New agegraphic dark energy driven reconstruction of <i>f</i>(<i>Q</i>) gravity and its cosmological implications

Abstract In this work, we perform reconstruction of f ( Q ) gravity inspired by the new agegraphic dark energy (NADE) model, aiming to account for the Universe’s late-time acceleration without invoking a cosmological constant. Utilizing a power law scale factor <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mrow> <mml:mi>a</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:mi>t</mml:mi> <mml:mo stretchy="false">)</mml:mo> <mml:mo>=</mml:mo> <mml:msub> <mml:mi>a</mml:mi> <mml:mn>0</mml:mn> </mml:msub> <mml:msup> <mml:mi>t</mml:mi> <mml:mi>h</mml:mi> </mml:msup> </mml:mrow> </mml:math> , we derive an analytic form for f ( Q ) based on a correspondence with NADE, where the conformal time serves as the infrared cutoff. The resulting model naturally recovers general relativity in the limit and exhibits a geometrically motivated dark energy component. We constrain the model parameters using recent Baryon acoustic oscillation (BAO) data from DESI DR2 BAO and previous BAO observations through the Markov Chain Monte Carlo analysis. The reconstructed Hubble parameter H ( z ) demonstrates excellent agreement with observational data, achieving high R 2 values and low <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mrow> <mml:msubsup> <mml:mi>χ</mml:mi> <mml:mrow> <mml:mo movablelimits="true">min</mml:mo> </mml:mrow> <mml:mn>2</mml:mn> </mml:msubsup> </mml:mrow> </mml:math> , AIC, and BIC scores, outperforming the standard ΛCDM model. Further, we investigate the cosmological evolution using the deceleration parameter q ( z ), effective equation of state <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mrow> <mml:msub> <mml:mi>ω</mml:mi> <mml:mrow> <mml:mrow> <mml:mi>eff</mml:mi> </mml:mrow> </mml:mrow> </mml:msub> <mml:mo stretchy="false">(</mml:mo> <mml:mi>z</mml:mi> <mml:mo stretchy="false">)</mml:mo> </mml:mrow> </mml:math> , and Om diagnostics. The model exhibits a clear transition from deceleration to acceleration with a present value <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mrow> <mml:mi>q</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="false">)</mml:mo> <mml:mo>∈</mml:mo> <mml:mrow> <mml:mo>[</mml:mo> <mml:mo>−</mml:mo> <mml:mn>0.5879</mml:mn> <mml:mo>,</mml:mo> <mml:mo>−</mml:mo> <mml:mn>0.3333</mml:mn> <mml:mo>]</mml:mo> </mml:mrow> </mml:mrow> </mml:math> and transition redshift <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mrow> <mml:msub> <mml:mi>z</mml:mi> <mml:mrow> <mml:mrow> <mml:mi>tr</mml:mi> </mml:mrow> </mml:mrow> </mml:msub> <mml:mo>∼</mml:mo> <mml:mn>0.5209</mml:mn> <mml:mo>−</mml:mo> <mml:mn>0.8126</mml:mn> </mml:mrow> </mml:math> , while maintaining <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> <mml:mo>&lt;</mml:mo> <mml:msub> <mml:mi>ω</mml:mi> <mml:mrow> <mml:mrow> <mml:mi>eff</mml:mi> </mml:mrow> </mml:mrow> </mml:msub> <mml:mo stretchy="false">(</mml:mo> <mml:mi>z</mml:mi> <mml:mo stretchy="false">)</mml:mo> <mml:mo>&lt;</mml:mo> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> <mml:mrow> <mml:mo>/</mml:mo> </mml:mrow> <mml:mn>3</mml:mn> </mml:mrow> </mml:math> , indicating quintessence like behavior. Om diagnostics consistently show a negative slope, further confirming deviation from ΛCDM. Energy condition analysis reveals that WEC, DEC, and NEC are satisfied, while SEC is violated only at low redshifts, which is consistent with cosmic acceleration. Also, stability analysis for the model shows stable behavior under scalar perturbations. Overall, the reconstructed f ( Q ) model provides a viable, stable, observationally consistent, and theoretically motivated alternative to standard dark energy scenarios.