• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt;10</td><td>p</td><td>90</td><td>0</td><td>0.8</td><td>BERGER</td><td>91</td><td>FREJ</td></tr><tr><td>&gt;52</td><td>p</td><td>90</td><td>2</td><td>1.55</td><td>HIRATA</td><td>89c</td><td>KAMI</td></tr><tr><td>&gt;10</td><td>p</td><td>90</td><td>1</td><td>&lt;1</td><td>ARISAKA</td><td>85</td><td>KAMI</td></tr></table>

$\tau(N \to \nu K^*(892))$

T22

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;51</td><td>p</td><td>90</td><td>7</td><td>9.1</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr><tr><td>&gt;78</td><td>n</td><td>90</td><td>40</td><td>50</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt;22</td><td>p</td><td>90</td><td>0</td><td>2.1</td><td>BERGER</td><td>89</td><td>FREJ</td></tr><tr><td>&gt;17</td><td>p</td><td>90</td><td>0</td><td>2.4</td><td>BERGER</td><td>89</td><td>FREJ</td></tr><tr><td>&gt;20</td><td>p</td><td>90</td><td>5</td><td>2.1</td><td>HIRATA</td><td>89c</td><td>KAMI</td></tr><tr><td>&gt;21</td><td>n</td><td>90</td><td>4</td><td>2.4</td><td>HIRATA</td><td>89c</td><td>KAMI</td></tr><tr><td>&gt;10</td><td>p</td><td>90</td><td>7</td><td>6</td><td>HAINES</td><td>86</td><td>IMB</td></tr><tr><td>&gt; 5</td><td>n</td><td>90</td><td>8</td><td>7</td><td>HAINES</td><td>86</td><td>IMB</td></tr><tr><td>&gt; 8</td><td>p</td><td>90</td><td>3</td><td>2</td><td>KAJITA</td><td>86</td><td>KAMI</td></tr><tr><td>&gt; 6</td><td>n</td><td>90</td><td>2</td><td>1.6</td><td>KAJITA</td><td>86</td><td>KAMI</td></tr><tr><td>&gt; 5.8</td><td>p (free)</td><td>90</td><td>10</td><td>16</td><td>BLEWITT</td><td>85</td><td>IMB</td></tr><tr><td>&gt; 9.6</td><td>p</td><td>90</td><td>7</td><td>6</td><td>BLEWITT</td><td>85</td><td>IMB</td></tr><tr><td>&gt; 7</td><td>n</td><td>90</td><td>1</td><td>4</td><td>PARK</td><td>85</td><td>IMB</td></tr><tr><td>&gt; 2.1</td><td>p</td><td>90</td><td>1</td><td>1</td><td>1 BATTISTONI</td><td>82</td><td>NUSX</td></tr></table>

¹ We have converted 1 possible event to 90% CL limit.

Antilepton + mesons

$\tau(p \to e^+ \pi^+ \pi^-)$

T23

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;82</td><td>p</td><td>90</td><td>16</td><td>23.1</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt;21</td><td>p</td><td>90</td><td>0</td><td>2.2</td><td>BERGER</td><td>91</td><td>FREJ</td></tr></table>

$\tau(p \to e^+ \pi^0 \pi^0)$

T24

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;147</td><td>p</td><td>90</td><td>2</td><td>0.8</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 38</td><td>p</td><td>90</td><td>1</td><td>0.5</td><td>BERGER</td><td>91</td><td>FREJ</td></tr></table>

$\tau(n \to e^+ \pi^- \pi^0)$

T25

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;52</td><td>n</td><td>90</td><td>38</td><td>34.2</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt;32</td><td>n</td><td>90</td><td>1</td><td>0.8</td><td>BERGER</td><td>91</td><td>FREJ</td></tr></table>

$\tau(p \to \mu^+ \pi^+ \pi^-)$

T26

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;133</td><td>p</td><td>90</td><td>25</td><td>38.0</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 17</td><td>p</td><td>90</td><td>1</td><td>2.6</td><td>BERGER</td><td>91</td><td>FREJ</td></tr><tr><td>&gt; 3.3</td><td>p</td><td>90</td><td>0</td><td>0.7</td><td>PHILLIPS</td><td>89</td><td>HPW</td></tr></table>

$\tau(p \to \mu^+ \pi^0 \pi^0)$

T27

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;101</td><td>p</td><td>90</td><td>3</td><td>1.6</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 33</td><td>p</td><td>90</td><td>1</td><td>0.9</td><td>BERGER</td><td>91</td><td>FREJ</td></tr></table>

$\tau(n \to \mu^+ \pi^- \pi^0)$

T28

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;74</td><td>n</td><td>90</td><td>17</td><td>20.8</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt;33</td><td>n</td><td>90</td><td>0</td><td>1.1</td><td>BERGER</td><td>91</td><td>FREJ</td></tr></table>

$\tau(n \to e^+ K^0 \pi^-)$

T29

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;18</td><td>n</td><td>90</td><td>1</td><td>0.2</td><td>BERGER</td><td>91</td><td>FREJ</td></tr></tbody></table>

Lepton + meson

$\tau(n \to e^- \pi^+)$

T30

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;65</td><td>n</td><td>90</td><td>0</td><td>1.6</td><td>SEIDEL</td><td>88</td><td>IMB</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt;55</td><td>n</td><td>90</td><td>0</td><td>1.09</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr><tr><td>&gt;16</td><td>n</td><td>90</td><td>9</td><td>7</td><td>HAINES</td><td>86</td><td>IMB</td></tr><tr><td>&gt;25</td><td>n</td><td>90</td><td>2</td><td>4</td><td>PARK</td><td>85</td><td>IMB</td></tr></table>

$\tau(n \to \mu^- \pi^+)$

T31

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;49</td><td>n</td><td>90</td><td>0</td><td>0.5</td><td>SEIDEL</td><td>88</td><td>IMB</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt;33</td><td>n</td><td>90</td><td>0</td><td>1.40</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr><tr><td>&gt; 2.7</td><td>n</td><td>90</td><td>0</td><td>0.7</td><td>PHILLIPS</td><td>89</td><td>HPW</td></tr><tr><td>&gt;25</td><td>n</td><td>90</td><td>7</td><td>6</td><td>HAINES</td><td>86</td><td>IMB</td></tr><tr><td>&gt;27</td><td>n</td><td>90</td><td>2</td><td>3</td><td>PARK</td><td>85</td><td>IMB</td></tr></table>

$\tau(n \to e^- \rho^+)$

T32

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;62</td><td>n</td><td>90</td><td>2</td><td>4.1</td><td>SEIDEL</td><td>88</td><td>IMB</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt;12</td><td>n</td><td>90</td><td>13</td><td>6</td><td>HAINES</td><td>86</td><td>IMB</td></tr><tr><td>&gt;12</td><td>n</td><td>90</td><td>5</td><td>3</td><td>PARK</td><td>85</td><td>IMB</td></tr></table>

$\tau(n \to \mu^- \rho^+)$

T33

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;7</td><td>n</td><td>90</td><td>1</td><td>1.1</td><td>SEIDEL</td><td>88</td><td>IMB</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt;2.6</td><td>n</td><td>90</td><td>0</td><td>0.7</td><td>PHILLIPS</td><td>89</td><td>HPW</td></tr><tr><td>&gt;9</td><td>n</td><td>90</td><td>7</td><td>5</td><td>HAINES</td><td>86</td><td>IMB</td></tr><tr><td>&gt;9</td><td>n</td><td>90</td><td>2</td><td>2</td><td>PARK</td><td>85</td><td>IMB</td></tr></table>

$\tau(n \to e^- K^+)$

T34

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;32</td><td>n</td><td>90</td><td>3</td><td>2.96</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 0.23</td><td>n</td><td>90</td><td>0</td><td>0.7</td><td>PHILLIPS</td><td>89</td><td>HPW</td></tr></table>

$\tau(n \to \mu^- K^+)$

T35

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;57</td><td>n</td><td>90</td><td>0</td><td>2.18</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 4.7</td><td>n</td><td>90</td><td>0</td><td>0.7</td><td>PHILLIPS</td><td>89</td><td>HPW</td></tr></table>

Lepton + mesons

$\tau(p \to e^- \pi^+ \pi^+)$

T36

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;30</td><td>p</td><td>90</td><td>1</td><td>2.50</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 2.0</td><td>p</td><td>90</td><td>0</td><td>0.7</td><td>PHILLIPS</td><td>89</td><td>HPW</td></tr></table>

$\tau(n \to e^- \pi^+ \pi^0)$

T37

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;29</td><td>n</td><td>90</td><td>1</td><td>0.78</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></tbody></table>

$\tau(p \to \mu^- \pi^+ \pi^+)$

T38

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;17</td><td>p</td><td>90</td><td>1</td><td>1.72</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 7.8</td><td>p</td><td>90</td><td>0</td><td>0.7</td><td>PHILLIPS</td><td>89</td><td>HPW</td></tr></table>

$\tau(n \to \mu^- \pi^+ \pi^0)$

T39

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;34</td><td>n</td><td>90</td><td>0</td><td>0.78</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></tbody></table>

$\tau(p \to e^- \pi^+ K^+)$

T40

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;75</td><td>p</td><td>90</td><td>81</td><td>127.2</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt;20</td><td>p</td><td>90</td><td>3</td><td>2.50</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></table>

$\tau(p \to \mu^- \pi^+ K^+)$

T41

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;245</td><td>p</td><td>90</td><td>3</td><td>4.0</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 5</td><td>p</td><td>90</td><td>2</td><td>0.78</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></table>

Antilepton + photon(s)

$\tau(p \to e^+ \gamma)$

T42

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;670</td><td>p</td><td>90</td><td>0</td><td>0.1</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr></tbody></table>
# Baryon Particle Listings

p

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt;133</td><td>p</td><td>90</td><td>0</td><td>0.3</td><td>BERGER</td><td>91</td><td>FREJ</td></tr><tr><td>&gt;460</td><td>p</td><td>90</td><td>0</td><td>0.6</td><td>SEIDEL</td><td>88</td><td>IMB</td></tr><tr><td>&gt;360</td><td>p</td><td>90</td><td>0</td><td>0.3</td><td>HAINES</td><td>86</td><td>IMB</td></tr><tr><td>&gt; 87</td><td>p (free)</td><td>90</td><td>0</td><td>0.2</td><td>BLEWITT</td><td>85</td><td>IMB</td></tr><tr><td>&gt;360</td><td>p</td><td>90</td><td>0</td><td>0.2</td><td>BLEWITT</td><td>85</td><td>IMB</td></tr><tr><td>&gt; 0.1</td><td>p</td><td>90</td><td></td><td></td><td>1 GURR</td><td>67</td><td>CNTR</td></tr></table>

¹ We have converted half-life to 90% CL mean life.

$\tau(p \to \mu^+\gamma)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;478</td><td>p</td><td>90</td><td>0</td><td>0.1</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr></tbody></table>

τ43

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt;155</td><td>p</td><td>90</td><td>0</td><td>0.1</td><td>BERGER</td><td>91</td><td>FREJ</td></tr><tr><td>&gt;380</td><td>p</td><td>90</td><td>0</td><td>0.5</td><td>SEIDEL</td><td>88</td><td>IMB</td></tr><tr><td>&gt; 97</td><td>p</td><td>90</td><td>3</td><td>2</td><td>HAINES</td><td>86</td><td>IMB</td></tr><tr><td>&gt; 61</td><td>p (free)</td><td>90</td><td>0</td><td>0.2</td><td>BLEWITT</td><td>85</td><td>IMB</td></tr><tr><td>&gt;280</td><td>p</td><td>90</td><td>0</td><td>0.6</td><td>BLEWITT</td><td>85</td><td>IMB</td></tr><tr><td>&gt; 0.3</td><td>p</td><td>90</td><td></td><td></td><td>1 GURR</td><td>67</td><td>CNTR</td></tr></table>

¹ We have converted half-life to 90% CL mean life.

$\tau(n \to \nu\gamma)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;550</td><td></td><td>90</td><td></td><td></td><td>TAKHISTOV</td><td>15</td><td>SKAM</td></tr></tbody></table>

τ44

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 28</td><td>n</td><td>90</td><td>163</td><td>144.7</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr><tr><td>&gt; 24</td><td>n</td><td>90</td><td>10</td><td>6.86</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr><tr><td>&gt; 9</td><td>n</td><td>90</td><td>73</td><td>60</td><td>HAINES</td><td>86</td><td>IMB</td></tr><tr><td>&gt; 11</td><td>n</td><td>90</td><td>28</td><td>19</td><td>PARK</td><td>85</td><td>IMB</td></tr></table>

$\tau(p \to e^+\gamma\gamma)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;100</td><td>p</td><td>90</td><td>1</td><td>0.8</td><td>BERGER</td><td>91</td><td>FREJ</td></tr></tbody></table>

τ45

$\tau(n \to \nu\gamma\gamma)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;219</td><td>n</td><td>90</td><td>5</td><td>7.5</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr></tbody></table>

τ46

Antilepton + single massless

$\tau(p \to e^+\chi)$

<table><thead><tr><th>VALUE (10<sup>30</sup> years)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;790</td><td>90</td><td>TAKHISTOV</td><td>15</td><td>SKAM</td></tr></tbody></table>

τ47

$\tau(p \to \mu^+\chi)$

<table><thead><tr><th>VALUE (10<sup>30</sup> years)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;410</td><td>90</td><td>TAKHISTOV</td><td>15</td><td>SKAM</td></tr></tbody></table>

τ48

Three (or more) leptons

$\tau(p \to e^+e^+e^−)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;34000</td><td>p</td><td>90</td><td>0</td><td>0.58</td><td>TANAKA</td><td>20</td><td>SKAM</td></tr></tbody></table>

τ49

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 793</td><td>p</td><td>90</td><td>0</td><td>0.5</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr><tr><td>&gt; 147</td><td>p</td><td>90</td><td>0</td><td>0.1</td><td>BERGER</td><td>91</td><td>FREJ</td></tr><tr><td>&gt; 510</td><td>p</td><td>90</td><td>0</td><td>0.3</td><td>HAINES</td><td>86</td><td>IMB</td></tr><tr><td>&gt; 89</td><td>p (free)</td><td>90</td><td>0</td><td>0.5</td><td>BLEWITT</td><td>85</td><td>IMB</td></tr><tr><td>&gt; 510</td><td>p</td><td>90</td><td>0</td><td>0.7</td><td>BLEWITT</td><td>85</td><td>IMB</td></tr></table>

$\tau(p \to e^+\mu^+\mu^−)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;9200</td><td>p</td><td>90</td><td>1</td><td>0.27</td><td>TANAKA</td><td>20</td><td>SKAM</td></tr></tbody></table>

τ50

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 359</td><td>p</td><td>90</td><td>1</td><td>0.9</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr><tr><td>&gt; 81</td><td>p</td><td>90</td><td>0</td><td>0.16</td><td>BERGER</td><td>91</td><td>FREJ</td></tr><tr><td>&gt; 5.0</td><td>p</td><td>90</td><td>0</td><td>0.7</td><td>PHILLIPS</td><td>89</td><td>HPW</td></tr></table>

$\tau(p \to e^+\nu\nu)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;170</td><td>p</td><td>90</td><td>1</td><td>0.27</td><td>1 TAKHISTOV</td><td>14</td><td>SKAM</td></tr></tbody></table>

τ51

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 17</td><td>p</td><td>90</td><td>152</td><td>153.7</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr><tr><td>&gt; 11</td><td>p</td><td>90</td><td>11</td><td>6.08</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></table>

¹ Allowed events at 90% CL are 459.

$\tau(n \to e^+e^−\nu)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;257</td><td>n</td><td>90</td><td>5</td><td>7.5</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr></tbody></table>

τ52

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 74</td><td>n</td><td>90</td><td>0</td><td>&lt; 0.1</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr><tr><td>&gt; 45</td><td>n</td><td>90</td><td>5</td><td>5</td><td>HAINES</td><td>86</td><td>IMB</td></tr><tr><td>&gt; 26</td><td>n</td><td>90</td><td>4</td><td>3</td><td>PARK</td><td>85</td><td>IMB</td></tr></table>

$\tau(n \to \mu^+e^−\nu)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;83</td><td>n</td><td>90</td><td>25</td><td>29.4</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr></tbody></table>

τ53

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt;47</td><td>n</td><td>90</td><td>0</td><td>&lt; 0.1</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></table>

$\tau(n \to \mu^+\mu^−\nu)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;79</td><td>n</td><td>90</td><td>100</td><td>145</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr></tbody></table>

τ54

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt;42</td><td>n</td><td>90</td><td>0</td><td>1.4</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr><tr><td>&gt; 5.1</td><td>n</td><td>90</td><td>0</td><td>0.7</td><td>PHILLIPS</td><td>89</td><td>HPW</td></tr><tr><td>&gt;16</td><td>n</td><td>90</td><td>14</td><td>7</td><td>HAINES</td><td>86</td><td>IMB</td></tr><tr><td>&gt;19</td><td>n</td><td>90</td><td>4</td><td>7</td><td>PARK</td><td>85</td><td>IMB</td></tr></table>

$\tau(p \to \mu^+e^+e^−)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;23000</td><td>p</td><td>90</td><td>0</td><td>0.5</td><td>TANAKA</td><td>20</td><td>SKAM</td></tr></tbody></table>

τ55

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 529</td><td>p</td><td>90</td><td>0</td><td>1.0</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr><tr><td>&gt; 91</td><td>p</td><td>90</td><td>0</td><td>&le; 0.1</td><td>BERGER</td><td>91</td><td>FREJ</td></tr></table>

$\tau(p \to \mu^−e^+e^+)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;19000</td><td>p</td><td>90</td><td>0</td><td>0.5</td><td>TANAKA</td><td>20</td><td>SKAM</td></tr></tbody></table>

τ56

$\tau(p \to \mu^+\mu^+\mu^−)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;10000</td><td>p</td><td>90</td><td>1</td><td>0.4</td><td>TANAKA</td><td>20</td><td>SKAM</td></tr></tbody></table>

τ57

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 675</td><td>p</td><td>90</td><td>0</td><td>0.3</td><td>MCGREW</td><td>99</td><td>IMB3</td></tr><tr><td>&gt; 119</td><td>p</td><td>90</td><td>0</td><td>0.2</td><td>BERGER</td><td>91</td><td>FREJ</td></tr><tr><td>&gt; 10.5</td><td>p</td><td>90</td><td>0</td><td>0.7</td><td>PHILLIPS</td><td>89</td><td>HPW</td></tr><tr><td>&gt; 190</td><td>p</td><td>90</td><td>1</td><td>0.1</td><td>HAINES</td><td>86</td><td>IMB</td></tr><tr><td>&gt; 44</td><td>p (free)</td><td>90</td><td>1</td><td>0.7</td><td>BLEWITT</td><td>85</td><td>IMB</td></tr><tr><td>&gt; 190</td><td>p</td><td>90</td><td>1</td><td>0.9</td><td>BLEWITT</td><td>85</td><td>IMB</td></tr><tr><td>&gt; 2.1</td><td>p</td><td>90</td><td>1</td><td></td><td>1 BATTISTONI</td><td>82</td><td>NUSX</td></tr></table>

¹ We have converted 1 possible event to 90% CL limit.

$\tau(p \to \mu^+\nu\nu)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;220</td><td>p</td><td>90</td><td>0</td><td>7</td><td>11.23</td><td>1 TAKHISTOV</td><td>14</td><td>SKAM</td></tr></tbody></table>

τ58

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 21</td><td>p</td><td>90</td><td>7</td><td>11.23</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></table>

¹ Allowed events at 90% CL are 286.

$\tau(p \to e^−\mu^+\mu^+)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;11000</td><td>p</td><td>90</td><td>1</td><td>0.27</td><td>TANAKA</td><td>20</td><td>SKAM</td></tr></tbody></table>

τ59

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt; 6.0</td><td>p</td><td>90</td><td>0</td><td>0.7</td><td>PHILLIPS</td><td>89</td><td>HPW</td></tr></table>

$\tau(n \to 3\nu)$

See also the “to anything” and “disappearance” limits for bound nucleons in the “p Mean Life” data block just in front of the list of possible p decay modes. Such modes could of course be to three (or five) neutrinos, and the limits are stronger, but we do not repeat them here.

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;0.00049</td><td>n</td><td>90</td><td>2</td><td>2</td><td>1 SUZUKI</td><td>93B</td><td>KAMI</td></tr></tbody></table>

τ60

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&gt;0.0023</td><td>n</td><td>90</td><td></td><td></td><td>2 GLICENSTEIN 97</td><td>91B</td><td>FREJ</td></tr><tr><td>&gt;0.00003</td><td>n</td><td>90</td><td>11</td><td>6.1</td><td>3 BERGER</td><td>91B</td><td>FREJ</td></tr><tr><td>&gt;0.00012</td><td>n</td><td>90</td><td>7</td><td>11.2</td><td>3 BERGER</td><td>91B</td><td>FREJ</td></tr><tr><td>&gt;0.0005</td><td>n</td><td>90</td><td>0</td><td></td><td>LEARNED</td><td>79</td><td>RVUE</td></tr></table>

¹ The SUZUKI 93B limit applies to any of $\nu_e\nu_e\bar{\nu}_e$, $\nu_\mu\nu_\mu\bar{\nu}_\mu$, or $\nu_\tau\nu_\tau\bar{\nu}_\tau$.

² GLICENSTEIN 97 uses Kamioka data and the idea that the disappearance of the neutron's magnetic moment should produce radiation.

³ The first BERGER 91B limit is for $n \to \nu_e\nu_e\bar{\nu}_e$, the second is for $n \to \nu_\mu\nu_\mu\bar{\nu}_\mu$.

$\tau(n \to 5\nu)$

See the note on $\tau(n \to 3\nu)$ on the previous data block.

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;0.0017</td><td>n</td><td>90</td><td></td><td></td><td>1 GLICENSTEIN 97</td><td>91B</td><td>KAMI</td></tr></tbody></table>

τ61

¹ GLICENSTEIN 97 uses Kamioka data and the idea that the disappearance of the neutron's magnetic moment should produce radiation.
Inclusive modes

$\tau(N \to e^+ anything)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;0.6</td><td>p, n</td><td>90</td><td></td><td></td><td>1 LEARNED</td><td>79</td><td>RVUE</td></tr></tbody></table>

$\tau(N \to \mu^+ anything)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;12</td><td>p, n</td><td>90</td><td>2</td><td></td><td>1,2 CHERRY</td><td>81</td><td>HOME</td></tr></tbody></table>

<table><tbody><tr><td>&gt; 1.8</td><td>p, n</td><td>90</td><td>2</td><td>COWSIK</td><td>80</td><td>CNTR</td></tr><tr><td>&gt; 6</td><td>p, n</td><td>90</td><td>2</td><td>LEARNED</td><td>79</td><td>RVUE</td></tr></tbody></table>

$\tau(N \to \nu anything)$

Anything = $\pi, \rho, K$, etc.

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>• • • We do not use the following data for averages, fits, limits, etc.</td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td>&gt;0.0002</td><td>p, n</td><td>90</td><td>0</td><td></td><td>LEARNED</td><td>79</td><td>RVUE</td></tr></tbody></table>

$\tau(N \to e^+ \pi^0 anything)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;0.6</td><td>p, n</td><td>90</td><td>0</td><td></td><td>LEARNED</td><td>79</td><td>RVUE</td></tr></tbody></table>

$\tau(N \to 2 bodies, \nu-free)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>PARTICLE</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>• • • We do not use the following data for averages, fits, limits, etc.</td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td>&gt;1.3</td><td>p, n</td><td>90</td><td>0</td><td></td><td>ALEKSEEV</td><td>81</td><td>BAKS</td></tr></tbody></table>

$\Delta B = 2$ dinucleon modes

$\tau(pp \to \pi^+ \pi^+)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;72.2</td><td>90</td><td>2</td><td>4.45</td><td>GUSTAFSON</td><td>15</td><td>SKAM</td></tr><tr><td>• • • We do not use the following data for averages, fits, limits, etc.</td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td>&gt; 0.7</td><td>90</td><td>4</td><td>2.34</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></tbody></table>

$\tau(pp \to \pi^+ \pi^0)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;170</td><td>90</td><td></td><td></td><td>GUSTAFSON</td><td>15</td><td>SKAM</td></tr><tr><td>• • • We do not use the following data for averages, fits, limits, etc.</td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td>&gt; 2.0</td><td>90</td><td>0</td><td>0.31</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></tbody></table>

$\tau(nn \to \pi^+ \pi^-)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;0.7</td><td>90</td><td>4</td><td>2.18</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></tbody></table>

$\tau(nn \to \pi^0 \pi^0)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;404</td><td>90</td><td></td><td></td><td>GUSTAFSON</td><td>15</td><td>SKAM</td></tr><tr><td>• • • We do not use the following data for averages, fits, limits, etc.</td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td>&gt; 3.4</td><td>90</td><td>0</td><td>0.78</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></tbody></table>

$\tau(pp \to K^+ K^+)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;170</td><td>90</td><td>0</td><td>0.28</td><td>LITOS</td><td>14</td><td>SKAM</td></tr></tbody></table>

$\tau(pp \to e^+ e^+)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;5.8</td><td>90</td><td>0</td><td>&lt;0.1</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></tbody></table>

$\tau(pp \to e^+ \mu^+)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;3.6</td><td>90</td><td>0</td><td>&lt;0.1</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></tbody></table>

$\tau(pp \to \mu^+ \mu^+)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;1.7</td><td>90</td><td>0</td><td>0.62</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></tbody></table>

$\tau(pp \to e^+ \nu)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;260</td><td>90</td><td></td><td></td><td>TAKHISTOV</td><td>15</td><td>SKAM</td></tr><tr><td>• • • We do not use the following data for averages, fits, limits, etc.</td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td>&gt; 2.8</td><td>90</td><td>5</td><td>9.67</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></tbody></table>

$\tau(p n \to \mu^+ \nu)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;200</td><td>90</td><td></td><td></td><td>TAKHISTOV</td><td>15</td><td>SKAM</td></tr><tr><td>• • • We do not use the following data for averages, fits, limits, etc.</td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td>&gt; 1.6</td><td>90</td><td>4</td><td>4.37</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td>τ per iron nucleus</td></tr></tbody></table>

$\tau(p n \to \tau^+ \nu_\tau)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;29</td><td>90</td><td></td><td></td><td>TAKHISTOV</td><td>15</td><td>SKAM</td></tr><tr><td>• • • We do not use the following data for averages, fits, limits, etc.</td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td>&gt; 1</td><td>90</td><td>1</td><td>4</td><td>BRYMAN</td><td>14</td><td>CHER</td></tr></tbody></table>

$\tau(n n \to invisible)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;1.4</td><td>90</td><td></td><td></td><td>1 ARAKI</td><td>06</td><td>KLND n n → invisible</td></tr><tr><td>• • • We do not use the following data for averages, fits, limits, etc.</td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td>&gt;0.015</td><td>90</td><td>2,3</td><td>ALLEGA</td><td>22</td><td>SNO+ n n → invisible</td></tr><tr><td>&gt;0.13</td><td>90</td><td>2</td><td>ANDERSON</td><td>19A</td><td>SNO+ n n → invisible</td></tr><tr><td>&gt;0.00042</td><td>90</td><td>4</td><td>TRETYAK</td><td>04</td><td>CNTR n n → invisible</td></tr><tr><td>&gt;0.00049</td><td>90</td><td>5</td><td>BACK</td><td>03</td><td>BORX n n → invisible</td></tr><tr><td>&gt;0.00012</td><td>90</td><td>6</td><td>BERNABEI</td><td>00B</td><td>DAMA n n → invisible</td></tr></tbody></table>

$\tau(n n \to \nu_e \bar{\nu}_e)$

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&gt;0.000012</td><td>90</td><td>5</td><td>9.7</td><td>BERGER</td><td>91B</td><td>FREJ</td></tr></tbody></table>

$\tau(n n \to \nu_\mu \bar{\nu}_\mu)$

See the proceeding data block. "Invisible modes" would include any multi-neutrino mode.

<table><thead><tr><th>LIMIT<br>(10<sup>30</sup> years)</th><th>CL%</th><th>EVTS</th><th>BKGD EST</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead></table>

> 1.4 (CL=90%) OUR LIMIT

<table><thead><tr><th>• • • We do not use the following data for averages, fits, limits, etc.</th><th></th><th></th><th></th><th></th><th></th><th></th></tr><tr><th>&gt;0.000006</th><th>90</th><th>4</th><th>4.4</th><th>BERGER</th><th>91B</th><th>FREJ</th><th>τ per iron nucleus</th></tr></thead></table>

$\tau(p n \to invisible)$

This violates charge conservation as well as baryon number conservation.

<table><thead><tr><th>VALUE (10<sup>30</sup> years)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;0.06</td><td>90</td><td>1,2</td><td>ALLEGA</td><td>22</td><td>SNO+</td></tr></tbody></table>

<table><tbody><tr><td>&gt;0.026</td><td>90</td><td>1</td><td>ANDERSON</td><td>19A</td><td>SNO+</td></tr><tr><td>&gt;0.00021</td><td>90</td><td>3</td><td>TRETYAK</td><td>04</td><td>CNTR</td></tr></tbody></table>

$\tau(p p \to invisible)$

This violates charge conservation as well as baryon number conservation.

<table><thead><tr><th>VALUE (10<sup>30</sup> years)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th></tr></thead><tbody><tr><td>&gt;0.11</td><td>90</td><td>1</td><td>ALLEGA</td><td>22</td><td>SNO+</td></tr></tbody></table>

<table><tbody><tr><td>&gt;0.047</td><td>90</td><td>1</td><td>ANDERSON</td><td>19A</td><td>SNO+</td></tr><tr><td>&gt;0.00005</td><td>90</td><td>2</td><td>BACK</td><td>03</td><td>BORX</td></tr><tr><td>&gt;0.0000055</td><td>90</td><td>3</td><td>BERNABEI</td><td>00B</td><td>DAMA</td></tr></tbody></table>

<footnote n="1">¹The electron may be primary or secondary.</footnote>

<footnote>• • • We do not use the following data for averages, fits, limits, etc. • • •</footnote>

<footnote n="1">¹We have converted 2 possible events to 90% CL limit.</footnote>

<footnote n="2">²The muon may be primary or secondary.</footnote>

<footnote n="1">¹BRYMAN 14 uses a MCGREW 99 limit on the $p \to e^+ \nu \nu$ lifetime to extract this value.</footnote>

<footnote n="1">¹ARAKI 06 looks for signs of de-excitation of the residual nucleus after disappearance of two neutrons from the s shell of $^{12}$C.</footnote>

<footnote n="2">²ALLEGA 22 and ANDERSON 19A look for $\gamma$ rays from the de-excitation of a residual $^{14}$O* following the disappearance of $n n$ in $^{16}$O.</footnote>

<footnote n="3">³ALLEGA 22 replaces the previous SNO+ value of ANDERSON 19A.</footnote>

<footnote n="4">⁴TRETYAK 04 uses data from an old Homestake-mine radiochemical experiment on limits for invisible decays of $^{39}$K to $^{37}$Ar.</footnote>

<footnote n="5">⁵BACK 03 looks for decays of unstable nuclides left after $N N$ decays of parent $^{12}$C, $^{13}$C, $^{16}$O nuclei. These are "invisible channel" limits.</footnote>

<footnote n="6">⁶BERNABEI 00b looks for the decay of a $^{127}$Xe nucleus following the disappearance of an $n n$ pair in the otherwise-stable $^{129}$Xe nucleus. The limit here applies as well to $n n \to \nu_\mu \bar{\nu}_\mu$, $n n \to \nu_\tau \bar{\nu}_\tau$, or any "disappearance" mode.</footnote>

<footnote>• • • We do not use the following data for averages, fits, limits, etc. • • •</footnote>

<footnote n="1">¹ALLEGA 22 and ANDERSON 19A look for $\gamma$ rays from the de-excitation of a residual $^{14}$N* following the disappearance of $p n$ in $^{16}$O.</footnote>

<footnote n="2">²ALLEGA 22 replaces the previous SNO+ value of ANDERSON 19A.</footnote>

<footnote n="3">³TRETYAK 04 uses data from an old Homestake-mine radiochemical experiment on limits for invisible decays of $^{39}$K to $^{37}$Ar.</footnote>

<footnote>• • • We do not use the following data for averages, fits, limits, etc. • • •</footnote>

<footnote n="1">¹ALLEGA 22 look for $\gamma$ rays from the de-excitation of a residual $^{14}$C* following the disappearance of $p p$ in $^{16}$O. Supersedes ANDERSON 19A result.</footnote>

<footnote n="2">²BACK 03 looks for decays of unstable nuclides left after $N N$ decays of parent $^{12}$C, $^{13}$C, $^{16}$O nuclei. These are "invisible channel" limits.</footnote>

<footnote n="3">³BERNABEI 00b looks for the decay of a $^{127}$Xe nucleus following the disappearance of a $p p$ pair in the otherwise-stable $^{129}$Xe nucleus.</footnote>
$$ \Delta B = 1 $$

## $\bar{p}$ PARTIAL MEAN LIVES

The "partial mean life" limits tabulated here are the limits on $\tau/B_j$, where $\tau$ is the total mean life for the antiproton and $B_j$ is the branching fraction for the mode in question.

$$ \tau(\bar{p} \to e^{-} \gamma) \qquad \begin{array}{c} \text{VALUE (years)} \\ > 7 \times 10^5 \end{array} \qquad \begin{array}{c} \text{CL\%} \\ 90 \end{array} \qquad \begin{array}{c} \text{DOCUMENT ID} \\ \text{GEER} \end{array} \qquad \begin{array}{c} \text{TEC} \\ \text{00} \end{array} \qquad \begin{array}{c} \text{COMMENT} \\ \text{APEX 8.9 GeV/c $\bar{p}$ beam} \end{array} \qquad \text{T83} $$

• • • We do not use the following data for averages, fits, limits, etc. • • •

>1848 95 GEER 94 CALO 8.9 GeV/c $\bar{p}$ beam

$$ \tau(\bar{p} \to \mu^{-} \gamma) \qquad \begin{array}{c} \text{VALUE (years)} \\ > 5 \times 10^4 \end{array} \qquad \begin{array}{c} \text{CL\%} \\ 90 \end{array} \qquad \begin{array}{c} \text{DOCUMENT ID} \\ \text{GEER} \end{array} \qquad \begin{array}{c} \text{TEC} \\ \text{00} \end{array} \qquad \begin{array}{c} \text{COMMENT} \\ \text{APEX 8.9 GeV/c $\bar{p}$ beam} \end{array} \qquad \text{T84} $$

• • • We do not use the following data for averages, fits, limits, etc. • • •

>5.0 × 10⁴ 90 HU 98B APEX 8.9 GeV/c $\bar{p}$ beam

$$ \tau(\bar{p} \to e^{-} \pi^0) \qquad \begin{array}{c} \text{VALUE (years)} \\ > 4 \times 10^5 \end{array} \qquad \begin{array}{c} \text{CL\%} \\ 90 \end{array} \qquad \begin{array}{c} \text{DOCUMENT ID} \\ \text{GEER} \end{array} \qquad \begin{array}{c} \text{TEC} \\ \text{00} \end{array} \qquad \begin{array}{c} \text{COMMENT} \\ \text{APEX 8.9 GeV/c $\bar{p}$ beam} \end{array} \qquad \text{T85} $$

• • • We do not use the following data for averages, fits, limits, etc. • • •

>554 95 GEER 94 CALO 8.9 GeV/c $\bar{p}$ beam

$$ \tau(\bar{p} \to \mu^{-} \pi^0) \qquad \begin{array}{c} \text{VALUE (years)} \\ > 5 \times 10^4 \end{array} \qquad \begin{array}{c} \text{CL\%} \\ 90 \end{array} \qquad \begin{array}{c} \text{DOCUMENT ID} \\ \text{GEER} \end{array} \qquad \begin{array}{c} \text{TEC} \\ \text{00} \end{array} \qquad \begin{array}{c} \text{COMMENT} \\ \text{APEX 8.9 GeV/c $\bar{p}$ beam} \end{array} \qquad \text{T86} $$

• • • We do not use the following data for averages, fits, limits, etc. • • •

>4.8 × 10⁴ 90 HU 98B APEX 8.9 GeV/c $\bar{p}$ beam

$$ \tau(\bar{p} \to e^{-} \eta) \qquad \begin{array}{c} \text{VALUE (years)} \\ > 2 \times 10^4 \end{array} \qquad \begin{array}{c} \text{CL\%} \\ 90 \end{array} \qquad \begin{array}{c} \text{DOCUMENT ID} \\ \text{GEER} \end{array} \qquad \begin{array}{c} \text{TEC} \\ \text{00} \end{array} \qquad \begin{array}{c} \text{COMMENT} \\ \text{APEX 8.9 GeV/c $\bar{p}$ beam} \end{array} \qquad \text{T87} $$

• • • We do not use the following data for averages, fits, limits, etc. • • •

>171 95 GEER 94 CALO 8.9 GeV/c $\bar{p}$ beam

$$ \tau(\bar{p} \to \mu^{-} \eta) \qquad \begin{array}{c} \text{VALUE (years)} \\ > 8 \times 10^3 \end{array} \qquad \begin{array}{c} \text{CL\%} \\ 90 \end{array} \qquad \begin{array}{c} \text{DOCUMENT ID} \\ \text{GEER} \end{array} \qquad \begin{array}{c} \text{TEC} \\ \text{00} \end{array} \qquad \begin{array}{c} \text{COMMENT} \\ \text{APEX 8.9 GeV/c $\bar{p}$ beam} \end{array} \qquad \text{T88} $$

• • • We do not use the following data for averages, fits, limits, etc. • • •

>7.9 × 10³ 90 HU 98B APEX 8.9 GeV/c $\bar{p}$ beam

$$ \tau(\bar{p} \to e^{-} K_0^S) \qquad \begin{array}{c} \text{VALUE (years)} \\ > 900 \end{array} \qquad \begin{array}{c} \text{CL\%} \\ 90 \end{array} \qquad \begin{array}{c} \text{DOCUMENT ID} \\ \text{GEER} \end{array} \qquad \begin{array}{c} \text{TEC} \\ \text{00} \end{array} \qquad \begin{array}{c} \text{COMMENT} \\ \text{APEX 8.9 GeV/c $\bar{p}$ beam} \end{array} \qquad \text{T89} $$

• • • We do not use the following data for averages, fits, limits, etc. • • •

> 29 95 GEER 94 CALO 8.9 GeV/c $\bar{p}$ beam

$$ \tau(\bar{p} \to \mu^{-} K_0^S) \qquad \begin{array}{c} \text{VALUE (years)} \\ > 4 \times 10^3 \end{array} \qquad \begin{array}{c} \text{CL\%} \\ 90 \end{array} \qquad \begin{array}{c} \text{DOCUMENT ID} \\ \text{GEER} \end{array} \qquad \begin{array}{c} \text{TEC} \\ \text{00} \end{array} \qquad \begin{array}{c} \text{COMMENT} \\ \text{APEX 8.9 GeV/c $\bar{p}$ beam} \end{array} \qquad \text{T90} $$

• • • We do not use the following data for averages, fits, limits, etc. • • •

>4.3 × 10³ 90 HU 98B APEX 8.9 GeV/c $\bar{p}$ beam

$$ \tau(\bar{p} \to K_0^S) \qquad \begin{array}{c} \text{VALUE (years)} \\ > 9 \times 10^3 \end{array} \qquad \begin{array}{c} \text{CL\%} \\ 90 \end{array} \qquad \begin{array}{c} \text{DOCUMENT ID} \\ \text{GEER} \end{array} \qquad \begin{array}{c} \text{TEC} \\ \text{00} \end{array} \qquad \begin{array}{c} \text{COMMENT} \\ \text{APEX 8.9 GeV/c $\bar{p}$ beam} \end{array} \qquad \text{T91} $$

• • • We do not use the following data for averages, fits, limits, etc. • • •

>9 95 GEER 94 CALO 8.9 GeV/c $\bar{p}$ beam

$$ \tau(\bar{p} \to \mu^{-} K_0^L) \qquad \begin{array}{c} \text{VALUE (years)} \\ > 7 \times 10^3 \end{array} \qquad \begin{array}{c} \text{CL\%} \\ 90 \end{array} \qquad \begin{array}{c} \text{DOCUMENT ID} \\ \text{GEER} \end{array} \qquad \begin{array}{c} \text{TEC} \\ \text{00} \end{array} \qquad \begin{array}{c} \text{COMMENT} \\ \text{APEX 8.9 GeV/c $\bar{p}$ beam} \end{array} \qquad \text{T92} $$

• • • We do not use the following data for averages, fits, limits, etc. • • •

>6.5 × 10³ 90 HU 98B APEX 8.9 GeV/c $\bar{p}$ beam

$$ \tau(\bar{p} \to e^{-} \gamma\gamma) \qquad \begin{array}{c} \text{VALUE (years)} \\ > 2 \times 10^4 \end{array} \qquad \begin{array}{c} \text{CL\%} \\ 90 \end{array} \qquad \begin{array}{c} \text{DOCUMENT ID} \\ \text{GEER} \end{array} \qquad \begin{array}{c} \text{TEC} \\ \text{00} \end{array} \qquad \begin{array}{c} \text{COMMENT} \\ \text{APEX 8.9 GeV/c $\bar{p}$ beam} \end{array} \qquad \text{T93} $$

• • • We do not use the following data for averages, fits, limits, etc. • • •

$$ \tau(\bar{p} \to \mu^{-} \gamma\gamma) \qquad \begin{array}{c} \text{VALUE (years)} \\ > 2 \times 10^4 \end{array} \qquad \begin{array}{c} \text{CL\%} \\ 90 \end{array} \qquad \begin{array}{c} \text{DOCUMENT ID} \\ \text{GEER} \end{array} \qquad \begin{array}{c} \text{TEC} \\ \text{00} \end{array} \qquad \begin{array}{c} \text{COMMENT} \\ \text{APEX 8.9 GeV/c $\bar{p}$ beam} \end{array} \qquad \text{T94} $$

• • • We do not use the following data for averages, fits, limits, etc. • • •

>2.3 × 10⁴ 90 HU 98B APEX 8.9 GeV/c $\bar{p}$ beam

$$ \tau(\bar{p} \to e^{-} \omega) \qquad \begin{array}{c} \text{VALUE (years)} \\ > 200 \end{array} \qquad \begin{array}{c} \text{CL\%} \\ 90 \end{array} \qquad \begin{array}{c} \text{DOCUMENT ID} \\ \text{GEER} \end{array} \qquad \begin{array}{c} \text{TEC} \\ \text{00} \end{array} \qquad \begin{array}{c} \text{COMMENT} \\ \text{APEX 8.9 GeV/c $\bar{p}$ beam} \end{array} \qquad \text{T95} $$

• • • We do not use the following data for averages, fits, limits, etc. • • •

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BLANPIED 01 PR C64 025203

HORI 01 PR 87 093401

OLMOSDELL 01 PR EJ A10 207

TRETYAK 01 PR 85 0590

BERNABEI 00B PR 84 590

GEER 00B PR D82 052004

Also 00B PR 85 3546 (errat.)

GEER 00D S.H. Geer, D.C. Kennedy

SENGUPTA 00 PR B484 275

WALL 00 PR D61 072004

WALL 00B PR D62 092003

GABRIELSE 99 PR B2 3198

HAYATO 99 PR B3 1529

MCGREW 99 PR D59 052004

MOHR 99 PR JPCRD 28 1713

Also 01 PR 72 351

TORII 99 PR B427 217

ALLISON 98 PR D58 111101

HU 98B PR D58 111101

SHIOZAWA 98 PR B1 3319

GLICENSTEIN 97 PR B411 326

GABRIELSE 97 PR C52 5544

MCGIBBON 95 PR C52 2097

GEER 94 PR 72 1596

HALLIN 93 PR C48 1497

SUZUKI 93B PR B311 357

HUGHES 92 PR B69 578

ZIEGER 92 PR B278 34

Also 92 PR B281 417 (errat.)

BERGER 91 SPHY C50 385

BERGER 91B PR B269 227

FEDERSPIEL 91 PR 67 1511

BECKER-SZ. 90 PR C224 2974

ERICSON 90 EPL 11 295

GABRIELSE 90 PR 65 1317

BERGER 89 NP B313 509

CHO 89 PR 63 2559

HIRATA 89C PR B220 308

PHILLIPS 89 PR B224 348

KREISSL 88 ZPHY C37 557

SEIDEL 88 PR 61 2522

Also 88 S. Seugupta (Soudan-2 Collab.)
²ARZUMANOV 15 is a reanalysis of their 2008–2010 dataset, with improved systematic corrections of ARZUMANOV 00 and ARZUMANOV 12.

³STEYERL 12 is a detailed reanalysis of neutron storage loss corrections to the raw data of MAMPE 89, and it replaces that value.

⁴WILSON 21 extract the value from the flux of n escaping the moon using data from the Lunar Prospector Neutron Spectrometer.

⁵YUE 13 differs from NICO 05 in that a different and better method was used to measure the neutron density in the fiducial volume. This shifted the lifetime by +1.4 seconds and reduced the previously largest source of systematic uncertainty by a factor of five.

⁶ARZUMANOV 12 reanalyzes its systematic corrections in ARZUMANOV 00 and obtains this corrected value.

⁷IGNATOVICH 95 calls into question some of the corrections and averaging procedures used by MAMPE 93. The response, BONDARENKO 96, denies the validity of the criticisms.

⁸The NESVIZHEVSKII 92 measurement has been withdrawn by A. Serebrov.

⁹The BYRNE 80 measurement has been withdrawn (J. Byrne, private communication, 1990).

WEIGHTED AVERAGE
878.4±0.5 (Error scaled by 1.8)

<figure><img src="image_712.png" /></figure>

neutron mean life (s)

## n MAGNETIC MOMENT

See the “Quark Model” review.

<table><thead><tr><th>VALUE (μ<sub>N</sub>)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><b>-1.91304273±0.00000045</b></td><td>TIESINGA</td><td>21</td><td>RVUE 2018 CODATA value</td></tr><tr><td>• • • We do not use the following data for averages, fits, limits, etc. • • •</td><td></td><td></td><td></td></tr><tr><td>-1.91304273±0.00000045</td><td>MOHR</td><td>16</td><td>RVUE 2014 CODATA value</td></tr><tr><td>-1.91304272±0.00000045</td><td>MOHR</td><td>12</td><td>RVUE 2010 CODATA value</td></tr><tr><td>-1.91304273±0.00000045</td><td>MOHR</td><td>08</td><td>RVUE 2006 CODATA value</td></tr><tr><td>-1.91304273±0.00000045</td><td>MOHR</td><td>05</td><td>RVUE 2002 CODATA value</td></tr><tr><td>-1.91304272±0.00000045</td><td>MOHR</td><td>99</td><td>RVUE 1998 CODATA value</td></tr><tr><td>-1.91304275±0.00000045</td><td>COHEN</td><td>87</td><td>RVUE 1986 CODATA value</td></tr><tr><td>-1.91304277±0.00000048</td><td><sup>1</sup>GREENE</td><td>82</td><td>MRS</td></tr></tbody></table>

¹GREENE 82 measures the moment to be (1.04187564 ± 0.00000026) × 10⁻³ Bohr magnetons. The value above is obtained by multiplying this by $m_p/m_e = 1836.152701 ± 0.000037$ (the 1986 CODATA value from COHEN 87).

## n ELECTRIC DIPOLE MOMENT

A nonzero value is forbidden by both *T* invariance and *P* invariance. A number of early results have been omitted. See RAMSEY 90, GOLUB 94, and LAMOREAUX 09 for reviews.

The results are upper limits on $|d_n|$.

<table><thead><tr><th>VALUE (10<sup>-25</sup> e cm)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><b>&lt; 0.18</b></td><td>90</td><td><sup>1</sup>ABEL</td><td>20</td><td>MRS UCN</td></tr><tr><td>• • • We do not use the following data for averages, fits, limits, etc. • • •</td><td></td><td></td><td></td><td></td></tr><tr><td>&lt; 0.22</td><td>95</td><td><sup>2</sup>SAHOO</td><td>17</td><td><sup>199</sup>Hg atom EDM + theory</td></tr><tr><td>&lt; 0.16</td><td>95</td><td>GRANER</td><td>16</td><td>MRS <sup>199</sup>Hg atom EDM + theory</td></tr><tr><td>&lt; 0.30</td><td>90</td><td><sup>3</sup>PENDLEBURY</td><td>15</td><td>MRS Supersedes BAKER 06</td></tr><tr><td>&lt; 0.55</td><td>90</td><td>SEREBROV</td><td>15</td><td>MRS UCN's, hν = 2μ<sub>n</sub>B ± 2d<sub>n</sub>E</td></tr><tr><td>&lt; 0.55</td><td>90</td><td><sup>4</sup>SEREBROV</td><td>14</td><td>MRS See SEREBROV 15</td></tr><tr><td>&lt; 0.29</td><td>90</td><td><sup>5</sup>BAKER</td><td>06</td><td>MRS See PENDLEBURY 15</td></tr><tr><td>&lt; 0.63</td><td>90</td><td><sup>6</sup>HARRIS</td><td>99</td><td>MRS d = (-0.1 ± 0.36) × 10<sup>-25</sup></td></tr><tr><td>&lt; 0.97</td><td>90</td><td>ALTAREV</td><td>96</td><td>MRS See SEREBROV 14</td></tr><tr><td>&lt; 1.1</td><td>95</td><td>ALTAREV</td><td>92</td><td>MRS See ALTAREV 96</td></tr><tr><td>&lt; 1.2</td><td>95</td><td>SMITH</td><td>90</td><td>MRS See HARRIS 99</td></tr><tr><td>&lt; 2.6</td><td>95</td><td>ALTAREV</td><td>86</td><td>MRS d = (-1.4 ± 0.6) × 10<sup>-25</sup></td></tr><tr><td>0.3 ± 4.8</td><td></td><td>PENDLEBURY</td><td>84</td><td>MRS Ultracold neutrons</td></tr><tr><td>&lt; 6</td><td>90</td><td>ALTAREV</td><td>81</td><td>MRS d = (2.1 ± 2.4) × 10<sup>-25</sup></td></tr><tr><td>&lt;16</td><td>90</td><td>ALTAREV</td><td>79</td><td>MRS d = (4.0 ± 7.5) × 10<sup>-25</sup></td></tr></tbody></table>

¹ABEL 20 reports $d = (0.0 ± 1.1 ± 0.2) × 10^{-26}$ e cm value corresponding to the listed limit.

²SAHOO 17 develops theory to calculate this limit from the measured limit by GRANER 16 of the <sup>199</sup>Hg atom EDM.

³PENDLEBURY 15 reports $d = (-0.21 ± 1.82) × 10^{-26}$ e cm value corresponding to the listed limit.

⁴SEREBROV 14 includes the data of ALTAREV 96.

⁵LAMOREAUX 07 faults BAKER 06 for not including in the estimate of systematic error an effect due to the Earth's rotation. BAKER 07 replies (1) that the effect was included implicitly in the analysis and (2) that further analysis confirms that the BAKER 06 limit is correct as is. See also SILENKO 07.

⁶This HARRIS 99 result includes the result of SMITH 90. However, the averaging of the results of these two experiments has been criticized by LAMOREAUX 00.

## n MEAN-SQUARE CHARGE RADIUS

The mean-square charge radius of the neutron, $\langle r_n^2 \rangle$, is related to the neutron-electron scattering length $b_n e$ by $\langle r_n^2 \rangle = 3(m_e a_0 / m_n) b_n e$, where $m_e$ and $m_n$ are the masses of the electron and neutron, and $a_0$ is the Bohr radius. Numerically, $\langle r_n^2 \rangle = 86.34 b_n e$, if we use $a_0$ for a nucleus with infinite mass.

<table><thead><tr><th>VALUE (fm<sup>2</sup>)</th><th>DOCUMENT ID</th><th>COMMENT</th></tr></thead><tbody><tr><td><b>-0.1155 ± 0.0017</b> OUR AVERAGE</td><td></td><td></td></tr><tr><td>-0.115 ± 0.002 ± 0.003</td><td>KOPECKY</td><td>ne scattering (Pb)</td></tr><tr><td>-0.124 ± 0.003 ± 0.005</td><td>KOPECKY</td><td>ne scattering (Bi)</td></tr><tr><td>-0.114 ± 0.003</td><td>KOESTER</td><td>ne scattering (Pb, Bi)</td></tr><tr><td>-0.115 ± 0.003</td><td><sup>1</sup>KROHN</td><td>ne scattering (Ne, Ar, Kr, Xe)</td></tr><tr><td>• • • We do not use the following data for averages, fits, limits, etc. • • •</td><td></td><td></td></tr><tr><td>-0.1101 ± 0.0089</td><td><sup>2</sup>HEACOCK</td><td>n interferometry</td></tr><tr><td>-0.106 <sup>+0.007</sup><sub>-0.005</sub></td><td><sup>3</sup>FILIN</td><td>chiral EFT analysis</td></tr><tr><td>-0.117 <sup>+0.007</sup><sub>-0.011</sub></td><td>BELUSHKIN</td><td>Dispersion analysis</td></tr><tr><td>-0.113 ± 0.003 ± 0.004</td><td>KOPECKY</td><td>ne scattering (Pb)</td></tr><tr><td>-0.134 ± 0.009</td><td>ALEKSANDR...</td><td>ne scattering (Bi)</td></tr><tr><td>-0.114 ± 0.003</td><td>KOESTER</td><td>ne scattering (Pb, Bi)</td></tr><tr><td>-0.118 ± 0.002</td><td>KOESTER</td><td>ne scattering (Pb)</td></tr><tr><td>-0.120 ± 0.002</td><td>KOESTER</td><td>ne scattering (Bi)</td></tr><tr><td>-0.116 ± 0.003</td><td>KROHN</td><td>ne scattering (Ne, Ar, Kr, Xe)</td></tr></tbody></table>

¹KROHN 73 measured -0.112 ± 0.003 fm². This value is as corrected by KOESTER 76.

²HEACOCK 21 extract the value from Pendeliosung interferometry to measure the neutron structure factors of silicon. This value is strongly anti-correlated with the mean-square thermal atomic displacement.

³FILIN 20 extract the value based on their chiral-EFT calculation of the deuteron structure radius and use as input the atomic data for the difference of the deuteron and proton charge radii.

## n MAGNETIC RADIUS

This is the rms magnetic radius, $\sqrt{\langle r_M^2 \rangle}$.

<table><thead><tr><th>VALUE/E (fm)</th><th>DOCUMENT ID</th><th>COMMENT</th></tr></thead><tbody><tr><td><b>0.864 <sup>+0.009</sup><sub>-0.008</sub></b> OUR AVERAGE</td><td></td><td></td></tr><tr><td>0.89 ± 0.03</td><td>EPSTEIN</td><td>14 Using e<sub>p</sub>, e<sub>n</sub>, ππ data</td></tr><tr><td>0.862 <sup>+0.009</sup><sub>-0.008</sub></td><td>BELUSHKIN</td><td>07 Dispersion analysis</td></tr></tbody></table>

## n ELECTRIC POLARIZABILITY $\alpha_n$

Following is the electric polarizability $\alpha_n$ defined in terms of the induced electric dipole moment by $D = 4\pi\epsilon_0\alpha_n E$. For a review, see SCHMIED-MAYER 89.

For a very complete reviews of the polarizability of the nucleon and Compton scattering, see SCHUMACHER 05, updated in SCHUMACHER 19, and GRIESSHAMMER 12.

<table><thead><tr><th>VALUE (10<sup>-4</sup> fm<sup>3</sup>)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><b>11.8 ± 1.1</b> OUR AVERAGE</td><td></td><td></td><td></td></tr><tr><td>11.55 ± 1.25 ± 0.8</td><td>MYERS</td><td>14 CNTR γd → γd</td><td></td></tr><tr><td>12.5 ± 1.8 <sup>+1.6</sup><sub>-1.3</sub></td><td><sup>1</sup>KOSSERT</td><td>03 CNTR γd → γp n</td><td></td></tr><tr><td>12.0 ± 1.5 ± 2.0</td><td>SCHMIEDM...</td><td>91 CNTR n Pb transmission</td><td></td></tr><tr><td>10.7 <sup>+3.3</sup><sub>-10.7</sub></td><td>ROSE</td><td>90B CNTR γd → γnp</td><td></td></tr><tr><td>• • • We do not use the following data for averages, fits, limits, etc. • • •</td><td></td><td></td><td></td></tr><tr><td>8.8 ± 2.4 ± 3.0</td><td><sup>2</sup>LUNDIN</td><td>03 CNTR γd → γd</td><td></td></tr><tr><td>13.6</td><td><sup>3</sup>KOLB</td><td>00 CNTR γd → γnp</td><td></td></tr><tr><td>0.0 ± 5.0</td><td><sup>4</sup>KOESTER</td><td>95 CNTR n Pb, n Bi transmission</td><td></td></tr><tr><td>11.7 <sup>+4.3</sup><sub>-11.7</sub></td><td>ROSE</td><td>90 CNTR See ROSE 90B</td><td></td></tr><tr><td>8 ± 10</td><td>KOESTER</td><td>88 CNTR n Pb, n Bi transmission</td><td></td></tr><tr><td>12 ± 10</td><td>SCHMIEDM...</td><td>88 CNTR n Pb, n C transmission</td><td></td></tr></tbody></table>

¹KOSSERT 03 gets $\alpha_n - \beta_n = (9.8 ± 3.6^{+2.1}_{-1.1} ± 2.2) × 10^{-4}$ fm³, and uses $\alpha_n + \beta_n = (15.2 ± 0.5) × 10^{-4}$ fm³ from LEVCHUK 00. Thus the errors on $\alpha_n$ and $\beta_n$ are anti-correlated.

²LUNDIN 03 measures $\alpha_N - \beta_N = (6.4 ± 2.4) × 10^{-4}$ fm³ and uses accurate values for $\alpha_p$ and $\alpha_n$ and a precise sum-rule result for $\alpha_n + \beta_n$. The second error is a model
uncertainty, and errors on $\alpha_n$ and $\beta_n$ are anticorrelated. The data from this paper are included in the analysis of MYERS 14.

³KOLB 00 obtains this value with a lower limit of $7.6 \times 10^{-4} \text{ fm}^3$ but no upper limit from this experiment alone. Combined with results of ROSE 90, the 1-$\sigma$ range is $(7.6-14.0) \times 10^{-4} \text{ fm}^3$.

⁴ KOESTER 95 uses natural Pb and the isotopes 208, 207, and 206. See this paper for a discussion of methods used by various groups to extract $\alpha_n$ from data.

## n MAGNETIC POLARIZABILITY $\beta_n$

<table><thead><tr><th>VALUE (10<sup>-4</sup> fm<sup>3</sup>)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>3.7 ±1.2</strong> OUR AVERAGE</td><td></td><td></td><td></td></tr><tr><td>3.65 ±1.25 ±0.8</td><td>MYERS</td><td>14</td><td>CNTR γd → γd</td></tr><tr><td>2.7 ±1.8 <sup>+1.3</sup><sub>-1.6</sub></td><td><sup>1</sup> KOSSERT</td><td>03</td><td>CNTR γd → γpn</td></tr><tr><td>6.5 ±2.4 ±3.0</td><td><sup>2</sup> LUNDIN</td><td>03</td><td>CNTR γd → γd</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>1.6</td><td><sup>3</sup> KOLB</td><td>00</td><td>CNTR γd → γnp</td></tr></table>

¹ KOSSERT 03 gets $\alpha_n - \beta_n = (9.8 \pm 3.6^{+2.1}_{-1.1} \pm 2.2) \times 10^{-4} \text{ fm}^3$, and uses $\alpha_n + \beta_n = (15.2 \pm 0.5) \times 10^{-4} \text{ fm}^3$ from LEVCHUK 00. Thus the errors on $\alpha_n$ and $\beta_n$ are anti-correlated.

² LUNDIN 03 measures $\alpha_N - \beta_N = (6.4 \pm 2.4) \times 10^{-4} \text{ fm}^3$ and uses accurate values for $\alpha_p$ and $\alpha_p$ and a precise sum-rule result for $\alpha_n + \beta_n$. The second error is a model uncertainty, and errors on $\alpha_n$ and $\beta_n$ are anticorrelated.

³ KOLB 00 obtains this value with an upper limit of $7.6 \times 10^{-4} \text{ fm}^3$ but no lower limit from this experiment alone. Combined with results of ROSE 90, the 1-$\sigma$ range is $(1.2-7.6) \times 10^{-4} \text{ fm}^3$.

## n CHARGE

See also "$|q_p + q_e|/e$" in the proton Listings.

<table><thead><tr><th>VALUE (10<sup>-21</sup> e)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>- 0.2± 0.8</strong> OUR AVERAGE</td><td></td><td></td><td></td></tr><tr><td>- 0.1± 1.1</td><td><sup>1</sup> BRESSI</td><td>11</td><td>Neutrality of SF<sub>6</sub></td></tr><tr><td>- 0.4± 1.1</td><td><sup>2</sup> BAUMANN</td><td>88</td><td>Cold n deflection</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>-15 ±22</td><td><sup>3</sup> GAEHLER</td><td>82</td><td>CNTR Cold n deflection</td></tr></table>

¹ As a limit, this BRESSI 11 value is $< 1 \times 10^{-21} e$.

² The BAUMANN 88 error $\pm 1.1$ gives the 68% CL limits about the value $-0.4$.

³ The GAEHLER 82 error $\pm 22$ gives the 90% CL limits about the value $-15$.

## LIMIT ON $n\bar{n}$ OSCILLATIONS

### Mean Time for $n\bar{n}$ Transition

A test of $\Delta B=2$ baryon number nonconservation. MOHAPATRA 80 and MOHAPATRA 89 discuss the theoretical motivations for looking for $n\bar{n}$ oscillations. DOVER 83 and DOVER 85 give phenomenological analyses. The best limits come from looking for the decay of neutrons bound in nuclei. However, these analyses require model-dependent corrections for nuclear effects. See KABIR 83, DOVER 89, ALBERICO 91, and GAL 00 for discussions. Direct searches for $n \to \pi\bar{n}$ transitions using reactor neutrons are cleaner but give somewhat poorer limits. We include limits for both free and bound neutrons in the Summary Table. See MOHAPATRA 09 and PHILLIPS 16 for recent reviews.

<table><thead><tr><th>VALUE (s)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>&gt;4.7 × 10<sup>8</sup></strong></td><td>90</td><td><sup>1</sup> ABE</td><td>21</td><td>CNTR n bound in oxygen</td></tr><tr><td><strong>&gt;8.6 × 10<sup>7</sup></strong></td><td>90</td><td>BALDO...</td><td>94</td><td>CNTR (free) neutrons</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tbody><tr><td>&gt;1.37 × 10<sup>8</sup></td><td>90</td><td><sup>2</sup> AHARMIM</td><td>17</td><td>SNO n bound in deuteron</td></tr><tr><td>&gt;2.7 × 10<sup>8</sup></td><td>90</td><td>ABE</td><td>15C</td><td>CNTR n bound in oxygen</td></tr><tr><td>&gt;1.3 × 10<sup>8</sup></td><td>90</td><td>CHUNG</td><td>02B</td><td>SOU2 n bound in iron</td></tr><tr><td>&gt;1 × 10<sup>7</sup></td><td>90</td><td>BALDO...</td><td>90</td><td>CNTR See BALDO-CEOLIN 94</td></tr><tr><td>&gt;1.2 × 10<sup>8</sup></td><td>90</td><td>BERGER</td><td>90</td><td>FREJ n bound in iron</td></tr><tr><td>&gt;4.9 × 10<sup>5</sup></td><td>90</td><td>BRESSI</td><td>90</td><td>CNTR Reactor neutrons</td></tr><tr><td>&gt;4.7 × 10<sup>5</sup></td><td>90</td><td>BRESSI</td><td>89</td><td>CNTR See BRESSI 90</td></tr><tr><td>&gt;1.2 × 10<sup>8</sup></td><td>90</td><td>TAKITA</td><td>86</td><td>CNTR n bound in oxygen</td></tr><tr><td>&gt;1 × 10<sup>6</sup></td><td>90</td><td>FIDECARO</td><td>85</td><td>CNTR Reactor neutrons</td></tr><tr><td>&gt;8.8 × 10<sup>7</sup></td><td>90</td><td>PARK</td><td>85B</td><td>CNTR</td></tr><tr><td>&gt;3 × 10<sup>7</sup></td><td></td><td>BATTISTONI</td><td>84</td><td>NUSX</td></tr><tr><td>&gt; 0.27-1.1 × 10<sup>8</sup></td><td></td><td>JONES</td><td>84</td><td>CNTR</td></tr><tr><td>&gt;2 × 10<sup>7</sup></td><td></td><td>CHERRY</td><td>83</td><td>CNTR</td></tr></tbody></table>

¹ ABE 21 supersedes ABE 15c.

² The AHARMIM 17 value is an unbounded limit (it does not assume a positive lifetime). The bounded limit is $1.23 \times 10^8$ sec.

## LIMIT ON $nn'$ OSCILLATIONS

Lee and Yang (LEE 56) proposed the existence of mirror world in an attempt to restore global parity symmetry. A possible candidate for dark matter. Limits depend on assumptions about fields $B$ and $B'$.$^1$ See the papers for details. See BEREZHIANI 18 for a recent discussion.

<table><thead><tr><th>VALUE (s)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>&gt;448</strong></td><td>90</td><td>SEREBROV</td><td>09A</td><td>CNTR Assumes B' &lt; 100 nT</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tbody><tr><td>&gt; 1</td><td>95</td><td><sup>1</sup> BAN</td><td>23</td><td>CNTR scan of B field</td></tr><tr><td>&gt; 1</td><td>95</td><td><sup>2</sup> ALMAZAN</td><td>22</td><td>CNTR STEREO, hidden neutron search |m<sub>n</sub> - m<sub>p</sub>| ≥ 0.</td></tr><tr><td>&gt; 9</td><td>95</td><td><sup>3</sup> ABEL</td><td>21</td><td>CNTR UCN, scan of B field</td></tr><tr><td>&gt; 17</td><td>95</td><td><sup>4</sup> BEREZHIANI</td><td>18</td><td>CNTR UCN, scan of B field</td></tr><tr><td>&gt; 12</td><td>95</td><td><sup>5</sup> ALTAREV</td><td>09A</td><td>CNTR UCN, scan 0 ≤ B ≤ 12.5 μT</td></tr><tr><td>&gt;414</td><td>90</td><td>SEREBROV</td><td>08</td><td>CNTR UCN, B field on &amp; off</td></tr><tr><td>&gt;103</td><td>95</td><td>BAN</td><td>07</td><td>CNTR UCN, B field on &amp; off</td></tr></tbody></table>

¹ BAN 23 determine limits on the oscillation time for the $|\delta m(nn')|$ range of 2-59 peV. The quoted value is $\tau_{nn'}/\sqrt{\cos(\beta)} > 1$ sec. for B in 30-1143 μT, for the case $\beta = 0$.

² ALMAZAN 22 reports an experimental constraint on the probability for neutron conversion into a hidden neutron, $p < 3.1 \times 10^{-11}$ at 95% CL, which may be used to set a limit on the $nn'$ oscillation time.

³ ABEL 21 determine several limits on the oscillation time as a function of the mirror magnetic field $B'$, and of the fixed angle, $\beta$, between the applied magnetic field and $B'$. The latter is assumed to be bound to Earth. Two values are quoted from two analysis methods: (i) $\tau_{nn'}/\sqrt{\cos(\beta)} > 9$ sec for $B'$ in 5-25.4 μT, and (ii) for any angle $\beta$, $\tau_{nn'} > 6$ sec for $B'$ in 0.4-25.7 μT. The authors also quote a limit of 352 sec for the case $B' = 0$ T.

⁴ The B field was set to (0.09, 0.12, 0.21) G. Limits on oscillation time are valid for any mirror field $B'$ in (0.08-0.17) G, and for aligned fields $B$ and $B'$. For larger values of $B'$, the limits are significantly reduced.

⁵ Losses of neutrons due to oscillations to mirror neutrons would be maximal when the magnetic fields $B$ and $B'$ in the two worlds were equal. Hence the scan over B by ALTAREV 09A: the limit applies for any $B'$ over the given range. At $B' = 0$, the limit is 141 s (95% CL).

## n DECAY MODES

<table><thead><tr><th>Mode</th><th>Fraction (Γ<sub>f</sub>/Γ)</th><th>Confidence level</th></tr></thead></table>

Γ<sub>1</sub> $pe^{-\bar{\nu}_e}$ 100 %

Γ<sub>2</sub> $pe^{-\bar{\nu}_e\gamma}$ [a] (9.2±0.7) × 10<sup>-3</sup>

Γ<sub>3</sub> hydrogen-atom $\bar{\nu}_e$ < 2.7 × 10<sup>-3</sup>

### Charge conservation (Q) violating mode

Γ<sub>4</sub> $p\nu_e\bar{\nu}_e$ Q < 8 × 10<sup>-27</sup>

### Baryon number violating decay

Γ<sub>5</sub> $e^+e^-$ invisible

[a] This limit is for $\gamma$ energies between 0.4 and 782 keV.

## n BRANCHING RATIOS

<table><thead><tr><th>Γ(p e<sup>-</sup>ν<sub>e</sub>γ)/Γ<sub>total</sub></th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>9.17±0.24±0.64</strong></td><td></td><td><sup>1</sup> BALES</td><td>16</td><td>RDK2 Two different set-ups</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tbody><tr><td>3.09±0.11±0.30</td><td><sup>2</sup> COOPER</td><td>10</td><td>CNTR See BALES 16</td></tr><tr><td>3.13±0.11±0.33</td><td>NICO</td><td>06</td><td>CNTR See COOPER 10</td></tr><tr><td>&lt;6.9</td><td><sup>3</sup> BECK</td><td>02</td><td>CNTR γ, p, e<sup>-</sup> coincidence</td></tr></tbody></table>

¹ BALES 16 gets a branching fraction of $(5.82 \pm 0.23 \pm 0.62) \times 10^{-3}$ for a photon energy range 0.4 to 14.0 keV, and with a different detector array, $(3.35 \pm 0.05 \pm 0.15) \times 10^{-3}$ for 14.1 to 782 keV. Our result above is the sum; the error on the sum is completely dominated by the error on the lower range.

² This COOPER 10 result is for $\gamma$ energies between 15 and 340 keV.

³ This BECK 02 limit is for $\gamma$ energies between 35 and 100 keV.

<table><thead><tr><th>Γ(hydrogen-atom ν<sub>e</sub>)/Γ<sub>total</sub></th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>&lt;0.27 × 10<sup>-2</sup></strong></td><td>95</td><td><sup>1</sup> CZARNECKI</td><td>18</td><td>Lifetime analysis</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>&lt;3 × 10<sup>-2</sup></td><td>95</td><td><sup>2</sup> GREEN</td><td>90</td><td>RVUE</td></tr></table>

¹ CZARNECKI 18 limit from an analysis of experimental discrepancies on the neutron lifetime and axial coupling applies as well to other possible exotic neutron decays.

² GREEN 90 infers that $\tau(\text{hydrogen-atom } \bar{\nu}_e) > 3 \times 10^4$ s by comparing neutron lifetime measurements made in storage experiments with those made in $\beta$-decay experiments. However, the result depends sensitively on the lifetime measurements, and does not of course take into account more recent measurements of same.

<table><thead><tr><th>Γ(pν<sub>e</sub>ν<sub>e</sub>)/Γ<sub>total</sub></th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>&lt;8 × 10<sup>-27</sup></td><td>68</td><td><sup>1</sup> NORMAN</td><td>96</td><td>RVUE <sup>71</sup>Ga → <sup>71</sup>Ge neutrals</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tbody><tr><td>&lt;9.7 × 10<sup>-18</sup></td><td>90</td><td>ROY</td><td>83</td><td>CNTR <sup>113</sup>Cd → <sup>113</sup>Mnneut.</td></tr><tr><td>&lt;7.9 × 10<sup>-21</sup></td><td></td><td>VAIDYA</td><td>83</td><td>CNTR <sup>87</sup>Rb → <sup>87</sup>MnSrneut.</td></tr><tr><td>&lt;9 × 10<sup>-24</sup></td><td>90</td><td>BARABANOV</td><td>80</td><td>CNTR <sup>71</sup>Ga → <sup>71</sup>GeX</td></tr><tr><td>&lt;3 × 10<sup>-19</sup></td><td></td><td>NORMAN</td><td>79</td><td>CNTR <sup>87</sup>Rb → <sup>87</sup>MnSrneut.</td></tr></tbody></table>

¹ NORMAN 96 gets this limit by attributing SAGE and GALLEX counting rates to the charge-nonconserving transition $^{71}$Ga → $^{71}$Ge+neutrals rather than to solar-neutrino reactions.
## $\Gamma(e^+ e^- \text{invisibl e})/\Gamma_{\text{total}}$

Baryon number violating decay

<table><thead><tr><th>VALUE</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>• • •</td><td></td><td></td><td></td><td>We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>&lt;0.01</td><td>90</td><td>1 KLOPF</td><td>19</td><td>CNTR re-interpretation of MUND 13</td></tr><tr><td>&lt;1 × 10<sup>-4</sup></td><td>90</td><td>2 SUN</td><td>18</td><td>SPEC Ultracold n, polarized</td></tr><tr><td colspan="5"><sup>1</sup>KLOPF 19 value is for baryon number violating decay of neutron to electrons plus an invisible state, χ. The limit is valid for KE(e<sup>+</sup> e<sup>-</sup>) range between 32 keV and 664 keV, strengthening to few × 10<sup>-4</sup> above approximately 100 keV.</td></tr><tr><td colspan="5"><sup>2</sup>SUN 18 value is for baryon number violating decay of neutron to electrons plus an invisible state, χ. The limit is valid for 644 keV > KE(e<sup>+</sup> e<sup>-</sup>) > 100 keV. Assuming this decay χe e is the only allowed χ decay channel, a 0.01 BR is ruled out for 644 keV > E(e<sup>+</sup> e<sup>-</sup>) > 100 keV at over 5σ.</td></tr></tbody></table>

## See the related review(s):

### Baryon Decay Parameters

#### $n \to p e^- \nu_e$ DECAY PARAMETERS

See the above "Note on Baryon Decay Parameters." For discussions of recent results, see the references cited at the beginning of the section on the neutron mean life. For discussions of the values of the weak coupling constants $g_A$ and $g_V$ obtained using the neutron lifetime and asymmetry parameter $A$, comparisons with other methods of obtaining these constants, and implications for particle physics and for astrophysics, see DUBBERS 91 and WOOLCOCK 91. For tests of the $V-A$ theory of neutron decay, see EROZOLIMSKII 91B, MOSTOVOI 96, NICO 05, SEV-ERIJNS 06, and ABELE 08.

#### $\lambda \equiv g_A / g_V$

<table><caption>WEIGHTED AVERAGE
-1.2754±0.0013 (Error scaled by 2.7)</caption><thead><tr><th>VALUE</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><b>-1.2754 ± 0.0013</b></td><td><b>OUR AVERAGE</b></td><td></td><td>Error includes scale factor of 2.7. See the ideogram below.</td></tr><tr><td>-1.2796 ± 0.0062</td><td>1 HASSAN</td><td>21</td><td>SPEC Proton recoil spectrum</td></tr><tr><td>-1.2677 ± 0.0028</td><td>2 BECK</td><td>20</td><td>SPEC Proton recoil spectrum</td></tr><tr><td>-1.27641 ± 0.00045 ± 0.00033</td><td>3 MAERKISCH</td><td>19</td><td>SPEC pulsed cold n, polarized</td></tr><tr><td>-1.2772 ± 0.0020</td><td>4 BROWN</td><td>18</td><td>UCNA Ultracold n, polarized</td></tr><tr><td>-1.2748 ± 0.0008 + 0.0010<br>-0.0011</td><td>5 MUND</td><td>13</td><td>SPEC Cold n, polarized</td></tr><tr><td>-1.275 ± 0.006 ± 0.015</td><td>SCHUMANN</td><td>08</td><td>CNTR Cold n, polarized</td></tr><tr><td>-1.2686 ± 0.0046 ± 0.0007</td><td>6 MOSTOVOI</td><td>01</td><td>CNTR A and B × polarizations</td></tr><tr><td>-1.266 ± 0.004</td><td>LIAUD</td><td>97</td><td>TPC Cold n, polarized, A</td></tr><tr><td>-1.2594 ± 0.0038</td><td>7 YEROZLIM...</td><td>97</td><td>CNTR Cold n, polarized, A</td></tr><tr><td>-1.262 ± 0.005</td><td>BOPP</td><td>86</td><td>SPEC Cold n, polarized, A</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>-1.27607 ± 0.00068</td><td>8 SAUL</td><td>20</td><td>SPEC Cold n, polarized, A</td></tr><tr><td>-1.284 ± 0.014</td><td>9 DARIUS</td><td>17</td><td>SPEC Cold n, unpolarized</td></tr><tr><td>-1.2755 ± 0.0030</td><td>10 MENDENHALL13</td><td></td><td>UCNA See BROWN 18</td></tr><tr><td>-1.27590 ± 0.00239 + 0.00331<br>-0.00377</td><td>11 PLASTER</td><td>12</td><td>UCNA See MENDENHALL 13</td></tr><tr><td>-1.27590 + 0.00409<br>-0.00445</td><td>LIU</td><td>10</td><td>UCNA See PLASTER 12</td></tr><tr><td>-1.2739 ± 0.0019</td><td>12 ABELE</td><td>02</td><td>SPEC See MUND 13</td></tr><tr><td>-1.274 ± 0.003</td><td>ABELE</td><td>97d</td><td>SPEC Cold n, polarized, A</td></tr><tr><td>-1.266 ± 0.004</td><td>SCHRECK...</td><td>95</td><td>TPC See LIAUD 97</td></tr><tr><td>-1.2544 ± 0.0036</td><td>EROZOLIM...</td><td>91</td><td>CNTR See YEROZOLIM-SKY 97</td></tr><tr><td>-1.226 ± 0.042</td><td>MOSTOVOY</td><td>83</td><td>RVUE</td></tr><tr><td>-1.261 ± 0.012</td><td>EROZOLIM...</td><td>79</td><td>CNTR Cold n, polarized, A</td></tr><tr><td>-1.259 ± 0.017</td><td>13 STRATOWA</td><td>78</td><td>CNTR p recoil spectrum, A</td></tr><tr><td>-1.263 ± 0.015</td><td>EROZOLIM...</td><td>77</td><td>CNTR See EROZOLIMSKII 79</td></tr><tr><td>-1.250 ± 0.036</td><td>13 DOBROZE...</td><td>75</td><td>CNTR See STRATOWA 78</td></tr><tr><td>-1.258 ± 0.015</td><td>14 KROHN</td><td>75</td><td>CNTR Cold n, polarized, A</td></tr><tr><td>-1.263 ± 0.016</td><td>15 KROPF</td><td>74</td><td>RVUE n decay alone</td></tr><tr><td>-1.250 ± 0.009</td><td>15 KROPF</td><td>74</td><td>RVUE n decay + nuclear ft</td></tr></tbody></table>

<figure><img src="image_713.png" /></figure>

## $\Gamma_S/\Gamma$

## $e^-$ ASYMMETRY PARAMETER A

This is the neutron-spin electron-momentum correlation coefficient. Unless otherwise noted, the values are corrected for radiative effects and weak magnetism. In the Standard Model, A is related to $\lambda \equiv g_A/g_V$ by $A = -2 \lambda (\lambda + 1) / (1 + 3\lambda^2)$; this assumes that $g_A$ and $g_V$ are real.

<table><caption>WEIGHTED AVERAGE
-0.11958±0.00021 (Error scaled by 1.2)</caption><thead><tr><th>VALUE</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><b>-0.11958 ± 0.00021</b></td><td><b>OUR AVERAGE</b></td><td></td><td>Error includes scale factor of 1.2. See the ideogram below.</td></tr><tr><td>-0.11985 ± 0.00017 ± 0.00012</td><td>1 MAERKISCH</td><td>19</td><td>SPEC pulsed cold n, polarized</td></tr><tr><td>-0.12015 ± 0.00034 ± 0.00063</td><td>2 BROWN</td><td>18</td><td>UCNA Ultracold n, polarized</td></tr><tr><td>-0.11926 ± 0.0031 + 0.00036<br>-0.00042</td><td>3 MUND</td><td>13</td><td>SPEC Cold n, polarized</td></tr><tr><td>-0.1160 ± 0.0009 ± 0.0012</td><td>LIAUD</td><td>97</td><td>TPC Cold n, polarized</td></tr><tr><td>-0.1135 ± 0.0014</td><td>4 YEROZLIM...</td><td>97</td><td>CNTR Cold n, polarized</td></tr><tr><td>-0.1146 ± 0.0019</td><td>BOPP</td><td>86</td><td>SPEC Cold n, polarized</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>-0.11972 ± 0.00025</td><td>5 SAUL</td><td>20</td><td>SPEC Cold n, polarized</td></tr><tr><td>-0.11952 ± 0.00110</td><td>6 MENDENHALL13</td><td></td><td>UCNA See BROWN 18</td></tr><tr><td>-0.11966 ± 0.00089 + 0.00123<br>-0.00140</td><td>7 PLASTER</td><td>12</td><td>UCNA See MENDENHALL 13</td></tr><tr><td>-0.11966 ± 0.00089 + 0.00123<br>-0.00140</td><td>LIU</td><td>10</td><td>UCNA See PLASTER 12</td></tr><tr><td>-0.1138 ± 0.0046 ± 0.0021</td><td>PATTIE</td><td>09</td><td>SPEC Ultracold n, polarized</td></tr><tr><td>-0.1189 ± 0.0007</td><td>8 ABELE</td><td>02</td><td>SPEC See MUND 13</td></tr><tr><td>-0.1168 ± 0.0017</td><td>9 MOSTOVOI</td><td>01</td><td>CNTR Inferred</td></tr><tr><td>-0.1189 ± 0.0012</td><td>ABELE</td><td>97d</td><td>SPEC Cold n, polarized</td></tr><tr><td>-0.1160 ± 0.0009 ± 0.0011</td><td>SCHRECK...</td><td>95</td><td>TPC See LIAUD 97</td></tr><tr><td>-0.1116 ± 0.0014</td><td>EROZOLIM...</td><td>91</td><td>CNTR See YEROZOLIM-SKY 97</td></tr><tr><td>-0.114 ± 0.005</td><td>10 EROZOLIM...</td><td>79</td><td>CNTR Cold n, polarized</td></tr><tr><td>-0.113 ± 0.006</td><td>10 KROHN</td><td>75</td><td>CNTR Cold n, polarized</td></tr></tbody></table>

<figure><img src="image_714.png" /></figure>

<footnote n="1">¹ HASSAN 21 include earlier data of DARIUS 17. The value is extracted from the angular correlation coefficient a.</footnote>

<footnote n="2">² BECK 20 calculates this value from the measurement of the $\beta$-decay $e^- \nu_e$ angular correlation coefficient a.</footnote>

<footnote n="3">³ MAERKISCH 19 gets $A = -0.11985 \pm 0.00017 \pm 0.00012$.</footnote>

<footnote n="4">⁴ BROWN 18 gets $A = -0.12054 \pm 0.00044 \pm 0.00068$ and $\lambda = -1.2783 \pm 0.0022$. We quote the combined values that include the earlier UCNA measurements (MENDEN-HALL 13).</footnote>

<footnote n="5">⁵ This MUND 13 value includes earlier PERKEO II measurements (ABELE 02 and ABELE 97d).</footnote>

<footnote n="6">⁶ MOSTOVOI 01 measures the two P-odd correlations A and B, or rather SA and SB, where S is the n polarization, in free neutron decay.</footnote>

<footnote n="7">⁷ YEROZOLIMSKY 97 makes a correction to the EROZOLIMSKII 91 value.</footnote>

<footnote n="8">⁸ SAUL 20 quote this value of $\lambda$ under the SM assumption of the Fierz term $b = 0$. In a combined fit authors extract a value of $\lambda = -1.2792 \pm 0.0060$.</footnote>

<footnote n="9">⁹ DARIUS 17 calculates this value from the measurement of the a parameter (see below). Data is included in HASSAN 21.</footnote>

<footnote n="10">¹⁰ MENDENHALL 13 gets $A = -0.11954 \pm 0.00055 \pm 0.00098$ and $\lambda = -1.2756 \pm 0.0030$. We quote the nearly identical values that include the earlier UCNA measurement (PLASTER 12), with a correction to that result.</footnote>

<footnote n="11">¹¹ This PLASTER 12 value is identical with that given in LIU 10, but the experiment is now described in detail.</footnote>

<footnote n="12">¹² This is the combined result of ABELE 02 and ABELE 97d.</footnote>

<footnote n="13">¹³ These experiments measure the absolute value of $g_A/g_V$ only.</footnote>

<footnote n="14">¹⁴ KROHN 75 includes events of CHRISTENSEN 70.</footnote>

<footnote n="15">¹⁵ KROPF 74 reviews all data through 1972.</footnote>

<footnote n="1">¹ MAERKISCH 19 further derive a value for the CKM-element $|V_{ub}| = 0.97351 \pm 0.00060$, using $\tau_n = 879.7(8)$ sec and the relation from CZARNECKI 18.</footnote>

<footnote n="2">² BROWN 18 gets $A = -0.12054 \pm 0.00044 \pm 0.00068$ and $\lambda = -1.2783 \pm 0.0022$. We quote the combined values that include the earlier UCNA measurements (MENDEN-HALL 13).</footnote>

<footnote n="3">³ This MUND 13 value includes earlier PERKEO II measurements (ABELE 02 and ABELE 97d), with a correction to those results.</footnote>

<footnote n="4">⁴ YEROZOLIMSKY 97 makes a correction to the EROZOLIMSKII 91 value.</footnote>

<footnote n="5">⁵ Under the SM assumption that the Fierz term $b = 0$, SAUL 20 obtain the quoted asymmetry parameter A and $\lambda = -1.27607 \pm 0.00068$. In a combined fit authors extract the values $A = -0.1209 \pm 0.0015$, $\lambda = -1.2792 \pm 0.0060$, and $b = 0.017 \pm 0.021$.</footnote>
⁶ MENDENHALL 13 gets $A = -0.11954 \pm 0.00055 \pm 0.00098$ and $\lambda = -1.2756 \pm 0.0030$. We quote the nearly identical values that include the earlier UCNA measurement (PLASTER 12), with a correction to that result.

⁷ This PLASTER 12 value is identical with that given in LIU 10, but the experiment is now described in detail.

⁸ This is the combined result of ABELE 02 and ABELE 97d.

⁹ MOSTOVOI 01 calculates this from its measurement of $\lambda = g_A/g_V$ above.

¹⁰ These results are not corrected for radiative effects and weak magnetism, but the corrections are small compared to the errors.

## $\nu_e$ ASYMMETRY PARAMETER B

This is the neutron-spin antineutrino-momentum correlation coefficient. In the Standard Model, B is related to $\lambda \equiv g_A/g_V$ by $B = 2\lambda(\lambda - 1) / (1 + 3\lambda^2)$; this assumes that $g_A$ and $g_V$ are real.

<table><thead><tr><th>VALUE</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>0.9807 ± 0.0030</strong></td><td><strong>OUR AVERAGE</strong></td><td></td><td></td></tr><tr><td>0.9802 ± 0.0034 ± 0.0036</td><td>SCHUMANN</td><td>07</td><td>CNTR Cold n, polarized</td></tr><tr><td>0.967 ± 0.006 ± 0.010</td><td>KREUZ</td><td>05</td><td>CNTR Cold n, polarized</td></tr><tr><td>0.9801 ± 0.0046</td><td>SEREBROV</td><td>98</td><td>CNTR Cold n, polarized</td></tr><tr><td>0.9894 ± 0.0083</td><td>KUZNETSOV</td><td>95</td><td>CNTR Cold n, polarized</td></tr><tr><td>1.00 ± 0.05</td><td>CHRISTENSEN</td><td>70</td><td>CNTR Cold n, polarized</td></tr><tr><td>0.995 ± 0.034</td><td>EROZOLIM...</td><td>70c</td><td>CNTR Cold n, polarized</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>0.9876 ± 0.0004</td><td>1</td><td>MOSTOVOI</td><td>01</td><td>CNTR Inferred</td></tr></table>

¹ MOSTOVOI 01 calculates this from its measurement of $\lambda = g_A/g_V$ above.

## PROTON ASYMMETRY PARAMETER C

Describes the correlation between the neutron spin and the proton momentum. In the Standard Model, C is related to $\lambda \equiv g_A/g_V$ by $C = -x_c(A + B) = x_c 4\lambda / (1 + 3\lambda^2)$, where $x_c = 0.27484$ is a kinematic factor; this assumes that $g_A$ and $g_V$ are real.

<table><thead><tr><th>VALUE</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>-0.2377 ± 0.0010 ± 0.0024</strong></td><td><strong>SCHUMANN</strong></td><td><strong>08</strong></td><td><strong>CNTR Cold n, polarized</strong></td></tr></tbody></table>

## $e\bar{e}$ ANGULAR CORRELATION COEFFICIENT a

For a review of past experiments and plans for future measurements of the a parameter, see WIETFELDT 05. In the Standard Model, a is related to $\lambda \equiv g_A/g_V$ by $a = (1 - \lambda^2) / (1 + 3\lambda^2)$; this assumes that $g_A$ and $g_V$ are real.

<table><thead><tr><th>VALUE</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>-0.1049 ± 0.0013</strong></td><td><strong>OUR AVERAGE</strong></td><td></td><td>Error includes scale factor of 1.8.</td></tr><tr><td>-0.10782 ± 0.00124 ± 0.00133</td><td>1 HASSAN</td><td>21</td><td>SPEC Proton recoil spectrum</td></tr><tr><td>-0.10430 ± 0.00084</td><td>BECK</td><td>20</td><td>SPEC Proton recoil spectrum</td></tr><tr><td>-0.1054 ± 0.0055</td><td>BYRNE</td><td>02</td><td>SPEC Proton recoil spectrum</td></tr><tr><td>-0.1017 ± 0.0051</td><td>STATOWA</td><td>08</td><td>CNTR Cold n, polarized</td></tr><tr><td>-0.091 ± 0.039</td><td>GRIGOREV</td><td>68</td><td>SPEC Proton recoil spectrum</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>-0.1090 ± 0.0030 ± 0.0028</td><td>2 DARIUS</td><td>17</td><td>SPEC Cold n, unpolarized</td></tr></table>

<table><tr><td>-0.1045 ± 0.0014</td><td>3</td><td>MOSTOVOI</td><td>01</td><td>CNTR Inferred</td></tr></table>

¹ The result of HASSAN 21 includes the data of DARIUS 17, and thus supersedes those entries. HASSAN 21 uses the asymmetry in time-of-flight between the beta electron and recoil proton in delayed coincidence.

² DARIUS 17 exploits a “wishbone” correlation, where the p time of flight is correlated with the momentum of the electron in delayed coincidence. Data is included in HASSAN 21.

³ MOSTOVOI 01 calculates this from its measurement of $\lambda = g_A/g_V$ above.

## $\phi_{AV}$, PHASE OF $g_A$ RELATIVE TO $g_V$

Time reversal invariance requires this to be 0 or 180°. This is related to D given in the next data block and $\lambda \equiv g_A/g_V$ by $\sin(\phi_{AV}) = D(1+3\lambda^2)/2|\lambda|$; this assumes that $g_A$ and $g_V$ are real.

<table><thead><tr><th>VALUE (°)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>180.017 ± 0.026</strong></td><td><strong>OUR AVERAGE</strong></td><td></td><td></td><td></td></tr><tr><td>180.012 ± 0.028</td><td>68</td><td>CHUPP</td><td>12</td><td>CNTR Cold n, polarized &gt; 91%</td></tr><tr><td>180.04 ± 0.09</td><td>SOLDNER</td><td>04</td><td>CNTR Cold n, polarized</td></tr><tr><td>180.08 ± 0.13</td><td>LISING</td><td>00</td><td>CNTR Polarized &gt; 93%</td></tr></tbody></table><table><thead><tr><th>VALUE (°)</th><th>CL%</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>180.013 ± 0.028</strong></td><td>MUMM</td><td>11</td><td>CNTR See CHUPP 12</td></tr><tr><td>179.71 ± 0.39</td><td>EROZOLIM...</td><td>78</td><td>CNTR Cold n, polarized</td></tr><tr><td>180.35 ± 0.43</td><td>EROZOLIM...</td><td>74</td><td>CNTR Cold n, polarized</td></tr><tr><td>181.1 ± 1.3</td><td>1</td><td>KROPF</td><td>74</td><td>RVUE n decay</td></tr><tr><td>180.14 ± 0.22</td><td>STEINBERG</td><td>74</td><td>CNTR Cold n, polarized</td></tr></tbody></table>

¹ KROPF 74 reviews all data through 1972.

## TRIPLE CORRELATION COEFFICIENT D

These are measurements of the component of n spin perpendicular to the decay plane in β decay. Should be zero if T invariance is not violated.

<table><thead><tr><th>VALUE (units 10<sup>-4</sup>)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>-1.2 ± 2.0</strong></td><td><strong>OUR AVERAGE</strong></td><td></td><td></td></tr><tr><td>-0.94 ± 1.89 ± 0.97</td><td>CHUPP</td><td>12</td><td>CNTR Cold n, polarized &gt; 91%</td></tr><tr><td>-2.8 ± 6.4 ± 3.0</td><td>SOLDNER</td><td>04</td><td>CNTR Cold n, polarized</td></tr><tr><td>-6 ± 12 ± 5</td><td>LISING</td><td>00</td><td>CNTR Polarized &gt; 93%</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><thead><tr><th>VALUE (units 10<sup>-4</sup>)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>-0.96 ± 1.89 ± 1.01</strong></td><td>MUMM</td><td>11</td><td>CNTR See CHUPP 12</td></tr><tr><td>+22 ± 30</td><td>EROZOLIM...</td><td>78</td><td>CNTR Cold n, polarized</td></tr><tr><td>-27 ± 50</td><td>1</td><td>EROZOLIM...</td><td>74</td><td>CNTR Cold n, polarized</td></tr><tr><td>-11 ± 17</td><td>STEINBERG</td><td>74</td><td>CNTR Cold n, polarized</td></tr></tbody></table>

¹ EROZOLIMSKII 78 says asymmetric proton losses and nonuniform beam polarization may give a systematic error up to $30 \times 10^{-4}$, thus increasing the EROZOLIMSKII 74 error to $50 \times 10^{-4}$. STEINBERG 74 and STEINBERG 76 estimate these systematic errors to be insignificant in their experiment.

## TRIPLE CORRELATION COEFFICIENT R

Another test of time-reversal invariance. R measures the polarization of the electron in the direction perpendicular to the plane defined by the neutron spin and the electron momentum. R = 0 for T invariance.

<table><thead><tr><th>VALUE</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>+0.004 ± 0.012 ± 0.005</strong></td><td><strong>1 KOZELA</strong></td><td><strong>12</strong></td><td><strong>CNTR Mott polarimeter</strong></td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>+0.008 ± 0.015 ± 0.005</td><td>KOZELA</td><td>09</td><td>CNTR See KOZELA 12</td></tr></table>

¹ KOZELA 12 also measures the polarization of the electron along the direction of the neutron spin. This is nonzero in the Standard Model; the correlation coefficient is $N = -0.067 \pm 0.011 \pm 0.004$.

## FIERZ INTERFERENCE TERM b

The coefficient of the Fierz interference term, b, probes additional contributions to the differential decay rate of the neutron from scalar or tensor current interactions, beyond the Standard Model.

<table><thead><tr><th>VALUE</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>0.017 ± 0.020 ± 0.003</strong></td><td><strong>1 SAUL</strong></td><td><strong>20</strong></td><td><strong>SPEC Cold n, polarized</strong></td></tr></tbody></table>

¹ In a combined fit SAUL 20 extract this best fit value of the Fierz interference term b and the values $A = -0.1209 \pm 0.0015$ and $\lambda = -1.2792 \pm 0.0060$. For b it translates into a 90% CL region of $-0.018 \le b \le 0.052$ as a function of A.

## n REFERENCES

We have omitted some papers that have been superseded by later experiments. See our earlier editions.

<table><tbody><tr><td>BAN</td><td>PR 131 191801</td><td>G. Ban et al.</td><td>(CAEN, ZURI, ISNG, SORB+)</td></tr><tr><td>ALMAZAN</td><td>PR 128 061801</td><td>H. Almazan et al.</td><td>(STEREO Collab.)</td></tr><tr><td>ABE</td><td>PR D103 012008</td><td>K. Abel et al.</td><td>(Super-Kamiokande Collab.)</td></tr><tr><td>ABEL</td><td>PL B812 135993</td><td>C. Abel et al.</td><td>(nEDM Collab.)</td></tr><tr><td>GONZALEZ</td><td>PR 127 162501</td><td>F.M. Gonzalez et al.</td><td>(UCNTau Collab.)</td></tr><tr><td>HASSAN</td><td>PR C103 045502</td><td>M.T. Hassan et al.</td><td>(aCORN Collab.)</td></tr><tr><td>HEADOCK</td><td>PR 124 082501</td><td>B. Heacock et al.</td><td>(NIST, RIKEN, NAGO+)</td></tr><tr><td>TIESINGA</td><td>RMP 93 025010</td><td>E. Tiesinga et al.</td><td>(NIST)</td></tr><tr><td>WILSON</td><td>PR C104 045501</td><td>J.T. Wilson et al.</td><td>(JHU, DURH)</td></tr><tr><td>ABEL</td><td>PR 124 081803</td><td>C. Abel et al.</td><td>(nEDM Collab.)</td></tr><tr><td>BECK</td><td>PR C101 055506</td><td>M. Beck et al.</td><td>(aSPECT Collab.)</td></tr><tr><td>FILIN</td><td>PR 124 082501</td><td>A.A. Filin et al.</td><td>(PERKEQ III Collab.)</td></tr><tr><td>SAUL</td><td>PR 125 112501</td><td>H. Saul et al.</td><td>(PERKEQ II Collab.)</td></tr><tr><td>KLOPF</td><td>PR 122 222503</td><td>M. Klopf et al.</td><td>(PERKEQ II Collab.)</td></tr><tr><td>MAERKISCH</td><td>PR 122 242501</td><td>B. Maerkisch et al.</td><td>(TUM, ILL+)</td></tr><tr><td>SCHUMACHER</td><td>LHEP 4.4</td><td>M. Schumacher</td><td>(GOET)</td></tr><tr><td>BEREZHNIK</td><td>EPI C78 717</td><td>Z. Berezhian et al.</td><td>(AQUIN, INFJ, ILLG+)</td></tr><tr><td>BROWN</td><td>PR C97 035505</td><td>M.A.-P. Brown et al.</td><td>(UCNA Collab.)</td></tr><tr><td>CZARNECKI</td><td>PR 120 200202</td><td>A. Czarnecki, W.J. Marciano, A. Sirlin</td><td>(ALBE+)</td></tr><tr><td>EZHOV</td><td>JETPL 107 671</td><td>V.F. Ehzhov et al.</td><td>(PNPI, LENSU, CAEN+)</td></tr><tr><td>PATTIE</td><td>SCI 360 627</td><td>R.W. Pattie Jr. et al.</td><td>(LASL, IND, NCSU+)</td></tr><tr><td>SEREBROV</td><td>PR C97 055503</td><td>A.P. Serebrov et al.</td><td>(PNPI, ILLG, RAL)</td></tr><tr><td>Also</td><td>JETPL 106 623</td><td>A.P. Serebrov et al.</td><td>(PNPI, ILLG, RAL)</td></tr><tr><td>SUN</td><td>PR C97 052501</td><td>X. Sun et al.</td><td>(UCNA Collab.)</td></tr><tr><td>AHARMIM</td><td>PR D96 092005</td><td>B. Aharmin et al.</td><td>(SNO Collab.)</td></tr><tr><td>DARIUS</td><td>PR 119 042502</td><td>G. Darius et al.</td><td>(aCORN at NIST)</td></tr><tr><td>SAHOO</td><td>PR D95 013002</td><td>B.K. Sahoo</td><td>(AHMEB)</td></tr><tr><td>BALES</td><td>PR 116 242501</td><td>M.J. Bales et al.</td><td>(RDK II Collab.)</td></tr><tr><td>GRANER</td><td>PR 116 161601</td><td>B. Graner et al.</td><td>(WASH)</td></tr><tr><td>Also</td><td>PR 119 119911 (erat.)</td><td>B. Graner et al.</td><td>(WASH)</td></tr><tr><td>MOHR</td><td>RMP 88 035009</td><td>P.J. Mohr, D.B. Newell, B.N. Taylor</td><td>(NIST)</td></tr><tr><td>PHILLIPS</td><td>PRPL 612 1</td><td>D.G. Phillips II et al.</td><td>(MICH, UCB, WASH+)</td></tr><tr><td>ABE</td><td>PR D91 072006</td><td>K. Abel et al.</td><td>(GWU, MCHS+)</td></tr><tr><td>ARZUMANOV</td><td>PL B745 79</td><td>S. Arzumanov et al.</td><td>(ILLG, KIAE)</td></tr><tr><td>PENDLEBURY</td><td>PR D92 092001</td><td>J.M. Pendlebury et al.</td><td>(ETHZ, PSI, SUSS)</td></tr><tr><td>SEREBROV</td><td>PR C92 055501</td><td>A.P. Serebrov et al.</td><td>(PNPI, ILLG, IOFF)</td></tr><tr><td>EPSTEIN</td><td>PR D90 074027</td><td>Z. Steinig, G. Paz, J. Roy</td><td>(UMD, WAYN)</td></tr><tr><td>MYERS</td><td>PR 113 262506</td><td>L.S. Myers et al.</td><td>(COMPTON/MAX-lab Collab.)</td></tr><tr><td>SEREBROV</td><td>PR 111 1162501</td><td>M.P. Mendenhall et al.</td><td>(PNPI, ILLG, IOFF)</td></tr><tr><td>MENDENHALL</td><td>PR C87 032501</td><td>M. Mendenhall et al.</td><td>(UCNA Collab.)</td></tr><tr><td>MUND</td><td>PR 110 172502</td><td>D. Mund et al.</td><td>(HEID, ILLG)</td></tr><tr><td>YUE</td><td>PR 111 222501</td><td>A.T. Yue et al.</td><td>(UMD, NIST, TENN, ORNL+)</td></tr><tr><td>ARZUMANOV</td><td>JETPL 95 224</td><td>S.S. Arzumanov et al.</td><td>(KIAE)</td></tr><tr><td>CHUPP</td><td>PR C86 035505</td><td>T.E. Chupp et al.</td><td>(MICH, UCB, WASH+)</td></tr><tr><td>GRIESSHAM...</td><td>PPNP 57 841</td><td>H.W. Griesshammer et al.</td><td>(GWU, MCHS+)</td></tr><tr><td>KOZELA</td><td>PR C85 045501</td><td>A. Kozeia et al.</td><td>(nTRV Collab.)</td></tr><tr><td>MOHR</td><td>RMP 84 1527</td><td>P.J. Mohr, B.N. Taylor, D.B. Newell</td><td>(NIST)</td></tr><tr><td>PLASTER</td><td>RMP 99 055501</td><td>B. Plaster et al.</td><td>(UCNA Collab.)</td></tr><tr><td>STEYERL</td><td>PR C95 065503</td><td>A. Steyerl et al.</td><td>(URI, SUSS)</td></tr><tr><td>BRESSI</td><td>PR A83 052101</td><td>G. Bressi et al.</td><td>(LEGN, PAVIL, PADO, TRST+)</td></tr><tr><td>DUBBERS</td><td>RMP 83 1111</td><td>D. Dubbers, M.G. Schmidt</td><td>(HEID)</td></tr><tr><td>MUMM</td><td>PR 107 102301</td><td>H.P. Mumm et al.</td><td>(NIST, WASH, MICH, LBL+)</td></tr><tr><td>WIETFELDT</td><td>PR C83 1329</td><td>F.E. Wietfelt, G.L. Greene</td><td>(TULA, TENN)</td></tr><tr><td>COOPER</td><td>PR C81 035501</td><td>R.L. Cooper et al.</td><td>(MICH, NIST, TULA+)</td></tr><tr><td>LIU</td><td>PR 105 181803</td><td>J. Liu et al.</td><td>(UCNA Collab.)</td></tr><tr><td>Also</td><td>PR 105 219903 (erat.)</td><td>J. Liu et al.</td><td>(UCNA Collab.)</td></tr><tr><td>PICHMAIER</td><td>PL B869 221</td><td>A. Pichmaier et al.</td><td>(TUM, PNPI, ILLG)</td></tr><tr><td>ALAREV</td><td>PR D80 03200</td><td>I. Altarev et al.</td><td>(TUM, RAR, CAEN+)</td></tr><tr><td>KOZELA</td><td>PR 102 172301</td><td>A. Kozeia et al.</td><td>(JAGL, CRAC, PSI, CAEN+)</td></tr><tr><td>LAMOREAUX</td><td>JP G36 104002</td><td>S.K. Lamoreaux, R. Golub</td><td>(YALE, NCSU)</td></tr><tr><td>LAMOPATRA</td><td>JP G36 104006</td><td>M.N. Mohapatra</td><td>(UMD)</td></tr><tr><td>PATTIE</td><td>PR 102 012301</td><td>R.W. Pattie Jr. et al.</td><td>(Los Alamos UCNA Collab.)</td></tr><tr><td>SEREBROV</td><td>NIM A611 137</td><td>A.P. Serebrov et al.</td><td>(PNPI, IOFF, ILLG+)</td></tr><tr><td>ABELE</td><td>PPNP 50 51</td><td>H. Abele</td><td>(HEID)</td></tr><tr><td>MOHR</td><td>RMP 80 633</td><td>P.J. Mohr, B.N. Taylor, D.B. Newell</td><td>(NIST)</td></tr><tr><td>SCHUMANN</td><td>PR 105 151801</td><td>M. Schumann et al.</td><td>(HEID, ILLG, KARL+)</td></tr><tr><td>SEREBROV</td><td>PL B663 181</td><td>A.P. Serebrov et al.</td><td>(PNPI, IOFF, ILLG+)</td></tr><tr><td>BAKER</td><td>PR 98 149102</td><td>C.A. Baker et al.</td><td>(RAL, SUSS, ILLG)</td></tr><tr><td>BAN</td><td>RMP 99 16103</td><td>G. Ban et al.</td><td>(CAEN, JAGL, PSI, JINR+)</td></tr><tr><td>BELUSHKIN</td><td>PR C75 035201</td><td>M.A. Belushkin, H.W. Hammer, U.-G. Meissner (BONN+)</td><td></td></tr><tr><td>LAMOREAUX</td><td>PR 98 194021</td><td>S.K. Lamoreaux, R. Golub</td><td>(YALE, NCSU)</td></tr><tr><td>SCHUMANN</td><td>PR 99 191803</td><td>M. Schumann et al.</td><td>(HEID, ILLG, KARL+)</td></tr><tr><td>SILENKO</td><td>PRPL 4 468</td><td>A.Ya. Silenko</td><td>(Bеляруssian U.)</td></tr><tr><td>BAKER</td><td>PR 97 131801</td><td>C.A. Baker et al.</td><td>(RAL, SUSS, ILLG)</td></tr><tr><td>NICO</td><td>NAT 444 1059</td><td>J.S. Nico et al.</td><td>(NIST, TULN, MICH, UMD+)</td></tr><tr><td>SEVERIJNS</td><td>RMP 78 991</td><td>N. Severijns, M. Beck, O. Navilat-Cuncic</td><td>(LEUV+)</td></tr><tr><td>KREUZ</td><td>PL B619 263</td><td>M. Kreuz et al.</td><td>(HEID, ILLG, MAINZ, KARL+)</td></tr><tr><td>MOHR</td><td>RMP 77 1</td><td>P.J. Mohr, B.N. Taylor</td><td>(NIST)</td></tr><tr><td>NICO</td><td>PR C71 055502</td><td>J.S. Nico et al.</td><td>(NIST, TULN, IND, TENN+)</td></tr><tr><td>SCHUMACHER</td><td>PPNP 55 567</td><td>M. Schumacher</td><td>(GOET)</td></tr><tr><td>SEREBROV</td><td>PL B605 72</td><td>A.P. Serebrov et al.</td><td>(PNPI, JINR, ILLG)</td></tr><tr><td>Also</td><td>SPU 48 867</td><td>A.P. Serebrov et al.</td><td>(PPNI, JINR, ILLG)</td></tr><tr><td></td><td></td><td>Translated from UFEAN 175 905.</td><td></td></tr></tbody></table>
<table><tbody><tr><td>WIETFEELDT</td><td>05</td><td>MPL A20 1783</td><td>F. Wistfeldt</td><td>(TULN)</td></tr><tr><td>SOLDNER</td><td>04</td><td>PL B581 49</td><td>T. Soldner et al.</td><td>(ILLG, TUM)</td></tr><tr><td>DEWEY</td><td>03</td><td>PRL 91 152302</td><td>M.S. Dewey et al.</td><td>(NIST, TULN, IND+)</td></tr><tr><td>KOSSERT</td><td>03</td><td>EPJ A16 259</td><td>K. Kossert et al.</td><td>(Mainz MAMI Collab.)</td></tr><tr><td>Also</td><td>03</td><td>PRL 88 162301</td><td>K. Kossert et al.</td><td>(Mainz MAMI Collab.)</td></tr><tr><td>LUNDIN</td><td>02</td><td>PRL 90 192501</td><td>M. Lundin et al.</td><td></td></tr><tr><td>ABELLE</td><td>02</td><td>PRL 88 211801</td><td>H. Abele et al.</td><td></td></tr><tr><td>BECK</td><td>02</td><td>JETP 76 332</td><td>M. Beck et al.</td><td>(PERKEO-II Collab.)</td></tr><tr><td>Byrne</td><td>02</td><td>JP G28 1325</td><td>J. Byrne et al.</td><td>(LEUV, SUSS, KIAE, PNI)</td></tr><tr><td>CHUNG</td><td>02B</td><td>PRL D66 032004</td><td>J. Chung et al.</td><td></td></tr><tr><td>Mostovoi</td><td>01</td><td>PAN 64 1955</td><td>A. Mostovoi et al.</td><td></td></tr><tr><td>ARZUMANOV</td><td>00</td><td>PL B483 15</td><td>S. Arzumanov et al.</td><td></td></tr><tr><td>GAL</td><td>00</td><td>PRL C61 08201</td><td>A. Gal</td><td></td></tr><tr><td>KOLB</td><td>00</td><td>PL 85 1388</td><td>N.R. Kolb et al.</td><td></td></tr><tr><td>LOMOREAUX</td><td>00</td><td>PRL D61 051301</td><td>S. Lamoreaux, R. Golub</td><td></td></tr><tr><td>LEVCHUK</td><td>00</td><td>NP A674 449</td><td>M.I. Levchuk, A.I. L'vov</td><td>(BELA, LEBD)</td></tr><tr><td>LISING</td><td>00</td><td>PRL C62 055501</td><td>L.J. Lising et al.</td><td>(NIST emiT Collab.)</td></tr><tr><td>HARRIS</td><td>99</td><td>PRL 82 904</td><td>P.G. Harris et al.</td><td></td></tr><tr><td>KESSLER</td><td>99</td><td>PL A255 221</td><td>E.G. Kessler Jr. et al.</td><td></td></tr><tr><td>MOHR</td><td>99</td><td>PRL D52 1713</td><td>P.J. Mohr, B.N. Taylor</td><td>(NIST)</td></tr><tr><td>Also</td><td>03</td><td>RMP 72 351</td><td>P.J. Mohr, B.N. Taylor</td><td>(NIST)</td></tr><tr><td>SEREBROV</td><td>98</td><td>JETP 86 1074</td><td>A.P. Serebrov et al.</td><td></td></tr><tr><td>ABELE</td><td>97D</td><td>PL ZETF 113 1963</td><td></td><td></td></tr><tr><td>KOPECKY</td><td>97</td><td>PL B407 212</td><td>H. Abele et al.</td><td>(HEIDP, ILLG)</td></tr><tr><td>LIAUD</td><td>97</td><td>PRL C56 2229</td><td>S. Kopecky et al.</td><td></td></tr><tr><td>YEROZILIM...</td><td>97</td><td>NP A612 53</td><td>P. Llaud et al.</td><td>(ILLG, LAPP)</td></tr><tr><td>ALTAREV</td><td>96</td><td>PL B412 240</td><td>B.G. Erozolimsky et al.</td><td>(HARV, PNI, KIAE)</td></tr><tr><td>Also</td><td>96</td><td>PAN 59 1152</td><td>I.S. Altarev et al.</td><td>(PNI)</td></tr><tr><td>BONDAREN...</td><td>96</td><td>Transl. from YAF 59 1204.</td><td></td><td></td></tr><tr><td>Byrne</td><td>96</td><td>JETP 64 416</td><td>L.N. Bondarenko et al.</td><td>(KIAE)</td></tr><tr><td>Mostovoi</td><td>96</td><td>EPL 33 187</td><td>J. Byrne et al.</td><td></td></tr><tr><td>Byrne</td><td>96</td><td>PAN 59 968</td><td>Y.A. Mostovoy</td><td></td></tr><tr><td>IGNATOVICH</td><td>96</td><td>Transl. from YAF 59 1013.</td><td></td><td></td></tr><tr><td>NORMAN</td><td>95</td><td>PR D53 4086</td><td>E.B. Norman, J.N. Bahcall, M. Goldhaber</td><td>(LBL+)</td></tr><tr><td>Also</td><td>95</td><td>JETP 62 1</td><td>V.K. Ignatovich</td><td>(JINR)</td></tr><tr><td>KOESTER</td><td>95</td><td>Transl. from ZETF 62 3.</td><td>L. Koester et al.</td><td>(TUM, JINR, LATV)</td></tr><tr><td>KOPECKY</td><td>95</td><td>PRL 74 2427</td><td>S. Kopecky et al.</td><td></td></tr><tr><td>KUZNETSOV</td><td>95</td><td>PL 75 794</td><td>I.A. Kuznetsov et al.</td><td>(PNI, KIAE, HARY+)</td></tr><tr><td>SCHRECK...</td><td>95</td><td>PL B349 427</td><td>K. Schreckenbach et al.</td><td>(TUM, ILLG, LAPP)</td></tr><tr><td>BALDO...</td><td>94</td><td>ZPHY C63 409</td><td>M. Baldo-Ceolin et al.</td><td>(HEID, ILLG, PADO+)</td></tr><tr><td>DIFILIPPPO</td><td>94</td><td>PRL 73 1481</td><td>F. DiFilippo et al.</td><td>(IMD)</td></tr><tr><td>Also</td><td>94</td><td>PRL 71 1998</td><td>V. Natarajan et al.</td><td>(MIT)</td></tr><tr><td>GOLUB</td><td>94</td><td>PRPL 237C 1</td><td>R. Golub, K. Lamoreaux</td><td>(HAHN, WASH)</td></tr><tr><td>MAMPE</td><td>93</td><td>JETP 57 82</td><td>B. Mampe et al.</td><td>(KIAE)</td></tr><tr><td>ALTAREV</td><td>92</td><td>Transl. from ZETF 57 77.</td><td></td><td></td></tr><tr><td>ALTAREV</td><td>92</td><td>PL B276 242</td><td>I.S. Altarev et al.</td><td>(PNI)</td></tr><tr><td>ALTZVHEV...</td><td>92</td><td>JETP 75 405</td><td>V.Y. Nesvizhsky et al.</td><td>(PNI, JINR)</td></tr><tr><td>ALBERICO</td><td>91</td><td>NP A523 488</td><td>W.M. Alberico, A. de Pace, M. Pignone</td><td>(TORI)</td></tr><tr><td>DUBBERS</td><td>91</td><td>NP A527 239c</td><td>D. Dubbers</td><td>(ILLG)</td></tr><tr><td>Also</td><td>91</td><td>EPL 11 195</td><td>D. Dubbers, W. Mampe, J. Dohner</td><td>(ILLG, HEID)</td></tr><tr><td>EROZOLIM...</td><td>91</td><td>PL B236 33</td><td>B.G. Erozolimsky et al.</td><td>(PNI, KIAE)</td></tr><tr><td>Also</td><td>91</td><td>SJPN 52 999</td><td>B.G. Erozolimsky et al.</td><td>(PNI, KIAE)</td></tr><tr><td>EROZOLIM...</td><td>91B</td><td>SJPN 53 260</td><td>B.G. Erozolimsky, Y.A. Mostovoy</td><td>(KIAE)</td></tr><tr><td>SCHMIEDM...</td><td>91</td><td>PRL 66 1015</td><td>J. Schmiedmayer et al.</td><td>(TUW, ORNL)</td></tr><tr><td>WOOLCOCK</td><td>91</td><td>MPL A6 2579</td><td>W.S. Woolcock</td><td>(CABN)</td></tr><tr><td>ALFIMENKOV</td><td>90</td><td>JETP 52 373</td><td>J. Aifimenkov et al.</td><td>(PNI, JINR)</td></tr><tr><td>BALDO...</td><td>90</td><td>PL B236 95</td><td>M. Baldo-Ceolin et al.</td><td>(PADO, PAVI, HEIDP+)</td></tr><tr><td>BERGER</td><td>90</td><td>PL B240 237</td><td>C. Berger et al.</td><td>(FREJUS Collab.)</td></tr><tr><td>BRESSI</td><td>90</td><td>NC 103A 731</td><td>G. Bressi et al.</td><td>(PAVI, ROMA, MILA)</td></tr><tr><td>BURNE</td><td>90</td><td>JP 65 289</td><td>J. Burne et al.</td><td>(SUSS, NBS, SCOT, CBNM)</td></tr><tr><td>GREEN</td><td>90</td><td>JP G16 L75</td><td>K. Green, D. Thompson</td><td>(RAL)</td></tr><tr><td>RAMSEY</td><td>90</td><td>ARNPS 40 1</td><td>N.F. Ramsey</td><td>(HARV)</td></tr><tr><td>ROSE</td><td>90</td><td>PL B234 460</td><td>K.W. Rose et al.</td><td>(GOET, MPCM, MAINZ)</td></tr><tr><td>ROSE</td><td>90B</td><td>NP A514 621</td><td>K.W. Rose et al.</td><td>(GOET, MPCM)</td></tr><tr><td>SMITH</td><td>90B</td><td>NP B234 191</td><td>K.F. Smith et al.</td><td>(SUSS, RAL, HARY+)</td></tr><tr><td>BRESSI</td><td>89</td><td>ZPHY C43 175</td><td>B.G. Bressi et al.</td><td>(INFN, MILA, PAVI, ROMA)</td></tr><tr><td>DOVER</td><td>89</td><td>NIM A284 13</td><td>C.B. Dover, A. Gal, J.M. Richard</td><td>(BNL, HEBR+)</td></tr><tr><td>KOSSAKOW...</td><td>89</td><td>NP A503 473</td><td>R. Kossakowski et al.</td><td>(LAPP, SAVO, ISNG+)</td></tr><tr><td>MAMPE</td><td>89</td><td>PRL 63 593</td><td>W. Mampe et al.</td><td>(ILLG, RISL, SUSS, URI)</td></tr><tr><td>MOHAPATRA</td><td>89</td><td>NP A284 1</td><td>R.N. Mohapatra</td><td>(IMD)</td></tr><tr><td>PAUL</td><td>89</td><td>ZPHY C45 25</td><td>W. Paul et al.</td><td>(BONN, WUPP, MPIK, ILLG)</td></tr><tr><td>SCHMIEDM...</td><td>89</td><td>NIM A284 137</td><td>J. Schmiedmayer, H. Rauch, P. Riehs</td><td>(WIEN)</td></tr><tr><td>BAUMANN</td><td>88</td><td>PR D37 3107</td><td>J. Baumann et al.</td><td>(BAYR, MUNI, ILLG)</td></tr><tr><td>KOESTER</td><td>88</td><td>ZPHY A329 229</td><td>L. Koester, W. Waschkowski, J. Meier</td><td>(MUNI, TUM)</td></tr><tr><td>LAST</td><td>88</td><td>PRL 60 995</td><td>I. Last et al.</td><td>(HEIDP, ILLG, ANL)</td></tr><tr><td>SCHMIEDM...</td><td>88</td><td>PRL 61 1065</td><td>J. Schmiedmayer, H. Rauch, P. Riehs</td><td>(TUW)</td></tr><tr><td>Also</td><td>88</td><td>PRL 61 2509 (errat.)</td><td>J. Schmiedmayer, H. Rauch, P. Riehs</td><td>(TUW)</td></tr><tr><td>SPIVAK</td><td>88</td><td>PRL 67 1735</td><td>P.E. Spivak</td><td>(KIAE)</td></tr><tr><td>COHEN</td><td>87</td><td>Transl. from ZETF 94 1.</td><td></td><td></td></tr><tr><td>COHEN</td><td>87</td><td>RMP 59 1121</td><td>E.R. Cohen, B.N. Taylor</td><td>(RISC, NBS)</td></tr><tr><td>ALEKSANDR...</td><td>86</td><td>SJPN 44 900</td><td>Yu.A. Aleksandrov et al.</td><td></td></tr><tr><td>ALTAREV</td><td>86</td><td>JETPL 44 460</td><td>I.S. Altarev et al.</td><td>(PNI)</td></tr><tr><td>BOPP</td><td>86</td><td>Transl. from ZETF 44 360</td><td>P. Bopp et al.</td><td>(HEIDP, ANL, ILLG)</td></tr><tr><td>Also</td><td>86</td><td>ZPHY C37 179</td><td>E. Klemp et al.</td><td>(HEIDP, ANL, ILLG)</td></tr><tr><td>CRESTI</td><td>86</td><td>PL B177 206</td><td>M. Cresti et al.</td><td>(PADO)</td></tr><tr><td>Also</td><td>86</td><td>PRL B200 587 (errat.)</td><td>M. Cresti et al.</td><td>(PADO)</td></tr><tr><td>GREENE</td><td>86</td><td>PRL 56 819</td><td>G.L. Greene et al.</td><td>(NBS, ILLG)</td></tr><tr><td>KOESTER</td><td>86</td><td>Physica B137 282</td><td>L. Koester et al.</td><td></td></tr><tr><td>KOSVINTSEV</td><td>86</td><td>JETPL 44 571</td><td>Y.Y. Kosvintsev, V.I. Morozov, G.I. Terekhov</td><td>(KIAE)</td></tr><tr><td>TAKITA</td><td>86</td><td>Transl. from ZETF 44 444.</td><td></td><td></td></tr><tr><td>DOVER</td><td>86</td><td>PL D34 902</td><td>M. Takita et al.</td><td>(KEK, TOKY+)</td></tr><tr><td>85</td><td>PL C31 1423</td><td>C.B. Dover, A. Gal, J.M. Richard</td><td>(BNL)</td></tr><tr><td>FIDECARO</td><td>85</td><td>PL 156B 122</td><td>G. Fidecaro et al.</td><td>(CERN, ILLG, PADO+)</td></tr><tr><td>PARK</td><td>85B</td><td>NP B252 261</td><td>H.S. Park et al.</td><td>(IMB Collab.)</td></tr><tr><td>BATTISTONI</td><td>84</td><td>PL 133B 454</td><td>G. Battistoni et al.</td><td>(NUSEX Collab.)</td></tr><tr><td>JONES</td><td>84</td><td>PL 52 720</td><td>T.W. Jones et al.</td><td>(IMB Collab.)</td></tr><tr><td>PENDLEBURY</td><td>84</td><td>PL 136B 327</td><td>J.M. Pendlebury et al.</td><td>(SUSS, HARY, RAL+, PADD+)</td></tr><tr><td>CHERRY</td><td>83</td><td>PL 50 1354</td><td>M. Cherry et al.</td><td>(PENN, BNL)</td></tr><tr><td>DOVER</td><td>83</td><td>PRL D27 1090</td><td>C.B. Dover, A. Gal, J.M. Richard</td><td>(BNL)</td></tr><tr><td>KABIR</td><td>83</td><td>PRL 51 231</td><td>P.K. Kabir</td><td>(HARV)</td></tr><tr><td>Mostovoi</td><td>83</td><td>JETP 37 196</td><td>Y.A. Mostovoy</td><td>(KIAE)</td></tr><tr><td>Byrne</td><td>80</td><td>Transl. from ZETF 37 162.</td><td></td><td></td></tr><tr><td>Byrne</td><td>80</td><td>PL 92B 274</td><td>A. Roy et al.</td><td>(TATA)</td></tr><tr><td>VAIDYA</td><td>83</td><td>PRL D28 1770</td><td></td><td>(TATA)</td></tr><tr><td>GAEHLER</td><td>82</td><td>PRL D27 486</td><td>S.C. Vaidya et al.</td><td>(TATA)</td></tr><tr><td>GREENE</td><td>82</td><td>PRL D25 2887</td><td>R. Gahler, J. Kalus, W. Mampe</td><td>(BAYR, ILLG)</td></tr><tr><td>ALTAREV</td><td>81</td><td>Metrolgia 18 93</td><td>G.L. Greene et al.</td><td>(YALE, HARY, ILLG+)</td></tr><tr><td>ALTAREV</td><td>81</td><td>PL 102B 13</td><td>I.S. Altarev et al.</td><td>(PNI)</td></tr><tr><td>BARABANOV</td><td>80</td><td>JETPL 32 359</td><td>J. Barabanov et al.</td><td>(PNI)</td></tr><tr><td>Byrne</td><td>80</td><td>Transl. from ZETF 32 384.</td><td></td><td></td></tr><tr><td>Byrne</td><td>80</td><td>PL 92B 274</td><td>J. Byrne et al.</td><td>(SUSS, RL)</td></tr><tr><td>KOSVINTSEV</td><td>80</td><td>JETPL 31 236</td><td>Y.Y. Kosvintsev et al.</td><td>(JINR)</td></tr><tr><td>MOHAPATRA</td><td>80</td><td>Transl. from ZETF 31 162.</td><td>R.N. Mohapatra, R.E. Marshak</td><td>(CUNY, VPI)</td></tr><tr><td>ALTAREV</td><td>79</td><td>JETP 29 730</td><td>I.S. Altarev et al.</td><td>(PNI)</td></tr><tr><td>ALTAREV</td><td>79</td><td>Transl. from ZETF 29 794.</td><td></td><td></td></tr></tbody></table>

<table><tbody><tr><td>EROZOLIM...</td><td>79</td><td>SJNP 30 356</td><td>B.G. Erozolimsky et al.</td><td>(KIAE)</td></tr><tr><td>NORMAN</td><td>79</td><td>PRL 43 1226</td><td>E.B. Norman, A.G. Seamster</td><td>(WASH)</td></tr><tr><td>BONDAREN...</td><td>78</td><td>JETPL 28 303</td><td>L.N. Bondarenko et al.</td><td>(KIAE)</td></tr><tr><td>Also</td><td>78</td><td>Translated from ZETF 28 328.</td><td>Solmenic Conf.</td><td>(KIAE)</td></tr><tr><td>EROZOLIM...</td><td>78</td><td>SJNP 28 48</td><td>B.G. Erozolimsky et al.</td><td>(KIAE)</td></tr><tr><td>STRATOWA</td><td>78</td><td>PR D18 3970</td><td>C. Stratowa, R. Dobrozemsky, P. Weinzler</td><td>(SEIB)</td></tr><tr><td>EROZOLIM...</td><td>77</td><td>JETPL 23 663</td><td>B.G. Erozolimsky et al.</td><td>(KIAE)</td></tr><tr><td>KOESTER</td><td>76</td><td>PRL 36 1021</td><td>L. Koester et al.</td><td></td></tr><tr><td>STEINBERG</td><td>76</td><td>PR D13 2469</td><td>R.J. Steinberg et al.</td><td>(YALE, ISNG)</td></tr><tr><td>DOBROZEW...</td><td>75</td><td>PR D11 510</td><td>R. Dobrozemsky et al.</td><td>(SEIB)</td></tr><tr><td>KROHN</td><td>75</td><td>PL 55B 175</td><td>V.E. Krohn, G.R. Ringo</td><td>(ANL)</td></tr><tr><td>EROZOLIM...</td><td>74</td><td>JETPL 20 345</td><td>B.G. Erozolimsky et al.</td><td></td></tr><tr><td>KROPF</td><td>74</td><td>ZPHY 267 129</td><td>H. Kropf, E. Paul</td><td>(LINZ)</td></tr><tr><td>Also</td><td>74</td><td>NP A154 160</td><td>H. Paul</td><td>(VIEN)</td></tr><tr><td>STEINBERG</td><td>74</td><td>PRL 33 41</td><td>R.J. Steinberg et al.</td><td>(YALE, ISNG)</td></tr><tr><td>COHEN</td><td>73</td><td>JPCRD 2 664</td><td>E.R. Cohen, B.N. Taylor</td><td>(RISC, NBS)</td></tr><tr><td>KROHN</td><td>73</td><td>PR D8 1305</td><td>V.E. Krohn, G.R. Ringo</td><td></td></tr><tr><td>CHRISTENSEN</td><td>72</td><td>PR D5 1628</td><td>C.J. Christensen et al.</td><td>(RISO)</td></tr><tr><td>CHRISTENSEN</td><td>70</td><td>PR C1 1693</td><td>C.J. Christensen, V.E. Krohn, G.R. Ringo</td><td>(ANL)</td></tr><tr><td>EROZOLIM...</td><td>70C</td><td>PL 33B 351</td><td>B.G. Erozolimsky et al.</td><td>(KIAE)</td></tr><tr><td>GRIGOREV</td><td>68</td><td>SJNP 26 239</td><td>V.K. Grigoriev et al.</td><td>(ITEP)</td></tr><tr><td>KROHN</td><td>66</td><td>Translated from YAF 6 329.</td><td>V.E. Krohn, G.R. Ringo</td><td></td></tr><tr><td>LEE</td><td>56</td><td>PR 148 1303</td><td>T.D. Lee, C.N. Yang</td><td>(COLU, BNL)</td></tr></tbody></table>

See the related review(s):

N and Δ Resonances

$$N(1440) \frac{1}{2}^+$$

$$I(J^P) = \frac{1}{2}(\frac{1}{2}^+) \text{ Status: } \cdots\cdots$$

Older and obsolete values are listed and referenced in the 2014 edition, Chinese Physics C38 070001 (2014).

## N(1440) POLE POSITION

### REAL PART

VALUE (MeV) DOCUMENT ID TECN COMMENT

### 1360 to 1380 (≈ 1370) OUR ESTIMATE

<table><tbody><tr><td>1353 ± 1</td><td>ROENCHEN</td><td>22</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>1369 ± 3</td><td>SOKHOYAN</td><td>15A</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>1363 ± 2 ± 2</td><td><sup>1</sup>SVARC</td><td>14</td><td>L+P</td><td>πN → πN</td></tr><tr><td>1375 ± 30</td><td>CUTKOSKY</td><td>80</td><td>IPWA</td><td>πN → πN</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tbody><tr><td>1360</td><td>HUNT</td><td>19</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>1355</td><td>ROENCHEN</td><td>15A</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>1386</td><td>SHKLYAR</td><td>13</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>1370 ± 4</td><td>ANISOVICH</td><td>12A</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>1363 ± 11</td><td>BATINIC</td><td>10</td><td>DPWA</td><td>πN → Nπ, Nη</td></tr><tr><td>1359</td><td>ARNDT</td><td>06</td><td>DPWA</td><td>πN → πN</td></tr><tr><td>1383</td><td>VRANA</td><td>00</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>1385</td><td>HOEHLER</td><td>93</td><td>SPED</td><td>πN → πN</td></tr></tbody></table>

¹Fit to the amplitudes of HOEHLER 79.

### -2x IMAGINARY PART

VALUE (MeV) DOCUMENT ID TECN COMMENT

### 180 to 205 (≈ 190) OUR ESTIMATE

<table><tbody><tr><td>203 ± 2</td><td>ROenchEN</td><td>22</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>189 ± 5</td><td>SOKHOYAN</td><td>15A</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>180 ± 4 ± 5</td><td><sup>1</sup>SVARC</td><td>14</td><td>L+P</td><td>πN → πN</td></tr><tr><td>180 ± 40</td><td>CUTKOSKY</td><td>80</td><td>IPWA</td><td>πN → πN</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

¹Fit to the amplitudes of HOEHLER 79.

## N(1440) ELASTIC POLE RESIDUE

### MODULUS |r|

VALUE (MeV) DOCUMENT ID TECN COMMENT

### 50 to 60 (≈ 55) OUR ESTIMATE

<table><tbody><tr><td>59 ± 1</td><td>ROenchEN</td><td>22</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>49 ± 3</td><td>SOKHOYAN</td><td>15A</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>50 ± 1 ± 2</td><td><sup>1</sup>SVARC</td><td>14</td><td>L+P</td><td>πN → πN</td></tr><tr><td>52 ± 5</td><td>CUTKOSKY</td><td>80</td><td>IPWA</td><td>πN → πN</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •
PHASE θ

<table><thead><tr><th>VALUE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4">-100 to -80 (≈ -90) OUR ESTIMATE</td></tr><tr><td>-104 ± 2</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>- 82 ± 5</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>- 88 ± 1 ± 2</td><td>1 SVARC</td><td>14</td><td>L+P πN → πN</td></tr><tr><td>-100 ± 35</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>- 98</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>- 60</td><td>SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>- 78 ± 4</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>- 88</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>- 98</td><td>ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr></tbody></table>

N(1440) INELASTIC POLE RESIDUE

The “normalized residue” is the residue divided by $Γ_{pole}/2$.

Normalized residue in $Nπ → N(1440) → Nη$

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.084 ± 0.002</td><td>-28 ± 2</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.078</td><td>-27</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

Normalized residue in $Nπ → N(1440) → Δπ, P-wave$

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.27 ± 0.02</td><td>38 ± 5</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.27 ± 0.02</td><td>40 ± 5</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr></tbody></table>

Normalized residue in $Nπ → N(1440) → ΛK$

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.025 ± 0.005</td><td>-92 ± 43</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.016</td><td>145</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

Normalized residue in $Nπ → N(1440) → ΣK$

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.002 ± 0.003</td><td>-32 ± 77</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.027</td><td>113</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

Normalized residue in $Nπ → N(1440) → N (ππ)_{5-wave}$

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.21 ± 0.04</td><td>-136 ± 4</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.21 ± 0.05</td><td>-135 ± 7</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr></tbody></table>

N(1440) BREIT-WIGNER MASS

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4">1410 to 1470 (≈ 1440) OUR ESTIMATE</td></tr><tr><td>1417 ± 4</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>1430 ± 10</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>1515 ± 15</td><td>1 SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>1485.0 ± 1.2</td><td>1 ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr><tr><td>1440 ± 30</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr><tr><td>1410 ± 12</td><td>HOEHLER</td><td>79</td><td>IPWA πN → πN</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>1430 ± 8</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>1412 ± 2</td><td>1 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>1439 ± 19</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>1518 ± 5</td><td>PENNER</td><td>02C</td><td>DPWA Multichannel</td></tr><tr><td>1479 ± 80</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr></tbody></table>

N(1440) BREIT-WIGNER WIDTH

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4">250 to 450 (≈ 350) OUR ESTIMATE</td></tr><tr><td>257 ± 11</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>360 ± 30</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>605 ± 90</td><td>1 SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>284 ± 18</td><td>1 ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr><tr><td>340 ± 70</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr><tr><td>135 ± 10</td><td>HOEHLER</td><td>79</td><td>IPWA πN → πN</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>365 ± 35</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>248 ± 5</td><td>1 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>437 ± 141</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>668 ± 41</td><td>PENNER</td><td>02C</td><td>DPWA Multichannel</td></tr><tr><td>490 ± 120</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr></tbody></table>

N(1440) DECAY MODES

The following branching fractions are our estimates, not fits or averages.

<table><thead><tr><th>Mode</th><th>Fraction (Γ<sub>f</sub>/Γ)</th></tr></thead><tbody><tr><td>Γ<sub>1</sub></td><td>55-75%</td></tr><tr><td>Γ<sub>2</sub></td><td>&lt;1%</td></tr><tr><td>Γ<sub>3</sub></td><td>17-50%</td></tr><tr><td>Γ<sub>4</sub></td><td>Δ(1232)π, P-wave</td><td>6-27%</td></tr><tr><td>Γ<sub>5</sub></td><td>Nσ</td><td>11-23%</td></tr><tr><td>Γ<sub>6</sub></td><td>pγ, helicity=1/2</td><td>0.035-0.048%</td></tr><tr><td>Γ<sub>7</sub></td><td>nγ, helicity=1/2</td><td>0.02-0.04%</td></tr></tbody></table>

N(1440) BRANCHING RATIOS

$Γ(Nπ)/Γ_{total}$

<table><thead><tr><th>VALUE (%)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>55 to 75 (≈ 65) OUR ESTIMATE</td><td></td><td></td><td></td></tr><tr><td>59 ± 2</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>63 ± 2</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>56 ± 2</td><td>1 SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>78.7 ± 1.6</td><td>1 ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr><tr><td>68 ± 4</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr><tr><td>51 ± 5</td><td>HOEHLER</td><td>79</td><td>IPWA πN → πN</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tbody><tr><td>62 ± 3</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>64.8 ± 0.9</td><td>1 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>62 ± 4</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>57 ± 1</td><td>PENNER</td><td>02C</td><td>DPWA Multichannel</td></tr><tr><td>72 ± 5</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr></tbody></table>

$Γ(Nη)/Γ_{total}$

<table><thead><tr><th>VALUE (%)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0 ± 1</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr></tbody></table>

$Γ(Δ(1232)π, P-wave)/Γ_{total}$

<table><thead><tr><th>VALUE (%)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>6 to 27 (≈ 15) OUR ESTIMATE</td><td></td><td></td><td></td></tr><tr><td>22 ± 4</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>12 ± 5</td><td>SHKLYAR</td><td>16</td><td>DPWA Multichannel</td></tr><tr><td>20 ± 7</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tbody><tr><td>21 ± 8</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>6.5 ± 0.8</td><td>1 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>16 ± 1</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr></tbody></table>

$Γ(Nσ)/Γ_{total}$

<table><thead><tr><th>VALUE (%)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>16 ± 3</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>27 ± 4</td><td>SHKLYAR</td><td>16</td><td>DPWA Multichannel</td></tr><tr><td>17 ± 6</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tbody><tr><td>17 ± 7</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>27 ± 1</td><td>1 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>12 ± 1</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr></tbody></table>

N(1440) PHOTON DECAY AMPLITUDES AT THE POLE

$N(1440) → pγ, helicity-1/2 amplitude A<sub>1/2</sub>$

<table><thead><tr><th>MODULUS (GeV<sup>-1/2</sup>)</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>-0.090 ± 0.007</td><td>-30 ± 3</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>-0.044 ± 0.005</td><td>-40 ± 8</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>-0.060</td><td>-23</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

$N(1440) → nγ, helicity-1/2 amplitude A<sub>1/2</sub>$

<table><thead><tr><th>MODULUS (GeV<sup>-1/2</sup>)</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.041 ± 0.005</td><td>23 ± 10</td><td>ANISOVICH</td><td>17E</td><td>DPWA Multichannel</td></tr></tbody></table>

N(1440) BREIT-WIGNER PHOTON DECAY AMPLITUDES

$N(1440) → pγ, helicity-1/2 amplitude A<sub>1/2</sub>$

<table><thead><tr><th>VALUE (GeV<sup>-1/2</sup>)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>-0.080 to -0.050 (≈ -0.065) OUR ESTIMATE</td><td></td><td></td><td></td></tr><tr><td>-0.091 ± 0.007</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr></tbody></table>

<footnote n="1">¹Fit to the amplitudes of HOEHLER 79.</footnote>

<footnote n="1">¹Statistical error only.</footnote>

<footnote n="1">¹Statistical error only.</footnote>

<footnote n="1">¹Statistical error only.</footnote>

<footnote n="1">¹Statistical error only.</footnote>

<footnote n="1">¹Statistical error only.</footnote>
<table><tr><td>-0.061 ± 0.006</td><td>SOKHOYAN</td><td>15A</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>-0.085 ± 0.003</td><td>SHKLYAR</td><td>13</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>-0.056 ± 0.001</td><td>WORKMAN</td><td>12A</td><td>DPWA</td><td>γN → Nπ</td></tr><tr><td>-0.051 ± 0.002</td><td>DUGGER</td><td>07</td><td>DPWA</td><td>γN → πN</td></tr></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>-0.061 ± 0.008</td><td>ANISOVICH</td><td>12A</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>-0.084 ± 0.003</td><td>SHRESTHA</td><td>12A</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>-0.061</td><td>DRECHSEL</td><td>07</td><td>DPWA</td><td>γN → πN</td></tr><tr><td>-0.087</td><td>PENNER</td><td>02D</td><td>DPWA</td><td>Multichannel</td></tr></table>

¹Statistical error only.

N(1440) → nγ, helicity-1/2 amplitude A₁/₂

<table><thead><tr><th>VALUE (GeV<sup>-1/2</sup>)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>0.035 to 0.055 (≈ 0.045) OUR ESTIMATE</strong></td></tr><tr><td>0.013 ± 0.012</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>0.053 ± 0.007</td><td>ANISOVICH</td><td>17E</td><td>DPWA Multichannel</td></tr><tr><td>0.048 ± 0.004</td><td>1 CHEN</td><td>12A</td><td>DPWA γN → πN</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.043 ± 0.012</td><td>ANISOVICH</td><td>13B</td><td>DPWA Multichannel</td></tr><tr><td>0.040 ± 0.005</td><td>SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>0.054</td><td>DRECHSEL</td><td>07</td><td>DPWA γN → πN</td></tr><tr><td>0.121</td><td>PENNER</td><td>02D</td><td>DPWA Multichannel</td></tr></tbody></table>

¹Statistical error only.

N(1440) REFERENCES

For early references, see Physics Letters **111B** 1 (1982).

<table><tr><td>ROENCHEN</td><td>22</td><td>EPJ A58 229</td><td>D. Roenchen et al.</td><td>(JULI, GWU, BONN+)</td></tr><tr><td>HUNT</td><td>19</td><td>PR C99 055205</td><td>B.C. Hunt, D.M. Manley</td><td></td></tr><tr><td>ANISOVICH</td><td>17E</td><td>PR C96 055202</td><td>A.V. Anisovich et al.</td><td>(BONN, PNPI, JLAB+)</td></tr><tr><td>SHKLYAR</td><td>16</td><td>PR C93 045206</td><td>V. Shklyar, H. Lenske, U. Mosel</td><td>(GIES)</td></tr><tr><td>ROENCHEN</td><td>15A</td><td>EPJ A51 70</td><td>D. Roenchen et al.</td><td></td></tr><tr><td>SOKHOYAN</td><td>15A</td><td>EPJ A51 95</td><td>V. Sokhoyan et al.</td><td>(CBELSA/TAPS Collab.)</td></tr><tr><td>PDG</td><td>14</td><td>CP C38 070001</td><td>K. Olive et al.</td><td>(PDG Collab.)</td></tr><tr><td>SVARC</td><td>14</td><td>PR C89 045205</td><td>A. Svarc et al.</td><td>(RBI Zagreb, UNI Tuzla)</td></tr><tr><td>ANISOVICH</td><td>13B</td><td>EPJ A49 67</td><td>A.V. Anisovich et al.</td><td></td></tr><tr><td>SHKLYAR</td><td>13</td><td>PR C07 015201</td><td>V. Shklyar, H. Lenske, U. Mosel</td><td>(GIES)</td></tr><tr><td>ANISOVICH</td><td>12A</td><td>EPJ A48 15</td><td>A.V. Anisovich et al.</td><td>(BONN, PNPI)</td></tr><tr><td>CHEN</td><td>12A</td><td>PR C86 015206</td><td>W. Chen et al.</td><td>(DUKE, GWU, MSST, ITEP+)</td></tr><tr><td>SHRESTHA</td><td>12A</td><td>PR C86 055203</td><td>M. Shrestha, D.M. Manley</td><td>(KSU)</td></tr><tr><td>WORKMAN</td><td>12A</td><td>PR C86 015202</td><td>R. Workman et al.</td><td>(GWU)</td></tr><tr><td>BATINIC</td><td>10</td><td>PR C02 038203</td><td>M. Batinic et al.</td><td>(ZAGR)</td></tr><tr><td>DRECHSEL</td><td>07</td><td>EPJ A34 69</td><td>D. Dreschel, S.S. Kamalov, L. Tiator</td><td>(MAINZ, JINR)</td></tr><tr><td>DUGGER</td><td>07</td><td>PR C76 025211</td><td>M. Dugger et al.</td><td>(JLab CLAS Collab.)</td></tr><tr><td>ARNDT</td><td>06</td><td>PR C74 045205</td><td>R.A. Arndt et al.</td><td>(GWU)</td></tr><tr><td>PENNER</td><td>02C</td><td>PR C66 055211</td><td>G. Penner, U. Mosel</td><td>(GIES)</td></tr><tr><td>PENNER</td><td>02D</td><td>PR C66 055212</td><td>G. Penner, U. Mosel</td><td>(GIES)</td></tr><tr><td>VRANA</td><td>00</td><td>PRPL 328 181</td><td>T.P. Vrana, S.A. Dytm, T.-S.H. Lee</td><td>(PITT, ANL)</td></tr><tr><td>HOEHLER</td><td>93</td><td>πN Newsletter 9 1</td><td>G. Hohler</td><td>(KARL)</td></tr><tr><td>CUTKOSKY</td><td>80</td><td>Toronto Conf. 19</td><td>R.E. Cutkosky et al.</td><td>(CMU, LBL) IJP</td></tr><tr><td>Also</td><td></td><td>PR D20 2839</td><td>R.E. Cutkosky et al.</td><td>(CMU, LBL) IJP</td></tr><tr><td>HOEHLER</td><td>79</td><td>PDAT 12-1</td><td>G. Hohler et al.</td><td>(KARLT) IJP</td></tr><tr><td>Also</td><td></td><td>Toronto Conf. 3</td><td>R. Koch</td><td>(KARLT) IJP</td></tr></table>

$$N(1520) 3/2^{-}$$

$$I(J^{P}) = \frac{1}{2}(\frac{3}{2}^{-}) \text{ Status: ****}$$

Older and obsolete values are listed and referenced in the 2014 edition, Chinese Physics **C38** 070001 (2014).

N(1520) POLE POSITION

REAL PART

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>1505 to 1515 (≈ 1510) OUR ESTIMATE</strong></td></tr><tr><td>1482 ± 3</td><td>ROENCHEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>1507 ± 2</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>1506 ± 1 ± 1</td><td>1 SVARC</td><td>14</td><td>L+P πN → πN</td></tr><tr><td>1510 ± 5</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>1500</td><td>HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>1512</td><td>ROENCHEN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>1492</td><td>SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>1507 ± 3</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>1506 ± 9</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>1515</td><td>ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr><tr><td>1504</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr><tr><td>1510</td><td>HOEHLER</td><td>93</td><td>ARGD πN → πN</td></tr></tbody></table>

¹Fit to the amplitudes of HOEHLER 79.

-2×IMAGINARY PART

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>105 to 120 (≈ 110) OUR ESTIMATE</strong></td></tr><tr><td>126 ± 9</td><td>ROENCHEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>111 ± 3</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>115 ± 2 ± 1</td><td>1 SVARC</td><td>14</td><td>L+P πN → πN</td></tr><tr><td>114 ± 10</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>117</td><td>HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>89</td><td>ROENCHEN</td><td>15A</td><td>DPWA Multichannel</td></tr></table>

<table><tr><td>94</td><td>SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>111 ± 5</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>122 ± 9</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>113</td><td>ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr><tr><td>112</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr><tr><td>120</td><td>HOEHLER</td><td>93</td><td>ARGD πN → πN</td></tr></table>

¹Fit to the amplitudes of HOEHLER 79.

N(1520) ELASTIC POLE RESIDUE

MODULUS |r|

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>32 to 38 (≈ 35) OUR ESTIMATE</strong></td></tr><tr><td>27 ± 11</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>36 ± 2</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>33 ± 1 ± 1</td><td>1 SVARC</td><td>14</td><td>L+P πN → πN</td></tr><tr><td>35 ± 2</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>37</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>27</td><td>SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>36 ± 3</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>35</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>38</td><td>ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr><tr><td>32</td><td>HOEHLER</td><td>93</td><td>ARGD πN → πN</td></tr></tbody></table>

¹Fit to the amplitudes of HOEHLER 79.

PHASE θ

<table><thead><tr><th>VALUE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>-15 to -5 (≈ -10) OUR ESTIMATE</strong></td></tr><tr><td>-36 ± 24</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>-14 ± 3</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>-15 ± 1 ± 1</td><td>1 SVARC</td><td>14</td><td>L+P πN → πN</td></tr><tr><td>-12 ± 5</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>-6</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>-35</td><td>SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>-14 ± 3</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>-7</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>-5</td><td>ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr><tr><td>-8</td><td>HOEHLER</td><td>93</td><td>ARGD πN → πN</td></tr></tbody></table>

¹Fit to the amplitudes of HOEHLER 79.

N(1520) INELASTIC POLE RESIDUE

The "normalized residue" is the residue divided by $Γ_{pole}/2$.

Normalized residue in $Nπ → N(1520) → Δπ, S-wave

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.33 ± 0.04</td><td>155 ± 15</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.33 ± 0.05</td><td>150 ± 20</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr></tbody></table>

Normalized residue in $Nπ → N(1520) → Δπ, D-wave

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.25 ± 0.03</td><td>105 ± 18</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.25 ± 0.03</td><td>100 ± 20</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr></tbody></table>

Normalized residue in $Nπ → N(1520) → Nη$

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.021 ± 0.009</td><td>34 ± 27</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.026</td><td>95</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

Normalized residue in $Nπ → N(1520) → ΛK$

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.026 ± 0.010</td><td>127 ± 24</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.069</td><td>158</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

Normalized residue in $Nπ → N(1520) → ΣK$

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.010 ± 0.006</td><td>94 ± 34</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.049</td><td>-41</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

Normalized residue in $Nπ → N(1520) → Nσ$

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.08 ± 0.03</td><td>-45 ± 25</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>
## N(1520) BREIT-WIGNER MASS

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>1510 to 1520 (≈ 1515) OUR ESTIMATE</strong></td></tr><tr><td>1512.0 ± 1.5</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>1516 ± 2</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>1505 ± 4</td><td>1 SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>1514.5 ± 0.2</td><td>1 ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr><tr><td>1525 ± 10</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr><tr><td>1519 ± 4</td><td>HOEHLER</td><td>79</td><td>IPWA πN → πN</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>1517 ± 3</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>1512.6 ± 0.5</td><td>1 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>1522 ± 8</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>1509 ± 1</td><td>PENNER</td><td>02C</td><td>DPWA Multichannel</td></tr><tr><td>1518 ± 3</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr></tbody></table>

¹Statistical error only.

## N(1520) BREIT-WIGNER WIDTH

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>100 to 120 (≈ 110) OUR ESTIMATE</strong></td></tr><tr><td>121 ± 3</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>113 ± 4</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>100 ± 2</td><td>1 SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>103.6 ± 0.4</td><td>1 ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr><tr><td>120 ± 15</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr><tr><td>114 ± 7</td><td>HOEHLER</td><td>79</td><td>IPWA πN → πN</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>114 ± 5</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>117 ± 1</td><td>1 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>132 ± 11</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>100 ± 2</td><td>PENNER</td><td>02C</td><td>DPWA Multichannel</td></tr><tr><td>124 ± 4</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr></tbody></table>

¹Statistical error only.

## N(1520) DECAY MODES

The following branching fractions are our estimates, not fits or averages.

<table><thead><tr><th>Mode</th><th>Fraction (Γ<sub>j</sub>/Γ)</th></tr></thead><tbody><tr><td>Γ<sub>1</sub> Nπ</td><td>55–65 %</td></tr><tr><td>Γ<sub>2</sub> Nη</td><td>0.07–0.09 %</td></tr><tr><td>Γ<sub>3</sub> Nππ</td><td>25–35 %</td></tr><tr><td>Γ<sub>4</sub> Δ(1232)π</td><td>22–34 %</td></tr><tr><td>Γ<sub>5</sub> Δ(1232)π, S-wave</td><td>15–23 %</td></tr><tr><td>Γ<sub>6</sub> Δ(1232)π, D-wave</td><td>7–11 %</td></tr><tr><td>Γ<sub>7</sub> Nρ</td><td>10–16 %</td></tr><tr><td>Γ<sub>8</sub> Nρ, S=3/2, S-wave</td><td>10–16 %</td></tr><tr><td>Γ<sub>9</sub> Nρ, S=1/2, D-wave</td><td>0.2–0.4 %</td></tr><tr><td>Γ<sub>10</sub> Nσ</td><td>&lt;10 %</td></tr><tr><td>Γ<sub>11</sub> pγ</td><td>0.31–0.52 %</td></tr><tr><td>Γ<sub>12</sub> pγ, helicity=1/2</td><td>0.01–0.02 %</td></tr><tr><td>Γ<sub>13</sub> pγ, helicity=3/2</td><td>0.30–0.50 %</td></tr><tr><td>Γ<sub>14</sub> nγ</td><td>0.30–0.53 %</td></tr><tr><td>Γ<sub>15</sub> nγ, helicity=1/2</td><td>0.04–0.10 %</td></tr><tr><td>Γ<sub>16</sub> nγ, helicity=3/2</td><td>0.25–0.45 %</td></tr></tbody></table>

## N(1520) BRANCHING RATIOS

<table><thead><tr><th>Γ(Nπ)/Γ<sub>total</sub></th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>55 to 65 (≈ 60) OUR ESTIMATE</strong></td></tr><tr><td>58.3 ± 1.5</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>61 ± 2</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>57 ± 2</td><td>1 SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>63.2 ± 0.1</td><td>1 ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr><tr><td>58 ± 3</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr><tr><td>54 ± 3</td><td>HOEHLER</td><td>79</td><td>IPWA πN → πN</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>62 ± 3</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>62.7 ± 0.5</td><td>1 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>55 ± 5</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>56 ± 1</td><td>PENNER</td><td>02C</td><td>DPWA Multichannel</td></tr><tr><td>63 ± 2</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr></tbody></table>

¹Statistical error only.

<table><thead><tr><th>Γ(Nη)/Γ<sub>total</sub></th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>Γ(Δ(1232)π, S-wave)/Γ<sub>total</sub></strong></td></tr><tr><td>&lt;0.1</td><td>MUELLER</td><td>20</td><td>DPWA Multichannel</td></tr><tr><td>0.03 ± 0.01</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>0.08 ± 0.01</td><td>TIATOR</td><td>99</td><td>DPWA γp → pη</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>&lt;1</td><td>SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>0.1 ± 0.1</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>0.2 ± 0.1</td><td>THOMA</td><td>08</td><td>DPWA Multichannel</td></tr><tr><td>0.08 to 0.12</td><td>ARNDT</td><td>05</td><td>DPWA Multichannel</td></tr><tr><td>0.23 ± 0.04</td><td>PENNER</td><td>02C</td><td>DPWA Multichannel</td></tr><tr><td>0 ± 1</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr><tr><td colspan="4">¹Statistical error only.</td></tr></tbody></table>

<table><thead><tr><th>Γ(Δ(1232)π, D-wave)/Γ<sub>total</sub></th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>12.1 ± 2.1</td><td>ADAMCZEW... 20</td><td>DPWA Multichannel</td><td></td></tr><tr><td>21 ± 2</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>19 ± 4</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>19 ± 4</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>9.3 ± 0.7</td><td>1 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>15 ± 2</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr><tr><td colspan="4">¹Statistical error only.</td></tr></tbody></table>

<table><thead><tr><th>Γ(Δ(1232)π, D-wave)/Γ<sub>total</sub></th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>6 ± 2</td><td>ADAMCZEW... 20</td><td>DPWA Multichannel</td><td></td></tr><tr><td>6 ± 1</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>9 ± 2</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>9 ± 2</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>6.3 ± 0.5</td><td>1 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>11 ± 2</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr><tr><td colspan="4">¹Statistical error only.</td></tr></tbody></table>

<table><thead><tr><th>Γ(Nρ, S=3/2, S-wave)/Γ<sub>total</sub></th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>10–16 % OUR EVALUATION</strong></td></tr><tr><td>11.8 ± 1.9</td><td>ADAMCZEW... 20</td><td>DPWA Multichannel</td><td></td></tr><tr><td>14.1 ± 1.5</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td colspan="4">¹Statistical error only</td></tr></tbody></table>

<table><thead><tr><th>Γ(Nρ, S=1/2, D-wave)/Γ<sub>total</sub></th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>0.2–0.4 % OUR EVALUATION</strong></td></tr><tr><td>0.4 ± 0.2</td><td>ADAMCZEW... 20</td><td>DPWA Multichannel</td><td></td></tr></tbody></table><table><thead><tr><th>Γ(Nσ)/Γ<sub>total</sub></th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>&lt;10 % OUR ESTIMATE</strong></td></tr><tr><td>7 ± 3</td><td>ADAMCZEW... 20</td><td>DPWA Multichannel</td><td></td></tr><tr><td>&lt;0.7</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>&lt;2</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>&lt;1</td><td>1 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>&lt;4</td><td>THOMA</td><td>08</td><td>DPWA Multichannel</td></tr><tr><td>1 ± 1</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr><tr><td colspan="4">¹Statistical error only.</td></tr></tbody></table>

## N(1520) PHOTON DECAY AMPLITUDES AT THE POLE

<table><thead><tr><th>N(1520) → pγ, helicity-1/2 amplitude A<sub>1/2</sub></th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>-0.043 ± 0.013</td><td>ROENCHEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>-0.023 ± 0.004</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>-0.031</td><td>ROENCHEN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

<table><thead><tr><th>N(1520) → pγ, helicity-3/2 amplitude A<sub>3/2</sub></th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.112 ± 0.032</td><td>ROENCHEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>0.131 ± 0.006</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.075</td><td>ROENCHEN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

<table><thead><tr><th>N(1520) → nγ, helicity-1/2 amplitude A<sub>1/2</sub></th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>-0.045 ± 0.005</td><td>ANISOVICH</td><td>17E</td><td>DPWA Multichannel</td></tr></tbody></table>
$N(1520) \rightarrow n\gamma$, helicity-3/2 amplitude $A_{3/2}$

<table><thead><tr><th>MODULUS (GeV<sup>-1/2</sup>)</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>-0.119 ± 0.005</td><td>5 ± 4</td><td>ANISOVICH</td><td>17E</td><td>DPWA Multichannel</td></tr></tbody></table>

$N(1520)$ BREIT-WIGNER PHOTON DECAY AMPLITUDES

$N(1520) \rightarrow p\gamma$, helicity-1/2 amplitude $A_{1/2}$

<table><thead><tr><th>VALUE (GeV<sup>-1/2</sup>)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>-0.030 to -0.015 (≈ -0.025) OUR ESTIMATE</strong></td></tr><tr><td>-0.034 ± 0.003</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>-0.024 ± 0.004</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>-0.015 ± 0.001</td><td>1 SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>-0.019 ± 0.002</td><td>1 WORKMAN</td><td>12A</td><td>DPWA γN → Nπ</td></tr><tr><td>-0.028 ± 0.002</td><td>1 DUGGER</td><td>07</td><td>DPWA γN → πN</td></tr><tr><td>-0.038 ± 0.003</td><td>1 AHRENS</td><td>02</td><td>DPWA γN → πN</td></tr><tr><td>-0.022 ± 0.004</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>-0.034 ± 0.001</td><td>SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>-0.027</td><td>DRECHSEL</td><td>07</td><td>DPWA γN → πN</td></tr><tr><td>-0.003</td><td>PENNER</td><td>02D</td><td>DPWA Multichannel</td></tr><tr><td>-0.052 ± 0.010 ± 0.007</td><td>1 MUKHOPAD...</td><td>98</td><td>γp → ηp</td></tr></tbody></table>

¹Statistical error only.

$N(1520) \rightarrow p\gamma$, helicity-3/2 amplitude $A_{3/2}$

<table><thead><tr><th>VALUE (GeV<sup>-1/2</sup>)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>0.135 to 0.145 (≈ 0.140) OUR ESTIMATE</strong></td></tr><tr><td>0.142 ± 0.003</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>0.130 ± 0.006</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>0.146 ± 0.001</td><td>1 SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>0.141 ± 0.002</td><td>1 WORKMAN</td><td>12A</td><td>DPWA γN → Nπ</td></tr><tr><td>0.143 ± 0.002</td><td>1 DUGGER</td><td>07</td><td>DPWA γN → πN</td></tr><tr><td>0.147 ± 0.010</td><td>1 AHRENS</td><td>02</td><td>DPWA γN → πN</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.131 ± 0.010</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>0.127 ± 0.003</td><td>SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>0.161</td><td>DRECHSEL</td><td>07</td><td>DPWA γN → πN</td></tr><tr><td>0.151</td><td>PENNER</td><td>02D</td><td>DPWA Multichannel</td></tr><tr><td>0.130 ± 0.020 ± 0.015</td><td>1 MUKHOPAD...</td><td>98</td><td>γp → ηp</td></tr></tbody></table>

¹Statistical error only.

$N(1520) \rightarrow n\gamma$, helicity-1/2 amplitude $A_{1/2}$

<table><thead><tr><th>VALUE (GeV<sup>-1/2</sup>)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>-0.055 to -0.040 (≈ -0.050) OUR ESTIMATE</strong></td></tr><tr><td>-0.072 ± 0.003</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>-0.046 ± 0.005</td><td>ANISOVICH</td><td>17E</td><td>DPWA Multichannel</td></tr><tr><td>-0.046 ± 0.006</td><td>1 CHEN</td><td>12A</td><td>DPWA γN → πN</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>-0.049 ± 0.008</td><td>ANISOVICH</td><td>13B</td><td>DPWA Multichannel</td></tr><tr><td>-0.038 ± 0.003</td><td>SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>-0.077</td><td>DRECHSEL</td><td>07</td><td>DPWA γN → πN</td></tr><tr><td>-0.084</td><td>PENNER</td><td>02D</td><td>DPWA Multichannel</td></tr></tbody></table>

¹Statistical error only.

$N(1520) \rightarrow n\gamma$, helicity-3/2 amplitude $A_{3/2}$

<table><thead><tr><th>VALUE (GeV<sup>-1/2</sup>)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>-0.120 to -0.100 (≈ -0.115) OUR ESTIMATE</strong></td></tr><tr><td>-0.123 ± 0.006</td><td>1 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>-0.118 ± 0.005</td><td>ANISOVICH</td><td>17E</td><td>DPWA Multichannel</td></tr><tr><td>-0.115 ± 0.005</td><td>1 CHEN</td><td>12A</td><td>DPWA γN → πN</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>-0.113 ± 0.012</td><td>ANISOVICH</td><td>13B</td><td>DPWA Multichannel</td></tr><tr><td>-0.101 ± 0.004</td><td>SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>-0.154</td><td>DRECHSEL</td><td>07</td><td>DPWA γN → πN</td></tr><tr><td>-0.159</td><td>PENNER</td><td>02D</td><td>DPWA Multichannel</td></tr></tbody></table>

¹Statistical error only.

$N(1520)$ REFERENCES

For early references, see Physics Letters **111B** 1 (1982). For very early references, see Reviews of Modern Physics **37** 633 (1965).

ROENCHEN 22 EPJ A58 229
ADAMCZEW... 20 PR C102 024001
MUELLER 20 PL B803 135323
HUNT 19 PR C99 055205
ANISOVICH 17E PR C96 055202
ROENCHEN 15A EPJ A51 70
SOKHOYAN 15A EPJ A51 95
PDG 14 CP C38 070001
SVARC 14 PR C89 045205
ANISOVICH 13B EPJ A49 67
SHKLYAR 13 PR C87 015201
ANISOVICH 12A EPJ A48 15
CHEN 12A PR C86 015206
SHRESTHA 12A PR C86 055203
WORKMAN 12A PR C86 015202

D. Roenchen et al. (JULI, GWU, BONN+)
J. Adamczewski-Musch et al. (HADES Collab.)
J. Mueller et al. (CBELSA/TAPS Collab.)
B.C. Hunt, D.M. Manley (BONN, PNPI, JLAB+)
A.V. Anisovich et al. (CBELSA/TAPS Collab.)
D. Roenchen et al. (PDG Collab.)
V. Sokhoyan et al. (BONN, PNPI)
A.V. Anisovich et al. (DUKE, GWU, MSST, ITEP+)
W. Chen et al. (KSU)
M. Shrestha, D.M. Manley (KSU)
R. Workman et al. (GWU)

BATINIC 10 PR C82 038203
THOMA 08 PL B659 87
DRECHSEL 07 EPJ A34 69
DUGGER 07 PR C76 025211
ARNDT 06 PR C74 045205
ARNDT 05 PR C72 045202
AHRENS 02 PRL 88 232002
PENNER 02C PR C66 055211
PENNER 02D PR C66 055212
VRANA 00 PRPL 328 181
TIATOR 99 PR C60 035210
MUKHOPAD... 98 PL B444 7
HOEHLER 93 πN Newsletter 9 1
CUTKOSKY 80 Toronto Conf. 19 (KARL)
Also 79 PDAT 12-1
HOEHLER 79 PDWA Multichannel
Also Toronto Conf. 3

M. Batinic et al. (ZAGR)
U. Thoma et al. (CB-ELSA Collab.)
D. Drechsel, S.S. Kamalov, L. Tiator (MAINZ, JNR)
M. Dugger et al. (JLab CLAS Collab.)
R.A. Arndt et al. (GWU)
R.A. Arndt et al. (GWU, PNPI)
J. Ahrens et al. (Mainz MAMI GDH/A2 Collab.)
G. Penner, U. Mosel (GIES)
G. Penner, U. Mosel (GIES)
T.P. Vrana, S.A. Dytmant, T.-S.H. Lee (PITT, ANL)
L. Tiator et al.
N.C. Mukhopadhyay, N. Mathur (KARL)
G. Hohler 93 πN Newsletter 9 1
R.E. Cutkosky et al. (CMU, LBL) JP
R.E. Cutkosky et al. (CMU, LBL) JP
G. Hohler et al. (KARL) JP
R. Koch (KARL) JP

$$N(1535) 1/2^{-}$$

$$I(J^P) = \frac{1}{2}(\frac{1}{2}^{-}) \text{ Status: } ****$$

Older and obsolete values are listed and referenced in the 2014 edition, Chinese Physics **C38** 070001 (2014).

$N(1535)$ POLE POSITION

REAL PART

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>1500 to 1520 (≈ 1510) OUR ESTIMATE</strong></td></tr><tr><td>1504 ± 0</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>1496 ± 4</td><td>AFZAL</td><td>20</td><td>DPWA Multichannel</td></tr><tr><td>1500 ± 4</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>1509 ± 4 ± 2</td><td>1 SVARC</td><td>14</td><td>L+P πN → πN</td></tr><tr><td>1510 ± 50</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>1496</td><td>HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>1499</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>1490</td><td>SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>1501 ± 4</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>1521 ± 14</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>1502</td><td>ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr><tr><td>1525</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr><tr><td>1487</td><td>HOEHLER</td><td>93</td><td>SPED πN → πN</td></tr></tbody></table>

¹Fit to the amplitudes of HOEHLER 79.

-2xIMAGINARY PART

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>80 to 130 (≈ 110) OUR ESTIMATE</strong></td></tr><tr><td>74 ± 1</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>125 ± 6</td><td>AFZAL</td><td>20</td><td>DPWA Multichannel</td></tr><tr><td>128 ± 9</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>118 ± 9 ± 2</td><td>2 SVARC</td><td>14</td><td>L+P πN → πN</td></tr><tr><td>260 ± 80</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tbody><tr><td>119</td><td>HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>104</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>100</td><td>SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>134 ± 11</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>190 ± 28</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>95</td><td>ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr><tr><td>102</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr></tbody></table>

²Fit to the amplitudes of HOEHLER 79.

$N(1535)$ ELASTIC POLE RESIDUE

MODULUS $|r|$

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>15 to 35 (≈ 25) OUR ESTIMATE</strong></td></tr><tr><td>18 ± 1</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>29 ± 4</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>22 ± 2 ± 0.4</td><td>3 SVARC</td><td>14</td><td>L+P πN → πN</td></tr><tr><td>120 ± 40</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tbody><tr><td>22</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>15</td><td>SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>31 ± 4</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>68</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>16</td><td>ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr></tbody></table>

³Fit to the amplitudes of HOEHLER 79.

PHASE $\theta$

<table><thead><tr><th>VALUE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>-40 to 0 (≈ -20) OUR ESTIMATE</strong></td></tr><tr><td>-37 ± 2</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>-20 ± 10</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>-5 ± 5 ± 3</td><td>4 SVARC</td><td>14</td><td>L+P πN → πN</td></tr><tr><td>+15 ± 45</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr></tbody></table>
• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tr><td>-46</td><td>ROENCHEN</td><td>15A</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>-51</td><td>SHKLYAR</td><td>13</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>-29 ± 5</td><td>ANISOVICH</td><td>12A</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>12</td><td>BATINIC</td><td>10</td><td>DPWA</td><td>πN → Nπ, ηN</td></tr><tr><td>-16</td><td>ARNDT</td><td>06</td><td>DPWA</td><td>πN → πN, ηN</td></tr></table>

⁴ Fit to the amplitudes of HOEHLER 79.

## N(1535) INELASTIC POLE RESIDUE

The "normalized residue" is the residue divided by $\Gamma_{pole}/2$.

### Normalized residue in $N\pi \to N(1535) \to N\eta$

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.50±0.02</td><td>118 ± 1</td><td>ROENCHEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>0.43±0.03</td><td>-76 ± 5</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.51</td><td>112</td><td>ROENCHEN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

### Normalized residue in $N\pi \to N(1535) \to \Lambda K$

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.26±0.01</td><td>-67 ± 2</td><td>ROENCHEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.05</td><td>32</td><td>ROENCHEN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

### Normalized residue in $N\pi \to N(1535) \to \Sigma K$

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.28±0.01</td><td>92 ± 2</td><td>ROENCHEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.05</td><td>-69</td><td>ROENCHEN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

### Normalized residue in $N\pi \to N(1535) \to \Delta\pi, D$-wave

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.11±0.02</td><td>160 ± 20</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.12±0.03</td><td>145 ± 17</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr></tbody></table>

### Normalized residue in $N\pi \to N(1535) \to N\sigma$

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.16±0.07</td><td>25 ± 40</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

### Normalized residue in $N\pi \to N(1535) \to N(1440)\pi$

<table><thead><tr><th>MODULUS</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.21±0.14</td><td>-45 ± 50</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

## N(1535) BREIT-WIGNER MASS

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>1515</strong> to <strong>1545</strong> (≈ <strong>1530</strong>) OUR ESTIMATE</td><td></td><td></td><td></td></tr><tr><td>1525 ± 2</td><td>5 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>1528 ± 6</td><td>KASHEVAROV</td><td>17</td><td>DPWA γp → ηp, η'p</td></tr><tr><td>1517 ± 4</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>1526 ± 2</td><td>5 SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>1547.0 ± 0.7</td><td>5 ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr><tr><td>1550 ± 40</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr><tr><td>1526 ± 7</td><td>HOEHLER</td><td>79</td><td>IPWA πN → πN</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>1519 ± 5</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>1538 ± 1</td><td>5 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>1553 ± 8</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>1546.7 ± 2.2</td><td>ARNDT</td><td>04</td><td>DPWA πN → πN, ηN</td></tr><tr><td>1526 ± 2</td><td>PENNER</td><td>02C</td><td>DPWA Multichannel</td></tr><tr><td>1530 ± 10</td><td>BAI</td><td>01B</td><td>BES J/ψ → pπη</td></tr><tr><td>1522 ± 11</td><td>THOMPSON</td><td>01</td><td>CLAS γ* p → pη</td></tr><tr><td>1542 ± 3</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr><tr><td>1532 ± 5</td><td>ARMSTRONG</td><td>99B</td><td>DPWA γ* p → pη</td></tr></tbody></table>

⁵ Statistical error only.

## N(1535) BREIT-WIGNER WIDTH

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td><strong>125</strong> to <strong>175</strong> (≈ <strong>150</strong>) OUR ESTIMATE</td><td></td><td></td><td></td></tr><tr><td>147 ± 5</td><td>6 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>163 ± 25</td><td>KASHEVAROV</td><td>17</td><td>DPWA γp → ηp, η'p</td></tr><tr><td>120 ± 10</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>131 ± 12</td><td>6 SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>188.4 ± 3.8</td><td>6 ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr><tr><td>240 ± 80</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr><tr><td>120 ± 20</td><td>HOEHLER</td><td>79</td><td>IPWA πN → πN</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>128 ± 14</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>141 ± 4</td><td>6 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>182 ± 25</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr></tbody></table>

<table><tr><td>129 ± 8</td><td>PENNER</td><td>02C</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>95 ± 25</td><td>BAI</td><td>01B</td><td>BES</td><td>J/ψ → pπη</td></tr><tr><td>143 ± 18</td><td>THOMPSON</td><td>01</td><td>CLAS</td><td>γ* p → pη</td></tr><tr><td>112 ± 19</td><td>VRANA</td><td>00</td><td>DPWA</td><td>γ* p → pη</td></tr><tr><td>154 ± 20</td><td>ARMSTRONG</td><td>99B</td><td>DPWA</td><td>γ* p → pη</td></tr></table>

⁶ Statistical error only.

## N(1535) DECAY MODES

The following branching fractions are our estimates, not fits or averages.

<table><thead><tr><th>Mode</th><th>Fraction (Γ<sub>f</sub>/Γ)</th></tr></thead><tbody><tr><td>Γ<sub>1</sub> Nπ</td><td>32-52%</td></tr><tr><td>Γ<sub>2</sub> Nη</td><td>30-55%</td></tr><tr><td>Γ<sub>3</sub> Nππ</td><td>4-31%</td></tr><tr><td>Γ<sub>4</sub> Δ(1232)π, D-wave</td><td>1-4%</td></tr><tr><td>Γ<sub>5</sub> Nρ</td><td>2-17%</td></tr><tr><td>Γ<sub>6</sub> Nρ, S=1/2, S-wave</td><td>2-16%</td></tr><tr><td>Γ<sub>7</sub> Nρ, S=3/2, D-wave</td><td>&lt;1%</td></tr><tr><td>Γ<sub>8</sub> Nσ</td><td>2-10%</td></tr><tr><td>Γ<sub>9</sub> N(1440)π</td><td>5-12%</td></tr><tr><td>Γ<sub>10</sub> pγ, helicity=1/2</td><td>0.15-0.30%</td></tr><tr><td>Γ<sub>11</sub> nγ, helicity=1/2</td><td>0.01-0.25%</td></tr></tbody></table>

## N(1535) BRANCHING RATIOS

### $\Gamma(N\pi)/\Gamma_{\text{total}}$

<table><thead><tr><th>VALUE (%)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>32-52% OUR ESTIMATE</strong></td></tr><tr><td>42 ± 2</td><td>7 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>52 ± 5</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>35 ± 3</td><td>7 SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>35.5 ± 0.2</td><td>7 ARNDT</td><td>06</td><td>DPWA πN → πN, ηN</td></tr><tr><td>50 ± 10</td><td>CUTKOSKY</td><td>80</td><td>IPWA πN → πN</td></tr><tr><td>38 ± 4</td><td>HOEHLER</td><td>79</td><td>IPWA πN → πN</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>54 ± 5</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>37 ± 1</td><td>7 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>46 ± 7</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr><tr><td>36 ± 1</td><td>PENNER</td><td>02C</td><td>DPWA Multichannel</td></tr><tr><td>35 ± 8</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr></tbody></table>

⁷ Statistical error only.

### $\Gamma(N\eta)/\Gamma_{\text{total}}$

<table><thead><tr><th>VALUE (%)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>30-55% OUR ESTIMATE</strong></td></tr><tr><td>41±4</td><td>MUELLER</td><td>20</td><td>DPWA Multichannel</td></tr><tr><td>43±3</td><td>8 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>41±4</td><td>9 KASHEVAROV</td><td>17</td><td>DPWA γp → ηp, η'p</td></tr><tr><td>58±4</td><td>8 SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>33±5</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>53±1</td><td>PENNER</td><td>02C</td><td>DPWA Multichannel</td></tr><tr><td>51±5</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>41±2</td><td>8 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>50±7</td><td>BATINIC</td><td>10</td><td>DPWA πN → Nπ, Nη</td></tr></tbody></table>

⁸ Statistical error only.

⁹ Assuming $A_{1/2} = 0.115$ GeV$^{-1/2}$.

### $\Gamma(N\eta)/\Gamma(N\pi)$

<table><thead><tr><th>VALUE (%)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>0.95±0.03</td><td>AZNAURYAN</td><td>09</td><td>CLAS π, η electroproduction</td></tr></tbody></table>

### $\Gamma(\Delta(1232)\pi, D$-wave)/$\Gamma_{\text{total}}$

<table><thead><tr><th>VALUE (%)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>1-4% OUR ESTIMATE</strong></td></tr><tr><td>3 ± 1</td><td>ADAMCZEW...</td><td>20</td><td>DPWA Multichannel</td></tr><tr><td>&lt;1.1</td><td>10 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>2.5±1.5</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td colspan="5">• • • We do not use the following data for averages, fits, limits, etc. • • •</td></tr><tr><td>2.5±1.5</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>1.8±0.8</td><td>10 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>1 ± 1</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr></tbody></table>

¹⁰ Statistical error only.

### $\Gamma(N\rho, S=1/2, S$-wave)/$\Gamma_{\text{total}}$

<table><thead><tr><th>VALUE (%)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>2-16% OUR ESTIMATE</strong></td></tr><tr><td>2.7±0.6</td><td>ADAMCZEW...</td><td>20</td><td>DPWA Multichannel</td></tr><tr><td>14 ± 2</td><td>11 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr></tbody></table>

¹¹ Statistical error only.
$\Gamma(N\rho, S=3/2, D-wave)/\Gamma_{\text{total}}$

<table><thead><tr><th>VALUE (%)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>&lt;1 % OUR ESTIMATE</strong></td></tr><tr><td>0.5 ± 0.5</td><td>ADAMCZEW... 20</td><td>DPWA</td><td>Multichannel</td></tr><tr><td>&lt;0.3</td><td>12 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td colspan="4"><sup>12</sup>Statistical error only.</td></tr></tbody></table>

$\Gamma(N\sigma)/\Gamma_{\text{total}}$

<table><thead><tr><th>VALUE (%)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>2-10 % OUR ESTIMATE</strong></td></tr><tr><td>&lt;1</td><td>13 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>6 ± 4</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td colspan="4"><strong>• • • We do not use the following data for averages, fits, limits, etc. • • •</strong></td></tr><tr><td>1.5 ± 0.5</td><td>13 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>2 ± 1</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr><tr><td colspan="4"><sup>13</sup>Statistical error only.</td></tr></tbody></table>

$\Gamma(N(1440)\pi)/\Gamma_{\text{total}}$

<table><thead><tr><th>VALUE (%)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>5-12 % OUR ESTIMATE</strong></td></tr><tr><td>&lt; 0.01</td><td>14 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>12 ± 8</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>8 ± 2</td><td>14 STAROSTIN</td><td>03</td><td>$\pi^- p \to n3\pi^0$</td></tr><tr><td colspan="4"><strong>• • • We do not use the following data for averages, fits, limits, etc. • • •</strong></td></tr><tr><td>&lt; 1</td><td>14 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>10 ± 9</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr></tbody></table>

$^{14}$This value is an estimate made using simplest assumptions.

N(1535) PHOTON DECAY AMPLITUDES AT THE POLE

$N(1535) \to p\gamma$, helicity-1/2 amplitude $A_{1/2}$

<table><thead><tr><th>MODULUS (GeV<sup>-1/2</sup>)</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>0.084 ± 0.002</td><td>-12 ± 2</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>0.093 ± 0.009</td><td>8 ± 4</td><td>ANISOVICH</td><td>17D</td><td>DPWA Multichannel</td></tr><tr><td colspan="5"><strong>• • • We do not use the following data for averages, fits, limits, etc. • • •</strong></td></tr><tr><td>0.114 ± 0.008</td><td>10 ± 5</td><td>ANISOVICH</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>0.106</td><td>5.2</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>0.114 ± 0.008</td><td>10 ± 5</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

$N(1535) \to n\gamma$, helicity-1/2 amplitude $A_{1/2}$

<table><thead><tr><th>MODULUS (GeV<sup>-1/2</sup>)</th><th>PHASE (°)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td>-0.088 ± 0.004</td><td>5 ± 4</td><td>ANISOVICH</td><td>17D</td><td>DPWA Multichannel</td></tr><tr><td colspan="5"><strong>• • • We do not use the following data for averages, fits, limits, etc. • • •</strong></td></tr><tr><td>-0.095 ± 0.006</td><td>8 ± 5</td><td>ANISOVICH</td><td>15A</td><td>DPWA Multichannel</td></tr></tbody></table>

N(1535) BREIT-WIGNER PHOTON DECAY AMPLITUDES

$N(1535) \to p\gamma$, helicity-1/2 amplitude $A_{1/2}$

<table><thead><tr><th>VALUE (GeV<sup>-1/2</sup>)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>0.090 to 0.120 (≈ 0.105) OUR ESTIMATE</strong></td></tr><tr><td>0.107 ± 0.003</td><td>15 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>0.101 ± 0.007</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>0.091 ± 0.004</td><td>15 SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>0.128 ± 0.004</td><td>15 WORKMAN</td><td>12A</td><td>DPWA $\gamma N \to N\pi$</td></tr><tr><td>0.091 ± 0.002</td><td>15 DUGGER</td><td>07</td><td>DPWA $\gamma N \to \pi N$</td></tr><tr><td colspan="4"><strong>• • • We do not use the following data for averages, fits, limits, etc. • • •</strong></td></tr><tr><td>0.105 ± 0.010</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>0.059 ± 0.003</td><td>15 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>0.066</td><td>DRECHSEL</td><td>07</td><td>DPWA $\gamma N \to \pi N$</td></tr><tr><td>0.090</td><td>PENNER</td><td>02D</td><td>DPWA Multichannel</td></tr></tbody></table>

$^{15}$Statistical error only.

$N(1535) \to n\gamma$, helicity-1/2 amplitude $A_{1/2}$

<table><thead><tr><th>VALUE (GeV<sup>-1/2</sup>)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>-0.095 to -0.055 (≈ -0.075) OUR ESTIMATE</strong></td></tr><tr><td>-0.055 ± 0.006</td><td>16 HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>-0.081 ± 0.006</td><td>ANISOVICH</td><td>17E</td><td>DPWA Multichannel</td></tr><tr><td>-0.058 ± 0.006</td><td>16 CHEN</td><td>12A</td><td>DPWA $\gamma N \to \pi N$</td></tr><tr><td colspan="4"><strong>• • • We do not use the following data for averages, fits, limits, etc. • • •</strong></td></tr><tr><td>-0.093 ± 0.011</td><td>ANISOVICH</td><td>13B</td><td>DPWA Multichannel</td></tr><tr><td>-0.049 ± 0.003</td><td>16 SHRESTHA</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>-0.051</td><td>DRECHSEL</td><td>07</td><td>DPWA $\gamma N \to \pi N$</td></tr><tr><td>-0.024</td><td>PENNER</td><td>02D</td><td>DPWA Multichannel</td></tr></tbody></table>

$^{16}$Statistical error only.

$N(1535) \to N\gamma$, ratio $A_{1/2}^N/A_{1/2}^P$

<table><thead><tr><th>VALUE (GeV<sup>-1/2</sup>)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>• • • We do not use the following data for averages, fits, limits, etc. • • •</strong></td></tr><tr><td>-0.84 ± 0.15</td><td>MUKHOPAD... 95B</td><td>IPWA</td><td></td></tr></tbody></table>

N(1535) REFERENCES

For early references, see Physics Letters **111B** 1 (1982).

<table><tbody><tr><td>ROenchEN</td><td>22</td><td>EJ A58 229</td><td>D. Roenchen et al.</td><td>(JULL GWU, BONN+)</td></tr><tr><td>ADAMCZEW...</td><td>20</td><td>PR C102 024001</td><td>J. Adamczewski-Musch et al.</td><td>(HADES Collab.)</td></tr><tr><td>AFZAL</td><td>20</td><td>PR L125 152002</td><td>F. Afzal et al.</td><td>(CBELSA/TAPS Collab.)</td></tr><tr><td>MUELLER</td><td>20</td><td>PL B803 135323</td><td>J. Mueller et al.</td><td>(CBELSA/TAPS Collab.)</td></tr><tr><td>HUNT</td><td>19</td><td>PR C99 055205</td><td>B.C. Hunt, D.M. Manley</td><td></td></tr><tr><td>ANISOVICH</td><td>17D</td><td>PR C95 035211</td><td>A.V. Anisovich et al.</td><td>(BONN, PNPI, JLAB+)</td></tr><tr><td>ANISOVICH</td><td>17E</td><td>PR C96 055202</td><td>A.V. Anisovich et al.</td><td>(A2/MAMI Collab.)</td></tr><tr><td>KASHEVAROV</td><td>17</td><td>PR L118 212001</td><td>V.L. Kashevarov et al.</td><td></td></tr><tr><td>ANISOVICH</td><td>15A</td><td>EPJ A51 72</td><td>A.V. Anisovich et al.</td><td></td></tr><tr><td>ROenchEN</td><td>15A</td><td>EPJ A51 70</td><td>D. Roenchen et al.</td><td></td></tr><tr><td>SOKHOYAN</td><td>15A</td><td>EPJ A51 95</td><td>V. Sokhoyan et al.</td><td>(CBELSA/TAPS Collab.)</td></tr><tr><td>PDG</td><td>14</td><td>CP C38 070001</td><td>K. Olive et al.</td><td>(PDG Collab.)</td></tr><tr><td>SVARC</td><td>14</td><td>PR C89 045205</td><td>A. Svarc et al.</td><td>(RBI Zagreb, UNI Tuza)</td></tr><tr><td>ANISOVICH</td><td>13B</td><td>EPJ A49 67</td><td>A.V. Anisovich et al.</td><td></td></tr><tr><td>SHKLYAR</td><td>13</td><td>PR C87 015201</td><td>V. Shklyar, H. Lenske, U. Mosel</td><td>(GIES)</td></tr><tr><td>ANISOVICH</td><td>12A</td><td>EPJ A48 15</td><td>A.V. Anisovich et al.</td><td>(BONN, PNPI)</td></tr><tr><td>CHEN</td><td>12A</td><td>PR C86 015206</td><td>W. Chen et al.</td><td>(DUKE, GWU, MSST, ITEP+)</td></tr><tr><td>SHRESTHA</td><td>12A</td><td>PR C86 055203</td><td>M. Shrestha, D.M. Manley</td><td>(KSU)</td></tr><tr><td>WORKMAN</td><td>12A</td><td>PR C86 015202</td><td>R. Workman et al.</td><td>(GWU)</td></tr><tr><td>BATINIC</td><td>10</td><td>PR C82 038203</td><td>M. Batinic et al.</td><td>(ZAGR)</td></tr><tr><td>AZNAURYAN</td><td>09</td><td>PR C80 055203</td><td>I.G. Aznauryan et al.</td><td>(JLab CLAS Collab.)</td></tr><tr><td>DRECHSEL</td><td>07</td><td>EPJ A34 69</td><td>D. Drechsel, S.S. Kamalov, L. Tiator</td><td>(MAINZ, JINR)</td></tr><tr><td>DUGGER</td><td>07</td><td>PR C76 025211</td><td>M. Dugger et al.</td><td>(JLab CLAS Collab.)</td></tr><tr><td>ARNDT</td><td>06</td><td>PR C74 045205</td><td>R.A. Arndt et al.</td><td>(GWU)</td></tr><tr><td>ARNDT</td><td>04</td><td>PR C69 035213</td><td>R.A. Arndt et al.</td><td>(GWU, TRIU)</td></tr><tr><td>STAROSTIN</td><td>03</td><td>PR C67 068201</td><td>A. Starostin et al.</td><td>(BNL Crystal Ball Collab.)</td></tr><tr><td>PENNER</td><td>02C</td><td>PR C66 055211</td><td>G. Penner, U. Mosel</td><td>(GIES)</td></tr><tr><td>PENNER</td><td>02D</td><td>PR C66 055212</td><td>G. Penner, U. Mosel</td><td>(GIES)</td></tr><tr><td>BAI</td><td>01B</td><td>PL B510 75</td><td>J.Z. Bai et al.</td><td>(BES Collab.)</td></tr><tr><td>THOMPSON</td><td>01</td><td>PR L86 1702</td><td>R. Thompson et al.</td><td>(JLab CLAS Collab.)</td></tr><tr><td>VRANA</td><td>00</td><td>PRPL 328 181</td><td>T.P. Vrana, S.A. Dytman, T.-S.H. Lee</td><td>(PITT, ANL)</td></tr><tr><td>ARMSTRONG</td><td>99B</td><td>PR D60 052004</td><td>C.S. Armstrong et al.</td><td></td></tr><tr><td>MUKHOPAD...</td><td>95B</td><td>PL B346 1</td><td>N.C. Mukhopadhyay, J.F. Zhang, M. Benmerrouche</td><td></td></tr><tr><td>HOEHLER</td><td>93</td><td>$\pi^N$ Newsletter 9 1</td><td>G. Hohler</td><td>(KARL)</td></tr><tr><td>CUTKOSKY</td><td>80</td><td>Toronto Conf. 19</td><td>R.E. Cutkosky et al.</td><td>(CMU, LBL) JP</td></tr><tr><td>Also</td><td></td><td>PR D20 2839</td><td>R.E. Cutkosky et al.</td><td>(CMU, LBL) JP</td></tr><tr><td>Also</td><td>79</td><td>PDAT 12-1</td><td>G. Hohler et al.</td><td>(KARLT) JP</td></tr><tr><td></td><td></td><td>Toronto Conf. 3</td><td>R. Koch</td><td>(KARLT) JP</td></tr></tbody></table>

$N(1650) 1/2^-$

$I(J^P) = \frac{1}{2}(\frac{1}{2}^-)$ Status: ****

Older and obsolete values are listed and referenced in the 2014 edition, Chinese Physics **C38** 070001 (2014).

N(1650) POLE POSITION

REAL PART

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>1650 to 1680 (≈ 1665) OUR ESTIMATE</strong></td></tr><tr><td>1678 ± 2</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>1664 ± 4</td><td>AFZAL</td><td>20</td><td>DPWA Multichannel</td></tr><tr><td>1658 ± 10</td><td>ANISOVICH</td><td>17A</td><td>DPWA Multichannel</td></tr><tr><td>1660 ± 5</td><td>1 ANISOVICH</td><td>17A</td><td>L+P $\gamma p, \pi^- p \to K\Lambda$</td></tr><tr><td>1660 ± 3.5 ± 1</td><td>2 SVARC</td><td>14</td><td>L+P $\pi N \to \pi N$</td></tr><tr><td>1640 ± 20</td><td>CUTKOSKY</td><td>80</td><td>IPWA $\pi N \to \pi N$</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tbody><tr><td>1656</td><td>HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>1672</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>1652 ± 7</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>1650</td><td>SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>1647 ± 6</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>1646 ± 8</td><td>BATINIC</td><td>10</td><td>DPWA $\pi N \to N\pi, N\eta$</td></tr><tr><td>1648</td><td>ARNDT</td><td>06</td><td>DPWA $\pi N \to \pi N, \eta N$</td></tr><tr><td>1663</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr><tr><td>1670</td><td>HOEHLER</td><td>93</td><td>ARGD $\pi N \to \pi N$</td></tr></tbody></table>

¹Statistical error only.

²Fit to the amplitudes of HOEHLER 79.

-2xIMAGINARY PART

<table><thead><tr><th>VALUE (MeV)</th><th>DOCUMENT ID</th><th>TECN</th><th>COMMENT</th></tr></thead><tbody><tr><td colspan="4"><strong>100 to 170 (≈ 135) OUR ESTIMATE</strong></td></tr><tr><td>127 ± 2</td><td>ROenchEN</td><td>22</td><td>DPWA Multichannel</td></tr><tr><td>98 ± 6</td><td>AFZAL</td><td>20</td><td>DPWA Multichannel</td></tr><tr><td>102 ± 8</td><td>ANISOVICH</td><td>17A</td><td>DPWA Multichannel</td></tr><tr><td>59 ± 16</td><td>1 ANISOVICH</td><td>17A</td><td>L+P $\gamma p, \pi^- p \to K\Lambda$</td></tr><tr><td>167 ± 8 ± 2</td><td>2 SVARC</td><td>14</td><td>L+P $\pi N \to \pi N$</td></tr><tr><td>150 ± 30</td><td>CUTKOSKY</td><td>80</td><td>IPWA $\pi N \to \pi N$</td></tr></tbody></table>

• • • We do not use the following data for averages, fits, limits, etc. • • •

<table><tbody><tr><td>130</td><td>HUNT</td><td>19</td><td>DPWA Multichannel</td></tr><tr><td>137</td><td>ROenchEN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>102 ± 8</td><td>SOKHOYAN</td><td>15A</td><td>DPWA Multichannel</td></tr><tr><td>89</td><td>SHKLYAR</td><td>13</td><td>DPWA Multichannel</td></tr><tr><td>103 ± 8</td><td>ANISOVICH</td><td>12A</td><td>DPWA Multichannel</td></tr><tr><td>204 ± 17</td><td>BATINIC</td><td>10</td><td>DPWA $\pi N \to N\pi, N\eta$</td></tr><tr><td>80</td><td>ARNDT</td><td>06</td><td>DPWA $\pi N \to \pi N, \eta N$</td></tr><tr><td>240</td><td>VRANA</td><td>00</td><td>DPWA Multichannel</td></tr><tr><td>163</td><td>HOEHLER</td><td>93</td><td>ARGD $\pi N \to \pi N$</td></tr></tbody></table>

¹Statistical error only.

²Fit to the amplitudes of HOEHLER 79.