| • • • We do not use the following data for averages, fits, limits, etc. • • • |
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FLAT |
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FLAT |
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3 |
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FLAT |
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4 |
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HESS |
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5 |
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MGIC |
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6 |
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HAWC |
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7 |
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HAWC |
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8 |
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ICCB |
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9 |
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ICCB |
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10 |
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ICCB |
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11 |
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ANTR |
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12 |
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VRTS |
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13 |
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ICCB |
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14 |
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HESS |
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15 |
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ANTR |
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16 |
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MGFL |
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17 |
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BAIK |
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18 |
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THEO |
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18 |
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THEO |
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19 |
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HESS |
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20 |
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FLAT |
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FLAT |
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22 |
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FLAT |
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23 |
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THEO |
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24 |
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SKAM |
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25 |
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MGIC |
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26 |
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BAIK |
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27 |
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ICCB |
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28 |
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HESS |
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29 |
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COSM |
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30 |
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BAKS |
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29 |
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ASTR |
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29 |
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COSM |
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31 |
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ICCB |
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32 |
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HESS |
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33 |
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FLAT |
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34 |
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FLAT |
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35 |
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AMND |
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36 |
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AMND |
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RVUE |
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38 |
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SKAM |
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MCRO |
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RVUE |
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KAMI |
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COSM |
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RVUE |
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COSM |
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44 |
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RVUE |
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45 |
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KAMI |
| $\text{none 4-15 GeV}$ |
46 |
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COSM |
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1
DI-MAURO 2019 sets limits on the dark matter annihilation from gamma-ray searches in M31 and M33 galaxies using Fermi LAT data.
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2
JOHNSON 2019 sets limits on p-wave dark matter annihilations in the galactic center using Fermi data.
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LI 2019D sets limits on dark matter annihilation cross sections searching for line-like signals in the all-sky Fermi data.
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4
ABDALLAH 2018 places constraints on the dark matter annihilation cross section for annihilations into gamma-rays in the Galactic center for masses between 300 GeV to 70 TeV. This updates ABDALLAH 2016 .
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AHNEN 2018 uses observations of the dwarf satellite galaxy Ursa Major II to obtain upper limits on annihilation cross sections for dark matter in various channels for masses between $0.1 - 100$ TeV.
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6
ALBERT 2018B sets limits on the annihilation cross section of dark matter with mass between 1 and 100 TeV from gamma-ray observations of the Andromeda galaxy.
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ALBERT 2018C sets limits on the spin-dependent coupling of dark matter to protons from dark matter annihilation in the Sun.
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8
AARTSEN 2017 is based on data collected during 327 days of detector livetime with IceCube. They looked for interactions of ${{\mathit \nu}}$'s resulting from neutralino annihilations in the Earth over a background of atmospheric neutrinos and set 90$\%$ CL limits on the spin independent neutralino-proton cross section for neutralino masses in the range $10 - 10000$ GeV.
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AARTSEN 2017A is based on data collected during 532 days of livetime with the IceCube 86-string detector including the DeepCore sub-array. They looked for interactions of ${{\mathit \nu}}$'s from neutralino annihilations in the Sun over a background of atmospheric neutrinos and set 90$\%$ CL limits on the spin dependent neutralino-proton cross section for neutralino masses in the range $10 - 10000$ GeV. This updates AARTSEN 2016C.
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10
AARTSEN 2017C is based on 1005 days of running with the IceCube detector. They set a limit on the annihilation cross section for dark matter with masses between $10 - 1000$ GeV annihilating in the Galactic center assuming an NFW profile. The limit is of $1.2 \times 10^{23}$ cm${}^{3}$s${}^{-1}$ in the ${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$ channel. Supercedes AARTSEN 2015E.
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ALBERT 2017A is based on data from the ANTARES neutrino telescope. They looked for interactions of ${{\mathit \nu}}$'s from neutralino annihilations in the Milky Way galaxy over a background of atmospheric neutrinos and set 90$\%$ CL limits on the muon neutrino flux. They also obtain limits on the thermally averaged cross section for neutralino masses in the range 50 to 100,000 GeV. This updates ADRIAN-MARTINEZ 2015 .
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12
ARCHAMBAULT 2017 performs a joint statistical analysis of four dwarf galaxies with VERITAS looking for gamma-ray emission from neutralino annihilation. They set limits on the neutralino annihilation cross section.
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AARTSEN 2016D is based on 329 live days of running with the DeepCore subdetector of the IceCube detector. They set a limit of $10^{-23}$ cm${}^{3}$s${}^{-1}$ on the annihilation cross section to ${{\mathit \nu}}{{\overline{\mathit \nu}}}$ . This updates AARTSEN 2015C.
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14
ABDALLAH 2016A place upper limits on the annihilation cross section with final states in the energy range of 0.1 to 2 TeV. This complements ABRAMOWSKI 2013 .
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15
ADRIAN-MARTINEZ 2016 is based on data from the ANTARES neutrino telescope. They looked for interactions of ${{\mathit \nu}}$'s from neutralino annihilations in the Sun over a background of atmospheric neutrinos and set 90$\%$ CL limits on the muon neutrino flux. They also obtain limits on the spin dependent and spin independent neutralino-proton cross section for neutralino masses in the range 50 to 5,000 GeV. This updates ADRIAN-MARTINEZ 2013 .
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AHNEN 2016 combines 158 hours of Segue 1 observations with MAGIC with 6 year observations of 15 dwarf satellite galaxies by Fermi-LAT to set limits on annihilation cross sections for dark matter masses between 10 GeV and 100 TeV.
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AVRORIN 2016 is based on 2.76 years with Lake Baikal neutrino telescope. They derive 90$\%$ upper limits on the annihilation cross section from dark matter annihilations in the Galactic center.
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CIRELLI 2016 and LEITE 2016 derive bounds on the annihilation cross section from radio observations.
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ABRAMOWSKI 2015 places constraints on the dark matter annihilation cross section for annihilations in the Galactic center for masses between 300 GeV to 10 TeV.
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ACKERMANN 2015 is based on 5.8 years of data with Fermi-LAT and search for monochromatic gamma-rays in the energy range of $0.2 - 500$ GeV from dark matter annihilations. This updates ACKERMANN 2013A.
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ACKERMANN 2015A is based on 50 months of data with Fermi-LAT and search for dark matter annihilation signals in the isotropic gamma-ray background as well as galactic subhalos in the energy range of a few GeV to a few tens of TeV.
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ACKERMANN 2015B is based on 6 years of data with Fermi-LAT observations of Milky Way dwarf spheroidal galaxies. Set limits on the annihilation cross section from ${\mathit m}_{{{\mathit \chi}}}$ = 2 GeV to 10 TeV. This updates ACKERMANN 2014 .
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BUCKLEY 2015 is based on 5 years of Fermi-LAT data searching for dark matter annihilation signals from Large Magellanic Cloud.
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24
CHOI 2015 is based on 3903 days of SuperKamiokande data searching for neutrinos produced from dark matter annihilations in the sun. They place constraints on the dark matter-nucleon scattering cross section for dark matter masses between $4 - 200$ GeV.
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25
ALEKSIC 2014 is based on almost 160 hours of observations of Segue 1 satellite dwarf galaxy using the MAGIC telescopes between 2011 and 2013. Sets limits on the annihilation cross section out to ${\mathit m}_{{{\mathit \chi}}}$ = 10 TeV.
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AVRORIN 2014 is based on almost 2.76 years with Lake Baikal neutrino telescope. They derive 90$\%$ upper limits on the fluxes of muons and muon neutrinos from dark matter annihilations in the Sun.
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AARTSEN 2013C is based on data collected during 339.8 effective days with the IceCube 59-string detector. They looked for interactions of ${{\mathit \nu}_{{\mu}}}$'s from neutralino annihilations in nearby galaxies and galaxy clusters. They obtain limits on the neutralino annihilation cross section for neutralino masses in the range $30 - 100$ GeV.
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28
ABRAMOWSKI 2013 place upper limits on the annihilation cross section with ${{\mathit \gamma}}{{\mathit \gamma}}$ final states in the energy range of $0.5 - 25$ TeV.
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29
BERGSTROM 2013 , JIN 2013 , and KOPP 2013 derive limits on the mass and annihilation cross section using AMS-02 data. JIN 2013 also sets a limit on the lifetime of the dark matter particle.
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30
BOLIEV 2013 is based on data collected during 24.12 years of live time with the Bakson Underground Scintillator Telescope. They looked for interactions of ${{\mathit \nu}_{{\mu}}}$'s from neutralino annihilations in the Sun over a background of atmospheric neutrinos and set 90$\%$ CL limits on the muon flux. They also obtain limits on the spin dependent and spin independent neutralino-proton cross section for neutralino masses in the range $10 - 1000~$GeV.
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31
ABBASI 2012 is based on data collected during 812 effective days with AMANDA II and 149 days of the IceCube 40-string detector combined with the data of ABBASI 2009B. They looked for interactions of ${{\mathit \nu}_{{\mu}}}$'s from neutralino annihilations in the Sun over a background of atmospheric neutrinos and set 90$\%$ CL limits on the muon flux. No excess is observed. They also obtain limits on the spin dependent neutralino-proton cross section for neutralino masses in the range $50 - 5000$ GeV.
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32
ABRAMOWSKI 2011 place upper limits on the annihilation cross section with ${{\mathit \gamma}}{{\mathit \gamma}}$ final states.
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33
ABDO 2010 place upper limits on the annihilation cross section with ${{\mathit \gamma}}{{\mathit \gamma}}$ or ${{\mathit \mu}^{+}}{{\mathit \mu}^{-}}$ final states.
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ACKERMANN 2010 place upper limits on the annihilation cross section with ${{\mathit b}}{{\overline{\mathit b}}}$ or ${{\mathit \mu}^{+}}{{\mathit \mu}^{-}}$ final states.
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35
ACHTERBERG 2006 is based on data collected during 421.9 effective days with the AMANDA detector. They looked for interactions of ${{\mathit \nu}_{{\mu}}}$s from the centre of the Earth over a background of atmospheric neutrinos and set 90 $\%$ CL limits on the muon flux. Their limit is compared with the muon flux expected from neutralino annihilations into ${{\mathit W}^{+}}{{\mathit W}^{-}}$ and ${{\mathit b}}{{\overline{\mathit b}}}$ at the centre of the Earth for MSSM parameters compatible with the relic dark matter density, see their Fig. 7.
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36
ACKERMANN 2006 is based on data collected during 143.7 days with the AMANDA-II detector. They looked for interactions of ${{\mathit \nu}_{{\mu}}}$s from the Sun over a background of atmospheric neutrinos and set 90 $\%$ CL limits on the muon flux. Their limit is compared with the muon flux expected from neutralino annihilations into ${{\mathit W}^{+}}{{\mathit W}^{-}}$ in the Sun for SUSY model parameters compatible with the relic dark matter density, see their Fig. 3.
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37
DEBOER 2006 interpret an excess of diffuse Galactic gamma rays observed with the EGRET satellite as originating from ${{\mathit \pi}^{0}}$ decays from the annihilation of neutralinos into quark jets. They analyze the corresponding parameter space in a supergravity inspired MSSM model with radiative electroweak symmetry breaking, see their Fig. 3 for the preferred region in the (, ) plane of a scenario with large tan $\beta $.
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38
AMBROSIO 1999 and DESAI 2004 set new neutrino flux limits which can be used to limit the parameter space in supersymmetric models based on neutralino annihilation in the Sun and the Earth.
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39
LOSECCO 1995 reanalyzed the IMB data and places lower limit on ${\mathit m}_{{{\widetilde{\mathit \chi}}_{{1}}^{0}}}$ of 18 GeV if the LSP is a photino and 10 GeV if the LSP is a higgsino based on LSP annihilation in the sun producing high-energy neutrinos and the limits on neutrino fluxes from the IMB detector.
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40
MORI 1993 excludes some region in $\mathit M_{2}--\mu $ parameter space depending on tan $\beta $ and lightest scalar Higgs mass for neutralino dark matter ${\mathit m}_{{{\widetilde{\mathit \chi}}^{0}}}>{\mathit m}_{{{\mathit W}}}$, using limits on upgoing muons produced by energetic neutrinos from neutralino annihilation in the Sun and the Earth.
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41
BOTTINO 1992 excludes some region $\mathit M_{2}-{{\mathit \mu}}$ parameter space assuming that the lightest neutralino is the dark matter, using upgoing muons at Kamiokande, direct searches by Ge detectors, and by LEP experiments. The analysis includes top radiative corrections on Higgs parameters and employs two different hypotheses for nucleon-Higgs coupling. Effects of rescaling in the local neutralino density according to the neutralino relic abundance are taken into account.
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BOTTINO 1991 excluded a region in $\mathit M_{2}−{{\mathit \mu}}$ plane using upgoing muon data from Kamioka experiment, assuming that the dark matter surrounding us is composed of neutralinos and that the Higgs boson is not too heavy.
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GELMINI 1991 exclude a region in $\mathit M_{2}−\mu $ plane using dark matter searches.
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KAMIONKOWSKI 1991 excludes a region in the $\mathit M_{2}-{{\mathit \mu}}$ plane using IMB limit on upgoing muons originated by energetic neutrinos from neutralino annihilation in the sun, assuming that the dark matter is composed of neutralinos and that ${\mathit m}_{{{\mathit H}_{{1}}^{0}}}{ {}\lesssim{} }$ 50 GeV. See Fig.$~$8 in the paper.
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MORI 1991B exclude a part of the region in the $\mathit M_{2}-{{\mathit \mu}}$ plane with ${\mathit m}_{{{\widetilde{\mathit \chi}}_{{1}}^{0}}}{ {}\lesssim{} }$ 80 GeV using a limit on upgoing muons originated by energetic neutrinos from neutralino annihilation in the earth, assuming that the dark matter surrounding us is composed of neutralinos and that ${\mathit m}_{{{\mathit H}_{{1}}^{0}}}{ {}\lesssim{} }$ 80 GeV.
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46
OLIVE 1988 result assumes that photinos make up the dark matter in the galactic halo. Limit is based on annihilations in the sun and is due to an absence of high energy neutrinos detected in underground experiments. The limit is model dependent.
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