CTA SKA Synergies. Stefan Wagner Landessternwarte (CTA Project Office) Heidelberg

Transcription

1 CTA SKA Synergies Stefan Wagner Landessternwarte (CTA Project Office) Heidelberg

2 CTA SKA Synergies Stefan Wagner Landessternwarte (CTA Project Office) Heidelberg

3 CTA SKA Synergies CTA Science: How and Why The Non-thermal Universe Interstellar Matter Cosmology & Fundamental Physics CTA Observatory Partners Timescales Operation and Access CTA & SKA Strategic synergies Scientific cooperation (individuals) Cooperation (Projects/Observatories)

4 CTA Science: How Some non-thermally dominated sources radiate throughout EM spectrum with (nearly) identical E-losses. 20 OoM in frequency 40 OoM in photon density need a very large collection area (i.e. a square-km-array) Atmosphere acts as detector volume.

5 Stereoscopic Cherenkov Imaging

6 Meteor track very dim few light quanta per m2 short flash of a few nano-seconds

7 HESS II Camera 2048 pixels On-board electronics 2.5 m

8 few large telescopes for lowest energies ~km2 array of medium-sized telescopes large 7 km2 array of small telescopes, 4 LSTs ~70 SSTs ~25 MSTs plus ~28 SCTs extension

9 SENSITIVITY (IN UNITS OF CRAB FLUX) FOR DETECTION IN EACH 0.2-DECADE ENERGY BAND background and systematics limited rate (=area) limited background limited LST SST MST

10 TELESCOPE SPECS SST small MST medium LST large SCT medium 2-M Number 70 (S) 25 (S) 15 (N) 4 (S) 4 (N) 36 (S) Spec d range > few TeV 200 GeV to 10 TeV 20 GeV to 1 TeV 200 GeV to 10 TeV Eff. mirror area > 5 m2 > 88 m2 > 330 m2 > 40 m2 Field of view > 8o > 7o > 4.4o > 7o Pixel size ~PSF q 80 < 0.25o < 0.18o < 0.11o < 0.075o Positioni ng time 90 s, 60 s goal 90 s, 60 s goal 50 s, 20 s goal 90 s, 60 s goal Availability > 3 h/week 6 h/week 9 h/week 6 h/week Target 420 k 1.6 M 7.4 M 2.0 M

11 CTA Science: Why Bild General science case examples

12 THE TEV SKY

13 THE TEV SKY Gamma rays probe cosmic accelerators (& their environment) Gamma ray yield = beam x target

14 THE TEV SKY

15 Exact shape of spectral cutoff what limits the acceleration mechanism? In the spectral shape universal across the remnant? Short (year) time scale phenomena like in X-rays? Emission from compact molec. clouds inside remnant, penetrated by CR Which particles are accelerated? Exactly how are they accelerated? On what time scales? When and how are they released? Spectral variation across shock precursor driven by VHE particles? Do SNR quantitatively explain the bulk of galactic CR? Illumination of molec. clouds outside remnant

16 Nebula: Electrons (somehow) diffusing away Origin of asymmetry? Pulsar Evolution: Building up nebula? Pulsar Origin of VHE pulsed emission? VHE Variability? Are nuclei accelerated? Color encodes gamma-ray energy Escape from nebula? Compact object in Binary Electrons confined by radiative losses

17 CTA Science: Why? The Non-thermal Universe BH ergospheres Jet acceleration, beaming paradigm Inflation of lobes/clusters with nonthermal particles Feedback, shocks, plasma turbulence... Interstellar Matter Interaction of CR fluid with ISM Probing dense molecular cores... Cosmology & Fundamental Physics DM Radiation fields, Magnetic fields,...

18 Persistent GRBs Flares by factors > 100 on time-scales of minutes (PKS , HESS; Mrk 501, MAGIC; Mrk 421, VERITAS) Variability time-scales and BH mass: 300 nano-sec per solar mass Causality-inferred diameter ~ 100 million km, ie < 1 AU <<< 1 pc

19 ThemeCTA 1: Cosmic Particle Acceleration Science: Why What are the sites of particle acceleration in our own galaxy, filling the Milky Way with particles of beyond PeV energies? Where exactly are the sites of particles acceleration in the jets and lobes of AGN? What are the mechanisms, for cosmic particle acceleration up to very high energies in many astrophysical systems? and of particle transport? What role do accelerated particles play in feedback on star formation and galaxy evolution? Theme 2: Probing Extreme Environments What physical process are at work close to neutron stars and black holes? What happens in the relativistic jets, winds and explosions? What are the contents radiation fields, magnetic fields, particles of cosmic voids, and how did these evolve over the history of the Universe? What role do relativistic particles play in the energetics of starburst regions, normal galaxies, active galaxy jets and lobes, and in clusters of galaxies? Theme 3: 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?

20 CTA Observatory Partners CTA Consortium (Institutes) CTAO GmbH (15 countries?) Funding countries (construction and operations (10 yrs)) Timescales 2012: DoI (13 countries) AR+AU+BR+CH+ES+FR+GE+IT+JP+NAM+PL+UK+ZA 2013: major reviews, TDR 2014: CTAO GmbH, site decision 2015: funding agreement, begin construction 2017: begin science operations

21 CTA CONSORTIUM

22 TIME LINE Site decision Start deployment Formal approval Design Phase Preparatory Phase / Pre-Construction Phase Negotiations with host countries, IKC agreements, site development, telescope deployment Completion of deployment, operation

23 CTA Observatory Operation and Access No final decisions (subject to funding agreement, expected 2015) CTAO operating HQ (Europe) + Southern array + Northern Array ~10 countries expected to join from the beginning, others join late Subsequent construction and start of operation whenever accepted and verified performance exceeds existing arrays. Observatory open to scientific communities of countries supporting CTA (dependend on funding agreements). CTAC (or IKC parties) will be awarded guaranteed time. CTAC expected to conduct surveys formal cooperations?

24 CTA and SKA Strategic synergies Similarities in project organisation (major astrophysics research infrastructure, EU-headed, 5 continents, technical and management challenges, access, archives,...) Scientific cooperation (individuals) Anyone interested should talk to us (or join CTAC). Ultimately CTA shall be operated as an observatory (demand access!)

25 CTAO CTAOCouncil Council Finance Finance Committee Committee Technical Technical Committee Committee Science Science/ /Pr. Pr. Committee Committee Directorate Admin. Admin.Director Director Director DirectorGeneral General Scientific ScientificDirector Director Technical TechnicalDirector Director One scenario for observatory organization Safety DG unit: Outreach,

26 CTA and SKA Cooperation (Projects/Observatories) CTA will be a survey instrument At 100 GeV 1 TeV 300 times faster than H.E.S.S. Guaranteed time to be used (largely) for (a) survey(s) Community cooperation strongly encouraged CTA will be a flexible pointed instrument 100 telescopes, 4 orders of magnitude in energy Quality rather than quantity (by comparison to SKA, GAIA, LSST) cooperative projects in open time.