First narrow-line flux ratios for lensed quasar RXJ1131-1231 measured with JWST/NIRSpec IFS at ~5% precision, detecting cusp anomaly consistent with prior work.
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representative citing papers
Self-regulating AGN jets in MHD simulations of cool-core clusters yield realistic FRI radio morphologies viewed along the jet axis and account for frequency-independent lobe extents via 1-50 μG fields allowing both young and old electrons to radiate.
SIDM simulations of dwarf halos show that quiescent merger histories produce gravothermal core collapse while sustained mergers prevent collapse and can yield central densities below gravothermal fluid model predictions.
The W cloud is reinterpreted as a disrupting galaxy group with a dynamically coherent tidal tail delivering low-mass star-forming dwarfs to the Virgo cluster.
Future subhalos show a pre-infall bias to higher progenitor masses, modeled in extended Press-Schechter theory by multiplying the collapse barrier by β(x,a)=(1-x)^{1.20+0.14a} for M200c, leading to 10-15% higher central concentration.
Shock-to-shock distances in double radio relic clusters serve as a merger chronometer to set a 68% upper limit of sigma/m < 0.22 cm²/g on dark matter self-interaction, marginalizing over mass, angle, speed, phase, impact parameter, and gas slope.
Advection-only galactic wind models fail to reproduce observed vertical radio profiles without unrealistic velocities, synchrotron spectra are biased toward young electrons in dense regions, and bremsstrahlung/Coulomb losses cannot be neglected even when subdominant.
A Gaussian decomposition via integral transform computes lensing quantities for arbitrary elliptical mass profiles, unifying with existing kinematic analysis.
PHANTOM is a public MATLAB/Octave toolbox for linear field statistics and halo observables in dark matter cosmology, validated to sub-percent agreement with Python packages colossus, hmf, and halomod.
A six-parameter function of peak height ν, power spectrum slope n_eff, and growth rate α_eff accurately describes median halo mass accretion rates from simulations in ΛCDM and Einstein-de Sitter cosmologies at z=0-14.
A ~60-minute microlensing event is interpreted via Bayesian modeling as a ~0.03 Earth-mass primordial black hole in the Milky Way dark-matter halo.
Mutual information analysis of TNG50 simulations shows gravitational potential and total energy retain merger mass and infall time information longest, while radial velocity loses it within ~5 Gyr, with washout depending on radius, merger age, and mass.
CosmoPostProcess delivers simulation-calibrated radial corrections for projection-induced selection bias (20-40% amplitude near 1 h^{-1} Mpc) and baryonic effects in Euclid richness-selected cluster weak lensing profiles.
Lagrangian tracers show mixing with low-entropy seeds drives most condensation in cluster cores; magnetic fields cause earlier divergence, higher vorticity, lower Mach numbers, and slower cold-cloud motion via tension.
Deep Chandra data confirms three cold fronts in RXJ2014.8-2430 with widths indicating suppressed diffusion and identifies a concave structure consistent with either a Kelvin-Helmholtz instability or a powerful AGN cavity of radius 200-330 kpc.
Simulations indicate that 2500 LSST strong lenses can exclude 74% and 36% of the prior volume on halo mass function parameters at 3σ and 5σ, with sensitivity from both high- and low-mass halos plus line-of-sight contributions.
Milky Way-mass dark matter density profiles in IllustrisTNG are largely insensitive to astrophysics and cosmology variations, dominated by halo-to-halo variance instead.
JWST prism spectroscopy of 200 massive galaxies at z~3-15 shows normal star-forming galaxies dominate at z>6 while dusty systems and quiescent galaxies increase at lower redshift, with evidence for multiple quenching pathways.
KMeans clustering of star-formation histories for 6051 LAEs in IllustrisTNG100 at z=2 yields four classes, with 35% showing the typical recent-burst profile and 65% having bursts 0.3-1.3 Gyr earlier.
The first circumgalactic dust reddening measurement from Rubin DP1 data finds A_V proportional to r_perp to the -1.8 power within 120 kpc, consistent with prior SDSS/KiDS/DES results despite 1000x smaller area and fainter foreground sample.
Empirical universal fitting formula for the peak (most probable) concentration of dark matter halos derived from lognormal fits to simulation distributions and shown to be invariant across cosmologies.
The Via Project is a planned five-year dual-hemisphere spectroscopic survey targeting over 2 million stars with 100 m/s RV stability and transient spectroscopy to r~24 using instruments on MMT and Magellan/Clay telescopes starting in 2027.
Derives three closed-form basis sets using a single Jacobi polynomial in prolate spheroidal and cylindrical coordinates and shows transformations between spherical, prolate spheroidal, bispherical, and toroidal systems.
Power-law modeling of gas mass fraction and temperature variation reconciles observed X-ray scaling relations in galaxy clusters, reducing >3σ tensions from 49% to 11% and yielding a redshift-independent mass proxy Y_LGT0.
citing papers explorer
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The pre-infall bias of subhalos
Future subhalos show a pre-infall bias to higher progenitor masses, modeled in extended Press-Schechter theory by multiplying the collapse barrier by β(x,a)=(1-x)^{1.20+0.14a} for M200c, leading to 10-15% higher central concentration.
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A New Robust Constraint on the Self-interaction Cross-section of Dark Matter with Double Radio Relic Clusters
Shock-to-shock distances in double radio relic clusters serve as a merger chronometer to set a 68% upper limit of sigma/m < 0.22 cm²/g on dark matter self-interaction, marginalizing over mass, angle, speed, phase, impact parameter, and gas slope.
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Unified lensing and kinematic analysis for any elliptical mass profile
A Gaussian decomposition via integral transform computes lensing quantities for arbitrary elliptical mass profiles, unifying with existing kinematic analysis.
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PHANTOM: A MATLAB and Octave Toolbox Connecting Linear Field Statistics to Dark Matter Halo Observables
PHANTOM is a public MATLAB/Octave toolbox for linear field statistics and halo observables in dark matter cosmology, validated to sub-percent agreement with Python packages colossus, hmf, and halomod.
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A universal model for the accretion rates and formation times of dark matter halos
A six-parameter function of peak height ν, power spectrum slope n_eff, and growth rate α_eff accurately describes median halo mass accretion rates from simulations in ΛCDM and Einstein-de Sitter cosmologies at z=0-14.
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AMPM II. A Lunar-Mass Primordial Black Hole Microlensing Candidate in the Milky Way Halo
A ~60-minute microlensing event is interpreted via Bayesian modeling as a ~0.03 Earth-mass primordial black hole in the Milky Way dark-matter halo.
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Euclid preparation. CosmoPostProcess: A simulation calibrated framework for weak lensing selection bias in richness-selected galaxy clusters
CosmoPostProcess delivers simulation-calibrated radial corrections for projection-induced selection bias (20-40% amplitude near 1 h^{-1} Mpc) and baryonic effects in Euclid richness-selected cluster weak lensing profiles.
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LSST Strong Lensing Systems Dark Matter Sensitivity Analysis with Neural Ratio Estimators
Simulations indicate that 2500 LSST strong lenses can exclude 74% and 36% of the prior volume on halo mass function parameters at 3σ and 5σ, with sensitivity from both high- and low-mass halos plus line-of-sight contributions.
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Universal Fitting Formulae for the Peak Concentration of Dark Matter Halos
Empirical universal fitting formula for the peak (most probable) concentration of dark matter halos derived from lognormal fits to simulation distributions and shown to be invariant across cosmologies.
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Beyond Self-Similarity: Reconciling X-Ray Scaling Relations in Galaxy Clusters and Groups
Power-law modeling of gas mass fraction and temperature variation reconciles observed X-ray scaling relations in galaxy clusters, reducing >3σ tensions from 49% to 11% and yielding a redshift-independent mass proxy Y_LGT0.
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Constraining Galaxy Cluster Triaxiality via Weak Lensing -- I. Preparation for the Rubin Data Beyond Leading Order
Galaxy clusters have an average projected ellipticity of 0.310 with axis ratio 0.527, showing no significant mass or redshift dependence, measured via weak lensing on DES Y3 data and verified with mocks.
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Non-conservation and time non-locality of biased tracers
Non-conserved biased tracers debias more rapidly than conserved tracers, leading to time-dependent suppression of large-scale power.
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Inferring Halo Mass and Scale Radius of Galaxy Clusters Using Convolutional Neural Networks and Uchuu-UniverseMachine Catalogs
Convolutional neural networks can infer galaxy cluster virial masses and scale radii from 2D projected position and line-of-sight velocity distributions with nearly unbiased results and reduced scatter when richness is added or training is limited to relaxed systems.
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Adaptive Reconstruction of Cluster Halos (ARCH): Integrating Shear and Flexion for Substructure Detection
ARCH introduces a staged optimization pipeline for joint shear-flexion gravitational lensing reconstruction that recovers cluster and subcluster masses consistent with prior weak+strong lensing results on Abell 2744 and El Gordo.
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Probing Baryonic Feedback Effect with CSST Weak Lensing and Future FRB Measurements
Forecasts using mock CSST lensing and SKA/DSA-2000 FRB DM data show joint analysis improves log10 T_AGN precision from 3.1% to 0.4% and tightens sum m_nu upper limit to <0.47 eV.
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Accurate Galaxy Cluster Shear and Mass Calibration for LSST with AnaCal
AnaCal recovers input shear with low bias in high-shear cluster regimes under LSST-like conditions, producing 0.24% mean mass bias.
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UNIONS-3500 Weak Lensing: I. A Galaxy Shape Catalogue in the Northern Sky
A catalogue of 62 million galaxy shapes from 3500 sq deg of UNIONS r-band imaging achieves an effective source density of 4.96 arcmin^{-2} and shape noise of 0.27 after PSF calibration and validation.
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Probing the Nature of Dark Matter Self-Interactions Through Observations of Massive Black Hole Mergers
Simulations indicate LISA could statistically distinguish CDM from SIDM (constant 1 cm²/g cross-section) with at least ~70 high-SNR massive black hole merger detections.