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${{\mathit \phi}{(1020)}}$ WIDTH

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VALUE (MeV) EVTS DOCUMENT ID TECN  COMMENT $\bf{ 4.249 \pm0.013}$ OUR AVERAGE  Error includes scale factor of 1.1. $4.212$ $\pm0.20$ $\pm0.13$ 1.28M 1 ACHASOV 2024 SND ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit K}_L^0}$ ${{\mathit K}_S^0}$ $4.245$ $\pm0.013$ 2.3M 2 KOZYREV 2018 CMD3 ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit K}^{+}}{{\mathit K}^{-}}$ , ${{\mathit K}_S^0}$ ${{\mathit K}_L^0}$ $4.205$ $\pm0.103$ $\pm0.067$ 28k 3 LEES 2014 H BABR ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit K}_S^0}$ ${{\mathit K}_L^0}$ ${{\mathit \gamma}}$ $4.29$ $\pm0.04$ $\pm0.07$ 4 LEES 2013 Q BABR ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit K}^{+}}{{\mathit K}^{-}}{{\mathit \gamma}}$ $4.30$ $\pm0.06$ $\pm0.17$ 105k AKHMETSHIN 2006 CMD2 $0.98 - 1.06$ ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \pi}^{+}}{{\mathit \pi}^{-}}{{\mathit \pi}^{0}}$ $4.280$ $\pm0.033$ $\pm0.025$ 272k 5 AKHMETSHIN 2004 CMD2 ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit K}_L^0}$ ${{\mathit K}_S^0}$ $4.21$ $\pm0.04$ 1900k 6 ACHASOV 2001 E SND ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit K}^{+}}{{\mathit K}^{-}}$, ${{\mathit K}_{{{S}}}}{{\mathit K}_{{{L}}}}$, ${{\mathit \pi}^{+}}{{\mathit \pi}^{-}}{{\mathit \pi}^{0}}$ $4.44$ $\pm0.09$ 55600 AKHMETSHIN 1995 CMD2 ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ hadrons $4.5$ $\pm0.7$ 1500 ARENTON 1982 AEMS 11.8 polar. ${{\mathit p}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit K}}{{\mathit K}}$ $4.2$ $\pm0.6$ 766 7 IVANOV 1981 OLYA 1$-$1.4 ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit K}^{+}}{{\mathit K}^{-}}$ $4.3$ $\pm0.6$ 7 CORDIER 1980 DM1 ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \pi}^{+}}{{\mathit \pi}^{-}}{{\mathit \pi}^{0}}$ $4.36$ $\pm0.29$ 3681 7 BUKIN 1978 C OLYA ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ hadrons $4.4$ $\pm0.6$ 984 7 BESCH 1974 CNTR 2 ${{\mathit \gamma}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit p}}{{\mathit K}^{+}}{{\mathit K}^{-}}$ $4.67$ $\pm0.72$ 681 7 BALAKIN 1971 OSPK ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ hadrons $4.09$ $\pm0.29$ BIZOT 1970 OSPK ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ hadrons • • We do not use the following data for averages, fits, limits, etc. • • $4.151$ $\pm0.018$ 8 DUBNICKA 2024 RVUE ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit K}^{+}}{{\mathit K}^{-}}$ , ${{\mathit K}_S^0}$ ${{\mathit K}_L^0}$ $4.681$ $\pm0.277$ 34M 9 IGNATOV 2024 CMD3 ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \pi}^{+}}{{\mathit \pi}^{-}}$ $4.07$ $\pm0.13$ $\pm0.01$ 10 HOID 2020 RVUE ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \pi}^{0}}{{\mathit \gamma}}$ $4.23$ $\pm0.04$ $\pm0.02$ 11 HOFERICHTER 2019 RVUE ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \pi}^{+}}{{\mathit \pi}^{-}}{{\mathit \pi}^{0}}$ $4.249$ $\pm0.015$ 1.7M KOZYREV 2018 CMD3 ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit K}^{+}}{{\mathit K}^{-}}$ $4.240$ $\pm0.017$ 610k KOZYREV 2016 CMD3 ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit K}_S^0}$ ${{\mathit K}_L^0}$ $4.37$ $\pm0.02$ LEES 2013 F BABR ${{\mathit D}^{+}}$ $\rightarrow$ ${{\mathit K}^{+}}{{\mathit K}^{-}}{{\mathit \pi}^{+}}$ $4.24$ $\pm0.02$ $\pm0.03$ 542k 12 AKHMETSHIN 2008 CMD2 1.02 ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit K}^{+}}{{\mathit K}^{-}}$ $4.28$ $\pm0.13$ 12540 13 AUBERT,B 2005 J BABR ${{\mathit D}^{0}}$ $\rightarrow$ ${{\overline{\mathit K}}^{0}}{{\mathit K}^{+}}{{\mathit K}^{-}}$ $4.45$ $\pm0.06$ 271k DIJKSTRA 1986 SPEC 100 ${{\mathit \pi}^{-}}{}^{}\mathrm {Be}$ $3.6$ $\pm0.8$ 337 7 COOPER 1978 B HBC 0.7$-$0.8 ${{\overline{\mathit p}}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit K}_S^0}$ ${{\mathit K}_L^0}$ ${{\mathit \pi}^{+}}{{\mathit \pi}^{-}}$ $4.5$ $\pm0.50$ 1300 13, 7 AKERLOF 1977 SPEC 400 ${{\mathit p}}$ ${}^{}\mathrm {A}$ $\rightarrow$ ${{\mathit K}^{+}}{{\mathit K}^{-}}$ X $4.5$ $\pm0.8$ 500 13, 7 AYRES 1974 ASPK 3$-$6 ${{\mathit \pi}^{-}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit K}^{+}}{{\mathit K}^{-}}{{\mathit n}}$, ${{\mathit K}^{-}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit K}^{+}}{{\mathit K}^{-}}{{\mathit \Lambda}}$ $/{{\mathit \Sigma}^{0}}$ $3.81$ $\pm0.37$ COSME 1974 B OSPK ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit K}_L^0}$ ${{\mathit K}_S^0}$ $3.8$ $\pm0.7$ 454 7 BORENSTEIN 1972 HBC 2.18 ${{\mathit K}^{-}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit K}}{{\overline{\mathit K}}}{{\mathit n}}$ 1  From a fit of the cross section in the energy region 1.000 $<$ $\sqrt {s }$ $<$ 1.100 GeV using a vector meson dominance model with contribution from ${{\mathit \phi}{(1020)}}$, ${{\mathit \rho}{(770)}}$, ${{\mathit \omega}{(782)}}$ and higher vector resonances. The the first three points near the threshold are removed in the fit. 2  Average of KOZYREV 2016 and KOZYREV 2018 values taking into account the correlated uncertainties. Supersedes individual KOZYREV 2016 and KOZYREV 2018 results. 3  Using a vector meson dominance model with contribution from ${{\mathit \phi}{(1020)}}$ and higher mass excitations of ${{\mathit \rho}{(770)}}$, ${{\mathit \omega}{(782)}}$, and ${{\mathit \phi}{(1020)}}$. 4  Using a phenomenological model based on KUHN 1990 with a sum of Breit-Wigner resonances for ${{\mathit \rho}{(770)}}$, ${{\mathit \omega}{(782)}}$, ${{\mathit \phi}{(1020)}}$ and their higher mass excitations. 5  Update of AKHMETSHIN 1999D 6  From the combined fit assuming that the total ${{\mathit \phi}{(1020)}}$ production cross section is saturated by those of ${{\mathit K}^{+}}{{\mathit K}^{-}}$, ${{\mathit K}_{{{S}}}}{{\mathit K}_{{{L}}}}$, ${{\mathit \pi}^{+}}{{\mathit \pi}^{-}}{{\mathit \pi}^{0}}$, and ${{\mathit \eta}}{{\mathit \gamma}}$ decays modes and using ACHASOV 2000B for the ${{\mathit \eta}}{{\mathit \gamma}}$ decay mode. 7  Width errors enlarged by us to 4${}\Gamma /\sqrt {\mathit N }$; see the note with the ${{\mathit K}^{*}{(892)}}$ mass. 8  From the fit to data of CMD3, BABAR and BES3. 9  From a fit of the pion form factor in the energy range 0.32 $<$ $\sqrt {s }$ $<$ 1.2 GeV using the GOUNARIS 1968 parametrization with the complex phase of the ${{\mathit \rho}}−{{\mathit \omega}}$ interference leaving ${{\mathit \rho}{(1450)}}$, ${{\mathit \rho}{(1700)}}$ resonances as free parameters of the fit. Systematic errors not estimated. 10  The values were extracted from a dispersively improved Breit-Wigner parameterization. 11  The values were extracted from a dispersively improved Breit-Wigner parameterization and do not include vacuum polarization. 12  Strongly correlated with AKHMETSHIN 2004. 13  Systematic errors not evaluated.

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