hidden photon limits - a cookbook
TRANSCRIPT
Andrea Caputo, Alex Millar, Ciaran O’Hare, Edoardo Vitagliano arXiv:2105.04565
Hidden Photon Limits: A Cookbook
Alex Millar
Hidden/Dark photons
• New U(1) gauge boson with tiny kinetic mixing with the visible photon • Can be non-thermally produced as a good dark matter candidate • Very similar behaviour to axions
2
Alex Millar
Hidden Photons vs ALPs
• Key difference: HP has a polarisation!
• May be randomised or fixed depending on the production mechanism (or somewhere in-between)
• Structure formation may change this, but no detailed studies
3
Alex Millar
Haloscopes for HP DM
• In principle, any axion haloscope using axion-photon mixing is sensitive to HPs
• For an example, take a cavity haloscope
4C. BOUTAN/PACIFIC NORTHWEST NATIONAL LABORATORY; ADAPTED BY APS/ALAN STONEBRAKER
Alex Millar
Haloscopes for HP DM
• Two key differences
• HP does not need a B-field
• The polarisation direction of the HP matters
• (Usually) easy to convert between the two sensitivities
5C. BOUTAN/PACIFIC NORTHWEST NATIONAL LABORATORY; ADAPTED BY APS/ALAN STONEBRAKER
Alex Millar
Reinterpreting axion experiments
• Actually need to be very careful: many experiments use B-field vetos which people have neglected before now
• Polarisations can give a highly non-trivial time varying signal
• Timing and directional data rarely given
6
Alex Millar
Current HP Experiments
• Currently HP experiments make lots of different assumptions
• Some assume fixed, some random: few provide enough information in the results to properly calculate a limit for fixed polarisations
7
Alex Millar
What should an experiment assume?
• Totally randomised is the most optimistic (just factors of 1/3 or 2/3 for )
• Totally constant polarisation is the trickiest scenario
• Simplest analysis (arXiv:1201.5902) gives factors of 0.0025 or 0.0975
• Both time varying and constant signals should be considered
• How do we make our worse case scenario match the best case scenario?
cos2 θ
8
Alex Millar
HP Polarisations
• How do you deal with a fixed polarisation?
• Experiments are sensitive to an axis or a plane
9
Axial experiment(Zenith-pointing)
Planar experiment(North-facing)
Possible DP Polarisations
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Alex Millar
HP Polarisations
• Earth rotates!
• Long measurements sample a cone (or analogue)
• Short measurements sample a single random direction (very bad)
10
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Geocentric coordinates Detector-centric coordinates
Polarisation with respect to an axis
Polarisation with respect
to plane
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North-facingWest-facing
Zenith-facing
Alex Millar
Day long measurements
• To get a sense, one can take the simplest case: measurements lasting n-days exactly
• Experiments sensitive to an axis sweep out a cone (sensitive to a plane is simply the compliment)
11
Optimal (~35°) Unideal (~0°) Worst (90°)
Alex Millar
Day long measurements
• Need find the distribution of angles over some measurement
• Depends strongly on alignment and location (basically, there is a perfect angle with the pole around 35°)
12
Alex Millar
Improvement with long measurements
• Up to an order of magnitude improvement on limits for long measurements
13
Alex Millar
What about for short measurements? • Most experiments do single, short measurements
• Can be made better!
• Split each measurement into parts, and space those parts over the course of a day
• Best results: three if sensitive to an axis, two if sensitive to a plane
14
Alex Millar 15
• Order of magnitude improvement on coupling just from three measurements!
• Does not increase overall data taking time
• Also have to be careful of rescans
• Always rescan with the same alignment
What about for short measurements?
Alex Millar
Current HP Limits
• Rescaled for fixed polarisation (conservative case)
• *Dark E-field assumes time varying signal so may not apply to randomly polarised HP 16
10°6 10°5
Dark photon mass, mX [eV]
10°16
10°15
10°14
10°13
10°12
10°11
10°10
10°9
Kin
etic
mix
ing,
c
Frequency [GHz]10°1 100
Dark photons as dark matterDark photons as dark matter
WISPDMXWISPDMX
Dark E-fieldADMX-1
ADMX-2 ADMX-3
AD
MX
-Sidecar
AD
MX
-Sidecar
CA
PP-1
CA
PP-2
CA
PP-3
HA
YST
AC
-1
HA
YST
AC
-2
SQuAD
SHUKET
rDM = 0.45 GeV cm°3
Alex Millar
Future experiments
• Many more axion and HP experiments coming soon
• We should optimise scanning strategies to ensure robust limits regardless of DP scenario
• Need dedicated HP analyses!
17
10°1510°
1410°
1310°
1210°
1110°
1010°
910°
810°
710°
610°
510°
410°
310°
210°
1100
101102
103104
105
Dark photon mass, mX [eV]
10°18
10°17
10°16
10°15
10°14
10°13
10°12
10°11
10°10
10°9
10°8
10°7
10°6
10°5
10°4
10°3
Kin
etic
mix
ing,
cStandard projection
Optimised projection
Hz kHz MHz GHz THz eV keV
Dark photondark matter
g ! X
Stellarbounds
DM-Radio
DarkE-field
ALPHAMADMAX
LAMPOST
SuperCDMS
LZ
Alex Millar
Conclusions
• Most important message: axion experiments should do dedicated analysis, not just leave them for people to try to reinterpret them
• Polarisation can be very non-trivial: detailed timing and directional data is needed
• Can improve limits be an order of magnitude
• Effects of structure formation should be simulated
18
10°1510°
1410°
1310°
1210°
1110°
1010°
910°
810°
710°
610°
510°
410°
310°
210°
1100
101102
103104
105
Dark photon mass, mX [eV]
10°1810°1710°1610°1510°1410°1310°1210°1110°1010°910°810°710°610°510°410°310°210°1
100
Kin
etic
mix
ing,
c
AD
MX CA
PPH
AY
STA
C
QU
AX
LSW-AD
MX
LSW-UW
A
LSW-SPring-8LSW-SPring-8ALPSALPS
CROW
S
CROW
S CAST
CAST
SHIPSSHIPS
Plimpton-Lawton
Plimpton-Lawton
AFMAFM
Cavendish-Coulomb
Cavendish-Coulomb
Spectroscopy
SpectroscopyTEXONOTEXONO
XENON
DAMIC
SENSEISuperCDMS
FUNK
Tokyo-3
Toky
o-2
Tokyo-1
SHU
KET
Dar
kE-
field
WISPDMX
SQuA
D
DMPathfinder
Solar HB RGSolar HB RG
JupiterJupiter EarthEarth CrabCrabnebulanebula
IGMIGM
Leo TLeo T
Gas clouds
Gas clouds
Neutron stars
Neutron stars
Darkphoton
DM
Hz kHz MHz GHz THz eV keV
DPDM HeIIReionisation(Caputo et al.)
DPDM(Witte et al.)
DPDM(Arias et al.)
COBE/FIRASg ! X
DPDM heatingDPDM heating
Black holesuperradiance