Status and physics prospects for the International AXion Observatory IAXO Igor G Irastorza Universidad de Zaragoza
WkhWorkshop "Vist as in AiAxion Physi cs” AilApril 2012 Institute for Nuclear Theory, Seattle, University of Washington Outline
Outline: – Axions: motivation,motivation, theory,theory, cosmologycosmology.. – SlSolar axi ons & Talk partially based on the axion helioscope concept JCAP 06 (2011) 013 ––PreviousPrevioushelioscopes & CAST ––IAXOIAXO project:project: technicalprospects for a new helioscope . Magnet . XX--rayrayoptics . Low background detectors – Sensitivity prospects – Status of project ––ConclusionsConclusions
INT Washington, April 2012 Igor G. Irastorza / Universidad de 2 Zaragoza AXION motivation
Strong CP problem: why strong interactions seem not to violate CP? – CP violating term in QCD is not forbidden . But neutron electric dipole moment not observed. Natural answer if Peccei-Quinn mechanism exist. – New U(1) gl lob al symmet ry spontlbktaneously broken.
As a result, new pseudoscalar, neutral and very light particle is predicted, the axion. It couples to the photon in every model. PRIMAKOFF EFFECT
INT Washington, April 2012 Igor G. Irastorza / Universidad de 3 Zaragoza AXION motivation: Cosmology
Axions are produced in the earlyyy Universe by a number of processes: – Axion realignment – Decay of axion strings NONNON--RELATIVISTICRELATIVISTIC – Decay of axion walls (COLD) AXIONS
In general, Range of axion masses of 10--66 ––1010--33 eV are of interest for the axionto be the (main component of the) CDM.
– Thermal production RELATIVISTIC (HOT) AXIONS
In order to have substantial relativistic axiondensity, the axionmass must be close to 1 eV.eV. (ma >1.02 eV gives densities too much in excess to be
compatible with latest CMB data) Hannestad et al, JCAP 0804 (2008) 019 [0803.1585 (astro-ph)]
INT Washington, April 2012 Igor G. Irastorza / Universidad de 4 Zaragoza Axion parameter space
Astroppyhysical hints for ALPs
Axions as HDM
CDM CDM CDM White “anthropic window” Defects dominate “classical window” Dwarfs hep-ph/1202-5851 Vaxuum mis. + defects INT Washington, April 2012 Igor G. Irastorza / Universidad de 5 Zaragoza Beyond axions
Hidden photons Miniccagedharged AXIONS Chamaleons / paraphotons ALPS particles
WISPs (WklWeakly itinteracti ng Slim PtilParticle)
Diverse theory motivation ––HigherHigher scale symmsymm.. breaking ––StringStringtheory – DM / DE candidates – Astrophysical hints
Generic Axion- Axion-likelikeparticles ((ALPsALPs)) parameterspace
INT Washington, April 2012 Igor G. Irastorza / Universidad de 6 Zaragoza Detecting axions Relic Axions ––AxionsAxionsthat are part of galactic dark matter halo: . AAionxion Halosc opes
Solar Axions – Emitted by the solar core. . Crystal detectors . Axion Helioscopes (CAST IAXO)
AiAxions ithlbin the lab . “Light shinning through wall” experiments . Vacuum birrefringence experiments
INT Washington, April 2012 Igor G. Irastorza / Universidad de 7 Zaragoza Solar Axions
SlSolar axi ons prod uced db by ph otonoton--toto-- axion conversion of the solar plasma photons
Solar axion flux [van Bibber PRD 39 (89)] [CAST JCAP 04(2007)010]
Solar physics + Primakoff effect
Only one unknown
parameter ga
Igor G. Irastorza / Universidad de INT Washington, April 2012 Zaragoza 8 Axion Helioscope principle
Axion helioscope [Sikivie [Sikivie,, PRL 51 ((83)]83)]
AXION PHOTON CONVERSION
INT Washington, April 2012 Igor G. Irastorza / Universidad de 9 Zaragoza COHERENCE 1 Axion Helioscopes Previous helioscopes: – First implementation at Brookhaven (just few hours of data) [Lazarus et at. PRL 69 (92)] – TOKYO Helioscope (SUMICO): 2 .3 m long 4 T magnet
Presently running: – CERN Axion Solar Telescope (CAST) INT Washington, April 2012 Igor G. Irastorza / Universidad de 10 Zaragoza CAST experiment @ CERN Decommissioned LHC test magnet (L=10m, B=9 T) Moving platform ±8°V ±40°H (to allow up to 50 days / year of alignment) 4 magnet bores to look for X rays 3 X rays detector prototypes being used. X ray Focusing System to increase signal/noise ratio.
LHC test magnet
Micromegas TPC (<2007) & 2 Micromegas CCD/Telescope (>2008)
INT Washington, April 2012 Igor G. Irastorza / Universidad de 11 Zaragoza Low background x-ray detectors
Microbulk Micromegas ––LowLowradioactivity materials [[Astropart.PhAstropart.Ph.. 2011,34,354] ––HighHighgranularity readout powerful offline discrimination of events in gas X-ray window – Shielding techniques
Shielding Readout Copper & pattern kapton
56 mm
INT Washington, April 2012 Igor G. Irastorza / Universidad de 12 Zaragoza Micromegas detectors @CAST@ CAST Since 2008 2 new Micromegas detectors replaced the multiwire TPC in the sunset side. – Better shielding At sunrise side. The Micromegas detector substantially upgraded: – microbulk, shielding, monitoring, frontal calibration, flow controller, In overall increasingly better Sunset backgrounds & sensitivity Micromegas
Sunrise Micromegas
INT Washington, April 2012 Igor G. Irastorza / Universidad de 13 Zaragoza Micromegas detectors @CAST@ CAST
New detectors for 2012 New Sunset design – New microbulkMicromegas for sunset side – Improved shielding . Thickness . Coverage ––SomeSome components replaced ((radiopurityradiopurity)) – Possible muon veto Tests of lowbackground strategies developed Setup to be mounted at CAST Test mounting neetxt weekee ! See talk (Zaragoza) T. Dafni INT Washington, April 2012 Igor G. Irastorza / Universidad de 14 Zaragoza CAST X -ray telescope
CAST innovationof the “helioscope concept”
Wolter I typegrazing incident optics (prototype (prototype for ABRIXAS mission)mission) From Ø43 mm ( magnet bore) Ø3mmspot3 mm spot improves signal to background ratio
INT Washington, April 2012 Igor G. Irastorza / Universidad de 15 Zaragoza CAST X -ray telescope
Tracking data Signal simulation Spot from the telescope on the CCD detector Determination of the spot position by calibrations and precise alignment of tltelescope. Counts inside the spot compatible with background level
INT Washington, April 2012 Igor G. Irastorza / Universidad de 16 Zaragoza 16 Buffer gas to go to higher masses
X ray detector Transverse magnetic field (B) X ray axions A
L Extending the coherence to higher axion masses... •Coherence condition ( qL << 1) is recovered for a narrow mass range around m
3 Ne: number of electrons/cm : gas density (g/cm 3) See talk J. Ruz INT Washington, April 2012 Igor G. Irastorza / Universidad de 17 Zaragoza Latest CAST results
Results from first 3He (2008) data (red line). Masses 0. 39 – 0650.65 eV excluded down to 2-25x2.5 x 10--1010 GeV--11 S. Aune et al. (CAST collaboration) Touching KSVZ benchmark models for the first PRL 107 (2011) 261302 (arXiv:1106.3919v1) time He3 data up to 1.15 eV taken, being analyzed.
INT Washington, April 2012 Igor G. Irastorza / Universidad de 18 Zaragoza Latest CAST results: preliminary
All 3He data (2008 -11) in progress. Masses up to 1.15 eV Final He3 result paper in preparation
INT Washington, April 2012 Igor G. Irastorza / Universidad de 19 Zaragoza Future prospects
CAST Near term future: – CAST will revisit phase II He4 in 2012 and again the vacuum phase I in 2013 -14 with better detectors better sensitivity. – Search in parallel for exotica: chamaleons,chamaleons, paraphotons,paraphotons, non standard axions (visible wavelenghts)
Longer term future: – Studies for a new generation axion helioscope (>1 order of magnitude more sensitive than CAST):
The International Axion Observatory IAXO
INT Washington, April 2012 Igor G. Irastorza / Universidad de 20 Zaragoza The International Axion Observator y IAXO: towards a new generationaxion helioscope
Ingredients of a successful helioscope CAST is established as a reference result in experimental axion physics CAST PRL2004 most cited experimental paper in axion physics No other technique can realistically improve CAST in such wide mass Large & powerful magnet... range.
Next step IAXO, a new gener ation aionaxion helioscope ...X-ray optics,...
Build up on CAST innovations to impro ve the helioscope techniq ue …
...and low background detectors
INT Washington, April 2012 Igor G. Irastorza / Universidad de Zaragoza 21 Axion Helioscopes FOM
3 elements drive the sensitivity of anaxion helioscope
X-RAY X-RAY MAGNET OPTICS DETECTORS
INT Washington, April 2012 Igor G. Irastorza / Universidad de 22 Zaragoza IAXO sensitivity scenarios
Scenario 1 Scenario 2 Scenario 3 Scenario 4
IGI et al. JCAP 016 (2011)
INT Washington, April 2012 Igor G. Irastorza / Universidad de 23 Zaragoza New magnet for IAXO
CAST enjjyoys one of the best existing magnets than one can “recycle” for axion physics (LHC test magnet)
Only way to make a step further is to built a new magnet, specially conceived for IAXO.
After prel. study best option seems to be a toroidal configuration: – Much bigger aperture than CAST: ~0.5~0.5--11 m per bore – Relatively Light (no iron yoke) – Bores at room temperature (?) Cross section of the magnet
INT Washington, April 2012 Igor G. Irastorza / Universidad de 24 Zaragoza Inspired by ATLAS… ?
INT Washington, April 2012 Igor G. Irastorza / Universidad de 25 Zaragoza IAXO magnet: 1st concept
Total R = 2 m Bore diameter = 600 mm N bores = 8 Average B in bore = 4 T (in critical surface) MFOM = 770
IAXO scenario2 conservative Surpass IAXO scenario3 is possible Further optimization ongoing See talk I. Shilon INT Washington, April 2012 Igor G. Irastorza / Universidad de 26 Zaragoza X-ray optics for IAXO
CAST xx--rayray optics “recycled” from xx--rayray astronomy – High technology, expensive, “unique” objects, due to exquisite imaging properties required for x-x-rayray astronomy.
IAXO optics: – Exquisite imaging not required – BUT, large area (~ 22m m2) to be covered. Require fabrication of dedicated optics cost effective solution. – Good throughput (0.3 ––0.5)0.5) – Small focal point (~1 cm2)
Pursued solution: thermallythermally--formedformed glass su bstr ates optic s – Successfully used in NUSTAR – Leverage existing infrastructure. Minimize costs & risks
INT Washington, April 2012 Igor G. Irastorza / Universidad de 27 Zaragoza Thermally-formed glass substrates
NASA has recently built NuSTAR,NuSTAR, a hard x-ray telescope
NuSTAR uses thin glass substrates coated with multilayers to enhance reflectivity up to 80 keV
The speci ali zed t ooli ng t o sh ape th e NSTARNuSTAR optics assembl y machi ne substrates and assemble the optics is now available NuSTAR telescope
Hardware can be easily configured to make optics with a variety of designs and sizes
Key institutions in NuSTAR optics: LLNL, See talk UClU. Columbi biDTUDa, DTU Denmark kAlliIAXO!. All in IAXO ! M. Pivovaroff 28 INT Washington, April 2012 Igor G. Irastorza / Universidad de Zaragoza Ultralow-b detectors for IAXO
Goal: at least 10--77 c/c/keVkeV/cm/cm2/s, dt10down to 10-8 c/kVkeV/cm2/if/s if simulations possible. Work ongggoing: – Experimental tests with current detectors at CERN, Saclay & Zaragoza – Especially: underground setup at Canfranc Lab – Simulation works to build up a background model ––DesiDesign a new detector with improvements implemented R&D low background Micromegas Latest Micromegas: x20 improved History of background improvement of Micromegas detectors at CAST background ––ShieldingShielding 2003 Nominal values at CAST – Radiopurity. New manufacturingtechnique 2004 2006 (microbulk readouts) ––MoreMore powerful offline cuts 2008-10 Tests in controlled conditions underground at Canfranc: – Better shielding coverage – Thicker shielding
Backgrounds around 2x10-7 c/keV/s/cm2 with improved shielding ~ x30 better than CAST Pathfinder detector+optics
CllbCollaborati on SlSaclayay,, Zaragoza, LLNL, DTU, U. Columbia Small xx--raray optics (~5 cm aperture) ––FabricatedFabricatedpurposely using thermally formed glass substrates Micromegas low background detector: – Apply lessons learned in R&D: compactnesscompactness,, better shieldingshielding,, radiopurit yy,…,… ––GoalGoal:: 10--77 c/c/keVkeV/s/cm2/s/cm2 or better
To be operated in CAST in 2013 Tests of techniques and know-know-howhow for IAXO See talk T. Dafni INT Washington, April 2012 Igor G. Irastorza / Universidad de 31 Zaragoza IAXO: Possible CtlConceptual DiDesign (LLNL)
Igor G. Irastorza / Universidad de INT Washington, April 2012 32 Zaragoza IAXO: Possible CtlConceptual DiDesign (LLNL)
Igor G. Irastorza / Universidad de INT Washington, April 2012 33 Zaragoza IAXO: Possible CtlConceptual DiDesign (LLNL)
X‐ray optics
Igor G. Irastorza / Universidad de INT Washington, April 2012 34 Zaragoza IAXO: Possible CtlConceptual DiDesign (LLNL)
Detectors & shieldings
Igor G. Irastorza / Universidad de INT Washington, April 2012 35 Zaragoza IAXO sensitivity prospects
Factor 8 to 30 better in 6 ga (4000 to 10 in signal strength!!)
Conservative scenario Realistic scenario
Optimistic scenarios
INT Washington, April 2012 Igor G. Irastorza / Universidad de 36 Zaragoza IAXO sensitivity prospects
Much larger QCD axion region explored
IAXO
IAXO ppprospects
In combination with dark Astrophysical matter axion searches a hints for ALPs big part of the QCD axion modldel region could ldb be explored next decade.
INT Washington, April 2012 Igor G. Irastorza / Universidad de 37 Zaragoza The cooling of white dwarfts (Isern et al. 2008,2010) Luminosity function (WD’s (WD’sper unit magnitudemagnitude)) altered by axion cooling Claim of detection of new cooling mechanism (Isern 2008 ) AxionAxion--electronelectron coupling of ~1x10--1313 ( axion massesof 2-2-55 meVor larger) fits data .
DFSZ axion (cos=1)
INT Washington, April 2012 Igor G. Irastorza / Universidad de 38 Zaragoza The cooling of white dwarfs
meV masses seem out of reach of EXTRA bremstrahlung emission ~50 times even an improved axion helioscope… helioscope… larger than standard Primakoff emission BUT Axion-electron coupling provides extra axion emission from the SunSun…… Extra emission concentrated at lower energies (~1 keV)
Such axion could produce a detectable signal in IAXO
INT Washington, April 2012 Igor G. Irastorza / Universidad de 39 Zaragoza Further physics cases
Mooere specifi c ALP orrWIWISS(P (weakl y inteeacractin gslim partic l e) model s could be searched for at thelow energy frontier of particlephysics: physics: – Paraphotons / hidden photons – Chamaleons ––NonNon--standardstandardscenarios of axion production
If equipped with microwave cavitiescavities,, dark matter halo axionscould be searched forfor.. under study [[BakerBaker et al. PRD 85]
IAXO as a true ““axionaxionfacility” facility” open to the community: community: Groupssinvitedinvitedto contribute and enrichthe science ppgrogramme of IAXO.
INT Washington, April 2012 Igor G. Irastorza / Universidad de 40 Zaragoza IAXO: project status & timetable
ProtoProto--collaborationcollaboration being formed. formed. – Most CAST groups ––NewNew groups + extended expertises ((magnetmagnet,, optics).optics). ––OOpen for new interested ggproups Conceptual DesignReport in preparation Letter of Intent to be submitted to CERN soon
CAST
IAXO
INT Washington, April 2012 Igor G. Irastorza / Universidad de 41 Zaragoza European Astroparticle IAXO in ASPERA Roadmap
Latest draft of the ASPERA roadmap 2011
INT Washington, April 2012 Igor G. Irastorza / Universidad de 42 Zaragoza Conclusions CAST is the most powerful axion helioscope toto--date.date. – Established as a reference result in axion physics. ––FirstFirstCAST PRL most cited axion experimental result ever. ever. ––ExpertiseExpertise gathered in magnet,magnet, optics,optics, low back detectors
IAXO: International Axion Observatory. Observatory. ––AA new generationaxion helioscope – First results (JCAP 016) sh ow good prospects to improve CAST 11--1.51.5 orders of magnitude in ga. ––FirstFirstsolid steps towards conceptual design
In combination with dark matter axion searches (ADMX) a bigpart of the QCD axion model region could be explored next decadedecade.. Potential for other physics cases: white dwarfts e-coupled axions?, relic axionsaxions?,?, ALPs?…ALPs?… IAXO as a ““axionaxion/ALP/ALP research facility”. facility”. New groups to enlarge and enrich IAXO.
INT Washington, April 2012 Igor G. Irastorza / Universidad de 43 Zaragoza