Table 6.

Breakdown of ${10}^{10}\times a_{\mu }[\pi \pi ]$ by energy intervals. The displayed data for CHS18, DHMZ19 and KNT19 are extracted from Table 6 in [2]. The ${\text{EBHLS}}_2$ fits are reported using BaBar and KLOE10/12, and the latter only together with the NSK, BESIII and Cleo-c dipion spectra, globally referred to as X. The data collected in the 1980s [76] are also part of X

$\sqrt{s}$ Interval (GeV)	$\sqrt{s}\le 0.6$	$0.6\le \sqrt{s}\le 0.9$	$0.9\le \sqrt{s}\le 1.0$	$\sqrt{s}\le 1.0$
CHS18 [89]	$110.1\pm 0.9$	$369.6\pm 1.7$	$15.3\pm 0.1$	$495.0\pm 2.6$
DHMZ19 [90]	$110.4\pm 0.4\pm 0.5$	$371.5\pm 1.5\pm 2.3$	$15.5\pm 0.1\pm 0.2$	$497.4\pm 1.8\pm 3.1$
KNT19 [91]	$108.7\pm 0.9$	$369.8\pm 1.3$	$15.3\pm 0.1$	$493.8\pm 1.9$
KLOE + BaBar + X	${\chi }^2/N_{\mathit{pts}}$: BaBar = 1.45, KLOE = 1.15, NSK = 1.10
Prob = 11.4%	$108.83\pm 0.09$	$369.06\pm 0.62$	$15.36\pm 0.38$	$493.19\pm 0.73$
KLOE +X	${\chi }^2/N_{\mathit{pts}}$: KLOE = 1.03, NSK = 1.09
Prob = 90.0% (incl. $\tau$)	$107.79\pm 0.12$	$366.76\pm 0.73$	$15.16\pm 0.42$	$489.70\pm 0.84$
Prob = 93.3% (excl. $\tau$)	$107.67\pm 0.13$	$367.21\pm 0.84$	$15.17\pm 0.48$	$490.05\pm 0.98$