the best-studied stellar system, in an external-galaxy context. To analyse the MW as an extragalactic system, we construct an integrated-light view of it using two complementary approaches: composite stellar populations built from a selection-function-free orbit-superposition solution constrained by APOGEE DR17, and full SKIRT radiative-transfer modelling of a hydrodynamical MW simulation initialised from the same solution. In both cases, the MW data are assembled into mock IFU datacubes and analysed with with full spectral fitting (pPXF). We find, however, that the underlying LOSVD is more complex than can be captured by a Gauss-Hermite parametrisation, as is likely the case in MW-like late-type barred galaxies. For the composite-population mocks, we recover the main large-scale kinematic structures, including the rotation and velocity-dispersion patterns associated with the thin and thick discs and the bar/bulge, together with the mean stellar-population maps. The known disc chemical bimodality in [\alpha/M]-[M/H] cannot be recovered directly from the IFU, regardless of the \alpha-resolution of the SSP templates, but its MW-like spatially varying double-sequence behaviour is recovered across the disc. The broad global star-formation history is reproduced, although artificial bursts, likely driven by the age-metallicity degeneracy, remain even after regularisation. For the radiative-transfer mocks, the main kinematic maps are recovered with moderate accuracy, whereas higher-order moments and stellar-population properties remain difficult to constrain, primarily because of the lower spectral resolution and lower statistical SNR of the datacubes. These results indicate that forward panchromatic modelling remains challenging for high-resolution IFU-like observations.
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All authors Sergey Khoperskov, Alina Boecker, Nikolay Kacharov, Davor Krajnović, Matthias Steinmetz, Glenn van de Ven, Jakob C. Walcher

Cosmology and Nongalactic Astrophysics

Cosmological Tensions in a Gauge-Invariant Modified Gravity

Zahra Tabatabaei, Sohrab Rahvar and Shahin Rouhani

In this work, we investigate a gauge-invariant formulation of modified gravity (GIMOG) wherein the gravitational interaction emerges dynamically from a scalar field following a first-order phase transition. This framework offers a unified cosmological history: it naturally generates a pre-inflationary phase, smoothly recovers the standard radiation and matter-dominated eras, and accounts for late-time cosmic acceleration without the need for a cosmological constant or dark energy. We evaluate the phenomenological viability of the model by confronting it with observational data across distinct cosmological epochs. At late times, the model is constrained using Pantheon+ Type Ia supernova data. In the early Universe, we impose bounds from Big Bang Nucleosynthesis (BBN), specifically utilizing the primordial $^{4}\mathrm{He}$ abundance. Our analysis reveals a distinct phenomenological tension: while late-time observations favor a stronger effective gravitational coupling, BBN constraints tightly restrict early-universe deviations from general relativity. We demonstrate that reconciling these constraints requires a smooth time variation of the effective gravitational constant, $G$, establishing a clear theoretical target for future precision cosmological tests.
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Cosmology and Nongalactic Astrophysics

The Peculiar Growth of Structure: Validating $f\sigma_8$ Measurements from TITAN Type Ia Supernovae and the Uchuu Simulations

Mitchell Dixon, David O. Jones, Nicole E. Drakos et al. (+11 more)

The growth rate of cosmic structure, parameterized by $f\sigma_8$, is a fundamental test of $\Lambda$CDM and general relativity. Using Type Ia supernova (SN Ia) peculiar velocities in conjunction with galaxy redshift surveys may be one of the most precise pathways to measuring $f\sigma_8$ in the local Universe, yet existing analyses have not quantified its systematic uncertainties. Here, we present an end-to-end simulated $f\sigma_8$ measurement tailored to the Type Ia Supernova Trove from ATLAS in the Nearby Universe (TITAN) survey, using ~2000 simulated SNe Ia at $z < 0.067$. We use the Uchuu $N$-body simulations to generate mock galaxy catalogs and SN Ia simulations with realistic, correlated peculiar velocities, and use these catalogs to reconstruct density fields that replicate the 2M++ redshift survey. Using a modified forward likelihood framework across eight mock realizations, we recover $\langle f\sigma_8 \rangle = 0.429 \pm 0.038$ ($\sigma_{\rm stat} = 0.030$, $\sigma_{\rm sys} = 0.023$), consistent with the Uchuu simulation input $f\sigma_8 = 0.428$ to within 0.1%. The mock-to-mock scatter of 0.031 is consistent with our uncertainties, highlighting the reliability of our error estimates. Our measurement is dominated by the statistical uncertainty, with approximately equal contributions from SN Ia ($\sigma_{\rm sys}^{\rm SN}=0.017$) and density reconstruction ($\sigma_{\rm sys}^{\rm recon}=0.016$) systematic uncertainties. The assumed intrinsic scatter model is the largest single systematic contribution, and a different model choice can shift $f\sigma_8$ to lower values, largely driven by red SNe with a skewed color distribution. Our analysis provides the first systematic uncertainty budget for the "reconstruction-and-scaling" method of measuring $f\sigma_8$ with SNe Ia, and demonstrates that SNe Ia are a competitive probe of the growth of structure in the local Universe.
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All authors Mitchell Dixon, David O. Jones, Nicole E. Drakos, Bastien Carreres, Jack W. Tweddle, Yukei S. Murakami, Chris Ashall, Dillon Brout, Thomas de Jaeger, Aaron Do, Elijah G. Marlin, David Rubin, Stephen J. Smartt, Ken W. Smith

Astrophysics of Galaxies

Probing Direct Contributions of Galaxies and AGN to Cosmic Reionization in a Quasar Field J0226+0302 with JWST NIRCam and NIRSpec

Xiangyu Jin, Jinyi Yang, Feige Wang et al. (+19 more)

We present JWST Cycle 2 NIRCam and NIRSpec observations in a quasar field J0226+0302 at z=6.5412 to probe the direct connections between the intergalactic medium (IGM), galaxies, and AGN during reionization. This field was previously observed by the JWST ASPIRE program, detecting eight [OIII]-emitting galaxies at 5.3<z<6.4 with a single NIRCam pointing. Using new NIRCam and NIRSpec observations, we identify 65 additional line-emitting galaxies at 5.3<z<6.4. The IGM-galaxy cross-correlation function shows a ~2-sigma excess IGM transmission at ~10-40 cMpc from galaxies, suggesting a significant contribution from regions traced by star-forming galaxies to the local ionizing background. The IGM-galaxy cross-correlation function in this field is consistent with THESAN simulations for an IGM neutral fraction of 5%-7% and an average galaxy ionizing photon escape fraction f_esc of 6%, although a single field is subject to substantial cosmic variance and cannot constrain these quantities independently. Among 49 line-emitting galaxies observed by NIRSpec, we identify four AGN with broad H-alpha emission lines, resulting in an AGN fraction of (8+/-4)%. From the IGM effective optical depth and the IGM-AGN cross-correlation function, we find that the IGM transmission is higher within 5 cMpc/h of four AGN than around the majority of [OIII] emitters. We interpret the excess transmission as resulting from the local radiation enhancement by the AGN, and estimate f_esc~50%-100%, based on our illustrative model for the IGM-AGN cross-correlation function. Future JWST NIRSpec observations in quasar fields will yield a more constraining IGM-AGN cross-correlation function, providing further insights into the roles of galaxies and AGN in reionization.
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All authors Xiangyu Jin, Jinyi Yang, Feige Wang, Koki Kakiichi, Xiaohui Fan, Enrico Garaldi, Jaclyn B. Champagne, George D. Becker, Yongda Zhu, Yunjing Wu, Marianne Vestergaard, Huanqing Chen, Valentina D'Odorico, Anna-Christina Eilers, Jiamu Huang, Hyunsung D. Jun, Mingyu Li, Maria Pudoka, Wei Leong Tee, Minghao Yue, Huanian Zhang, Siwei Zou

Astrophysics of Galaxies

A Comparative Study of Isothermal Turbulence Statistics: Fourier Space Driving vs. Point Source Driving

Tejahni Desire, Chang-Goo Kim and Rajsekhar Mohapatra

The turbulence driving parameter ($b \equiv \sigma_{\rho/\langle \rho \rangle}/\mathcal{M}$; the ratio of the density to velocity fluctuations) is widely used to infer the dominant mode of energy injection in interstellar turbulence. Numerical simulations of turbulence using Fourier Space Driving (FSD) establish a mapping from $b\approx 1/3$ for purely solenoidal to $b\approx 1$ for purely compressive driving. We test the robustness of this calibration by comparing FSD against Point Source Driving (PSD), which stochastically injects radial momentum at random locations mimicking supernovae. Using isothermal hydrodynamic simulations in a periodic box with AthenaK, we run a suite of carefully curated simulations to match Mach numbers between the two driving methods and compare morphology, probability density functions, and power spectra of density and velocity. Despite injecting purely compressive motions, the PSD models yield $b=0.33$ to $0.49$, values that the FSD calibration would associate with more solenoidal driving. With mass-weighted mean Mach number, excluding high-velocity bubble interiors, $b_M=0.74$ to $0.79$ still does not recover the expected $b\approx 1$ for volume-filling, purely compressive driving. More broadly, the PSD models show density and velocity statistics closer to solenoidal and compressive FSD models, respectively, and exhibit unique features, including non-Gaussian velocity tails and a positive density-Mach number correlation at high densities. Within the FSD framework itself, varying the forcing correlation time changes $b$ by a factor of more than 3 for compressive driving. These results demonstrate that $b$ is degenerate with both the spatial locality and the temporal correlation of the driving, limiting its utility as a standalone diagnostic of the energy injection mode.
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Instrumentation and Methods for Astrophysics

Direct High-Resolution Imaging of Earth-like Exoplanets with the Solar Gravitational Lens

Slava G. Turyshev

We present a scalar, aperture-averaged observability benchmark for resolved exoplanet imaging with the solar gravitational lens (SGL). A real Earth luminance map is propagated through a scanned SGL image plane using source-to-image-plane compression, a finite-aperture SGL kernel, and an Einstein-ring photon-count model. We inject photon noise, finite-exposure smear, cloud-like temporal variability, coronal and detector-calibration residuals, optical-operator mismatch, and navigation error, then reconstruct with a regularized Fourier/Wiener inverse. For an Earth-radius planet at 30 pc observed from 650 AU with a 1 m telescope, the projected image cylinder is 1.338 km across; a $128\times128$ raster has 10.46 m image-plane pitch, 99.55 km source pixels, and convolved-image SNR 43.16 for 1800 s per sample. With the stated ring-extraction, temporal, background, calibration, and navigation mitigations, the fiducial reconstruction reaches SNR 6.89, structural similarity 0.848, normalized RMS error 0.439, and a 232 km Fourier-ring-correlation resolution proxy. A higher-count case reaches SNR 10.49, structural similarity 0.927, normalized RMS error 0.287, and the 199 km two-pixel grid floor. Controlled cloud tests show that a static inverse fails for rotating cloudy data, whereas phase-registered robust coadds recover persistent surface-proxy structure in the scalar model. The dominant requirements are temporal sampling, coronal and detector calibration, ring extraction, image-plane metrology, optical-operator knowledge, and dynamic inversion, not calibrated monopole SGL blur. The benchmark demonstrates recoverable 200-230 km-class broadband spatial contrast in the stated scalar model, but does not validate propulsion, communications, coronagraphic or external-occulter propagation, physical solar multipoles, physical cloud fields, or a full dynamic retrieval pipeline.
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Astrophysics of Galaxies

Galaxy Spiral Arm Count vs. Concentration and Mass: A First Look with Euclid

Beverly J. Smith, Sydnie Bergner, Mark L. Giroux et al. (+1 more)

Using catalogued information from Euclid Quick Data Release 1, we compare 2-armed and 3-armed spiral galaxies as classified by the Euclid Zoobot software. Two-armed galaxies have larger concentrations, lower stellar masses (M*), and lower star formation rates (SFRs) on average than 3-armed galaxies. For a given M*, 2-armed galaxies have larger concentrations than 3-armed galaxies. These trends have been seen before in nearby galaxies; with Euclid we extend the patterns to redshifts z = 0.4 - 1. Two-armed galaxies have lower SFRs because they have lower masses; at fixed M*, 2-armed and 3-armed galaxies have similar SFRs. We see a bend in the concentration-log M* relation for 2-armed galaxies at M* = 10^10.3 M(sun). Above this mass, 2-armed galaxies show significantly larger concentrations than their lower mass counterparts. The observed concentrations of 2-armed galaxies decrease with increasing redshift, perhaps from morphological K-corrections and resolution differences. About 60% - 70% of Euclid spirals are 2-armed, and about 15% - 20% are 3-armed. One-armed galaxies are rare, with low masses compared to 2-armed spirals. We compare these statistics with Galaxy Zoo Sloan Digital Sky Survey arm counts at low z, and tentatively with JWST at higher z. We discuss these results in terms of theoretical models of spiral arm generation and evolution, and compare with statistics of grand design, multi-armed, and flocculent galaxies. There is a need for more quantitative measurements of arm structure beyond arm counts provided by the Zoobot/Galaxy Zoo or the three standard arm classes.
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All authors Beverly J. Smith, Sydnie Bergner, Mark L. Giroux, Curtis Struck

High Energy Astrophysical Phenomena · Cross-listed from gr-qc

Tidal Stripping of Matter Bound to the Secondary in Extreme Mass-Ratio Inspirals

Sreejith Nair and Sayak Datta

Environmental studies of extreme mass-ratio inspirals (EMRIs) have focused almost entirely on matter surrounding the primary supermassive black hole. We instead consider matter bound to the stellar-mass secondary (e.g., gas or dark matter); which can be progressively tidally stripped during the LISA-band inspiral. This changes the bound mass of the inspiraling object, modifying the gravitational-wave (GW) phase at leading order in the secondary mass. Furthermore, as the signal interpolates from an initially dressed inspiral to a nearly bare one, it can produce a characteristic inflection in the residual phase with constant mass waveform templates. Even for an environmental mass $\sim 10^{-3}\,M_{\odot}$, the cumulative dephasing relative to in band initial bound mass waveform can be larger than unity. In subsolar mass cases, the relative dephasing can reach $O(10^3)\, \rm rad$. Neglecting this effect may bias inferred EMRI parameters at the level of the fractional change in the in-band bound mass. The tidal stripping phenomena carry information about the mass and the compactness of the bound matter, enabling probes of sub-AU, planetary- to subsolar-mass environments surrounding stellar-mass black holes.
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Astrophysics of Galaxies

COSMOS-Web: A Multi-wavelength Morphological Catalog of ~780,000 Galaxies

Lilan Yang, Jeyhan S. Kartaltepe, Nicole E. Drakos et al. (+20 more)

We present multi-wavelength morphological measurements for all galaxies in the COSMOS-Web survey, i.e., $\sim$780,000 galaxies contained in the COSMOS2025 catalog. We perform both parametric (e.g., single and double Sérsic modeling) and non-parametric (e.g., Gini-$M_{20}$) morphology analyses in four NIRCam bands, independently. Our parametric fits reveal a strong correlation between galaxy structure and star formation activity up to $z\sim4$, as evidenced by the dependence of the Sérsic index ($n_{\rm s\'ersic}$) and bulge-to-total ratio ($B/T$) on the position of the star formation rate-stellar mass plane. A tight correlation between $n_{\rm s\'ersic}$ and $B/T$ is observed. The evolution of $n_{\rm s\'ersic}$ and $B/T$ depends on stellar mass; for example, the median $n_{\rm s\'ersic}$ increases from $\sim1$ at $z\sim6$ to $\sim2.5$ at $z\sim2$ for massive galaxies with $M_*>10^{10.5} M_{\odot}$, while lower mass galaxies remain $n_{\rm s\'ersic}\sim1.2$ at all epochs. The UV $n_{\rm s\'ersic}$ values are systematically smaller than those in the optical, although both exhibit similar evolutionary trends. From non-parametric analyses, we demonstrate the distribution of galaxies on the Gini-$M_{20}$ and asymmetry-concentration planes, and find that morphological classifications based on non-parametric indicators are consistent with those derived from the Sérsic index. The resulting catalog provides the largest and most detailed set of JWST multi-wavelength morphological measurements to date, serving as a valuable community resource for studies of structural transformation, bulge growth, and galaxy-supermassive black hole coevolution across cosmic time.
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All authors Lilan Yang, Jeyhan S. Kartaltepe, Nicole E. Drakos, Andreas L. Faisst, Carter Flayhart, Maximilien Franco, Anton M. Koekemoer, Olivier Ilbert, Hollis B. Akins, Caitlin M. Casey, Xuheng Ding, Ali Hadi, Santosh Harish, Ronaldo Laishram, Daizhong Liu, Georgios E. Magdis, Felix Martinez III, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Greta Toni

Astrophysics of Galaxies

Physical characterization of the local system NGC 1313: A flattening in its chemical abundance by past interactions

Belén Ojeda-Díaz, Sergio Torres-Flores, Daniela E. Olave-Rojas et al. (+5 more)

Interacting galaxies provide unique information on morphological transformation, enhanced star formation, and chemical evolution, and thus contribute to understanding the complex evolution of galaxies. We investigated the local interacting system NGC 1313 by analyzing its main physical and kinematical properties to understand how the interaction has influenced the evolutionary state of the galaxy. We used multi-slit GMOS-S spectroscopy to study 19 regions across the galaxy, encompassing its main body and the complex southwest region. We derived oxygen abundances using the N2 method and computed their chemical gradient. We derived electron densities using the S[II] ratio, ages from the EW(H-alpha), and stellar masses of the regions from DR10 Legacy Survey images. We used H-alpha Fabry-Perot data to analyze the kinematics of the systems and search for signs of past interactions. The Baldwin-Phillips-Terlevich (BPT) and EW(H-alpha) versus N[II]/H-alpha (WHAN) diagnostics confirm photoionization by star formation. The galaxy has a low oxygen abundance (8.0<12+log(O/H)<8.2), with a mainly flat oxygen abundance gradient, suggesting gas mixing processes. Electron densities span $n_e$<10 to 142 cm$^{-3}$. The blue and red Wolf-Rayet bumps detected in two regions corroborate a young population. We find ages ranging from 2.7 Myr to 6.0 Myr. The velocity field shows complex kinematics in the northern region of NGC 1313, characterized by asymmetric line profiles. NGC 1313 thus provides an ideal laboratory for studying how minor interactions affect star formation, chemical enrichment, and the kinematics of low-mass barred spiral galaxies.
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All authors Belén Ojeda-Díaz, Sergio Torres-Flores, Daniela E. Olave-Rojas, Ciria Lima-Dias, Paulo J. A. Lago, Claudia Mendes de Oliveira, Philippe Amram, Bruno C. Quint