${{\boldsymbol X}^{0}}$ Annihilation Cross Section INSPIRE search

Limits are on ${{\mathit \sigma}}{{\mathit v}}$ for ${{\mathit X}^{0}}$ pair annihilation at threshold.
VALUE (cm${}^{3}$s${}^{-1}$) CL% DOCUMENT ID TECN  COMMENT
• • • We do not use the following data for averages, fits, limits, etc. • • •
$<4 \times 10^{-26}$ 95 1
CHEUNG
2019
${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ ${{\mathit e}^{+}}{{\mathit e}^{-}}$ and ${{\mathit b}}{{\overline{\mathit b}}}$
$<4 \times 10^{-28}$ 95 2
ABDALLAH
2018
HESS ${{\mathit X}^{0}}$ ${{\mathit X}^{0}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit X}}$ ; galactic halo
$<1 \times 10^{-23}$ 95 3
AHNEN
2018
MGIC ${{\mathit X}^{0}}$ ${{\mathit X}^{0}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit X}}$ ; Ursa Major II
$<1 \times 10^{-22}$ 95 4
ALBERT
2018B
HAWC ${{\mathit X}^{0}}$ ${{\mathit X}^{0}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit X}}$ ; Andromeda
$<1 \times 10^{-26}$ 95 5
CHANG
2018A
${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ ${{\mathit b}}{{\overline{\mathit b}}}$ $\rightarrow$ ${{\mathit \gamma}}$
6
LISANTI
2018
THEO Fermi, ${{\mathit \gamma}}$; galaxy groups
7
MAZZIOTTA
2018
FLAT Fermi-LAT CRE data
$<1.2 \times 10^{-23}$ 95 8
AARTSEN
2017C
ICCB ${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ neutrinos
$<5 \times 10^{-25}$ 90 9
ALBERT
2017A
ANTR ${{\mathit \nu}}$, Milky Way
$<1.32 \times 10^{-25}$ 95 10
ARCHAMBAULT
2017
VRTS ${{\mathit \gamma}}$ dwarf galaxies
$<7 \times 10^{-21}$ 90 11
AVRORIN
2017
BAIK cosmic ${{\mathit \nu}}$
$<1 \times 10^{-28}$ 12
BOUDAUD
2017
MeV DM to ${{\mathit e}^{+}}{{\mathit e}^{-}}$
13
AARTSEN
2016D
ICCB ${{\mathit \nu}}$, galactic center
$<6 \times 10^{-26}$ 95 14
ABDALLAH
2016
HESS Central Galactic Halo
$<1 \times 10^{-27}$ 95 15
ABDALLAH
2016A
HESS WIMP+WIMP $\rightarrow$ ${{\mathit \gamma}}{{\mathit \gamma}}$ ; galactic center
$<3 \times 10^{-26}$ 95 16
AHNEN
2016
MGFL Satellite galaxy, $\mathit m$(WIMP)=100 GeV
$<1.9 \times 10^{-21}$ 90 17
AVRORIN
2016
BAIK ${{\mathit \nu}}$s from galactic center
$<3 \times 10^{-26}$ 95 18
CAPUTO
2016
FLAT small Magellanic cloud
$<1 \times 10^{-25}$ 95 19
FORNASA
2016
FLAT Fermi-LAT ${{\mathit \gamma}}$-ray anisotropy
$<5 \times 10^{-27}$ 20
LEITE
2016
WIMP, radio
$<2 \times 10^{-26}$ 95 21
LI
2016
FLAT dwarf galaxies
$<1 \times 10^{-25}$ 95 22
LI
2016A
FLAT Fermi-LAT; M31
$<1 \times 10^{-26}$ 23
LIANG
2016
FLAT Fermi-LAT, gamma line
$<1 \times 10^{-25}$ 95 24
LU
2016
FLAT Fermi-LAT and AMS-02
$<1 \times 10^{-23}$ 95 25
SHIRASAKI
2016
FLAT extra galactic
26
AARTSEN
2015C
ICCB ${{\mathit \nu}}$, Galactic halo
27
AARTSEN
2015E
ICCB ${{\mathit \nu}}$, Galactic center
28
ABRAMOWSKI
2015
HESS Galactic center
29
ACKERMANN
2015
FLAT monochromatic ${{\mathit \gamma}}$
30
ACKERMANN
2015A
FLAT isotropic ${{\mathit \gamma}}$ background
31
ACKERMANN
2015B
FLAT Satellite galaxy
32
ADRIAN-MARTIN..
2015
ANTR ${{\mathit \nu}}$, Galactic center
$<2.90 \times 10^{-26}$ 95 33, 34
ACKERMANN
2014
FLAT Satellite galaxy, $\mathit m$ = 10 GeV
$<1.84 \times 10^{-25}$ 95 33, 35
ACKERMANN
2014
FLAT Satellite galaxy, $\mathit m$ = 100 GeV
$<1.75 \times 10^{-24}$ 95 33, 35
ACKERMANN
2014
FLAT Satellite galaxy, $\mathit m$ = 1 TeV
$<4.52 \times 10^{-24}$ 95 36
ALEKSIC
2014
MGIC Segue 1, $\mathit m$ = 1.35 TeV
37
AARTSEN
2013C
ICCB Galaxies
38
ABRAMOWSKI
2013
HESS Central Galactic Halo
39
ACKERMANN
2013A
FLAT Galaxy
40
ABRAMOWSKI
2012
HESS Fornax Cluster
41
ACKERMANN
2012
FLAT Galaxy
42
ACKERMANN
2012
FLAT Galaxy
43
ALIU
2012
VRTS Segue 1
$<1 \times 10^{-22}$ 90 44
ABBASI
2011C
ICCB Galactic halo, $\mathit m$=1 TeV
$<3 \times 10^{-25}$ 95 45
ABRAMOWSKI
2011
HESS Near Galactic center, $\mathit m$=1 TeV
$<1 \times 10^{-26}$ 95 46
ACKERMANN
2011
FLAT Satellite galaxy, $\mathit m$=10 GeV
$<1 \times 10^{-25}$ 95 46
ACKERMANN
2011
FLAT Satellite galaxy, $\mathit m$=100 GeV
$<1 \times 10^{-24}$ 95 46
ACKERMANN
2011
FLAT Satellite galaxy, $\mathit m$=1 TeV
1  CHEUNG 2019 derive model-dependent bounds on $\langle \sigma \cdot{}v\rangle $ from EDGES data: $<$ $4 \times 10^{-26}$ cm${}^{3}$/s for ${{\mathit e}^{+}}{{\mathit e}^{-}}$ and ${{\mathit b}}{{\overline{\mathit b}}}$ for m(${{\mathit \chi}}$) = 100 GeV (including boost factor).
2  ABDALLAH 2018 search for WIMP WIMP $\rightarrow$ ${{\mathit \gamma}}{{\mathit X}}$ in central galactic halo, 10 years of data; limits placed in $\langle \sigma \cdot{}v\rangle $ vs. m(WIMP) plane for m(WIMP): $0.3 - 70$ TeV.
3  AHNEN 2018 search for WIMP WIMP $\rightarrow$ ${{\mathit \gamma}}{{\mathit X}}$ from Ursa Major II; limits set in $\langle \sigma \cdot{}v\rangle $ vs. m(WIMP) plane for ${{\mathit b}}{{\overline{\mathit b}}}$ , ${{\mathit W}^{+}}{{\mathit W}^{-}}$ , ${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$ , and ${{\mathit \mu}^{+}}{{\mathit \mu}^{-}}$ annihilation modes.
4  ALBERT 2018B search for TeV-scale WIMPs with WIMP WIMP $\rightarrow$ ${{\mathit \gamma}}{{\mathit X}}$ in Andromeda galaxy using HAWC Observatory; limits set in $\langle \sigma \cdot{}v\rangle $ vs m(WIMP) plane.
5  CHANG 2018A examine ${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ ${{\mathit b}}{{\overline{\mathit b}}}$ $\rightarrow$ ${{\mathit \gamma}}$ using Fermi Pass 8 data; no signal; require $\langle \sigma \cdot{}v\rangle $ $<$ $10^{-26}$ cm${}^{3}$/s for m(${{\mathit \chi}}$) = 50 GeV.
6  LISANTI 2018 examine Fermi Pass 8 ${{\mathit \gamma}}$-ray data from galaxy groups; report m(WMP) $>$ 30 GeV for annihilation in ${{\mathit b}}{{\overline{\mathit b}}}$ channel.
7  MAZZIOTTA 2018 examine Fermi-LAT electron and positron spectra searching for features originating from DM particles annihilation into ${{\mathit e}^{+}}{{\mathit e}^{-}}$ pairs, from 45 GeV to 2 TeV; no signal found, limits are obtained.
8  AARTSEN 2017C use 1005 days of IceCube data to search for ${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ neutrinos via various annihilation channels. Limits set.
9  ALBERT 2017A maximum sensitivity to thermally averaged annihilation cross-section is for m(WIMP) = 10${}^{5}$ GeV, where they require via ${{\mathit \tau}}{{\mathit \tau}}$ channel, $\langle \sigma \cdot{}v\rangle $ $<$ $5 \times 10^{-25}$ cm${}^{3}$/s assuming NFW halo profile, $\langle \sigma \cdot{}v\rangle $ $<$ $2 \times 10^{-24}$ cm${}^{3}$/s assuming McMillan profile, $\langle \sigma \cdot{}v\rangle $ $<$ $1.2 \times 10^{-23}$ cm${}^{3}$/s assuming Burkert profile.
10  ARCHAMBAULT 2017 set limits for WIMP mass between 100 GeV and 1 TeV on $\langle \sigma \cdot{}v\rangle $ for ${{\mathit W}^{+}}{{\mathit W}^{-}}$ , ${{\mathit Z}}{{\mathit Z}}$ , ${{\mathit b}}{{\overline{\mathit b}}}$ , ${{\mathit s}}{{\overline{\mathit s}}}$ , ${{\mathit u}}{{\overline{\mathit u}}}$ , ${{\mathit d}}{{\overline{\mathit d}}}$ , ${{\mathit t}}{{\overline{\mathit t}}}$ , ${{\mathit e}^{+}}{{\mathit e}^{-}}$ , ${{\mathit g}}{{\mathit g}}$ , ${{\mathit c}}{{\overline{\mathit c}}}$ , ${{\mathit h}}{{\mathit h}}$ , ${{\mathit \gamma}}{{\mathit \gamma}}$ , ${{\mathit \mu}^{+}}{{\mathit \mu}^{-}}$ , ${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$ annihilation channels.
11  AVRORIN 2017 find upper limits for the annhilation cross section in various channels for DM particle mass between 30 GeV and 10 TeV. Strongest upper limits coming from the two neutrino channel require $\langle \sigma \cdot{}v\rangle $ $<$ $6 \times 10^{-20}$ cm${}^{3}$/s in dwarf galaxies and $\langle \sigma \cdot{}v\rangle $ $<$ $7 \times 10^{-21}$ cm${}^{3}$/s in LMC for 5 TeV WIMP mass.
12  BOUDAUD 2017 use data from the spacecraft Voyager 1, beyond the heliopause, and from AMS02 on ${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ ${{\mathit e}^{+}}{{\mathit e}^{-}}$ to require $\langle \sigma \cdot{}v\rangle <1. \times 10^{-28}$ cm${}^{3}$/s for m(${{\mathit \chi}}$) = 10 MeV.
13  AARTSEN 2016D search for GeV ${{\mathit \nu}}$s from WIMP annihilation in galaxy; limits set on $\langle \sigma \cdot{}v\rangle $ in Fig. 6, 7.
14  ABDALLAH 2016 require $\langle \sigma \cdot{}v\rangle $ $<$ $6 \times 10^{-26}$ cm${}^{3}$/s for $\mathit m$(WIMP) = 1.5 TeV from 254 hours observation ( ${{\mathit W}}{{\mathit W}}$ channel) and $<$ $2 \times 10^{-26}$ cm${}^{3}$/s for $\mathit m$(WIMP) = 1.0 TeV in ${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$ channel.
15  ABDALLAH 2016A search for line spectra from WIMP + WIMP $\rightarrow$ ${{\mathit \gamma}}{{\mathit \gamma}}$ in 18 hr HESS data; rule out previous 130 GeV WIMP hint from Fermi-LAT data.
16  AHNEN 2016 require $\langle \sigma \cdot{}v\rangle <3 \times 10^{-26}$ cm${}^{3}$/s for $\mathit m$(WIMP) = 100 GeV ( ${{\mathit W}}{{\mathit W}}$ channel).
17  AVRORIN 2016 require $\langle $s.v$\rangle $ $<$ $1.91 \times 10^{-21}$ cm${}^{3}$/s from WIMP annihilation to ${{\mathit \nu}}$s via ${{\mathit W}}{{\mathit W}}$ channel for $\mathit m$(WIMP) = 1 TeV.
18  CAPUTO 2016 place limits on WIMPs from annihilation to gamma rays in Small Magellanic Cloud using Fermi-LaT data: $\langle \sigma \cdot{}v\rangle <3 \times 10^{-26}$cm${}^{3}$/s for $\mathit m$(WIMP) = 10 GeV.
19  FORNASA 2016 use anisotropies in the ${{\mathit \gamma}}$-ray diffuse emission detected by Fermi-LAT to bound $\langle \sigma \cdot{}v\rangle $ $<$ $10^{-25}$cm${}^{3}$/s for m(WIMP) = 100 GeV in ${{\mathit b}}{{\overline{\mathit b}}}$ channel: see Fig. 28. The limit is driven by dark-matter subhalos in the Milky Way and it refers to their Most Constraining Scenario.
20  LEITE 2016 constrain WIMP annihilation via search for radio emissions from Smith cloud; $\langle \sigma \cdot{}v\rangle $ $<$ $5 \times 10^{-27}$cm${}^{3}$/s in ${{\mathit e}}{{\mathit e}}$ channel for m(WIMP) = 5 GeV.
21  LI 2016 re-analyze Fermi-LAT data on 8 dwarf spheroidals; set limit $\langle \sigma \cdot{}v\rangle <2 \times 10^{-26}$ cm${}^{3}$/s for $\mathit m$(WIMP) = 100 GeV in ${{\mathit b}}{{\overline{\mathit b}}}$ mode with substructures included.
22  LI 2016A constrain $\langle \sigma \cdot{}v\rangle $ $<$ $10^{-25}$cm${}^{3}$/s in ${{\mathit b}}{{\overline{\mathit b}}}$ channel for m(WIMP) = 100 GeV using Fermi-LAT data from M31; see Fig. 6.
23  LIANG 2016 search dwarf spheroidal galaxies, Large Magellanic Cloud, and Small Magellanic Cloud for ${{\mathit \gamma}}$-line in Fermi-LAT data.
24  LU 2016 re-analyze Fermi-LAT and AMS-02 data; require $\langle \sigma \cdot{}v\rangle $ $<10^{-25}$cm${}^{3}$/s for ${\mathit m}_{{{\mathit m}}}$(WIMP) = 1 TeV in ${{\mathit b}}{{\overline{\mathit b}}}$ channel .
25  SHIRASAKI 2016 re-anayze Fermi-LAT extra-galactic data; require $\langle \sigma \cdot{}v\rangle <10^{-23}$cm${}^{3}$/s for $\mathit m$(WIMP) = 1 TeV in ${{\mathit b}}{{\overline{\mathit b}}}$ channel; see Fig. 8.
26  AARTSEN 2015C search for neutrinos from ${{\mathit X}^{0}}$ annihilation in the Galactic halo. See their Figs. 16 and 17, and Table 5 for limits on $\sigma \cdot{}$v for ${{\mathit X}^{0}}$ mass between 100 GeV and 100 TeV.
27  AARTSEN 2015E search for neutrinos from ${{\mathit X}^{0}}$ annihilation in the Galactic center. See their Figs. 7 and 9, and Table 3 for limits on $\sigma \cdot{}$v for ${{\mathit X}^{0}}$ mass between 30 GeV and 10 TeV.
28  ABRAMOWSKI 2015 search for ${{\mathit \gamma}}$ from ${{\mathit X}^{0}}$ annihilation in the Galactic center. See their Fig. 4 for limits on $\sigma \cdot{}$v for ${{\mathit X}^{0}}$ mass between 250 GeV and 10 TeV.
29  ACKERMANN 2015 search for monochromatic ${{\mathit \gamma}}$ from ${{\mathit X}^{0}}$ annihlation in the Galactic halo. See their Fig. 8 and Tables $2 - 4$ for limits on $\sigma \cdot{}$v for ${{\mathit X}^{0}}$ mass between 0.2 GeV and 500 GeV.
30  ACKERMANN 2015A search for ${{\mathit \gamma}}$ from ${{\mathit X}^{0}}$ annihilation (both Galactic and extragalactic) in the isotropic ${{\mathit \gamma}}$ background. See their Fig. 7 for limits on $\sigma \cdot{}$v for ${{\mathit X}^{0}}$ mass between 10 GeV and 30 TeV.
31  ACKERMANN 2015B search for ${{\mathit \gamma}}$ from ${{\mathit X}^{0}}$ annihilation in 15 dwarf spheroidal satellite galaxies of the Milky Way. See their Figs. 1 and 2 for limits on $\sigma \cdot{}$v for ${{\mathit X}^{0}}$ mass between 2 GeV and 10 TeV.
32  ADRIAN-MARTINEZ 2015 search for neutrinos from ${{\mathit X}^{0}}$ annihilation in the Galactic center. See their Figs. 10 and 11 and Tables 1 and 2 for limits on $\sigma \cdot{}$v for ${{\mathit X}^{0}}$ mass between 25 GeV and 10 TeV.
33  ACKERMANN 2014 search for ${{\mathit \gamma}}$ from ${{\mathit X}^{0}}$ annihilation in 25 dwarf spheroidal satellite galaxies of the Milky Way. See their Tables II--VII for limits assuming annihilation into ${{\mathit e}^{+}}{{\mathit e}^{-}}$ , ${{\mathit \mu}^{+}}{{\mathit \mu}^{-}}$ , ${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$ , ${{\mathit u}}{{\overline{\mathit u}}}$ , ${{\mathit b}}{{\overline{\mathit b}}}$ , and ${{\mathit W}^{+}}{{\mathit W}^{-}}$ , for ${{\mathit X}^{0}}$ mass ranging from 2 GeV to 10 TeV.
34  Limit assuming ${{\mathit X}^{0}}$ pair annihilation into ${{\mathit b}}{{\overline{\mathit b}}}$ .
35  Limit assuming ${{\mathit X}^{0}}$ pair annihilation into ${{\mathit W}^{+}}{{\mathit W}^{-}}$ .
36  ALEKSIC 2014 search for ${{\mathit \gamma}}$ from ${{\mathit X}^{0}}$ annihilation in the dwarf spheroidal galaxy Segue 1. The listed limit assumes annihilation into ${{\mathit W}^{+}}{{\mathit W}^{-}}$ . See their Figs. 6, 7, and 16 for limits on $\sigma \cdot{}$v for annihilation channels ${{\mathit \mu}^{+}}{{\mathit \mu}^{-}}$ , ${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$ , ${{\mathit b}}{{\overline{\mathit b}}}$ , ${{\mathit t}}{{\overline{\mathit t}}}$ , ${{\mathit \gamma}}{{\mathit \gamma}}$ , ${{\mathit \gamma}}{{\mathit Z}}$ , ${{\mathit W}^{+}}{{\mathit W}^{-}}$ , ${{\mathit Z}}{{\mathit Z}}$ for ${{\mathit X}^{0}}$ mass between and $10^{4}$ GeV.
37  AARTSEN 2013C search for neutrinos from ${{\mathit X}^{0}}$ annihilation in nearby galaxies and galaxy clusters. See their Figs. $5 - 7$ for limits on $\sigma \cdot{}$v for ${{\mathit X}^{0}}$ ${{\mathit X}^{0}}$ $\rightarrow$ ${{\mathit \nu}}{{\overline{\mathit \nu}}}$ , ${{\mathit \mu}^{+}}{{\mathit \mu}^{-}}$ , ${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$ , and ${{\mathit W}^{+}}{{\mathit W}^{-}}$ for ${{\mathit X}^{0}}$ mass between 300 GeV and 100 TeV.
38  ABRAMOWSKI 2013 search for monochromatic ${{\mathit \gamma}}$ from ${{\mathit X}^{0}}$ annihilation in the Milky Way halo in the central region. Limit on $\sigma \cdot{}$v between $10^{-28}$ and $10^{-25}$ cm${}^{3}$ s${}^{-1}$ (95$\%$ CL) is obtained for ${{\mathit X}^{0}}$ mass between 500 GeV and 20 TeV for ${{\mathit X}^{0}}$ ${{\mathit X}^{0}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit \gamma}}$ . ${{\mathit X}^{0}}$ density distribution in the Galaxy by Einasto is assumed. See their Fig. 4.
39  ACKERMANN 2013A search for monochromatic ${{\mathit \gamma}}$ from ${{\mathit X}^{0}}$ annihilation in the Milky Way. Limit on $\sigma \cdot{}$v for the process ${{\mathit X}^{0}}$ ${{\mathit X}^{0}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit \gamma}}$ in the range $10^{-29} - 10^{-27}$ cm${}^{3}$ s${}^{-1}$ (95$\%$ CL) is obtained for ${{\mathit X}^{0}}$ mass between 5 and 300 GeV. The limit depends slightly on the assumed density profile of ${{\mathit X}^{0}}$ in the Galaxy. See their Tables VII$−$X and Fig.10. Supersedes ACKERMANN 2012 .
40  ABRAMOWSKI 2012 search for ${{\mathit \gamma}}$'s from ${{\mathit X}^{0}}$ annihilation in the Fornax galaxy cluster. See their Fig. 7 for limits on $\sigma \cdot{}$v for ${{\mathit X}^{0}}$ mass between 0.1 and 100 TeV for the annihilation channels ${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$ , ${{\mathit b}}{{\overline{\mathit b}}}$ , and ${{\mathit W}^{+}}{{\mathit W}^{-}}$ .
41  ACKERMANN 2012 search for monochromatic ${{\mathit \gamma}}$ from ${{\mathit X}^{0}}$ annihilation in the Milky Way. Limit on $\sigma \cdot{}$v in the range $10^{-28} - 10^{-26}$ cm${}^{3}$s${}^{-1}$ (95$\%$ CL) is obtained for ${{\mathit X}^{0}}$ mass between 7 and 200 GeV if ${{\mathit X}^{0}}$ annihilates into ${{\mathit \gamma}}{{\mathit \gamma}}$ . The limit depends slightly on the assumed density profile of ${{\mathit X}^{0}}$ in the Galaxy. See their Table III and Fig. 15.
42  ACKERMANN 2012 search for ${{\mathit \gamma}}$ from ${{\mathit X}^{0}}$ annihilation in the Milky Way in the diffuse ${{\mathit \gamma}}$ background. Limit on $\sigma \cdot{}$v of $10^{-24}$ cm${}^{3}$s${}^{-1}$ or larger is obtained for ${{\mathit X}^{0}}$ mass between 5 GeV and 10 TeV for various annihilation channels including ${{\mathit W}^{+}}{{\mathit W}^{-}}$ , ${{\mathit b}}{{\overline{\mathit b}}}$ , ${{\mathit g}}{{\mathit g}}$ , ${{\mathit e}^{+}}{{\mathit e}^{-}}$ , ${{\mathit \mu}^{+}}{{\mathit \mu}^{-}}$ , ${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$ . The limit depends slightly on the assumed density profile of ${{\mathit X}^{0}}$ in the Galaxy. See their Figs. $17 - 20$.
43  ALIU 2012 search for ${{\mathit \gamma}}$'s from ${{\mathit X}^{0}}$ annihilation in the dwarf spheroidal galaxy Segue 1. Limit on $\sigma \cdot{}$v in the range $10^{-24} - 10^{-20}$ cm${}^{3}$s${}^{-1}$ (95$\%$ CL) is obtained for ${{\mathit X}^{0}}$ mass between 10 GeV and 2 TeV for annihilation channels ${{\mathit e}^{+}}{{\mathit e}^{-}}$ , ${{\mathit \mu}^{+}}{{\mathit \mu}^{-}}$ , ${{\mathit \tau}^{+}}{{\mathit \tau}^{-}}$ , ${{\mathit b}}{{\overline{\mathit b}}}$ , and ${{\mathit W}^{+}}{{\mathit W}^{-}}$ . See their Fig. 3.
44  ABBASI 2011C search for ${{\mathit \nu}_{{\mu}}}$ from ${{\mathit X}^{0}}$ annihilation in the outer halo of the Milky Way. The limit assumes annihilation into ${{\mathit \nu}}{{\mathit \nu}}$ . See their Fig. 9 for limits with other annihilation channels.
45  ABRAMOWSKI 2011 search for ${{\mathit \gamma}}$ from ${{\mathit X}^{0}}$ annihilation near the Galactic center. The limit assumes Einasto DM density profile.
46  ACKERMANN 2011 search for ${{\mathit \gamma}}$ from ${{\mathit X}^{0}}$ annihilation in ten dwarf spheroidal satellite galaxies of the Milky Way. The limit for $\mathit m$ = 10 GeV assumes annihilation into ${{\mathit b}}{{\overline{\mathit b}}}$ , the others ${{\mathit W}^{+}}{{\mathit W}^{-}}$ . See their Fig. 2 for limits with other final states. See also GERINGER-SAMETH 2011 for a different analysis of the same data.
  References:
CHEUNG 2019
PL B789 137 The impact of EDGES 21-cm data on dark matter interactions
ABDALLAH 2018
PRL 120 201101 Search for $\gamma$-Ray Line Signals from Dark Matter Annihilations in the Inner Galactic Halo from 10 Years of Observations with H.E.S.S.
AHNEN 2018
JCAP 1803 009 Indirect dark matter searches in the dwarf satellite galaxy Ursa Major II with the MAGIC Telescopes
ALBERT 2018B
JCAP 1806 043 Search for Dark Matter Gamma-ray Emission from the Andromeda Galaxy with the High-Altitude Water Cherenkov Observatory
CHANG 2018A
PR D98 123004 Search for dark matter annihilation in the Milky Way halo
LISANTI 2018
PRL 120 101101 Search for Dark Matter Annihilation in Galaxy Groups
MAZZIOTTA 2018
PR D98 022006 Search for features in the cosmic-ray electron and positron spectrum measured by the Fermi Large Area Telescope
AARTSEN 2017C
EPJ C77 627 Search for Neutrinos from Dark Matter Self-Annihilations in the Center of the Milky Way with 3 Years of IceCube/DeepCore
ALBERT 2017A
PL B769 249 Results from the Search for Dark Matter in the Milky Way with 9 Years of Data of the ANTARES Neutrino Telescope
ARCHAMBAULT 2017
PR D95 082001 Dark Matter Constraints from a Joint Analysis of Dwarf Spheroidal Galaxy Observations with VERITAS
AVRORIN 2017
JETP 125 80 Dark Matter Constraints from an Observation of dSphs (dwarf spheroidal galaxies) and the LMC (Large Magellanic Cloud) with the Baikal NT200
BOUDAUD 2017
PRL 119 021103 Novel Cosmic-ray Electron and Positron Constraints on MeV Dark Matter Particles
AARTSEN 2016D
EPJ C76 531 All-flavour Search for Neutrinos from Dark Matter Annihilations in the Milky Way with IceCube/DeepCore
ABDALLAH 2016A
PRL 117 151302 H.E.S.S. Limits on Linelike Dark Matter Signatures in the 100 GeV to 2 TeV Energy Range Close to the Galactic Center
ABDALLAH 2016
PRL 117 111301 Search for Dark Matter Annihilations Towards the Inner Galactic Halo from 10 Years of Observations with H.E.S.S
AHNEN 2016
JCAP 1602 039 Limits to Dark Matter Annihilation Cross-Section from a Combined Analysis of MAGIC and Fermi-LAT Observations of Dwarf Satellite Galaxies
AVRORIN 2016
ASP 81 12 A Search for Neutrino Signal from Dark Matter Annihilation in the Center of the Milky Way with Baikal NT200
CAPUTO 2016
PR D93 062004 Search for Gamma-ray Emission from Dark Matter Annihilation in the Small Magellanic Cloud with the Fermi Large Area Telescope
FORNASA 2016
PR D94 123005 Angular Power Spectrum of the Diffuse Gamma-Ray Emission as Measured by the Fermi Large Area Telescope and Constraints on its Dark Matter Interpretation
LEITE 2016
JCAP 1611 021 Synchrotron Emission from Dark Matter in Galactic Subhalos. A Look into the Smith Cloud
LI 2016
PR D93 043518 Search for Gamma-Ray Emission from Eight dwarf Spheroidal Galaxy Candidates Discovered in Year Two of Dark Energy Survey with Fermi-LAT Data
LI 2016A
JCAP 1612 028 Constraints on the Dark Matter Annihilation from Fermi-LAT Observation of M31
LIANG 2016
PR D94 103502 Search for Gamma-Ray Line Features from Milky Way Satellites with Fermi LAT Pass 8 Data
LU 2016
PR D93 103517 Limits on Dark Matter from AMS-02 Antiproton and Positron Fraction Data
SHIRASAKI 2016
PR D94 063522 Cosmological Constraints on Dark Matter Annihilation and Decay: Cross-Correlation Analysis of the Extragalactic ${{\mathit \gamma}}$-ray Background and Cosmic Shear
AARTSEN 2015C
EPJ C75 20 Multipole Analysis of IceCube Data to Search for Dark Matter Accumulated in the Galactic Halo
AARTSEN 2015E
EPJ C75 492 Search for Dark Matter Annihilation in the Galactic Center with IceCube-79
ABRAMOWSKI 2015
PRL 114 081301 Constraints on an Annihilation Signal from a Core of Constant Dark Matter Density around the Milky Way Center with H.E.S.S.
ACKERMANN 2015A
JCAP 1509 008 Limits on Dark Matter Annihilation Signals from the Fermi LAT 4-year Measurement of the Isotropic Gamma-Ray Background
ACKERMANN 2015
PR D91 122002 Updated Search for Spectral Lines from Galactic Dark Matter Interactions with Pass 8 Data from the Fermi Large Area Telescope
ACKERMANN 2015B
PRL 115 231301 Searching for Dark Matter Annihilation from Milky Way Dwarf Spheroidal Galaxies with Six Years of Fermi Large Area Telescope Data
ADRIAN-MARTINEZ 2015
JCAP 1510 068 Search of Dark Matter Annihilation in the Galactic Centre using the ANTARES Neutrino Telescope
ACKERMANN 2014
PR D89 042001 Dark Matter Constraints from Observations of 25 Milky Way Satellite Galaxies with the Fermi Large Area Telescope
ALEKSIC 2014
JCAP 1402 008 Optimized Dark Matter Searches in Deep Observations of Segue 1 with MAGIC
AARTSEN 2013C
PR D88 122001 IceCube Search for Dark Matter Annihilation in Nearby Galaxies and Galaxy Clusters
ABRAMOWSKI 2013
PRL 110 041301 Search for Photon Line-Like Signatures from Dark Matter Annihilations with H.E.S.S
ACKERMANN 2013A
PR D88 082002 Search for Gamma-Ray Spectral Lines with the Fermi Large Area Telescope and Dark Matter Implications
ABRAMOWSKI 2012
APJ 750 123 Search for Dark Matter Annihilation Signals from the Fornax Galaxy Cluster with H.E.S.S
ACKERMANN 2012
PR D86 022002 Fermi LAT (Large Area Telescope) Search for Dark Matter in Gamma-Ray Lines and the Inclusive Photon Spectrum
ALIU 2012
PR D85 062001 VERITAS Deep Observations of the Dwarf Spheroidal Galaxy Segue 1
ABBASI 2011C
PR D84 022004 Search for Dark Matter from the Galactic Halo with the IceCube Neutrino Telescope
ABRAMOWSKI 2011
PRL 106 161301 Search for a Dark Matter Annihilation Signal from the Galactic Center Halo with H.E.S.S.
ACKERMANN 2011
PRL 107 241302 Constraining Dark Matter Models from a Combined Analysis of Milky Way Satellites with the Fermi Large Area Telescope