We present the JWST/NIRSpec G395H transmission spectrum of the young (10 - 20 Myr old) transiting planet V1298 Tau b (9.85+/-0.35 Re, Teq=670K). Combined HST and JWST observations reveal a haze free, H/He dominated atmosphere with a large scale height (~1500km), allowing detection of CO2 (35 sigma), H2O (30 sigma), CO (10 sigma), CH4 (6 sigma), SO2 (4 sigma) and OCS (3.5 sigma). Our observations probe several scale heights (~4.4 in the CO2 4.3 microns and ~3 in the 2.7 micron water band). The planet's mass, inferred from atmospheric scale height using free retrieval and grid modelling is 12+/-1 and 15+/-1.7Me respectively which is significantly lower than previous radial velocity estimates and confirm it as a 'gas-dwarf' sub-Neptune progenitor. We find an atmospheric super-solar metallicity (logZ=0.6^+0.4_-0.6 x solar) and a sub-solar C/O ratio (0.22^+0.06_-0.05). The atmospheric metallicity is low compared to matured sub-Neptunes by an order of magnitude. The CH4 abundance ([CH4]=-6.1^+0.2_-0.3) is ~7 sigma lower than equilibrium chemistry prediction. To adjust for the low methane abundance, the self-consistent grids favour a high internal temperature (~500K) and vertical mixing (Kzz ~10^7-10^8 cm2/s). These internal temperatures are inconsistent with predictions from evolutionary models, which expect ~100 - 200K at the current system age. We estimate a gas-to-core mass fraction between 0.1 - 8 %, with a core mass of 11 - 12 Me, consistent with in-situ gas dwarf formation. A deep atmospheric metallicity gradient may explain both the high internal temperature and low observable metallicity. Over time, mass loss from such an atmosphere could enhance its metallicity, potentially reconciling V1298 Tau b with mature sub-Neptunes.

The transient optical source MASTER OT J072007.30+451611.6 has been recently discovered and proposed as a peculiar polar with an unusually high amplitude of the orbital brightness variation in the optical of $\sim$3 mag. To clarify its nature, we performed multiband time-series optical photometry with 1.5-m class telescopes and spectroscopy with the 10.4-m Gran Telescopio Canarias. We also analysed archival data of different optical surveys and detected the source in X-rays with the Spectrum-RG/eROSITA telescope. We confirm the orbital period of $\approx$1.5 h with the high amplitude of the brightness modulation. Compiling survey data, covering $\sim$19 yr, we find high and low brightness states of the object at time scales of years, likely explained by different accretion rates. Our data were obtained in the high brightness state. Optical spectra with hydrogen and helium emission lines, consisting of broad and narrow components, indicate the presence of an accretion stream without disk. The Doppler tomography shows that the narrow component is mainly emitted from the Lagrangian L$_1$ point, while the broad component is from the region where the accretion stream interacts with the white dwarf magnetosphere. The ratio of equivalent widths of HeII 4686 and H$\beta$ emission lines is $<$0.4, which is curiously low for polars. The X-ray spectrum of the source can be described by the thermal plasma emission model with parameters consistent with values observed for polars.

We examine recent astronomical data to assess whether the sun and Solar System possess anomalous properties compared to other stars and exoplanetary systems, providing context for astrobiology research. Utilising data primarily from large surveys like {\it Gaia}, {\it Kepler}, {\it TESS}, and ground-based spectroscopy (e.g., GALAH, LAMOST, HARPS), we construct comparison samples (e.g., nearby stars, solar analogues and twins within 20-200 pc) and employ statistical methods, including regression analysis, to account for parameter dependencies. We find that the sun is modestly metal-rich compared to nearby solar-age stars. More anomalous solar properties include its mass (top $\sim$8 percent locally), low photometric variability on short timescales ($\sim$0.2 percent), specific light and heavy element abundance patterns (high beryllium, low lithium, low carbon/oxygen and nitrogen/oxygen ratios, and low heavy neutron capture and refractory elements), slow rotation, and low superflare rate. The sun has average $\alpha$/iron, phosphorus/iron, and Ytterbium/iron abundance ratios. It also has average chromospheric activity as measured by R$^{\rm '}_{\rm HK}$(T$_{\rm eff}$), R$^{\rm +}_{\rm HK}$, and H$\alpha$ indices. The Solar System is unusual in its lack of super-Earths despite hosting a cold Jupiter ($\sim$3 percent), the low eccentricities of its planets (especially considering detectability, $<2$ percent), its large size scale for a multi-planet system ($\sim$6 percent), and potentially the sun's obliquity. The sun's galactic orbit is less eccentric and has lower vertical excursions than $\sim$95 percent of nearby solar analogues. Its current position is near perigalacticon and minimum distance from the Galactic plane, resulting in a higher local star density than 98.8 percent of randomly chosen times from $-0.5$ to $+0.5$ Gyrs.

Galaxy simulations have come a long way from the early days of simple N-body calculations, which considered only gravitational interactions, to the complex, multi-physics models used today. Beginning with initial conditions representative of the Universe shortly after the Big Bang, these modern simulations integrate the relevant physical processes involved in galaxy formation, such as gravity, gas dynamics, cooling, star formation, and feedback, while accounting for cosmic expansion and structure formation. This review provides an introductory overview of cosmological galaxy simulations, outlining the essential components and methods used to model the formation and evolution of galaxies on the computer. It also discusses common steps in the post-processing analysis, essential for extracting physical insights from these numerical experiments, along with basic tests to assess simulation validity and accuracy. Looking forward, next-generation simulations aim to push resolution boundaries, incorporate additional physical processes, and improve the robustness of the numerical models, promising to lead to a deeper understanding of how galaxies emerged and evolved over cosmic time.

The majority of Little Red Dots (LRDs) hosting Active Galactic Nuclei (AGN) exhibits broad H$\alpha$ emission, which recent studies propose originates from scattering off free electrons within an ionized and dense medium embedding the Broad Line Region (BLR), rather than directly from the BLR itself. This model suggests that the observed broad lines may be intrinsically narrower than observed, which would lead to black hole masses that are up to two orders of magnitude smaller than what inferred when assuming that the whole broad line comes from the BLR. To test this model, we present a joint analysis of multiple hydrogen recombination lines in the ''Rosetta Stone''AGN, the brightest known LRD at $z$=2.26. We show that H$\alpha$, H$\beta$ and Pa$\beta$ have different spectral profiles, which is inconsistent with the predictions of the simple electron scattering scenario. Additionally, we test a variety of exponential models and show that none of them can simultaneously reproduce all three line profiles with physically plausible parameters. The inadequacy of these models for the Rosetta Stone implies that the scenario of electron scattering by an ionized medium surrounding the BLR is not universally applicable to LRDs and AGN, and therefore provides a counterexample to the claim of a universal and systematic overestimation of black hole masses.

Large-scale structure surveys can be used to measure the dipole in the cosmic microwave background (CMB), in the luminosity distances inferred from type-Ia supernova observations, and in the spatial distribution of galaxies and quasars. The measurements of these cosmic dipoles appear to be mutually inconsistent, even though they are expected to indicate the common observer velocity. This observational tension may represent a significant challenge to the standard model of cosmology. Here we study in detail what contributes to the cosmic dipoles from CMB, supernova, and galaxy survey in the standard $\Lambda$CDM model, though our theoretical model can be applied beyond the standard model. While measurements of the cosmic dipoles yield the relative velocities between the source samples and the observer velocity, the motion of the observer is the dominant contribution in the conformal Newtonian gauge, and the intrinsic velocities of the samples fall steeply with increasing redshift of the sources. Hence the cosmic dipoles of CMB, type-Ia supernovae, and galaxies should be aligned but can have different amplitudes. We also clarify several misconceptions that are commonly found in the literature.

We investigate the far-infrared (far-IR) incidence of X-ray-selected active galactic nuclei (AGN) and non-AGN galaxies as a function of stellar mass (M$_*$), star formation rate (SFR), and specific black hole accretion rate ($\lambda_{\text{sBHAR}}$), using data from five extragalactic fields (COSMOS, XMM-LSS, Stripe82, ELAIS-S1, and CDFS-SWIRE). We construct spectral energy distributions (SEDs) from optical-to-far-IR photometry to derive host galaxy properties and assess AGN obscuration. X-ray absorption is quantified using the 4XMM-DR11s catalog. Our final sample includes 172,697 non-AGN galaxies (53% Herschel-detected) and 2,417 X-ray AGN (73% Herschel-detected), with $10 < log\,[M_*/M_\sun] < 12$ and $0 < z < 2$. X-ray AGN exhibit a relatively flat far-IR detection rate across stellar mass and specific SFR ($sSFR = SFR / M_*$), unlike non-AGN galaxies, where detection correlates strongly with SFR. Among AGN, far-IR detection declines with increasing $\lambda_{\text{sBHAR}}$, despite rising SFR. Our results suggest X-ray AGN are preferentially found in gas-rich environments, where star formation and black hole accretion coexist. Far-IR incidence remains high across all sSFR bins, supporting a scenario in which AGN feedback regulates, rather than abruptly quenches, star formation. Comparing AGN and non-AGN SFRs without separating Herschel-detected from non-detected sources introduces biases. Obscured AGN show ~10% higher far-IR detection rates than unobscured ones, yet at similar $\lambda_{\text{sBHAR}}$, unobscured AGN tend to have higher SFR. This may suggest obscured AGN inhabit dustier systems with moderate star formation contributing to the far-IR. Our findings support a regulatory AGN feedback mode operating over extended timescales in gas-rich galaxies.

It has been demonstrated that one can track down galaxies in absorption 'hidden' in the Lyman-$\alpha$ forest through the use of 'strong, blended Lyman-$\alpha$' (or SBLA) absorption. Specifically a series of publications studied SBLA absorption systems with Lyman-$\alpha$ flux transmission, $F_{Ly \alpha} < 0.25$ on scales of 138 km s$^{-1}$ in the Sloan Digital Sky Survey (SDSS). In order to better understand the connection between halos and these SBLAs, we make use of several million synthetic absorption spectra from the TNG50 cosmological simulation, at z=2 and z=3. We explore spectra with SDSS-like resolution in order to understand the nature of SBLAs as defined thus far, as well as with high resolution (or 'resolved') spectra to generalise and optimise SBLAs as halo finders. For the SDSS SBLAs, we find that up to 78% of these absorption systems reside in hlaos, where the stronger the absorption and the lower the redshift, the higher the probability. We also manage to recover a mean halo mass of $10^{12.25} M_{\odot}$, in line with what is measured in observations. For the resolved SBLAs, we expand on the previous definition and allow the SBLA spectra size to vary between 54 km s$^{-1}$ and 483 km s$^{-1}$. We find that the largest absorbers have the highest probability of finding halos. When applying a hierarchical framework, where we allow the largest SBLAs to consume the smaller ones, we find that the halo mass distributions for each SBLA spectral size becomes narrower with respect to the non-hierarchical case. We are also able to probe halo masses from $M_h \approx 10^{9.5} M_{\odot}$ (for 100 km s$^{-1}$ SBLAs) to $M_h \approx 10^{11.5} M_{\odot}$ (for 450 km s$^{-1}$ SBLAs). With these results, we show that we are able to transform the Lyman-$\alpha$ forest into a powerful halo finding machine for not only identifying CGM regions, but also estimating their host halo masses.

In this letter, we call attention to a gap in binaries in the Kuiper belt in the mass range between $\approx$10$^{19}$-10$^{20}$ kg, with a corresponding dearth in binaries between 4th and 5th absolute magnitude $H$. The low-mass end of the gap is consistent with the truncation of the cold classical population at 400 km, as suggested by the OSSOS survey, and predicted by simulations of planetesimal formation by streaming instability. The distribution of magnitudes for all KBOs is continuous, which means that many objects exist in the gap, but the binaries in this range have either been disrupted, or the companions are too close to the primary and/or too dim to be detected with the current generation of observational instruments. At the high-mass side of the gap, the objects have small satellites at small separations, and we find a trend that as mass decreases, the ratio of primary radius to secondary semimajor increases. If this trend continues into the gap, non-Keplerian effects should make mass determination more challenging.

Massive galaxy clusters act as prominent strong-lenses. Due to a combination of observational biases, cluster evolution and lensing efficiency, most of the known cluster lenses lie typically at $z_{l}\sim0.2-0.7$, with only a few prominent examples at higher redshifts. Here we report a first strong-lensing analysis of the massive galaxy cluster SPT-CL J0546-5345 at a redshift $z_l=1.07$. This cluster was first detected through the Sunyaev-Zel'dovich effect, with a high estimated mass for its redshift of $M_{200,c} = (7.95 \pm 0.92) \times 10^{14}\,M_{\odot}$. Using recent JWST/NIRCam and archival HST imaging, we identify at least 10 secure and 6 candidate sets of multiply imaged background galaxies, which we use to constrain the mass distribution in the cluster. We derive effective Einstein radii of $\theta_{E}= 18.1 \pm 1.8 ''$ for a source at $z_{s}=3$, and $\theta_{E}= 27.9 \pm 2.8 ''$ for a source at $z_{s}=9$. The total projected mass within a $200$ kpc radius around the strong-lensing region is $M(<200\,\mathrm{kpc}) = (1.9 \pm 0.3) \times 10^{14}\,M_{\odot}$. While our results rely on photometric redshifts warranting spectroscopic follow-up, this central mass resembles that of the Hubble Frontier Fields clusters - although SPT-CL J0546-5345 is observed when the Universe was $\sim 3-4$ Gyr younger. Amongst the multiply-imaged sources, we identify a hyperbolic-umbilic-like configuration, and, thanks to its point-like morphology, a possible Active Galactic Nucleus (AGN). If confirmed spectroscopically, it will add to just a handful of other quasars and AGN known to be multiply lensed by galaxy clusters.

As cosmological simulations and their associated software become increasingly complex, physicists face the challenge of searching through vast amounts of literature and user manuals to extract simulation parameters from dense academic papers, each using different models and formats. Translating these parameters into executable scripts remains a time-consuming and error-prone process. To improve efficiency in physics research and accelerate the cosmological simulation process, we introduce SimAgents, a multi-agent system designed to automate both parameter configuration from the literature and preliminary analysis for cosmology research. SimAgents is powered by specialized LLM agents capable of physics reasoning, simulation software validation, and tool execution. These agents collaborate through structured communication, ensuring that extracted parameters are physically meaningful, internally consistent, and software-compliant. We also construct a cosmological parameter extraction evaluation dataset by collecting over 40 simulations in published papers from Arxiv and leading journals that cover diverse simulation types. Experiments on the dataset demonstrate a strong performance of SimAgents, highlighting its effectiveness and potential to accelerate scientific research for physicists. Our demonstration video is available at: https://youtu.be/w1zLpm_CaWA. The complete system and dataset are publicly available at https://github.com/xwzhang98/SimAgents.

The Mid-Infrared Instrument (MIRI) on the James Webb Space Telescope (JWST) enables the characterisation of young self-luminous gas giants at previously inaccessible wavelengths, revealing physical processes in gas, dust, and clouds. We characterise the young planetary system TWA 27 (2M1207) in the mid-infrared (MIR), studying the atmosphere and disk spectra of the M9 brown dwarf TWA 27A and its L6 planetary-mass companion TWA 27b. We obtained data with the MIRI Medium Resolution Spectrometer (MRS) from 4.9 to 20 um, and MIRI Imaging in the F1000W and F1500W filters. We applied high-contrast imaging methods to extract the companion's spectral energy distribution up to 15 um at 0.78 arcsec separation and a contrast of 60. Combining these with published JWST/NIRSpec spectra, we analysed the 1-20 um range using self-consistent atmospheric grids and 0D slab models for molecular disk emission. The atmosphere of TWA 27A is well fitted by a BT-SETTL model with Teff 2780 K, log g 4.3, plus a 740 K blackbody for the inner disk rim. The disk shows at least 11 organic molecules, with no water or silicate dust emission detected. The atmosphere of TWA 27b is matched by a Teff 1400 K low-gravity model with extinction, best fit by the ExoREM grid. MIRI spectra and photometry for TWA 27b reveal a silicate cloud absorption feature between 8-10 um and significant (>5 sigma) infrared excess at 15 um consistent with circumplanetary disk emission. These MIRI observations provide new insights into TWA 27, revealing diverse features to study the formation and evolution of circumplanetary disks and young dusty atmospheres.

Microlensing surveys suggest the presence of a surprisingly large population of free-floating planets, with a rate of about two Neptunes per star. The origin of such objects is not known, neither do we know if they are truly unbound or are merely orbiting at large separations from their host stars. Here, we investigate planet-planet scattering as a possible origin through numerical simulations of unstable multi-planet systems. We find that planet ejection by scattering can be slow, often taking more than billions of years for Neptune-mass scatterers orbiting at a few AU and beyond. Moreover, this process invariably delivers planets to orbits of hundreds of AU that are protected from further scattering. We call these ''detached" planets. Under the scattering hypothesis, we estimate that about half of the reported ''free-floating" Neptunes are not free but merely ''detached".

We investigate the star formation histories (SFHs) of 983 early-type dwarf galaxies classified into five morphological subtypes, dS0, dE, dEbc, dSph, and dEbl,across six environments ranging from the field to rich clusters such as Ursa Major and Virgo. Using full spectral fitting of SDSS spectra with the starlight code, we derive detailed SFHs and chemical enrichment patterns. We find that SFHs are primarily shaped by morphology, with environment playing a secondary but non-negligible role. Red early-type dwarfs (dS0, dE, dSph) typically formed most of their stars early and quenched rapidly, whereas blue early-type dwarfs (dEbc, dEbl) exhibit extended or ongoing star formation and host extremely metal-poor stars, suggesting continued pristine gas accretion. Environmental dependence is clearest in low-mass systems: field galaxies often show prolonged SFHs and delayed enrichment, while Virgo Cluster galaxies tend to quench earlier and enrich more rapidly. Cumulative SFHs reinforce these trends, with dSph galaxies showing the earliest quenching and least environmental dependence, indicating a likely primordial origin. Metallicity evolution also varies with mass and environment, progressing most slowly in low-mass field galaxies and most rapidly in high-mass cluster galaxies. Our results highlight the combined influence of morphology, stellar mass, and environment on the evolutionary diversity of early-type dwarfs, and suggest that both internal processes (nature) and external conditions (nurture) are intricately linked in shaping their star formation and chemical enrichment histories.

We evaluate the feasibility of Bose-Einstein condensate stars (BECS) as models for the interior of neutron stars. BECS are compact objects composed of bosons, formed through the spin-parallel pairing of neutrons. Here, we utilize the astronomical data from GW170817, XMMU J173203.3-344518 (the lightest neutron star known), and a novel lower limit on neutron star core heat capacity to scrutinize the compatibility of BECS with these recent observations of neutron stars. Our specific focus is to constrain the values of the scattering length $a$, a parameter determining the strength of particle interactions in the model. Our analysis suggests that if the stars involved in GW170817 were BECSs, the scattering length of their constituent bosons should fall within the $4$ to $10$ fm range. Additionally, at a scattering length of $a\sim 3.1-4$ fm, stars with mass and radius characteristics akin to XMMU J173203.3-344518 are identified. Moreover, we find that the heat capacity depends of the mass and temperature of BECS, and surpasses the established lower bound for neutron star cores when $a>2-5$ fm. In summary, our results endorse BECS models with $a\sim 4$ fm, providing neutron star observables in robust agreement with diverse observations and contributing to the ongoing understanding of neutron star interiors.

The detection of extensive air showers using radio antennas has evolved into a mature technique, complementing particle detector arrays by providing sensitivity to the longitudinal development of the showers and enabling an independent determination of the cosmic-ray energy. Both the Pierre Auger Observatory in Argentina and the IceCube Neutrino Observatory at the South Pole have been undergoing upgrades, including the integration of radio antennas. The next-generation neutrino detector IceCube-Gen2 will also feature a surface array for PeV-EeV cosmic-ray detection, consisting of scintillation detectors and radio antennas. Prototype stations for this upgrade have been in operation for several years at both, the South Pole and the Auger Observatory, enabling cross-checks and potentially a cross-calibration of the energy scales between the two experiments. In this contribution, we present an analysis of air showers observed with the radio antennas of the IceCube-Gen2 prototype station, coinciding with detections by the water-Cherenkov detectors of the densest part of the Pierre Auger Observatory's surface array, featuring a 433 m spacing.

We present an analysis of the correlation between the depth of the maximum of air-shower profiles and the signal in water-Cherenkov stations in events registered simultaneously by the fluorescence and surface detectors of the Pierre Auger Observatory. The analysis enables us to place constraints on the spread of nuclear masses in ultra-high-energy cosmic rays with a minor impact from the experimental systematic uncertainties and uncertainties in air-shower simulations. Due to this unique feature, the correlation analysis has previously allowed us to exclude all pure and proton-helium compositions near the ankle in the cosmic-ray energy spectrum at 5$\sigma$ confidence level. The same property makes the correlation analysis an effective tool for testing the consistency of predictions of the post-LHC hadronic interaction models, including their latest versions such as EPOS LHC-R, QGSJet-III-01, Sibyll${}^\bigstar$ and Sibyll 2.3e. In this work, the correlation analysis using the Phase I hybrid data from the Pierre Auger Observatory is presented. The analysis uses the newest generation of hadronic interaction models and covers an extended energy range around the ankle in the cosmic-ray spectrum.

We present ongoing radio observations of the tidal disruption event (TDE) AT2018hyz, which was first detected in the radio at 972 days after disruption, following multiple non-detections from earlier searches. The new observations presented here span approximately 1370-2160 days and 0.88-240 GHz. We find that the light curves continue to rise at all frequencies during this time period, following a power law of about F ~ t^3 (compared to F_nu ~ t^5.7 at 972-1400 days), and reaching a peak luminosity of L~ 10^40 erg/s, comparable to the luminosity of the relativistic TDE Swift 1644+57 on the same timescale. The multi-frequency data indicate that the peak frequency does not significantly evolve over the 1030-day span of our observations, while the peak flux density increases by an order of magnitude. The observed behavior is consistent with two possible scenarios: (i) a delayed spherical outflow launched about 620 days post-disruption with a velocity of ~0.3c and an energy of ~10^50 erg, and (ii) a highly off-axis (~80-90 deg) relativistic jet with a Lorentz factor of Gamma ~8 and E_K ~ 10^52 erg. Continued radio observations to capture the light curve peak, as well as VLBI observations, could distinguish between these scenarios.

Afterglows of GRBs are, in general, well described by the fireball model. Yet, deducing the full set of model parameters from observations without prior assumptions has been possible for only a handful of GRBs. With GROND, a 7-channel simultaneous optical and near-infrared imager at the 2.2m telescope of the Max-Planck Society at ESO/La Silla, a dedicated gamma-ray burst (GRB) afterglow observing program was performed between 2007 and 2016. Here, we combine GROND observations of four particularly well-sampled GRBs with public Swift/XRT data and partly own sub-mm and radio data to determine the basic fireball afterglow parameters. We find that all four bursts exploded into a wind environment. We are able to infer the evolution of the magnetic field strength from our data, and find evidence for its origin through shock amplification of the magnetic field of the circumburst medium.

Neutron-rich outflows in neutron-star mergers (NSMs) or other explosive events can be subject to substantial heating through the release of rest-mass energy in the course of the rapid neutron-capture (r-) process. This r-process heating can potentially have a significant impact on the dynamics determining the velocity distribution of the ejecta, but due to the complexity of detailed nuclear networks required to describe the r-process self-consistently, hydrodynamic models of NSMs often neglect r-process heating or include it using crude parametrizations. In this work, we present a conceptually new method, RHINE, for emulating the r-process and concomitant energy release in hydrodynamic simulations via machine-learning algorithms. The method requires the evolution of only a few additional quantities characterizing the composition, of which the nuclear rates of change are obtained at each location and time step from neural networks trained by a large set of trajectories from full nuclear-network calculations. The scheme is tested by comparing spherically symmetric wind simulations and long-term simulations of NSMs using RHINE with post-processing results from nucleosynthesis calculations, where we find very good agreement. In our NSM models on average about 2.3MeV, 0.7MeV, and 2.1MeV are released per baryon in dynamical ejecta, NS-torus ejecta, and black-hole (BH) torus ejecta, respectively. The strongest velocity boost is observed for BH-torus ejecta, which also become 40% more massive with r-process heating. The nucleosynthesis yields are only mildly affected by r-process heating, but the kilonova gets significantly brighter once the BH-torus ejecta become visible. RHINE can be readily implemented in existing hydrodynamics codes using pre-trained machine-learning data and routines for source-term prediction that we provide online.

The filamentary dark cloud complex in Norma reveals signs of active low-mass star formation including protostars, H-alpha emission line stars, Herbig Haro objects, and the eruptive FU Orionis-like star V346 Nor. We present results of the first pointed X-ray observations of the Norma dark cloud, focusing on the westernmost Sandqvist 187 region. Chandra detected 75 X-ray sources and a complementary XMM-Newton observation detected 92 sources within the Chandra field-of-view, of which 46 are cross-matched to Chandra, yielding 121 unique X-ray sources. We present a catalog of X-ray sources along with basic X-ray properties and candidate IR and optical counterparts. Existing near-IR photometry reveals several X-ray sources with color excesses as typical of young stars with disks. Gaia parallaxes single out foreground stars and X-ray sources with distances of 500 - 1000 pc that are probable cloud members. The known emission line stars Sz 136 and Sz 137 were detected but V346 Nor was not. Interestingly, the optical and IR counterparts of the brightest Chandra source are not known with certainty but the prime suspects are very faint. Thus, the nature of the object responsible for the bright X-ray emission remains speculative. The X-ray observations presented here will serve as a pathfinder for identifying and characterizing the young stellar population in the Norma dark cloud.

In the quest to understand the climates and atmospheres of exoplanets, 3D global climate models (GCMs) have become indispensable. The ability of GCMs to predict atmospheric conditions complements exoplanet observations, creating a feedback loop that enhances our understanding of exoplanetary atmospheres and their environments. This paper discusses the capabilities of the Global Exoplanet Spectra (GlobES) module of the Planetary Spectrum Generator (PSG), which incorporates 3D atmospheric and surface information into spectral simulations, offering a free, accessible tool for the scientific community to study realistic planetary atmospheres. Through detailed case studies, including simulations of TRAPPIST1 b, TRAPPIST-1 e, and Earth around Sun, this paper demonstrates the use of GlobES and its effectiveness in simulating transit, emission and reflected spectra, thus supporting the ongoing development and refinement of observational strategies using the James Webb Space Telescope (JWST) and future mission concept studies (e.g., Habitable Worlds Observatory [HWO]) in exoplanet research.

NASA's Nancy Grace Roman Space Telescope is a flagship astrophysics mission planned for launch no later than May 2027. The Coronagraph Instrument (CGI) aboard Roman will demonstrate the technology for direct imaging and spectroscopy of exoplanets around nearby stars and starlight suppression that surpass previous space-based and ground-based coronagraphs. This is accomplished using active wavefront control in space with deformable mirrors. CGI requires a star acquisition system capable of acquiring reference and target stars to achieve this goal. This paper describes two CGI star acquisition system methods: EXCAM and Raster Scan. Furthermore, it will detail the results of the CGI thermal vacuum (TVAC) tests conducted to evaluate system-level star acquisition and verify its performance requirements.

We present analog clocks fitted to the Mars solar day. These clocks use the standard Earth-based second of the International System of Units (SI) as their operational unit of time, unlike current practice for Mars timekeeping. We discuss the importance of preserving the SI second. On this basis, we identify the two analog clocks most suitable for public use by a future Mars population. These are a 20-hour clock with a hand motion similar to that of the standard Earth clock, and a 24-hour clock with a novel "Martian" hand motion which strikes the hour when all 3 hands converge onto that hour mark on the dial. Both clocks have Earth-day equivalents to assist learning. We also present a 24-hour "SpaceClock", similar to the Martian clock but with no favored reference plane, hence equally readable from any viewing orientation.

We argue that the "Little Red Dots" (LRDs) discovered with the James Webb Space Telescope are quasi-stars in their late stages of evolution. Quasi-stars are hypothetical objects predicted to form following the core collapse of supermassive stars, and consist of black holes accreting from massive envelopes at a super-Eddington rate. We show that models of late-stage quasi-stars, with black hole masses exceeding $\sim 10\%$ of the total, predict thermal and radiative properties that are insensitive to both black hole and envelope mass, and spectrally resemble LRDs. Specifically, we show that they are likely to exhibit reddish colors, a strong Balmer break, and possess conditions favorable to the production of Balmer lines that are broadened by electron scattering. Their huge electron column densities suppress any X-rays. Late-stage quasi-stars, with black hole masses $\gtrsim 10^6 M_\odot$, should dominate the overall quasi-star population. Their short predicted lifetimes (tens of Myr), coupled with the high observed comoving density of LRDs, suggest that most or all supermassive black holes go through a quasi-star/LRD phase during their formation and growth.

In recent years, the existence of a gap in the mass spectrum of compact objects formed from stellar collapse, between the heaviest neutron stars and the lightest black holes, has been a matter of significant debate. The presence or absence of a mass gap has implications for the supernova mechanism, as well as being a fundamental property of the compact object mass function. In X-ray binaries containing black holes a gap is observed, but it is not known whether this is representative of a true gap in the mass function or due to selection effects or systematic biases in mass estimation. Binary black hole mergers detected from gravitational waves in the GWTC-3 transient catalog furnish a large sample of several tens of low-mass black holes with a well-understood selection function. Here we analyze the \nevts{} GWTC-3 merger events (along with GW230529\_181500) with at least one black hole ($3 \, M_\odot < m_1$) and chirp masses below those of a $20\,M_\odot$--$20\,M_\odot$ merger ($\mathcal{M} < 17.41 M_{\odot}$) to uncover the structure of the low-mass black hole mass function. Using flexible parameterized models for the mass function, we find, similar to existing studies, a sharp peak in the mass function at $m \simeq (8-10 M_{\odot})$. We observe a steady decline in the merger rate to lower masses, but by less than an order of magnitude in total, and find that the first percentile of black hole masses in our most flexible model is $m_{1\%} =3.13^{+0.18}_{-0.04}$. In other words, this sample of low-mass black holes is not consistent with the existence of a mass gap.

Gravitational lensing by massive galaxy clusters enables faint distant galaxies to be more abundantly detected than in blank fields, thereby allowing one to construct galaxy luminosity functions (LFs) to an unprecedented depth at high redshifts. Intriguingly, photometric redshift catalogs (e.g. Shipley et al. (2018)) constructed from the Hubble Frontier Fields survey display an excess of z$\gtrsim$4 galaxies in the cluster lensing fields and are not seen in accompanying blank parallel fields. The observed excess, while maybe a gift of gravitational lensing, could also be from misidentified low-z contaminants having similar spectral energy distributions as high-z galaxies. In the latter case, the contaminants may result in nonphysical turn-ups in UV LFs and/or wash out faint end turnovers predicted by contender cosmological models to $\Lambda$CDM. Here, we employ the concept of magnification bias to perform the first statistical estimation of contamination levels in HFF lensing field photometric redshift catalogs. To our great worry, while we were able to reproduce a lower-z lensed sample, it was found $\sim56\%$ of $3.5 < z_{phot} < 5.5$ samples are likely low-z contaminants! Widely adopted Lyman Break Galaxy-like selection rules in literature may give a 'cleaner' sample magnification bias-wise but we warn readers the resulting sample would also be less complete. Individual mitigation of the contaminants is arguably the best way for the investigation of faint high-z Universe, and this may be made possible with JWST observations.

There is a relatively large population of known double white dwarfs (DWDs) that were mostly discovered through spectroscopic observations and by measuring their radial velocity variations. Photometric observations from these systems give us additional information about their faint components by manifesting eclipsing or lensing signals or periodic trends such as ellipsoidal variations or Doppler boosting. To find these signals and trends we probe the public photometric data collected by the Transiting Exoplanet Survey Satellite (TESS) telescope from 17 known DWD systems. We use the Singular Spectrum Analysis (SSA) technique to de-noise their light curves. For DWD systems J1717$+$6757, J1557$+$2823, LP400$-$22, J1449$+$1717, J2132$+$0754, and J2151$+$1614 we find regular and periodic trends in their TESS light curves. The periodic trend in light curve J1449$+$1717 is caused by the blending effect due to a variable and bright star close to it which are unresolvable in the TESS observations. The discovered periodic trend for J1717$+$6757 was recovered by the TESS data. The periodic trends in light curves of J1557$+$2823 and J2151$+$1614 have the False Alarm Probability (FAP) values $\simeq 14.8,~36.5\%$. So their detected trends are likely noises with non-orbital origins. Periods of trends in light curves of LP400$-$22 and J2132$+$0754 are the same as and half of orbital periods, respectively. We evaluate possible ranges for Doppler boosting and ellipsoidal variations's amplitudes for these targets. This study highlights the importance of TESS data for identifying periodic trends such as ellipsoidal or intrinsic variations rather than short eclipsing/lensing signals in DWD light curves specially bright targets with ignorable blending.

The hottest, most ionized, and fastest winds driven by accretion onto massive black holes have the potential to reshape their host galaxies. Calorimeter-resolution X-ray spectroscopy is the ideal tool to understand this feedback mode, as it enables accurate estimates of physical characteristics needed to determine the wind's kinetic power. We report on a photoionization analysis of five observations of the Seyfert-1.5 galaxy NGC 4151, obtained with XRISM/Resolve in 2023 and 2024. In the Fe K band, individual spectra require as many as six wind absorption components. Slow "warm absorbers" (WAs, $v_{\mathrm{out}} \sim 100 - 1000~\mathrm{km~s^{-1}}$), very fast outflows (VFOs, $v_{\mathrm{out}} \sim 10^3~{\rm km}~{\rm s}^{-1} - 10^4~{\rm km}~{\rm s}^{-1}$), and ultra-fast outflows (UFOs, $v_{\mathrm{out}} \sim 10^4~{\rm km}~{\rm s}^{-1} - 10^5~{\rm km}~{\rm s}^{-1}$ or $0.033 - 0.33~c$) are detected simultaneously, and indicate a stratified, multiphase wind. Fast and variable emission components suggest that the wind is axially asymmetric. All of the wind components have mass flow rates comparable to or in excess of the mass accretion rate, though the slowest zones may be "failed" winds that do not escape. Two UFO components have kinetic luminosities that exceed the theoretical threshold of $L_{kin} \geq 0.5\% L_{Edd}$ necessary to strip the host bulge of gas and halt star formation, even after corrections for plausible filling factors. The bulk properties of the observed winds are consistent with magnetocentrifugal driving, where the density depends on radius as $n \propto r^{-1.5}$, but radiative driving and other mechanisms may also be important. Numerous complexities and variability require further analysis.

The Pierre Auger Observatory has led to significant advances in our understanding of ultra-high-energy cosmic rays. These new insights have driven a major upgrade of the Observatory, known as AugerPrime, through which the experiment has entered its Phase II, a new period of data collection. A key part of the upgrade is adding surface scintillator detectors (SSD) on top of the existing water-Cherenkov detectors (WCD). The main goal is to leverage their different responses to the electromagnetic and muonic shower components, enhancing the reconstruction of the primary cosmic-ray mass. In this contribution, we present the methods that involve analyzing peak and charge distributions of atmospheric muons for accurate calibration during extensive air-shower event reconstruction, along with the development of a rate-based algorithm for independent calibration. We also show the performance of the SSDs with Phase-II data, including PMT reliability and stability of key parameters, such as gain and signal-to-noise ratio.

Constraints on the cosmological parameters of Torsion Condensation (TorC) are investigated using Planck 2018 Cosmic Microwave Background data. TorC is a case of Poincar\'e gauge theory -- a formulation of gravity motivated by the gauge field theories underlying fundamental forces in the standard model of particle physics. Unlike general relativity, TorC incorporates intrinsic torsion degrees of freedom while maintaining second-order field equations. At specific parameter values, it reduces to the $\Lambda$CDM model, providing a natural extension to standard cosmology. The base model of TorC introduces two parameters beyond those in $\Lambda$CDM: the initial value of the torsion scalar field and its time derivative -- one can absorb the latter by allowing the dark energy density to float. To constrain these parameters, 'PolyChord' nested sampling algorithm is employed, interfaced via 'Cobaya' with a modified version of 'CAMB'. Our results indicate that TorC allows for a larger inferred Hubble constant, offering a potential resolution to the Hubble tension. Tension analysis using the $R$-statistic shows that TorC alleviates the statistical tension between the Planck 2018 and SH0Es 2020 datasets, though this improvement is not sufficient to decisively favour TorC over $\Lambda$CDM in a Bayesian model comparison. This study highlights TorC as a compelling theory of gravity, demonstrating its potential to address cosmological tensions and motivating further investigations of extended theories of gravity within a cosmological context. As current and upcoming surveys -- including Euclid, Roman Space Telescope, Vera C. Rubin Observatory, LISA, and Simons Observatory -- deliver data on gravity across all scales, they will offer critical tests of gravity models like TorC, making the present a pivotal moment for exploring extended theories of gravity.

Weak gravitational lensing (WL) peak statistics capture cosmic non-linear structures and can provide additional cosmological information complementary to cosmic shear two-point correlation analyses. They have been applied to different WL surveys successfully. To further facilitate their high precision applications, it is very timely to investigate the impacts of different systematics on WL peak statistics and how to mitigate them. Concerning the influence from galaxy intrinsic alignments (IAs), in this paper, we develop a theoretical model for WL high peaks taking into account the IA effects. It is an extension of our previous halo-based model. The IA corrections mainly include the modification of the lensing profile of clusters of galaxies due to the alignments of satellite galaxies and the additional shape noise correlations. We validate our model using simulations with the semi-analytical galaxy formation. We consider the cases where the satellite galaxies are averagely radially aligned toward the centers of their host clusters but with different dispersions $\sigma_{\theta}$. We show that our model works well for $\sigma_{\theta}>45^{\circ}$. If the IA corrections are not included in the model, for the Euclid/CSST-like source galaxy distribution and the survey area of $\sim 1000 deg^2$, the IA induced bias on $S_8$ can reach $\sim 8\sigma$ even for $\sigma_{\theta}=75^{\circ}$. With our model, not only the bias can be well mitigated, but also we can constrain the satellite IA to the level of {\bf $\sigma(\sigma_{\theta})\sim \pm 24^{\circ}$} simultaneously from WL high peak analyses alone using data from such a survey.

We present a multi-frequency analysis of the candidate double-double radio galaxy (DDRG) J2349-0003, exhibiting a possible lobe misalignment. High-resolution uGMRT observations at Bands 3 and 4 reveal a complex radio morphology featuring a pair of inner and outer lobes, and the radio core, while the Band 5 image detects the core and the compact components. The positioning of both pairs of lobes with the central core supports its classification as a DDRG. Spectral age estimates for the inner and outer lobes indicate two distinct episodes of active galactic nucleus (AGN) activity interspaced by a short quiescent phase. The possible compact steep spectrum nature of the core, together with its concave spectral curvature, suggests ongoing or recent jet activity, suggesting the possibility that J2349-0003 may be a candidate triple-double radio galaxy. With a projected linear size of 1.08 Mpc, J2349-0003 is classified as a giant radio galaxy (GRG), although its moderate radio power (~10^24 W/Hz) suggests a sparse surrounding environment. Arm-length (R_theta) and flux density ratios (R_S) indicates environmental influences on source symmetry. The observed lobe misalignment and the presence of nearby galaxies in the optical image suggest that merger-driven processes may have played a key role in shaping the source's evolution.

Ultra-high-energy photons have long been sought as tracers of the most energetic processes in the Universe. Several sources can contribute to a diffuse photon flux, including interactions of cosmic rays with Galactic matter and radiation fields, as well as more exotic scenarios such as the decay of super-heavy dark matter. Regardless of their origin, the expected flux is extremely low, making direct detection impractical and thereby requiring indirect detection by extensive ground-based detector arrays. In this contribution, we present a novel method for photon-hadron discrimination in the energy range of $50$ to $300\,\text{PeV}$ based on deep learning algorithms. Our approach relies on information from both the Surface Detector (SD) and the Underground Muon Detector (UMD) of the Pierre Auger Observatory. The SD consists of an array of water-Cherenkov detectors. It is used to measure the electromagnetic and muonic components of extensive air showers at ground level. Meanwhile, the UMD is composed of buried scintillator modules. It is sensitive to air-shower muons with energies above ${\sim}1\,\text{GeV}$, enhancing the identification of muon-poor air showers as initiated by photon primaries. Our method represents air-shower events as graphs, and consequently, the network architecture is composed of graph attention layers. We assess the performance of the method on a data subset and discuss the implications of unblinding the full current dataset, as well as the prospects of the increasing data volume expected in the coming years, particularly in terms of sensitivity to various diffuse fluxes from theoretical predictions.

The Dainotti relation empirically connects the isotropic plateau luminosity ($L_X$) in gamma-ray bursts (GRBs) X-ray afterglows to the rest-frame time at which the plateau ends ($T_a^*$), enabling both the standardization of GRBs and their use as cosmological probes. However, the precise physical mechanisms underlying this correlation remain an active area of research. Although magnetars, highly magnetized neutron stars, have been proposed as central engines powering GRB afterglows, traditional dipole spin-down radiation models fail to account for the full diversity of observed behaviors. This limitation necessitates a more comprehensive framework. We propose that multipolar magnetic field emissions from magnetars offer a plausible explanation for the Dainotti relation. Unlike simple dipole fields, higher-order multipolar configurations enable more complex energy dissipation processes. The coexistence of multiple components can plausibly explain the range of afterglow decay indices found from a sample of 238 GRBs with plateau features from the Swift-XRT database up to the end of December 2024, the majority of which deviate from the dipolar prediction of $\alpha = -2$, and more crucially, the spin-down physics yields a link between $L_X$ and $T_a^*$ in a way that preserves the Dainotti correlation with a slope of $b = - 1$, independent of the specific multipole order. Moreover, we find that the inclusion of higher order multipoles can explain the range of plateau energies found in the Dainotti relations. Thus, a unified picture emerges in which multipolar fields are able to reproduce both the slope and the normalization of the correlation.

Central compact objects (CCOs) are a subclass of neutron stars with a dipole magnetic field strength considerably weaker than those of radio pulsars and magnetars. One possible explanation for such weak magnetic fields in the CCOs is the hidden magnetic field scenario, in which supernova fallback submerges the magnetosphere of a proto-neutron star beneath a newly formed crust. However, the fallback mass and timescale required for this submergence process remain uncertain. We perform one-dimensional general relativistic magnetohydrodynamic simulations of the supernova fallback onto a magnetized proto-neutron star, while considering neutrino cooling. In our simulations, the infalling material compresses the magnetic field and drives a strong shock. The shock initially expands outward, but eventually stalls and recedes as neutrino cooling becomes significant. After the shock stalls, the gas density above the magnetosphere increases rapidly, potentially leading to the formation of a new crust. To understand the shock dynamics, we develop semi-analytic models that describe the resulting magnetospheric and shock radii when the shock stalls. By comparing the fallback time scale with the shock stalling time scale, corresponding to the waiting time for the new crust formation, we derive a necessary condition for the submergence of the PNS magnetic field. Our results will provide guidance for investigating the diversity of young isolated neutron stars through multidimensional simulations.

The L 98-59 system, identified by TESS in 2019, features three transiting exoplanets in compact orbits of 2.253, 3.691, and 7.451 days around an M3V star, with an outer 12.83-day non-transiting planet confirmed in 2021 using ESPRESSO. The planets exhibit a diverse range of sizes (0.8-1.6 R$_{\oplus}$), masses (0.5-3 M$_{\oplus}$), and likely compositions (Earth-like to possibly water-rich), prompting atmospheric characterization studies with HST and JWST. Here, we analyze 16 new TESS sectors and improve radial velocity (RV) precision of archival ESPRESSO and HARPS data using a line-by-line framework, enabling stellar activity detrending via a novel differential temperature indicator. We refine the radii of L 98-59 b, c, and d to 0.837 $\pm$ 0.019 R$_{\oplus}$, 1.329 $\pm$ 0.029 R$_{\oplus}$, 1.627 $\pm$ 0.041 R$_{\oplus}$, respectively. Combining RVs with transit timing variations (TTV) of L 98-59 c and d from TESS and JWST provides unprecedented constraints on the masses and eccentricities of the planets. We report updated masses of 0.46 $\pm$ 0.11 M$_{\oplus}$ for b, 2.00 $\pm$ 0.13 M$_{\oplus}$ for c, and 1.64 $\pm$ 0.07 M$_{\oplus}$ for d, and a minimum mass of 2.82 $\pm$ 0.19 M$_{\oplus}$ for e. We additionally confirm L 98-59\,f, a non-transiting super-Earth with a minimal mass of 2.80 $\pm$ 0.30 M$_{\oplus}$ on a 23.06-day orbit inside the Habitable Zone. The TTVs of L 98-59 c and d (<3 min, $P_{\rm TTV} = 396$ days) constrain the eccentricities of all planets to near-circular orbits ($e \lesssim 0.04$). An internal structure analysis of the transiting planets reveals increasing water-mass fractions ($f_{\rm H_{2}O}$) with orbital distance, reaching $f_{\rm H_{2}O} \approx 0.16$ for L 98-59\ d. We predict eccentricity-induced tidal heating in L 98-59 b with heat fluxes comparable to those of Io, potentially driving volcanic activity.

The cosmological principle is a cornerstone of the standard cosmological model. However, recent observations suggest potential deviations from this assumption, hinting at a small anisotropic expansion. Such an expansion can arise from sources that break rotational invariance. A minimal realization of this scenario is described by a Bianchi I geometry, where each spatial direction evolves at a different rate, and the degree of anisotropy is quantified by the shear parameter $\Sigma$. In this work, we constrain the present-day value of the shear, $\Sigma_0$, by confronting theoretical predictions with recent cosmological data. We implement various anisotropic models within the Boltzmann code \texttt{CLASS} and explore their parameter space using the sampler \texttt{MontePython}. Although our results show that $\Sigma_0$ is model-dependent, notably, in one specific scenario considering a homogeneous scalar field coupled to a 2-form field, $\Sigma_0 = 0$ is excluded at the $2\sigma$ confidence level, with mean value around $|\Sigma_0| \sim 10^{-4}$ while remaining consistent with observations. These findings challenge the conventional assumption that cosmic shear is negligible in the present universe. Moreover, the anisotropic expansion in this model is driven by a steep scalar field potential, a feature often found in supergravity-inspired scenarios. While anisotropic models offer interesting alternatives and could help explain some cosmological anomalies, they generally introduce additional parameters, making the standard $\Lambda$CDM model statistically favored in most cases. Still, they remain compatible with current observations and provide new perspectives on features not fully explained within the standard framework. These results highlight the importance of further exploring anisotropic cosmologies to better understand their implications.

DG CVn is an eruptive variable star and represents the closest member of the known sample of complex periodic variables, or scallop-shell stars. Over the years, this M dwarf binary system has shown significant flaring activity at a wide range of frequencies. Here, we present a detailed analysis of $\sim 14$ hours of radio observations of this stellar system, taken with the Karl G.Jansky Very Large Array at band L, centered at 1.5 GHz. In both $7$-hour long observations, we have found a quiescent, weakly polarized component, that could be ascribable to the incoherent, gyro-synchrotron emission coming from the magnetosphere surrounding one or both stars, along with multiple $\sim90\%$ right-circularly polarized bursts, some of which last for a few minutes, while others being longer, $\gtrsim$ 30 minutes. Some of these bursts show a drift in frequency and time, possibly caused due to beaming effects or the motion of the plasma responsible for the emission. We assess the possible modulation of burst frequency with the primary and secondary periods, and discuss the properties of these bursts, favoring electron cyclotron maser over plasma emission as the likely underlying mechanism. We compare DG CVn's dynamic spectrum to other young M dwarfs and find many similarities. A dedicated proper radio/optical simultaneous follow-up is needed to monitor the long-term variability, increase the statistics of bursts, in order to test whether the co-rotating absorbers detected in optical can drive the observed radio emission, and whether the occurrence of radio bursts correlates with the rotational phase of either stars.

We present a systematic analysis of automatic differentiation (AD) applications in astrophysics, identifying domains where gradient-based optimization could provide significant computational advantages. Building on our previous work with GRAF (Gradient-based Radar Ambiguity Functions), which discovered optimal radar waveforms achieving 4x computational speedup by exploring the trade-off space between conflicting objectives, we extend this discovery-oriented approach to astrophysical parameter spaces. While AD has been successfully implemented in several areas including gravitational wave parameter estimation and exoplanet atmospheric retrieval, we identify nine astrophysical domains where, to our knowledge, gradient-based exploration methods remain unexplored despite favorable mathematical structure. These opportunities range from discovering novel solutions to the Einstein field equations in exotic spacetime configurations to systematically exploring parameter spaces in stellar astrophysics and planetary dynamics. We present the mathematical foundations for implementing AD in each domain and propose GRASP (Gradient-based Reconstruction of Astrophysical Systems & Phenomena), a unified framework for differentiable astrophysical computations that transforms traditional optimization problems into systematic exploration of solution spaces. To our knowledge, this is the first work to systematically delineate unexplored domains in astrophysics suitable for automatic differentiation and to provide a unified, mathematically grounded framework (GRASP) to guide their implementation.

We present new observations of the PDS 70 disc obtained with the Atacama Large Millimeter/sub-millimeter Array (ALMA) in Band 9 (671 GHz) at 0.242$^{\prime\prime}$ resolution, which provide valuable insights into the spatial distribution of sub-millimetre grains in the disc. The data reveal a ring-like morphology, with a radial peak located between those previously observed at infrared wavelengths and longer millimetre observations. Additionally, we detect a tentative outer shoulder in Band 9 that is not observed at longer wavelengths. These findings suggest that small grains ($\sim 100 \mu$m) traced by Band 9 may be escaping from the pressure bump both radially inwards and outwards, or may be tracing different disc layers than those probed at longer wavelengths. A multi-wavelength analysis of the disc at millimetre wavelengths and the best fit to the spectral energy distribution shows the presence of centimetre grains around the ring location, where the dust surface density also peaks, compatible with dust trap models. The grain size in the disc cavity is not well constrained but is consistent with grains as small as 10 $\mu$m, supporting the hypothesis that small dust grain filters through the cavity. We use dust evolution models to demonstrate that a turbulent viscosity of $\alpha \gtrsim 10^{-3}$ allows small grains to filter through the disc gap, while $\alpha \lesssim 5 \times 10^{-3}$ is required to retain large grains in the pressure bump. The Band 9 observations of PDS 70 validate theoretical models and confirm the presence of pebble flux through the disc gap.

We introduce MVPinn, a Physics-Informed Neural Network (PINN) approach tailored for solving the Milne-Eddington (ME) inversion problem, specifically applied to spectropolarimetric observations from the Big Bear Solar Observatory's Near-InfraRed Imaging Spectropolarimeter (BBSO/NIRIS) at the Fe I 1.56 {\mu}m lines. Traditional ME inversion methods, though widely used, are computationally intensive, sensitive to noise, and often struggle to accurately capture complex profile asymmetries resulting from gradients in magnetic field strength, orientation, and line-of-sight velocities. By embedding the ME radiative transfer equations directly into the neural network training as physics-informed constraints, our MVPinn method robustly and efficiently retrieves magnetic field parameters, significantly outperforming traditional inversion methods in accuracy, noise resilience, and the ability to handle asymmetric and weak polarization signals. After training, MVPinn infers one magnetogram in about 15 seconds, compared to tens of minutes required by traditional ME inversion on high-resolution spectropolarimetric data. Quantitative comparisons demonstrate excellent agreement with well-established magnetic field measurements from the SDO/HMI and Hinode/SOT-SP instruments, with correlation coefficients of approximately 90%. In particular, MVPINN aligns better with Hinode/SOT-SP data, indicating some saturation of HMI data at high magnetic strengths. We further analyze the physical significance of profile asymmetries and the limitations inherent in the ME model assumption. Our results illustrate the potential of physics-informed machine learning methods in high-spatial-temporal solar observations, preparing for more sophisticated, real-time magnetic field analysis essential for current and next-generation solar telescopes and space weather monitoring.

The orbital eccentricities of brown dwarfs encode valuable information of their formation and evolution history, providing insights into whether they resemble giant planets or stellar binaries. Here, we report the discovery of TOI-5575b, a long-period, massive brown dwarf orbiting a low-mass M5V star ($\rm 0.21\pm0.02\,M_\odot$) delivered by the TESS mission. The companion has a mass and radius of $\rm 72.4\pm4.1\,M_J$ and $\rm 0.84\pm0.07\,R_J$ on a 32-day moderately eccentric orbit ($e=0.187\pm0.002$), making it the third highest-mass-ratio transiting brown dwarf system known to date. Building on this discovery, we investigate the eccentricity distributions of a sample of transiting long-period ($10\leq P\lesssim 1000$ days, $\sim$0.1-1.5 AU) giant planets, brown dwarfs and low-mass stars. We find that brown dwarfs exhibit an eccentricity behavior nearly identical to that of giant planets: a preference for circular orbits with a long tail toward high eccentricities. Such a trend contrasts sharply with direct imaging findings, where cold (5-100 AU) brown dwarfs and giant planets display distinct eccentricity distributions. Our results suggest that transiting long-period brown dwarfs and giant planets probably 1) form in different routes at exterior orbits but undergo analogous dynamical evolution processes and migrate inwards; or 2) both contain two sub-groups, one with widely spread eccentricities while the other has circular orbits, that jointly sculpt the eccentricity distributions. The low-mass-star systems appear to be a distinctive population, showing a peak eccentricity at about 0.3, akin to more massive stellar binaries.

The origin of very metal-poor (VMP; [Fe/H] $\leq -2.0$) stars on planar orbits has been the subject of great attention since their first discovery. However, prior to the release of the Gaia BP/RP (XP) spectra, and large photometric samples such as SkyMapper, SAGES, J-PLUS and S-PLUS, most studies have been limited due to their small sample sizes or strong selection effects. Here, we cross-match photometric metallicities derived from Gaia XP synthetic photometry and geometric distances from Bailer-Jones et al., and select 12,000 VMP stars (1604 dwarfs and 10,396 giants) with available high-quality astrometry. After calculating dynamical parameter estimates using \texttt{AGAMA}, we employ the non-negative matrix factorization technique to the $v_\phi$ distribution across bins in $Z_{\rm max}$ (the maximum height above or below the Galactic plane during the stellar orbit). We find three primary populations of the selected VMP stars: halo, disk system, and the Gaia Sausage/Enceladus (GSE) structure. The fraction of disk-like stars decreases with increasing $Z_{\rm max}$ (as expected), although it is still $\sim 20$\% for stars with $Z_{\rm max}$ $\sim 3 $ kpc. Similar results emerge from the application of the Hayden criterion, which separates stellar populations on the basis of their orbital inclination angles relative to the Galactic plane. We argue that such high fractions of disk-like stars indicate that they are an independent component, rather than originating solely from Galactic building blocks or heating by minor mergers. We suggest that most of these VMP stars are members of the hypothesized ''primordial" disk.

Gravitational wave astronomy presents a promising opportunity to directly observe scalar-induced gravitational waves originating from the early universe. Future experiments, including ground-based interferometers like LIGO and Virgo, the Pulsar Timing Array, and telescopes such as FAST and SKA, are poised to significantly enhance sensitivity to these gravitational waves. In this paper, we combined Cosmic Microwave Background data with upper or lower limits of the stochastic gravitational wave background provided by FAST or SKA, to constrain scalar-induced gravitational waves. To provide a comprehensive forecast, we consider two scenarios: one where FAST or SKA does not detect scalar-induced gravitational waves, thereby setting an upper limit on the fractional energy density; and another where these waves are detected successfully, thus establishing a lower limit on the fractional energy density. In the $\Lambda$CDM+$r$ model, the scalar spectral index of the power-law power spectrum is constrained to $n_s=0.9589^{+0.0021}_{-0.0011}$ from the combinations of CMB+BAO+SKA datasets in the upper limit scenario. The constraint shifts to $n_s = 0.9661^{+0.0027}_{-0.0039}$ in the lower limit scenario. Comparing with the constraint from the combinations of CMB+BAO datasets, the scalar spectral index $n_s$ exhibits significant changes, which could serve as an indicator for detecting scalar-induced gravitational waves. In the $\Lambda$CDM+$\alpha_s$+$r$ model and the $\Lambda$CDM+$\alpha_s$+$\beta_s$+$r$ model, the running of the scalar spectral index $\alpha_s$ and the running of the running of the scalar spectral index $\beta_s$ also show notable variations, suggesting potential indicators. The numerical findings clearly demonstrate the impact of the upper and lower limits provided by FAST or SKA.

Active galactic nuclei (AGNs), among the universe's most luminous objects, radiate across the entire electromagnetic spectrum. They are powered by gravitational energy released from material feeding central supermassive black holes (SMBHs). However, current AGN theory remains largely phenomenological, relying on envisioned structures beyond accretion disks to produce broad optical emission lines (broad line regions, BLRs) and X-ray emission (corona). It struggles to explain accretion disk sizes, optical line diversity, BLR radial inflows/outflows, and crucially, rapid X-ray and optical variability (line width, line shape, inflow/outflow switch, emitting region) on timescales significantly shorter than disk accretion. Here we show that moderately eccentric flows around SMBHs-formed via circumnuclear gas accretion or tidal disruption events-generate eccentricity cascades in the BLRs (from 0.8 to 0.2 outwards), explaining multi-wavelength emission and variability. The flows' non-axisymmetric temperature structures explain dust sublimation asymmetries, different BLR components and their radial motions. The innermost BLR links to the SMBH vicinity through highly eccentric streams producing soft X-rays at periapsis. General relativistic precession further compresses these flows, generating a hard X-ray continuum near the SMBHs. Precession of the eccentric flow drives optical/X-ray variability, reproducing the observed X-ray power spectral density and occasional X-ray quasi-periodic eruptions. We thus propose eccentric accretion disks as a physical AGN model unifying the elusive BLRs and X-ray corona. This model enables detailed anatomy of AGNs and maximises their potential as cosmological standard candles.

The Giant Radio Array for Neutrino Detection (GRAND) is an envisioned observatory of ultra-high-energy particles of cosmic origin, with energies in excess of 100 PeV. GRAND uses large surface arrays of antennas to look for the radio emission from extensive air showers that are triggered by the interaction of ultra-high-energy cosmic rays, gamma rays, and neutrinos in the atmosphere or underground. In particular, for ultra-high-energy neutrinos, the future final phase of GRAND aims to be sensitive enough to detect them in spite of their plausibly tiny flux. Three prototype GRAND radio arrays have been in operation since 2023: GRANDProto300, in China, GRAND@Auger, in Argentina, and GRAND@Nan\c{c}ay, in France. Their goals are to field-test the GRAND detection units, understand the radio background to which they are exposed, and develop tools for diagnostic, data gathering, and data analysis. This list of contributions to the 39th International Cosmic Ray Conference (ICRC 2025) presents an overview of GRAND, in its present and future incarnations, and a first look at data collected by GRANDProto300 and GRAND@Auger, including the first cosmic-ray candidates detected by them.

We present the main-sequence binary (MSMS) Catalog derived from Gaia Data Release 3 BP/RP (XP) spectra. Leveraging the vast sample of low-resolution Gaia XP spectra, we develop a forward modeling approach that maps stellar mass and photometric metallicity to XP spectra using a neural network. Our methodology identifies binary systems through statistical comparison of single- and binary-star model fits, enabling detection of binaries with mass ratios between 0.4 and 1.0 and flux ratios larger than 0.1. From an initial sample of 35 million stars within 1 kpc, we identify 14 million binary candidates and define a high-confidence "golden sample" of 1 million binary systems. This large, homogeneous sample enables detailed statistical analysis of binary properties across diverse Galactic environments, providing new insights into binary star formation and evolution. In addition, the $\chi^2$ comparison allows us to distinguish stars with luminous companions from single stars or binaries with dark companions, such as white dwarfs, neutron stars and black hole candidates, improving our understanding of compact object populations.

Neutrinos can experience fast flavor conversions (FFCs) in highly dense astrophysical environments, such as core-collapse supernovae and neutron star mergers, potentially affecting energy transport and other processes. The simulation of fast flavor conversions under realistic astrophysical conditions requires substantial computational resources and involves significant analytical challenges. While machine learning methods like Multilayer Perceptrons have been used to accurately predict the asymptotic outcomes of FFCs, their 'black-box' nature limits the extraction of direct physical insight. To address this limitation, we employ two distinct interpretable machine learning frameworks-Kolmogorov-Arnold Networks (KANs) and Sparse Identification of Nonlinear Dynamics (SINDy)-to derive physically insightful models from a FFC simulation dataset. Our analysis reveals a fundamental trade-off between predictive accuracy and model simplicity. The KANs demonstrates high fidelity in reconstructing post-conversion neutrino energy spectra, achieving accuracies of up to $90\%$. In contrast, SINDy uncovers a remarkably concise, low-rank set of governing equations, offering maximum interpretability but with lower predictive accuracy. Critically, by analyzing the interpretable model, we identify the number density of heavy-lepton neutrinos as the most dominant factor in the system's evolution. Ultimately, this work provides a methodological framework for interpretable machine learning that supports genuine data-driven physical discovery in astronomy and astrophysics, going beyond prediction alone.

Context: In a recent publication, we established a close relationship between light-curve asymmetries in Mira variables and indicators of their dust mass-loss rate. The light-curve asymmetries appear to be related to the stars' third dredge-up (3DUP) activity. Aims: We aim to reveal the evolutionary status of M-type Miras with light-curve asymmetries ('bumps') within the spectral sequence M -- S -- C, determine their mass-loss properties, and check possible evolutionary scenarios. Methods: We analysed a sample of 3100 Miras collected from the ASAS database, distinguishing between symmetric and asymmetric light curves. We determined their periods, luminosity functions, and period-luminosity relations, their locations relative to the Galactic midplane, as well as mass-loss rate indicators through the 2MASS-WISE colours and the Gaia-2MASS diagram. Results: The M-type Miras with symmetric light curves are generally found to have shorter periods, lower luminosities, a larger average distance to the Galactic midplane, and lower initial masses than the M-type Miras with asymmetries. In addition, 25 Miras are proposed as candidates for new carbon stars. Conclusions: We propose that the M-type Miras have two distinct populations: M-type Miras with symmetric light curves, which have lower initial mass progenitors than M-type Miras with asymmetries, which show signs of 3DUP activity and are the link to the S-type Miras.

We investigate the circumstances which allow a black hole to remain put at the galactic centre when the stellar core is anisotropic. We use N-body calculations to study the response of stellar orbit families embedded in a larger, isotropic isochrone (H\'enon) background potential. When the BH orbits in an odd f[E,Lz] velocity distribution function, they transfer angular momentum to it. We call this dynamical traction: it takes place whenever the kinetic energy drawn from f[E,Lz] has an excess of streaming motion over its (isotropic) v-dispersion. For a dynamically cold disc, the outcome depends on both the orbit of the BH and that of a Jeans-unstable stellar sub-structures. When the stellar clumps have much binding energy, a BH may scatter off of them after they formed. In the process the BH may be dislodged from the centre and migrate outward due to dynamical traction. When the stellar clumps are less bound, they may still migrate to the centre where they either dissolve or merge with the BH. The final configuration is similar to a nuclear star cluster which may yet be moving at ~10 km/s wrt the barycentre. The angular momentum transferred to a BH by dynamical traction delays the migration to the galactic centre by several hundred million years. The efficiency of angular momentum transfer is a strong function of the fragmented (cold) state of the stellar space density. In a dynamically cold environment, a BH is removed from the central region through a two-stage orbital migration instability. A criterion against this instability is proposed in the form of a threshold in isotropic velocity dispersion compared to streaming motion. For a BH to settle at the heart of a galaxy on time-scales of ~ 300 Myr or less requires that a large fraction of Lz be dissipated, or, alternatively, that the BH grows in situ in an isotropic environment devoid of sub-structures.

The outer Galaxy presents a distinctive environment for investigating star formation. This study develops a novel approach to identify true cluster members based on unsupervised clustering using astrometry with significant uncertainties. As a proof of concept, we analyze three outer Galactic Young Stellar Object (YSO) clusters at different distances and densities within 65 < l < 265 degrees, each known to contain >100 members based on the Star Formation in Outer Galaxy catalog. The 618 YSO clusters in the SFOG dataset were based on 2-dimensional clustering. In this contribution, we apply the HDBSCAN* algorithm to the precise Gaia DR3 astrometry to assign YSO cluster membership. Monte Carlo simulation, coupled with HDBSCAN* (HDBSCAN-MC algorithm), addresses YSO astrometric uncertainties while 5-dimensional clustering. We introduce the Generation Of cLuster anD FIeld STar (GOLDFIST) simulation, to enable robust membership determination, performing an unsupervised clustering analysis in higher-dimensional feature space while accommodating measurement errors. In this study, we extended our approach to distant outer galaxy YSOs and clusters with larger astrometric uncertainties. The results include the discovery of new members in the previously identified clusters. We also analyze the known stars in the clusters and confirm their membership. The derived membership probabilities are included in the provided cluster catalogs. The more accurately predicted simulation distance estimates closely agree, within uncertainty limits, with the median distance estimates derived from Gaia data, and are compared with the kinematic distances from the WISE HII survey.

In January of 1985, more than 40 years ago, a group of astronomers met with NASA officials to map out the future of NASA space astronomy. Their efforts led to the Great Observatories program, linking four powerful space telescopes to study the heavens in four regions of the spectrum. The successful launch and operation of the Spitzer Space Telescope in the Fall of 2003 completed the launch of the Great Observatories, almost 20 years after the program was formulated, and two of the Observatories, Hubble and Chandra, continue to operate very productively. The scientific and public education results of the Great Observatories are well-known. Here we emphasize that fulfilling the extraordinary vision of the Great Observatories was a triumph of human ingenuity, dedication, and determination.

We reanalyze the chemical composition of the metal-poorest tail of the Galactic halo using highly accurate atmospheric parameters Giribaldi et al. (2021, 2023) and cutting-edge 3D NLTE models Amarsi et al (2018). Most [Mg/Fe] versus [Fe/H] diagrams in the literature exhibit significant scatter at [Fe/H] $\lesssim -2$ dex, often interpreted as evidence of inhomogeneous enrichment during the early phases of galaxy evolution Rossi et al. (2021). However, our analysis of observational data reveals that in the range $-3.5 <$ [Fe/H] $< -2$ dex, the [Mg/Fe] versus [Fe/H] distribution is relatively narrow. This finding suggests a low degree of stochastic enrichment in magnesium during these epochs in the Milky Way halo.

Measuring the autocorrelation of galaxy shapes, the so-called intrinsic-intrinsic (II) correlation is important for both cosmology and understanding the formation of massive elliptical galaxies. However, such measurements are significantly more challenging than the cross-correlation with galaxy density (GI correlation) due to the much lower signal-to-noise ratio. In this paper, we report the first observational evidence for large-scale intrinsic alignments measured from the ellipticity autocorrelations, extending out to $100\,h^{-1}\,{\rm Mpc}$. From SDSS and SDSS-III BOSS, we analyze over the redshift range $0.16\leq z\leq 0.70$ luminous red galaxies (LRG), LOWZ and CMASS galaxy samples, the latter two of which are cross-matched with high-quality DESI imaging data. By expanding one of the two II correlation functions, II($-$), in terms of the associated Legendre polynomials, we effectively isolate the line-of-sight projection effects and enhance the signal. The resulting correlation for all three samples exhibits a clear power-law form. We also show that combining the two II correlations, II($+$) and II($-$), increases the detection significance by $\sim 10\%$, though they appear equivalent mathematically under the linear alignment model. Importantly, this measurement opens a new observational window for probing signals uniquely encoded in shape autocorrelations, such as tensor perturbations from the gravitational waves. This analysis establishes a practical framework for probing such effects.

Nuclear rings are long-lived structures, allowing the molecular gas inside to become sufficiently dense to initiate star formation. This makes them a crucial element in the study of secular evolution. However, the morphology of nuclear rings, and their potential correlations with that of the galactic hosts, remains an open subject. We examine 52 star-forming nuclear rings from the Atlas of Images of NUclear Rings (AINUR) and correlate the overall galaxy morphology, in particular non-axisymmetric features, with the morphology of the nuclear ring. We define three different classes of nuclear rings: two-armed rings dominated by two dust lanes, twoarms+ rings crowded with secondary dust lanes in addition to the two main ones, and many-armed rings with multiple armlets of similar prevalence. We employ unsharp-masked Hubble Space Telescope images to study the structure of nuclear rings. We find that two-armed rings are more common in early-type grand design galaxies with strong bars. Twoarms+ rings are related to later-type and more weakly barred galaxies, both grand design and multi-armed. Lastly, many-armed rings are typically associated with later-type flocculent and multi-armed galaxies with the weakest bars. In addition, we examine the regions inside the nuclear rings and observe nuclear spirals in 28 galaxies ( 90 % of those galaxies for which the interior of the nuclear ring is resolved). We conclude that the global morphology of the host galaxy and, more precisely, the presence and properties of a bar play a fundamental role in determining the morphology of the nuclear ring and the nuclear region. We suggest that two-armed rings are associated with a 180deg structure forced by a strong bar, many-armed rings are associated with a very weak or absent 180deg structure, and twoarms+ rings are found in intermediate cases.

The IceCube Neutrino Observatory has observed a sample of high purity, primarily atmospheric, muon neutrino events over 11 years from all directions below the horizon, spanning the energy range 500 GeV to 100 TeV. While this sample was initially used for an eV-scale sterile neutrino search, its purity and spanned parameter space can also be used to perform an earth tomography. This flux of neutrinos traverses the earth and is attenuated in varying amounts depending on the energy and traversed column density of the event. By parameterizing the earth as multiple constant--density shells, IceCube can measure the upgoing neutrino flux as a function of the declination, yielding an inference of the density of each shell. In this talk, the latest sensitivities of this analysis and comparisons with the previous measurement are presented. In addition, the analysis procedure, details about the data sample, and systematic effects are also explained. This analysis is one of the latest, weak-force driven, non-gravitational, measurements of the earth's density and mass.

Understanding where elements were formed has been a key goal in astrophysics for nearly a century, with answers involving cosmology, stellar burning, and cosmic explosions. Since 1957, the origin of the heaviest elements (formed via the rapid neutron capture process; r-process) has remained a mystery, identified as a key question to answer this century by the US National Research Council. With the advent of gravitational wave astronomy and recent measurements by the James Webb Space Telescope we now know that neutron star mergers are a key site of heavy element nucleosynthesis. We must now understand the heavy element yield of these events as well as mapping when these mergers occurred back through cosmic time, currently thought to peak when the universe was half its current age. This requires an extremely sensitive ultraviolet, optical, and infrared telescope which can respond rapidly to external discoveries of neutron star mergers. We here describe how the Habitable Worlds Observatory can provide the first complete answer to one of the questions of the century.

Cosmological N-body simulations are among the primary tools for studying structure formation in the Universe. Analyses of these simulations critically depend on accurately identifying and tracking dark matter subhalos over time. In recent years, several new algorithms have been developed to improve the accuracy and consistency of subhalo tracking in cold dark matter simulations. These algorithms should be revisited in the context of new physics beyond gravity, which can modify the evolution and final properties of subhalo populations. In this work, we apply the particle-tracking-based subhalo finder Symfind to velocity-dependent self-interacting dark matter simulations with large cross section amplitudes to assess the performance of particle-tracking methods beyond the CDM paradigm. We find that the core-particle-tracking technique, which is key to the success of these algorithms in CDM, does not always yield accurate results in SIDM. The interplay between dark matter self-interactions and tidal stripping can cause the diffusion of core particles to larger radii, leading particle-tracking-based algorithms to prematurely lose track of SIDM subhalos. For massive core-expansion subhalos and core-collapse subhalos that experience close or repeated pericentric passages, a significant fraction of core particles can be lost, and particle-tracking-based finders such as Symfind offer no clear advantage over traditional methods that rely on identifying phase-space overdensities. On the other hand, for subhalos with large pericentric distances or fewer, more distant passages, Symfind tends to outperform. These differences depend sensitively on the cross section amplitude and turnover velocity of the underlying SIDM model. We therefore recommend a hybrid approach that leverages the strengths of both techniques to produce complete and robust catalogs of core-expansion and core-collapse SIDM subhalos.

The combined data of Fluorescence and Surface Detectors of the Pierre Auger Observatory has recently provided the strongest constraints on the validity of predictions from current models of hadronic interactions. The unmodified predictions of these models on the depth of shower maximum ($X_\text{max}$) and the hadronic part of the ground signal are unable to accurately describe the measured data at a level of more than 5$\sigma$ in the energy range 3-10 EeV. This inconsistency has been shown to originate not only from the predicted amount of muons at the ground level, but also from the predicted scale of $X_\text{max}$, which must be adjusted to better match the observed data. The resulting deeper $X_\text{max}$ scales of the models imply a heavier mass composition to be interpreted from the $X_\text{max}$ measurements. We show the results of the test with an updated data set of the Pierre Auger Observatory, studying also the energy evolution of the fitted modification parameters and new versions of the models of hadronic interactions. Additionally, we discuss the phenomenological consequences of the deeper $X_\text{max}$ scale of models on the interpretation of the features of the energy spectrum and the muon problem in air-shower modelling.

The VERITAS observatory, located in southern Arizona, is engaged in an exploration of the gamma-ray sky at energies above 85 GeV. Observations of Galactic and extragalactic sources in the TeV band provide clues to the highly energetic processes occurring in these objects, and could provide indirect evidence for the origin of cosmic rays and the sites of particle acceleration in the Universe. In this chapter, we describe the VERITAS telescopes and their operation, as well as analysis procedures, and present results from scientific observations, which include extragalactic science, Galactic physics, and studies of fundamental physics and cosmology.

The dust-to-gas ratio in the protoplanetary disk, which is likely imprinted into the host star metallicity, is a property that plays a crucial role during planet formation. We aim at constraining planet formation and evolution processes by statistically analysing planetary systems generated by the Generation III Bern model, comparing with the correlations derived from observational samples. Using synthetic planets biased to observational completeness, we find that (1) the occurrence rates of large giant planets and Neptune-size planets are positively correlated with [Fe/H], while small sub-Earths exhibit an anti-correlation. In between, for sub-Neptune and super-Earth, the occurrence rate first increases and then decreases with increasing [Fe/H] with an inflection point at 0.1 dex. (2) Planets with orbital periods shorter than ten days are more likely to be found around stars with higher metallicity, and this tendency weakens with increasing planet radius. (3) Both giant planets and small planets exhibit a positive correlation between the eccentricity and [Fe/H], which could be explained by the self-excitation and perturbation of outer giant planets. (4) The radius valley deepens and becomes more prominent with increasing [Fe/H], accompanied by a lower super-Earth-to-sub-Neptune ratio. Furthermore, the average radius of the planets above the valley increases with [Fe/H]. Our nominal model successfully reproduces many observed correlations with stellar metallicity, supporting the description of physical processes and parameters included in the Bern model. However, the dependences of orbital eccentricity and period on [Fe/H] predicted by the synthetic population is however significantly weaker than observed. This discrepancy suggests that long-term dynamical interactions between planets, along with the impact of binaries/companions, can drive the system towards a dynamically hotter state.

We determine magnetic fields from the photosphere to the upper chromosphere combining data from the Hinode satellite and the CLASP2.1 sounding rocket experiment. CLASP2.1 provided polarization profiles of the Mg~{|sc ii} $h$ and $k$ lines, as well as of the Mn~{|sc i} lines around 2800~{|AA}, across various magnetic structures in an active region, containing a plage, a pore, and the edges of a sunspot penumbra. By applying the Weak-Field Approximation (WFA) to the circular polarization profiles of these spectral lines, we obtain a longitudinal magnetic field map at three different heights in the chromosphere (lower, middle, and upper). This is complemented by data from Hinode (photospheric magnetic field), IRIS, and SDO (high-spatial-resolution observations of the chromosphere and corona). We quantify the height expansion of the plage magnetic fields and find that the magnetic fields expand significantly in the middle chromosphere, shaping the moss observed above in the transition region and corona. We identified an area with polarity reversal at the upper chromosphere around the edge of the pore, suggesting the presence of a magnetic discontinuity in the upper chromosphere. Transient and recurrent jet-like events are observed in this region, likely driven by magnetic reconnection. Around the penumbral edge, we find large-scale magnetic fields corresponding to the superpenumbral fibrils seen in the upper chromosphere. In the superpenumbral fibrils, we find Zeeman-induced linear polarization signals, suggesting the presence of a significantly inclined magnetic field, as strong as 1000~G in the upper chromosphere.

The central engine of gamma-ray burst is considered. Blandford-Znajek (BZ) process is reconsidered under the asymtotic magnetic condition ${\bf B}=B_0\hat{z}$ (rotation axis) at $r\gg r_H$. Another scenario of $\nu \overline{\nu} \to e^+ e^-$ driven jet are combined to BZ process to compliment it.

Magnetic reconnection and Magnetohydrodynamic (MHD) waves may well be both playing a role in coronal heating. In this paper, we simulate reconnection in the corona as a response to the convergence of opposite-polarity magnetic sources at the base of the corona. A current sheet forms at a magnetic null and undergoes impulsive bursty reconnection which drives natural modes of oscillation of the current sheet by a process of symbiosis. These are leaky surface sausage modes which cause the length of the current sheet to oscillate. Interaction of the oscillations and reconnection outflows with the magnetic Y-points at the ends of the sheet acts as sources for magnetoacoustic waves. Fast-mode waves propagate outwards into the coronal environment, while slow-mode waves propagate along the separatrices extending from the ends of the current sheet. The periodicities for sausage oscillations of the current sheet, for the current sheet length, and for the propagating large-scale magnetoacoustic waves are all estimated to be approximately 91 s for the parameters of our experiment.

Context. The evolution of massive star-forming clumps that are progenitors of high-mass young stellar objects are often classified based on a variety of observational indicators ranging from near-IR to radio wavelengths. Among them, the ratio between the bolometric luminosity and the mass of their envelope, $L/M$, has been observationally diagnosed as a good indicator for the evolutionary classification of parsec-scale star-forming clumps in the Galaxy. Aims. We have developed the Rosetta Stone project$\unicode{x2013}$an end-to-end framework designed to enable an accurate comparison between simulations and observations for investigating the formation and evolution of massive clumps. In this study, we calibrate the $L/M$ indicator in relation to the star formation efficiency (SFE) and the clump age, as derived from our suite of simulations. Methods. We perform multi-wavelength radiative transfer post-processing of RMHD simulations of the collapse of star-forming clumps fragmenting into protostars. We generate synthetic observations to obtain far-infrared emission from $70$ to $500\ \mu$m, as was done in the Hi-GAL survey and at $24\ \mu$m in the MIPSGAL survey, which are then used to build the spectral energy distributions (SEDs) and estimate the $L/M$ parameter. An additional $1.3$ mm wavelength in ALMA Band 6 has also been produced for the comparison with observational data. We have applied observational techniques, commonly employed by observers, to the synthetic data, in order to derive the corresponding physical parameters. Results. We find a correlation between $L/M$ and the SFE, with a power-law form $L/M\propto {\rm SFE}^{1.20^{+0.02}_{-0.03}}$. This correlation is independent of the mass of the clumps and the choice of initial conditions of the simulations in which they formed. (Abridged)

Lensing studies are typically carried out around high density regions, such as groups and clusters, where the lensing signals are significant and indicative of rich density structures. However, a more comprehensive test of the cosmological model should also include the lensing effect in low density regions. In this work, we incorporate the stacked weak lensing signals around the low density positions, alongside galaxy-galaxy lensing and galaxy-galaxy two point correlation function to perform a joint cosmological analysis on $\sigma_8$. The low density positions are constructed from the DR9 data release of the DESI legacy imaging survey, using galaxies with r-band absolute magnitude cut M$<$-21.5 and in the redshift range of 0.18$<$z$<$0.28. In doing so, we simultaneously parameterize photometric redshift errors and halo mass uncertainties while building mock catalogs from simulations using the method of SubHalo Abundance Matching (SHAM). For the weak lensing measurements, we use the shear estimators derived from the DECaLS DR8 imaging data, processed by the Fourier\_Quad pipeline. The survey boundaries and masks are fully taken into account. Our analysis achieves a total significance of $31.1\sigma$ detection for lensing in the low density positions, which significantly improve the $\sigma_8$ constraint compared to galaxy-galaxy lensing and galaxy-galaxy two point correlation function by 14$\%$. For flat $\Lambda$CDM model, we constrain $\sigma_8$ =$0.824^{+0.015}_{-0.015}$, which shows a good agreement with the PLANCK result. Additionally, the halo mass uncertainty $\sigma_{\lg M}$ and photometric redshift error $\sigma_z$ are constrained to be $0.565^{+0.086}_{-0.070}$ and $0.004^{+0.004}_{-0.003}$ respectively, which are somewhat different from our expectations due to the significant degeneracy of the two parameters.

Massive protoclusters at z~1.5-4, the peak of the cosmic star formation history, are key to understanding the formation mechanisms of massive galaxies in today's clusters. However, studies of protoclusters at these high redshifts remain limited, primarily due to small sample sizes and heterogeneous selection criteria. In this work, we conduct a systematic investigation of the star formation and cold gas properties of member galaxies of eight massive protoclusters in the COSMOS field, using the statistical and homogeneously selected sample from the Noema formIng Cluster survEy (NICE). Our analysis reveals a steep increase in the star formation rates per halo mass ($\Sigma_{\rm SFR} /M_{\rm halo}$) with redshifts in these intensively star-forming protoclusters, reaching values one to two orders of magnitude higher than those observed in the field at z>2. We further show that, instead of an enhancement of starbursts, this increase is largely driven by the concentration of massive and gas-rich star-forming galaxies in the protocluster cores. The member galaxies still generally follow the same star formation main sequence as in the field, with a moderate enhancement at the low mass end. Notably, the most massive protocluster galaxies ($M_{\rm halo}$>8$\times$10$^{10}$M$_\odot$) exhibit higher $f_{\rm gas}$ and $\tau_{\rm gas}$ than their field counterparts, while remaining on the star forming main sequence. These gas-rich, massive, and star-forming galaxies are predominantly concentrated in the protocluster cores and are likely progenitors of massive ellipticals in the center of today's clusters. These results suggest that the formation of massive galaxies in such environments is sustained by substantial gas reservoirs, which support persistent star formation and drive early mass assembly in forming cluster cores.

We present 3D hydrodynamical modelling of supernova-induced binary-interaction-powered supernovae; a scenario proposed for the peculiar type Ic supernova SN2022jli. In this scenario, supernova ejecta of a stripped-envelope star impacts a close-by stellar companion, temporarily inflating the envelope. The expanded envelope engulfs the neutron star, causing strong mass accretion at super-Eddington rates. Feedback from the accretion powers the supernova light curve with periodic undulations. Our simulations capture key features of SN2022jli, both the overall decline and the superimposed undulations of the light curve. Based on our parameter study, we find that (i) the accretion feedback should be sufficiently geometrically confined and the eccentricity of the post-supernova binary orbit should be $0.7\lesssim e\lesssim0.9$ to sustain a high accretion rate, and (ii) the viewing angle should be close to edge-on to match the low undulation amplitude ($\Delta L/L\sim0.1$) of SN2022jli. Different combinations of parameters could account for other supernovae like SN2022mop, SN2009ip and SN2015ap. We also discuss possible explanations for other key features of SN2022jli such as the $\gamma$-ray detection at $\sim200~\mathrm{d}$ and the rapid optical drop at $\sim250~\mathrm{d}$. Finally, we speculate on the future evolution of the system and its relation to existing neutron star binaries.

Analyses by the Dark Energy Spectroscopic Instrument (DESI) collaboration suggest a significant deviation from the $\Lambda$CDM model when their baryon acoustic oscillation (BAO) measurements are combined with Planck cosmic microwave background (CMB) data and various Type Ia supernova (SNIa) samples. In this work, we systematically investigate the origin of the deviations from the $\Lambda$CDM reported in recent cosmological analyses by combining different CMB datasets, BAO measurements, and DESY5 SNIa samples within the $w_0w_a$CDM framework. We find that the DESY5 SNIa sample, particularly its low-redshift component (DES-lowz), the Planck CMB data, the lensing measurements of Planck and ACT-DR6, and the DESI-DR2 BAO measurements contribute most significantly to the observed tensions. In contrast, combinations involving DES-SN, WMAP, SPT, and ACT-DR6 remain consistent with $\Lambda$CDM within $\sim1\sigma$. Our results highlight the critical impact of SNIa systematics, CMB data, and the choice of BAO dataset on constraints of dynamical dark energy models. These findings underscore the importance of improved calibration, homogeneity, and cross-validation of observational datasets to robustly assess potential deviations from the standard cosmological model.

The possible occurrence of a first-order hadron-quark phase transition (FOPT) in neutron-star interiors remains an open question. Whether such a transition can be directly tested with improved observations is a key challenge. Here, we incorporate the latest constraints, especially a new NICER radius measurement for PSR J0614--3329, into a nonparametric Gaussian Process (GP) EOS framework that explicitly includes a first-order transition. We find a Bayes factor of $B\approx2.3$ when comparing models with and without an explicit phase transition, marginally favoring its presence. At $68\%$ credibility, the transition onset density $n_{\rm PT}$ is either below $2\,n_s$ (corresponding to masses $\lesssim1\,M_\odot$, with density jump $\Delta n\sim0.5\,n_s$) or, more prominently, above $4\,n_s$ (near the central density of the heaviest NS, with $\Delta n\sim3\,n_s$), where $n_s$ represents the nuclear saturation density. In addition, by using symmetry-energy expansion at low densities ($<1.1\,n_s$), we infer a slope parameter $L=40.2^{+19.3}_{-14.3}$ MeV, in good agreement with nuclear-experiment values. Intriguingly, $L$ correlates positively with the radius difference between $1.4\,M_\odot$ and $2.0\,M_\odot$ stars.

Parametric instability of Alfv\'en wave packets with monochromatic carrier wave in low-$\beta$ plasma is studied using one-dimensional magnetohydrodynamic simulations. The results show spatial growth of incoming perturbations as they propagate through the mother wave. For sufficiently short packets, the perturbations emerge downstream of the packet as small-amplitude reverse Alfv\'en waves and forward slow magnetosonic waves. For larger packets the perturbations reach non-linear amplitude while still inside the mother wave. In this case, a downstream section of the mother wave collapses but the remaining upstream section stays largely intact and enters the phase of very slow evolution. The length scale separating the linear and non-linear regimes, as well as determining the size of the surviving section in the non-linear regime, is set by the Alfv\'en crossing time of the packet, the growth rate of the parametric instability for the unmodulated carrier wave, and the amplitude of incoming perturbations. The results are discussed in connection with the physics of solar wind.

Active galactic nucleus (AGN) disk provide dense environments to influence on the star formation, evolution, and migration. In AGN disks, pressure gradients and migration accelerations could create the anisotropy of the core-collapse supernovae (CCSNe) when the massive stars explode at the end of their lives. In this study, we construct the equilibrium equations by considering the above two factors and then compute the light curves for three types of progenitor stars at different locations of AGN disks for the different supermassive black hole (SMBH) masses, accretion efficiencies, explosion energies, and masses of ejecta. The results show that the migration acceleration has more significant effects on the anisotropic explosions than the pressure gradients of the AGN disks. The anisotropic luminosities are pronounced at large radii, and massive SMBHs would suppress the anisotropy and reduce the total luminosity.

A simple, fully connected neural network with a single hidden layer is used to estimate stellar masses for star-forming galaxies. The model is trained on broad-band photometry - from far-ultraviolet to mid-infrared wavelengths - generated by the Semi-Analytic Model of galaxy formation (SHARK), along with derived colour indices. It accurately reproduces the known SHARK stellar masses with respective root-mean-square and median errors of only 0.085 and 0.1 dex over the three decades in stellar mass. Analysis of the trained network's parameters reveals several colour indices to be particularly effective predictors of stellar mass. In particular, the FUV - NUV colour emerges as a strong determinant, suggesting that the network has implicitly learned to account for attenuation effects in the ultraviolet bands, thereby increasing the diagnostic power of this index. Traditional methods such as spectral energy distribution fitting, though widely used, are often complex, computationally expensive, and sensitive to model assumptions and parameter degeneracies. In contrast, the neural network relies solely on easily obtained observables, enabling rapid and accurate stellar mass predictions at minimal computational cost. The model derives its predictions exclusively from patterns learned in the data, without any built-in physical assumptions (such as stellar initial mass function). These results demonstrate the utility of this study's machine learning approach in astrophysical parameter estimation and highlight its potential to complement conventional techniques in upcoming large galaxy surveys.

The Spectrum-Roentgen-Gamma (SRG) observatory continues to operate successfully in orbit at the Lagrange point L2. The Mikhail Pavlinsky ART-XC telescope has demonstrated high efficiency in conducting X-ray surveys both over large sky regions and the entire celestial sphere. A recently published source catalog, based on data from the first four and partially completed fifth sky scans, contains 1,545 objects detected in the 4-12 keV energy range. In this work, using the same sky survey data, we assess the sensitivity to point source detection across the celestial sphere based on X-ray aperture photometry - that is, we calculate the upper flux limit in the 4-12 keV band at any given significance level. The method is implemented using both Poisson statistics and Bayesian inference, with consistent results between the two approaches. This information is important for studying variable and transient X-ray sources, as well as sources that are not detected with sufficient statistical significance in the ART-XC all-sky survey. The ART-XC upper limit service is available at https://www.srg.cosmos.ru/uplim.

The role of magnetic fields in the formation of dense filamentary structures in molecular clouds is critical for understanding the star formation process. The Snake filament in or close to the Pipe Nebula s neighboring, a prominent example of such structures, offers an ideal environment to study the interplay between magnetic fields and gas dynamics in the early stages of star formation. This study aims to investigate how magnetic fields influence the structure and dynamics of the Snake filament, using both polarization data and molecular line observations. Our goal is to understand the role of magnetic fields in shaping the filamentary structure and explore the kinematics within the filament. We conducted polarization observations in the optical and near-infrared bands using the 1.6 m and 60 cm telescopes at the Observatorio do Pico dos Dias/Laboratorio Nacional de Astrof\isica (OPD/LNA). Molecular line observations of the C18O and 13CO lines were obtained using the IRAM 30m telescope. We analyzed the data to characterize polarization and gas properties within the filament, with a focus on understanding the magnetic field orientation and its relationship with the filament s structure. Our findings reveal that the polarization vectors align with the filament s spine, indicating a magnetic field structure that is predominantly parallel to the filament at lower-density regions. A velocity gradient along the filament is observed in both C18O and 13CO lines, with C18O tracing the denser regions of the gas. The polarization efficiency decreases with increasing visual extinction, consistent with reduced grain alignment in higher-density regions. The filament s mass-to-length ratio is below the critical value required for gravitational collapse, indicating stability.

This paper focuses on extending the use of Minkowski Tensors to analyze anisotropic signals in cosmological data, focusing on those introduced by redshift space distortion. We derive the ensemble average of the two translation-invariant, rank-2 Minkowski Tensors for a matter density field that is perturbatively non-Gaussian in redshift space. This is achieved through the Edgeworth expansion of the joint probability density function of the field and its derivatives, expressing the ensemble averages in terms of cumulants up to cubic order. Our goal is to connect these theoretical predictions to the underlying cosmological parameters, allowing for parameter estimation by measuring them from galaxy surveys. The work builds on previous analyses of Minkowski Functionals in both real and redshift space and addresses the effects of Finger-of-God velocity dispersion and shot noise. We validate our predictions by matching them to measurements of the Minkowski Tensors from dark matter simulation data, finding that perturbation theory is a qualified success. Non-perturbative Finger-of-God effects remain significant at relatively large scales (R< 20 Mpc/h) and are particularly pronounced in the components parallel to the line of sight.

The mass discrepancy problem, observed in high-mass stars within eclipsing binaries, highlights systematic differences between dynamical and evolutionary mass estimates, challenging the accuracy of stellar evolution models. We aim to determine whether analysis methods directly contribute to this discrepancy and to assess how methodological improvements might reduce or clarify it. To address this, we developed a new self-contained framework that simultaneously models the photometric and spectroscopic data, minimising biases introduced by traditional iterative approaches and enabling consistent parameter optimisation. We present this framework alongside validation tests on synthetic data and demonstrate its application to three well-studied observed binaries, including one system known for its pronounced mass discrepancy. The framework recovers multiple viable solutions from distinct local minima, including one that reduces the mass discrepancy. These results illustrate how methodological biases, rather than evolutionary model assumptions, can contribute to the mass discrepancy problem. We further highlight that external constraints, such as independent distance estimates or evolutionary models, may be necessary to distinguish between degenerate solutions. Expanding this analysis to a larger sample will provide a more complete understanding, with forthcoming results in the next paper in this series.

We present a comprehensive comparative analysis of three pivotal epochs in cosmic history: structure formation, recombination, and matter-radiation equality, within the framework of $f(R, L_m)$ gravity and the standard $\Lambda$CDM cosmology. Using a nonlinear evolution equation for density perturbations, we determine the collapse redshift ($z_c$), showing that cosmic structures form earlier in $f(R, L_m)$ gravity due to enhanced effective gravitational coupling. Recombination is studied via the visibility function $g(z)$, peaking at $z_{\mathrm{rec}} \approx 1092.6$ in both models, consistent with Planck 2018 data. We compute the full width at half maximum (FWHM) of $g(z)$ and find a slightly extended decoupling duration in $f(R, L_m)$. Finally, we analyze the evolution of energy densities and determine the matter-radiation equality redshift as $z_{\mathrm{eq}} \approx 4203$ in $f(R, L_m)$ and $z_{\mathrm{eq}} \approx 2779$ in $\Lambda$CDM, with corresponding cosmic times of approximately $67{,}756$ and $67{,}232$ years, respectively. These results confirm that $f(R, L_m)$ gravity retains key cosmological landmarks while introducing testable deviations from the standard paradigm.

The Rosetta spacecraft escorted comet 67P/Churyumov-Gerasimenko for two years, gathering a rich and variable dataset. Amongst the data from the Rosetta Plasma Consortium (RPC) suite of instruments are measurements of the total electron density from the Mutual Impedance Probe (MIP) and Langmuir Probe (LAP). At low outgassing, the plasma density measurements can be explained by a simple balance between the production through ionisation and loss through transport. Ions are assumed to travel radially at the outflow speed of the neutral gas. Near perihelion, the assumptions of this field-free chemistry-free model are no longer valid, and plasma density is overestimated. This can be explained by enhanced ion transport by an ambipolar electric field inside the diamagnetic cavity, where the interplanetary magnetic field does not reach. In this study, we explore the transition between these two regimes, at intermediate outgassing ($5.4 \times10^{26}~\mathrm{s^{-1}}$), when the interaction between the cometary and solar wind plasma influences the transport of the ions. We use a 3D collisional test-particle model, adapted from Stephenson et al. 2022 to model the cometary ions with input electric and magnetic fields from a hybrid simulation for 2.5-3 au. The total plasma density from this model is then compared to data from MIP/LAP and to the field-free chemistry-free model. In doing so, we highlight the limitations of the hybrid approach and demonstrate the importance of modelling collisional cooling of the electrons to understand the ion dynamics close to the nucleus.

We report on a quasi-periodic variation at $\sim1$ Hz during a fast X-ray outburst of a high-mass X-ray binary MAXI J0709$-$159 / LY CMa observed by the Neutron-star interior composition explorer (NICER). The new X-ray transient MAXI J0709$-$159 was discovered on 2022 January 25. Due to the transient X-ray behavior characterized by the short (a few hours) outburst duration, rapid ($\lesssim$ 1 s) variability with spectral change, and large luminosity swing from $10^{32}$ erg s$^{-1}$ to $10^{37}$ erg s$^{-1}$, the object was considered likely to be a supergiant X-ray binary with a neutron star (NS) categorized as a Supergiant Fast X-ray Transient (SFXT). Follow-up NICER and NuSTAR observations confirmed that the position of the new X-ray object is consistent with a Be star, LY CMa, which has been also identified as a B supergiant. We analyzed the NICER data obtained from 3 hours to 6 days after the discovery. The light curve reveals that the X-ray activity continued for $\sim7$ hours in sparse short flares, each lasting $\lesssim 100$ seconds, and the luminosity instantaneously reached up to $\sim 1\times 10^{38}$ erg s$^{-1}$. The light-curve and spectral features reasonably agree with those expected from accretion of a clumpy stellar-wind onto a magnetized NS. The variability power spectrum during the brightest flare shows a broad peak at $1.1$ Hz resembling a quasi-periodic oscillation (QPO). If the QPO is attributed to the Keplerian orbital frequency at the inner edge of a transient accretion disk truncated by the NS magnetosphere, the NS surface magnetic field is estimated to be $\sim 10^{12}$ G.

The receiver N3AR operating at a frequency range between 67 and 116 GHz has been commissioned at the APEX telescope in October 2024. This adds a new low-frequency band for APEX, with the capability of simultaneous dual-frequency observations using a dichroic beamsplitter. The 3 mm receiver also allows APEX to join the existing 3 mm global VLBI network. One of our commissioning goals was to perform simultaneous dual-band VLBI observations at 86 and 258 GHz using receivers with shared-optical-paths (SOP) to correct the atmospheric phase fluctuations using the frequency phase transfer (FPT) technique. This was possible together with the IRAM 30 m telescope, which has already developed such a capability. We aimed to verify the expected phase coherence and sensitivity improvement at the higher frequency achievable by applying FPT. With the dual-band, single baseline data, we applied the FPT method, which uses the lower frequency data to correct the simultaneously observed higher-frequency data. We evaluate the improvement compared to the conventional single-band observing mode by analyzing the coherence factor in the higher frequency data. Our results show that the phase fluctuations at the two bands are well correlated. After applying FPT, the interferometric phases at the higher frequency vary much slower and the coherence factor is significantly improved. Our analysis confirms the feasibility of applying FPT to frequencies above 250 GHz with SOP receivers. Future observations in this mode could dramatically improve the sensitivity and imaging fidelity of high-frequency VLBI.

The ionospheric Pedersen and Hall conductances play an important role in understanding the exchanges of angular momentum, energy and matter between the magnetosphere and the ionosphere/thermosphere at Jupiter, modifying the composition and temperature of the planet. In the high latitude regions, these conductances are enhanced by the auroral electron precipitation. The effect of a broadband precipitating electron energy distribution, similar to the observed electron distributions through particle measurements, on the conductance values is investigated. The new values are compared to the ones obtained from previous studies, notably when considering a mono-energetic distribution. The broadband precipitating electron energy distribution is modeled by a kappa distribution, which is used as an input in an electron transport model that computes the density vertical profiles of ionospheric ions. The vertical profiles of the Pedersen and Hall conductivities are then evaluated assuming that the conductivities are mostly governed by the densities of H3+ and CH5+. Finally, the Pedersen and Hall conductances are computed by integrating the corresponding conductivities over altitude. The Pedersen and Hall conductances are globally higher when considering a broadband electron energy distribution rather than a mono-energetic distribution. In addition, the use of the direct outputs of an electron transport model rather than the analytical expression presented in Hiraki and Tao (2008) as well as a change in the electron collision cross-sections also have significant impacts on the conductance values. Comparison between our results and the ones deduced from the corotation enforcement theory suggests that either a physical mechanism limits the field-aligned currents or the auroral electrons precipitating in the atmosphere are also accelerated by processes not associated with the field-aligned currents.

Millisecond pulsars are known to show complex radio pulse profiles and polarisation position angle evolution with rotational phase. Small scale surface magnetic fields and multipolar components are believed to be responsible for this complexity due to the radiation mechanisms occurring close to the stellar surface but within the relatively small light-cylinder compared to the stellar radius. In this work, we use the latest NICER phase aligned thermal X-ray pulse profile of PSR~J0740+6620 combined with radio and $\gamma$-ray pulse profiles and radio polarisation to deduce the best magnetic field configuration that can simultaneously reproduce the light-curves in these respective bands. We assume a polar cap model for the radio emission and use the rotating vector model for the associated polarisation, a striped wind model for the $\gamma$-ray light-curves and rely on the NICER collaboration results for the hot spot geometry. We demonstrate that an almost centred dipole can account for the hot spot location with a magnetic obliquity of $\alpha \approx 51 \deg$ and a line of sight inclination angle of $\zeta \approx 82 \deg$. However, with this geometry, the hot spot areas are three times too large. We found a better solution consisting of two dipoles located just below the surface in approximately antipodal positions. Our double dipole model is able to reproduce all the salient radio and $\gamma$-ray characteristics of PSR~J0740+6620 including radio polarisation data. A double dipole solution is more flexible than an off-centred dipole because of two independent magnetic axes and could hint at a magnetic field mostly concentrated within the crust and not in the core.

The Pierre Auger Observatory has the capability to identify neutrino-induced extensive air showers above $10^{17}$ eV by using its large Surface Detector (SD) array. Data from the Observatory have been used to set some of the most stringent upper limits to the neutrino flux in the ultra-high energy (UHE) range. The data have also been used for follow-up detection of transient events in the context of multi-messenger astrophysics. In mid-2013, two additional SD triggers (Time-over-Threshold-deconvolved (ToTd) and Multiplicity-of-Positive Steps (MoPS)) were shown to increase the detection capability for the neutrino-induced air showers in the energy regime below $10^{19}$ eV by a factor of 5-10. This contribution will give an overview of the ongoing work regarding the searches for UHE neutrinos at the Pierre Auger Observatory. The impact of the ToTd and MoPS triggers for neutrino search in the zenith angle range of $60^{\circ} < \theta < 75^{\circ}$ is discussed. A novel neutrino identification method, which integrates these triggers, is applied to observational data to look for neutrino-like events using a $\textit{blind}$ search strategy. New constraints to point-like sources of UHE neutrinos will be presented for the angular range explored.

Pulsars, the cosmic lighthouses, are strongly self-gravitating objects with core densities significantly exceeding nuclear density. Since the discovery of the Hulse--Taylor pulsar 50 years ago, binary pulsar studies have delivered numerous stringent tests of General Relativity (GR) in the strong-field regime as well as its radiative properties -- gravitational waves (GWs). These systems also enable high-precision neutron star mass measurements, placing tight constraints on the behaviour of matter at extreme densities. In addition, pulsars act as natural detectors for nanohertz GWs, primarily from supermassive black hole binaries, culminating in the first reported evidence of a stochastic GW background in 2023. In this article, I review key milestones in pulsar research and highlight some of contributions from my own work. After a brief overview of the gravity experiments in \S 1, I review the discovery of pulsars -- particularly those in binaries -- and their critical role in gravity experiments (\S 2) that laid the foundation for recent advances. In \S 3, I present the latest efforts on GR tests using the Double Pulsar and a pioneer technique to constrain the dense matter equation of state. \S 4 demonstrates the potential of binary pulsars on testing alternative theories to GR. Advances in nanohertz GW detection with pulsar timing arrays are discussed in \S 5. I outline some of the current challenges in \S 6 and conclude with final remarks in \S 7.

In the era of real-time astronomy, citizen scientists play an increasingly important role in the discovery and follow-up of transient astrophysical phenomena. From local astronomical societies to global initiatives, amateur astronomers contribute valuable observational data that complement professional efforts. Astro-COLIBRI facilitates these contributions by providing a user-friendly platform that integrates real-time alerts, data visualization tools, and collaborative features to support astronomers at all levels. The Astro-COLIBRI Citizen Science Program provides engagement opportunities across multiple scales. At the grassroots level, we collaborate with local astronomy clubs, equipping them with accessible tools for transient event monitoring. National and international networks, such as RAPAS in France, leverage Astro-COLIBRI's real-time capabilities for coordinated observations. On a global scale, we actively participate in high-impact citizen science and capacity building initiatives, including the International Astronomical Union (IAU) Citizen Science Program and the "Open Universe" initiative led by the United Nations Office for Outer Space Affairs (UNOOSA). These collaborations enhance the accessibility of real-time astrophysical data and foster inclusive participation in cutting-edge astronomy. In this contribution, we will present the Astro-COLIBRI Citizen Science Program, highlighting its technical framework, community impact, and case studies of successful amateur contributions. We will showcase how our platform facilitates the rapid exchange of information between professional and amateur astronomers, democratizing access to multi-messenger astrophysics and enabling the global community to contribute meaningfully to time-domain discoveries.

Simulate the entire GRB dynamics since its production until the jet's break-out from the star envelope is computationally expensive. In this work, we aim to investigate jet production at the black hole horizon and its subsequent evolution beyond the envelope boundary. We perform 2.5-dimensional GRMHD simulations using, as initial conditions, remapped massive star progenitors previously evolved with a state-of-the-art stellar evolutionary codes. Specifically, we adopt the Wolf-Rayet star models 12TH and 16TI from the Woosley \& Heger framework, and we evolve our own Long GRB progenitor with the MESA code. A dipolar magnetic field is imposed, with variations in field strength to explore its influence. We find that the jets are magnetically dominated, with their thermal and kinetic components remaining comparable during propagation through the stellar envelope. The cocoon is thermally dominated in most cases. Jet launching is successful when the magnetic field has a dipolar configuration and spin $a=0.9$, in contrast, a hybrid magnetic field does not result in jet formation. We observe disk formation in cases without a magnetized jet, however, the formation of a well-defined funnel is not evident and the expansion of such wind does not break the star for longer times. Our simulations show that a collapsar launches a successful, relativistic jet only when a strong, large-scale dipolar field, driving a magnetically arrested disk. Such jets collimate, accelerate, and break out of progenitor stars in $1.5\lesssim t\lesssim3.5$ s, while weaker or non-magnetised flows stall inside the star. The resulting jets have luminosities of $L_{j}\sim10^{49}$--$10^{53}\,$erg\,s$^{-1}$ and the final energy structure reveals that magnetisation distribution and progenitor stratification as the key determinants of jet structure and success.

In the build-up of galactic discs gas infall is an important ingredient and it produces radial gas inflows as a physical consequence of angular momentum conservation, since the infalling gas on to the disc at a specific radius has lower angular momentum than the circular motions of the gas at the point of impact. NGC300 is a well studied isolated, bulge-less, and low-mass disc galaxy ideally suited for an investigation of galaxy evolution with radial gas inflows. To investigate the effects of radial gas inflows on the physical properties of NGC300, a chemical evolution model for NGC300 is constructed by assuming its disc builds up progressively by infalling of metall-free gas and outflowing of metal-enriched gas. Radial gas inflows are also considered in the model. Our model including the radial gas inflows and an inside-out disc formation scenario can simultaneously reproduce the present-day observed radial profiles of HI gas mass surface density, SFR surface density, sSFR, gas-phase and stellar metallicity. We find that, although the value of radial gas inflow velocity is as low as -0.1 km/s, the radial gas inflows steepen the present-day radial profiles of HI gas mass surface density, SFR surface density, and metallicity, but flatten the radial sSFR profile. Incorporating radial gas inflows significantly improves the agreement between our model predicted present-day sSFR profile and the observations of NGC300. It predicts a significant flattening of the metallicity gradient with cosmic time. We also find that the model predicted star formation has been more active recently, indicating that the radial gas inflows may be help to sustain star formation in local spirals, at least in NGC300.

The Pierre Auger Observatory consists of 1660 water-Cherenkov detectors (WCDs) and 27 fluorescence telescopes, covering a surface of 3000 km2 in the province of Mendoza, Argentina. After almost two decades, Auger Phase I has ended the data taking and has already delivered many outstanding physics results. The Auger Observatory is currently running in Phase II, with upgraded detectors for enhanced data of ultra-high-energy cosmic rays (UHECRs). During Phase I, several engineering detectors were developed and tested. Some of those developments led to new detectors, which are now part of the upgraded Observatory. For Phase II, the WCDs were upgraded with a surface-scintillator detector, a radio detector, a small photomultiplier, and an upgraded electronics board, facilitating mass-sensitive measurements for source identification of UHECRs. Moreover, an underground muon detector allows for a direct measurement of the muon content of air showers. The Offline framework is the main software for the event reconstruction and detector simulation at the Pierre Auger Observatory. It is continuously being developed to accommodate changes in the detector and new algorithms. It allows the running of various applications, which are made up of individual modules, either on raw data or simulations on an event-by-event basis. Large productions of shower and detector reference libraries are done with CORSIKA 7 and Offline on the European Grid Infrastructure (EGI) using the Virtual Organization Auger. Various air-shower geometries (up to 89 degrees in zenith) were considered, as well as several primary particles (from light to ultra-heavy nuclei, photons, and neutrinos), hadronic interaction models and detector configurations for Phase I and Phase II. In this contribution, we present the actual efforts and updates on software for data production and reference Monte Carlo simulations for Auger data analysis.

The Chinese Plate-Digitizing Project has digitized a total number of about 30,000 astronomical plates from 11 telescopes of five observatories (SHAO, NAOC, PMO, YNAO, and QDO) in China, spanning nearly 100 years of observations. In this work, we present a photometric calibration method to calibrate about 15,000 single-exposure plates to the JKC photometric system. Using standard stars constructed from the BEST database, we have identified and corrected various systematic effects (including the magnitude term, color term, and flat-field term) to a high precision. The final photometric precision is typically 0.15, 0.23, 0.17, 0.11, 0.19 mag for plates collected in SHAO, NAOC, PMO, YNAO, and QDO, respectively, with best cases reaching 0.07, 0.08, 0.06, 0.05, and 0.11 mag, respectively. Candidates of variable sources are also identified. The catalogs are publicly available at the China National Astronomical Data Center. Such a dataset will provide a valuable resource for conducting long-term, temporal-scale astronomical research. Our calibration method can also be applied to other digitized astronomical plates in general.

Diffusive shock acceleration and diffusion propagation are essential components of the standard cosmic ray model. These theories are based on extensive observations of high-energy solar processes, providing substantial direct evidence in the MeV energy range. Although the model is widely and successfully used to explain high-energy cosmic phenomena, direct validation has been elusive. The multi-wavelength spectra and angular profile measurements of the Geminga pulsar wind nebula and its pulsar halo, particularly the precise spectral observations by HAWC and LHAASO-KM2A in recent years, offer a rare opportunity to test these theories with cosmic rays energies between 1 TeV and several hundred TeV. These observations are expected to elevate the direct testing of theoretical models from multi-MeV to sub-PeV energies. In this work, a method is developed to test the diffusive shock acceleration and diffusion propagation model between one and several hundred TeV energies through the latest spectral and morphological data of the Geminga region from HAWC and Fermi-LAT. Our results show that the theories of diffusive shock acceleration and diffusion propagation are consistent with experimental observations. However, the published morphological data adopted rather wide energy bins and currently do not allow a high precision test of the inferred energy dependent diffusion coefficient by observed energy spectra with DSA theory. It is anticipated that future HAWC and LHAASO-KM2A observations will yield higher-precision results, and the confirmation of a rapidly increasing diffusion coefficient above 100 TeV would serve as important evidence supporting the diffusive shock acceleration and diffusion propagation theory.

The Pierre Auger Observatory has driven the field of ultra-high-energy cosmic ray (UHECR) physics, producing several groundbreaking observations over the last 20 years. One of the most striking findings has been the complex evolution of UHECR mass composition, as revealed by detailed analyses of observables such as the depth of shower maximum ($X_{\rm max}$) and the muon content of showers. As more data are collected and sophisticated analyses are undertaken, not only are new fine details emerging, but the general picture of UHECR mass composition is becoming increasingly robust. This contribution presents recent results on the mass composition of UHECRs derived from surface, fluorescence, and radio detectors. Together with other key findings from the Observatory, these results converge to present a coherent picture of UHECR mass composition, effectively ruling out proton dominance and challenging the interpretation of the observed flux features as purely proton-induced propagation effects. To finish the contribution, we compare the $X_{\rm max}$ data from the southern and northern equatorial bands of the exposure of the Pierre Auger Observatory fluorescence detector to evaluate the possibility of changes in composition as a function of declination.

Solar activity events release vast amounts of energy, including radio waves, X-rays, ultraviolet radiation, and energetic particles, which interact with the ionosphere of the Earth and can disrupt radio wave propagation, affecting radio communications. They can either enhance reflections, improving long-distance terrestrial communications, or cause signal degradation and absorption, respectively, depending on whether the increased ionization affects the upper or lower layers of the ionosphere. In the first case, the solar cycle modulates the Maximum Usable Frequency (MUF), the highest frequency usable for radio communication between two Earth-based points. The Auger Engineering Radio Array (AERA) of the Pierre Auger Observatory was developed to measure the radio emission from extensive air showers in the $30-80$ MHz band. We examine the impact of solar activity on AERA data collected over approximately 11 years. We report the detection of different types of solar radio bursts and we investigate how increased solar radiation - particularly in the X-ray and extreme ultraviolet bands - also affects measurements in the AERA energy band. Our results show a remarkable correlation between the MUF and the broadband noise observed in the $30-40$ MHz frequency range. Radio blackouts are also observed in AERA spectrograms in coincidence with those reported by the National Oceanic and Atmospheric Administration (NOAA). Additionally, we performed a search for temporal coincidences between AERA data and independent observations of solar radio burst events from the e-CALLISTO network and the SWAVES instrument. These findings highlight the complex interplay between solar activity and radio wave propagation, which is also relevant for cosmic-ray detection.

The analysis of HAWC data is done using a likeihood-based systematic multi-source search procedure utilizing the threeML software package and the HAL Plugin. This approach was inspired by the extended source search described in the Fermi-LAT Extended Source Search Catalog. The pipeline to search for point sources and extended sources within the region of interest (ROI) is described in the recent HAWC papers. This procedure is computationally intensive and often requires multiple days to produce a final model for a region. Often this approach misses fainter sources, which need to be added manually later. This blind search could be complemented by providing a method to seed source locations, which can be assessed and evaluated by likelihood analysis, thereby significantly reducing the computational time and resources spent on finding a model.

PG 1159 stars are thought to be progenitors of the majority of H-deficient white dwarfs. Their unusual He-, C-, and O-dominated surface composition is typically believed to result from a late thermal pulse experienced by a single (pre-)white dwarf. Yet, other formation channels - involving close binary evolution - have recently been proposed and could lead to similar surface compositions. Here we present a non-local thermodynamic equilibrium spectral analysis based on new UV and archival optical spectra of one of the hottest PG 1159 stars, $\text{RX J}0122.9\text{ -}7521$. We find $T_\text{eff} = 175$ kK and a surface gravity of log $g = 7.7$, and an astonishingly low O/C ratio of $7.3 \times 10^{-3}$ by mass. By combining the spectroscopic surface gravity and Gaia parallax with a spectral energy distribution fit, we derive a mass of $M_\text{spec} = 1.8^{+1.1}_{-0.7}$ $M_\odot$. Although this spectroscopic mass is higher than predicted by evolutionary models, it is subject to substantial uncertainty. Furthermore, we find that $\text{RX J}0122.9\text{ -}7521$ shows strongly rotationally broadened lines, suggesting that the previously reported photometric period of $41$ min indeed corresponds to the rotational period of this star. Our kinematic analysis shows that $\text{RX J}0122.9\text{ -}7521$ belongs to the Galactic halo, which - assuming single-star evolution - is in stark contrast to its relatively high mass. The rapid rotation, high mass, and halo kinematics, as well as the lack of evidence for a close companion, lead us to believe that $\text{RX J}0122.9\text{ -}7521$ formed through the merger of two white dwarfs. Yet, none of the current models can explain the surface abundances of $\text{RX J}0122.9\text{ -}7521$.

We present a novel non-parametric method for inferring smooth models of the mean velocity field and velocity dispersion tensor of the Milky Way from astrometric data. Our approach is based on Stochastic Variational Gaussian Process Regression (SVGPR) and provides an attractive alternative to binning procedures. SVGPR is an approximation to standard GPR, the latter of which suffers severe computational scaling with N and assumes independently distributed Gaussian Noise. In the Galaxy however, velocity measurements exhibit scatter from both observational uncertainty and the intrinsic velocity dispersion of the distribution function. We exploit the factorization property of the objective function in SVGPR to simultaneously model both the mean velocity field and velocity dispersion tensor as separate Gaussian Processes. This achieves a computational complexity of O(M^3) versus GPR's O(N^3), where M << N is a subset of points chosen in a principled way to summarize the data. Applied to a sample of ~8 x 10^5 stars from the Gaia DR3 Radial Velocity Survey, we construct differentiable profiles of the mean velocity and velocity dispersion as functions of height above the Galactic midplane. We find asymmetric features in all three diagonal components of the velocity dispersion tensor, providing evidence that the vertical dynamics of the Milky Way are in a state of disequilibrium. Furthermore, our dispersion profiles exhibit correlated structures at several locations in |z|, which we interpret as signatures of the Gaia phase spiral. These results demonstrate that our method provides a promising direction for data-driven analyses of Galactic dynamics.

Meteoroid entry into planetary atmospheres generates bow shocks, resulting in high-temperature gas conditions that drive chemical reactions. In this paper, we perform three-dimensional hydrodynamic simulations of meteoroid entry using the Athena++ code, coupled with chemistry calculations via Cantera to model the non-equilibrium chemistry triggered by atmospheric entry. Our aerodynamical simulations reveal the formation of complex shock structures, including secondary shock waves, which influence the thermodynamic evolution of the gas medium. By tracking thermodynamic parameters along streamlines, we analyze the effects of shock heating and subsequent expansion cooling on chemical reaction pathways. Our results demonstrate that chemical quenching occurs when the cooling timescale surpasses reaction rates, leading to the formation of distinct chemical products that deviate from equilibrium predictions. We show that the efficiency of molecular synthesis depends on the object\textquotesingle s size and velocity, influencing the composition of the post-entry gas mixture. Applying our model to Titan, we demonstrate that organic matter can be synthesized in the present environment of Titan. Also, we find that nitrogen, the dominant atmospheric component, remains stable, while water vapor is efficiently removed, a result inconsistent with equilibrium chemistry assumptions. Moreover, we compare our simulation results with laser experiments and find good agreement in chemical yields. Finally, we also evaluate the impact on Titan\textquotesingle s atmosphere as a whole, showing that meteoroid entry events could have played a significant role in supplying molecules such as HCN during early Titan\textquotesingle s history.

We describe distinctive stellar features indicating the presence of hyperons in neutron stars. A strongly negative curvature of the mass-radius relation R(M) is characteristic of hyperons, which can be determined from measurements of neutron stars with three different masses. Similarly, a reduced second derivative of the tidal deformability as function of mass $\lambda(M)$ points to hyperonic degrees of freedom in NS matter. The slopes of such curves R(M) and \lambda(M) can distinguish a hyperonic equation of state from purely nucleonic models if they appear increased (decreased for \lambda(M)) relative to the maximum mass of neutron stars.

In the framework of the coherent curvature radiation model of pulsar radio emission, charged particles responsible for the radio emission are generated on the polar cap in the localized pair cascade processes called sparks. When a pulsar can no longer sustain the sparking process on its polar cap, the coherent radio emission from the pulsar stops, and the pulsar is called dead. In this work, we revisit the pulsar death phenomena under two popular voltage gap models: vacuum voltage gap and partially screened voltage gap. We notice that a dying pulsar resorts to a single spark on the polar cap to sustain the pair production under both voltage gap frameworks. The presence of only one spark on the polar cap has important implications for the radio emission properties of the pulsar. We study the emission properties of five pulsars close to the lower boundary on the $P-\dot{P}$ plane of the current pulsar population, as these pulsars are expected to be dying. We find that the dying pulsars in our sample and the normal pulsar population have very similar emission properties. We show that the majority of pulsars in the pulsar death valley, including five pulsars in our sample, show evidence of multiple sparks as opposed to what is expected from single spark death line models.

The nuclear rates for reactions involving 12C and 16O are key to compute the energy release and nucleosynthesis of massive stars during their evolution. These rates shape the stellar structure and evolution, and impact the nature of the final compact remnant. We explore the impact of new nuclear reaction rates for 12C({\alpha},{\gamma})16O, 12C+12C, 12C+16O and 16O+16O reactions for massive stars. We aim to investigate how the structure and nucleosynthesis evolve and how these processes influence the stellar fate. We computed stellar models using the GENEC code, including updated rates for 12C({\alpha},{\gamma})16O and, for the three fusion reactions, new rates following a fusion suppression scenario and new theoretical rates obtained with TDHF calculations. The updated 12C({\alpha},{\gamma})16O rates mainly impact the chemical structure evolution changing the 12C/16O ratio with little effect on the CO core mass. This variation in the 12C/16O ratio is critical for predicting the stellar fate, which is very sensitive to 12C abundance. The combined new rates for 12C+12C and 16O+16O fusion reactions according to the HIN(RES) model lead to shorter C- and O-burning lifetimes, and shift the ignition conditions to higher temperatures and densities. Theoretical TDHF rates primarily affect C-burning, increasing its duration and lowering the ignition temperature. These changes alter the core chemical structure, the carbon shell size and duration, and hence the compactness. They also affect nucleosynthesis. This work shows that accurate reaction rates for key processes in massive star evolution drive significant changes in stellar burning lifetimes, chemical evolution, and stellar fate. In addition, discrepancies between experimental and theoretical rates introduce uncertainties in model predictions, influencing both the internal structure and the supernova ejecta composition.

As the two Voyager spacecraft traveled beyond the heliosphere, they encountered a magnetic field environment that had never been observed before. Studies have attempted to characterize this new regime by examining the magnetic field intermittency. This is typically done by fitting the optimal kappa distribution function and interpreting its so-called q-statistics to characterize the magnetic field increments. Using this approach, recent findings concluded that beyond a certain distance, the magnetic field increments in the very local interstellar medium (VLISM) follow Gaussian statistics, unlike those both inside the heliosphere and in the region just beyond the widely accepted heliopause location, raising questions about the heliopause identification. This study explores this issue in detail by (1) optimizing the derivation of the distribution function, (2) examining whether and how the results depend on increment windows and time periods, and (3) determining the statistical behavior of the examined time series. Using magnetic field measurements from Voyager 1, we present two independent techniques and introduce a statistical framework to systematically analyze the distributions of magnetic field increments. Contrary to previous findings, we find that magnetic field increments in the VLISM do not follow a Gaussian distribution (k to infinity) and instead are in the non-Gaussian range of kappa values (3-7, when analyzed on a 30-day statistical period). We further demonstrate how erroneous, statistically induced results can arise that mimic Gaussian-like results when mixing different structures in such analyses. Our results show that Voyager 1 still travels in the intermittent magnetic field environment of the VLISM.

Isotopic ratios have been used as chemical diagnostics to investigate the origin of the material in the Solar System. We have determined the HCN, HNC, and N2H+ isotopic ratios and the chemical age in a large sample of 23 starless cores located in different environments. This work uses IRAM 30m data to constrain the D/H ratio of HCN, HNC, and N2H+ as well as the 14N/15N ratio of HCN and HNC. The observed abundances have been modeled using the chemical code DNAUTILUS 2.0. Deuterated compounds are detected in all of our sample cores, with average DNC/HNC, DCN/HCN, and N2D+/N2H+ values of 0.054$\pm$0.019, 0.036$\pm$0.033, and 0.15$\pm$0.11, respectively. The deuterium fractions (Dfrac) show a weak correlation with temperature and a large scatter that reflects that other factors such as core evolution could also play a significant role. Our chemical model is able to reproduce all the observed values with 0.2-0.3 Myr in Taurus and 0.3-0.5 Myr in Perseus and Orion. The 14N/15N isotopic ratio is found to be different between HCN/HC15N (430$\pm$120) and HNC/H15NC (296$\pm$64). We find no correlation between these ratios and the deuterium fractions, but we report a weak correlation with temperature. The Dfrac of HCN, HNC, and N2H+ can be used as evolutionary tracers of starless cores as long as the physical parameters are well constrained. The HCN/HC15N and HNC/H15NC ratios are not correlated with Dfrac, suggesting that the detected variations are not correlated with the core evolutionary stage. The average value of the HCN/HC15N ratio in our sample is significantly higher than the values measured in protostars and protoplanetary disks, possibly indicating that nitrogen fractionation processes are taking place during the protostellar phase.

We present new Chandra X-ray imaging spectroscopy of the compact galaxy group IC 2431, and compare with archival ultraviolet, optical, infrared, and radio images. IC 2431 is a starburst system containing three tidally-distorted disk galaxies. All three galaxies may have active nuclei. One galaxy is classified as an AGN based on its optical spectrum, a second is identified as a possible X-ray AGN based on the Chandra data, and the third galaxy may host a radio AGN. In optical images, a prominent dust lane crosses the southern galaxy, while Spitzer infrared images show a dusty bridge connecting the two brightest galaxies. Chandra maps reveal a massive (2 x 10^7 M(sun)) concentration of hot gas between these two galaxies, as well as several other knots of hot gas and non-thermal emission. The unabsorbed X-ray luminosity of the hot gas in IC 2431 is ~ 1 x 10^42 erg/s, which is enhanced by about a factor of four relative to the star formation rate, compared to other star-forming galaxies. In radio maps, a bright jet/ridge of radio continuum emission extends 4 kpc from one nucleus. We compare the properties of IC 2431 with those of other interacting galaxy systems, and discuss two different scenarios that may account for the peculiarities of IC 2431: ram pressure stripping of the interstellar medium during a head-on collision between two galaxies, or an AGN-powered radio jet that has been distorted by an interaction with interstellar gas during a tidal encounter between galaxies.

Ground-based full-sky studies of the angular distribution of arrival directions of ultra-high-energy cosmic rays require combining data from different observatories, such as the Pierre Auger Observatory (Auger) and the Telescope Array (TA), because no single array can cover all declinations. A working group comprising members from the Auger and TA collaborations has been tasked with performing such studies for more than a decade and has found several indications of full-sky anisotropies. Here, we update the results for the large- and medium-scale anisotropy analyses using the latest data from TA, which include corrections for daily and yearly atmospheric effects in data for large-scale anisotropies and looser selection criteria in data for medium-scale anisotropies. We extend the latter one by considering two more galaxy catalogues, consisting of jetted or all AGNs. Finally we also introduce a new angular harmonic space analysis that allows us to measure both the auto-correlation and cross-correlation with all catalogues for all multipoles independently ($\ell_\text{max} = 20$ in this work) and scanning the energy threshold.

Predictions for the acoustic attenuation coefficient and phase speed as functions of frequency and altitude in Saturn's atmosphere are presented and discussed. The pressure range considered in the study is 1 mbar to 1 bar, in windless and cloudless conditions. The atmospheric composition is represented by the major constituents, namely hydrogen (with its two spin isomers, ortho-H$_2$ and para-H$_2$) and helium. The H$_2$ and He concentrations are assumed constant with respect to altitude; however, non-uniform ortho- and para-H$_2$ profiles are considered. The acoustic wavenumber is obtained by incorporating a viscous, thermal, and internal molecular relaxation effects in a linearized fluid dynamics model. The ambient inputs are vertical profiles of the specific heats, shear viscosity, and thermal conductivity coefficients of the three-component (oH$_2$, pH$_2$, He) mixture, extracted at each pressure-temperature pair. The authors acknowledge funding from NASA-Ames Center for Innovation Fund (CIF).

Slow magnetoacoustic waves with a 3 minute period are upward-propagating waves traveling through the density-stratified umbral atmosphere. The decreasing density causes their amplitude to increase, developing into nonlinear waves through steepening and eventually forming shocks. To investigate the vertical evolution of this wave nonlinearity, we utilized multi-wavelength data from the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO), covering from the photosphere to the lower corona across 20 active regions. The steepening of the wave profile leads to the generation of higher harmonics. We quantify this using a nonlinearity index (NI), defined as the ratio of the amplitude of 2nd harmonic to the fundamental obtained using wavelet analysis. We find a characteristic pattern: nonlinearity increases from the photosphere through the lower chromosphere, peaking near the AIA 1700 \r{A} formation height, and decreases at higher altitudes, notably in the AIA 304 \r{A} channel. This trend indicates progressive wave steepening and subsequent energy dissipation before reaching the formation of AIA 304 \r{A}, consistent with shock formation in the lower atmosphere. An additional rise in NI is observed at the AIA 131 \r{A} channel, followed by a decline in AIA 171 \r{A}, suggesting a 2nd phase of wave nonlinearity evolution in the lower corona. Based on the NI profile and the formation heights of these channels, we conjecture that nonlinear wave processes are most prominent between the AIA 1700 \r{A} and AIA 304 \r{A} formation layers and again between AIA 131 \r{A} and AIA 171 \r{A}.

We present JWST/NIRSpec PRISM observations of three luminous ($M_{\rm UV}<-20$) galaxies at $z\sim10$ observed with the CAPERS Cycle 3 program. These galaxies exhibit extreme UV slopes compared to typical galaxies at $z=10$. Of the three sources, two of them are a close pair (0.22 - arcsec) of blue galaxies at $z=9.800\pm0.003$ and $z=9.808\pm0.002$ with UV slopes of $\beta=-2.87\pm0.15$ and $\beta=-2.46\pm0.10$ respectively, selected from PRIMER COSMOS NIRCam imaging. We perform spectrophotometric modeling of the galaxies which suggests extremely young stellar ages and a lack of dust attenuation. For the bluest galaxy, its UV slope also suggests significant Lyman continuum escape. In contrast, the third source (selected from CEERS NIRCam imaging) at $z=9.942\pm0.002$ exhibits a red UV slope with $\beta=-1.51\pm0.08$. We rule out the possibility of a strong nebular continuum due to the lack of a Balmer jump and find no evidence to support the presence of active galactic nucleus continuum due to a lack of strong UV emission lines and no broad component to H$\gamma$ or H$\beta$. Instead, it is most likely that the red UV slope is due to dust-reddening ($A_{\rm V}\simeq0.9$) implying a significant level of dust-obscured star-formation only $\simeq480\, \rm Myr$ after the Big Bang. Under standard assumptions for dust attenuation, EGS-25297 would be the most intrinsically UV-luminous galaxy ($M_{\mathrm{UV,corr}}\simeq -22.4^{+0.7}_{-1.1}$) yet spectroscopically confirmed at $z \sim 10$. This work highlights that luminous galaxies at $z\gtrsim10$ have a diversity of dust properties and that spectroscopy of these galaxies is essential to fully understand star-formation at $z\gtrsim10$.

The existence of galaxies with no elements such as Oxygen - formed by stars after Big Bang nucleosynthesis - is a key prediction of the cosmological model. Finding them would provide direct and transformative evidence of the formation of the first galaxies in extremely different conditions than those observed today. JWST has enabled the identification of galaxies all the way to cosmic times of a few hundred million years. However, no pristine "zero-metallicity" Population III galaxies have been identified so far. Here, we report the identification of an extremely metal-poor galaxy at redshift z = 5.725 ("AMORE6"), about one billion years after the Big Bang, observed near the critical line of a foreground galaxy cluster, and thus multiply imaged and magnified (mu = 39-78). Publicly available JWST NIRCam Wide Field Slitless Spectroscopy (WFSS) spectra consistently detect H$\beta$ at both image positions, but [O III]4960,5008 remains undetected. This places a firm upper limit on its oxygen abundance of 12+log(O/H) < 6.0 (1 sigma), or < 0.20% of solar metallicity. AMORE6 is characterized by low stellar mass (5.6+0.2-0.1 x 10^5 Msun), very blue rest-frame UV spectral slope, and extremely compact morphology (effective radius re = 4.0+1.4-1.4 pc). These properties are consistent with massive star formation in a pristine or near-pristine environment. The finding of such an example at a relatively late time in cosmic history is surprising. However, regardless of cosmic epoch, the identification of a potentially pristine object is a key validation of the Big Bang model.

2024 PT$_5$ is a tiny ($D\leq10$ m) near-Earth asteroid (NEA) discovered in August 2024. 2024 PT$_5$ was gravitationally bound to the Earth-Moon system from September to November 2024 and classified as a minimoon. Several quick response observations suggest the lunar ejecta origin of 2024 PT$_5$, while rotation state and albedo, essential properties to investigate its origin, are not well constrained. We performed visible to near-infrared multicolor photometry of 2024 PT$_5$ from data taken using the TriColor CMOS Camera and Spectrograph (TriCCS) on the Seimei 3.8 m telescope during 2025 January 4-10. The Seimei/TriCCS observations of 2024 PT$_5$ cover phase angles from 14 deg to 27 deg, and were obtained in the $g$, $r$, $i$, and $z$ bands in the Pan-STARRS system. In addition, we analyzed $Y$, $J$, $H$, and $K$ photometry taken with the Multi-Object Spectrograph for Infrared Exploration (MOSFIRE) on the Keck I 10-m telescope taken on 2025 January 16-17. Our lightcurves show brightness variations over time periods of several tens of minutes. We infer that 2024 PT$_5$ is in a tumbling state and has a lightcurve amplitude of about 0.3 mag. Visible and near-infrared color indices of 2024 PT$_5$, $g-r=0.567\pm0.044$, $r-i=0.155\pm0.009$, $r-z=0.147\pm0.066$, $Y-J=0.557\pm0.046$, $J-H=0.672\pm0.078$, and $H-Ks=0.148\pm0.098$, indicate that 2024 PT$_5$ is an S-complex asteroid, largely consistent with previous observations. Using the $H$-$G$ model, we derived an absolute magnitude $H_{V,HG}$ of $27.72\pm0.09$ and a slope parameter $G_V$ of $0.223\pm0.073$ in V-band. A geometric albedo of 2024 PT$_5$ is derived to be $0.26\pm0.07$ from the slope of its photometric phase curve. This albedo value is typical of the S- and Q-type NEAs. The color properties of 2024 PT$_5$ derived from our observations match rock samples taken from the lunar surface, which agrees with previous studies.

We report the deepest upper limits to date on the power spectrum of the 21-cm signal during the Cosmic Dawn (redshifts: $z>15$), using four nights of observations with the NenuFAR radio interferometer. The limits are derived from two redshift bins, centred at $z=20.3$ and $z=17.0$, with integration times of 26.1 h and 23.6 h, from observations of an optimal target field chosen to minimise sidelobe leakage from bright sources. Our analysis incorporates improvements to the data processing pipeline, particularly in subtracting strong radio sources in the primary beam sidelobes and mitigating low-level radio frequency interference, yielding a 50-fold reduction in the excess variance compared to a previous analysis of the north celestial pole field. At $z=20.3$, we achieve a best $2\sigma$ upper limit of $\Delta^{2}_{21}<4.6 \times 10^5 \, \textrm{mK}^{2}$ at $k=0.038$ $h\, \mathrm{cMpc}^{-1}$, while at $z=17.0$, the best limit is $\Delta^{2}_{21}<5.0 \times 10^6 \, \textrm{mK}^{2}$ at $k=0.041$ $h\, \mathrm{cMpc}^{-1}$. These are the strongest constraints on the 21-cm power spectrum at the respective redshifts, with the limit at $z = 20.3$ being deeper by more than an order of magnitude over all previous Cosmic Dawn power spectrum limits. Comparison against simulated exotic 21-cm signals shows that while the $z=20.3$ limits begin to exclude the most extreme models predicting signals stronger than the EDGES detection, an order-of-magnitude improvement would constrain signals compatible with EDGES. A coherence analysis reveals that the excess variance is largely incoherent across nights for the $z=20.3$ redshift bin, suggesting that deeper integrations could yield significantly stronger constraints on the 21-cm signal from the Cosmic Dawn.

Through studying rotation curves, which depict how the velocity of the stars and gas changes with distance from the center of the galaxy, it has been confirmed that dark matter dominates galaxy's outer regions, as their rotation curve remains flat. However, recent studies of star-forming galaxies at cosmic noon have shown a decline in their rotation curve beyond a certain point, suggesting a decrease of the abundance of dark matter in galactic halos during earlier times. In this work, we investigate the influence of cosmological surface brightness dimming and loss of resolution on observations of rotation curves at cosmic noon. We used a sample of 19 Lyman Break Analogs at $z \approx 0.2$ and artificially redshifted them as if they were at $z \approx 2.2$. By comparing both rotation curves of the observed and mocked objects, we find that the asymmetry of the cosmic noon galaxies is smaller than that of the low-$z$ galaxies. In low-$z$ galaxies, asymmetry increases with radius and becomes relevant at the external parts, where mergers and interactions cause more disturbance in the galaxy's gravitational field. In contrast, cosmic-noon galaxies appear smoother, smaller, and suitable for dynamical modeling -- when in reality, they are not. The combined effects of the cosmological bias and loss of resolution lead us to the conclusion that caution should be exercised when using cosmic-noon rotation curves, as they might not accurately trace the gravitational potential of the galaxy.

Spiral galaxy disks are thought to exist in a quasi-stationary state, between fresh gas accretion from cosmic filaments and disk star formation, self-regulated through supernovae feedback. Our goal here is to quantify these processes and probe their efficiency. While star formation can be traced at 10 Myr time-scales through H$\alpha$ emission, the signature of OB stars, and at 100 Myr scale with UV emission, the gas surface density is traced by HI emission for the atomic phase. We choose to investigate feedback processes using fountain effects in M101, a nearby well-observed face-on galaxy. Face-on studies are very complementary to the more frequent edge-on observations of these fountains in the literature. We use high-resolution data from THINGS for the HI emission GALEX for UV, and SITELLE/SIGNALS IFU for the H$\alpha$ tracer. We have identified 20 new HI holes, in addition to the 52 holes found by Kamphuis in 1993. We study in more detail the nine holes satisfying strong criteria to be true fountain effects, compute their physical properties, and derive their energy balance. Only one small HI hole still contains H$\alpha$ and young stars inside, while the largest hole of 2.4 kpc and oldest age (94 Myr) is deprived of H$\alpha$ and UV. For face-on disks, the possibility to study simultaneously the HI shell morphology, the stellar association, and kinematic evidence is of primordial importance. In M101, we have quantified how stellar feedback is responsible for carving the observed cavities in the atomic gas disk, and how it can expel above the disk the neutral gas, which is then unavailable for star formation during up to 100 Myr.

Consider a system of point masses in a spherical potential. In such systems objects execute planar orbits covering two-dimensional rings or annuli, represented by the angular-momentum vectors, which slowly reorient due to the persistent weak gravitational interaction between different rings. This process, called vector resonant relaxation, is much faster than other processes which change the size/shape of the rings. The interaction is stron9gest between objects with closely aligned angular-momentum vectors. In this paper, we show that nearly parallel angular-momentum vectors may form stable bound pairs in angular-momentum space. We examine the stability of such pairs against an external massive perturber, and determine the critical separation analogous to the Hill radius or tidal radius in the three-body problem, where the angular-momentum pairs are marginally disrupted, as a function of the perturber's mass, the orbital inclination, and the radial distance. Angular-momentum pairs or multiples closer than the critical inclination will remain bound and evolve together in angular-momentum-direction space under any external influence, such as anisotropic density fluctuations, or massive perturbers. This study has applications in various astrophysical contexts, including galactic nuclei, in particular the Milky Way's Galactic centre, globular clusters, or planetary systems. In nuclear star clusters with a central super-massive black hole, we apply this criterion to the disc of young, massive stars, and show that clusters in angular-momentum space may be used to constrain the presence of intermediate-mass black holes or the mass of the nearby gaseous torus.