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${{\mathit \rho}{(1700)}}$ WIDTH

2 ( ${{\mathit \pi}^{+}}{{\mathit \pi}^{-}}$ ) MODE

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M065W4

M065W4 VALUE (MeV) EVTS DOCUMENT ID TECN  COMMENT • • We do not use the following data for averages, fits, limits, etc. • • $357$ $\pm31$ $\pm49$ 1 ACHARYA 2026   ALCE 5 TeV ${}^{}\mathrm {Pb}$ ${}^{}\mathrm {Pb}$ $\rightarrow$ ${}^{}\mathrm {Pb}$ ${}^{}\mathrm {Pb}$ 4 ${{\mathit \pi}}$ $510$ $\pm40$ 2 CORDIER 1982   DM1 ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ 2( ${{\mathit \pi}^{+}}{{\mathit \pi}^{-}}$) $400$ $\pm50$ 3 ASTON 1981 E   OMEG 20$-$70 ${{\mathit \gamma}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit p}}$4 ${{\mathit \pi}}$ $400$ $\pm146$ 4 DIBIANCA 1981   DBC ${{\mathit \pi}^{+}}$ ${{\mathit d}}$ $\rightarrow$ ${{\mathit p}}{{\mathit p}}$2( ${{\mathit \pi}^{+}}{{\mathit \pi}^{-}}$) $700$ $\pm160$ 2 BACCI 1980   FRAG ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ 2( ${{\mathit \pi}^{+}}{{\mathit \pi}^{-}}$) $100$ 34 KILLIAN 1980   SPEC 11 ${{\mathit e}^{-}}$ ${{\mathit p}}$ $\rightarrow$ 2( ${{\mathit \pi}^{+}}{{\mathit \pi}^{-}}$) $600$ 5 ATIYA 1979 B   SPEC 50 ${{\mathit \gamma}}$ ${}^{}\mathrm {C}$ $\rightarrow$ ${}^{}\mathrm {C}$ 4 ${{\mathit \pi}^{\pm}}$ $340$ $\pm160$ 65 6 ALEXANDER 1975   HBC 7.5 ${{\mathit \gamma}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit p}}$4 ${{\mathit \pi}}$ $360$ $\pm100$ 3 CONVERSI 1974   OSPK ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ 2( ${{\mathit \pi}^{+}}{{\mathit \pi}^{-}}$) $400$ $\pm120$ 160 7 SCHACHT 1974   STRC 5.5$-$9 ${{\mathit \gamma}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit p}}$4 ${{\mathit \pi}}$ $850$ $\pm200$ 340 7 SCHACHT 1974   STRC 9$-$18 ${{\mathit \gamma}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit p}}$4 ${{\mathit \pi}}$ $650$ $\pm100$ 400 BINGHAM 1972 B   HBC 9.3 ${{\mathit \gamma}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit p}}$4 ${{\mathit \pi}}$ 1  From a two Breit-Wigner resonance fit to the 4${{\mathit \pi}}$ mass distribution produced in ultraperipheral ${}^{}\mathrm {Pb}−{}^{}\mathrm {Pb}$ collisions. 2  Simple relativistic Breit-Wigner fit with model-dependent width. 3  Simple relativistic Breit-Wigner fit with constant width. 4  One peak fit result. 5  Parameters roughly estimated, not from a fit. 6  Skew mass distribution compensated by Ross-Stodolsky factor. 7  Width errors enlarged by us to 4${}\Gamma /\sqrt {\mathit N }$; see the note with the ${{\mathit K}^{*}{(892)}}$ mass.

References

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