• • • We do not use the following data for averages, fits, limits, etc. • • • 
$0.949$ $\pm0.0028$ 
^{ 1} 

DAYA 

^{ 2} 

DAYA 
$0.944$ $\pm0.007$ $\pm0.003$ 
^{ 3} 

DAYA 
$0.944$ $\pm0.016$ $\pm0.040$ 
^{ 4} 

DCHZ 
$0.920$ $\pm0.009$ $\pm0.014$ 
^{ 5} 

RENO 
$0.940$ $\pm0.011$ $\pm0.004$ 
^{ 6} 

DAYA 
$1.08$ $\pm0.21$ $\pm0.16$ 
^{ 7} 

TEXO 
$0.658$ $\pm0.044$ $\pm0.047$ 
^{ 8} 

KLND 
$0.611$ $\pm0.085$ $\pm0.041$ 
^{ 9} 

KLND 
$1.01$ $\pm0.024$ $\pm0.053$ 
^{ 10} 


$1.01$ $\pm0.028$ $\pm0.027$ 
^{ 11} 

CHOZ 
$0.987$ $\pm0.006$ $\pm0.037$ 
^{ 12} 


$0.988$ $\pm0.004$ $\pm0.05$ 


CNTR 
$0.994$ $\pm0.010$ $\pm0.05$ 


CNTR 
$0.915$ $\pm0.132$ $\pm0.05$ 


CNTR 
$0.987$ $\pm0.014$ $\pm0.027$ 
^{ 13} 

CNTR 
$0.985$ $\pm0.018$ $\pm0.034$ 


CNTR 
$1.05$ $\pm0.02$ $\pm0.05$ 



$0.955$ $\pm0.035$ $\pm0.110$ 
^{ 14} 


$0.89$ $\pm0.15$ 
^{ 14} 


^{1}
AN 2017A use 1230 days of data of the Daya Bay experiment. The reported deficit is based on the ratio of the ${{\overline{\mathit \nu}}_{{e}}}$ signal observed by the far detectors versus the near detectors and correcting for differences in detector exposure. Supersedes AN 2013 .

^{2}
AN 2016 use 217 days of data (338k events) to determine the neutrino flux ratio relative to the prediction of MuellerHuber and ILLVogel models (see AN 2016 for details). The reported flux ratios were corrected for ${{\mathit \theta}_{{13}}}$ oscillation effect. The flux measurement is consistent with results from previous shortbaseline reactor experiments. The measured inverse beta decay yield is ($1.55$ $\pm0.04$) $ \times 10^{18}$ cm${}^{2}$/(GW day) or $\sigma _{f}$ = ($5.92$ $\pm0.14$) $ \times 10^{43}$ cm${}^{2}$/fission. About 4$\sigma $ excess of events was observed in the $4  6$ MeV prompt energy region.

^{3}
AN 2013 use six identical detectors, with three placed near the reactor cores (fluxweighted baselines of 470 and 576 m) and the remaining three at the far hall (at the flux averaged distance of 1648 m from all six reactor cores) to determine the mixing angle ${{\mathit \theta}_{{13}}}$ using the ${{\overline{\mathit \nu}}_{{e}}}$ observed interaction rate ratios. This rateonly analysis excludes the nooscillation hypothesis at 7.7 standard deviations. The value of $\Delta $m${}^{2}_{31}$ = $2.32 \times 10^{3}$ eV${}^{2}$ was assumed in the analysis. This is an improved result (2.5 times increase in statistics) compared to AN 2012 . Superseded by AN 2017A.

^{4}
ABE 2012 determine the ${{\overline{\mathit \nu}}_{{e}}}$ interaction rate in a single detector, located 1050 m from the cores of two reactors. The rate normalization is fixed by the results of the Bugey4 reactor experiment, thus avoiding any dependence on possible very short baseline oscillations.

^{5}
AHN 2012 use two identical detectors, placed at flux weighted distances of 408.56 m and 1433.99m from six reactor cores, to determine the ${{\overline{\mathit \nu}}_{{e}}}$ interaction rate ratio.

^{6}
AN 2012 use six identical detectors with three placed near the reactor cores (fluxweighted baselines of 470 m and 576 m) and the remaining three at the far hall (at the flux averaged distance of 1648 m from all six reactor cores) to determine the ${{\overline{\mathit \nu}}_{{e}}}$ interaction rate ratios. Superseded by AN 2013 .

^{7}
DENIZ 2010 observe reactor ${{\overline{\mathit \nu}}_{{e}}}{{\mathit e}}$ scattering with recoil kinetic energies $3  8$ MeV using CsI(Tl) detectors. The observed rate is consistent with the Standard Model prediction, leading to a constraint on sin$^2{{\mathit \theta}_{{W}}}$ = $0.251$ $\pm0.031$(stat)$\pm0.024$(sys).

^{8}
Updated result of KamLAND, including the data used in EGUCHI 2003 . Note that the survival probabilities for different periods are not directly comparable because the effective baseline varies with power output of the reactor sources involved, and there were large variations in the reactor power production in Japan in 2003.

^{9}
EGUCHI 2003 observe reactor neutrino disappearance at $\sim{}180~$km baseline to various Japanese nuclear power reactors.

^{10}
BOEHM 2001 search for neutrino oscillations at $0.75$ and $0.89~$km distance from the Palo Verde reactors.

^{11}
APOLLONIO 1999 , APOLLONIO 1998 search for neutrino oscillations at $1.1~$km fixed distance from Chooz reactors. They use ${{\overline{\mathit \nu}}_{{e}}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit e}^{+}}{{\mathit n}}$ in Gdloaded scintillator target. APOLLONIO 1999 supersedes APOLLONIO 1998 . See also APOLLONIO 2003 for detailed description.

^{12}
GREENWOOD 1996 search for neutrino oscillations at 18$~$m and 24$~$m from the reactor at Savannah River.

^{13}
DECLAIS 1994 result based on integral measurement of neutrons only. Result is ratio of measured cross section to that expected in standard $\mathit V\mathit A$ theory. Replaced by ACHKAR 1995 .

^{14}
KWON 1981 represents an analysis of a larger set of data from the same experiment as BOEHM 1980 .
