Transcript CAST - CERN Indico

CAST FRC-D 2010-30
8th MEETING OF THE FINANCE REVIEW COMMITTEE FOR CAST
CAST status report and perspectives
Konstantin Zioutas,
for the CAST collaboration
CERN
21st September 2010
(bld. 60/5-012)
Status Report
of
CAST
98th SPSC meeting 28th September 2010
T. PAPAEVANGELOU,
FOR THE
CAST COLLABORATION
CEA Saclay
CERN
Dogus University
Lawrence Livermore National Laboratory
Max-Planck-Institut for Solar System
Research/Katlenberg-Lindau
Max-Planck-Institut für extraterrestrische Physik
Max-Planck-Institut für Physik
National Center for Scientific Research Demokritos
NTUA Athens
Institut Ruđer Bošković
Institute for Nuclear Research (Moscow)
TU Darmstadt
University of British Columbia
University of Chicago
Universität Frankfurt
Universität Freiburg
University of Patras
University of Thessaloniki
Universita di Trieste
Universidad de Zaragoza
CAST
axion source
axion detection
H. Primakoff
1951
CAST
α
gvirtual
X
B
g
Axion–photon coupling vs. QCD-inspired axion rest mass
CDM
CDM
HDM
J.E. Kim, G. Carosi, Rev. Modern Phys. 82 (2010) 557
http://rmp.aps.org/pdf/RMP/v82/i1/p557_1
Data Analysis
The data analysis is ongoing.
No evidence of any axion signal has been seen.
Complicated analysis for 2008 exclusion plot due
to the leak, work in progress.
Expected sensitivity :
gag~ 2 10-10 GeV -1
for 0.39 eV < ma< 0.76 eV
(27.09.2009)
CAST Status Report, Theopisti Dafni (UNIZAR), 29.09.2009
7
Exclusion limit (95% CL) from the three Micromegas detectors
 2008 data
Detectors + XRTelescope
+
● Run in 2009 and 2010
● Study of the 3He dynamics !
● The shutdown 2009-2010
3He incidence
Magnet electrical insulation tests
QPS
Magnet Power Converter improvements
Magnet movement control system maintenance
…..
● Slow Control
● Upgrades of the 3He System
Filling 2008 Gaps!
●
●
●
(✔)
✔
3He
gas dynamics
83.39 mbar
35.85 mbar
Density profile along the two cold bores of the CAST magnet for different pressures of the 3He gas at ~1.8K.
Computational fluid dynamics simulations and experimental data agree within 200-300 ppm. For
comparison, a naïve calculation of the density results in deviations from data of as much as ~11% .
3He
gas dynamics
Effective coherence length of the magnetic field during 2009 & 2010. The maximum coherence
length is 926 cm, and the derived shorter coherence length with increasing density inside the
cold bores have to be taking into account in calculating CAST performance.
Comparison of March 2010 GRID with the September 2007 (left) and 2002 (right)
situation. The required precision of 1 arcmin is indicated by the green circle, while
the red one represents the 10% of the sun projected at 10 m.
Filming 2009
Star filming:
Solar filming 24.09.2009
• Ideal weather conditions
• Analysis is preliminary, but the first
results are encouraging
CAST Status Report, Theopisti Dafni (UNIZAR), 29.09.2009
• Same principle, same ‘classic’ setup
• Pointing at Stars
• Possible throughout the year
Diploma thesis
One frame from the Sun filming.
Alignment of the camera with the solar center.
2010
1300
y (pixels)
1350
alignment
1400
1450
Difference between pointing (solar center
from images) and alignment (axes of V1
magnet bore) from all images taken during
one filming  ~15% of the solar radius.
1500
pointing
2050
2100
x (pixels)
2150
2200
BaRBE optical telescope (optical fiber exiting
on the right).
Plunger rod (left) with vacuum manipulator assembly
First results from the CAST 3He phase.
S. Aune et al., (The CAST collaboration),
Publication in preparation.
Summary of CAST data taking in the period 2008-2010 and prospects for 2011
Year
Calendar
days
Tracking
days
2008
201
127
252
0.39-0.65
168 settings @ 1.0dP
85 settings @ 1.2dP
Step decreasing with time due to leaks
2009
149
124
247
0.64-0.85
247 settings @ 1.4dP
2010
58
118
53
~81
105
~162
0.39-0.65
0.85-0.99
Missing 105 settings 2008
122 settings @ 1.4dP (assuming 70%
data taking efficiency)
TOTAL
526 (80%
original)
385 (90%
original)
766
0.39-0.99
80% of the proposed pressure settings
~140
~98
196
2011
Settings Mass Range
covered
[eV/c2]
Comments
covered
0.99-1.16
196 settings @ 1.4dP (assuming 70%
data taking efficiency)
Search for 14.4 keV solar axions emitted in the M1-transition of
57Fe
with CAST
 Upper limit on the product gaγgaNeff vs. maxion imposed
by the search for 57Fe (14.4 keV) solar axions 
maxion< 0.03 eV/c2
1st CAST by-product
 Exclusion plot in the gaγ vs. maxion plane.
The limit achieved by CAST is given for
two values of the parameter
.
The CAST collaboration, S. Andriamonje et al, JCAP12(2009)002
Search for solar axions from nuclear decays with CAST  0.3 - 50 MeV
Tracking & background energy spectra for the 3 energy regions.
2nd CAST by-product
The CAST Collaboration, JCAP 1003:032, 2010
The workshop in Zurich was supported by
• CERN CHIPP DESY IPPP/Durham University
• University of Patras Zurich University

7th Patras workshop on axions, WIMPs & WISPs
Place
?? / Greece
26th June – 3rd July 2011
 growing interest!
Conclusions
>> past
•
The first preliminary results of the 3He data analysis show that the high rest
mass range (≤ 1.16 eV/c2) can be investigated with the targeted sensitivity.
•
CAST has not observed a direct solar axion signal, but has provided world class
limits for axions and WISPs including paraphotons.
•
In order to fully exploit the discovery potential of the 3He system, CAST plans
to extend the operation of the experiment in the first half of 2011 to
complete the missing ~15% in axion rest mass. The Collaboration is
requesting this extension to complete the initial basic program of CAST.
• "The 3He phase was and is a challenging project for CAST,
which turned out to be far more complex than even the experts had imagined“.
Envisaged measurements with upgraded CAST: 2011-2013
•
Solar axion & Chameleon search  improve own world best limit / most sensitive
search
 low noise MM
 low thresshold detectors
•
CAST as paraphoton helioscope  state-of-the-art
•
Low energy axions or other WISPs from the Sun (E ≳ 2eV)
+ linear polarization
+ Fabry-Perot resonator
•
Observation of stellar X-ray sources with CAST ?
•
R&D towards New Generation Axion Helioscope (detectors, optics, magnet)
•
more?
 upgraded / new detectors
 extensive interventions
CAST = Cern pAraphoton Solar Telescope
Mirror(s)
XRT present
XMM/Newton


low threshold
after axion run finishes without magnet
Solar paraphotons?
1 m Ø mirror
Reflectivity: <30eV
2 XMM-Newton Telescope  recycled state-of-the-art
For paraphotons
&
superCAST
 ~1eV – 15keV
XRT & ~60mm CCD
 2 x (1-2) MEUROs
and 4-5 years delivery
XMM mirror module
Collecting area:
~1900cm2 (<150 eV), ~1500cm2 (@ 2 keV),
~900cm2 (@ 7keV), ~350 cm2 (@ 10 keV).
Optically thick part: paraphoton flux calculated previously.
• Except for masses >1 eV, our results reproduce previous results.
• The difference with previous results at 1 eV < m < 200 eV is within
an order of magnitude
New results:
• calculation of the flux from the transparent part (mostly corona)
• estimate of the flux from a flare
• Resonant production for large regions in the corona
important enhancement of the total flux of light paraphotons
 All fluxes scale roughly as χ2 for the mixing parameter χ.
H. Bräuninger, M. Davenport, S.N. Gninenko, V.A. Matveev, S. Troitsky, K. Zioutas,
in preparation
Compilation of solar paraphoton fluxes at 1 keV
flare
LH scale:
mixing parameter
χ=10-5
RH scale:
mixing parameter
χ=10-10
OPAQUE SUN, CORONA, a large but not exceptional FLARE
(assuming flare photon flux 105 cm-2 s-1 ev-1)
H. Bräuninger, M. Davenport, S.N. Gninenko, V.A. Matveev, S. Troitsky, K. Zioutas,
in preparation
Conceptual design study of a future
axion helioscope
? “superCAST” ?
CAST mobilized CERN magnet experts
... work in progress 
Towards superCAST?
 10x better
 novel magnet, detectors and optics!
...more people & M€
Towards the new generation of axion helioscopes (CAST)
T. Papaevangelou, (The CAST Collaboration),
Presented in May 2009, in New Opportunities in the Physics Landscape at CERN.
ATLAS type Magnet:
8-Toroid
0.62 m
1.62 m
ATLAS type Magnet:
8-Toroid
ATLAS type Magnet:
8-Toroid
Sol lucet omnibus