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¹	ABBASI 2023A search for WIMP-WIMP annihilation to $ν$ 's. No signal observed. Require $⟨ σ \cdot v ⟩$ $<$ $10^{- 24}$ cm $^{3}$ /s for m( $χ$ ) $\sim$ $10 - 10 \times 10^{4}$ GeV for various halo profiles.

ABBASI 2023B search for PeV-scale WIMP-WIMP annihilation to

μ

b

pairs. No signal observed. Require

⟨ σ \cdot v ⟩

<

10^{- 22}

^{3}

/s for

χ

χ

\to

b \overset{―}{b}

with m(

χ

) about 1 PeV or

⟨ σ \cdot v ⟩

<

10^{- 23}

^{3}

/s for

χ

χ

\to

μ^{+} μ^{-}

with m(

χ

) about 1 PeV.

³	ABE 2023B search for WMP-WIMP annihilation to $γ$ in GC. No signal observed. Require $⟨ σ \cdot v ⟩$ $<$ $5 \times 10^{- 28}$ cm $^{3}$ /s for m( $χ$ ) = 1 TeV or $⟨ σ \cdot v ⟩$ $<$ $1 \times 10^{- 25}$ cm $^{3}$ /s for m( $χ$ ) = 100 TeV.

⁴	ALBERT 2023 search for WIMP pair annihilation to $γ$ in galactic halo. No signal observed. Limits placed in $⟨ σ \cdot v ⟩$ vs. mass ( $10 - 100$ TeV) plane for various annihilation channels.

⁵	CHENG 2023A provide updated combined Fermi-LAT/DAMPE search for gamma line from WIMP annihilation. No signal observed. Limits placed in $⟨ σ \cdot v ⟩$ vs. mass ( $6 - 200$ GeV) plane for various halo profiles.

⁶	FOSTER 2023 search for gamma ray line in Fermi-LAT data. No signal observed. Limits placed in $⟨ σ \cdot v ⟩$ vs. m( $χ$ ) plane. For Higgsino DM limit see Fig. 12.

⁷	GUO 2023 search with Five-hundred-meter Aperture Spherical Radio Telescope for synchrotron emission radio signal of DM annihilation from dwarf spheroidal galaxy. No signal observed. Limits set in $⟨ σ \cdot v ⟩$ vs. m( $χ$ ) plane for various annihilation final states.

⁸	GUO 2023A search in public IceCube data for DM annihilation to neutrinos. No signal observed. Limits placed in $⟨ σ \cdot v ⟩$ vs m( $χ$ ) plane for various annihilation assumptions.

⁹	LAVIS 2023 search for 2HDM+S DM and generic spectra using MeerKAT. No signal observed. Limits placed in $⟨ σ \cdot v ⟩$ vs. mass ( $10 - 1000$ GeV) plane for various annihilation channels.

¹⁰	ABDALLA 2022 search for WIMP annihilation in galactic center to gamma rays using HESS; no signal observed; limits set in mass vs $⟨ σ \cdot v ⟩$ plane for dominant annihilation to $W W$ or $τ \overset{―}{τ}$ . Limit here for $τ \overset{―}{τ}$ channel 0.7 TeV mass.

¹¹	ALBERT 2022A search for secluded PeV-scale DM annihilation to four final states; no signal detected; limits placed in $⟨ σ \cdot v ⟩$ vs. m( $χ$ ) plane for m( $χ$ ): $6 - 6000$ TeV for m(mediator) = 50, 250, and 1000 GeV.

¹²	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 $W W$ with parameters as in Fig. 4.

¹³	EGOROV 2022 derives limits on DM annihlation to $b \overset{―}{b}$ or $τ \overset{―}{τ}$ via radio signals from M31; quoted limit from $b \overset{―}{b}$ channel with LOFAR telescope as main data source, using parameters as in Fig. 10 (green curve) for m( $χ$ ) = 100 GeV.

¹⁴	MANCONI 2022 use polarized synchrotron emission data from Planck to constrain WIMP annihilation cross section in Galaxy; limits set in $⟨ σ \cdot v ⟩$ vs. m(DM) plane.

¹⁵	ABDALLAH 2021 search for WIMP-WIMP annihilation into 2 monoenergetic $γ$ rays in WLM dwarf irregular galaxy using HESS data. No signal. Limits placed in $⟨ σ \cdot v ⟩$ vs. m(WIMP) plane for a mass of 370 GeV.

¹⁶	CIRELLI 2021 derive limits on light DM annihilation to $e e$ , $μ μ$ , $π π$ that then produce X-rays using data published by INTEGRAL telescope. Limits placed in $⟨ σ \cdot v ⟩$ vs. m(DM) plane for m(DM) = $1 - 5000$ MeV.

¹⁷	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.

¹⁸	ABAZAJIAN 2020 derive new limits on WIMP annihilation in galactic center (GC): $⟨ σ \cdot v ⟩$ $<$ $2.5 \times 10^{- 27}$ cm $^{3}$ /s for m(WIMP) = 50 GeV: seems to rule out WIMP explanation for GC $γ$ excess, favouring an astrophysics origin.

¹⁹	ABDALLAH 2020 search for WIMP annihilation in newly discovered by DES dwarf satellite galaxies using HESS; limits placed in $⟨ σ \cdot v ⟩$ vs. m(DM) plane depending on annihilation channel and which dwarf satellite.

²⁰	ABE 2020G search Super-Kamiokande data for WIMP annihilation to neutrinos in galactic center/halo; no signal; limits placed in $⟨ σ \cdot v ⟩$ vs. m(DM) plane depending on annihilation channel and m(WIMP). Reported limit for annihilation to $ν \overset{―}{ν}$ at 1 GeV.

²¹	ALBERT 2020 search for TeV-scale WIMP annihlation to $γ γ$ in dwarf spheroidal galaxies; no signal; limits placed in $σ \cdot v$ vs m(WIMP) plane: e.g. $σ \cdot v$ $<$ $2.2 \times 10^{- 24}$ cm $^{3}$ /s for m(WIMP) = 1 TeV.

²²	ALBERT 2020A search for WIMP annihilation to $ν$ s in galactic center using Antares; limits placed in $σ \cdot$ v vs m(WIMP) plane e.g. $σ \cdot$ v $<$ $5 \times 10^{- 24}$ cm $^{3}$ /s for m(WIMP) = 1 TeV assuming annihilation dominantly to $τ \overset{―}{τ}$ .

²³	ALBERT 2020C report combined Antares + IceCube search for WIMP annihilation to $τ \overset{―}{τ}$ ; for NFW halo profile report $σ \cdot v$ $<$ $1 \times 10^{- 23}$ cm $^{3}$ /s for m(WIMP) = 100 GeV.

²⁴	ALVAREZ 2020 use profiling over J-factor distributions and background to derive new limits on $σ \cdot$ v; e.g. $σ \cdot$ v $<$ $8 \times 10^{- 26}$ cm $^{3}$ /s for m(WIMP) = 100 GeV.

²⁵

HOOF 2020 examine

γ

rays from 27 dwarf spheroidals using Fermi-LAT data; place limits in

σ \cdot

v vs m(WIMP) plane using profile likelihood and marginalized posterior techniques for DM annihilation to

τ \overset{―}{τ}

and

b \overset{―}{b}

; quoted limit uses first technique and

b \overset{―}{b}

channel for m(WIMP) = 100 GeV; results rule out WIMP explanation of galactic center excess.

²⁶

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.

χ

χ

\to

ϕ ϕ

\to

γ

. Limits placed on the SI and SD DM-nucleon cross sections in the

σ -

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.

²⁷	ABEYSEKARA 2019 search for $γ$ s from DM annihilation in galactic substructures with HAWC; no signal, limits placed in J $⟨ σ \cdot v ⟩$ vs. declination plane for m(DM) $\sim$ $1 - 108$ TeV.

²⁸	ALBERT 2019B search for DM signal from M31 galaxy in $μ$ , $τ$ , $t$ , $b$ , $W$ channels using HAWC for m(DM) $\sim$ $1 - 100$ TeV; no signal, limits placed in $⟨ σ \cdot v ⟩$ vs. m(DM) plane.

²⁹	CHEUNG 2019 derive model-dependent bounds on $⟨ σ \cdot v ⟩$ from EDGES data: $<$ $4 \times 10^{- 26}$ cm $^{3}$ /s for $e^{+} e^{-}$ and $b \overset{―}{b}$ for m( $χ$ ) = 100 GeV (including boost factor).

³⁰	DI-MAURO 2019 place limits on WIMP annihilation via Fermi-LAT observation of M31 and M33 galaxies: $⟨ σ \cdot v ⟩$ $<$ $7 \times 10^{- 27}$ cm $^{3}$ /s for m( $χ$ ) = 20 GeV from M31.

³¹	JOHNSON 2019 search for $γ$ -rays, $10 - 600$ GeV energy, from $P - w a v e$ annihilating DM around SgrA* BH using Fermi-LAT; limits set for various models.

³²	LI 2019D search for $χ$ $χ$ $\to$ $γ$ in Fermi-LAT data; no signal, require $⟨ σ \cdot v ⟩$ $<$ $2 \times 10^{- 26}$ cm $^{3}$ /s for m( $χ$ ) = 100 GeV.

³³	NG 2019 search for X-ray line from sterile $ν$ decay/annihilation using NuStar M-31; no signal: limits placed in m( $ν$ ) vs mixing angle and $⟨ σ \cdot v ⟩$ vs m( $ν$ ).

³⁴	QUEIROZ 2019 examine $χ$ $χ$ $\to$ $χ S M$ semi-annihilation of DM reaction; limits placed for various assumed $S M$ particles in $⟨ σ \cdot v ⟩$ vs. m( $χ$ ) plane.

³⁵	ABDALLAH 2018 search for WIMP WIMP $\to$ $γ X$ in central galactic halo, 10 years of data; limits placed in $⟨ σ \cdot v ⟩$ vs. m(WIMP) plane for m(WIMP): $0.3 - 70$ TeV.

³⁶	AHNEN 2018 search for WIMP WIMP $\to$ $γ X$ from Ursa Major II; limits set in $⟨ σ \cdot v ⟩$ vs. m(WIMP) plane for $b \overset{―}{b}$ , $W^{+} W^{-}$ , $τ^{+} τ^{-}$ , and $μ^{+} μ^{-}$ annihilation modes.

³⁷	ALBERT 2018B search for TeV-scale WIMPs with WIMP WIMP $\to$ $γ X$ in Andromeda galaxy using HAWC Observatory; limits set in $⟨ σ \cdot v ⟩$ vs m(WIMP) plane.

³⁸	CHANG 2018A examine $χ$ $χ$ $\to$ $b \overset{―}{b}$ $\to$ $γ$ using Fermi Pass 8 data; no signal; require $⟨ σ \cdot v ⟩$ $<$ $10^{- 26}$ cm $^{3}$ /s for m( $χ$ ) = 50 GeV.

³⁹	LISANTI 2018 examine Fermi Pass 8 $γ$ -ray data from galaxy groups; report m(WMP) $>$ 30 GeV for annihilation in $b \overset{―}{b}$ channel.

⁴⁰	MAZZIOTTA 2018 examine Fermi-LAT electron and positron spectra searching for features originating from DM particles annihilation into $e^{+} e^{-}$ pairs, from 45 GeV to 2 TeV; no signal found, limits are obtained.

⁴¹	AARTSEN 2017C use 1005 days of IceCube data to search for $χ$ $χ$ $\to$ neutrinos via various annihilation channels. Limits set.

⁴²	ALBERT 2017A search for DM annihilation to $ν$ s using ANTARES data from $2007 - 2015$ . No signal. Limits set in $⟨ σ \cdot v ⟩$ vs. m(DM) plane for m(DM) $\sim 10 - 10 \times 10^{5}$ GeV. The listed limit is for m(DM) = 100 TeV.

⁴³

ARCHAMBAULT 2017 set limits for WIMP mass between 100 GeV and 1 TeV on

⟨ σ \cdot v ⟩

for

W^{+} W^{-}

Z Z

b \overset{―}{b}

s \overset{―}{s}

u \overset{―}{u}

d \overset{―}{d}

t \overset{―}{t}

e^{+} e^{-}

g g

c \overset{―}{c}

h h

γ γ

μ^{+} μ^{-}, τ^{+} τ^{-}

annihilation channels.

⁴⁴

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

⟨ σ \cdot v ⟩

<

6 \times 10^{- 20}

^{3}

/s in dwarf galaxies and

⟨ σ \cdot v ⟩

<

7 \times 10^{- 21}

^{3}

/s in LMC for 5 TeV WIMP mass.

⁴⁵	BOUDAUD 2017 use data from the spacecraft Voyager 1, beyond the heliopause, and from AMS02 on $χ$ $χ$ $\to$ $e^{+} e^{-}$ to require $⟨ σ \cdot v ⟩ < 1. \times 10^{- 28}$ cm $^{3}$ /s for m( $χ$ ) = 10 MeV.

⁴⁶	AARTSEN 2016D search for GeV $ν$ s from WIMP annihilation in galaxy; limits set on $⟨ σ \cdot v ⟩$ in Fig. 6, 7.

⁴⁷	ABDALLAH 2016 require $⟨ σ \cdot v ⟩$ $<$ $6 \times 10^{- 26}$ cm $^{3}$ /s for $m$ (WIMP) = 1.5 TeV from 254 hours observation ( $W W$ channel) and $<$ $2 \times 10^{- 26}$ cm $^{3}$ /s for $m$ (WIMP) = 1.0 TeV in $τ^{+} τ^{-}$ channel.

⁴⁸	ABDALLAH 2016A search for line spectra from WIMP + WIMP $\to$ $γ γ$ in 18 hr HESS data; rule out previous 130 GeV WIMP hint from Fermi-LAT data.

⁴⁹	AHNEN 2016 require $⟨ σ \cdot v ⟩ < 3 \times 10^{- 26}$ cm $^{3}$ /s for $m$ (WIMP) = 100 GeV ( $W W$ channel).

⁵⁰	AVRORIN 2016 require $⟨$ s.v $⟩$ $<$ $1.91 \times 10^{- 21}$ cm $^{3}$ /s from WIMP annihilation to $ν$ s via $W W$ channel for $m$ (WIMP) = 1 TeV.

⁵¹	CAPUTO 2016 place limits on WIMPs from annihilation to gamma rays in Small Magellanic Cloud using Fermi-LaT data: $⟨ σ \cdot v ⟩ < 3 \times 10^{- 26}$ cm $^{3}$ /s for $m$ (WIMP) = 10 GeV.

⁵²

FORNASA 2016 use anisotropies in the

γ

-ray diffuse emission detected by Fermi-LAT to bound

⟨ σ \cdot v ⟩

<

10^{- 25}

^{3}

/s for m(WIMP) = 100 GeV in

b \overset{―}{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.

⁵³	LEITE 2016 constrain WIMP annihilation via search for radio emissions from Smith cloud; $⟨ σ \cdot v ⟩$ $<$ $5 \times 10^{- 27}$ cm $^{3}$ /s in $e e$ channel for m(WIMP) = 5 GeV.

⁵⁴	LI 2016 re-analyze Fermi-LAT data on 8 dwarf spheroidals; set limit $⟨ σ \cdot v ⟩ < 2 \times 10^{- 26}$ cm $^{3}$ /s for $m$ (WIMP) = 100 GeV in $b \overset{―}{b}$ mode with substructures included.

⁵⁵	LI 2016A constrain $⟨ σ \cdot v ⟩$ $<$ $10^{- 25}$ cm $^{3}$ /s in $b \overset{―}{b}$ channel for m(WIMP) = 100 GeV using Fermi-LAT data from M31; see Fig. 6.

⁵⁶	LIANG 2016 search dwarf spheroidal galaxies, Large Magellanic Cloud, and Small Magellanic Cloud for $γ$ -line in Fermi-LAT data.

⁵⁷	LU 2016 re-analyze Fermi-LAT and AMS-02 data; require $⟨ σ \cdot v ⟩$ $< 10^{- 25}$ cm $^{3}$ /s for $m_{m}$ (WIMP) = 1 TeV in $b \overset{―}{b}$ channel .

⁵⁸	SHIRASAKI 2016 re-anayze Fermi-LAT extra-galactic data; require $⟨ σ \cdot v ⟩ < 10^{- 23}$ cm $^{3}$ /s for $m$ (WIMP) = 1 TeV in $b \overset{―}{b}$ channel; see Fig. 8.

⁵⁹	AARTSEN 2015C search for neutrinos from $X^{0}$ annihilation in the Galactic halo. See their Figs. 16 and 17, and Table 5 for limits on $σ \cdot$ v for $X^{0}$ mass between 100 GeV and 100 TeV.

⁶⁰	AARTSEN 2015E search for neutrinos from $X^{0}$ annihilation in the Galactic center. See their Figs. 7 and 9, and Table 3 for limits on $σ \cdot$ v for $X^{0}$ mass between 30 GeV and 10 TeV.

⁶¹	ABRAMOWSKI 2015 search for $γ$ from $X^{0}$ annihilation in the Galactic center. See their Fig. 4 for limits on $σ \cdot$ v for $X^{0}$ mass between 250 GeV and 10 TeV.

⁶²	ACKERMANN 2015 search for monochromatic $γ$ from $X^{0}$ annihlation in the Galactic halo. See their Fig. 8 and Tables $2 - 4$ for limits on $σ \cdot$ v for $X^{0}$ mass between 0.2 GeV and 500 GeV.

⁶³	ACKERMANN 2015A search for $γ$ from $X^{0}$ annihilation (both Galactic and extragalactic) in the isotropic $γ$ background. See their Fig. 7 for limits on $σ \cdot$ v for $X^{0}$ mass between 10 GeV and 30 TeV.

⁶⁴	ACKERMANN 2015B search for $γ$ from $X^{0}$ annihilation in 15 dwarf spheroidal satellite galaxies of the Milky Way. See their Figs. 1 and 2 for limits on $σ \cdot$ v for $X^{0}$ mass between 2 GeV and 10 TeV.

⁶⁵	ADRIAN-MARTINEZ 2015 search for neutrinos from $X^{0}$ annihilation in the Galactic center. See their Figs. 10 and 11 and Tables 1 and 2 for limits on $σ \cdot$ v for $X^{0}$ mass between 25 GeV and 10 TeV.

⁶⁶

ACKERMANN 2014 search for

γ

from

X^{0}

annihilation in 25 dwarf spheroidal satellite galaxies of the Milky Way. See their Tables II--VII for limits assuming annihilation into

e^{+} e^{-}

μ^{+} μ^{-}

τ^{+} τ^{-}

u \overset{―}{u}

b \overset{―}{b}

, and

W^{+} W^{-}

, for

X^{0}

mass ranging from 2 GeV to 10 TeV.

⁶⁷	Limit assuming $X^{0}$ pair annihilation into $b \overset{―}{b}$ .

⁶⁸	Limit assuming $X^{0}$ pair annihilation into $W^{+} W^{-}$ .

⁶⁹

ALEKSIC 2014 search for

γ

from

X^{0}

annihilation in the dwarf spheroidal galaxy Segue 1. The listed limit assumes annihilation into

W^{+} W^{-}

. See their Figs. 6, 7, and 16 for limits on

σ \cdot

v for annihilation channels

μ^{+} μ^{-}

τ^{+} τ^{-}

b \overset{―}{b}

t \overset{―}{t}

γ γ

γ Z

W^{+} W^{-}

Z Z

for

X^{0}

mass between

10^{2}

and

10^{4}

GeV.

⁷⁰	AARTSEN 2013C search for neutrinos from $X^{0}$ annihilation in nearby galaxies and galaxy clusters. See their Figs. $5 - 7$ for limits on $σ \cdot$ v for $X^{0}$ $X^{0}$ $\to$ $ν \overset{―}{ν}$ , $μ^{+} μ^{-}$ , $τ^{+} τ^{-}$ , and $W^{+} W^{-}$ for $X^{0}$ mass between 300 GeV and 100 TeV.

⁷¹

ABRAMOWSKI 2013 search for monochromatic

γ

from

X^{0}

annihilation in the Milky Way halo in the central region. Limit on

σ \cdot

v between

10^{- 28}

and

10^{- 25}

^{3}

^{- 1}

(95

%

CL) is obtained for

X^{0}

mass between 500 GeV and 20 TeV for

X^{0}

X^{0}

\to

γ γ

X^{0}

density distribution in the Galaxy by Einasto is assumed. See their Fig. 4.

⁷²

ACKERMANN 2013A search for monochromatic

γ

from

X^{0}

annihilation in the Milky Way. Limit on

σ \cdot

v for the process

X^{0}

X^{0}

\to

γ γ

in the range

10^{- 29} - 10^{- 27}

^{3}

^{- 1}

(95

%

CL) is obtained for

X^{0}

mass between 5 and 300 GeV. The limit depends slightly on the assumed density profile of

X^{0}

in the Galaxy. See their Tables VII

-

X and Fig.10. Supersedes ACKERMANN 2012.

⁷³	ABRAMOWSKI 2012 search for $γ$ 's from $X^{0}$ annihilation in the Fornax galaxy cluster. See their Fig. 7 for limits on $σ \cdot$ v for $X^{0}$ mass between 0.1 and 100 TeV for the annihilation channels $τ^{+} τ^{-}$ , $b \overset{―}{b}$ , and $W^{+} W^{-}$ .

⁷⁴

ACKERMANN 2012 search for monochromatic

γ

from

X^{0}

annihilation in the Milky Way. Limit on

σ \cdot

v in the range

10^{- 28} - 10^{- 26}

^{3}

^{- 1}

(95

%

CL) is obtained for

X^{0}

mass between 7 and 200 GeV if

X^{0}

annihilates into

γ γ

. The limit depends slightly on the assumed density profile of

X^{0}

in the Galaxy. See their Table III and Fig. 15.

⁷⁵

ACKERMANN 2012 search for

γ

from

X^{0}

annihilation in the Milky Way in the diffuse

γ

background. Limit on

σ \cdot

v of

10^{- 24}

^{3}

^{- 1}

or larger is obtained for

X^{0}

mass between 5 GeV and 10 TeV for various annihilation channels including

W^{+} W^{-}

b \overset{―}{b}

g g

e^{+} e^{-}

μ^{+} μ^{-}

τ^{+} τ^{-}

. The limit depends slightly on the assumed density profile of

X^{0}

in the Galaxy. See their Figs.

17 - 20

⁷⁶

ALIU 2012 search for

γ

's from

X^{0}

annihilation in the dwarf spheroidal galaxy Segue 1. Limit on

σ \cdot

v in the range

10^{- 24} - 10^{- 20}

^{3}

^{- 1}

(95

%

CL) is obtained for

X^{0}

mass between 10 GeV and 2 TeV for annihilation channels

e^{+} e^{-}

μ^{+} μ^{-}

τ^{+} τ^{-}

b \overset{―}{b}

, and

W^{+} W^{-}

. See their Fig. 3.

⁷⁷	ABBASI 2011C search for $ν_{μ}$ from $X^{0}$ annihilation in the outer halo of the Milky Way. The limit assumes annihilation into $ν ν$ . See their Fig. 9 for limits with other annihilation channels.

⁷⁸	ABRAMOWSKI 2011 search for $γ$ from $X^{0}$ annihilation near the Galactic center. The limit assumes Einasto DM density profile.

⁷⁹

ACKERMANN 2011 search for

γ

from

X^{0}

annihilation in ten dwarf spheroidal satellite galaxies of the Milky Way. The limit for

m

= 10 GeV assumes annihilation into

b \overset{―}{b}

, the others

W^{+} 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

Except where otherwise noted, content of the 2024 Review of Particle Physics is licensed under a Creative Commons Attribution 4.0 International (CC BY 4.0) license. The publication of the Review of Particle Physics is supported by US DOE, MEXT (Japan), INFN (Italy) and CERN. Individual collaborators receive support for their PDG activities from their respective institutes or funding agencies. © 2024. See LBNL disclaimers.

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