WIMPS and LIPSS WIMPS and LIPSS A. Afanasev Afanasev, O.K. Baker - - PowerPoint PPT Presentation
WIMPS and LIPSS WIMPS and LIPSS A. Afanasev Afanasev, O.K. Baker (contact person), K. McFarlane , O.K. Baker (contact person), K. McFarlane A. Hampton University Hampton University for the LIPSS collaboration for the LIPSS collaboration
A.
Afanasev, O.K. Baker (contact person), K. McFarlane , O.K. Baker (contact person), K. McFarlane
Hampton University Hampton University for the LIPSS collaboration for the LIPSS collaboration CASA seminar CASA seminar Feb 2, 2006 Feb 2, 2006
– – overview only
– – how did all previous searches miss it? how did all previous searches miss it?
– – plans and history plans and history
based upon experimental idea of L. based upon experimental idea of L. Maiani Maiani, , R.
Petronzio, and E. , and E. Zavattini Zavattini, PLB 175, 359 , PLB 175, 359 (1986) (1986)
Dichroism Dichroism
rotation of polarization plane rotation of polarization plane Maiani Maiani et.al et.al., ., Phy Phy. . Lett
. B175 (1986); www.ts.infn.it/experiments/pvlas www.ts.infn.it/experiments/pvlas
2 2 2 2 2
4 1 1 2 sin 4 ⎥ ⎦ ⎤ ⎢ ⎣ ⎡ ⎪ ⎭ ⎪ ⎬ ⎫ ⎪ ⎩ ⎪ ⎨ ⎧ ⎥ ⎥ ⎦ ⎤ ⎢ ⎢ ⎣ ⎡ ⎟ ⎟ ⎟ ⎠ ⎞ ⎜ ⎜ ⎜ ⎝ ⎛ ⎟ ⎟ ⎠ ⎞ ⎜ ⎜ ⎝ ⎛ − − ⎟ ⎠ ⎞ ⎜ ⎝ ⎛ − = k LK N K k kL M L B
m m ext
ε
M: M: inverse inverse coupling coupling K Km
m :
:inverse inverse compton compton wavelength wavelength k: k: light light wavenumber wavenumber L: L: magnetic magnetic field region field region length length N: N: number of number of traversals traversals
rotation of polarization plane rotation of polarization plane hep hep-
ex/0507061 (2005); Phys Rev D47, 3707 (1993) Phys Rev D47, 3707 (1993)
ellipticity ellipticity
dispersion; photon dispersion; photon-
axion Maiani Maiani et.al et.al., ., Phy Phy. . Lett
. B175 (1986); www.ts.infn.it/experiments/pvlas www.ts.infn.it/experiments/pvlas
⎪ ⎪ ⎪ ⎭ ⎪ ⎪ ⎪ ⎬ ⎫ ⎪ ⎪ ⎪ ⎩ ⎪ ⎪ ⎪ ⎨ ⎧ ⎥ ⎥ ⎦ ⎤ ⎢ ⎢ ⎣ ⎡ ⎟ ⎟ ⎟ ⎠ ⎞ ⎜ ⎜ ⎜ ⎝ ⎛ ⎟ ⎟ ⎠ ⎞ ⎜ ⎜ ⎝ ⎛ − − − ⎟ ⎟ ⎠ ⎞ ⎜ ⎜ ⎝ ⎛ = k LK K k kL K M kL B
m m m ext
2 1 1 sin 1 4
2 2 2 2 2
ψ
M: M: inverse inverse coupling coupling K Km
m :
:inverse inverse compton compton wavelength wavelength k: k: light light wavenumber wavenumber L: L: magnetic magnetic field region field region length length N: N: number of number of traversals traversals
dispersion: photon dispersion: photon-
axion
hep hep-
ex/0507061 (2005); Phys Rev D47, 3707 (1993)
Phys Rev D47, 3707 (1993)
6 T ; 1 meter long dipole magnet 1064 nm ; 0.1 W laser 60 km path length in magnet using 6 meters long
cryostat rotation 0.3 Hz
PVLAS results PVLAS results zavattini zavattini et al; see et al; see www.ts.infn.it/experiments/pvlas
www.ts.infn.it/experiments/pvlas
B: B: 5 T 5 T L: L: 1 m 1 m ω ω: : 1.2 1.2 eV eV (1.064 (1.064 µ µ) ) OC: OC: 6.3 m 6.3 m N: N: 44000 44000
PVLAS example data PVLAS example data
www.ts.infn.it/experiments/pvlas www.ts.infn.it/experiments/pvlas
6 < g < 1.0 x 10
5 GeV
1
PVLAS effect is 104 stronger than QED (Euler-Heisenberrg) prediction!
light light pseudoscalar pseudoscalar particle particle weakly interacting weakly interacting (weakly interacting massive particle) (weakly interacting massive particle)
pseudoscalar pseudoscalar particle coupling to photons particle coupling to photons in present case, use laser light and magnetic field in present case, use laser light and magnetic field light polarization in direction of magnetic field light polarization in direction of magnetic field PVLAS claims to see effect in both PVLAS claims to see effect in both dichroism dichroism and and ellipticity ellipticity (using (using same apparatus). same apparatus). we want to test this result in a completely independent way we want to test this result in a completely independent way
B E g F F M L v v ) ⋅ = − = 4 4 1 ϕ ϕ
µν µν ϕγγ
A.
Ringwald; hep ; hep-
ph/0511184 K.
Zioutas et.al et.al., PRL 94, 121301 (2005) ., PRL 94, 121301 (2005)
possibilities . . . possibilities . . .
Peccei, Quin (1977); S. Weinberg (1978); F. Wilczek (1978)
Stars and galaxies are only ~0.5% Stars and galaxies are only ~0.5% Neutrinos are ~0.3 Neutrinos are ~0.3– –10% 10% Rest of ordinary matter (electrons and protons) Rest of ordinary matter (electrons and protons) are ~5% are ~5% Dark Matter ~30% Dark Matter ~30% Dark Energy ~65% Dark Energy ~65% Anti Anti-
Matter 0%
axion a dark matter candidate
two broad classes of two broad classes of axion axion searches searches
– – detect relic (big detect relic (big-
bang leftover), or solar, or stellar axions axions – – produce and then detect produce and then detect axions axions in terrestrial in terrestrial expt expt
more difficult, in general, since there are two factors of small more difficult, in general, since there are two factors of small couplings couplings LIPSS uses this strategy LIPSS uses this strategy BFRT collaboration also used this strategy BFRT collaboration also used this strategy
axions axions created created moments after moments after the big bang. the big bang. thermalized thermalized
mass range mass range must be must be consistent with consistent with astrophysical astrophysical
microwave cavity technique microwave cavity technique
Sikivie (1983); Ansel’m (1985); van Bibber et al (1987)
V: cavity volume V: cavity volume m (f) mass (coupling) m (f) mass (coupling) B: magnetic field B: magnetic field R: galactic halo R: galactic halo axion axion density on Earth density on Earth C: mode dependent constant (0.6) C: mode dependent constant (0.6) Q QL
L: cavity
: cavity’ ’s loaded quality factor s loaded quality factor Q Qa
a: galactic halo
: galactic halo axion axion quality factor (10 quality factor (106
6)
) P PN
N: average thermal noise power
: average thermal noise power T Ts
s cavity temperature plus noise
cavity temperature plus noise ‘ ‘temperature temperature’ ’
microwave cavity experiments find no microwave cavity experiments find no evidence for relic evidence for relic axions axions in parameter space in parameter space indicated indicated
decommissioned LHC test magnet decommissioned LHC test magnet
– – L = 10 m ; B = 9 T L = 10 m ; B = 9 T
moving platform moving platform
– – up to 50 days/year of alignment up to 50 days/year of alignment
4 magnet bores, for x 4 magnet bores, for x-
ray detection
– – solar temperature solar temperature keV keV axions axions keV keV x x-
rays
3 x ray detectors 3 x ray detectors x ray x ray focussing focussing system to increase S/N ratio system to increase S/N ratio
Ellis and Olive, 1987; Raffelt and Seckel, 1988; Turner, 1988, etc
CAST finds no evidence to date for solar CAST finds no evidence to date for solar axions axions in in parameter space indicated parameter space indicated SN1987A does not rule out PVLAS result SN1987A does not rule out PVLAS result
cryogenic dark matter search in cryogenic dark matter search in Soudan Soudan underground laboratory underground laboratory
D.S. D.S. Akerib Akerib et al, Phys. Rev. et al, Phys. Rev. Lett Lett 93, 211301 93, 211301-
1 (2004)
sensitive to massive (> eV) axions; none seen
(Phys. Rev. D47 3707 (1993 BFRT collaboration) (Phys. Rev. D47 3707 (1993 BFRT collaboration)
3707 (1993) 3707 (1993)
BFRT results: regeneration expt
no ps signal seen
dark current
direct light signal
the combination of accelerator searches, astrophysical, and the combination of accelerator searches, astrophysical, and cosmological arguments leaves open a search window cosmological arguments leaves open a search window massive massive axion axion discovery still solves the strong CP problem, but not discovery still solves the strong CP problem, but not the dark matter problem. search for light the dark matter problem. search for light axions axions (< (< eV eV) )
10-6 < ma < 10-3 eV
the combination of accelerator searches, astrophysical, and the combination of accelerator searches, astrophysical, and cosmological arguments leaves open a search window cosmological arguments leaves open a search window massive massive axion axion discovery still solves the strong CP problem, but not discovery still solves the strong CP problem, but not the dark matter problem. search for light the dark matter problem. search for light axions axions (< (< eV eV) )
10-6 < ma < 10-3 eV
2).
polarization plane rotation, polarization plane rotation, ellipticity ellipticity
reproduce PVLAS with different apparatus reproduce PVLAS with different apparatus
regeneration regeneration
FEL photons regeneration FEL photons regeneration Primakoff Primakoff photons regeneration photons regeneration
photon collisions photon collisions
wide angle wide angle axion axion production at wiggler center production at wiggler center polarization plane rotation polarization plane rotation four wave mixing in vacuum four wave mixing in vacuum
– – 2 2 2 or 3 2 or 3 1 1
microwave cavity microwave cavity
primordial primordial axions axions solar production and lab regeneration (a la CAST) solar production and lab regeneration (a la CAST)
couple polarized laser couple polarized laser light with magnetic light with magnetic field field Sikivie Sikivie (1983); (1983); Ansel Ansel’ ’m m (1985); Van Bibber et (1985); Van Bibber et al (1987) al (1987)
2 2 2 2
4 4 sin 4 1 ⎪ ⎪ ⎭ ⎪ ⎪ ⎬ ⎫ ⎪ ⎪ ⎩ ⎪ ⎪ ⎨ ⎧ ⎟ ⎟ ⎠ ⎞ ⎜ ⎜ ⎝ ⎛ ≈
→
ω ω
ϕ ϕ ϕ γ
L m L m gBL P
ps – photon (or photon-ps) conversion probability
JLAB FEL setup I: regeneration experiment JLAB FEL setup I: regeneration experiment
magnet 2 T; 1 m (?) detector light shield φ’s produced at JLAB FEL
“parasitic “
2B
2L
2/4
Prob Prob for photon for photon-
axion prod prod g = coupling constant (1/M) g = coupling constant (1/M) B = magnetic field B = magnetic field L = magnet length L = magnet length
1 P
2 ε
r+2)/2
yield (#/s) yield (#/s)
n n = photon flux (#/s) = photon flux (#/s) P1 (P2) P1 (P2) = production (regeneration) probability = production (regeneration) probability ε ε = detection efficiency = detection efficiency ∆Ω ∆Ω/ /Ω Ω = solid angle = solid angle N Nr
r =
= number of reflections number of reflections
B B-
field parallel to photon polarization photon photon-
axion coherence coherence large magnetic field large magnetic field shield detector from field; vacuum vessel shield detector from field; vacuum vessel
2
Hz 1 ~ / s ' 10 6 MHz 75 pulse / mJ . 1 10 4
2 23 11 2 2 2
≥
∆Ω
= × = = =
−
ε γ P n Y s N L B g P
axion-photon conversion probability, P JLAB FEL photon rate, n photon regeneration rate estimate, Y 2 T; 1 m magnet ε ~ 0.5; ∆Ω/Ω ~ 0.5
B Br
r (Tesla)
(Tesla) L Lr
r (meters)
(meters) g (eV g (eV-
1)
) rate (Hz) rate (Hz) 1.0 1.0 1.0 1.0 10 10-
15
.005 .005 1.0 1.0 1.0 1.0 5 x 10 5 x 10-
15
3.0 3.0 1.5 1.5 0.8 0.8 10 10-
15
.01 .01 1.5 1.5 0.8 0.8 5 x 10 5 x 10-
15
4.2 4.2 uses: dipole magnet at end of straight section: 1.0 m uses: dipole magnet at end of straight section: 1.0 m long and 0.31 Tesla long and 0.31 Tesla 100 kW (1 100 kW (1 eV eV) FEL laser light ) FEL laser light q.e q.e. ~ 0.3; detector . ~ 0.3; detector accep accep ~ 0.9 ~ 0.9
Hamamatsu R5509 PMT FEL tune dark current > nA
Rockwell Scientific Hawaii 1RG Rockwell Scientific Hawaii 1RG – – for example for example
< < 4 4 mW mW @ 100 kHz @ 100 kHz Power Dissipation Power Dissipation < < 15 e 15 e-
CDS @ 100 kHz Read noise (array mean) Read noise (array mean) < < 0.1 e 0.1 e-
/sec (77K, 2.5 µ µm) m) Dark Current (array mean) Dark Current (array mean) > > 95% 95% Pixel Operability Pixel Operability > > 100,000 e 100,000 e-
Charge storage capacity > > 65% 65% Quantum Efficiency (array Quantum Efficiency (array mean) mean) > > 30K 30K Operating temperature Operating temperature 0.3 0.3 -
5.3 µ µm m Spectral range Spectral range Signal: 1, 4, 32 selectable Signal: 1, 4, 32 selectable Guide Window and Reference Guide Window and Reference Output ports Output ports > > 98% 98% Fill factor Fill factor 18 18 µ µm m Pixel Pitch Pixel Pitch 1024 x 1024 1024 x 1024 Total pixels Total pixels 100 kHz to 5 MHz (continuously 100 kHz to 5 MHz (continuously adjustable) adjustable) Pixel readout rate Pixel readout rate Ripple Ripple Readout mode Readout mode SFD SFD Detector input circuit Detector input circuit MBE MBE HgCdTe HgCdTe or
Si PIN PIN Detector technology Detector technology Rockwell Rockwell FPAs FPAs FPA Parameter FPA Parameter
dark current and read noise quantum efficiency spectral range
begin with this? (on hand) begin with this? (on hand) SBIG ST SBIG ST-
237A
15 sec Parallel 75% 20,000e- 15e- 5e-/p/s 38 arcmin 18 3.7 x 4.9 7.4u 325,000 657 x 495 ST-237A 0.8 sec USB 2.0 83% 100,000 e- 17e- 1e-/p/s 52 arcmin 32 4.6 x 6.9 9u 390,000 765 x 510 ST-402ME Full Frame Transfer Compute r Interface Peak QE Full Well Capacity Read Noise Dark Current at 0 C. Diag FOV 11" Fastar (544mm FL) CCD Area mm2 CCD Size mm Pixe l Size Number
Pixel Array Camera
www.desy.de/~ringwald couple polarized laser couple polarized laser light with magnetic light with magnetic field field Sikivia Sikivia (1983); (1983); Ansel Ansel’ ’m m (1985); Van Bibber et (1985); Van Bibber et al (1987) al (1987)
2 2 2 2
4 4 sin 4 1 ⎪ ⎪ ⎭ ⎪ ⎪ ⎬ ⎫ ⎪ ⎪ ⎩ ⎪ ⎪ ⎨ ⎧ ⎟ ⎟ ⎠ ⎞ ⎜ ⎜ ⎝ ⎛ ≈
→
ω ω
ϕ ϕ ϕ γ
L m L m gBL P
ps – photon (or photon-ps) conversion probability
photon-ps coherence; {} ~ 1 mφ
2 < 4ω/L
coherence PVLAS ; BFRT
see web site: www.desy.de/ ~ringwald
ps ps-
photon coherence -
LIPSS
ω = 1.2 eV (1064 µ)
(same as PVLAS)
generation magnet ~1.2 m regeneration magnet ~ 1.0 m
( )
2 2 2 2
4 4 sin 4 1 ⎪ ⎪ ⎭ ⎪ ⎪ ⎬ ⎫ ⎪ ⎪ ⎩ ⎪ ⎪ ⎨ ⎧ ⎟ ⎟ ⎠ ⎞ ⎜ ⎜ ⎝ ⎛ ≈
→
ω ω
ϕ ϕ ϕ γ
L m L m gBL P
vertical - axis
PVLAS and BFRT: photon PVLAS and BFRT: photon-
axion coherence coherence
plots from K. McFarlane magnet length a limitation in BFRT
2
PVLAS and BFRT: photon PVLAS and BFRT: photon-
axion coherence coherence
plots from K. McFarlane magnet length a limitation in BFRT
2
LIPSS : IR FEL 1.6 µ ; 1.06 µ
uncertainty relation uncertainty relation – – ultralow ultralow count rates count rates
Heitler Heitler (1954); Rev. Mod. Phys 75, 777 (2003) (1954); Rev. Mod. Phys 75, 777 (2003)
– – ∆ ∆n n∆φ ∆φ > 1 > 1
n number of quanta detected n number of quanta detected φ φ phase of detected radiation phase of detected radiation
use use focussing focussing lens at end of regeneration magnet lens at end of regeneration magnet
– – focus on small pixel area focus on small pixel area better S/N better S/N
use new use new rf rf structure in upstairs lab with two structure in upstairs lab with two powerful magnets powerful magnets
– – purchase 2 ea ~ 0.5 m long, ~ 2 T magnets purchase 2 ea ~ 0.5 m long, ~ 2 T magnets
use B field of electron beam use B field of electron beam
– – can get ~100 T close to electron beam can get ~100 T close to electron beam – – probably too small an effect probably too small an effect
. . . . . .
focussing lense pixel array S/N ~ 1 per pixel
gap: 7.9 cm magnetic length: 0.42 m design field intergral: 5.92 KGauss. current 223.24 A have 4 extra magnets and their stands in Magnet Test and 2 mounted to stands in the FEL UV Line. a rarely used power supply for the 2G dump spectrometer is available in the FEL for quick response at slightly lower max
max field at 0.8 Tesla 1.5 Tesla with shims the GWs are 0.6 or so meters long
with current setup, IR light . . . with current setup, IR light . . .
JLAB in ~ 1 day with I R FEL
– – fast (can time relative to fast (can time relative to rf rf structure of beam) structure of beam)
reduce noise reduce noise
– – good quantum efficiency good quantum efficiency – – experience experience
– – axion axion-
photon coherence – – probability ~ L probability ~ L2
2
photon regeneration from photon regeneration from pseudoscalars pseudoscalars at x at x-
ray lasers
Rabadan Rabadan, , Ringwald Ringwald, , Sigurdson Sigurdson hep hep-
ph/0511103
JLAB in ~ 1 hour with UV FEL
A.
Ringwald; hep ; hep-
ph/0511184 K.
Zioutas et.al et.al., PRL 94, 121301 (2005) ., PRL 94, 121301 (2005)
JLAB in ~ 1 hour with UV FEL
– – 1.06 1.06 µ µ and 1.64 and 1.64 µ µ IR light IR light
– – 1.5 T, 1.0 meter long, acceptance ~ 0.8 1.5 T, 1.0 meter long, acceptance ~ 0.8
– – ~10% ~10% q.e q.e., low dark current (cps), on hand ., low dark current (cps), on hand
A.
Afanasev alerted alerted okb
> 2 years ago of importance of measurement measurement
made initial approaches to FEL people (Boyce, Shinn, etc), Shinn, etc), axion axion experts (Rosenberg); very low level experts (Rosenberg); very low level initial meetings began at Hampton ~ year ago; VFWM initial meetings began at Hampton ~ year ago; VFWM discussed; HU laser experiment discussed. discussed; HU laser experiment discussed. PVLAS result: PVLAS result: Afanasev Afanasev again emphasized importance again emphasized importance
experimentalists joined discussions experimentalists joined discussions initial meeting of interested Hampton and JLAB scientists initial meeting of interested Hampton and JLAB scientists (Williams, Boyce, etc); more serious now (Williams, Boyce, etc); more serious now series of meetings at JLAB; talks at TAWG and JLAB series of meetings at JLAB; talks at TAWG and JLAB
A.
Afanasev – – particle/nuclear theorist particle/nuclear theorist G.
Biallas – – FEL experimentalist FEL experimentalist
– FEL experimentalist FEL experimentalist O.K. Baker O.K. Baker – – particle/nuclear experimentalist particle/nuclear experimentalist
– graduate student graduate student
– graduate student graduate student
– particle experimentalist particle experimentalist J.T. J.T. Seo Seo – – optics experimentalist
– particle experimentalist particle experimentalist S.
Shukui – – FEL experimentalist FEL experimentalist V.
Vassilakopoulos – – particle experimentalist particle experimentalist
– optics experimentalist
Q.
Yiang – – optics experimentalist
axion axion search not just a shot in the dark now!! search not just a shot in the dark now!!
– – PVLAS result can be tested; new data point from PVLAS result can be tested; new data point from LIPSS LIPSS
can perform regeneration experiment to test can perform regeneration experiment to test PVLAS result at JLAB FEL PVLAS result at JLAB FEL
– – can reach interesting region of parameter space with can reach interesting region of parameter space with IR FEL IR FEL – – can perform definitive experiment with UV FEL can perform definitive experiment with UV FEL
this is particle physics at the FEL this is particle physics at the FEL
– – constraints on a new mass scale in particle physics constraints on a new mass scale in particle physics
PeV PeV scale!! scale!!