Cosmology and Nongalactic Astrophysics · Cross-listed from hep-ph
Leptophilic scalar dark matter in U(1)$_{L_\mu-L_\tau}$: Evading direct detection and prospective neutron star heating
Chengfeng Cai and Hong-Hao Zhang
Leptophilic dark matter (DM) is a well-motivated thermal weakly interacting massive particle framework that can evade stringent
nuclear-
recoil searches while remaining testable via DM-induced heating of
neutron stars (NSs). In this work, we study leptophilic scalar DM in a $U(1)_{L_\mu-L_\tau}$ gauge extension of the Standard Model, which provides a common leptophilic portal for all scenarios considered. To reproduce the observed relic abundance while suppressing direct-detection signals, we investigate three
benchmark realizations: (i) a secluded DM scenario in which the relic density is set by annihilation into $U(1)_{L_\mu-L_\tau}$ gauge
bosons and two pseudo-Nambu-Goldstone
boson (pNGB) DM models based on (ii) an $SO(4)$
symmetry and (iii) an $SO(3)$
symmetry. In the $SO(4)$ pNGB model, the DM mass arises at tree level from a soft breaking term, while the elastic scattering amplitude is suppressed by a
symmetry-protected cancellation. In the $SO(3)$ pNGB model, the DM mass is generated radiatively at one loop via the $U(1)_{L_\mu-L_\tau}$ gauge interaction, and we show that this gauging preserves the same cancellation mechanism, maintaining compatibility with direct-detection null results. We perform a systematic parameter scan imposing relic density, direct and indirect detection, and
neutrino trident constraints and identify viable sub-TeV to TeV DM candidates. Under the optimistic maximal-heating assumption that the capture rate reaches the
geometric limit and that the captured DM population efficiently thermalizes and attains capture-annihilation
equilibrium inside NSs, we find that the remaining parameter space can be tested by near-infrared observations of old NSs, providing sensitivity complementary to terrestrial searches in regions that are currently weakly constrained.
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Solar and Stellar Astrophysics
Energy and mass transport associated with impulsive spicular flows in solar coronal holes
Lei Ni, Jun Lin, Tanmoy Samanta et al. (+3 more)
How the
solar atmosphere is heated from a temperature of about $5,000-6,000$\,K in the lower atmosphere to about $1-2$\,MK in the corona has challenged the astrophysical community for about 80 years. The same puzzle exists for the
stellar coronae heating as well. In this study, we present a series of findings on
solar spicules and their subsequent impact on the corona within a coronal hole environment, characterized by locally open
magnetic field lines, combining insights from MHD simulations with observations. We find that the convective and turbulent motions around the
solar surface cause plenty of shocks and small-scale
magnetic reconnection in the lower atmosphere. The combined effects of shock compression and reconnection
outflows then drive the formation of groups of spicules with a quasi-period of about $300$\,s and width of $\sim 200-500$\,km. The spicule upflows provide an averaged mass flux above $10^{-9}$\,kg\,m$^{-2}$\,s$^{-1}$ in the lower corona to sustain the
solar wind in coronal holes, and they continuously trigger further new local slow-mode waves and shocks. These waves supply an energy flux of $10-100$\,W\,m$^{-2}$ in the lower corona, and they are dissipated by heat conduction and compression heating to sustain the corona temperature of about $1$\,MK. The results also indicate that the upward propagating disturbances (PDs) observed in extreme ultraviolet (EUV) passbands are caused by both spicule upflows and slow-mode waves and shocks. Our findings help to understand the long standing problem of coronal heating and the origin of
solar winds in coronal hole regions.
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All authors Lei Ni, Jun Lin, Tanmoy Samanta, Guanchong Cheng, Yifu Wang, Robert Erdelyi
Earth and Planetary Astrophysics
Probing Dust in the MWC 480 Disk from Millimeter to Centimeter Wavelengths
Yangfan Shi, Feng Long, Enrique Macías et al. (+12 more)
We present deep, high-resolution ($\sim$100 mas) Karl G. Jansky Very Large Array (VLA) Ka-band (9.1 mm) observations of the disk around MWC 480, and infer
dust properties through a combined analysis with archival Atacama Large Millimeter/submillimeter Array (ALMA) data at 0.87, 1.17, 1.33, and 3.0 mm. The prominent
dust ring at 95 au (B95) is detected at 9.1 mm for the first time, while the faint outer ring at 160 au is not revealed. Through non-parametric visibility modeling, we identified two new annular features: a plateau within 20-50 au across all wavelengths, and a shoulder exterior to the B95 ring at 0.87, 1.17 and 1.33 mm, consistent with signatures of
planet-disk interaction. We find that the width of the B95 ring remains constant across wavelengths, suggesting that fragmentation dominates over radial
diffusion or that unresolved substructure is present within the ring. Resolved spectral modeling yields two families of
dust solutions that reproduce the observations equally well: compact grains or highly porous (90%) grains, with carbonaceous components dominated by refractory organics or amorphous carbon, respectively. The inferred maximum grain sizes peak at the locations of the two rings and reach centimeter within the B95 ring. The total
dust masses are $860^{+95}_{-78}\rm~M_\oplus$/$1500^{+440}_{-330}\rm~M_\oplus$ (large/small-grain solution in inner disk) and $230^{+14}_{-13}\rm~M_\oplus$ for the two
dust mixtures. The B95 ring alone contains $100^{+5}_{-5}\rm~M_\oplus$ and $43^{+2}_{-2}\rm~M_\oplus$, respectively, sufficient to assemble the cores of
giant planets. Finally, we highlight the power of broadband, multi-wavelength observations in placing better constraints on
dust composition and porosity in protoplanetary disks.
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All authors Yangfan Shi, Feng Long, Enrique Macías, Gregory J. Herczeg, Paola Pinilla, Sean M. Andrews, David J. Wilner, Haochang Jiang, Ruobing Dong, Richard Teague, Ilaria Pascucci, Claudia Toci, Yuri Aikawa, Daniel Harsono, Yao Liu
High Energy Astrophysical Phenomena
Optical observations of the fast nova V1674 Herculis
Neeraj Singh Rawat, L. S. Sonith, U. S. Kamath et al. (+3 more)
We present the
evolution of optical spectra and lightcurves of the fast nova V1674 Herculis during 150 days past its eruption. Using the post-eruption AAVSO light curve, we have calculated the orbital period of V1674 Her to be 0.153 days. There is no unambiguous white
dwarf spin period in our data. The optical spectra show that the ionisation increases with time. A morpho-kinematic analysis of the H$\alpha$ line profile indicates a bipolar morphology with polar blobs and an equatorial ring. Lyman beta fluorescence is found to be the dominant mechanism for the excitation of neutral oxygen. On day 19.87, [Ne III] & [Ne V] lines are present, indicating the presence of the ONe white
dwarf. On day 147.66, the nebular lines are still present, implying that the nova had not gone into quiescence yet; this spectrum is
accretion-dominated.
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All authors Neeraj Singh Rawat, L. S. Sonith, U. S. Kamath, Yash Bhargava, G. C. Anupama, Kulinder Pal Singh
High Energy Astrophysical Phenomena
Investigating polarization signatures from GRB models
Pieter vd Merwe and Markus Böttcher
There is still much debate around the inner workings of the GRB
prompt emission phase with many questions still left unanswered. Polarization signatures offer a promising new avenue to discriminate between the various GRB
prompt emission models. The aim of this study is to estimate energy and time resolved polarization signatures resulting from Inverse Compton (IC) scattering for two specific GRB
prompt emission models, namely the backscatter-dominated cork model by \citet{Vyas2} and a Compton drag model by \citet{Lazzati2}. In order to achieve this we apply an IC polarization Monte Carlo (MC)
algorithm to those two GRB models in order to estimate the expected polarization signatures. For the backscatter-dominated cork model we find polarization signatures below $\sim 10$~%, likely below the detection limits of current or near-future X-ray and $\gamma$-ray polarimeters. Our results for the Compton drag model indicates polarization results consistent with that found by \citet{Lazzati3}. Furthermore, we find some energy and time dependence of the estimated polarization, particularly for the polarization angle.
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High Energy Astrophysical Phenomena
Winds of Change: XRISM Resolve X-ray spectroscopy of NGC 4051
James Reeves, Shoji Ogawa, Tracey Jane Turner et al. (+7 more)
NGC 4051 is a nearby (16.7 Mpc), Narrow Line Seyfert 1
galaxy (NLS1), which has a low black hole mass of $10^6$ M$_{\odot}$. It is also known for its rapid X-ray variability, on timescales of kilo-seconds and has a complex, multi component wind in both the soft X-ray and Fe K bands. Here we present the first high resolution XRISM Resolve spectrum of NGC 4051, which was captured in a historically bright state for a 150 ks exposure. XRISM resolves two blue-shifted Fe K shell absorption troughs in the mean spectrum, which can be ascribed to H-like iron and arises from two
outflow components with
outflow velocities of 0.025c and 0.04c. A time dependent spectral analysis shows that the iron K absorption is variable on timescales of less than a day, increasing in velocity over the duration of the observation. The velocity changes may be explained either by the passage of two separate transiting absorbers, of different velocities, or by a single accelerating
outflow of approximately constant column density. In the latter case, the wind acceleration is likely to be too large to be caused by radiation pressure and instead
magnetic driving is favored to accelerate the wind up to 0.04c. The
outflow can originate from an
accretion disk wind, whose kinetic power is sub-Eddington in contrast to recent examples of winds from powerful, luminous
quasars observed by XRISM.
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All authors James Reeves, Shoji Ogawa, Tracey Jane Turner, Valentina Braito, Satoshi Yamada, Steven Kraemer, Hirofumi Noda, Anna Trindade Falcão, Martin Elvis, Giuseppina Fabbiano
Instrumentation and Methods for Astrophysics · Cross-listed from cs.CE
GPU-Native Compressed Neighbor Lists with a Space-Filling-Curve Data Layout
Felix Thaler and Sebastian Keller
We have developed a compressed neighbor list for short-range particle-particle interaction based on a space- filling curve (SFC)
memory layout and particle clusters. The neighbor list can be constructed efficiently on GPUs, supporting NVIDIA and AMD hardware, and has a
memory footprint of only 4 bytes per particle to store approximately 200 neighbors. Compared to the highly-optimized domain-specific neighbor list implementation of GROMACS, a molecular dynamics code, it has a comparable cluster overhead and delivers similar performance in a neighborhood pass. Thanks to the SFC-based data layout and the support for varying interaction radii per particle, our neighbor list performs well for systems with high density contrasts, such as those encountered in many astrophysical and cosmological applications. Due to the close relation between SFCs and octrees, our neighbor list seamlessly integrates with octree-based domain decomposition and multipole-based methods for long-range gravitational or electrostatic interactions. To demonstrate the coupling between long- and short-range forces, we simulate an Evrard collapse, a standard test case for the coupling between hydrodynamical and gravitational forces, on up to 1024 GPUs, and compare our results to the analytical solution.
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High Energy Astrophysical Phenomena
A Bayesian Method for Air-Shower Reconstruction using Information Field Theory
Karen Terveer, Sjoerd Bouma, Stijn Buitink et al. (+12 more)
The
radio detection of extensive air showers provides a powerful method for studying the origin of high-energy
cosmic rays. The Low-Frequency Array (LOFAR) offers unprecedentedly detailed measurements of the
radio emission footprint. However, fully exploiting this information requires advanced reconstruction techniques. In this paper, we introduce a novel framework for air shower reconstruction based on
Bayesian inference and Information Field Theory (IFT). Our method is built on a fully differentiable forward model of the
radio signal, which incorporates a physical emission parameterization and a precise wavefront model. Additionally, we augment this physical model with Gaussian processes to account for systematic uncertainties in both the signal fluence and arrival timing. By leveraging gradient information, our approach enables efficient (three orders of magnitude acceleration w.r.t.\ the legacy method) and robust inference of the underlying physical shower parameters, such as primary energy and the depth of shower maximum, $X_\text{max}$. This work provides not only point estimates but also a rigorous quantification of uncertainties. We achieve a resolution in $X_\text{max}$ of $25\,\mathrm{g/cm^2}$ and a radiation energy resolution of $12\%$ on simulations for LOFAR.
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All authors Karen Terveer, Sjoerd Bouma, Stijn Buitink, Arthur Corstanje, Vital De Henau, Vincent Eberle, Torsten A. Enßlin, Philipp Frank, Tim Huege, Philipp Laub, Katharine Mulrey, Anna Nelles, Simon Strähnz, Satyendra Thoudam, Keito Watanabe
Astrophysics of Galaxies
Probing the Milky Way Halo with RR Lyrae Stars from Gaia Data Release 3
T. Muraveva, L. Monti, D. Massari et al. (+5 more)
The Milky Way (MW)
stellar halo, containing debris from past
accretion events, serves as a fossil record of hierarchical mass assembly. Due to their distinct properties, RR Lyrae
stars (RRLs) serve as excellent tracers for identifying and characterising the
halo's substructures. We analysed a sample of 4933 RRLs, for which we calculated the integrals of motion and orbital parameters. We applied the domain-informed novelty detection CLustering in Multiphase Boundaries (CLiMB) framework to identify RRL membership in the MW substructures. We analysed the
metallicity distributions of RRLs in major accreted system remnants as a snapshot of their chemical evolutionary status during early epochs. We calculated the weighted mean
metallicity ([Fe/H]) and the corresponding standard deviation for
Gaia Sausage/Enceladus ([Fe/H] = $-1.57 \pm 0.25$ dex), Sequoia ([Fe/H] =$ -1.64\pm0.26$ dex), and the Helmi streams ([Fe/H] = $-1.66\pm0.19$ dex). The
metallicity distribution of RRLs in Thamnos was found to be bimodal, with the metal-poor peak likely representing the genuine accreted Thamnos population ([Fe/H] = $-1.94\pm0.20$ dex), in agreement with recent works based on spectroscopic abundances. Our analysis shows that the substructures ED-1 and L-RL3 are highly contaminated by thick disc
stars. However, the metal-poor tails in their
metallicity distributions may be signatures of remnants from small accreted systems. We also identify over-densities of RRLs in correspondence with the recently reported substructures Shiva and Shakti, which we suggest are of in-situ origin. Finally, we applied the RRL-based mass-
metallicity relation of
galaxies to test the nature of the identified dynamical substructures.
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All authors T. Muraveva, L. Monti, D. Massari, M. De Leo, A. Garofalo, G. Clementini, E. Ceccarelli, U. Michelucci
Earth and Planetary Astrophysics
Apophis source population and Earth encounter frequency of Apophis-like bodies
M. Brož, R.P. Binzel, P. Vernazza et al. (+4 more)
We provide context for Apophis' 2029 Earth passage by analyzing its possible source populations, in particular, the Flora family, which has a similar composition, corresponding to LL chondrite meteorites. Out of ${\sim}3380$ NEOs larger or equal than Apophis (${\ge}420\,{\rm m}$), $610\pm 140$ are LL-like NEOs from Flora. Their mean encounter probability is $p = 86\times 10^{-18}\,{\rm km}^{-2}\,{\rm y}^{-1}$, corresponding to once per 13000 y frequency of encounters closer than 38000 km. However, this does not apply to Apophis alone, for which the specific encounter probability is higher, $p' = 1603\times 10^{-18}\,{\rm km}^{-2}\,{\rm y}^{-1}$, but the frequency is lower, only once per 430000 y, when we consider it as a single object. Our simulation of the Flora family over $\sim$1 billion years indicates that Apophis-like bodies have orbits that are particularly persistent in near-Earth space. The temporal distribution of encounter probabilities exhibits peaks (up to ${>}10^4$ in the same units) and the specific value for Apophis is not unusual (occurring ${\sim}70\%$ of time). In other words, there is always at least one Apophis-like body among NEOs. We find that such persistence also creates favorable opportunities for temporary capture as Earth coorbitals. Apophis-like bodies are ultimately removed from the inner
solar system by approaching the Sun or by impact into one of the terrestrial
planets, where the relative split between these outcomes is $(45\pm 2)\,\%$ and $(50\pm 2)\,\%$. While our current knowledge of Apophis' orbit guarantees no threat from Apophis in the next few centuries, we cannot predict any specific outcome for Apophis in the coming thousands or millions of years. Evaluating this statistically over the long term, we find that objects in Apophis-like orbits have a $(19\pm 2)\,\%$ chance of Earth impact over their lifetime of ${\sim}30\,{\rm My}$.
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All authors M. Brož, R.P. Binzel, P. Vernazza, M. Marsset, O. Chrenko, J. Ďurech, D. Herald
Solar and Stellar Astrophysics
Observational Evidence Linking Loop Length and Thermal-Nonthermal Peak Timing in Solar Flares
S. M. Perriyil, S. S. Sadangaya, C. G. Giménez de Castro et al. (+1 more)
We investigate how the
magnetic loop length of
solar flares relates to the timing between their thermal and nonthermal emission signatures. Our study analyzes a sample of 96 C-, M-, and X-class
flares observed between 2013 and 2015 with soft X-rays, hard X-rays, and extreme UV. For each event, we determine the time delay {\Delta}t between the hard X-ray and soft X-ray peak, and estimate the
flare loop length L from UV footpoints assuming a semicircular geometry. In every case, longer
flare loops are consistently associated with larger timing delays. Across the full sample, we find a strong correlation, R = 0.88 between L and {\Delta}t. We also quantify how closely each
flare follows the Neupert effect using a coefficient RN, defined as the Pearson correlation between the time derivative of the soft X-ray flux and the hard X-ray light curve. Applying correlation thresholds of RN > 0.5 and RN > 0.8 yields subsets of 87 and 46 events, respectively. In both cases, the linear relationship between loop length and peak delay remains clearly expressed. For the RN > 0.5 subset, the correlation is R = 0.87, while the more selective subset with RN > 0.8 displays an even stronger correlation of R = 0.91. These results show that the overall trend persists across increasingly stringent correlation thresholds. The results provide direct observational confirmation that
magnetic loop geometry plays a key role in governing the temporal
evolution of energy transport in
solar flares.
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All authors S. M. Perriyil, S. S. Sadangaya, C. G. Giménez de Castro, P. J. A. Simões
Cosmology and Nongalactic Astrophysics
Primordial Black Hole Formation in Rastall Gravity: Shifted Collapse Threshold and Exponential Abundance Sensitivity
Mayukh R. Gangopadhyay
Primordial black holes formed in the early universe are compelling candidates for dark matter. We investigate their production in Rastall
gravity, a modification of general relativity that introduces a non-minimal coupling between matter and geometry through the non-conservation of the energy-momentum tensor. Analyzing cosmological perturbations during radiation domination, we demonstrate that the Rastall parameter fundamentally alters the collapse dynamics, modifying the growth of density fluctuations, the critical threshold for black hole formation, and the fluctuation amplitude at horizon crossing if we consider the nearly conformal
plasma. Current cosmological constraints from Big Bang Nucleosynthesis, the
cosmic microwave background, and large-scale structure restrict the Rastall parameter to small values, yet within this allowed range PBH production can be altered by orders of magnitude compared to general relativity. Our results suggest that PBH formation provides a sensitive and independent probe of perturbation-level modifications in Rastall
gravity, complementary to large-scale structure and CMB tests.
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Instrumentation and Methods for Astrophysics
Direct comparison of SiPMs and PMTs in operation with a bright background and prospects of using SPADs as truly digital sensors
Razmik Mirzoyan, Alexander Hahn, David Fink et al. (+8 more)
The use of silicon photomultipliers (SiPMs) alongside conventional photomultiplier tubes (PMTs) is a remarkable technological development in modern ground-based very high energy gamma-ray astronomy. SiPMs exhibit comparable or even higher
photon detection efficiencies (PDEs) than PMTs. The sensitivity of a PMT matches well the spectral shape of Cherenkov radiation from extended air showers. In contrast to a PMT, the sensitivity of a SiPM is shifted toward longer wavelengths, where the intensity of light of night sky (LoNS), considered as unwanted noise, increases significantly. It is obvious that a SiPM with a higher PDE will indeed measure more Cherenkov light than a PMT, but it will also detect significantly higher LoNS noise; the question is which factor will predominate in the signal-to-noise-ratio (SNR). To compare the performance of a PMT with that of a SiPM, we built SiPM-based modules and installed these and operated in parallel in the imaging camera of the 17 m diameter MAGIC
telescope. Our long-term studies show that SiPM, despite their higher PDE, can deliver only a comparable to PMT performance. As already the name SiPM suggests, we use these
semiconductor sensors analogously to classical PMTs: We amplify their small signals, digitize, and calibrate the converted amplitudes. Although SiPM is essentially a digital sensor, its common-anode design does not allow one to directly profit from it. Numerous arrays of single-
photon avalanche diodes (SPADs) are being developed in various laboratories worldwide. Unlike SiPM, SPAD arrays digitize the incident
photons from the outset and count their number. We will dwell on the potential further developments of SPADs.
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All authors Razmik Mirzoyan, Alexander Hahn, David Fink, Antonios Dettlaff, Daniel Mazin, David Paneque, Olaf Reimann, Thomas Schweizer, Derek Strom, Masahiro Teshima, Yazhou Zhao
Earth and Planetary Astrophysics
Young system development in a cometary globule: An investigation into the eccentric disk around AT Pyx in terms of planet-formation and interaction with its surrounding environment
Dan McLachlan, Christian Ginski, Jake Byrne et al. (+5 more)
This paper presents new data and analyses of the AT Pyx system, a disk-hosting young
star located in a cometary globule in the Gum Nebula. This radiation-driven structure is an unusual environment for observations of
planet formation and differs greatly from the low-mass
star-forming regions disks are most commonly observed in. Aided by a collection of visual and spectroscopic data available for this system, this paper aims to infer the possibility of embedded
planets existing within the disk and how the system's environment may affect its disk morphology. Using data from the VLT's instruments XSHOOTER, ESPRESSO and - most prominently - SPHERE along with data from ALMA, we make a variety of measurements (
geometric, photometric and otherwise) to characterise the observed disk features and attributes such as spiral arms and eccentricity. Mapping of the velocity components is also undertaken using the ALMA gas line data to characterise disk orientation and determine the likelihood that the system is experiencing a late-stage infall event. The disk is found to be eccentric when deprojected. Under the assumption that the formation of a
planet is wholly responsible for the primary and secondary spiral arms, we find the mass of such a
planet can range between 0.004 and 3 Jupiter masses. Measurement of the velocities associated with nearby globule cloud material returns reasonable velocities for a late-stage infall event. We estimate far-ultraviolet field strength at AT Pyx's location to be low in comparison to other surveyed disks. We also find that AT Pyx is possibly a binary system. AT Pyx is the first disk within a cometary globule to be spatially resolved, and is now the first such disk to be investigated to this extent. The work of this paper could potentially be a first step into the further study of disks in the moderate-FUV environment of the Gum Nebula and its globules.
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All authors Dan McLachlan, Christian Ginski, Jake Byrne, Chloe Lawlor, Justyn Campbell-White, Rik Claes, Bin Ren, Anibal Sierra
Astrophysics of Galaxies
The morphological stability of open clusters: a new 2D perspective
Yuting Li, Qingshun Hu, Yufei Cai et al. (+3 more)
Open clusters (OCs) usually evolve gradually as the number of their members changes, which can be manifested in their morphological characteristics. We aim to investigate the morphological stability of 1,490 OCs and further explore the potential change of morphological stability of the OCs at different spatial positions, using the OC catalog from the literature. We define for the first time a new morphological stability parameter Ncore/Nouter, a ratio of member numbers between cluster core and outer areas within
tidal radii, which has a significant positive correlation against N, with a slope of 1.140$\pm$0.039, significantly steeper than the 0.720$\pm$0.026 measured for Score/Souter. This demonstrates that the
stellar density in the core is a more sensitive tracer for morphological stability than geometry. Spatially, the radial sample OCs have larger slopes of Ncore/Nouter and Score/Souter against N, with 1.083$\pm$0.116 and 0.733$\pm$0.080, respectively, whereas those in the tangential direction 1.013$\pm$0.110 and 0.529$\pm$0.075, respectively, which means that the impact on sample OCs from
tidal forces directed toward the
Galactic center is possibly stronger than that from the shear force caused by the differential rotation of the
Galactic disk. Besides, the sample OCs younger than 30 Myr display a shallow slope of 0.751$\pm$0.166, with those older than 800 Myr (1.442$\pm$0.128), reflecting that young OCs likely endure both internal disruptions, such as early dynamical heating weakening core binding and more severe external disturbances, compared to older OCs.
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All authors Yuting Li, Qingshun Hu, Yufei Cai, Yu Dai, Mingfeng Qin, Yangping Luo
Astrophysics of Galaxies
MIGHTEE: Discovery of a triple-double radio galaxy
Tombo F. Rarivoarinoro, Zara Randriamanakoto, Russ Taylor et al. (+8 more)
Triple-double
radio galaxies (TDRGs) are amongst the rarest subpopulations of
radio galaxies (RGs). They are characterised by three pairs of
radio lobes, where each pair of lobes represents an episode of
nuclear activity. Such a feature makes them key objects that can be used to constrain the duty cycle of RGs. In this paper, we report the discovery of J022248\m060934, a new TDRG, hosted by a
galaxy at a spectroscopic
redshift of $z \approx$ 0.94. We have used the MIGHTEE-DR1 data set and MIGHTEE sub-band images as our main data. In total intensity, J022248\m060934 has a bright core and triple-double, edge-brightened-like peaks of
radio emission. The polarimetry of the source reveals an inhomogeneous density of the hosting environment which is consistent with the more pronounced bending in its eastern lobes. The spectral index and
curvature maps suggest an inverted core and an ultra-steepening of the spectrum towards the outer lobes which reinforce a recurrent
nuclear activity. We perform individual spectral age fitting of the components of the source using the JP model and we found a lower limit total age of $\sim$16 Myr. We also derive a short inactive period between the active phases and a rapid duty cycle of 90 per cent for the first cycle of activity. Our spectral ageing analysis suggests that the triple-double structure in TDRGs is not the product of long quiescent periods, as deduced by previous works based on kinematic ages.
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All authors Tombo F. Rarivoarinoro, Zara Randriamanakoto, Russ Taylor, Marisa Brienza, Fabio Luchsinger, Sushant Dutta, Catherine Hale, Jacinta Delhaize, Ndivhuwo Netshiavha, Solohery Randriamampandry, Mattia Vaccari
Astrophysics of Galaxies
Chemodynamical properties of gas-rich galaxies: a comparison of observations and simulations
Anna Velichko, Yves Revaz, Annalisa De Cia et al. (+4 more)
We perform a comprehensive analysis of the chemical and dynamical properties of
quasar-damped Lyman-{\alpha} (DLA)
galaxies and compare these to the GEAR chemodynamical simulations. Specifically, we aim to constrain the behavior of {\alpha}-element enhancements with
metallicity, the dependence of [{\alpha}/Fe] on the specific
star formation rate (sSFR), and the absorption-line velocity widths ({\Delta}v90) vs.
stellar mass, {\Delta}v90 vs.
metallicity, and mass-
metallicity relations. For the comparison, we select five
galaxies simulated with the chemodynamical Tree-SPH code GEAR with
stellar masses in the range of log(M*/Msol) between 6.1 and 10.8, and at six different
redshifts between 0.33 and 4.12. We find that the abundance ratios [{\alpha}/Fe] and [M/H] observed in the interstellar medium (ISM) of DLA
galaxies overlap with the abundance trends in gas of the simulated
galaxies. Our findings corroborate a picture in which DLAs with {\Delta}v90 below and above 100 km/s trace
galaxies with masses in the ranges of log M* 6 - 8 and 8 - 11
solar masses, respectively. We suggest that observations should be used with caution when constraining the theoretical [{\alpha}/Fe] vs. sSFR relations because of systematics (if abundances are obtained from emission lines) or differences in the gas properties as probed by a DLA and its counterpart. So far, only the observations in absorption of inner gas of the LMC and SMC are in agreement with the simulated data. We confirm that DLAs detected at large impact parameters most likely probe the gas of satellite or other
halo galaxies which are adjacent to the central
galaxy. We further find that the velocity widths vs.
stellar masses and mass-
metallicity relations agree well with observations, while GEAR should be calibrated more carefully to reproduce the {\Delta}v90 vs.
metallicity relation.
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All authors Anna Velichko, Yves Revaz, Annalisa De Cia, Cédric Ledoux, Jens-Kristian Krogager, Céline Péroux, Benedetta Casavecchia
Solar and Stellar Astrophysics
Influence of Cross-sectional Expansion on Coronal Emissions from a Radiatively Cooling Solar Flare Loop
Yu Dai, Shihan Li, Wenlong Tang et al. (+2 more)
Loop-aligned hydrodynamic modelings help better understand the thermodynamic
evolution of flaring
plasma confined in
solar flare loops. Conventional loop modelings typically assume a uniform loop cross section. With a variation of the cross section taken into account, in this work we carry out both analytical and numerical modelings of the radiative cooling in a
solar flare loop. It is found that a cross-sectional expansion with height can efficiently suppress the draining of loop material from the corona while not significantly affecting the decrease of loop temperature. Reflected to the loop energetics, the coronal part of the loop cools more dominantly by radiation, and more importantly, the loop radiative outputs are shifted toward lower temperatures. These findings pose important physical implications for extreme-ultraviolet (EUV) late-phase emissions discovered in some
solar flares. The late-phase loops in these
flares are believed to bear a more notable cross-sectional expansion owing to their longer lengths. Compared with the main-phase loops, the late-phase loops would emit more effectively at middle temperatures, which could, to a certain degree, mitigate the severe heating requirement for the production of a prominent warm coronal late-phase peak. In addition, the cross-sectional expansion also affects the shape of the emission lights curves, causing a sharper decay after the emission peak. Such an emission pattern has been validated with the observations of an EUV late-phase
flare, and could serve as a potential diagnostic tool to judge the degree of loop cross-sectional expansion in an extended
flare dataset.
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All authors Yu Dai, Shihan Li, Wenlong Tang, Zhen Li, Mingde Ding
Earth and Planetary Astrophysics
Exo Skryer: A JAX-accelerated sub-stellar atmospheric retrieval framework
Elspeth K.H. Lee
Contemporary
exoplanet and brown
dwarf atmospheric research relies heavily on
retrieval frameworks to recover thermal and chemical properties and perform model comparison in an observational data-driven approach. However, the computational effort required for
retrieval modelling has rapidly increased, driven by JWST data that covers large spectral intervals at moderate spectral resolutions, and ground-based, high-resolution spectroscopy. To help tackle the computational burden faced by contemporary
retrieval requirements, I present a new sub-
stellar atmosphere
retrieval modelling framework, Exo Skryer, that utilises the JAX library for Python to enable scalable, computationally efficient forward modelling as well as posterior sampling. I present example
retrievals for pre- and current JWST era observations for both transmission and emission spectra, finding consistent results with previous
retrieval modelling efforts, apart from a WASP-107b test case. In addition, I present a new method to directly retrieve the real and imaginary optical constants ($n$, $k$) of suspected aerosol infrared absorption features. Due to its computational expediency, Exo Skryer will be highly suited for future demanding
retrieval efforts that incorporate more spatial dimensionality, complex forward models and high-dimensional parameter sets. Exo Skryer is available as open-source software on GitHub [https://github.com/ELeeAstro/Exo_Skryer].
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Earth and Planetary Astrophysics
Weak S-type asteroids compared to C-type explain the observed size distribution of the main belt
Michael Vávra and Miroslav Brož
The main belt, the region between the orbits of Mars and Jupiter, is home to more than 1 million asteroids. These asteroids form orbital groups, (i.e., asteroid families formed by collisions) and also spectral groups (taxonomies) with different chemical compositions, in particular carbonaceous (C-types) and silicate (S-types). In this paper, we extend the existing main-belt collisional model by finding the appropriate strength-versus-size dependence (also known as the scaling law) for these two groups. We used color indices and
geometric albedos of 56 and 72 spectroscopically confirmed C- and S-types (control samples), along with statistical methods on 1 065 034 asteroids, to assign C-, S-, or other types. This allowed us to construct observed size-frequency distributions (SFDs) for several subpopulations constrained by either semimajor axis (inner, middle, outer) or taxonomy (C, S, other). Then we used a Monte Carlo collisional model to compute the long-term collisional
evolution (4.5 billion years) and derive synthetic SFDs. Our best-fit scaling laws indicate that S-types must be weaker below approximately 0.2 km than C-types to explain the deficiency of asteroids in the inner part of the main belt near (and below) the observational limit. This may correspond to differences in chemical composition or material porosity. Future research will focus on the scaling laws of asteroids with rare or "extreme" taxonomies (e.g., V, M).
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Astrophysics of Galaxies
Searching for and characterizing halo substructures with the GALAH DR4 survey
Iryna Kushniruk, Kristopher Youakim, Karin Lind et al. (+12 more)
Recent studies show that the Milky Way
stellar halo is composed of populations of different origins, shaped by multiple
accretion events. To better understand the formation of the Milky Way and other spiral
galaxies, we characterize the chemical and kinematic properties of
halo substructures using GALAH DR4 and
Gaia data. We apply wavelet transforms in the space of sqrt(J_r) and azimuthal action (L_z) to identify kinematic overdensities.
Stars in the detected structures are analyzed in elemental abundance space to determine their origin. We further assess contamination using the unsupervised machine-learning
algorithm t-distributed
stochastic neighbor
embedding (t-SNE), performing chemical tagging with 15 elemental abundances. We recover five structures: the
Galactic disk, the Splash,
Gaia-Sausage-Enceladus (GSE), Thamnos1, and Thamnos2. GSE shows two peaks; one at sqrt(J_r) ~ 25 kpc km s^-1 is due to disk contamination, while the other above sqrt(J_r) ~ 40 kpc km s^-1 represents the cleanest GSE population. Thamnos exhibits three peaks linked to Thamnos1 and Thamnos2. Thamnos2 shows higher [alpha/Fe], iron-peak elements are enhanced in the Splash, and
halo groups retain a stronger r-process signature. The multiply peaked structures suggest that the splashed disk extends beyond prograde orbits. The distinct chemo-dynamical properties of the
halo groups support their extragalactic origin.
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All authors Iryna Kushniruk, Kristopher Youakim, Karin Lind, Sven Buder, Janes Kos, Diane Feuillet, Sarah L. Martell, Richard de Grijs, Geraint F. Lewis, Joss Bland-Hawthorn, Gary Da Costa, Michael Hayden, Daniel Zucker, Tomaz Zwitter, Sanjib Sharma
Astrophysics of Galaxies
MEDUSA I. Tracing magnetic field structures in tidal arms of the dwarf-dwarf merger NGC 1487
Sam Taziaux, Aritra Basu, Samata Das et al. (+11 more)
Dwarf galaxies are important laboratories for studying
cosmic magnetism because they can maintain strong
magnetic fields via the action of turbulent dynamo despite their low mass and weak gravitational potential. The
Magnetic-field
Evolution in
Dwarf galaxies from Ultra-deep SKA Analysis (MEDUSA) survey is the first SKA-pathfinder programme designed to obtain deep continuum, polarisation, and HI data for
dwarf galaxies, enabling a comprehensive study of their
radio spectra,
magnetic fields, and gas kinematics across a representative population. By analysing the
radio continuum spectra and polarisation of the
dwarf-
dwarf galaxy merger NGC 1487 from the MEDUSA sample, we aim to determine its
magnetic field strength and to characterise the large-scale and turbulent components of its
magnetic field. We utilise highly sensitive multi-band
radio continuum data from MeerKAT L-band (1.28 GHz) and Australia
Telescope Compact Array (ATCA) L/S (2.1 GHz), C (5.5 GHz), and X-bands (9 GHz). We analysed the
magnetic field configuration using polarisation and rotation measure (RM) synthesis. The integrated spectral energy distribution has a non-thermal spectral index of $\alpha_{\rm nth} = -0.678\pm0.085$. Synchrotron and inverse Compton losses cause a spectral break at $\nu_{\rm b} = 6.2\pm1.3$ GHz. In
star-forming regions, the
magnetic field exhibits strong small-scale fluctuations in RM, suggesting the action of a small-scale dynamo. Conversely, the field becomes more ordered, aligning with the
tidal arms toward the
galaxy's outskirts, showing a large-scale
magnetic field over $\approx3$ kpc. Observations of the
dwarf-
dwarf merger NGC 1487 show that even low-mass
galaxy mergers, likely the building blocks of larger
galaxies in the early Universe, can rapidly amplify and produce coherent large-scale
magnetic field structures, highlighting their key contribution in the early magnetisation of
galaxies.
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All authors Sam Taziaux, Aritra Basu, Samata Das, Dominik J. Bomans, Timothy J. Galvin, Alec J. M. Thomson, George H. Heald, Peter Kamphuis, Francesca Loi, Michael Stein, Krysztof T. Chyży, Christopher J. Riseley, Ralf-Jürgen Dettmar, Julia Becker Tjus
High Energy Astrophysical Phenomena
Unified study of nuclear physics and dark matter constraints through gravitational-wave observations of binary neutron star mergers
Nina Kunert, Guilherme Grams, William Newton et al. (+5 more)
Understanding the properties of strongly interacting matter at extreme densities is a central problem in fundamental physics, with
neutron star mergers offering a natural laboratory to probe this regime. However, the complexity of the merger process complicates the interpretation of the associated gravitational-wave and electromagnetic signals. This picture becomes even more complex in the potential scenario in which dark matter accumulates around and in
neutron stars, altering their structure and the associated observables. In this work, we study synthetic gravitational-wave observations of binary
neutron star mergers with next-generation detectors, investigating their potential to extract both
nuclear physics and dark matter constraints. We also examine how the potential presence of fermionic, non-self-interacting dark matter inside
neutron stars affects the inference of
nuclear empirical parameters. We find that combining observations can tighten constraints on
nuclear empirical parameters. However, the inferred values remain sensitive to systematic modeling biases and intrinsic degeneracies among the parameters. Conversely, our analysis reveals that for non-self-interacting fermionic dark matter at mass fractions below one percent, it will be unlikely to find decisive evidence for dark matter when analyzing gravitational-wave signals. Consequently, systematic biases in
nuclear empirical parameter inference potentially resulting from such a dark matter component are expected to be negligible even for observations with next-generation gravitational-wave detectors.
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All authors Nina Kunert, Guilherme Grams, William Newton, Edoardo Giangrandi, Anna Puecher, Hauke Koehn, Violetta Sagun, Tim Dietrich
Astrophysics of Galaxies
Probing dark matter distributions with the pericentre precession of the stellar orbits near the Galactic Centre black hole
Debojit Paul and Sanjeev Kalita
The
Galactic Centre black hole provides a naive environment for understanding unknown matter distribution and new gravitational physics. For this
stellar orbits in the
nuclear star cluster are reliable probes. We investigate different dark matter mass profiles through pericentre shift of
stellar orbits near the black hole. We also study capability of existing and upcoming astrometric facilities to detect dark matter induced precession and to distinguish between several dark matter profiles. Parameters of different dark matter density profiles are estimated by using the most recent upper bound on dark mass near the black hole. These profiles are then used for calculating the gravitational potential and hence the relativistic pericentre shift of both low and high eccentricity orbits of 13 S-
stars. We use the recently measured deviation parameter $f_{sp}$ for investigating competition between dark matter and gravitational physics within S2's orbit. The astrometric shift of the pericentres has been calculated and compared with existing and upcoming astrometric capabilities of large and extremely large
telescopes. The orbit of S2 is found to be insensitive to dark matter induced precession. Low eccentricity and wider orbits are prominent probes for measuring dark matter induced precession which is accessible to present and upcoming astrometric facilities such as Keck,
GRAVITY and TMT. The existing and upcoming facilities can distinguish between different dark matter profiles for some
stars and hence they posses the capability to distinguish between possible formation histories of the central region of our
Galaxy.
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High Energy Astrophysical Phenomena
A Realistic Pulsar – Supermassive Black Hole Timing Model
Zexin Hu, Ziming Wang and Lijing Shao
Timing observation of
pulsars orbiting around a supermassive black hole (SMBH) can measure the spacetime around the SMBH to a high precision and thus be a novel probe of the
gravity theory. Future high-frequency surveys of the
Galactic Centre (GC) region to be performed by the next-generation
radio telescopes, such as the SKA, may discover
pulsars that orbit around Sagittarius A* (Sgr A*), the SMBH dwelling in our GC. In this paper, we present a realistic
pulsar-SMBH timing model based on the post-Newtonian equations of motion of the
pulsar. Considering the expected timing precision in the future, we take into account several next-to-leading order light propagation time delays in the timing model. For the first time, we include the effects of proper motion of Sgr A*, which were expected to break the
spin measurement degeneracy. We forecast the measurement precision of various parameters of Sgr A*, and discuss the data analysis procedure in the presence of red noise, which can be strong if the
pulsar is a normal
pulsar. The realistic timing model constructed in this study will serve as a useful tool in future searching and timing of
pulsar-SMBH systems in the GC.
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Cosmology and Nongalactic Astrophysics · Cross-listed from gr-qc
Chaotic imprints of dark matter in extreme mass-ratio inspirals
Mustapha Azreg-Aïnou, Mubasher Jamil and Emmanuel N. Saridakis
Extreme mass-ratio inspirals (EMRIs) are among the most powerful probes of strong-field
gravity and of the environments surrounding supermassive compact objects. Motivated by the expected presence of dark matter near
galactic centers, we investigate the emergence and gravitational-wave imprints of chaotic dynamics in EMRIs evolving in non-
vacuum spacetimes. Within a unified dynamical framework, we analyze test-particle motion in a broad class ofdark-matter-embedded geometries, including singular black holes, regular black holes, naked singularities, and Einstein-cluster configurations. We show that environmental perturbations generically break integrability in the strong-field regime, giving rise to chaotic motion whose onset, duration, and termination depend sensitively on horizon structure, core regularization, and matter distribution. Using the numerical Kludge approach, we demonstrate that chaotic trajectories produce systematic qualitative modifications of the emitted gravitational radiation, such as irregular amplitude modulation and loss of phase coherence, in contrast to the smooth, quasi-periodic waveforms generated by regular motion. Our results establish the robustness of chaos in environmentally perturbed EMRIs and provide a clear conceptual link between nonlinear orbital dynamics, spacetime structure, and observable gravitational-wave signatures.
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Astrophysics of Galaxies
SMMAN: quasi-Simultaneous Multi-wavelength Monitoring of gamma-ray-loud AGNs with the Nanshan 26-m radio telescope
Lang Cui, Krishna Mohana A, Xin Wang et al. (+3 more)
Active
Galactic Nuclei (AGNs) are characterized by strong temporal flux density variability across the electromagnetic spectrum, offering insights into the complex physical processes governing
accretion and
plasma outflows. To systematically investigate AGNs flux density variability in
radio bands, a long-term program was initiated in late 2016: quasi-Simultaneous Multiwavelength Monitoring of gamma-ray-loud AGNs with the Nanshan 26-m
radio telescope (SMMAN). This work presents the first data release of the SMMAN program, spanning over eight years from 2016 to 2024 with observations at 4.8 and 23.6 GHz. The SMMAN sample includes 131 northern ($\delta >\sim0^{\circ}$) sources selected from the
Fermi Large Area
Telescope third source catalog. The characteristics of variability, spectral index, luminosity, and $\gamma$-ray loudness factor are examined for different AGN classes within the sample. Target sources exhibit stronger variability at 23.6 GHz compared to 4.8 GHz, with BL Lac objects being more variable than flat-spectrum
radio quasars (FSRQs). BL Lacs generally have flatter
radio spectra, while FSRQs, blazar candidates of uncertain type (BCUs), and
radio galaxies (RDGs) span a wider range from flat to steep. FSRQs are more
radio-luminous than BL Lacs and other classes, with BCUs intermediate and RDGs generally fainter. FSRQs and BL Lacs have higher $\gamma$-ray loudness factors than RDGs, while BCUs have intermediate values. The SMMAN
dataset, incorporated with other historical and ongoing monitoring programs, will provide a unique opportunity to investigate the
evolution of spectral energy distributions, search for quasi-periodic oscillations, and analyze supermassive black hole binary systems.
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All authors Lang Cui, Krishna Mohana A, Xin Wang, Ning Chang, Guiping Tan, Xiang Liu
Cosmology and Nongalactic Astrophysics
The Hydrostatic Mass Bias and the $\sigma_8$ Tension: A Multi-Probe Forecast for Stage-IV/V Surveys
Ayodeji Ibitoye, Prabhakar Tiwari, Qi Xiong et al. (+1 more)
The hydrostatic mass bias ($b_{\mathrm{HSE}}$) is a leading systematic uncertainty in cluster cosmology and a principal source of degeneracy with $\sigma_8$ and $\Omega_m$. We investigate the capability of Stage-IV CMB and optical surveys to calibrate $b_{\mathrm{HSE}}$ using tomographic cross-correlations between the thermal Sunyaev–Zel'dovich (tSZ) effect,
galaxy clustering, and weak
lensing. We perform a Fisher forecast incorporating realistic survey noise, foreground modeling for clustered CIB and
radio sources, and full marginalization over cosmological and astrophysical nuisance parameters, including per-bin
galaxy bias perturbations, photometric
redshift shifts, intrinsic
alignments, and baryonic feedback modeled with HMCode2020. With optimized tomographic binning (10 lens and 5 source bins for LSST; 6 lens and 5 source bins for CSST), we forecast marginalized constraints of $0.98\%$ for SO+LSST, $1.60\%$ for CMB-S4+LSST, and $2.40\%$ for CMB-S4+CSST.
Tomography improves $b_{\mathrm{HSE}}$ precision by factors of approximately three relative to non-tomographic analyses, reflecting the role of
redshift information in breaking the $b_{\mathrm{HSE}}$–$\sigma_8$ degeneracy. Optical-only probes provide no direct constraint on $b_{\mathrm{HSE}}$, whereas inclusion of tSZ-containing spectra enables percent-level calibration under realistic systematic assumptions. The results demonstrate that multi-probe tomographic analyses with Stage-IV surveys can achieve robust control of hydrostatic mass bias, strengthening cluster-based constraints on structure growth.
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All authors Ayodeji Ibitoye, Prabhakar Tiwari, Qi Xiong, Yan Gong
Earth and Planetary Astrophysics
Surface Properties, Orbital Dynamics, and Thermophysical Modeling of the Primitive Asteroid (269) Justitia
Leonardo Braga, Andre Amarante, Alessandra Ferreira et al. (+2 more)
The Emirates Mission to the Asteroid Belt (EMA) will study the ultra-red asteroid (269)~Justitia. In this work, we present the first detailed investigation of Justitia's surface dynamics using the newly developed 3-D polyhedral shape model with 574 vertices and 1,144 faces. We analyze its geopotential, surface acceleration, escape speeds, slopes, and
equilibrium points, and we also search for planar symmetric periodic orbits using an equivalent ellipsoidal approximation. Our results indicate that the lowest geopotential values occur at the poles, which also correspond to regions of maximum surface acceleration. The global slope distribution suggests preferred zones of material accumulation or migration, offering clues to Justitia's long-term morphological
evolution. Most slopes remain below $40^\circ$, implying that loose particles may settle stably across large portions of the surface. We identify five
equilibrium points consistent with Justitia's estimated density and slow rotational period. Two external points (E$_2$ and E$_4$) exhibit linear stability, and all
equilibrium locations lie relatively far from the surface due to the body's slow
spin. Additionally, we discover 28 new families of planar symmetric periodic orbits, then classify their
topologies and determine their linear stability, providing a dynamical framework relevant to future spacecraft operations near Justitia. Finally, thermal modeling reveals how thermal inertia and heliocentric distance shape Justitia's temperature distribution. The south pole receives more insolation than the north pole, reaching minimum temperatures of about 102~K and 87~K, respectively. These combined dynamical and thermal results offer valuable insights for the EMA mission and for understanding slowly rotating small bodies.
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All authors Leonardo Braga, Andre Amarante, Alessandra Ferreira, Filipe Monteiro, Maria Martins
Solar and Stellar Astrophysics
Long Photometric Cycles in Double Periodic Variables from Nodal Precession of a Tilted Accretion Disk
Cheng-Liang Jiao, Er-gang Zhao, Liying Zhu et al. (+1 more)
We investigate whether the long photometric cycles observed in double-periodic variables (DPVs) can arise from nodal precession of a tilted
accretion disk driven by the
tidal torque of the companion. Within a simple analytical framework, we derive testable relations linking the long-to-orbital period ratio to the binary mass ratio, the normalized disk size, and the disk tilt angle $\beta$, which itself can be inferred from the long-cycle amplitude, orbital inclination $i$, and disk luminosity fraction. The model naturally reproduces the two observed long-cycle light-curve morphologies – sinusoidal and double-hump – distinguished by the
geometric criterion $i+\beta \le 90^\circ$ versus $i+\beta>90^\circ$. Applying these relations to a sample of DPVs, we find that the inferred disk sizes are physically reasonable and consistent with independent light-curve modeling for a non-negligible subset of systems. Our results show that
tidal nodal precession represents a viable and potentially important contributor to the long-period variability of DPVs and provide a quantitative framework for future observational and theoretical studies.
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All authors Cheng-Liang Jiao, Er-gang Zhao, Liying Zhu, Azizbek Matekov