{"paper":{"title":"Late-time dark energy dynamics in $f(Q)$ gravity: A data-driven analysis","arxiv_id":"2609.01650","primary_cat":"gr-qc","submitted_at":"2026-08-30T11:06:22+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. No sentence in this record was written by a language model.","schema":"pith.compiled-record/v0","status":"compiled","abstract":{"source":"arXiv listing abstract v1","sentences":[{"i":0,"p":1.0,"id":"s0","own":false,"role":"background","text":"The increasing precision and complementarity of late-time cosmological observations provide new opportunities to test modified gravity against the observed expansion history of the universe.","hedge":{"p":0.81,"label":"asserted"},"own_p":0.05,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":1.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":1,"p":0.59,"id":"s1","own":false,"role":"method","text":"The combination of DESI DR2 BAO measurements with cosmic chronometers (CC) and independent Type Ia supernova compilations provides a data-driven test of cosmic acceleration.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.28,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.11,"role_probabilities":{"gap":0.0,"method":0.59,"result":0.0,"background":0.27,"limitation":0.0,"future_work":0.0,"contribution":0.14,"interpretation":0.0}},{"i":2,"p":0.86,"id":"s2","own":true,"role":"contribution","text":"Motivated by this progress, we investigate late-time dark energy dynamics in symmetric teleparallel $f(Q)$ gravity by adopting the power-law form $f(Q)=\\beta Q^{m+1}$ and characterizing cosmic evolution through the effective equation of state (EoS) parameter.","hedge":{"p":0.92,"label":"asserted"},"own_p":0.86,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.13,"role_probabilities":{"gap":0.0,"method":0.14,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.86,"interpretation":0.0}},{"i":3,"p":0.99,"id":"s3","own":true,"role":"method","text":"The model is constrained using CC, DESI DR2 BAO and three independent Type Ia supernova compilations, namely Pantheon+, DES-SN5YR and Union3.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.85,"main_claim_p":0.02,"quantitative":true,"quantitative_p":0.55,"role_probabilities":{"gap":0.0,"method":0.99,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"The inferred Hubble constant values are mutually consistent, yielding $H_0=67.60^{+1.60}_{-1.66}$, $67.08^{+1.66}_{-1.61}$ and $68.16^{+1.46}_{-1.43}\\,\\mathrm{km\\,s^{-1}\\,Mpc^{-1}}$, respectively.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.93,"main_claim_p":0.04,"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":0.97,"id":"s5","own":true,"role":"result","text":"Statistically, the proposed $f(Q)$ model yields lower $\\chi^2_{\\min}$ values and is favored by the AIC for all dataset combinations, whereas the BIC favors $\\Lambda$CDM for the CC + DESI DR2 + Pantheon+ and CC + DESI DR2 + DES-SN5YR combinations and indicates no meaningful preference between the two models for the CC + DESI DR2 + Union3 dataset combinations.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.95,"main_claim_p":0.16,"quantitative":true,"quantitative_p":0.96,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.97,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.03}},{"i":6,"p":0.72,"id":"s6","own":true,"role":"result","text":"The reconstructed EoS indicates quintessence-like behavior, while the negative deceleration parameter confirms the current accelerated expansion.","hedge":{"p":0.7,"label":"asserted"},"own_p":0.92,"main_claim_p":0.12,"quantitative":false,"quantitative_p":0.07,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.72,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.28}},{"i":7,"p":1.0,"id":"s7","own":true,"role":"result","text":"The transition from deceleration to acceleration occurs within $0.680\\leq z_t\\leq0.745$.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.92,"main_claim_p":0.04,"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":8,"p":0.9,"id":"s8","own":true,"role":"result","text":"Higher-order cosmographic parameters and the Statefinder and $Om(z)$ diagnostics consistently support this quintessence-like behavior, with the Statefinder trajectories approaching the $\\Lambda$CDM fixed point in the far future.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.91,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.28,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.9,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.1}},{"i":9,"p":0.95,"id":"s9","own":true,"role":"interpretation","text":"Overall, the power-law $f(Q)$ model provides a viable and competitive description of late-time cosmic acceleration.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.83,"main_claim_p":0.93,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.05,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.95}}]},"compiled":{"main_claim":{"p":1.0,"text":"Overall, the power-law $f(Q)$ model provides a viable and competitive description of late-time cosmic acceleration.","location":"abstract 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