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AstroArxiv
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
SOAPv4: A new step toward modeling stellar signatures in exoplanet research. E. Cristo et. al. https://arxiv.org/abs/2510.08319
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Tidal disruption of a neutron star near naked singularity. Ashok B. Joshi (Charotar Uni. and Ahmedabad Uni. et. al. https://arxiv.org/abs/2509.26108
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
An Introduction to Gravitational Wave Theory. Simone Speziale et. al. https://arxiv.org/abs/2508.21817
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Toward Low-Latency, High-Fidelity Calibration of the LIGO Detectors with Enhanced Monitoring Tools. M. Wade et. al. https://arxiv.org/abs/2508.08423
Figure 1 Figure 2 Figure 3 An example of line subtraction from data in the LIGO Hanford detector. This figure shows the amplitude spectral density (ASD) zoomed in on the 17.1 Hz Pcal line. The data with no line subtraction applied is shown in red. The data with line subtraction performed using a static 128 second runnin...
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Love beyond Einstein: Metric reconstruction and Love number in quadratic gravity using WEFT. Arpan Bhattacharyya et. al. https://arxiv.org/abs/2508.02785
Feynman diagrams contributing to the computation of the one-point function of $ $ and $ $ up to 1PN. We need to sum up these diagrams to perturbatively reconstruct the metric. Numeric vs analytic $F( )$ Numeric vs analytic $F( )$ Numeric vs analytic $H( )$
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Extended momentum-dependent interaction for transport models and neutron stars. Si-Pei Wang et. al. https://arxiv.org/abs/2507.02448
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Tidal heating in binary inspiral of strange quark stars. Suprovo Ghosh et. al. https://arxiv.org/abs/2504.07659
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Scalable Cosmic AI Inference using Cloud Serverless Computing. Mills Staylor et. al. https://arxiv.org/abs/2501.06249
AWS Lambda Memory Usage by Partition Data Size. We empirically size the dataset based on the partition data size in MB. CAI: number of AWS Lambda Function invocations for different data sizes. Similar to figure {fig:cai-throughput The parameter counts for recent deep learning-based methods developed for astronomy images, capable of inference across diverse computing environments—including a personal laptop, HPC CPUs, HPC GPUs, and our proposed cloud-based framework, CAI. A pre-trained AstroMAE model is used for the inferen... CAI framework overview using AWS Lambda Functions. It uses an AWS S3 bucket for data, code, and result storage. The state machine defines the workflow execution steps using AWS Lambda functions and distributed maps. Parallel execution is achieved through data partitions for almost linear high-per...
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Visions in Quantum Gravity. Luca Buoninfante et. al. https://arxiv.org/abs/2412.08696
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Lectures in Quantum Gravity. Ivano Basile et. al. https://arxiv.org/abs/2412.08690
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Comparison of global networks of third-generation gravitational-wave detectors. Michele Maggiore et. al. https://arxiv.org/abs/2411.05754
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Unitarity, Causality, and Solar System Bounds May Significantly Limit the Use of Gravitational Waves to Test General Relativity. Alexander Cassem et. al. https://arxiv.org/abs/2408.12118
Experimental bounds on the size of corrections to Newton's potential $ $ as a function of scale $ $; taken from Ref.~ {Adelberger:2003zx Experimental bounds on the size of corrections to Newton's potential $ $ as a function of scale $ $; taken from Ref.~ {Adelberger:2003zx Correction to the potential $ $ between point masses due to a scalar ($N=1$) running in a loop versus distance $r$. The black curve is the full numerical result from Fourier transforming Eq.~( {expanded version of Jq2 for total amplitude Figure 4
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Getting More Out of Black Hole Superradiance: a Statistically Rigorous Approach to Ultralight Boson Constraints from Black Hole Spin Measurements. Sebastian Hoof et. al. https://arxiv.org/abs/2406.10337
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
FIELDMAPS Data Release: Far-Infrared Polarization in the "Bones" of the Milky Way. Simon Coudé et. al. https://arxiv.org/abs/2509.25832
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Comparing Minimal and Non-Minimal Quintessence Models to 2025 DESI Data. Husam Adam et. al. https://arxiv.org/abs/2509.13302
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Tidal disruption events in active galactic nuclei: on orbital inclination and Schwarzschild apsidal precession. Minghao Zhang et. al. https://arxiv.org/abs/2509.07535
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
PowerBin: Fast Adaptive Data Binning with Centroidal Power Diagrams. Michele Cappellari (University of Oxford) https://arxiv.org/abs/2509.06903
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Multi-band Spectral and Astrometric Characterization of the HIP 99770 b Planet with SCExAO/CHARIS and Gaia. Danielle Bovie et. al. https://arxiv.org/abs/2509.02665
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Onset of CN Emission in 3I/ATLAS: Evidence for Strong Carbon-Chain Depletion. Luis E. Salazar Manzano et. al. https://arxiv.org/abs/2509.01647
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Group Therapy for Halos: Advancing Halo Mass Estimation for Galaxy Groups. Welsey Van Kempen et. al. https://arxiv.org/abs/2508.12556
Figure 1 Figure 2 Distribution of quenched fraction in the stellar mass–halo mass plane for galaxy groups in the observational dataset of {VanKempen2024 Figure 4
astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Analytical estimates for heliocentric escape of satellite ejecta. Jose Daniel Castro-Cisneros et. al. https://arxiv.org/abs/2508.06856
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Auriga Superstars: Improving the resolution and fidelity of stellar dynamics in cosmological galaxy simulations. Ruediger Pakmor et. al. https://arxiv.org/abs/2507.22104
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Hydrodynamical modeling of SN 2025kg associated with the Fast X-ray Transient EP250108a. L.M. Roman Aguilar et. al. https://arxiv.org/abs/2507.20457
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
All-sky neutrino point-source search with IceCube combined track and cascade data. R. Abbasi et. al. https://arxiv.org/abs/2507.07275
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astroarxiv.bsky.social
AstroArxiv @astroarxiv.bsky.social · 2d
Constraints on Cosmologically Coupled Black Holes from Planck 2018 and Other Cosmological Probes. Shintaro K. Hayashi https://arxiv.org/abs/2507.03408
Figure 1 Figure 2 Comoving BH mass functions at redshifts $z = 0$, $1$, $2$, $4$, $6$, $8$, and $10$, using the fitting function in Eq.~ {schechtergaussian Figure 4