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Physics Astrophysics

astro-ph Watch Astrophysics

Monday 5 January

Instrumentation and Methods for Astrophysics

Prospects for identifying pulsar candidates in radio surveys using scintillation

Jitendra Salal, Shriharsh P. Tendulkar and Visweshwar Ram Marthi

In our previous paper, we developed a technique for identifying pulsar candidates in interferometric radio images using their distinctive scintillation signatures. Building on this technique, the present study simulates a pulsar population using the PsrPopPy Python module to investigate the technique's limitations and detection capabilities. Among pulsars detectable exclusively by this technique, 50% have duty cycles exceeding the mean value of 0.09 observed in time-domain detections. Our pulsar population simulations revealed a set of observational parameters that optimize pulsar detection. An observation frequency of ~ 1420 MHz and a channel width of ~10 kHz emerge as the optimal configuration to maximize the pulsar detection efficiency. By applying a scintillation-based technique to future radio telescopes like DSA-2000, we can detect 56% of normal pulsars and 84% of MSPs in addition to those detected using non-imaging, time-domain surveys. These detected pulsars cannot be verified by time-domain searches.
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Cosmology and Nongalactic Astrophysics

Joint Constraints on Neutrinos and Dynamical Dark Energy in Minimally Modified Gravity

Artur Ladeira, Rafael C. Nunes, Supriya Pan et al. (+1 more)

The \(w_{\dagger}\)VCDM framework provides a theoretically well-controlled extension of \(\Lambda\)CDM within the class of minimally modified gravity theories, allowing for flexible cosmological background evolution and linear perturbation dynamics while remaining free of pathological instabilities. In this work, we have shown that this scenario remains robust when confronted with current cosmological observations, even in the presence of an extended neutrino sector. Combining Planck CMB data with DESI DR2 BAO and DESY5 supernovae, we obtain stringent constraints on neutrino physics, including \(\sum m_\nu < 0.11~\mathrm{eV}\) (95% CL) and \(N_{\rm eff} = 2.98^{+0.13}_{-0.14}\), fully consistent with Standard Model expectations. Crucially, the data exhibit a statistically significant preference for a late-time dark-energy transition, characterized by a robust quintessence–phantom crossing that remains stable across all dataset combinations and neutrino-sector extensions, including the presence of a sterile neutrino. The combined effects of modified late-time expansion and additional relativistic degrees of freedom systematically raise the inferred Hubble constant, substantially alleviating the \(H_0\) tension without invoking early dark energy or introducing theoretical instabilities. Overall, the \(w_{\dagger}\)VCDM scenario emerges as a compelling phenomenological framework that simultaneously accommodates current constraints on neutrino physics, provides an excellent fit to recent BAO and supernovae data, and offers a viable pathway toward resolving persistent tensions in the standard cosmological model.
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All authors Artur Ladeira, Rafael C. Nunes, Supriya Pan, Weiqiang Yang

Cosmology and Nongalactic Astrophysics

Nonlinear Scales in Luminal Horndeski – I. Halo mass function and power spectrum boost in models with Vainshtein screening

Dani de Boe, Mattia Pantiri, Gen Ye et al. (+1 more)

We investigate nonlinear structure formation in Horndeski gravity with luminal gravitational wave speed ($c_T = 1$), assuming Vainshtein screening within the spherical collapse model. We compute the critical and virial overdensities and evaluate the halo mass function. Building on the reaction approach, we present a framework for the computation of the reaction and the resulting nonlinear matter power spectrum using the EFTofDE formulation of Horndeski gravity. We show results for the case of EFT functions that trace the evolution of dark energy, and specialize to the cubic galileon and nDGP models for benchmarking against existing results. The framework interfaces with EFTCAMB for the linear evolution, though alternatives are possible. While restricted to Vainshtein-screened models, the current implementation focuses on qualitative trends and parameter dependencies. Further refinements and extensions to other screening mechanisms will be addressed in future work.
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All authors Dani de Boe, Mattia Pantiri, Gen Ye, Alessandra Silvestri

Solar and Stellar Astrophysics

A phoenix rises from the ashes: WOH G64 is still a red supergiant, for now

Jacco Th. van Loon and Keiichi Ohnaka

For a long time, WOH G64 was known as the most extreme red supergiant outside our Galaxy. However, in a matter of years it has faded, its pulsations have become suppressed and the spectrum has become dominated by emission lines from ionised gas, a far cry from the Mira-like pulsation and late M-type spectrum it used to display. Around the same time, a hot dust cloud was discovered using the VLT interferometer. WOH G64 has been claimed to have turned into a yellow hypergiant, which could signal a pre-supernova post-red supergiant evolution. Here we present spectra of WOH G64 obtained with the Southern African Large Telescope (SALT) between November 2024 and December 2025. Molecular absorption bands from TiO are seen at all times. This implies that WOH G64 is currently a red supergiant, and may never have ceased to be. However, the shallow, resolved bands and possible detection of VO hint at a highly extended atmosphere. The continuum appears to be varying, while the line emission shows a different behaviour, suggesting two separate components in the system. Meanwhile, atomic absorption lines are deepening. This places important constraints on scenarios for the dramatic events that are unfolding.
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Solar and Stellar Astrophysics

The SALT survey of helium-rich hot subdwarfs: unsupervised classification and kinematic analysis

Asish Philip Monai and C. Simon Jeffery

Hydrogen-deficient stars form sequences across the HR diagram from cool R CrB stars to helium-rich hot subdwarfs and PG1159 stars, tracing multiple evolution pathways. The Southern African Large Telescope (SALT) has been used to conduct a medium-resolution spectroscopic survey of 697 helium-rich hot subdwarfs and related stars. Using 587 stars from the full SALT sample, we define an unsupervised data-led classification system based on Principal Components Analysis (PCA) and Spectral Clustering (SC), designed as a data-discovery tool to identify possible new groups and sequences within the data. Using the first 3 principal components (PCs), we identify 6 major clusters of hot subdwarf spectra, identified with the traditional spectral classes of classical sdB and sdO stars, helium-rich He-sdO stars and very hot subdwarfs. Two clusters covering large volumes of PC space include a) He-sdB and He-sdOB stars and b) intermediate iHe-sdB and iHe-sdOB stars. Most spectra in these major clusters form connected sequences in PC space. Using a second stage of PCA and SC, we identify sub-clusters within 4 major clusters, particularly in the He-sdB/OB and iHe-sdB/OB clusters. In comparison with traditional MK-like classification, we find that the PC clusters are reasonably well separated, with some overlap at cluster boundaries. For very hot sdOs, where the number of standards is small, PC classification has led to a revision of the Drilling MK-like system. Gaia DR3 measurements have been used to determine kinematic parameters for the PC-defined classes. Although disk stars account for a significant fraction of all classes, He-sdOs and Hot-sdOs include a higher fraction of halo stars.
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High Energy Astrophysical Phenomena

Disc Winds From Accreting Systems in the 2040s

Noel Castro Segura, Virginia Cúneo, Francesco Tombesi et al. (+9 more)

What does the temporal evolution of disc winds tell us about accreting systems and the accretion process? Studies of accretion-disc outflows across all mass scales, including accreting white dwarfs, X-ray binaries, and active galactic nuclei, have shown that winds play a key role in regulating both the accretion flow and the surrounding environment. Disc winds therefore provide a common thread linking a broad range of scientific topics, from the microphysics of accretion to galaxy-scale feedback and evolution, as well as binary evolution and the predicted rates of energetic (multi-messenger) transient phenomena. Yet we still lack a comprehensive picture of the accretion-feedback process. Optical spectroscopy has revealed striking similarities across mass scales, hinting at common production mechanisms, and has shown that winds can evolve on timescales of only minutes. Progress, however, has been limited by their transient nature, sparse time coverage, and the lack of simultaneous, high-resolution spectroscopy. Time-domain facilities with high temporal and spectral resolution will allow us to track these events in high accretion-rate systems, constrain their launching mechanisms, and measure the mass, energy, and angular momentum they carry. This will provide crucial input for binary evolution models, wind feedback, and a unified view of accreting systems across mass scales.
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All authors Noel Castro Segura, Virginia Cúneo, Francesco Tombesi, Stefanie Fijma, Jesús Corral-Santana, Alexandra Veledina, Alessandra Ambrifi, David Buckley, Piergiorgio Casella, Deanne L. Coppejans, Domitilla de Martino, Simone Scaringi

Solar and Stellar Astrophysics

The Betelgeuse Enigma: The Betelbuddy Hypothesis

Priya Hasan

In the past six years, Betelgeuse has been in the news and drawn significant public interest. Starting in October 2019, Betelgeuse underwent a striking dimming event, fading from magnitude 0.5 to 1.7 by mid February 2020 a threefold decrease in brightness This gave rise to a number of speculative debates that the star was on the verge of a supernova, a moment of eerie quiet before the cosmic outburst. In a previous article, the author discussed the most accepted explanation to the dimming caused by episodic mass loss that released large dust grains, which obscured Betelgeuse's light and made it appear fainter. This interpretation suggested that the dimming was not a precursor to a supernova, as Betelgeuse is likely still far from reaching that stage. On 21 July 2025, the existence of the companion star was confirmed with direct imaging, for the first time, by the alopeke instrument on the 8.1 m Gemini North telescope. The companion is 6 magnitudes fainter than Betelgeuse and orbits close to Betelgeuse itself, within the supergiant star's extended outer atmosphere. The stellar companion was detected at an angular separation of 52 mas and a position angle of 115 deg east of north. These measurements, along with its brightness, being roughly 6 magnitudes fainter than Betelgeuse at 466 nm, are in excellent agreement with dynamical predictions. Although this was only a 1.5 sigma detection, the agreement in the companion's appearance, separation, position angle, magnitude difference, and estimated mass is reasonable, making the result tentatively acceptable. The next optimum period for observations is November 2027, when we hope to get better observations. This article describes the interesting twists and turns of this study and what lies in the future for Betelgeuse and its companion, Betelbuddy or Siwarha.
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Cosmology and Nongalactic Astrophysics

Euclid: Improving redshift distribution reconstruction using a deep-to-wide transfer function

Y. Kang, S. Paltani, W. G. Hartley et al. (+165 more)

The Euclid mission seeks to understand the Universe expansion history and the nature of dark energy, which requires a very accurate estimate of redshift distribution. Achieving this accuracy relies on reference samples with spectroscopic redshifts, together with a procedure to match them to survey sources for which only photometric redshifts are available. One important source of systematic uncertainty is the mismatch in photometric properties between galaxies in the Euclid survey and the reference objects. We develop a method to degrade the photometry of objects with deep photometry to match the properties of any shallower survey in the multi-band photometric space, preserving all the correlations between the fluxes and their uncertainties. We compare our transfer method with more demanding image-based methods, such as Balrog from the Dark Energy Survey Collaboration. According to metrics, our method outperforms Balrog. We implement it in the redshift distribution reconstruction, based on the self-organising map approach of arXiv:1509.03318, and test it using a realistic sample from the Euclid Flagship Simulation. We find that the key ingredient is to ensure that the reference objects are distributed in the colour space the same way as the wide-survey objects, which can be efficiently achieved with our transfer method. In our best implementation, the mean redshift biases are consistently reduced across the tomographic bins, bringing a significant fraction of them within the Euclid accuracy requirements in all tomographic bins. Equally importantly, the tests allow us to pinpoint which step in the calibration pipeline has the strongest impact on achieving the required accuracy. Our approach also reproduces the overall redshift distributions, which are crucial for applications such as angular clustering.
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All authors Y. Kang, S. Paltani, W. G. Hartley, M. Bolzonella, A. H. Wright, F. Dubath, F. J. Castander, D. C. Masters, W. d'Assignies, H. Hildebrandt, O. Ilbert, M. Manera, W. Roster, S. A. Stanford, N. Aghanim, B. Altieri, S. Andreon, N. Auricchio, H. Aussel, C. Baccigalupi, M. Baldi, S. Bardelli, P. Battaglia, A. Biviano, E. Branchini, M. Brescia, J. Brinchmann, S. Camera, G. Cañas-Herrera, V. Capobianco, C. Carbone, V. F. Cardone, J. Carretero, S. Casas, M. Castellano, G. Castignani, S. Cavuoti, K. C. Chambers, A. Cimatti, C. Colodro-Conde, G. Congedo, L. Conversi, Y. Copin, A. Costille, F. Courbin, H. M. Courtois, M. Cropper, H. Degaudenzi, G. De Lucia, H. Dole, C. A. J. Duncan, X. Dupac, S. Dusini, A. Ealet, S. Escoffier, M. Farina, R. Farinelli, S. Farrens, F. Faustini, S. Ferriol, F. Finelli, N. Fourmanoit, M. Frailis, E. Franceschi, M. Fumana, S. Galeotta, K. George, B. Gillis, C. Giocoli, J. Gracia-Carpio, A. Grazian, F. Grupp, S. V. H. Haugan, H. Hoekstra, W. Holmes, F. Hormuth, A. Hornstrup, P. Hudelot, K. Jahnke, M. Jhabvala, B. Joachimi, E. Keihänen, S. Kermiche, A. Kiessling, B. Kubik, M. Kümmel, M. Kunz, H. Kurki-Suonio, R. Laureijs, A. M. C. Le Brun, S. Ligori, P. B. Lilje, V. Lindholm, I. Lloro, G. Mainetti, D. Maino, E. Maiorano, O. Mansutti, S. Marcin, O. Marggraf, M. Martinelli, N. Martinet, F. Marulli, R. J. Massey, E. Medinaceli, S. Mei, Y. Mellier, M. Meneghetti, E. Merlin, G. Meylan, A. Mora, M. Moresco, L. Moscardini, R. Nakajima, C. Neissner, S.-M. Niemi, C. Padilla, F. Pasian, K. Pedersen, V. Pettorino, S. Pires, G. Polenta, M. Poncet, L. A. Popa, L. Pozzetti, F. Raison, A. Renzi, J. Rhodes, G. Riccio, E. Romelli, M. Roncarelli, R. Saglia, Z. Sakr, A. G. Sánchez, D. Sapone, B. Sartoris, P. Schneider, T. Schrabback, A. Secroun, G. Seidel, S. Serrano, P. Simon, C. Sirignano, G. Sirri, L. Stanco, J. Steinwagner, P. Tallada-Crespí, A. N. Taylor, I. Tereno, N. Tessore, S. Toft, R. Toledo-Moreo, F. Torradeflot, I. Tutusaus, J. Valiviita, T. Vassallo, A. Veropalumbo, Y. Wang, J. Weller, G. Zamorani, F. M. Zerbi, I. A. Zinchenko, E. Zucca, J. García-Bellido, J. Martín-Fleitas, V. Scottez, M. Viel, R. Teyssier

High Energy Astrophysical Phenomena

Proton Acceleration by Collisionless Shocks in Supermassive Black Hole Coronae: Implications for High-Energy Neutrinos

Minh Nhat Ly, Yoshiyuki Inoue, Yasuhiko Sentoku et al. (+1 more)

Recent observations by the IceCube Neutrino Observatory have revealed a significant excess of high-energy neutrinos from nearby Seyfert galaxies, such as NGC~1068, without a corresponding flux of high-energy gamma-rays. This suggests that neutrinos are produced via hadronic interactions in a region opaque to gamma-rays, likely a hot corona surrounding the central supermassive black hole. However, the mechanism responsible for accelerating the parent protons to the required energies ($\sim 100$ TeV) remains an open question. In this study, we investigate diffusive shock acceleration (DSA) in active galactic nucleus (AGN) coronae using a suite of one-dimensional Particle-in-cell (PIC) simulations spanning a broad range of plasma parameters. We find that DSA is a robust and efficient mechanism for proton acceleration, consistently channeling approximately 10% of the shock's kinetic energy into non-thermal ions, even for shocks with sonic Mach number as low as $ M_s \approx 2$. In contrast, the efficiency of electron acceleration is highly variable and less efficient ($<1\%$) in our parameter survey. These findings provide strong, first-principles support for the hadronic models of neutrino production in AGN and offer quantitative constraints that can explain the observed gamma-ray deficit.
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All authors Minh Nhat Ly, Yoshiyuki Inoue, Yasuhiko Sentoku, Takayoshi Sano

Astrophysics of Galaxies

ODIN: Clustering Properties of Ly$\alpha$ Blobs at $z$ $\sim$ 2.4 and 3.1

Byeongha Moon, Yujin Yang, Eric Gawiser et al. (+18 more)

Spatially extended Ly$\alpha$ nebulae, known as Ly$\alpha$ blobs (LABs), are a rare population at $z > 2$ that are thought to trace proto-groups or the progenitors of massive galaxies in the present-day universe. However, their dark matter halo properties (e.g., halo mass) are still uncertain due to their rarity and strong field-to-field variation. The One-hundred-deg$^2$ DECam Imaging in Narrowbands (ODIN) survey has discovered 103 and 112 LABs in the extended ($\sim$9~\sqdeg) COSMOS field at $z\sim2.4$ and 3.1, respectively, enabling estimation of their bias and host halo masses through clustering analysis. We measure the angular auto-correlation functions (ACFs) of LABs and derive galaxy bias factors of $b$ = $4.0\pm0.8$ and $3.8\pm0.7$, corresponding to minimum halo masses of $2.8^{+3.0}_{-1.8}$ and $0.7^{+0.8}_{-0.5}\times10^{12}~M_\odot$ and median halo masses of $4.2^{+3.8}_{-2.5}$ and $1.1^{+1.1}_{-0.7}\times10^{12}~M_\odot$ at $z\sim2.4$ and 3.1, respectively. LABs occupy $\sim$11$^{+39}_{-8}$% and $\sim$3$^{+9}_{-2}$% of all dark matter halos above these minimum halo masses. These findings suggest that LABs inhabit massive dark matter halos, likely tracing proto-group environments that evolve into present-day massive halos ($\sim$10$^{13}~M_\odot$), where massive elliptical galaxies or galaxy groups reside, by $z=0$.
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All authors Byeongha Moon, Yujin Yang, Eric Gawiser, Kyoung-Soo Lee, Danisbel Herrera, Vandana Ramakrishnan, Nelson Padilla, Nicole M. Firestone, Seongjae Kim, Robin Ciardullo, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Julie B. Nantais, Changbom Park, Hyunmi Song

Astrophysics of Galaxies

Unveiling Fiber Networks and Core Formation in the DR21 South Filament

Kai Yang, Keping Qiu and Xing Pan

We present high-resolution ($\sim$1000 AU) 3 mm observations with the NOrthern Extended Millimeter Array toward the DR21 South Filament, aiming to reveal its internal fragmentation and search for deeply embedded star-forming activities. Both the continuum and molecular line emissions align well with the filament axis traced by the low-resolution ($\sim$18$^{\prime\prime}$) column density map. The 3 mm continuum, CS (2$-$1), and HCO$^+$ (1$-$0) emissions reveal continuous and diffuse structures with measured FWHM widths of 0.054, 0.029, and 0.030 pc, respectively. In contrast, the H$^{13}$CO$^+$ (1$-$0) emission appears more clumpy and localized. The non-thermal motion in the filament is predominantly subsonic to transonic. We detect 13 dense cores in NH$_2$D (1$_{11}-1_{01}$), three of which coincide with continuum peaks; virial analysis suggests most are gravitationally bound. Using a friend-of-friend algorithm, we identify 32, 34, and 22 velocity-coherent fibers from the CS, HCO$^+$, and H$^{13}$CO$^+$ data, respectively. Compared to fibers traced by CS and HCO$^+$, H$^{13}$CO$^+$ fibers are more frequently associated with NH$_2$D cold cores and exhibit higher average mass-per-unit-length values. Differences among CS, HCO$^+$, and H$^{13}$CO$^+$ emissions likely arise from variations in effective critical densities. These results are consistent with a hierarchical structure, in which the 3.6-pc DR21SF contains velocity-coherent fibers and gravitationally bound dense cores.
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High Energy Astrophysical Phenomena

Strangeon Ergostars

Haojia Xia, Shichuan Chen, Hong-Bo Li et al. (+2 more)

The nature of the central engine powering short gamma-ray bursts (sGRBs) in binary neutron star (BNS) mergers remains a key open question in the era of multi-messenger astronomy. The ergostar hypothesis, that a rapidly rotating star with an ergoregion can act as a powerful energy source, offers an alternative explanation to the black hole-accretion disk paradigm. In this work, however, we examine this hypothesis using a phenomenological EOS of strangeon matter, i.e., condensed matter with nucleon-like units for three flavors of quarks. By constructing a large suite of uniformly rotating equilibrium models, we systematically investigate the parameter space of the stable ergostars and calculate their maximum extractable energy. We demonstrate that strangeon matter supports a vast and robust parameter space for dynamically stable ergostars, even without requiring differential rotation. We find that the extractable rotational energy from these configurations can be on the order of $0.01 M_\odot$, representing a massive energy reservoir, even when accounting for baryonic mass variations (e.g., mass ejection and particle capture during the Penrose process). Our results suggest that BNS merger remnants composed of exotic matter could play a crucial, previously underestimated role in high-energy astrophysics.
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All authors Haojia Xia, Shichuan Chen, Hong-Bo Li, Enping Zhou, Ren-Xin Xu

Cosmology and Nongalactic Astrophysics

The Dilaton: A Natural Resolution to the Hubble Tension via Spontaneous Scale Symmetry Breaking

Arpit Kottur, Jui Mahajan and Raka Dabhade

The statistical tension between early and late universe measurements of the Hubble constant ($H_0$) suggests that the dark sector is dynamical rather than static. We propose that this dynamics arises from a fundamental symmetry principle: the Spontaneous Breaking of Scale Invariance. We introduce the Dilaton ($\chi$), a Pseudo-Nambu-Goldstone Boson (PNGB) associated with dilatation symmetry breaking. We demonstrate that a simple quadratic mass term in the fundamental theory transforms, via conformal coupling to gravity, into a ”thawing” exponential potential $V(\phi) \propto e^{-\lambda\phi}$ in the Einstein frame. Using recent Bayesian reconstructions of dark energy dynamics from Planck, Pantheon+, and SH0ES data, we constrain the potential slope to be $\lambda \approx 0.056$. We show that this observational value is not arbitrary but corresponds to a fundamental non-minimal coupling strength of $\xi \approx 7.8 \times 10^{-4}$. The Dilaton mechanism naturally generates the late-time equation of state evolution ($w_0 \approx -0.85$) required to alleviate the Hubble tension while protecting the field mass $m \sim H_0$ through approximate shift symmetry.
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Instrumentation and Methods for Astrophysics

Accelerating cosmological simulations on GPUs: a step towards sustainability and green-awareness

Giovanni Lacopo, Marius Daniel Lepinzan, David Goz et al. (+7 more)

The increasing complexity and scale of cosmological N-body simulations, driven by astronomical surveys like Euclid, call for a paradigm shift towards more sustainable and energy-efficient high-performance computing (HPC). The rising energy consumption of supercomputing facilities poses a significant environmental and financial challenge. In this work, we build upon a recently developed GPU implementation of pinocchio, a widely-used tool for the fast generation of dark matter (DM) halo catalogues, to investigate energy consumption. Using a different resource configuration, we confirmed the time-to-solution behavior observed in a companion study, and we use these runs to compare time-to-solution with energy-to-solution. By profiling the code on various HPC platforms with a newly developed implementation of the Power Measurement Toolkit (PMT), we demonstrate an 8x reduction in energy-to-solution and 8x speed-up in time-to-solution compared to the CPU-only version. Taken together, these gains translate into an overall efficiency improvement of up to 64x. Our results show that the GPU-accelerated pinocchio not only achieves substantial speed-up, making the generation of large-scale mock catalogues more tractable, but also significantly reduces the energy footprint of the simulations. This work represents an step towards “green-aware" scientific computing in cosmology, proving that performance and sustainability can be simultaneously achieved.
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All authors Giovanni Lacopo, Marius Daniel Lepinzan, David Goz, Giuliano Taffoni, Luca Tornatore, Pierluigi Monaco, Pascal Jahan Elahi, Ugo Varetto, Maciej Cytowski, Lubomir Riha

High Energy Astrophysical Phenomena

Pulsar Gleaners: Discovery of 19 Pulsars in FAST Archival Data at $|b|<5\deg$ and Decl.$<-5\deg$

Shi-Jie Gao, Yi-Xuan Shao and Xiang-Dong Li

We report the discovery of 19 new pulsars identified from archival observations of the Five-hundred-meter Aperture Spherical radio Telescope (FAST) within Galactic latitudes $|b|<5\deg$ and declinations ${\rm Decl.}<-5\deg$. The dataset was recorded using FAST's $L$-band 19-beam receiver and covered $\sim 3.6~{\rm deg}^2$ with a cumulative integration time of $\sim$ 500 hr and a total raw data volume of $\sim$ 700 TB. Our search employed fast Fourier transform (FFT)-based and fast folding algorithm (FFA)-based periodic searches, and the single-pulse search. These new pulsars have spin periods range from 0.03 to 5.54 s. Two have periods under 0.1 s, suggesting they are likely young pulsars or mildly recycled pulsars. Four pulsars exhibit dispersion measures (DMs) exceeding $1000~{\rm pc~cm^{-3}}$ with PSR J1839$-$0558t having the highest value in our sample at $\sim 1271~{\rm pc~cm^{-3}}$, providing valuable samples for pulsar studies in the high-DM regime. Two rotating radio transients, PSRs J1836$-$0552t and J1847$-$0624t, were detected by FFA and single-pulse searches but failed with the FFT-based searches. In addition, three faint pulsars that were also missed by FFT-based searches were successfully detected using FFA. These discoveries demonstrate the critical role of FFA in uncovering faint, long-period, and sporadic pulsars, and highlight the significant potential of FAST archival data, especially when combined with longer integration times and complementary search techniques, to reveal rare and weak pulsar populations.
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High Energy Astrophysical Phenomena · Cross-listed from hep-ph

Color-Singlet and Color-Octet Quark Matters

Cheuk-Yin Wong

Quarks and antiquarks carry color and electric charges and belong to the color-triplet $3$ group and the color-antitriplet $\bar 3$ group respectively. The product groups of $3$ and $\bar 3$ consist of the color-singlet $1$ and the color-octet $8$ subgroups. Therefore, quarks and antiquarks combine to form color-singlet $[q \bar q]^1$ quark matter and color-octet $[q \bar q]^8$ quark matter. The color-octet quark matter corresponds to the $q\bar q$ quark matter as envisaged in the realm of present knowledge but the color-singlet quark matter is as yet unexplored and now submitted for exploration. The color-singlet quark matter with two flavors can be separated into charged and neutral color-singlet quark matters. In the neutral color-singlet quark matter, the quark and the antiquark interacting only in the QED interaction may form stable and confined colorless QED mesons non-perturbatively at about 17 MeV and 38 MeV (PRC81,064903(2010) and JHEP(2020(8),165). It is proposed that the possible existence of the QED mesons may be a signature of the neutral color-singlet quark matter at $T=0$. The observations of the anomalous soft photons at CERN, and the anomalous bosons with mass about 17 MeV at ATOMKI, DUBNA, and HUS, and mass about 38 MeV at DUBNA hold promising experimental evidence for the existence of such QED mesons, pending further confirmations.
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Astrophysics of Galaxies

How our proto-nuclear star cluster formed and grew due to early globular cluster disruption. I. Case of low masses

D. Kuvatova, M. Ishchenko, P. Berczik et al. (+3 more)

We investigate the accretion of globular cluster stars on early cosmological timescales through detailed N-body simulations of theoretical GC models to assess the role of this mechanism in Milky Way-like galaxies. For the dynamical modelling, we used the updated parallel N-body code phi-GPU, including stellar evolution. We prepared three sets of GC models with different half-mass radii (r_hm), each consisting of 50 full N-body GC models, and integrated these models in an external, time-variable MW-like potential taken from the cosmological database IllustrisTNG-100. The simulations cover the time interval from -10 Gyr to -5 Gyr, enabling us to assess the rate of early stellar accretion onto the proto-NSC. We find that GC models with average orbital eccentricities of 0.4-0.5 and orbits oriented perpendicular to the galactic disc contribute most significantly to the mass of the proto-NSC formation. Accretion is especially efficient in the first billion years and in compact GC models with r_hm = 1 pc. In all sets, the dominant accreted stellar population consists of low-mass stars (~0.33 Msun). However, the accreted mass alone is insufficient to fully account for the current NSC mass. Based on our extended set of numerical simulations, we obtained an average lower limit of mass contribution (~6 percent) to the NSC from investigated GCs. The fraction of mass contribution from individual disrupted GCs can significantly vary from 0.1 percent up to 90 percent. Generally, we conclude that the GC stellar accretion channel alone might not be sufficient to ensure the present-day MW galaxy NSC mass budget.
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All authors D. Kuvatova, M. Ishchenko, P. Berczik, O. Veles, O. Sobodar, T. Panamarev

Solar and Stellar Astrophysics

Statistical Study of Appearance Timing of H$\alpha$ Postflare Loops: Simple Scaling Law Based on Radiative Cooling

Takato Otsu, Ayumi Asai, Kai Ikuta et al. (+1 more)

Recent Sun-as-a-star studies have shown that postflare loops can manifest as a secondary peak in the H$\alpha$ light curve, suggesting that stellar postflare loops are detectable. To understand what determines the timing of such a secondary peak in the H$\alpha$ light curve associated with postflare loops, we must quantitatively identify the key physical processes controlling the appearance of H$\alpha$ postflare loops. Previous case studies have indicated that the appearance timing of H$\alpha$ postflare loops is likely governed by radiative cooling. However, the statistical characteristics of the timing of H$\alpha$ postflare loops appearance remain insufficiently investigated. In this study, we statistically investigated the appearance timing of H$\alpha$ postflare loops to quantify their cooling processes. As a result, we found a negative correlation between the time difference between the soft X-ray peak and the appearance of the H$\alpha$ postflare loops ($\Delta t$) and the soft X-ray peak flux ($F_\mathrm{X}$). This relationship is consistent with the theoretical scaling between radiative cooling timescale ($\tau_{\mathrm{rad}}$) and $F_\mathrm{X}$, where $\tau_{\mathrm{rad}} \propto~F_\mathrm{X}^{-1/2}$. This statistical result indicates that the appearance timing of H$\alpha$ postflare loops relative to the soft X-ray peak is primarily controlled by radiative cooling. Furthermore, we examined the dependence of the scaling law on flare spatial scales ($L$). Consequently, we demonstrated that spatial scale of unresolved stellar flares can be estimated using the following scaling law: $L\propto F_\mathrm{X}^{1/3}\Delta t^{2/3}$. Our results are useful for interpreting secondary peaks in the H$\alpha$ data of stellar flares and provide new method to estimate spatial scale of unresolved stellar flares.
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All authors Takato Otsu, Ayumi Asai, Kai Ikuta, Kazunari Shibata

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

Asymmetric Dark Matter from Low-Scale Spontaneous Leptogenesis

Hiroki Takahashi and Juntaro Wada

We investigate a novel type of asymmetric dark matter (ADM) model in which the dark matter asymmetry and the baryon asymmetry in our universe (BAU) are produced simultaneously via low-scale spontaneous leptogenesis, where the mass scale of right-handed neutrino is much lower than the Davidson-Ibarra bound $M_1 \ll 10^{9}~\rm{GeV}$. In our scenario, both asymmetries are predominantly sourced by a dynamical $CP$ phase, namely the majoron. Its kinetic misalignment provides a sufficiently large, time-dependent effective $CP$ phase, allowing efficient asymmetry production even for low-scale right-handed neutrinos. In our framework, the sources of $CP$ violation responsible for the BAU and ADM are correlated with each other, leading to a predictive relation for the dark matter mass. In particular, when the dark matter asymmetry reaches its equilibrium value before freeze-out, the dark matter mass is typically predicted to lie in the range $\mathcal{O}(0.1)~\mathrm{GeV} \lesssim m_{\chi} \lesssim \mathcal{O}(100)~\mathrm{GeV}$, which lies within the sensitivity of direct detection experiments. On the other hand, if the dark matter asymmetry does not reach its equilibrium value due to weak coupling, the allowed mass range extends over a broader interval, $\mathcal{O}(0.1)~\mathrm{GeV} \lesssim m_{\chi} \lesssim \mathcal{O}(10)~\rm{TeV}$.
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Astrophysics of Galaxies

Extended Ionized Fe Objects in the UWIFE Survey

Kim Yesol, Koo Bon-Chul, Pyo Tae-Soo et al. (+7 more)

We explore systematically the shocked gas in the first Galactic quadrant of the Milky Way using the United Kingdom Infrared Telescope (UKIRT) Wide-field Infrared Survey for Fe+ (UWIFE). The UWIFE survey is the first imaging survey of the Milky Way in the [Fe II] 1.644 um emission line and covers the Galactic plane in the first Galactic quadrant (7 deg < l < 62 deg; |b| < 1.5 deg). We identify 204 extended ionized Fe objects (IFOs) using a combination of a manual and automatic search. Most of the IFOs are detected for the first time in the [Fe II] 1.644 um line. We present a catalog of the measured sizes and fluxes of the IFOs and searched for their counterparts by performing positional cross-matching with known sources. We found that IFOs are associated with supernova remnants (25), young stellar objects (100), H II regions (33), planetary nebulae (17), and luminous blue variables (4). The statistical and morphological properties are discussed for each of these.
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All authors Kim Yesol, Koo Bon-Chul, Pyo Tae-Soo, Froebrich Dirk, Jeong Woong-Seob, Lee Jae-Joon, Lee Yong-Hyun, Lee Ho-Gyu, Kim Hyun-Jeong, Varricatt P. Watson

Earth and Planetary Astrophysics

A new solar radiation pressure model for some orbit types in the cislunar space

Haohan Li, Yuxuan Miao, Xiyun Hou et al. (+4 more)

For satellites in the cislunar space, solar radiation pressure (SRP) is the third largest perturbation, which is only less significant than the lunisolar gravity perturbations. It is the primary factor limiting the accuracy of orbit determination for such satellites. Up to now, numerous SRP models have been proposed for artificial satellites close to the Earth, but these models have their shortcomings when applied to satellites in the cislunar space. In this study, we concentrate on various scenarios of cislunar satellites in periodic or quasi-periodic orbits. We first employ the box-wing model to simulate the SRP effects and then propose an appropriate general SRP model based on these simulations, termed Empirical NJU Cislunar Model (ENCM). Additionally, several scenario-specific sub-models suited to different mission profiles are developed. Furthermore, the proposed model is verified in the orbit determination process. Comparisons with the conventional cannonball and ECOM models demonstrate that the ENCM model yields a significant improvement in orbit determination accuracy, showing promising potential for future cislunar missions.
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All authors Haohan Li, Yuxuan Miao, Xiyun Hou, Jinjun Zheng, Xiangjun Wu, Haihong Wang, Guodong Zhang

Astrophysics of Galaxies

When the Shadow Meets Its Measure: Assessing the Feasibility of Submillimeter Black Hole Shadow Imaging in Megamaser Disk AGN

Roman N. Burridge and Geoffrey C. Bower

Active galactic nuclei (AGN) hosting water megamaser disks provide precise geometric measurements of black hole mass, distance, maser disk orientation, and dynamical center. In anticipation of space-based very long baseline interferometry, these systems offer a path to black hole shadow (BHS) imaging beyond Sgr A* and M87*. We present new Submillimeter Array continuum observations of water megamaser galaxies, supplemented by archival ALMA and VLA measurements, to assess whether their AGN cores are bright enough for BHS-scale imaging. For a 21-source parent sample, we map the predicted BHS diameters of systems with published SMBH masses to submillimeter/millimeter (submm-mm) baseline requirements, estimate AGN core flux densities at 230 GHz while bounding thermal dust and extended-jet contamination and checking whether variability could affect the continuum estimates, and evaluate the astrometric precision required to detect spin-dependent BHS offsets for NGC 4258. NGC 4258 is the only source resolvable on Earth-L2 baselines; other targets require longer baselines approaching Earth-L4/L5 distances, and only a handful have $S_{230} \gtrsim 10$ mJy beam$^{-1}$. We also find a submillimeter excess in NGC 4258, suggesting that its disk remains geometrically thin to $\lesssim 100$ Schwarzschild radii before transitioning to an advection-dominated flow. Even for maximal spin, the formal 230 GHz BHS centroid precision is not the limiting term: the measurement would require locating the 22 GHz water maser dynamical center and registering it to the 230 GHz BHS image roughly seventy times more precisely than current maser astrometry allows, making the spin-offset measurement infeasible with present data.
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Solar and Stellar Astrophysics

Light curve modeling of the nearest neutron star candidate LAMOST J235456.73+335625.9

Qing-bo Han, Mouyuan Sun, Zhi-Xiang Zhang et al. (+1 more)

The discovery of heavy radioactive elements (e.g., $^{60}\mathrm{Fe}$) on Earth suggests that supernova explosions may have occurred near our planet within the past million years, potentially having a significant impact on the ecological environment. This finding has motivated the search for nearby neutron stars in the Solar neighborhood. In a recent study, a candidate for one of the closest neutron stars to Earth, LAMOST J235456.73+335625.9 (hereafter J2354), was reported. Based on dynamical mass measurements under different inclination angle assumptions, the inferred mass range for the unseen compact companion in the system is $1.4$–$1.6$ $M_{\odot}$. Hence, the unseen companion in J2354 is either a massive cold white dwarf or a neutron star. Here we model the flux variations of J2354 as a combination of ellipsoidal modulation and surface spots. We test both cold spot and hot spot models, setting the number of spots to two in each case, and constrain the spot properties through light curve fitting. In the cold spot scenario, the spots are mostly visible at phases $0.5$–$0.75$, whereas in the hot spot scenario, the spots appear predominantly at phases $0.25$–$0.5$. The hot spot model shows better agreement with the observed H$\alpha$ phase variation than the cold spot model. Furthermore, the thermal radiation of a massive but cold white dwarf cannot produce the level of localized heating required to explain the hot spot unless additional heating mechanisms are involved; in contrast, a neutron star can naturally provide such heating through energetic winds. Our results are consistent with the neutron star interpretation of the compact object in J2354.
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All authors Qing-bo Han, Mouyuan Sun, Zhi-Xiang Zhang, Ling-Lin Zheng

Astrophysics of Galaxies

Exploring the interplay between molecular and ionized gas in HII regions

S. Khan, A. M. Jacob, M. R. Rugel et al. (+8 more)

We aim to constrain the kinetic temperature and H$_2$ volume density of massive star-forming clumps associated with HII regions using multiple para-H$_2$CO transitions. In addition, we investigate the interplay between ionized gas, molecular gas, and dust to probe how massive stars influence their parental clumps. We observed the $J_{K_aK_c}$ transitions of para-H2CO (within its J = 3-2 and 4-3 states) with the Atacama Pathfinder EXperiment (APEX) 12 m submillimeter telescope using the nFLASH230 and SEPIA345 receivers towards a sample of 61 HII regions. Spectral line parameters are derived via multi-component Gaussian fitting, which was then used to constrain the physical conditions determined using PyRADEX, a non-local thermodynamic equilibrium (LTE) radiative transfer code in combination with Markov Chain Monte Carlo (MCMC) analysis. The non-LTE analysis yielded kinetic temperatures ($T_{kin}$) ranging from 33.7 K to 265 K and H2 densities (n(H$_2$)) between 0.8 X $10^4$ to 1.05 X $10^7$ cm$^{-3}$, providing a detailed characterization of the dense molecular gas contained in these clumps. In addition to the para-H$_2$CO emission arising from the targeted clump a large fraction (57%) of the sources exhibit multiple para-H$_2$CO components, with the secondary components being characterized by higher $T_{kin}$ and broader linewidths. Investigating the nature of the secondary component revealed its association with supersonic non-thermal motions and turbulent gas. When comparing the physical properties of the molecular gas and dust components with those of the ionizing gas, we find that parameters directly linked to the central high-mass star such as bolometric luminosity and Lyman continuum photon rate, show stronger and more systematic correlations. Emphasizing the role of the central star in governing the interplay between the molecular and ionized gas.(Abridged)
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All authors S. Khan, A. M. Jacob, M. R. Rugel, J. S. Urquhart, S. Neupane, F. Wyrowski, A. Brunthaler, J. D. Pandian, Y. Gong, I. Barlach Christensen, K. M. Menten

Solar and Stellar Astrophysics

Inferring physical parameters of solar filaments from simultaneous longitudinal and transverse oscillations

Upasna Baweja, Vaibhav Pant, Iñigo Arregui et al. (+1 more)

Context. Different modes of oscillations are frequently observed in solar prominences/filaments, and prominence seismology helps estimate important physical parameters like the magnetic field strength. Although the simultaneous detection of longitudinal and transverse oscillations in the same filament is not common, such rare observations provide a unique opportunity to constrain the physical parameters of interest. Aims. In this study, we aim to estimate the physical parameters of prominences undergoing simultaneous longitudinal and transverse oscillations. Methods. We apply Bayesian seismology techniques to observations of longitudinal and transverse filament oscillations to infer the magnetic field strength, the length, and the number of twists in the flux tube holding the prominence plasma. We first use the observations of longitudinal oscillations and the pendulum model to infer the posterior probability density for the magnetic field strength. The obtained marginal posterior of the magnetic field, combined with the observations of the transverse oscillations, is then used to estimate the probable values of the length of the magnetic flux tube that supports the filament material using Bayesian inference. This estimated length is used to compute the number of twists in the flux tube. Results. For the prominences under study, we find that the length of the flux tubes supporting the quiescent prominences can be very large (from 100 to 1000 Mm) and the number of twists in the flux tube are not more than three. Conclusions. Our results demonstrate that Bayesian analysis offers valuable methods to perform parameter inference in the context of prominence seismology.
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All authors Upasna Baweja, Vaibhav Pant, Iñigo Arregui, M. Saleem Khan

Astrophysics of Galaxies

Dynamical properties and star formation history of a low-mass quenched galaxy at Cosmic Noon

K. Ito, F. Valentino, W.M. Baker et al. (+12 more)

We present the spectroscopic confirmation and in-depth analysis of AURORA-LQG1, a low-mass quiescent galaxy at $z_{\rm spec}=2.0834$ with $\log(M_\star/M_\odot)=9.6$ observed with medium-resolution JWST/NIRSpec spectroscopy. The deep medium-resolution spectrum enables the measurement of its stellar velocity dispersion ($\sigma_\star = 95_{-33}^{+38}\,{\rm km\,s^{-1}}$), the smallest value recorded among spectroscopically confirmed quiescent galaxies at $z\sim2$. Coupled with a compact size ($0.41\pm0.03\, {\rm kpc}$), it yields a dynamical mass estimate of $\log(M_{\rm dyn}/M_\odot)=9.75_{-0.38}^{+0.29}$. Its star formation history suggests that half of the stellar mass was in place $\sim1\,{\rm Gyr}$ before the observed epoch, with quenching occurring $\sim0.2\,{\rm Gyr}$ prior to $z=2.08$. These results confirm that AURORA-LQG1 is genuinely quenched, rather than in a temporary phase of suppressed star formation rate. AURORA-LQG1 is consistent with the mass fundamental plane at $z\sim2$, previously constrained only by massive quiescent systems. Compared with more massive counterparts at the same epoch observed with NIRSpec grating spectroscopy, the time since quenching for AURORA-LQG1 is among the shortest observed. The galaxy resides in a possible dense group-scale ($\sim50$ kpc) environment containing one companion with tentative spectroscopic redshift and five companion candidates, and it is embedded in a known protocluster on Mpc scales. A potential environmental influence on its evolution could explain the outside-in quenching suggested by the positive gradient of size with wavelength. This study demonstrates that deep JWST/NIRSpec spectroscopy enables low-mass quiescent galaxies at Cosmic Noon to be characterized with a level of detail long reserved for massive systems, offering valuable new insights into how quenching operates in these underexplored low-mass systems. [Abridged]
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All authors K. Ito, F. Valentino, W.M. Baker, G. Brammer, R. Gottumukkala, T. Kakimoto, C.D.P. Lagos, M. Onodera, A. Pensabene, G. Scarpe, M. Tanaka, K.E. Whitaker, N.A. Reddy, R.L. Sanders, A.E. Shapley

Cosmology and Nongalactic Astrophysics · Cross-listed from gr-qc

Comparison of MOND and Verlinde's emergent gravity in dwarf spheroidals

Youngsub Yoon, Sanghyeon Han and Ho Seong Hwang

We apply Modified Newtonian Dynamics (MOND) and Verlinde's emergent gravity separately to calculate the radial accelerations in 23 dwarf spheroidals. Then, we compare them with the observed radial accelerations. In our earlier work, we determined that, when the data set is considered in its entirety without isolating individual dwarf spheroidal, Verlinde's emergent gravity is in close agreement with the observed values. In the present work, we additionally confirm that, for 21 of the 23 samples examined, Verlinde's emergent gravity follows the trend of the observed values within each dwarf spheroidal more closely than MOND. Combining the statistical significance of all the 23 samples, ranging from $-0.25\sigma$ to 3.41$\sigma$, we conclude that Verlinde's emergent gravity is favored over MOND at 5.2$\sigma$.
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Astrophysics of Galaxies

Accelerated evolution of galaxy host halo masses during Cosmic Dawn from deep JWST clustering

Nicolò Dalmasso, Giovanni Ferrami, Nicha Leethochawalit et al. (+2 more)

We present the deepest clustering analysis of early galaxies to date, analyzing $N_{\rm{g}} \simeq 6500$ photometrically-selected Lyman Break Galaxies from JWST's Advanced Deep Extragalactic Survey (JADES) to reveal how galaxies and dark matter evolved during cosmic dawn ($5 \leq z < 11$). Using halo occupation distribution (HOD) modeling of the two-point angular correlation function, we trace the galaxy-halo relationships across the first billion years of cosmic history. Our analysis reveals that galaxies at $z = 10.6$ reside in dark matter halos over an order of magnitude less massive ($M_{\rm{h}} \sim 10^{10.12} M_{\odot}$) than their counterparts at $z = 5.5$ ($M_{\rm{h}} \sim 10^{11.45} M_{\odot}$), while exhibiting correspondingly higher effective bias values ($b_{\rm{g}}^{\rm{eff}} = 8.13^{+0.04}_{-0.02}$ compared to $5.64^{+0.10}_{-0.13}$). Correspondingly, the satellite galaxy fraction hints at a declining trend with decreasing redshift, reaching $<1\%$ by $z \sim 5-6$. However, the significant systematic and random uncertainties in the data-model comparison prevent us from drawing robust conclusions on the evolution - if any - of the satellite fraction during the epoch of reionization. These results provide the first view of the coevolution between galaxies and dark matter evolved at redshift $\gtrsim 10$, offering additional and independent constraints on early galaxy formation models tuned to reproducing luminosity function evolution.
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All authors Nicolò Dalmasso, Giovanni Ferrami, Nicha Leethochawalit, Emanuele M. Ventura, Michele Trenti

Sunday 4 January

Astrophysics of Galaxies

Exactly solved model of a one dimensional self gravitating system

Rajaram Nityananda

A model one-dimensional self consistent steady state collisionless self-gravitating system in which all the particles have the same energy is presented. This has the remarkable property that the position and velocity of the particles orbiting in their own self consistent potential are given exactly, in terms of time, by the truncations of sine and cosine functions to the first two terms in their respective Taylor series. The potential and density also have simple analytic expressions in terms of time as parameter. It is not being claimed that this system has any direct astronomical application. However, it does motivate a conjecture about the behaviour of the density, potential, and orbits near caustics in simulations of cold collisionless dark matter. It is a rather surprising result which might interest practitioners of stellar dynamics and serve as an elementary example in teaching the subject.
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High Energy Astrophysical Phenomena

Decoding Cygnus X-2: The Critical Role of Reflection in IXPE Data

Honghui Liu, Jiachen Jiang, Adam Ingram et al. (+10 more)

We present a spectro-polarimetric re-analysis of the first IXPE observation of Cygnus X-2 which we determine to be mainly in the normal branch, from quasi-simultaneous observations with NuSTAR, NICER, and INTEGRAL. We measure the hard X-ray polarization angle and find it to be consistent with the previously measured position angle of the radio jet. Leveraging NuSTAR's detection of both the relativistic Fe K emission line and the Compton hump, we constrain the flux contribution of the reflected emission from the inner accretion disk to be 10% of the total X-ray flux in the IXPE energy band. Unlike previous studies that modeled only the Fe K emission line, we fit the full-band reflection spectrum using a fully relativistic disk model. There is strong degeneracy between the Comptonized and reflection components. Given that the Comptonized component is not expected to be highly polarized, a polarization degree of approximately 20% for the reflection component could explain the X-ray polarization data from IXPE. We also discuss the disk inclination angle inferred from our spectro-polarimetric modeling, as well as other possible explanations for the data.
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All authors Honghui Liu, Jiachen Jiang, Adam Ingram, Cosimo Bambi, Andrew C. Fabian, Ruben Farinelli, Renee Ludlam, Nathalie Degenaar, Jakub Podgorny, Andrea Santangelo, James F. Steiner, Andrew J. Young, Zuobin Zhang