58
3 Phenomenology of the Massive Dark Photon
[MeV]
A'
m
8
−
10
7
−
10
6
−
10
5
−
10
4
−
10
3
−
10
2
−
10
1
−
10
1
ε
17
−
10
16
−
10
15
−
10
14
−
10
13
−
10
12
−
10
11
−
10
10
−
10
9
−
10
Da rk Ma tte r
FUNK
DAMIC
XENON10
XENON100
CDEX-10
XENON-1T (2019)
XENON-1T (2020)
SuperCDMS
EDELWEISS-III
SENSEI
XMASS
Fig. 3.8 Zoom in the range 10 −8 MeV ∼ < M A ∼ < 1 MeV and 10 −17 ∼ < ε ∼ < 10 −9 for the current
limits on massive dark photon for m A < 1 MeV. Results from dark matter direct detection experiments (XENON10 and XENON100 ([73] based on XENON10 [75] and XENON100 [74] data),
XENON1T (2019) [76]; XENON1T (2020) [77]; DAMIC [78]; SuperCDMS [79]; CDEX-10 [80];
EDELWEISS-III [81]; SENSEI [82]; XMASS [83]; FUNK [84])
– astrophysical bounds on dwarf galaxies [89]. These limits apply for values of
m A < 10
−19 MeV and are not shown in Fig. 3.7 measurements of the temperature
of the intergalactic medium at the epoch of He
++ re-ionization in the presence of
inhomogeneities [60–62],
– cold Galactic Center gas clouds heating rates [90];
– cosmic microwave background spectral distortions (μ and y-type) [62];
– energy deposition during the dark ages [63],
– the number of relativistic species
eff during big-bang nucleosynthesis and
recombination [91] and
– the diffuse X-ray background [92]
yield a series of limits on the upper value of ε for different values of M A . These
limits are depicted together by the curve labelled “Dark Matter” in Fig. 3.7.
In addition, there are limits from:
• Dark matter direct detection experiments: These experiments are part of the ongoing search for dark matter through its direct detection. Data from XENON10/XE
NON100 ([73] based on XENON10 [75] and XENON100 [74]), XENON1T [76],
DAMIC [78], SuperCDMS [79], CDEX-10 [80], EDELWEISS-III [81],
SENSEI [82], XMASS [83] and FUNK [84] can be used to constrain the massive dark photon parameters;
• Haloscopes: Searches with microwave cavities for relic axion converting to photons [93] can be translated into limits (not shown in Fig. 3.7 on the dark photon
3 Phenomenology of the Massive Dark Photon
[MeV]
A'
m
8
−
10
7
−
10
6
−
10
5
−
10
4
−
10
3
−
10
2
−
10
1
−
10
1
ε
17
−
10
16
−
10
15
−
10
14
−
10
13
−
10
12
−
10
11
−
10
10
−
10
9
−
10
Da rk Ma tte r
FUNK
DAMIC
XENON10
XENON100
CDEX-10
XENON-1T (2019)
XENON-1T (2020)
SuperCDMS
EDELWEISS-III
SENSEI
XMASS
Fig. 3.8 Zoom in the range 10 −8 MeV ∼ < M A ∼ < 1 MeV and 10 −17 ∼ < ε ∼ < 10 −9 for the current
limits on massive dark photon for m A < 1 MeV. Results from dark matter direct detection experiments (XENON10 and XENON100 ([73] based on XENON10 [75] and XENON100 [74] data),
XENON1T (2019) [76]; XENON1T (2020) [77]; DAMIC [78]; SuperCDMS [79]; CDEX-10 [80];
EDELWEISS-III [81]; SENSEI [82]; XMASS [83]; FUNK [84])
– astrophysical bounds on dwarf galaxies [89]. These limits apply for values of
m A < 10
−19 MeV and are not shown in Fig. 3.7 measurements of the temperature
of the intergalactic medium at the epoch of He
++ re-ionization in the presence of
inhomogeneities [60–62],
– cold Galactic Center gas clouds heating rates [90];
– cosmic microwave background spectral distortions (μ and y-type) [62];
– energy deposition during the dark ages [63],
– the number of relativistic species
eff during big-bang nucleosynthesis and
recombination [91] and
– the diffuse X-ray background [92]
yield a series of limits on the upper value of ε for different values of M A . These
limits are depicted together by the curve labelled “Dark Matter” in Fig. 3.7.
In addition, there are limits from:
• Dark matter direct detection experiments: These experiments are part of the ongoing search for dark matter through its direct detection. Data from XENON10/XE
NON100 ([73] based on XENON10 [75] and XENON100 [74]), XENON1T [76],
DAMIC [78], SuperCDMS [79], CDEX-10 [80], EDELWEISS-III [81],
SENSEI [82], XMASS [83] and FUNK [84] can be used to constrain the massive dark photon parameters;
• Haloscopes: Searches with microwave cavities for relic axion converting to photons [93] can be translated into limits (not shown in Fig. 3.7 on the dark photon