These papers generally exclude regions in the $\mathit M_{2}~-~{{\mathit \mu}}$ parameter plane assuming that ${{\widetilde{\mathit \chi}}_{{1}}^{0}}$ is the dominant form of dark matter in the galactic halo. These limits are based on the lack of detection in laboratory experiments, telescopes, or by the absence of a signal in underground neutrino detectors. The latter signal is expected if ${{\widetilde{\mathit \chi}}_{{1}}^{0}}$ accumulates in the Sun or the Earth and annihilates into high-energy ${{\mathit \nu}}$'s.

VALUE DOCUMENT ID TECN • • We do not use the following data for averages, fits, limits, etc. • • 1 ABBASI 2022 B ICCB 2 ABDALLA 2022 HESS 3 ABDALLAH 2021 HESS 4 ABAZAJIAN 2020 FLAT 5 ABDALLAH 2020 HESS 6 ABE 2020 G SKAM 7 ALBERT 2020 HAWC 8 ALBERT 2020 A ANTR 9 ALBERT 2020 C ANIC 10 ALVAREZ 2020 FLAT 11 HOOF 2020 FLAT 12 DI-MAURO 2019 FLAT 13 JOHNSON 2019 FLAT 14 LI 2019 D FLAT 15 AHNEN 2018 MGIC 16 ALBERT 2018 B HAWC 17 ALBERT 2018 C HAWC 18 AARTSEN 2017 ICCB 19 AARTSEN 2017 A ICCB 20 AARTSEN 2017 C ICCB 21 ARCHAMBAULT 2017 VRTS 22 ADRIAN-MARTIN.. 2016 ANTR 23 AHNEN 2016 MGFL 24 AVRORIN 2016 BAIK 25 CIRELLI 2016 THEO 25 LEITE 2016 THEO 26 ACKERMANN 2015 FLAT 27 ACKERMANN 2015 A FLAT 28 ACKERMANN 2015 B FLAT 29 BUCKLEY 2015 THEO 30 CHOI 2015 SKAM 31 ALEKSIC 2014 MGIC 32 AVRORIN 2014 BAIK 33 AARTSEN 2013 C ICCB 34 BERGSTROM 2013 COSM 35 BOLIEV 2013 BAKS 34 JIN 2013 ASTR 34 KOPP 2013 COSM 36 ACKERMANN 2010 FLAT 37 ACHTERBERG 2006 AMND 38 ACKERMANN 2006 AMND 39 DEBOER 2006 RVUE 40 DESAI 2004 SKAM 40 AMBROSIO 1999 MCRO 41 LOSECCO 1995 RVUE 42 MORI 1993 KAMI 43 BOTTINO 1992 COSM 44 BOTTINO 1991 RVUE 45 GELMINI 1991 COSM 46 KAMIONKOWSKI 1991 RVUE 47 MORI 1991 B KAMI $\text{none 4-15 GeV}$ 48 OLIVE 1988 COSM 1  ABBASI 2022B presents 7 years of data from a search of neutrinos from dark matter annihilations in the sun using the DeepCore sub-array of IceCube. Annihilation cross section limits applies to dark matter masses between $5 - 100$ GeV. 2  ABDALLA 2022 uses gamma-ray observations in the Galactic center to constrain the dark matter annihilation cross section for annihilations into ${{\mathit W}}{{\mathit W}}$ and ${{\mathit \tau}}{{\mathit \tau}}$ for dark matter masses between 200 GeV to 70 TeV. This updates ABDALLAH 2018 . 3  ABDALLAH 2021 places constraints on the dark matter annihilation cross section for annihilations into gamma-rays from the dwarf irregular galaxy WLM for masses between 0.15 to 10 TeV. 4  ABAZAJIAN 2020 sets constraints on the dark matter annihilation from gamma-ray searches from Fermi LAT observations of the Galactic center. 5  ABDALLAH 2020 places constraints on the dark matter annihilation cross section for annihilations into gamma-rays from Milky Way dwarf galaxy satellites for masses between 0.2 to 40 TeV. 6  ABE 2020G is based on SuperKamiokande data taken from 1996 to 2016 searching for neutrinos produced from dark matter annihilations in the galactic center or halo. They place constraints on the dark matter-nucleon scattering cross section for dark matter masses between 1 GeV and 10 TeV. 7  ALBERT 2020 sets limits on the annihilation cross section of dark matter with mass between 1 and 100 TeV from gamma-ray observations of the local dwarf spheroidal galaxies. 8  ALBERT 2020A set limits on the dark matter annihilation cross section from neutrinos observations in the Galactic center using 11 years of ANTARES data. 9  ALBERT 2020C set limits on the dark matter annihilation cross section from neutrinos observations in the Galactic center combining Antares and IceCube data. 10  ALVAREZ 2020 set limits on the dark matter annihilation from gamma-ray searches from Fermi LAT observations in the directions of dwarf spheroidal galaxies. 11  HOOF 2020 set limits on the dark matter annihilation from gamma-ray searches from Fermi LAT observations in the directions of dwarf spheroidal galaxies. 12  DI-MAURO 2019 sets limits on the dark matter annihilation from gamma-ray searches in M31 and M33 galaxies using Fermi LAT data. 13  JOHNSON 2019 sets limits on p-wave dark matter annihilations in the galactic center using Fermi data. 14  LI 2019D sets limits on dark matter annihilation cross sections searching for line-like signals in the all-sky Fermi data. 15  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. 16  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. 17  ALBERT 2018C sets limits on the spin-dependent coupling of dark matter to protons from dark matter annihilation in the Sun. 18  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. 19  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. 20  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. 21  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. 22  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 . 23  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. 24  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. 25  CIRELLI 2016 and LEITE 2016 derive bounds on the annihilation cross section from radio observations. 26  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. 27  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. 28  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 . 29  BUCKLEY 2015 is based on 5 years of Fermi-LAT data searching for dark matter annihilation signals from Large Magellanic Cloud. 30  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. 31  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. 32  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. 33  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. 34  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. 35  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. 36  ACKERMANN 2010 place upper limits on the annihilation cross section with ${{\mathit b}}{{\overline{\mathit b}}}$ or ${{\mathit \mu}^{+}}{{\mathit \mu}^{-}}$ final states. 37  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. 38  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. 39  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 (${\mathit m}_{{{\mathit 0}}}$, ) plane of a scenario with large tan $\beta $. 40  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. 41  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. 42  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. 43  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. 44  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. 45  GELMINI 1991 exclude a region in $\mathit M_{2}−\mu $ plane using dark matter searches. 46  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. 47  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. 48  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.

References:

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