CAST FRC-D th MEETING OF THE FINANCE REVIEW COMMITTEE FOR CAST CAST status report and perspectives Konstantin Zioutas, for the CAST collaboration CERN 21 st September 2010 (bld. 60/5-012)

Status Report of CAST 98 th SPSC meeting 28 th September 2010 T. P APAEVANGELOU, FOR THE CAST C OLLABORATION 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

 B X  virtual α CAST

Axion–photon coupling vs. QCD-inspired axion rest mass

CDM HDM CDM J.E. Kim, G. Carosi, Rev. Modern Phys. 82 (2010) 557

Data Analysis CAST Status Report, Theopisti Dafni (UNIZAR), 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 : g a  ~ 2  GeV -1 for 0.39 eV < m a < 0.76 eV ( )

Exclusion limit (95% CL) from the three Micromegas detectors  2008 data

Detectors + XRT Detectors + XRTelescope ✔+ ● Run in 2009 and 2010 ● Study of the 3 He dynamics ! ● The shutdown He incidence Magnet electrical insulation tests QPS Magnet Power Converter improvements Magnet movement control system maintenance ….. ● Slow Control ● Upgrades of the 3 He System Filling 2008 Gaps! ● ● ( ✔)

Density profile along the two cold bores of the CAST magnet for different pressures of the 3 He gas at ~1.8K. Computational fluid dynamics simulations and experimental data agree within ppm. For comparison, a naïve calculation of the density results in deviations from data of as much as ~11% mbar mbar 3 He gas dynamics

Effective coherence length of the magnetic field during 2009 & 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. 3 He gas dynamics

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 CAST Status Report, Theopisti Dafni (UNIZAR), Diploma thesis

One frame from the Sun filming. Alignment of the camera with the solar center 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.

BaRBE optical telescope (optical fiber exiting on the right). Plunger rod (left) with vacuum manipulator assembly

First results from the CAST 3 He phase. S. Aune et al., (The CAST collaboration), Publication in preparation.

Year Calendar days Tracking days Settings covered Mass Range [eV/c 2 ] Comments dP dP Step decreasing with time due to leaks dP ~ ~ Missing 105 settings dP (assuming 70% data taking efficiency) TOTAL 526 (80% original) 385 (90% original) % of the proposed pressure settings covered 2011 ~140~ dP (assuming 70% data taking efficiency) Summary of CAST data taking in the period and prospects for 2011

Search for 14.4 keV solar axions emitted in the M1-transition of 57 Fe with CAST Search for 14.4 keV solar axions emitted in the M1-transition of 57 Fe with CAST The CAST collaboration, S. Andriamonje et al, JCAP12(2009)002 1 st CAST by-product   Upper limit on the product g a γ g aN eff vs. m axion imposed by the search for 57 Fe (14.4 keV) solar axions  m axion < 0.03 eV/c 2   Exclusion plot in the g a γ vs. m axion plane. The limit achieved by CAST is given for two values of the parameter.

The CAST Collaboration, JCAP 1003:032, nd CAST by-product Search for solar axions from nuclear decays with CAST  MeV Tracking&background Tracking & background energy spectra for the 3 energy regions.

 7 th  7 th Patras workshop on axions, WIMPs & WISPs Place ?? / Greece 26 th June – 3 rd July 2011 The workshop in Zurich was supported by CERN CERN CHIPP DESY IPPP/Durham University University of Patras Zurich University  growing interest!

Conclusions >> past The first preliminary results of the 3 He data analysis show that the high rest ≤ 1.16 eV/c 2 mass range (≤ 1.16 eV/c 2 ) 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 3 He 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 3 He 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: 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  low threshold XMM/Newton  after axion run finishes without magnet

1 m Ø mirror <30eV Reflectivity: <30eV Solar paraphotons ?

2 XMM-Newton Telescope  recycled state-of-the-art XMM mirror module Collecting area: ~1900cm 2 (<150 eV), ~1500cm 2 2 keV), ~900cm 2 7keV), ~350 cm 2 10 keV). For paraphotons & superCAST  ~1eV – 15keV XRT & ~60mm CCD  2 x (1-2) MEUROs and 4-5 years delivery

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 χ 2 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 LH scale: mixing parameter χ=10 -5 RH scale: mixing parameter χ= OPAQUE SUN, CORONAFLARE OPAQUE SUN, CORONA, a large but not exceptional FLARE (assuming flare photon flux 10 5 cm -2 s -1 ev -1 ) H. Bräuninger, M. Davenport, S.N. Gninenko, V.A. Matveev, S. Troitsky, K. Zioutas, in preparation flare

Conceptual design study of a future axion helioscope ? “superCAST” ? CAST mobilized CERN magnet experts... work in progress 

Towards superCAST?  novel magnet, detectors and optics!  10x better...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.

0.62 m 1.62 m ATLAS type Magnet: 8-Toroid

Sol lucet omnibus