Cosmology and Nongalactic Astrophysics · Cross-listed from gr-qc
Herglotz-type $f(R,T)$ gravity
Marek Wazny, Lehel Csillag, Miguel A. S. Pinto et al. (+1 more)
The non-conservation of the energy-momentum tensor in $f(R,T)$
gravity can be interpreted as an effective manifestation of dissipation. Motivated by this, we propose a new formulation of $f(R,T)$
gravity based on the Herglotz variational principle, which extends the usual {Hamilton} variational principle to dissipative systems by allowing the Lagrangian to depend explicitly on the action. The resulting gravitational field equations extend those of $f(R,T)$
gravity by including Herglotz contributions. In the Newtonian limit, these contributions modify the gravitational potential, allowing us to constrain the Herglotz vector through Mercury's perihelion precession and the relativistic light deflection. The Herglotz corrections lead to a scaling law consistent with observations from the Cassini spacecraft. Examining two representative cosmological models, the Herglotz vector effectively reduces to a single function that, under suitable conditions, can play the role of a cosmological constant, providing an alternative mechanism for the Universe's accelerated expansion. Within the Herglotz variational approach, the linear $f(R,T)=R+\alpha T$ model, previously ruled out in the standard formulation due to its fixed deceleration parameter, becomes consistent with observations {for a certain choice of the Herglotz vector.
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All authors Marek Wazny, Lehel Csillag, Miguel A. S. Pinto, Tiberiu Harko
Cosmology and Nongalactic Astrophysics
Absorption effects in the expanding Universe: spectral transmittance functions of the intergalactic medium for distant sources
Anguohao Yang, Bohdan Novosyadlyj, Bohdan Melekh et al. (+1 more)
We construct two self-consistent analytic approximations to the neutral hydrogen fraction, $x_{\rm HI}(z)$, and the helium ionization fractions, $x_{\rm HeI}(z)$, $x_{\rm HeII}(z)$, and $x_{\rm HeIII}(z)$, that are consistent with current constraints inferred from
quasar spectra,
galaxy surveys, and CMB polarization measurements. These approximations describe observationally motivated early- and late-reionization scenarios. Using these histories, we analyse the formation of broad absorption troughs in the continuum spectra of high-
redshift sources over $1\leq z_{\rm s}\leq15$. We assume that neutral hydrogen and helium in a homogeneous diffuse intergalactic medium reside predominantly in their ground states and absorb radiation through the Lyman-series lines and continua of HI, HeI, and HeII. We compute the wavelength-dependent optical depths for the first 39 Lyman-series lines of HI and HeII, the first 10 lines of HeI, and the corresponding continua, and use them to derive spectral transmittance functions, $T(\lambda;z_{\rm s})$. As illustrative applications, we apply them to toy-model continuum spectra of starless
haloes and to model spectra of a low-
metallicity dwarf galaxy at different
redshifts. Spectral features in sources at $5\lesssim z_{\rm s}\lesssim7$ caused by intergalactic absorption are found to be particularly sensitive to the adopted hydrogen and helium ionization histories
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All authors Anguohao Yang, Bohdan Novosyadlyj, Bohdan Melekh, Gennadii Milinevsky
Instrumentation and Methods for Astrophysics · Cross-listed from hep-ex
Development and Testing of a Modular Large-Area Cosmic Ray Telescope Using Scintillator-Fiber Hybrid Design for Millimeter-Level Muon Tracking
Yan Niu, Anqing Wang, Xiangxiang Ren et al. (+2 more)
Cosmic-ray
muons, owing to their high penetration power and abundance, have been widely employed as a natural probe in experimental particle physics. We developed a meter-scale
cosmic-ray
muon telescope, consisting of two parallel super-layers (1 m $\times$ 1 m) separated vertically by one meter. A super-layer is composed of two orthogonal detection layers, of which each consists of eighteen modules arranged in parallel and packed closely together. A module consists of a plastic scintillating bar precisely aligned and stacked on top of an underlying scintillating fiber mat in which fibers are arranged in a row of bundles. For a detection layer, each scintillator bar is coupled to a PMT while fiber bundles at the same position within all modules are coupled to a single PMT. Signals from scintillating bars and fibers are combined together to determine hit positions. With this detection scheme, the
telescope can meet the requirement of spatial resolution and reduce the number of readout electronic channels. This article presents the comprehensive development of the
telescope, encompassing its
geometric design, data acquisition system, and performance evaluation. Experimental results show that the
telescope achieves a position resolution better than 2 mm and an overall detection efficiency of $\sim$85%. The innovative design keeps the manufacturing cost low while maintaining high spatial resolution and detection efficiency.
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All authors Yan Niu, Anqing Wang, Xiangxiang Ren, Dong Liu, Meng Wang
Instrumentation and Methods for Astrophysics
Accelerating reionization constraints: An ANN-emulator framework for the SCRIPT Semi-numerical Model
Saptarshi Sarkar and Tirthankar Roy Choudhury
Constraining the Epoch of Reionization (EoR) with physically motivated simulations is hampered by the high cost of conventional parameter inference. We present an efficient emulator-based framework that dramatically reduces this bottleneck for the
photon-conserving semi-numerical code SCRIPT. Our approach combines (i) a reliable coarse-resolution MCMC to locate the high-likelihood region (exploiting the large-scale convergence of SCRIPT) with (ii) an adaptive, targeted sampling strategy to build a compact high-resolution training set for an artificial neural network based emulator of the model likelihood. With only $\approx 10^3$ high-resolution simulations, the trained emulators achieve excellent predictive accuracy ($R^2 \approx 0.97-0.99$) and, when embedded within an MCMC framework, reproduce posterior distributions from full high-resolution runs. Compared to conventional MCMC, our pipeline reduces the number of expensive simulations by a factor of $\sim 100$ and lowers total CPU cost by up to a factor of $\sim 70$, while retaining statistical fidelity. This computational speedup makes inference in much higher-dimensional models tractable (e.g., those needed to incorporate JWST and upcoming 21 cm
datasets) and provides a general strategy for building efficient emulators for next generation of EoR constraints.
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Cosmology and Nongalactic Astrophysics · Cross-listed from gr-qc
Temperature definitions and phase transitions within non-minimal large and small inflationary potentials
Jesus Anaya-Galeana, Orlando Luongo and Hernando Quevedo
We explore and compare two distinct temperature definitions for scalar field inflation in the context of small- and large-field potentials. The first is based on a real gas, fluid-like temperature, $T_{RG}$, while the second corresponds to a relativistic species-like temperature, $T_{RS}$. We derive the fundamental thermodynamic relations for both and analyze their implications for the most viable inflationary potentials, consistent with Planck constraints. We also investigate non-minimally coupled scenarios, finding that $T_{RS}$ is the most self-consistent choice, as it decreases during inflation, satisfies standard thermodynamic laws, and exhibits frame-independent behavior in both the Jordan and Einstein frames. Remarkably, the $T_{RS}$ approach shows that the inflaton's dynamics is well-described by Van der Waals-like isotherms, linking inflationary
evolution to thermodynamic phase transitions. We find that the onset of inflation is associated with a phase transition acting as the “trigger” of the inflationary epoch. Our analysis highlights inconsistencies in the hilltop potential and, more generally, in small-field potentials unless a non-minimal coupling is introduced. Conversely, the Starobinsky and $\alpha$-attractor models emerge as the most suitable paradigms. We further show that frame independence is achieved only for coupling values $\zeta \leq 1/6$, supporting very small values. Finally, our study of natural inflation with non-minimal coupling reveals a strong dependence on the coupling parameter, where bounds associated with thermodynamic phase transitions coincide with observationally viable ranges, suggesting that thermodynamic considerations may provide an additional criterion to discriminate among inflationary scenarios.
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Earth and Planetary Astrophysics
Dynamical simulation of the Interstellar Comet 3I/ATLAS
Goldy Ahuja and Shashikiran Ganesh
Comet 3I/ATLAS, also known as C/2025 N1, was discovered on 2025 July 1 UT by NASA Asteroid Terrestrial-impact Last Alert System (ATLAS), with a v$_{\infty}$ $\sim$ 58 kms$^{-1}$. This is the fastest among the three interstellar objects discovered so far. In this work, we study the interaction of the 3I/ATLAS with Mars, pre-perihelion, and Jupiter post-perihelion. We also present the results of the dynamical simulations of the orbital
evolution of the comet for a hundred years in the past and future. For our analysis, we have used REBOUND, an N-Body simulation package, to study these situations. We use the adaptive size mathematical integrator Ias15, with a 1-day time step for long-term integration, and a 1-hour time step to study the effect of the
planets on this body during the close encounters. We have seen an effect of Jupiter on the orbital parameters of the comet, which affects its post-perijove trajectory significantly. The impact of Mars on this comet is minimal compared to the effect of Jupiter. This is consistent with the point that the comet moves well past Mars's Hill radius but very close to Jupiter's Hill radius at the respective close approaches. However, the effect of non-gravitational forces will alter the results. Since the non-gravitational forces are not yet known, we predict the variation of the orbital parameters considering a range of possible magnitudes of the non-gravitational acceleration.
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High Energy Astrophysical Phenomena
Constraining the Corona Geometry of Cyg X-1 with Broad Band Spectrum and Polarimetric Analysis Based on Observations in May 2022
Sixuan Zhang, Tsunefumi Mizuno, Tomohisa Kawashima et al. (+6 more)
Cygnus X-1 (Cyg X-1) exhibited a low hard state in 2022, observed by several missions. The IXPE reported that the polarization angle is aligned with the
radio jet and gave a polarization degree approximately 4 times higher than the general expectations of $1\%$ through the analysis of the time-integrated data with a simple spectral model, indicating that the disk inclination is higher than a canonical value of about $30^{\circ}$. Many subsequent theoretical studies employed a non-standard model to explain this high PD. Here, we revisit the disk/corona spectrum through a detailed joint analysis using IXPE, NuSTAR, and NICER data. By investigating the time variability of the spectrum, we find that the two-Comptonization components model can better reproduce the data than the one-Comptonization component model originally adopted. We observed a lower disk
photon temperature of about 0.15 keV. Detailed simulation suggests that lowering the disk temperature by a factor of 2 increases the PD by roughly 2 percentage points in the IXPE 2–8 keV band for a slab-like corona geometry, helping to reconcile the observed high PD with theoretical predictions. However, The simulated PDs are still significantly lower than the observed ones - even for a rather high $60^{\circ}$ inclination. We also investigated the polarization properties of a simple wedge-shaped corona with a truncated disk and a sandwiching slab corona. We find that the slab corona predicts an apparent energy dependence in PD while PA remains constant in the IXPE band, in agreement with the observed polarization. Therefore, we suggest that Cyg X-1 in 2022 May exhibits a two-Comptonization coronal emission with different optical depths, and the hard one is in a sandwiching slab geometry. We also discuss how the polarization is affected by other parameters of the black hole and the corona.
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All authors Sixuan Zhang, Tsunefumi Mizuno, Tomohisa Kawashima, Chris Done, Yasushi Fukazawa, Hiromitsu Takahashi, Ryusei Komine, Koudai Takebayashi, Ken Ohsuga
Cosmology and Nongalactic Astrophysics
Constraining interacting dark energy models with black hole superradiance
Zhen-Hong Lyu, Rong-Gen Cai, Shao-Jiang Wang et al. (+1 more)
The recent preference for a dynamical dark energy (DE) from the Dark Energy Spectroscopic Instrument seems to call for interactions between DE and dark matter (DM), either from direct DE-DM interaction or indirect interaction induced by modified
gravity. Therefore, an independent probe for these kinds of DE-DM interactions would be appealing from observational aspects. In this paper, we propose the black hole superradiance as a novel astrophysical probe for field-theoretic interacting DE-DM models, providing complementary constraints independent of large-scale cosmological observations. The core principle is that the DE-DM interaction can alter the effective mass of the superradiant ultralight
boson, thereby modifying its superradiant instability rate around spinning black holes. We explore this connection through two distinct scenarios: a model where the DE field mediates a dark fifth force within the DM sector, affecting the superradiance from DM particles; and a novel mechanism where the DE field itself becomes superradiant due to the effective mass enhancement induced by dense DM spikes around supermassive black holes. By applying a statistical framework to black hole observations in both scenarios, we derive constraints on the fundamental DE-DM coupling strength. Although the current constraints are rather loose due to small samples and inaccurate measurements, our work provides new astrophysical constraints on these interacting DE-DM scenarios and establishes a new synergy between black hole physics and cosmology for probing the fundamental nature of the dark sector.
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All authors Zhen-Hong Lyu, Rong-Gen Cai, Shao-Jiang Wang, Xiang-Xi Zeng
Earth and Planetary Astrophysics
Asteroid phase curve modeling with empirical correction for shape and viewing geometry
Dagmara Oszkiewicz. Przemysław Bartczak, Milagros Colazo and Antti Penttilä
We present a novel empirical method for correcting asteroid phase curves for rotational and geometrical effects using precomputed
spin-and-shape models. Our approach normalizes sparse photometric data to a pole-on geometry, enabling consistent phase-curve fitting across apparitions. We fit both the H,G1,G2 and H,G12 phase functions to the normalized data. We also numerically derive new constraints on parameter ranges that ensure physically meaningful solutions. These constraints are based on the requirement that the reduced magnitude must monotonically decrease with phase angle and remain within plausible slope bounds. Compared to earlier bounds, our new constraints are more permissive. We also compare derivative-based and derivative-free optimization methods, highlighting convergence issues with the HG12 function and offering mitigation strategies. We applied our method to over 25,000 asteroids observed by the ATLAS survey, demonstrating its usability. The new method enables the selection of the preferred
spin-and-shape solution based on either statistical phase-curve model selection criteria and/or physically motivated constraints on the phase-curve shape.
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Astrophysics of Galaxies
Hidden metallic iron in amorphous silicate dust? Insights from condensation experiments and mid-infrared spectroscopy
Hanako Enomoto, Aki Takigawa, Hiroki Chihara et al. (+1 more)
Amorphous silicate
dust is a major component in the interstellar and circumstellar
dust formed in the
outflow of asymptotic
giant branch (AGB)
stars. Although iron depletion is observed in the interstellar medium (ISM), the exact form and fraction of iron in solid remains under debate. In particular, it is unclear whether amorphous silicate
dust around AGB
stars contains metallic iron. We aimed to provide optical constants of amorphous silicate nanoparticles and examine the effects of metallic iron on their spectral features to better constrain the
dust properties by producing amorphous silicate nanoparticles with and without metallic cores. We performed condensation experiments using an induction thermal
plasma system to produce
dust analogues of the CI chondritic composition in the Mg-Ca-Na-Al-Si-Fe-Ni-O and Mg-Ca-Na-Al-Si-O systems. We measured the absorbance and reflectance of the samples, observed the structure of the products, and determined the optical constants. Two types of amorphous silicate nanoparticles (10-200 nm in diameter) with nearly CI chondritic composition were produced: one contained kamacite (Fe: Ni=0.9: 0.1) cores with a diameter ratio ranging 0-0.87 (average ~0.50), and the other was iron-free homogeneous amorphous silicate. The amorphous silicates of the CI chondritic composition with various sized metallic cores may be prevalent in circumstellar and interstellar
dust.
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All authors Hanako Enomoto, Aki Takigawa, Hiroki Chihara, Chiyoe Koike
Instrumentation and Methods for Astrophysics
The Fluorescence Camera for the PBR mission
Francesco Saverio Cafagna
The Probe Of Extreme Multi-Messenger Astrophysics (POEMMA) Balloon with
Radio (PBR) is an instrument designed to be borne by a NASA suborbital Super Pressure Balloon (SPB), in a mission planned to last as long as 50 days. The PBR instrument consists of a 1.1 m aperture Schmidt
telescope, similar to the POEMMA design, with two cameras in its hybrid focal surface: a Fluorescence Camera (FC) and a Cherenkov Camera (CC), both mounted on a frame that can be tilted to point from nadir up to 13 degrees above the horizon. The FC camera is designed to detect the fluorescence emission of Extensive Air Showers produced by Ultra-High Energy
Cosmic Rays from sub-orbital altitudes. This measurement will validate the detection strategy for future space-based missions, such as POEMMA. The FC will be made of 4 Photo Detection Modules (PDMs), each consisting of a 6x6
matrix of 64-channel Multi Anode PhotoMulTipliers (MAPMT), for a grand total of 2304 pixels for each PDM. Custom-designed SPACIROC-3 ASICs perform single photoelectron counting on each pixel as well as charge integration on groups of 8 pixels to measure extremely bright or fast signals, reaching a double pulse resolution in the order of 10 ns for a 1 microsecond acquisition gate. A field flattener lens and a BG3 filter, to match the wavelength range of interest (300-400 nm), are mounted in front of the PDM. The camera will be able to detect showers in a field of view of 24x24 square degrees, with a pixel size on ground corresponding to 115 m. Details on the camera design and implementation will be given, along with the expected performance and the state of the construction.
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High Energy Astrophysical Phenomena
A pilot VLBI study of the SQUAB quasar sample featuring multiple Gaia detections
Yingkang Zhang, Tao An, Xiang Ji et al. (+5 more)
Our previous work identified a class of SDSS
quasars exhibiting multiple
Gaia detections, classifying them as candidates for various astrophysical systems such as
quasar-
star pairs, dual
quasars, and gravitationally lensed
quasars. In this paper, we present a pilot VLBI study targeting a
radio-bright subsample and report the first high-resolution imaging results. By leveraging the milliarcsecond-scale resolution of VLBI and its precise astrometric coordination incorporating with
Gaia, we aim to refine the classification of these multiple matched sources, search for potential dual AGNs, and assess the efficacy of the combined
Gaia-VLBI approach in resolving ambiguous
quasar systems. We cross-matched the SQUAB
quasar sample with the FIRST and NVSS catalogs, identifying 18
radio-emitting sources. The three brightest were selected for dual-frequency (1.6 and 4.9 GHz) VLBA observations. We performed VLBI imaging at both
Gaia positions, constructed spectral index maps, and estimated brightness temperatures to characterize the
radio morphology and physical properties. For the three target sources, our VLBI observations reveal compact
radio structures consistent with single AGN at the primary
Gaia positions. No significant emission is detected at the secondary
Gaia locations. These results support the interpretation of the sources as
quasar$-$
star pairs, in line with earlier studies. This pilot study demonstrates the value of
radio-VLBI high-resolution follow-ups on
Gaia-selected
quasar systems with multiple counterparts, showing how they can unambiguously reveal the true nature of these systems and help remove contaminants from dual AGN candidate samples.
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All authors Yingkang Zhang, Tao An, Xiang Ji, Zhenya Zheng, Yuanqi Liu, Qiqi Wu, Ruqiu Lin, Shilong Liao
Astrophysics of Galaxies
Two Epochs of VLBI Observations of 8 KISSR Seyfert & LINER Galaxies: Suggestions of Fast and Filamentary Outflows
Preeti Kharb, Anderson Caproni, Salmoli Ghosh et al. (+4 more)
We present here the results from a second epoch of phase-referenced VLBA observations of 8 Seyfert and LINER
galaxies from the KISSR sample. These sources were chosen based on the presence of double peaks or asymmetries in their emission lines as observed in SDSS spectra. Parsec-scale
radio emission is detected in 7 of the 8 sources in the second epoch. Jet-like features appear to persist over a $\sim4-9$ year timeline in these `
radio-quiet' AGN. A few sources like KISSR1494, however, show significantly different structures after a 9 year interval. KISSR102, which was previously suggested to be a binary black hole candidate based on the presence of two compact cores, shows the tentative signatures of superluminal jet motion ($1.05\pm0.45$c). Tentative superluminal motion in a jet
knot has been reported in another source, KISSR872 ($1.65\pm0.57$c). We present 1.5 GHz images from the VLA A-array of 4 sources. These images reveal core-lobe or core-
halo structures. The
alignment of the VLBI jet direction with the kpc-scale spectral index gradient, as well as the mismatch between the
star formation rate derived from the
radio and H$\alpha$ line emission, support the suggestion that the kpc-scale emission is AGN-jet-related. The jets in KISSR sources appear to lose collimation over spatial scales between 200 parsec and 1 kpc. Overall, the characteristics of the KISSR jets are reminiscent of similar properties observed in VLBI monitoring studies of `
radio-loud' AGN jets even as subtle differences related to the compactness and brightness of jet features remain.
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All authors Preeti Kharb, Anderson Caproni, Salmoli Ghosh, Daniel A. Schwartz, Mousumi Das, Smitha Subramanian, Sravani Vaddi
Astrophysics of Galaxies
MAMMOTH-Grism: Revisiting the Mass-Metallicity Relation in Protocluster Environments at Cosmic Noon
Yiming Yang, Xin Wang, Xianlong He et al. (+12 more)
We present one of the first measurements of the mass-
metallicity relation (MZR) in multiple massive protoclusters at
cosmic noon, using Hubble Space
Telescope (HST) G141 slitless spectroscopy from the MAMMOTH-Grism survey. We identify 63 protocluster member
galaxies across three overdense structures at $z = 2\text{-}3$ with robust detections of [OIII], H$\beta$, and [OII] emission. The sample spans gas-phase
metallicities of $12 + \log(\text{O/H}) = 8.2\text{-}8.6$,
dust-corrected H$\beta$-based
star formation rates (SFRs) of $10$-$250\,M_\odot\,\text{yr}^{-1}$, and
stellar masses of $M_\ast \sim 10^{9.4}$-$10^{10.5}\,M_\odot$, derived via spectral energy distribution fitting using deep HST and ground-based photometry. We stack spectra in five $M_\ast$ bins to obtain average
metallicities and SFRs. Relative to field
galaxies at similar
redshifts, protocluster members show elevated SFRs at $M_\ast < 10^{10.25}\,M_\odot$ and a systematically shallower MZR: $12 + \log(\text{O/H}) = (6.96 \pm 0.13) + (0.143 \pm 0.017) \times \log(M_{\ast}/M_{\odot})$. We detect a mass-dependent environmental offset: massive protocluster
galaxies are metal-poor compared to field counterparts of similar mass, whereas lower-mass systems exhibit comparable or mildly enhanced
metallicities. This trend is consistent with a scenario where cold-mode
accretion dilutes the interstellar medium (ISM) across the full mass range, while efficient recycling of feedback-driven
outflows preferentially enriches the ISM in low-mass
galaxies. Finally, we assess the dependence of
metallicity offsets on local overdensity and find no significant trend, likely reflecting the survey's bias toward protocluster cores.
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All authors Yiming Yang, Xin Wang, Xianlong He, Chao-Wei Tsai, Zheng Cai, Zihao Li, Matthew A. Malkan, Dong Dong Shi, Anahita Alavi, Fuyan Bian, James Colbert, Xiaohui Fan, Alaina L. Henry, Harry I. Teplitz, Xian Zhong Zheng
Earth and Planetary Astrophysics
Coupled atmospHere Interior modeL Intercomparison (CHILI) Protocol Version 1.0: A CUISINES Intercomparison Project of Magma Ocean Models
Tim Lichtenberg, Laura Schaefer, Joshua Krissansen-Totton et al. (+23 more)
Spectroscopic characterization of rocky
exoplanets with the James Webb Space
Telescope has brought the origin and
evolution of their atmospheres into the focus of
exoplanet science. Time-evolved models of the feedback between interior and atmosphere are critical to predict and interpret these observations and link them to the
Solar System terrestrial
planets. However, models differ in methodologies and input data, which can lead to significant differences in interpretation. In this paper, we present the experimental protocol of the Coupled atmospHere Interior modeL Intercomparison (CHILI) project. CHILI is an (exo-)
planet model intercomparison project within the Climates Using Interactive Suites of Intercomparisons Nested for
Exoplanet Studies (CUISINES) framework, which aims to support a diverse set of multi-model intercomparison projects in the
exoplanet community. The present protocol includes the initial set of participating magma ocean models, divided into evolutionary and static models, and two types of test categories, one focused on
Solar System
planets (Earth & Venus) and the other on
exoplanets orbiting low-mass M-
dwarfs. Both test categories aim to quantify the
evolution of key markers of the links between planetary atmospheres and interiors over geological timescales. The proposed tests would allow us to quantify and compare the differences between coupled atmosphere-interior models used by the
exoplanet and planetary science communities. Results from the proposed tests will be published in dedicated follow-up papers. To encourage the community to join this comparison effort and as an example, we present initial test results for the early Earth and TRAPPIST-1 b, conducted with models differing in the treatment of energy transport in the planetary interior and atmosphere, surface boundary layer, geochemistry, and the in- and outgassing of volatile compounds.
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All authors Tim Lichtenberg, Laura Schaefer, Joshua Krissansen-Totton, Yamila Miguel, Denis E. Sergeev, Philipp Baumeister, Jessica Cmiel, Leoni J. Janssen, T. Giang Nguyen, Yoshinori Miyazaki, Harrison Nicholls, Alexandra Papesh, Hugo Pelissard, Bo Peng, Junellie Perez, Emma Postolec, Mariana Sastre, Arnaud Salvador, Hanno Spreeuw, Andrea Zorzi, Thomas J. Fauchez, Keiko Hamano, Jérémy Leconte, Maxime Maurice, Lena Noack, Laurent Soucasse
Cosmology and Nongalactic Astrophysics
Creation of Viscous Dark Energy by the Hubble Flow: Comparison with SNe Ia Master Sample Binned Data
Iolanda Navone, Maria Giovanna Dainotti, Elisa Fazzari et al. (+3 more)
We study a family of cosmological models featuring dynamical dark energy (DE), based on the idea that the creation of its constituents arises from the gravitational field of the expanding universe, whose non-
equilibrium physics is described by a non-zero bulk viscosity coefficient. We consider the complete scenario, in which both matter creation and bulk viscosity are present, together with its two limiting cases, in which only one of the two effects is retained. Once each model is constrained by requiring its present-day deceleration parameter $q_0$ to match specific values, the complete scenario introduces up to two additional free parameters with respect to the $\Lambda$CDM model, one of which is the equation of state parameter $w$ of the created dark energy. We consider two choices for $q_0$: the value predicted by the $\Lambda$CDM model, and one obtained from a background analysis of Fazzari et al., JHEAp 49 (2026). To perform the analysis, we construct the effective running Hubble constant, i.e. a theoretical function corresponding to the ratio between the Hubble parameter of our models and the $\Lambda$CDM expansion rate. The theoretical predictions for the effective running Hubble constant of the three models are tested against the Master binned sample of Type Ia
Supernovae (SNe Ia), through a Markov Chain Monte Carlo procedure with up to four free parameters. The most important result emerging from this analysis is that, when using the cosmographic $q_0$, all three models exhibit a quintessence-to-phantom transition in the effective equation of state parameter of the dark energy; on the contrary, when using the $q_0$ coming from the $\Lambda$CDM limit, the transition cannot happen, and the effective equation of state parameter is entirely of phantom nature across the considered
redshift range.
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All authors Iolanda Navone, Maria Giovanna Dainotti, Elisa Fazzari, Giovanni Montani, Naoto Maki, Kazunori Kohri
Astrophysics of Galaxies
Chemical evolution of bulges of active galactic nuclei in the early Universe: roles of accreting stars
Shuo Zhai, Jian-Min Wang, Yan-Rong Li et al. (+2 more)
JWST/NIRCam observations reveal dense
stellar cores in high-
redshift galactic bulges, indicative of sustained
star formation and potential
stellar accretion. We introduce
accretion-modified
star (AMS) as a new component in the chemical
evolution of high-
redshift bulges hosting active
galactic nuclei (AGNs). The gas-phase chemical
evolution of bulge environments containing AMS is modeled within 1 Gyr by combining population
evolution and
galactic chemical
evolution formalisms, and observational signatures are tracked via photoionization modeling on Baldwin-Phillips-Terlevich (BPT) diagrams. Sustained high
accretion onto AMSs leads to rapid gas-phase metal enrichment of the bulge, producing abundance peaks up to five times
solar metallicity within 0.1 Gyr and significantly modifying elemental ratios in the gas phase. Atypical gas-phase abundance patterns during early, high-
accretion phases and gradually diminish as the
accretion rate declines. In BPT diagrams, high-AMS-
accretion scenarios shift the modeled emission-line sequence toward the local AGN branch and extend into the high-
metallicity regime. Super-
solar narrow-line regions observed in AGNs at z>15 may reflect such AMS-driven gas-phase enrichment of host bulge under extreme gas densities. While direct detection of AMSs within AGN bulges remains challenging, the model provides testable predictions for future spectroscopic surveys and motivates further exploration of non-canonical
stellar populations in AGN host bulges.
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All authors Shuo Zhai, Jian-Min Wang, Yan-Rong Li, Wei-Jian Guo, Gang Zhao
Solar and Stellar Astrophysics
Type II Cepheids: Period-Luminosity-Metallicity relations for the Population II distance scale
Susmita Das, Anupam Bhardwaj and Marcella Marconi
Type II Cepheids are a class of pulsating variable
stars that play a critical role in our understanding of
stellar evolution, distance measurement and tracing the structure and kinematics of old
stars in nearby
galaxies. This review provides a comprehensive summary of the current state of research on Type II Cepheids, including their observed properties, pulsation mechanisms and their distinction from other variable
stars. These pulsating variable
stars, found primarily in older
stellar populations, exhibit well-defined period-luminosity relations but with an added advantage that they exhibit weak or negligible dependence on
metallicity. We explore their relevance in the context of their role as distance indicators and potential calibrators of the first rung of the extragalactic distance ladder. Finally, the review highlights recent advancements in theoretical models, observations across different wavelengths and ongoing debates concerning their classification.
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Cosmology and Nongalactic Astrophysics
Forecasting the Constraint on the Hu-Sawicki $f(R)$ Modified Gravity in the CSST $3\times2$pt Photometric Survey
Jun-Hui Yan, Yan Gong, Qi Xiong et al. (+5 more)
We forecast the constraint on the Hu-Sawicki $f(R)$ model from the photometric survey operated by the Chinese Space Station Survey
Telescope (CSST). The simulated $3\times2$pt data of
galaxy clustering, weak
lensing, and
galaxy-
galaxy lensing measurements within 100 deg$^{2}$ are used in the analysis. The mock observational maps are constructed from a light cone,
redshift sampling and noise. The angular power spectra are measured with pseudo-$C_\ell$
estimators and compared to theory in the same basis using validated weighting functions and an analytic covariance
matrix that includes Gaussian, connected non-Gaussian, and super-sample terms. We model the theoretical spectra using two methods. The first one uses MGCAMB to compute the linear modified-
gravity clustering power spectra, and the second one adopts the FREmu emulator with a baseline of nonlinear $\Lambda$CDM prescription. Parameter inference is performed with Cobaya, and the cosmological and modified-
gravity parameters are sampled within the emulator training domain, which is jointly fitted with the systematic parameters. We find that the predictions from the two methods are in good agreement at the overlapping large scales, and the emulator method can correctly provide additional high-$\ell$ information. The $1\sigma$ upper bounds of $\log_{10}|f_{R0}|$ are found to be $<-5.42$ for
cosmic shear only case and $<-5.29$ for the 100 deg$^2$ CSST $3\times2$pt probe. The full CSST photometric survey with 17,500 deg$^2$ survey area is expected to further improve the constraint precision by about one order of magnitude. Our results demonstrate that the CSST $3\times2$pt survey can deliver strict tests on $f(R)$
gravity.
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All authors Jun-Hui Yan, Yan Gong, Qi Xiong, Xuelei Chen, Qi Guo, Ming Li, Yun Liu, Wenxiang Pei
Astrophysics of Galaxies
Too Quiet for Comfort: Local Little Red Dots Lack Variability over Decades
Colin J. Burke, Zachary Stone, Yue Shen et al. (+1 more)
Several local ($z\lesssim 0.2$) metal-poor
dwarf AGNs have remarkably similar properties to those of high-
redshift Little Red Dots (LRDs), and are recently proposed to be local analogs of LRDs. We use long-term photometric and spectroscopic observations of three local LRDs spanning $\sim 20$ years to measure variability in their rest-frame optical continuum and broad H$\alpha$ emission lines. Using ZTF light curves over a rest-frame $\sim 5$ yr baseline, the $r$-band intrinsic rms variability is $(9\times 10^{-5})_{\rm -9E-5}^{+0.014}$ mag (J1022), $0.025\pm0.004$ mag (J1025) and $0.020\pm0.005$ mag (J1047), indicating low intrinsic variability ($<3-4\%$ at 3$\sigma$). These rms variability amplitudes are much lower than those for
dwarf AGNs and more massive
quasars. There is little structure in the optical variability structure functions for the three local LRDs, in contrast to normal AGN variability. Using available multi-epoch spectra, we constrain the broad H$\alpha$ line flux variability to be less than a few percent, without significant profile changes, over a rest-frame baseline of $\sim 15$ yrs in J1025 and J1047, respectively. The three LRDs stand out in the Balmer line properties compared with normal broad-line AGNs, with exceptionally large H$\alpha$ equivalent widths and H$\alpha$/H$\beta$ ratios far exceeding the Case B recombination value. In the context of recent theoretical models of LRDs as dense gas-enshrouded massive black holes with super-Eddington
accretion, our results suggest that the photosphere emission is long-term stable and the broad Balmer lines are primarily collisonally excited. This scenario is consistent with the lack of variability, large H$\alpha$/H$\beta$ ratios and little
dust extinction, as well as the expected high gas density. Virial black hole mass estimates using broad H$\alpha$ assuming photoionization are therefore highly questionable for LRDs.
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All authors Colin J. Burke, Zachary Stone, Yue Shen, Yan-Fei Jiang
Astrophysics of Galaxies
Large gas inflow driven by a matured galactic bar in the early Universe
Shuo Huang, Ryohei Kawabe, Hideki Umehata et al. (+3 more)
Bar structures are present in about half of local disk
galaxies and play pivotal roles in secular
galaxy evolution. Bars impose a non-axisymmetric perturbation to the rotating disk and transport gas inward to feed central starburst and, possibly, the activity of the
nuclear supermassive black hole. They are believed to be long-lived structures and are now identified at
redshift $z>2$. Yet, little is known about the onset and effect of bars in the early
cosmic epoch because spectroscopy of distant bars at sufficient resolution is prohibitively expensive. Here, we report a kinematic study of a
galactic bar at
redshift 2.467, 2.6 billion years after the Big Bang. We observe the carbon monoxide and atomic carbon emission lines of the dusty
star-forming
galaxy J0107a and find the bar of J0107a has gas distribution and motion in a pattern identical to local bars. At the same time, the bar drives large-scale non-circular motions that dominate over disk rotation, funneling molecular gas into its center at a rate of $\approx600$
solar masses per year. Our results show that bar-driven dynamical processes and secular
evolution were already at play 11.1 billion years ago, powering active
star formation amid the gas-rich and far-infrared luminous growth phase in a massive disk
galaxy.
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All authors Shuo Huang, Ryohei Kawabe, Hideki Umehata, Kotaro Kohno, Yoichi Tamura, Toshiki Saito
Instrumentation and Methods for Astrophysics
Optimization design and analysis for the mechanical test platform of scientific probe module of the Cool Planet Imaging Coronagraph
Lingyi Kong, Jiangpei Dou, Wei Guo et al. (+3 more)
This paper optimizes the design and analysis of the mechanical test platform for the scientific probe module of the Cool
Planet Imaging Coronagraph, which is the fifth part of the China Space Station survey
Telescope. First, according to the module layout and economic requirements, the preliminary structural design of the module mechanical test platform is carried out, and the stiffness sensitive parameters of the assembly are identified to determine the optimization parameters. The Central Composite Design method is used to design the test platform, and a third-order regression model is constructed for response surface analysis. The third-order response surface model of the fundamental frequency and amplitude of the test platform is obtained by fitting the test data with the least squares method, and the structure of the module mechanical test platform is determined. The modal analysis is carried out to determine the fundamental frequency and vibration modes of the mechanical test platform. The vibration response of the platform is simulated by sine, random and swept frequency vibration simulations. The response surface fitting
algorithm is verified by the test platform swept frequency test. The agreement between the response surface fitting
algorithm and the experiment is good. The fundamental frequency of the test platform is 436.2Hz (>300Hz), which meets the design index requirements of the test platform and can accurately guide the optimization design work. At the same time, it provides the theoretical basis and design method for the structural design of the Chinese manned space station.
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All authors Lingyi Kong, Jiangpei Dou, Wei Guo, Mingming Xu, Shu Jiang, Bo Chen
Instrumentation and Methods for Astrophysics · Cross-listed from cs.NE
Neuromorphic Astronomy: An End-to-End SNN Pipeline for RFI Detection Hardware
Nicholas J. Pritchard, Andreas Wicenec, Richard Dodson et al. (+2 more)
Imminent
radio telescope observatories provide massive data rates making deep learning based processing appealing while simultaneously demanding real-time performance at low-energy; prohibiting the use of many artificial neural network based approaches. We begin tackling the scientifically existential challenge of
Radio Frequency Interference (RFI) detection by deploying deep Spiking Neural Networks (SNNs) on resource-constrained neuromorphic hardware. Our approach partitions large, pre-trained networks onto SynSense Xylo hardware using maximal splitting, a novel greedy
algorithm. We validate this pipeline with on-chip power measurements, achieving instrument-scaled inference at 100mW. While our full-scale SNN achieves state-of-the-art accuracy among SNN baselines, our experiments reveal a more important insight that a smaller un-partitioned model significantly outperforms larger, split models. This finding highlights that hardware co-design is paramount for optimal performance. Our work thus provides a practical deployment blueprint, a key insight into the challenges of model scaling, and reinforces
radio astronomy as a demanding yet ideal domain for advancing applied neuromorphic computing.
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All authors Nicholas J. Pritchard, Andreas Wicenec, Richard Dodson, Mohammed Bennamoun, Dylan R. Muir
Earth and Planetary Astrophysics
Analytical Solutions for Planet-Scattering Small Bodies
Yukun Huang, Brett Gladman and Eiichiro Kokubo
Gravitational scattering of small bodies (planetesimals) by a
planet remains a fundamental problem in celestial mechanics. It is traditionally modeled within the circular restricted three-body problem (CR3BP), where individual particle trajectories are obtained via numerical integrations. Here, we use Öpik's close-encounter framework to study the random walk of the orbital energy $x$ for an ensemble of test particles on
planet-crossing orbits. We show that the
evolution of each particle's orbital elements $(a, e, i)$ is fully encapsulated by the 3D rotation of the relative velocity vector $\bm{U}_\infty$, whose magnitude remains constant. Consequently, the system can be reduced to two degrees of freedom. By averaging over all possible flyby geometries, we derive explicit expressions for the drift and
diffusion coefficients of $x$. We then solve the resulting Fokker–Planck equation to obtain a closed-form solution for the time
evolution of the particle distribution. A characteristic scattering timescale naturally emerges, scaling as $(P_{p}/M_{p}^{2})/500$, where $P_{p}$ is the
planet's orbital period and $M_{p}$ its mass ratio to the central
star. The typical ejection speed of small bodies by a
planet is estimated to be $3 v_p M_{p}^{1/3}$, where $v_p$ is the
planet's orbital speed. Our analytical solution constitutes a universal law applicable to both the
Solar System and exoplanetary systems, providing a computationally efficient alternative to costly $N$-body simulations for studying the orbital distributions and ejection of planetesimals and
planets (e.g., Kuiper Belt, Oort Cloud, debris disks, interstellar objects, and free-floating
planets).
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Astrophysics of Galaxies
The PAU Survey: The $i$-band galaxy luminosity function from the present-day to $z = 2$
S. Koonkor, C. M. Baugh, G. Manzoni et al. (+13 more)
We present a measurement of the $i$-band
galaxy luminosity function from the present-day to $z = 2$, using over 1.1 million
galaxies from the Physics of the Accelerating Universe Survey (PAUS). PAUS combines broad-band imaging from the Canada-France-Hawaii
Telescope Lensing Survey with narrow-band photometry from PAUCam, enabling high-precision photometric
redshifts with an accuracy of $\sigma_{68} (\Delta z) = 0.019$ down to $i_{\textrm{AB}} = 23$. A synthetic lightcone mock catalogue built using the GALFORM semi-analytic model is used to simulate PAUS selection effects and photometric uncertainties, and to derive a machine-learning based estimate of the $k$-correction. We recover rest-frame $i$-band luminosities using a random forest regressor trained on simulated $ugriz$ photometry and
redshifts. Luminosity functions are estimated using the $1/V_{\textrm{max}}$ method, accounting for photometric
redshift and magnitude errors, and validated against mock data. We find good agreement between observations and models at $z < 1$, with increasing discrepancies at higher
redshifts due to photometric
redshift outliers. The bright-end of the luminosity function becomes flatter at high
redshift, primarily driven by
redshift errors. We show that the faint-end of the luminosity function becomes more incomplete with increasing
redshift, but is still useful for constraining models. We analyze the red and blue
galaxy populations separately, observing distinct evolutionary trends. The model overpredicts the number of both faint red and blue
galaxies. Our study highlights the importance of accurate
redshift estimation and selection modeling for robust luminosity function recovery, and demonstrates that PAUS can characterise the
galaxy population with photometric
redshifts across a wide
redshift baseline.
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All authors S. Koonkor, C. M. Baugh, G. Manzoni, D. Navarro-Gironés, P. Renard, H. Hoekstra, H. Hildebrandt, E. Gaztañaga, J. García-Bellido, P. Tallada-Crespí, F. J. Castander, J. De Vincente, R. Casas, R. Miquel, N. Sevilla-Noarbe, M. Eriksen
Cosmology and Nongalactic Astrophysics
Cosmological Constraints on the Phenomenological Interacting Dark Energy Model with Fermi Gamma-Ray Bursts and DESI DR2
Ziyan Zhu, Qingquan Jiang, Yu Liu et al. (+2 more)
In this work, we constrain the phenomenological interacting dark energy (IDE) model using
Fermi gamma-ray burst (GRB)
dataset and the latest
baryon acoustic oscillation (BAO) data from the Dark Energy Spectroscopic Instrument (DESI) Data Release 2 (DR2). Through a joint
Bayesian analysis, we perform a cosmological comparative assessment of the $\Lambda$CDM, $w$CDM, and CPL models with the phenomenological IDE model. For the phenomenological IDE model in a flat universe with
Fermi samples and DESI DR2, we obtain: $\xi=2.63^{+0.63}_{-0.52}$, $\xi + 3w_X = -0.98^{+1.90}_{-2.07}$ with the GOLD sample ($1.4\le z \le5.6$) and $\xi=2.83^{+0.63}_{-0.58}$, $\xi + 3w_X = 0.03^{+1.35}_{-1.33}$ with the FULL sample ($1.4\le z \le8.2$), respectively. Our analysis shows that the $\Lambda$CDM model without interaction ($\xi=3$, $\xi + 3w_X = 0$) is consistent with the latest
Fermi sample and DESI DR2 at $1\sigma$ confidence level. We find no significant deviations from the standard model using AIC and BIC criterias.
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All authors Ziyan Zhu, Qingquan Jiang, Yu Liu, Puxun Wu, Nan Liang
Astrophysics of Galaxies
JWST observations of cosmic-ray-excited H$_2$ in Barnard 68: spatial variations and constraints on cosmic-ray attenuation
David A. Neufeld, Kedron Silsbee, Alexei V. Ivlev et al. (+9 more)
We present James Webb Space
Telescope (JWST) NIRSpec observations of the starless dark cloud Barnard 68 that reveal the spatially-resolved signature of
cosmic-ray excited molecular hydrogen (CRXH$_2$) emissions for the first time. Following up on our initial detection of CRXH$_2$ emissions from B68 (Bialy et al. 2025), we now exploit JWST's sensitivity and spatial multiplexing to map CRXH$_2$ rovibrational lines across 16 sight lines through the cloud. By disentangling the CRXH$_2$ and UV-pumped H$_2$ components, we isolate the para-H$_2$-dominated spectrum attributable to
cosmic-ray excitation. We find that there are significant spatial variations in the ratio of the CRXH$_2$ line intensity to the line-of-sight H$_2$ column density; these cannot be accounted for by
dust extinction alone and demonstrate a clear attenuation of the
cosmic-ray flux with increasing shielding column. Modeling B68 as a Bonnor-Ebert sphere, we constrain both the unshielded
cosmic-ray ionization rate, $\zeta_{\rm H_2}$, and how it decreases with shielding column. At a reference depth of $N({\rm H}_2) = 3 \times 10^{21}$ cm$^{-2}$, we infer $\zeta_{\rm H_2} \approx 1.4 \times 10^{-16}$ s$^{-1}$, a factor of $\approx 3$ higher than the average value derived from H$_3^+$ absorption studies. These results provide the most direct probe to date of
cosmic-ray penetration into cold, dense gas, offering new constraints on both the microphysics of CR-H$_2$ interactions and the attenuation of low-energy
cosmic rays in molecular clouds. Our findings establish CRXH$_2$ emission as a powerful new diagnostic of the
cosmic-ray environment in interstellar space.
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All authors David A. Neufeld, Kedron Silsbee, Alexei V. Ivlev, Shmuel Bialy, Brandt A. L. Gaches, Marco Padovani, Sirio Belli, Thomas G. Bisbas, Amit Chemke, Benjamin Godard, James Muzerolle Page, Christian Rab
Solar and Stellar Astrophysics
Formation of Extremely Low-Mass White Dwarfs in Wide Orbits
Yangyang Zhang, Zhenwei Li and Xuefei Chen
Helium white
dwarfs (WDs) with masses less than 0.3 $\rm M_{\sun}$ are known as extremely low-mass WDs (ELM WDs), which cannot be produced by single
stellar evolution in theory. Generally, these
stars are believed to form through binary interactions. Recently, two ELM WDs in unusually wide orbits were reported, i.e., KIC 8145411 and HE 0430-2457. Their orbital separations are too wide to be produced by the binary
evolution scenario. In this work, we study the formation of wide-orbit ELM WD binaries from hierarchical triple systems. In this scenario, an ELM WD is formed from the inner binary and subsequently forms a wide binary system with the third object. We find that the merger of an evolved
star with a brown
dwarf in the inner binary fails to produce single ELM WDs, but Type Ia
supernovae (SNe Ia) explosions can successfully do so. Furthermore, we investigate the impact of the
supernova explosion on the orbital distribution of the surviving binary and find that this channel may have a probability of reproducing the orbital parameters of HE 0430-2457, but fails to reproduce the observed features of KIC 8145411. This supports recent observational recalibrations suggesting that KIC 8145411 resides in a triple system rather than a binary.
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Solar and Stellar Astrophysics
Solar Filament Physiognomy: Inferring Magnetic Quantities from Imaging Observations
P. F. Chen
Magnetic field is the key physical quantity in
solar physics as it controls all kinds of
solar activity, ranging from nanoflares to big
flares and coronal mass ejections (CMEs). However, so far only the
magnetic field on the
solar surface can be more or less precisely measured, and the most important coronal
magnetic field remains undetectable accurately. Without the knowledge of the coronal
magnetic field, it is even more difficult to obtain secondary quantities related to
magnetic field, such as the
magnetic helicity and
magnetic configuration, including the
curvature of field lines. The prevailing approaches to obtain the coronal
magnetic field include coronal
magnetic extrapolation and coronal seismology. Actually there were scattered efforts to derive secondary
magnetic quantities based on imaging observations of
solar filaments, without the help of polarization measurements. We call this approach
solar filament physiognomy. In this paper, we review these efforts made in the past decades, and point out that this approach will be promising as large
telescopes are being built and more fine structures of filament channels will be revealed.
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High Energy Astrophysical Phenomena
SN 2019vxm: A Shocking Coincidence between Fermi and TESS
Zachary G. Lane, Ryan Ridden-Harper, Sofia Rest et al. (+37 more)
Shock breakout and, in some cases, jet-driven high-energy emission are increasingly recognized as key signatures of the earliest phases of core-collapse
supernovae, especially in Type IIn systems due to their dense, interaction-dominated circumstellar environments. We present a comprehensive photometric analysis of SN 2019vxm, a long-duration, luminous Type IIn
supernova, $M_V^{}=-21.41\pm0.05\;{\rm mag}$, observed from X-ray to near-infrared. SN 2019vxm is the first superluminous
supernovae Type IIn to be caught with well-sampled TESS photometric data on the rise and has a convincing coincident X-ray source at the time of first light. The high-cadence TESS light curve captures the early-time rise, which is well described by a broken power law with an index of $n=1.41\pm0.04$, significantly shallower than the canonical $n=2$ behavior. From this, we constrain the time of first light to within 7.2 hours. We identify a spatial and temporal coincidence between SN 2019vxm and the X-ray transient GRB191117A, corresponding to a $3.3\sigma$ association confidence. Both the short-duration X-ray event and the lightcurve modeling are consistent with shock breakout into a dense, asymmetric circumstellar medium, indicative of a massive, compact progenitor such as a luminous blue variable transitioning to Wolf-Rayet phase embedded in a clumpy, asymmetric environment.
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All authors Zachary G. Lane, Ryan Ridden-Harper, Sofia Rest, Armin Rest, Conor L. Ransome, Qinan Wang, Clarinda Montilla, Micaela Steed, Igor Andreoni, Patrick Armstrong, Peter J. Brown, Jeffrey Cooke, David A. Coulter, Ori Fox, James Freeburn, Marco Galoppo, Avishay Gal-Yam, Jared A. Goldberg, Christopher Harvey-Hawes, Daichi Hiramatsu, Rebekah Hounsell, Brayden Leicester, Klára Lelkes, Itai Linial, Lászlo Molnár, Thomas Moore, Pierre Mourier, Anya E. Nugent, David O'Neill, Hugh Roxburgh, Koji Shukawa, Stephen J. Smartt, Nathan Smith, Ken W. Smith, Sebastian Vergara Carrasco, V. Ashley Villar, József Vinkó, Tal Wasserman, Zenati Yossef, Erez Zimmerman