  Recent measurements of baryon acoustic oscillations (BAO) by the Dark Energy
Spectroscopic Instrument (DESI) suggest a preference for a dynamic dark energy
model over a cosmological constant. This conclusion emerges from the
combination of DESI's BAO data with observations of the Cosmic Microwave
Background (CMB) and various type Ia supernova (SN Ia) catalogues. The
deviation observed in the cosmological constant ($\Lambda$) reflects a
departure from the standard cosmological model. Testing this deviation involves
examining the consistency between cosmological parameters derived from early
and late-time observations. Specifically, we focus on the matter density
parameter $\omega_m = \Omega_mh^2$ and introduce ${\rm ratio}(\omega_m)$ to
assess consistency, which is defined as the ratio of $\omega_m$ values
constrained by high and low-redshift measurements. This ratio serves as a
metric for quantifying deviations from the $\Lambda$CDM model. In this paper,
we find that the DESI BAO+CMB yields ${\rm ratio}(\omega_m)=1.0171\pm0.0066$.
Upon excluding the LRG1 and LRG2 data in DESI BAO, this ratio adjusts to ${\rm
ratio}(\omega_m)=1.0100\pm0.0082$. This shift, corresponding to a change from
$2.6\sigma$ to $1.2\sigma$, indicates that the deviation from the $\Lambda$CDM
model is predominantly driven by these two samples from the DESI BAO
measurements. To substantiate this conclusion, we utilized two cosmological
model-independent methods to reconstruct the cosmic expansion history. Both
reconstructions of the Hubble parameter $H(z)$ indicate that the evolving
features of dark energy are determined by the combined LRG1 and LRG2 data.
Therefore, different methods have reached the same conclusion, namely the
importance of accurately measuring the BAO feature in LRG1 and LRG2 data.
