$7.53$ $\pm0.18$ |
1 |
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FIT |
• • • We do not use the following data for averages, fits, limits, etc. • • • |
$7.55$ ${}^{+0.20}_{-0.16}$ |
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FIT |
$7.49$ ${}^{+0.19}_{-0.18}$ |
2 |
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FIT |
$4.8$ ${}^{+1.3}_{-0.6}$ |
3 |
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FIT |
$4.8$ ${}^{+1.5}_{-0.8}$ |
4 |
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FIT |
$3.2$ ${}^{+2.8}_{-0.2}$ |
5 |
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FIT |
$7.6$ ${}^{+0.19}_{-0.18}$ |
6 |
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FIT |
$7.50$ ${}^{+0.19}_{-0.17}$ |
7 |
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FIT |
$5.13$ ${}^{+1.29}_{-0.96}$ |
8, 9 |
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FIT |
$5.13$ ${}^{+1.49}_{-0.98}$ |
10, 9 |
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FIT |
$7.46$ ${}^{+0.20}_{-0.19}$ |
11, 9 |
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FIT |
$7.53$ ${}^{+0.19}_{-0.18}$ |
12 |
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FIT |
$7.54$ ${}^{+0.19}_{-0.18}$ |
13 |
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FIT |
$7.6$ $\pm0.2$ |
14 |
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FIT |
$6.2$ ${}^{+1.1}_{-1.9}$ |
15 |
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FIT |
$7.7$ $\pm0.3$ |
16 |
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FIT |
$6.0$ ${}^{+2.2}_{-2.5}$ |
17 |
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FIT |
$7.50$ ${}^{+0.16}_{-0.24}$ |
18 |
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FIT |
$5.2$ ${}^{+1.5}_{-0.9}$ |
19 |
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FIT |
$7.50$ ${}^{+0.19}_{-0.20}$ |
20 |
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FIT |
$7.49$ $\pm0.20$ |
21 |
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FIT |
$7.59$ ${}^{+0.20}_{-0.21}$ |
22, 23 |
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FIT |
$5.89$ ${}^{+2.13}_{-2.16}$ |
22, 24 |
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FIT |
$7.59$ $\pm0.21$ |
22, 25 |
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FIT |
$6.31$ ${}^{+2.49}_{-2.58}$ |
22, 26 |
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FIT |
$7.58$ ${}^{+0.14}_{-0.13}$ $\pm0.15$ |
27 |
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FIT |
$7.59$ $\pm0.21$ |
28 |
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FIT |
$7.59$ ${}^{+0.19}_{-0.21}$ |
29 |
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FIT |
$8.0$ $\pm0.3$ |
30 |
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FIT |
$8.0$ $\pm0.3$ |
31 |
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FIT |
$6.3$ ${}^{+3.7}_{-1.5}$ |
32 |
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FIT |
$\text{5 - 12}$ |
33 |
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FIT |
$8.0$ ${}^{+0.4}_{-0.3}$ |
34 |
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FIT |
$\text{3.3 - 14.4}$ |
35 |
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FIT |
$7.9$ ${}^{+0.4}_{-0.3}$ |
36 |
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FIT |
$7.1$ ${}^{+1.0}_{-0.3}$ |
37 |
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FIT |
$\text{3.2 - 13.7}$ |
38 |
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FIT |
$7.1$ ${}^{+0.6}_{-0.5}$ |
39 |
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FIT |
$6.0$ ${}^{+1.7}_{-1.6}$ |
40 |
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FIT |
$6.0$ ${}^{+2.5}_{-1.6}$ |
41 |
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FIT |
$\text{2.8 - 12.0}$ |
42 |
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FIT |
$\text{3.2 - 19.1}$ |
43 |
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FIT |
1
GANDO 2013 obtained this result by a three-neutrino oscillation analysis using KamLAND, global solar neutrino, short-baseline (SBL) reactor, and accelerator data, assuming CPT invariance. Supersedes GANDO 2011 .
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2
ABE 2016C obtained this result by a three-neutrino oscillation analysis, with a constraint of sin$^2({{\mathit \theta}_{{13}}})$ = $0.0219$ $\pm0.0014$ coming from reactor neutrino experiments, using all solar data and KamLAND data. $\mathit CPT$ invariance is assumed.
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3
ABE 2016C obtained this result by a three-neutrino oscillation analysis, with a constraint of sin$^2({{\mathit \theta}_{{13}}})$ = $0.0219$ $\pm0.0014$ coming from reactor neutrino experiments, using Super-Kamiokande (I+II+III+IV) and SNO data.
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4
ABE 2016C obtained this result by a three-neutrino oscillation analysis, with a constraint of sin$^2({{\mathit \theta}_{{13}}})$ = $0.0219$ $\pm0.0014$ coming from reactor neutrino experiments, by combining the four phases of the Super-Kamiokande solar data.
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5
ABE 2016C obtained this result by a three-neutrino oscillation analysis, with a constraint of sin$^2({{\mathit \theta}_{{13}}})$ = $0.0219$ $\pm0.0014$ coming from reactor neutrino experiments, using the Super-Kamiokande-IV data.
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6
FORERO 2014 performs a global fit to $\Delta $m${}^{2}_{21}$ using solar, reactor, long-baseline accelerator, and atmospheric neutrino data.
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7
GONZALEZ-GARCIA 2014 result comes from a frequentist global fit. The corresponding Bayesian global fit to the same data results are reported in BERGSTROM 2015 as ($7.50$ ${}^{+0.19}_{-0.17}$) $ \times 10^{-5}$ eV${}^{2}$ for normal and ($7.50$ ${}^{+0.18}_{-0.17}$) $ \times 10^{-5}$ eV${}^{2}$ for inverted mass ordering.
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8
AHARMIM 2013 obtained this result by a two-neutrino oscillation analysis using global solar neutrino data.
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9
AHARMIM 2013 global solar neutrino data include SNO's all-phases-combined analysis results on the total active ${}^{8}\mathrm {B}$ neutrino flux and energy-dependent ${{\mathit \nu}_{{e}}}$ survival probability parameters, measurements of ${}^{}\mathrm {Cl}$ (CLEVELAND 1998 ), ${}^{}\mathrm {Ga}$ (ABDURASHITOV 2009 which contains combined analysis with GNO (ALTMANN 2005 and Ph.D. thesis of F. Kaether)), and ${}^{7}\mathrm {Be}$ (BELLINI 2011A) rates, and ${}^{8}\mathrm {B}$ solar-neutrino recoil electron measurements of SK-I (HOSAKA 2006 ) zenith, SK-II (CRAVENS 2008 ), and SK-III (ABE 2011 ) day/night spectra, and Borexino (BELLINI 2010A) spectra.
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10
AHARMIM 2013 obtained this result by a three-neutrino oscillation analysis with the value of $\Delta {{\mathit m}^{2}}_{\mathrm {31}}$ fixed to $2.45 \times 10^{-3}$ eV${}^{2}$, using global solar neutrino data.
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11
AHARMIM 2013 obtained this result by a three-neutrino oscillation analysis with the value of $\Delta {{\mathit m}^{2}}_{\mathrm {31}}$ fixed to $2.45 \times 10^{-3}$ eV${}^{2}$, using global solar neutrino and KamLAND data (GANDO 2011 ). CPT invariance is assumed.
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12
GANDO 2013 obtained this result by a three-neutrino oscillation analysis using KamLAND and global solar neutrino data, assuming CPT invariance. Supersedes GANDO 2011 .
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13
GANDO 2013 obtained this result by a three-neutrino oscillation analysis using KamLAND data. Supersedes GANDO 2011 .
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14
ABE 2011 obtained this result by a two-neutrino oscillation analysis using solar neutrino data including Super-Kamiokande, SNO, Borexino (ARPESELLA 2008A), Homestake, GALLEX/GNO, SAGE, and KamLAND data. CPT invariance is assumed.
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15
ABE 2011 obtained this result by a two-neutrino oscillation analysis using solar neutrino data including Super-Kamiokande, SNO, Borexino (ARPESELLA 2008A), Homestake, GALLEX/GNO, and SAGE data.
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16
ABE 2011 obtained this result by a three-neutrino oscillation analysis with the value of $\Delta {{\mathit m}^{2}}_{\mathrm {32}}$ fixed to $2.4 \times 10^{-3}$ eV${}^{2}$, using solar neutrino data including Super-Kamiokande, SNO, Borexino (ARPESELLA 2008A), Homestake, GALLEX/GNO, SAGE, and KamLAND data. The normal neutrino mass ordering and CPT invariance are assumed.
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17
ABE 2011 obtained this result by a three-neutrino oscillation analysis with the value of $\Delta {{\mathit m}^{2}}_{\mathrm {32}}$ fixed to $2.4 \times 10^{-3}$ eV${}^{2}$, using solar neutrino data including Super-Kamiokande, SNO, Borexino (ARPESELLA 2008A), Homestake, and GALLEX/GNO data. The normal neutrino mass ordering is assumed.
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18
BELLINI 2011A obtained this result by a two-neutrino oscillation analysis using KamLAND, Homestake, SAGE, Gallex, GNO, Kamiokande, Super-Kamiokande, SNO, and Borexino (BELLINI 2011A) data and the SSM flux prediction in SERENELLI 2011 (Astrophysical Journal 743 24 (2011)) with the exception that the ${}^{8}\mathrm {B}$ flux was left free. CPT invariance is assumed.
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19
BELLINI 2011A obtained this result by a two-neutrino oscillation analysis using Homestake, SAGE, Gallex, GNO, Kamiokande, Super-Kamiokande, SNO, and Borexino (BELLINI 2011A) data and the SSM flux prediction in SERENELLI 2011 (Astrophysical Journal 743 24 (2011)) with the exception that the ${}^{8}\mathrm {B}$ flux was left free.
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20
GANDO 2011 obtain this result with three-neutrino fit using the KamLAND + solar data. Superseded by GANDO 2013 .
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21
GANDO 2011 obtain this result with three-neutrino fit using the KamLAND data only. Supersedes ABE 2008A.
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22
AHARMIM 2010 global solar neutrino data include SNO's low-energy-threshold analysis survival probability day/night curves, SNO Phase III integral rates (AHARMIM 2008 ), Cl (CLEVELAND 1998 ), SAGE (ABDURASHITOV 2009 ), Gallex/GNO (HAMPEL 1999 , ALTMANN 2005 ), Borexino (ARPESELLA 2008A), SK-I zenith (HOSAKA 2006 ), and SK-II day/night spectra (CRAVENS 2008 ).
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23
AHARMIM 2010 obtained this result by a two-neutrino oscillation analysis using global solar neutrino data and KamLAND data (ABE 2008A). $\mathit CPT$ invariance is assumed.
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24
AHARMIM 2010 obtained this result by a two-neutrino oscillation analysis using global solar neutrino data.
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25
AHARMIM 2010 obtained this result by a three-neutrino oscillation analysis with the value of $\Delta $ fixed to $2.3 \times 10^{-3}$ eV${}^{2}$, using global solar neutrino data and KamLAND data (ABE 2008A). $\mathit CPT$ invariance is assumed.
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26
AHARMIM 2010 obtained this result by a three-neutrino oscillation analysis with the value of $\Delta $ fixed to $2.3 \times 10^{-3}$ eV${}^{2}$, using global solar neutrino data.
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27
ABE 2008A obtained this result by a rate + shape + time combined geoneutrino and reactor two-neutrino fit for $\Delta $ and tan $^2\theta _{12}$, using KamLAND data only. Superseded by GANDO 2011 .
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28
ABE 2008A obtained this result by means of a two-neutrino fit using KamLAND, Homestake, SAGE, GALLEX, GNO, SK (zenith angle and E-spectrum), the SNO $\chi {}^{2}$-map, and solar flux data. $\mathit CPT$ invariance is assumed. Superseded by GANDO 2011 .
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29
AHARMIM 2008 obtained this result by a two-neutrino oscillation analysis using all solar neutrino data including those of Borexino (ARPESELLA 2008A) and Super-Kamiokande-I (HOSAKA 2006 ), and KamLAND data (ABE 2008A). $\mathit CPT$ invariance is assumed.
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30
HOSAKA 2006 obtained this result by a two-neutrino oscillation analysis using solar neutrino and KamLAND data (ARAKI 2005 ). $\mathit CPT$ invariance is assumed.
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31
HOSAKA 2006 obtained this result by a two-neutrino oscillation analysis using the data from Super-Kamiokande, SNO (AHMAD 2002 and AHMAD 2002B), and KamLAND (ARAKI 2005 ) experiments. $\mathit CPT$ invariance is assumed.
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32
HOSAKA 2006 obtained this result by a two-neutrino oscillation analysis using the Super-Kamiokande and SNO (AHMAD 2002 and AHMAD 2002B) solar neutrino data.
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33
HOSAKA 2006 obtained this result from the consistency between the observed and expected day-night flux asymmetry amplitude. The listed 68$\%$ CL range is derived from the 1$\sigma $ boundary of the amplitude fit to the data. Oscillation parameters are constrained to be in the LMA region. The mixing angle is fixed at tan $^2\theta $ = 0.44 because the fit depends only very weekly on it.
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34
AHARMIM 2005A obtained this result by a two-neutrino oscillation analysis using solar neutrino and KamLAND data (ARAKI 2005 ). $\mathit CPT$ invariance is assumed. AHARMIM 2005A also quotes $\Delta \mathit m{}^{2}$ = ($8.0$ ${}^{+0.6}_{-0.4}$) $ \times 10^{-5}$ eV${}^{2}$ as the error enveloping the 68$\%$ CL two-dimensional region.
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35
AHARMIM 2005A obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The listed range of the parameter envelops the 95$\%$ CL two-dimensional region shown in figure 35a of AHARMIM 2005A. AHARMIM 2005A also quotes $\Delta \mathit m{}^{2}$ = ($6.5$ ${}^{+4.4}_{-2.3}$) $ \times 10^{-5}$ eV${}^{2}$ as the error enveloping the 68$\%$ CL two-dimensional region.
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36
ARAKI 2005 obtained this result by a two-neutrino oscillation analysis using KamLAND and solar neutrino data. $\mathit CPT$ invariance is assumed. The 1$\sigma $ error shown here is provided by the KamLAND collaboration. The error quoted in ARAKI 2005 , $\Delta \mathit m{}^{2}$ = ($7.9$ ${}^{+0.6}_{-0.5}$) $ \times 10^{-5}$, envelops the 68$\%$ CL two-dimensional region.
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37
AHMED 2004A obtained this result by a two-neutrino oscillation analysis using solar neutrino and KamLAND data (EGUCHI 2003 ). $\mathit CPT$ invariance is assumed. AHMED 2004A also quotes $\Delta \mathit m{}^{2}$ = ($7.1$ ${}^{+1.2}_{-0.6}$) $ \times 10^{-5}$ eV${}^{2}$ as the error enveloping the 68$\%$ CL two-dimensional region.
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38
AHMED 2004A obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The listed range of the parameter envelops the 95$\%$ CL two-dimensional region shown in Fig. 5(a) of AHMED 2004A. The best-fit point is $\Delta \mathit m{}^{2}$ = $6.5 \times 10^{-5}$ eV${}^{2}$, tan $^2\theta $ = $0.40$ (sin$^22 \theta $ = $0.82$).
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39
SMY 2004 obtained this result by a two-neutrino oscillation analysis using solar neutrino and KamLAND data (IANNI 2003 ). $\mathit CPT$ invariance is assumed.
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40
SMY 2004 obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The 1$\sigma $ errors are read from Fig. 6(a) of SMY 2004 .
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41
SMY 2004 obtained this result by a two-neutrino oscillation analysis using the Super-Kamiokande and SNO (AHMAD 2002 and AHMAD 2002B) solar neutrino data. The 1$\sigma $ errors are read from Fig. 6(a) of SMY 2004 .
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42
AHMAD 2002B obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The listed range of the parameter envelops the 95$\%$ CL two-dimensional region shown in Fig. 4(b) of AHMAD 2002B. The best fit point is $\Delta \mathit m{}^{2}$ = $5.0 \times 10^{-5}$ eV${}^{2}$ and tan $\theta $ = $0.34$ (sin$^22 \theta $ = 0.76).
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43
FUKUDA 2002 obtained this result by a two-neutrino oscillation analysis using the data from all solar neutrino experiments. The listed range of the parameter envelops the 95$\%$ CL two-dimensional region shown in Fig. 4 of FUKUDA 2002 . The best fit point is $\Delta \mathit m{}^{2}$ = $6.9 \times 10^{-5}$ eV${}^{2}$ and tan $^2\theta $ = $0.38$ (sin$^22 \theta $ = 0.80).
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