1. Cherenkov Telescope Array
J. Carr
March 2014
Cherenkov Telescope Array, J. Carr

2. CTA Project A huge improvement in all aspects of performance
A factor ~10 in sensitivity, much wider energy coverage, much better resolution, field-of-view, full sky, …
A user facility / proposal-driven observatory
With two sites with a total of >100 telescopes
A 27 nation ~€200M project
Including everyone from HESS, MAGIC and VERITAS
Global project, >1000 scientists,
27 nations including of course Brazil
It will be an order of magnitude more sensitive than current instruments and also …
Requires the construction of over 100 Cherenkov telescopes
Timescale…
Prototypes:
First Science: ~2017
Completion: ~2020

3. E × F(>E) (TeV/cm2s) Sensitivity: Fermi HESS CTA Energy (TeV) SST10
-11
Fermi
1 year
HESS 10
-12
E × F(>E) (TeV/cm2s)
Sensitivity:
50 hours 10
-13
CTA 10
--14
0.01
0.1 1
Energy (TeV) 10
100
SST
Low energies
4 orders …
To achieve this level of sensitivity over a wide range of energies CTA requires three sizes of telescope
MST
LST

4. CTA MST Prototype in Berlin

5. Sites: Candidates A many sites Decisions 2014 Site development 2017
Tenerife
SPM - Mexico
Arizona (2)
Aar/HESS Namibia
Argentina (2)
Chile - Armazones
A many sites
Extensive studies taken place
Decisions 2014
Selection will take into account weather, construction / operations costs, performance (from simulations), risks, …
Site development 2017
First telescopes operating on site in 2017

6. CTA Science Cosmic Particle Acceleration, Propagation and Impact
Mechanisms for particle acceleration, galactic CR acceleration and Pevatrons, acceleration in jets and lobes of AGN, cosmic ray transport, …
What role do accelerated particles play in feedback on star formation and galaxy evolution?
Probing Extreme Environments
Neutron stars and black holes, relativistic jets, winds and explosions, the contents of cosmic voids, …
Physics Frontiers 
What is the nature of Dark Matter? How is it distributed?
Is the speed of light a constant for high-energy photons?
Do axion-like particles exist?
CTA has three science themes, the first of which is the main business of this conference – the study of relativistic cosmic particles: their acceleration sites…

7. Indirect Searches for Dark Matter
March 2014
Cherenkov Telescope Array, J. Carr

8. Targets for IDM Searches
March 2014
Cherenkov Telescope Array, J. Carr

9. Cherenkov Telescope Array, J. Carr
Comparison of targets
March 2014
Cherenkov Telescope Array, J. Carr

10. Internal Bremsstralung
March 2014
Cherenkov Telescope Array, J. Carr

11. Cherenkov Telescope Array, J. Carr
Reach of IDM searches
March 2014
Cherenkov Telescope Array, J. Carr

12. CTA Reach HESS Galactic objects Field of view + sens. CTA 5° 8°
Current Galactic
VHE sources (with
distance estimates)
HESS
Galactic objects
Newly born pulsars and the supernova remnants
have typical brightness such that HESS etc can see only relatively local (typically at a few kpc) objects
CTA will see whole Galaxy
Field of view + sens.
Survey speed ~300×HESS
CTA 5° 8°

13. Astroparticle Physics, J. Carr
Tycho SNR: “Pevatron”
Morlino and Caprioli Astro-ph/
March 2014
Astroparticle Physics, J. Carr

14. Astroparticle Physics, J. Carr
Hadronic SNRs
Manelartz and Tjus astro-ph/
Northern Sky
Southern Sky
March 2014
Astroparticle Physics, J. Carr

15. Cherenkov Telescope Array, J. Carr
Effective Area
CTA
10 TeV Energy
CTA: m2
ICECUBE: 10 m2
CTA sensitive to hadronic sources with fluxes 10-5 lower than ICECUBE (KM3NeT)
March 2014
Cherenkov Telescope Array, J. Carr

16. CTA Resolution CTA 10 Arcminutes Requirement Goal 1
point-source sensitivity is not the whole story and crtiically CTA will achieve by far the best angular resolution of any instrument above the X-ray band
below one arcminute at the highest energies, with resolved images of most objects and hence a deeper understanding of the astrophysics of these objects.
resolved systems -> more science
CTA
Goal 1

17. The Galactic Centre
CTA resolution+sensitivity can disentangle emission
HESS PSF
SNR G
Sgr A*
Sgr B2
CTA PSF
And to return to the galactic centre – it is clear that our curtent understanding is limited be resolution – in particular the ability to separate diffuse emission and point-like sources...
NRAO: 20cm, 1.1mm, 5 μm
HESS

18. Cherenkov Telescope Array, J. Carr
CTA Schedule
Design Study
Design development
CTA appears on key roadmaps
Preparatory Phase
EU FP7 funded activity
Preliminary Design Review 2013
Site Selection 2014
Critical Design Review 2015
Construction Phase
Site development and first telescopes on site 2017
First science 2017
Completion ~2020
March 2014
Cherenkov Telescope Array, J. Carr

19. Cherenkov Telescope Array, J. Carr
HESS
Science on HESS immediately to prepare for science on CTA
4 12m telescopes + 1  28m telescope operational
March 2014
Cherenkov Telescope Array, J. Carr