{"paper":{"title":"An analytical model for non-local stochastic field-level galaxy bias on the sphere","arxiv_id":"2610.12259","primary_cat":"astro-ph.CO","submitted_at":"2026-10-08T16:28:52+00:00","version_compiled":"v1"},"notice":"Every quoted sentence is the authors' text from the arXiv listing abstract. Labels and probabilities are the outputs of classifier-1.13.0 on the question bank abstract-p1-20260923, exactly as returned. 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to enter through fluctuations in the bias itself.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.9,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.91,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.09,"interpretation":0.0}},{"i":2,"p":0.85,"id":"s2","own":true,"role":"method","text":"The construction yields an explicit decomposition into a linear, non-local stochastic and deterministic components in harmonic space.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.92,"main_claim_p":0.08,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.85,"result":0.01,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.14,"interpretation":0.0}},{"i":3,"p":0.95,"id":"s3","own":true,"role":"method","text":"We fit the model parameters to the projected power spectra measured in large-volume hydrodynamical simulations (FLAMINGO), enabling sampling of galaxy populations from simulated matter fields while conditioning on galaxy properties such as halo mass or redshift.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.1,"quantitative":false,"quantitative_p":0.14,"role_probabilities":{"gap":0.0,"method":0.95,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.05,"interpretation":0.0}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"By construction, the model reproduces the two-point statistics down to the simulation resolution, and without being calibrated on it, BOLTS recovers the equilateral bispectrum within the sample variance of the simulation down to comoving scales of $\\mathcal{O}(10 \\, \\mathrm{Mpc})$ for halo masses $ M_{\\rm{h}} > 10^{11.5}\\,\\rm{M}_{\\odot} $ over redshifts $0 < z < 3$.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.28,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":5,"p":0.94,"id":"s5","own":true,"role":"result","text":"Relative to local bias prescriptions, it more accurately captures amplitude-phase correlations and mode coupling in the measured wavelet phase harmonics wherever the stochasticity of the tracers exceeds their discreteness, including low redshifts and lower halo masses $M_{\\rm{h}} = 10^{11.5}\\,\\rm{M}_{\\odot}$ where non-linearities become 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