An AstroParticle perspective for SKA and CTA

Transcription

1 NRF/NWO Meeting Oct. 18 th, 2012 An AstroParticle perspective for SKA and CTA Sergio Colafrancesco Wits University - DST/NRF SKA Research Chair Sergio.Colafrancesco@wits.ac.za CAP Center for Astroparticle Physics 1

2 Going larger Going deeper The large-scale astronomical experiments of the next decade will allow to address questions of fundamental physics SKA Dark Ages, B, Life, Unknown SKA COrE JWST E-ELT IXO CTA νk 3 Net Ton CR Lisa Inflation probe, Vacuum energy Dark Ages, Life, Galaxy origin Fine Structure const, p/e ratio Horizon physics Dark Matter, Extreme events Neutrino physics Cosmic Ray origin Gravitational waves AstroParticle Physics probes CTA 2

3 AstroParticle with SKA & CTA AstroParticle Physics probes of fundamental physics and cosmology in cosmic structures Dark Matter Cosmic Rays in LSS B-fields 1ES Coma SMBH feedback MS0735 Jet origin AGN B-field CIZAJ Extreme events UHE-p,ν 3

4 Dark Matter signals It is becoming more and more evident that Radio and Gamma-ray emission are the dominant probes for Dark Matter nature π0 γγ π± χ χ e± χ χ B Continuous γ-ray emission Continuous radio emission 4

5 Dark Matter with SKA & CTA Dwarf galaxies The darkest DM halos Galaxy clusters The largest DM halos γ-rays 0.1µG radio radio γ-rays 1µG 5

6 Dark Matter radio hr ATCA [S.C. et al. 2011] Segue-3 Carina Fermi 2yr Bootes Fornax ATCA 121hr MeerKAT SKA-P1 B= 1µG Improve current DM limits (γ-rays) by a factor: ~100 ATCA (20 µjy) ~1000 MeerKAT ( 1 µjy) ~10000 SKA-P1 ( 0.1µJy) 6

7 DM probes DM detectors + Astrophysics LHC + Astrophysics Direct Detection SKA SKA CTA Fermi Indirect Detection 7

8 ! Galaxy clusters! Radio Halos detected! γ-ray upper limits only Cosmic Rays in LSS! Galaxy outflows! (Hyper-) Winds! Mini-jets vs outflows! NGC253 >50% of E-budget is in (CRs + B)! Revise Galaxy Evolution!? 8

9 Radio Halos & Cosmic Rays STRATEGY for SKA Derive both n e and B from single SKA observations Combine: radio + ICS GHz + 30 GHz Synchrotron J ν ~ n e B (s+1)/2 ν (s-1)/2 ICS-SZE I ν ~ n e U CMB ν (s-1)/2 VLA E-VLA MerKAT SKA-P1 SKA-P2 9

10 BH AstroParticle: cores-jets-lobes! Radiogalaxies!! WMAP (23 GHz) Fermi-LAT Extreme CR events Lobes vs jet acceleration! LSS Feedback 1270 MOSKALENKO ET AL. Vo Jet base reconstructed down to 70 µ arcsec! BH scales!! Horizon physics Jet origin Figure 4. Radio map (at 408 MHz from Haslam et al. 1982) of the field centered on the nearby radio galaxy Cen A. The total extent of the north-south radio lobes is 9 and is centered on the AGN (the bright white region near the center of the field). The r = 3. 2 circles mark the positions of the UHECR events detected in the field by Auger (Abraham et al. 2008a). The numbers correspond to the event number as provided in Abraham et al. (2008a), and also in our Table 1. Note event #3 corresponds most closely to Cen B, a bright spot near the center of the circle, shown with higher resolution in Figure 5. (A color version of this figure is available in the online journal.) Figure 6. Radio image of the 200$$ 200$$ field around the radio PKS This VLA 4.9 GHz image at 2$$ resolution was mad a multiconfiguration data set consisting of a 1 hr observation in 1983 De (program AT45) and 10 minutes observation from Jun 1997 (AK444). T data set was obtained through the NRAO VLA Archive Survey (NVA location of the closest cosmic ray detected by Auger (#9) is indicated arrow pointing away from the radio nucleus. (This NVAS image was p as part of the NRAO VLA Archive Survey, (c) AUI/NRAO.) (A color version of this figure is available in the online journal.) 10

11 Ultra High-E particles from cosmic sites AGN E<19 19 ev p γ ν Cosmic String E>10 20 ev WISP ν 11

12 Ultra High-E particles from extreme sites U-H-E CRs from Radio Galaxies induce Cherenkov radiation detectable up to ν max ~ ν 0 E -1 W 1/2 E-H-E Neutrinos from Cosmic Strings induce Cherenkov radiation with peak flux density at radio freq. (~2.5 GHz) 12

13 Astro-Particle perspective! Astroparticle needs multi-disciplinary! Area of collaboration between SA and NL (theory)! Multi-disciplinary needs multi-ν! Area of collaboration between SA and NL (data analysis)! The South-Africa multi-ν platform! Present: KAT-7 HESS-II SALT! Mid-term: MeerKAT HESS-II SALT! Long-term: SKA-CTA - 13

14 HESS HESS-II The assembly of the steel structure for the 600 m2 H.E.S.S. II telescope was completed in Mirrors and camera installed in First Light in August Kookaburra in radio and TeV SNR RXJ GHz VLA radio image 14

15 Cherenkov Telescope Array HESS-II low-e Mini-Array high-e +Axion effects + QG probes Argentina Namibia 15

16 The CTA mini-array Reasons for a Mini-Array An Early Science Cycle of CTA can be carried out within a reasonable time frame, with improved capabilities compared to the current Cherenkov telescopes (at E > 10 TeV) HESS-II Simultaneous observations with other high energy observatories already approved for continuation up to 2016 (Swift, Fermi, ) Synergy: KAT-7, MeerKAT (SKA mini-arrays) SALT The implementation of a Mini-Array will boost the implementation of the entire CTA project. CTA Mini Array SA involved in the CTA mini-array -Colafrancesco (WITS) + -ASTRI Consortium requires SA scientific support -ASTRI Consortium sent a Letter to Namibia DST for local support 16

17 SKA-CTA connection AGN jet Radio - γ-rays origin model constraint Galaxy LSS CR electrons calorimeter SNR physics Radio - γ-rays Dark Matter Origin of electrons - Hadronic - Leptonic CTA site: Aar 0.1µG 1µG 17

18 CTA South Site (Namibia) Aar Kubub 18

19 Opportunities The largest platform for multi-ν Astronomy 250 km 19

20 THANKS for your attention! 20