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AstroArxiv
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
GW250114 reveals black hole horizon signatures. Neil Lu et. al. https://arxiv.org/abs/2510.01001
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Splitting the Gravitational Atom: Instabilities of Black Holes with Synchronized/Resonant Hair. Jordan Nicoules et. al. https://arxiv.org/abs/2509.20450
(Left) BHsSH in the simplest scalar model: a horizon inside a toroidal boson star. (Right) A thin ring of constant mass density (bottom) and its Newtonian potential (top). Figure 2 Figure 3 The BHSH configuration {C
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Small Progenitors, Large Couplings: Type Ic Supernova Constraints on Radiatively Decaying Particles. Francisco R. Candón et. al. https://arxiv.org/abs/2509.18253
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Space-based cm/kg-scale Laser Interferometer for Quantum Gravity. Nobuyuki Matsumoto et. al. https://arxiv.org/abs/2507.12899
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Projective Transformations for Regularized Central-Force Dynamics: Hamiltonian Formulation. Joseph T.A. Peterson et. al. https://arxiv.org/abs/2506.22681
Verification that $q= { {q Verification that the STM for $( {q Verification that the STM for $( {q Verifying accuracy of the canonical equations of motion for $( {q
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Radio emission from airplanes as observed with RNO-G. RNO-G Collaboration: S. Agarwal et. al. https://arxiv.org/abs/2506.17522
{Left Overview of the signals of two types of airplanes. {Left: Overview of the signals of two types of airplanes. {Left: {Left
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Accelerated inference of binary black-hole populations from the stochastic gravitational-wave background. G. Giarda et. al. https://arxiv.org/abs/2506.12572
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Electroluminescence and charge multiplication in liquid xenon with a VCC-like Microstrip Plate. Gonzalo Martínez-Lema et. al. https://arxiv.org/abs/2505.24611
Left: VCC plate mounted on a FR4 support: 13 parallel 2$ $m wide strips are connected to a square frame. Two stainless steel clamps provide connection to the external circuit using a multiple-folded aluminium foil to avoid damage to the metal coating. Right: Microphotograph of an anode strip at i... Figure 2 S2 signal area as a function of time of the VCC in xenon gas at room temperature after ramping (black) and after ramping (magenta). An exponential function is fitted to each dataset, from which a decay constant ($ $) is extracted. Comparison of different microstructures in liquid xenon in what concerns secondary light emission. Left: extent of the region along the shortest field line for which the electric field strength is above the electroluminescence threshold measured in {Aprile:2014ELthreshold
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Characterized behaviors of black hole thermodynamics in the supercritical region. Zi-Qiang Zhao et. al. https://arxiv.org/abs/2504.04995
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Verifiable type-III seesaw and dark matter in a gauged $\boldsymbol{U(1)_{\rm B-L}}$ symmetric model. Satyabrata Mahapatra et. al. https://arxiv.org/abs/2504.00109
Relic density as a function of DM mass, with the color bar indicating variations in Yukawa coupling $y_ $. Other free parameters are kept fixed as mentioned in the inset of the figure. Dependence of relic density on DM mass. Free parameters are varied as mentioned. A comparison of $ ^{ , 0 Figure 4
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Anatomy of singlet-doublet dark matter relic: annihilation, co-annihilation, co-scattering, and freeze-in. Partha Kumar Paul et. al. https://arxiv.org/abs/2412.02607
Allowed parameter space of DM for which DM is in equilibrium with SM bath and the $ {Z Spin-independent DM-nucleon scattering cross-section as a function of DM mass. Variation of DM relic density w.r.t. DM mass with the fixed mass splitting of $1~ {M {Right:
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Emergent Cosmological Expansion in Scalar-Tensor Theories of Gravity. Chad Briddon et. al. https://arxiv.org/abs/2406.01397
The magnitude of the gradient of the scalar field, outside of the spherical body at the centre of the cell. Colours correspond to the configurations from Fig. {spheres Scalar field profiles along a line connecting the centre of a cell and the centre of a cell face. Curves correspond to spheres of radius $0.04$ (red), $0.03$ (green), $0.02$ (purple) and $0.01$ (blue), and range from completely unscreened (red) to strongly screened (blue), with the screened value... Figure 3 Figure 4
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Extended mass distribution of PBHs during QCD phase transition: SGWB and mini-EMRIs. Nilanjandev Bhaumik et. al. https://arxiv.org/abs/2509.25083
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Dwarf galaxy halo masses from spectroscopic and photometric lensing in DESI and DES. Helena Treiber et. al. https://arxiv.org/abs/2509.20434
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
The redshift distribution of Einstein Probe transients supports their relation to gamma-ray bursts. Brendan O'Connor et. al. https://arxiv.org/abs/2509.07141
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
DIPLODOCUS I: Framework for the evaluation of relativistic transport equations with continuous forcing and discrete particle interactions. Christopher N. Everett et. al. https://arxiv.org/abs/2508.13296
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
In-Situ Formation of the Cold Classical Kuiper Belt. Rixin Li et. al. https://arxiv.org/abs/2508.04776
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Tidal heating in detached double white dwarf binaries. Lucy O. McNeill et. al. https://arxiv.org/abs/2507.21821
The masses and radii of eclipsing ELM WD binary components in the Galactic detached sample (Table~ {tab:WD1 {Reverse cumulative distribution function for DWDBs as a function of $f$, using the estimate for ELM DWDB production rates $ {R Evolution of temperature $T_ {eff Temperature evolution of the primary ELM WD component in six J1539--like binaries. These models are evolved from temperatures of 4,000~K, 5,000~K, 6,000~K, 7,000~K, 8,000~K and 9,000~K at $f=1.5$ mHz, corresponding to the secondary CO WD's formation and hence DWDB formation. All tracks (solid lin...
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Ultra-long MeV transient from a relativistic jet: a tidal disruption event candidate. Gor Oganesyan et. al. https://arxiv.org/abs/2507.18694
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Prospects for probing dark matter particles and primordial black holes with the Square Kilometre Array using the 21 cm power spectrum at cosmic dawn. Meng-Lin Zhao et. al. https://arxiv.org/abs/2507.02651
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
HeII emitters at cosmic noon and beyond. Characterising the HeII λ1640 emission with MUSE and JWST/NIRSpec. R. González-Díaz et. al. https://arxiv.org/abs/2506.11685
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Clustering analysis of BOSS-CMASS galaxies with semi-analytical model for galaxy formation and halo occupation distribution. Zhongxu Zhai et. al. https://arxiv.org/abs/2505.18748
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
The Giant Arc -- Filament or Figment?. Till Sawala (1 and 2) et. al. https://arxiv.org/abs/2505.11072
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Unveiling the trends between dust attenuation and galaxy properties at z ~ 2 - 12 with the James Webb Space Telescope. V. Markov et. al. https://arxiv.org/abs/2504.12378
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 5h
Enhancing the reliability of machine learning for gravitational wave parameter estimation with attention-based models. Hibiki Iwanaga et. al. https://arxiv.org/abs/2501.10486
An example spectrogram of simulated GW150914 data with an injected glitch of amplitude $1A$. Figure 2 Flow chart of uncertainty evaluation. Figure 4