# ${{\boldsymbol X}^{0}}$ 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. • • •
1
 2019
HAWC DM annihilation to ${{\mathit \gamma}}$s within galactic substructure
$<0.8 \times 10^{-22}$ 95 2
 2019 B
HAWC annihilation/decay to ${{\mathit \gamma}}$ in M31
$<4 \times 10^{-26}$ 95 3
 2019
${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ ${{\mathit e}^{+}}{{\mathit e}^{-}}$ and ${{\mathit b}}{{\overline{\mathit b}}}$
$<7 \times 10^{-27}$ 95 4
 2019
FLAT Fermi-LAT M31 and M33
5
 2019
FLAT ${\mathit P}{\mathrm -wave}$ DM; Fermi-LAT
$<2 \times 10^{-26}$ 95 6
 2019 D
FLAT ${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ ${{\mathit \gamma}}$
$<1 \times 10^{-32}$ 7
 2019
sterile ${{\mathit \nu}}$ decay/annihilation
8
 2019
semi-annihilating DM
$<4 \times 10^{-28}$ 95 9
 2018
HESS ${{\mathit X}^{0}}$ ${{\mathit X}^{0}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit X}}$ ; galactic halo
$<1 \times 10^{-23}$ 95 10
 2018
MGIC ${{\mathit X}^{0}}$ ${{\mathit X}^{0}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit X}}$ ; Ursa Major II
$<1 \times 10^{-22}$ 95 11
 2018 B
HAWC ${{\mathit X}^{0}}$ ${{\mathit X}^{0}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit X}}$ ; Andromeda
$<1 \times 10^{-26}$ 95 12
 2018 A
${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ ${{\mathit b}}{{\overline{\mathit b}}}$ $\rightarrow$ ${{\mathit \gamma}}$
13
 2018
THEO Fermi, ${{\mathit \gamma}}$; galaxy groups
14
 2018
FLAT Fermi-LAT CRE data
$<1.2 \times 10^{-23}$ 95 15
 2017 C
ICCB ${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ neutrinos
$<1 \times 10^{-23}$ 90 16
 2017 A
ANTR ${{\mathit \nu}}$, DM annihilation
$<1.32 \times 10^{-25}$ 95 17
 2017
VRTS ${{\mathit \gamma}}$ dwarf galaxies
$<7 \times 10^{-21}$ 90 18
 2017
BAIK cosmic ${{\mathit \nu}}$
$<1 \times 10^{-28}$ 19
 2017
MeV DM to ${{\mathit e}^{+}}{{\mathit e}^{-}}$
20
 2016 D
ICCB ${{\mathit \nu}}$, galactic center
$<6 \times 10^{-26}$ 95 21
 2016
HESS Central Galactic Halo
$<1 \times 10^{-27}$ 95 22
 2016 A
HESS WIMP+WIMP $\rightarrow$ ${{\mathit \gamma}}{{\mathit \gamma}}$ ; galactic center
$<3 \times 10^{-26}$ 95 23
 2016
MGFL Satellite galaxy, $\mathit m$(WIMP)=100 GeV
$<1.9 \times 10^{-21}$ 90 24
 2016
BAIK ${{\mathit \nu}}$s from galactic center
$<3 \times 10^{-26}$ 95 25
 2016
FLAT small Magellanic cloud
$<1 \times 10^{-25}$ 95 26
 2016
FLAT Fermi-LAT ${{\mathit \gamma}}$-ray anisotropy
$<5 \times 10^{-27}$ 27
 2016
$<2 \times 10^{-26}$ 95 28
 2016
FLAT dwarf galaxies
$<1 \times 10^{-25}$ 95 29
 2016 A
FLAT Fermi-LAT; M31
$<1 \times 10^{-26}$ 30
 2016
FLAT Fermi-LAT, gamma line
$<1 \times 10^{-25}$ 95 31
 2016
FLAT Fermi-LAT and AMS-02
$<1 \times 10^{-23}$ 95 32
 2016
FLAT extra galactic
33
 2015 C
ICCB ${{\mathit \nu}}$, Galactic halo
34
 2015 E
ICCB ${{\mathit \nu}}$, Galactic center
35
 2015
HESS Galactic center
36
 2015
FLAT monochromatic ${{\mathit \gamma}}$
37
 2015 A
FLAT isotropic ${{\mathit \gamma}}$ background
38
 2015 B
FLAT Satellite galaxy
39
 2015
ANTR ${{\mathit \nu}}$, Galactic center
$<2.90 \times 10^{-26}$ 95 40, 41
 2014
FLAT Satellite galaxy, $\mathit m$ = 10 GeV
$<1.84 \times 10^{-25}$ 95 40, 42
 2014
FLAT Satellite galaxy, $\mathit m$ = 100 GeV
$<1.75 \times 10^{-24}$ 95 40, 42
 2014
FLAT Satellite galaxy, $\mathit m$ = 1 TeV
$<4.52 \times 10^{-24}$ 95 43
 2014
MGIC Segue 1, $\mathit m$ = 1.35 TeV
44
 2013 C
ICCB Galaxies
45
 2013
HESS Central Galactic Halo
46
 2013 A
FLAT Galaxy
47
 2012
HESS Fornax Cluster
48
 2012
FLAT Galaxy
49
 2012
FLAT Galaxy
50
 2012
VRTS Segue 1
$<1 \times 10^{-22}$ 90 51
 2011 C
ICCB Galactic halo, $\mathit m$=1 TeV
$<3 \times 10^{-25}$ 95 52
 2011
HESS Near Galactic center, $\mathit m$=1 TeV
$<1 \times 10^{-26}$ 95 53
 2011
FLAT Satellite galaxy, $\mathit m$=10 GeV
$<1 \times 10^{-25}$ 95 53
 2011
FLAT Satellite galaxy, $\mathit m$=100 GeV
$<1 \times 10^{-24}$ 95 53
 2011
FLAT Satellite galaxy, $\mathit m$=1 TeV
1  ABEYSEKARA 2019 search for ${{\mathit \gamma}}$s from DM annihilation in galactic substructures with HAWC; no signal, limits placed in J$\langle \sigma \cdot{}v\rangle$ vs. declination plane for m(DM) $\sim{}$ $1 - 108$ TeV.
2  ALBERT 2019B search for DM signal from M31 galaxy in ${{\mathit \mu}}$, ${{\mathit \tau}}$, ${{\mathit t}}$, ${{\mathit b}}$, ${{\mathit W}}$ channels using HAWC for m(DM) $\sim{}$ $1 - 100$ TeV; no signal, limits placed in $\langle \sigma \cdot{}v\rangle$ vs. m(DM) plane.
3  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).
4  DI-MAURO 2019 place limits on WIMP annihilation via Fermi-LAT observation of M31 and M33 galaxies: $\langle \sigma \cdot{}v\rangle$ $<$ $7 \times 10^{-27}$cm${}^{3}$/s for m(${{\mathit \chi}}$) = 20 GeV from M31.
5  JOHNSON 2019 search for ${{\mathit \gamma}}$-rays, $10 - 600$ GeV energy, from ${\mathit P}{\mathrm -wave}$ annihilating DM around SgrA* BH using Fermi-LAT; limits set for various models.
6  LI 2019D search for ${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ ${{\mathit \gamma}}$ in Fermi-LAT data; no signal, require $\langle \sigma \cdot{}v\rangle$ $<$ $2 \times 10^{-26}$ cm${}^{3}$/s for m(${{\mathit \chi}}$) = 100 GeV.
7  NG 2019 search for X-ray line from sterile ${{\mathit \nu}}$ decay/annihilation using NuStar M-31; no signal: limits placed in m(${{\mathit \nu}}$) vs mixing angle and $\langle \sigma \cdot{}v\rangle$ vs m(${{\mathit \nu}}$).
8  QUEIROZ 2019 examine ${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ ${{\mathit \chi}}{{\mathit SM}}$ semi-annihilation of DM reaction; limits placed for various assumed ${{\mathit SM}}$ particles in $\langle \sigma \cdot{}v\rangle$ vs. m(${{\mathit \chi}}$) plane.
9  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.
10  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.
11  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.
12  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.
13  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.
14  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.
15  AARTSEN 2017C use 1005 days of IceCube data to search for ${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ neutrinos via various annihilation channels. Limits set.
16  ALBERT 2017A search for DM annihilation to ${{\mathit \nu}}$s using ANTARES data from $2007 - 2015$. No signal. Limits set in $\langle \sigma \cdot{}v\rangle$ vs. m(DM) plane for m(DM) $\sim{}10 - 10 \times 10^{5}$ GeV. The listed limit is for m(DM) = 100 TeV.
17  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.
18  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.
19  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.
20  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.
21  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.
22  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.
23  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).
24  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.
25  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.
26  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.
27  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.
28  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.
29  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.
30  LIANG 2016 search dwarf spheroidal galaxies, Large Magellanic Cloud, and Small Magellanic Cloud for ${{\mathit \gamma}}$-line in Fermi-LAT data.
31  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 .
32  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.
33  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.
34  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.
35  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.
36  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.
37  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.
38  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.
39  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.
40  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.
41  Limit assuming ${{\mathit X}^{0}}$ pair annihilation into ${{\mathit b}}{{\overline{\mathit b}}}$ .
42  Limit assuming ${{\mathit X}^{0}}$ pair annihilation into ${{\mathit W}^{+}}{{\mathit W}^{-}}$ .
43  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.
44  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.
45  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.
46  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 .
47  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 ${{\mathit W}^{+}}{{\mathit W}^{-}}$ .
48  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.
49  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. $17 - 20$.
50  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.
51  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.
52  ABRAMOWSKI 2011 search for ${{\mathit \gamma}}$ from ${{\mathit X}^{0}}$ annihilation near the Galactic center. The limit assumes Einasto DM density profile.
53  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:
 ABEYSEKARA 2019
JCAP 1907 022 Searching for Dark Matter Sub-structure with HAWC
 ALBERT 2019B
JCAP 1904 E01 Search for Dark Matter Gamma-ray Emission from the Andromeda Galaxy with the High-Altitude Water Cherenkov Observatory
 CHEUNG 2019
PL B789 137 The impact of EDGES 21-cm data on dark matter interactions
 DI-MAURO 2019
PR D99 123027 Search for $\gamma$-ray emission from dark matter particle interactions from Andromeda and Triangulum Galaxies with the Fermi Large Area Telescope
 JOHNSON 2019
PR D99 103007 Search for gamma-ray emission from $p$-wave dark matter annihilation in the Galactic Center
 LI 2019D
PR D99 123519 Search for line-like signals in the all-sky Fermi-LAT data
 NG 2019
PR D99 083005 New Constraints on Sterile Neutrino Dark Matter from $NuSTAR$ M31 Observations
 QUEIROZ 2019
JCAP 1904 048 Search for Semi-Annihilating Dark Matter with Fermi-LAT, H.E.S.S., Planck, and the Cherenkov Telescope Array
 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
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PL B769 249 Results from the Search for Dark Matter in the Milky Way with 9 Years of Data of the ANTARES Neutrino Telescope
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PR D95 082001 Dark Matter Constraints from a Joint Analysis of Dwarf Spheroidal Galaxy Observations with VERITAS
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PRL 119 021103 Novel Cosmic-ray Electron and Positron Constraints on MeV Dark Matter Particles
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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
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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
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 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
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 ACKERMANN 2015A
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 ACKERMANN 2015B
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 ACKERMANN 2015
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 ALEKSIC 2014
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 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
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 ABRAMOWSKI 2011
PRL 106 161301 Search for a Dark Matter Annihilation Signal from the Galactic Center Halo with H.E.S.S.
 ACKERMANN 2011
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