${{\mathit X}^{0}}$ Annihilation Cross Section

INSPIRE   PDGID:
S030DMA
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. • •
$<1.2 \times 10^{-26}$ 95 1
ABDALLA
2022
HESS DM annihilation to gamma rays
2
ALBERT
2022A
 ANTR PeV-scale DM search
$<1 \times 10^{-27}$ 3
CHAN
2022
DM annihilation from Omega Centauri X-rays
$<3 \times 10^{-26}$ 4
EGOROV
2022
DM annihilation to radio waves from M31
5
MANCONI
2022
polarized synchrotron emission from DM annihilation via Planck
$<5 \times 10^{-24}$ 95 6
ABDALLAH
2021
HESS WIMP annihilation in dwarf irregular galaxy
7
CIRELLI
2021
light DM annihilation producing X-rays
8
JOHN
2021
cosmic positron spectra limits on leptophilic DM
$<2.5 \times 10^{-27}$ 95 9
ABAZAJIAN
2020
FLAT ${{\mathit \gamma}}$ from galactic center
10
ABDALLAH
2020
HESS WIMP annihilation in dwarf satellite galaxies
$<1.2 \times 10^{-24}$ 90 11
ABE
2020G
 SKAM WIMP annihilation to neutrinos
$<2.2 \times 10^{-24}$ 95 12
ALBERT
2020
HAWC WIMP annihilation to ${{\mathit \gamma}}$
$<5 \times 10^{-24}$ 90 13
ALBERT
2020A
 ANTR WIMP annihilation to ${{\mathit \nu}}$s in galactic center
$<1 \times 10^{-23}$ 90 14
ALBERT
2020C
 ANTR Antares/IceCube search for WIMP annihilation to ${{\mathit \nu}}$s
$<8 \times 10^{-26}$ 15
ALVAREZ
2020
FLAT dwarf spheroidal; J-distribution
$<2 \times 10^{-26}$ 90 16
HOOF
2020
FLAT WIMP annihilation to ${{\mathit \gamma}}$
17
MAZZIOTTA
2020
FLAT DM annihilation in Sun to ${{\mathit \gamma}}$
18
ABEYSEKARA
2019
HAWC DM annihilation to ${{\mathit \gamma}}$s within galactic substructure
$<0.8 \times 10^{-22}$ 95 19
ALBERT
2019B
 HAWC annihilation/decay to ${{\mathit \gamma}}$ in M31
$<4 \times 10^{-26}$ 95 20
CHEUNG
2019
EDGS ${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ ${{\mathit e}^{+}}{{\mathit e}^{-}}$ and ${{\mathit b}}{{\overline{\mathit b}}}$
$<7 \times 10^{-27}$ 95 21
DI-MAURO
2019
FLAT Fermi-LAT M31 and M33
22
JOHNSON
2019
FLAT ${\mathit P}{\mathrm -wave}$ DM; Fermi-LAT
$<2 \times 10^{-26}$ 95 23
LI
2019D
 FLAT ${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ ${{\mathit \gamma}}$
$<1 \times 10^{-32}$ 24
NG
2019
sterile ${{\mathit \nu}}$ decay/annihilation
25
QUEIROZ
2019
semi-annihilating DM
$<4 \times 10^{-28}$ 95 26
ABDALLAH
2018
HESS ${{\mathit X}^{0}}$ ${{\mathit X}^{0}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit X}}$ ; galactic halo
$<1 \times 10^{-23}$ 95 27
AHNEN
2018
MGIC ${{\mathit X}^{0}}$ ${{\mathit X}^{0}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit X}}$ ; Ursa Major II
$<1 \times 10^{-22}$ 95 28
ALBERT
2018B
 HAWC ${{\mathit X}^{0}}$ ${{\mathit X}^{0}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit X}}$ ; Andromeda
$<1 \times 10^{-26}$ 95 29
CHANG
2018A
 ${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ ${{\mathit b}}{{\overline{\mathit b}}}$ $\rightarrow$ ${{\mathit \gamma}}$
30
LISANTI
2018
THEO Fermi, ${{\mathit \gamma}}$; galaxy groups
31
MAZZIOTTA
2018
FLAT Fermi-LAT CRE data
$<1.2 \times 10^{-23}$ 95 32
AARTSEN
2017C
 ICCB ${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ neutrinos
$<1 \times 10^{-23}$ 90 33
ALBERT
2017A
 ANTR ${{\mathit \nu}}$, DM annihilation
$<1.32 \times 10^{-25}$ 95 34
ARCHAMBAULT
2017
VRTS ${{\mathit \gamma}}$ dwarf galaxies
$<7 \times 10^{-21}$ 90 35
AVRORIN
2017
BAIK cosmic ${{\mathit \nu}}$
$<1 \times 10^{-28}$ 36
BOUDAUD
2017
MeV DM to ${{\mathit e}^{+}}{{\mathit e}^{-}}$
37
AARTSEN
2016D
 ICCB ${{\mathit \nu}}$, galactic center
$<6 \times 10^{-26}$ 95 38
ABDALLAH
2016
HESS Central Galactic Halo
$<1 \times 10^{-27}$ 95 39
ABDALLAH
2016A
 HESS WIMP+WIMP $\rightarrow$ ${{\mathit \gamma}}{{\mathit \gamma}}$ ; galactic center
$<3 \times 10^{-26}$ 95 40
AHNEN
2016
MGFL Satellite galaxy, $\mathit m$(WIMP)=100 GeV
$<1.9 \times 10^{-21}$ 90 41
AVRORIN
2016
BAIK ${{\mathit \nu}}$s from galactic center
$<3 \times 10^{-26}$ 95 42
CAPUTO
2016
FLAT small Magellanic cloud
$<1 \times 10^{-25}$ 95 43
FORNASA
2016
FLAT Fermi-LAT ${{\mathit \gamma}}$-ray anisotropy
$<5 \times 10^{-27}$ 44
LEITE
2016
WIMP, radio
$<2 \times 10^{-26}$ 95 45
LI
2016
FLAT dwarf galaxies
$<1 \times 10^{-25}$ 95 46
LI
2016A
 FLAT Fermi-LAT; M31
$<1 \times 10^{-26}$ 47
LIANG
2016
FLAT Fermi-LAT, gamma line
$<1 \times 10^{-25}$ 95 48
LU
2016
FLAT Fermi-LAT and AMS-02
$<1 \times 10^{-23}$ 95 49
SHIRASAKI
2016
FLAT extra galactic
50
AARTSEN
2015C
 ICCB ${{\mathit \nu}}$, Galactic halo
51
AARTSEN
2015E
 ICCB ${{\mathit \nu}}$, Galactic center
52
ABRAMOWSKI
2015
HESS Galactic center
53
ACKERMANN
2015
FLAT monochromatic ${{\mathit \gamma}}$
54
ACKERMANN
2015A
 FLAT isotropic ${{\mathit \gamma}}$ background
55
ACKERMANN
2015B
 FLAT Satellite galaxy
56
ADRIAN-MARTIN..
2015
ANTR ${{\mathit \nu}}$, Galactic center
$<2.90 \times 10^{-26}$ 95 57, 58
ACKERMANN
2014
FLAT Satellite galaxy, $\mathit m$ = 10 GeV
$<1.84 \times 10^{-25}$ 95 57, 59
ACKERMANN
2014
FLAT Satellite galaxy, $\mathit m$ = 100 GeV
$<1.75 \times 10^{-24}$ 95 57, 59
ACKERMANN
2014
FLAT Satellite galaxy, $\mathit m$ = 1 TeV
$<4.52 \times 10^{-24}$ 95 60
ALEKSIC
2014
MGIC Segue 1, $\mathit m$ = 1.35 TeV
61
AARTSEN
2013C
 ICCB Galaxies
62
ABRAMOWSKI
2013
HESS Central Galactic Halo
63
ACKERMANN
2013A
 FLAT Galaxy
64
ABRAMOWSKI
2012
HESS Fornax Cluster
65
ACKERMANN
2012
FLAT Galaxy
66
ACKERMANN
2012
FLAT Galaxy
67
ALIU
2012
VRTS Segue 1
$<1 \times 10^{-22}$ 90 68
ABBASI
2011C
 ICCB Galactic halo, $\mathit m$=1 TeV
$<3 \times 10^{-25}$ 95 69
ABRAMOWSKI
2011
HESS Near Galactic center, $\mathit m$=1 TeV
$<1 \times 10^{-26}$ 95 70
ACKERMANN
2011
FLAT Satellite galaxy, $\mathit m$=10 GeV
$<1 \times 10^{-25}$ 95 70
ACKERMANN
2011
FLAT Satellite galaxy, $\mathit m$=100 GeV
$<1 \times 10^{-24}$ 95 70
ACKERMANN
2011
FLAT Satellite galaxy, $\mathit m$=1 TeV
1  ABDALLA 2022 search for WIMP annihilation in galactic center to gamma rays using HESS; no signal observed; limits set in mass vs $\langle \sigma \cdot{}v\rangle $ plane for dominant annihilation to ${{\mathit W}}{{\mathit W}}$ or ${{\mathit \tau}}{{\overline{\mathit \tau}}}$ . Limit here for ${{\mathit \tau}}{{\overline{\mathit \tau}}}$ channel 0.7 TeV mass.
2  ALBERT 2022A search for secluded PeV-scale DM annihilation to four final states; no signal detected; limits placed in $\langle \sigma \cdot{}v\rangle $ vs. m(${{\mathit \chi}}$) plane for m(${{\mathit \chi}}$): $6 - 6000$ TeV for m(mediator) = 50, 250, and 1000 GeV.
3  CHAN 2022 derive a variety of limits on DM annihilation to various channels resulting in X-rays from dwarf galaxy Omega Centauri. Limits are very dependent on assumed DM density and diffusion coefficient. Quoted limit is for m(WIMP) = 100 GeV annihilating to ${{\mathit W}}{{\mathit W}}$ with parameters as in Fig. 4.
4  EGOROV 2022 derives limits on DM annihlation to ${{\mathit b}}{{\overline{\mathit b}}}$ or ${{\mathit \tau}}{{\overline{\mathit \tau}}}$ via radio signals from M31; quoted limit from ${{\mathit b}}{{\overline{\mathit b}}}$ channel with LOFAR telescope as main data source, using parameters as in Fig. 10 (green curve) for m(${{\mathit \chi}}$) = 100 GeV.
5  MANCONI 2022 use polarized synchrotron emission data from Planck to constrain WIMP annihilation cross section in Galaxy; limits set in $\langle \sigma \cdot{}v\rangle $ vs. m(DM) plane.
6  ABDALLAH 2021 search for WIMP-WIMP annihilation into 2 monoenergetic ${{\mathit \gamma}}$ rays in WLM dwarf irregular galaxy using HESS data. No signal. Limits placed in $\langle \sigma \cdot{}v\rangle $ vs. m(WIMP) plane for a mass of 370 GeV.
7  CIRELLI 2021 derive limits on light DM annihilation to ${{\mathit e}}{{\mathit e}}$ , ${{\mathit \mu}}{{\mathit \mu}}$ , ${{\mathit \pi}}{{\mathit \pi}}$ that then produce X-rays using data published by INTEGRAL telescope. Limits placed in $\langle \sigma \cdot{}v\rangle $ vs. m(DM) plane for m(DM) = $1 - 5000$ MeV.
8  JOHN 2021 derive limits on leptophilic DM annihilating to positrons by comparing expected spectra to AMS-02 data. The range m(DM): $60 - 300$ GeV appears excluded for this type of model, see Fig. 3.
9  ABAZAJIAN 2020 derive new limits on WIMP annihilation in galactic center (GC): ${{\mathit \sigma}}\cdot{}$v $<$ $2.5 \times 10^{-27}$ cm${}^{3}$/s for m(WIMP) = 50 GeV: seems to rule out WIMP explanation for GC ${{\mathit \gamma}}$ excess, favouring an astrophysics origin.
10  ABDALLAH 2020 search for WIMP annihilation in newly discovered by DES dwarf satellite galaxies using HESS; limits placed in $\langle \sigma \cdot{}v\rangle $ vs. m(DM) plane depending on annihilation channel and which dwarf satellite.
11  ABE 2020G search Super-Kamiokande data for WIMP annihilation to neutrinos in galactic center/halo; no signal; limits placed in $\langle \sigma \cdot{}v\rangle $ vs. m(DM) plane depending on annihilation channel and m(WIMP). Reported limit for annihilation to ${{\mathit \nu}}{{\overline{\mathit \nu}}}$ at 1 GeV.
12  ALBERT 2020 search for TeV-scale WIMP annihlation to ${{\mathit \gamma}}{{\mathit \gamma}}$ in dwarf spheroidal galaxies; no signal; limits placed in $\sigma \cdot{}v$ vs m(WIMP) plane: e.g. $\sigma \cdot{}v$ $<$ $2.2 \times 10^{-24}$ cm${}^{3}$/s for m(WIMP) = 1 TeV.
13  ALBERT 2020A search for WIMP annihilation to ${{\mathit \nu}}$s in galactic center using Antares; limits placed in ${{\mathit \sigma}}\cdot{}$v vs m(WIMP) plane e.g. ${{\mathit \sigma}}\cdot{}$v $<$ $5 \times 10^{-24}$ cm${}^{3}$/s for m(WIMP) = 1 TeV assuming annihilation dominantly to ${{\mathit \tau}}{{\overline{\mathit \tau}}}$ .
14  ALBERT 2020C report combined Antares + IceCube search for WIMP annihilation to ${{\mathit \tau}}{{\overline{\mathit \tau}}}$ ; for NFW halo profile report $\sigma \cdot{}v$ $<$ $1 \times 10^{-23}$ cm${}^{3}$/s for m(WIMP) = 100 GeV.
15  ALVAREZ 2020 use profiling over J-factor distributions and background to derive new limits on ${{\mathit \sigma}}\cdot{}$v; e.g. ${{\mathit \sigma}}\cdot{}$v $<$ $8 \times 10^{-26}$ cm${}^{3}$/s for m(WIMP) = 100 GeV.
16  HOOF 2020 examine ${{\mathit \gamma}}$ rays from 27 dwarf spheroidals using Fermi-LAT data; place limits in ${{\mathit \sigma}}\cdot{}$v vs m(WIMP) plane using profile likelihood and marginalized posterior techniques for DM annihilation to ${{\mathit \tau}}{{\overline{\mathit \tau}}}$ and ${{\mathit b}}{{\overline{\mathit b}}}$ ; quoted limit uses first technique and ${{\mathit b}}{{\overline{\mathit b}}}$ channel for m(WIMP) = 100 GeV; results rule out WIMP explanation of galactic center excess.
17  MAZZIOTTA 2020 use Fermi-LAT pointed-at-Sun data to search for DM annihilation in the Sun to long-lived mediators decaying into gamma rays, i.e. ${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ ${{\mathit \phi}}{{\mathit \phi}}$ $\rightarrow$ 4 ${{\mathit \gamma}}$ . Limits placed on the SI and SD DM-nucleon cross sections in the ${{\mathit \sigma}}-$DM mass plane for DM masses in the range 3 GeV $-$ 1.8 TeV. Limits are evaluated in both cases of equilibrium and non-equilibrium.
18  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.
19  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.
20  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).
21  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.
22  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.
23  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.
24  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(${{\mathit \nu}}$).
25  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.
26  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.
27  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.
28  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.
29  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.
30  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.
31  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.
32  AARTSEN 2017C use 1005 days of IceCube data to search for ${{\mathit \chi}}$ ${{\mathit \chi}}$ $\rightarrow$ neutrinos via various annihilation channels. Limits set.
33  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.
34  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.
35  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.
36  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.
37  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.
38  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.
39  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.
40  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).
41  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.
42  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.
43  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.
44  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.
45  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.
46  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.
47  LIANG 2016 search dwarf spheroidal galaxies, Large Magellanic Cloud, and Small Magellanic Cloud for ${{\mathit \gamma}}$-line in Fermi-LAT data.
48  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 .
49  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.
50  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.
51  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.
52  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.
53  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.
54  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.
55  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.
56  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.
57  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.
58  Limit assuming ${{\mathit X}^{0}}$ pair annihilation into ${{\mathit b}}{{\overline{\mathit b}}}$ .
59  Limit assuming ${{\mathit X}^{0}}$ pair annihilation into ${{\mathit W}^{+}}{{\mathit W}^{-}}$ .
60  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.
61  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.
62  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.
63  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 .
64  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 ${{\mathit W}^{+}}{{\mathit W}^{-}}$ .
65  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.
66  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. $17 - 20$.
67  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.
68  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.
69  ABRAMOWSKI 2011 search for ${{\mathit \gamma}}$ from ${{\mathit X}^{0}}$ annihilation near the Galactic center. The limit assumes Einasto DM density profile.
70  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.
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