S e a r c h f o r U l t r a H i g h E n e r g - PowerPoint PPT Presentation

S e a r c h f o r U l t r a H i g h E n e r g y p h o t o n s a t t h e P i e r r e A u g e r O b s e r v a t o r y & c o n t r i b u t i o n t o A u g e r P r i me In the Auger group. Thesis Supervisor : Corinne Berat

O u t l i n e ● U l t r a H i g h E n e r g y C o s m i c R a y s & E x t e n s i v e A i r S h o w e r s ● T h e P i e r r e A u g e r O b s e r v a t o r y & A u g e r P r i m e ● S c i n t i l l a t o r S u r f a c e D e t e c t o r s – C o n s t r u c t i o n & V a l i d a t i o n ● S e a r c h f o r U l t r a - H i g h E n e r g y p h o t o n p r i m a r i e s – M o t i v a t i o n s & M u l t i - V a r i a t e A n a l y s i s 2 T h e s i s M o n i t o r i n g P r e s e n t a t i o n J u l i e n S o u c h a r d

U l t r a - H i g h E n e r g y C o s m i c R a y s U l t r a - H i g h E n e r g y C o s m i c R a y s & & E x t e n s i v e A i r S h o w e r s E x t e n s i v e A i r S h o w e r s

U l t r a H i g h E n e r g y C o s m i c R a y s - S p e c t r u m UHECRs & EAS U l t r a H i g h E n e r g y C o s m i c R a y s ( U H E C R s ) : 1 8 - u l t r a h i g h e n e r g i e s : E > 1 0 e V - 2 - 1 - v e r y l i m i t e d fm u x : < 1 . k m . y e a r - f e a t u r e s i n t h e s p e c t r u m - n u c l e u s f r o m H t o F e & n e u t r a l s ( n / γ / ν ) 4 T h e s i s M o n i t o r i n g P r e s e n t a t i o n J u l i e n S o u c h a r d

A c c e l e r a t i o n & P r o p a g a t i o n UHECRs & EAS CRs ν ɣ 5 T h e s i s M o n i t o r i n g P r e s e n t a t i o n J u l i e n S o u c h a r d

M u l t i - M e s s e n g e r A s t r o p h y s i c s UHECRs & EAS Multi-Messenger era of astrophysics : CRs - combine cosmic rays, gamma, neutrino and gravitational wave observations ν ɣ - interplay between all these messengers Complementarity between the observations ● Gamma-rays : The 3 fluxes are linked! The 3 fluxes are linked! +: straight line - : UHE horizon < 10 Mpc ● Neutrinos : +: straight line, no interaction - : isotropic diffuse background ● Cosmic-Rays : +: direct accelerator probe - : deflected in magn. field 6 T h e s i s M o n i t o r i n g P r e s e n t a t i o n J u l i e n S o u c h a r d

UHECRs & EAS E x t e n s i v e A i r S h o w e r UHECRs interact with Earth’s atmosphere : generates an E xtensive A ir S hower ( EAS ) 3 main components : - muonic component (~4%) - hadronic component (~1%) - electromagnetic component (95%) At ground : ~5.10 10 particles (estimation for a 10 19 eV p-shower) 7 T h e s i s M o n i t o r i n g P r e s e n t a t i o n J u l i e n S o u c h a r d

UHECRs & EAS E x t e n s i v e A i r S h o w e r UHECRs interact with Earth’s atmosphere : generates an E xtensive A ir S hower ( EAS ) 3 main components : - muonic component - hadronic component - electromagnetic component Advantages of the EAS : - large footprint (up to 15 km) - multiple observations possibles - UHE hadronic physics laboratory... Disadvantages of the EAS : - indirect information on primary’s energy - inhomogeneous calorimeter - ...model dependent 8 T h e s i s M o n i t o r i n g P r e s e n t a t i o n J u l i e n S o u c h a r d

T h e P i e r r e A u g e r O b s e r v a t o r y T h e P i e r r e A u g e r O b s e r v a t o r y & & A u g e r P r i m e A u g e r P r i m e

T h e P i e r r e A u g e r O b s e r v a t o r y PAO & AugerPrime The Pierre Auger Observatory (PAO) : ● Officially completed in 2008 ● started taking data in 2004 ● 400 scientists from 18 countries ● Location : pampa near Malargüe, Argentina ● Altitude (mean) : 1400 m above sea-level ● Surface (SD) : 3000 km 2 F luorescence D etector ( FD ) : 24 telescopes ● located in 4 buildings. S urface D etector ( SD ) : Overlooking the ● ● 1660 Water atmosphere above Cherenkov Detector the array ● Triangular spacing Duty-Cycle : 14% ● of 1.5 km ● Duty-Cycle : 100% 10 T h e s i s M o n i t o r i n g P r e s e n t a t i o n J u l i e n S o u c h a r d

T h e P i e r r e A u g e r O b s e r v a t o r y PAO & AugerPrime The Pierre Auger Observatory (PAO) : ● Officially completed in 2008 ● started taking data in 2004 ● 400 scientists from 18 countries ● Location : pampa near Malargüe, Argentina ● Altitude (mean) : 1400 m above sea-level ● Surface (SD) : 3000 km 2 F luorescence D etector ( FD ) : W ater C herenkov D etector ( WCD ) : 24 telescopes ● Secondary particles (highly relativistic) going through the located in 4 buildings. detector produce Cherenkov light. S urface D etector ( SD ) : Overlooking the ● ● 1660 Water Collect timing and atmosphere above Cherenkov Detector the array signal to reconstruct ● Triangular spacing the showers. Duty-Cycle : 14% ● of 1.5 km ● Duty-Cycle : 100% Sensitive to e ± , γ , μ 11 T h e s i s M o n i t o r i n g P r e s e n t a t i o n J u l i e n S o u c h a r d

T h e P i e r r e A u g e r O b s e r v a t o r y PAO & AugerPrime The Pierre Auger Observatory (PAO) : ● Officially completed in 2008 ● started taking data in 2004 ● 400 scientists from 18 countries ● Location : pampa near Malargüe, Argentina ● Altitude (mean) : 1400 m above sea-level ● Surface (SD) : 3000 km 2 F luorescence T elescope : F luorescence D etector ( FD ) : An EAS excite the nitrogen molecules in the 24 telescopes ● atmosphere → Fluorescence Emission located in 4 buildings. S urface D etector ( SD ) : Telescopes collect Overlooking the ● ● 1660 Water this UV light atmosphere above Cherenkov Detector the array Direct measurement ● Triangular spacing Duty-Cycle : 14% ● of the shower of 1.5 km energy ● Duty-Cycle : 100% 12 T h e s i s M o n i t o r i n g P r e s e n t a t i o n J u l i e n S o u c h a r d

T h e P i e r r e A u g e r O b s e r v a t o r y PAO & AugerPrime The Pierre Auger Observatory (PAO) : ● Officially completed in 2008 ● started taking data in 2004 ● 400 scientists from 18 countries ● Location : pampa near Malargüe, Argentina ● Altitude (mean) : 1400 m above sea-level ● Surface (SD) : 3000 km 2 F luorescence D etector ( FD ) : 24 telescopes ● located in 4 buildings. S urface D etector ( SD ) : Overlooking the ● ● 1660 Water atmosphere above Cherenkov Detector the array ● Triangular spacing Duty-Cycle : 14% ● of 1.5 km ● Duty-Cycle : 100% 13 T h e s i s M o n i t o r i n g P r e s e n t a t i o n J u l i e n S o u c h a r d

H y b r i d D e t e c t i o n & O p e n q u e s t i o n s PAO & AugerPrime Hybrid Detection : Able to use the FD to calibrate the SD’s energy reconstruction Other complementary detection possible… Flux suppression around 10 20 eV : What is causing it ? What particles are making up the UHECRs flux ? 14 T h e s i s M o n i t o r i n g P r e s e n t a t i o n J u l i e n S o u c h a r d

A u g e r P r i m e U p g r a d e PAO & AugerPrime Science Motivation : ● Probe the flux suppression ● Look at the flux composition at the highest energies ● UHE hadronic physics AugerPrime : ● Add Scintillator Surface Detectors : on top of the WCD, to disentangle muon/EM components ● Upgraded electronics ● Radio Upgrade : add antennas on top of WCD to detect the showers radio-emissions 15 T h e s i s M o n i t o r i n g P r e s e n t a t i o n J u l i e n S o u c h a r d

S c i n t i l l a t o r S u r f a c e D e t e c t o r s S c i n t i l l a t o r S u r f a c e D e t e c t o r s - - C o n s t r u c t i o n & V a l i d a t i o n C o n s t r u c t i o n & V a l i d a t i o n