1. 1 Clusters of galaxies and future studies with SRT Luigina Feretti INAF Istituto di Radioastronomia

2. 2 1.Radio sources in Clusters of galaxies 2.Status of the Sardinia Radio Telescope 3.Science with the SRT

3. 3 phenomenology related to the evolutionary status of the cluster MACSJ0717+3745 Ma et al. 2008,2009 1.Radio sources in Clusters of galaxies

4. 4 Lewis et al 2003 A2029

5. 5 merging relaxed: cool core

6. 6 Diffuse Radio Sources in clusters : 1 - radio halos 2 – radio relics 3 – mini-halos at the center of cooling core clusters 4 – radio galaxies related to cD galaxies in cool core clusters, radio bubbles, ghost bubbles 5 - central relics  all steep spectrum sources MERGERRELAXEDMERGERRELAXED

7. 7 most distant & most powerful radio halo z= 0.55, P 1.4 GHz ~1.6 10 26 W/Hz (Bonafede et al 2009)

8. 8 A2345 Bonafede et al. 2009

9. 9 Diffuse Radio Sources in clusters : 1 - radio halos 2 – radio relics 3 – mini-halos at the center of cooling core clusters 4 – radio galaxies related to cD galaxies in cool core clusters, radio bubbles, ghost bubbles 5 - central relics  all steep spectrum sources MERGERRELAXEDMERGERRELAXED

10. 10 (X-ray : Forman et al. 2007) See : Mathews and Brighenti 2008 M 87 (Radio: Owen at el. 2000)

11. 11 Perseus – Fabian et al 2000 Chandra (Böhringer et al ROSAT) Minihalo = 350 kpc (Sijbring & De Bruyn 1993) X-ray Radio + X-ray Radio

12. 12 Hydra A – X-ray Chandra Mc Namara et al. 2000 Radio : Taylor et al. (VLA) Most radio sources in cavities are FRI

13. 13 Gitti Feretti Schindler 2006 RBS 797 Color: X-ray Contours:Radio

14. 14 The interaction between the AGN jets and the ICM is believed to be the primary feedback mechanism between the BH and its environment  one strong or several small episodes of energy release  radio bubbles  confinement

15. 15  interaction between CR and ICM: THE CRs AFFECT THE ICM - Cavities are filled with cosmic rays which inflate the cavities and form a much larger lobe - Bubbles can rise to the cluster outskirts - Eventually the cosmic rays diffuse away from the cavities, impact with/ leak into the surrounding medium

16. 16 Link between radio and X-ray emission  Understand the energetics and the dynamical evolution of plasma bubbles inflated by radio jets in the hot cluster atmosphere radio spectra correlations CR/gas interaction confinement energy budget lifetimes/duty cycles FUTURE PROSPECTS

17. 17 2. Status of the Sardinia Radio Telescope

18. 18 The Radiotelescope -Diameter: 64 m -Frequency range : 300 MHz – 100 GHz -Actively controlled surface : 1008 panels 1116 mechanical actuators - Multiple focal positions P, G, BWG - Frequency agility - State-of-art receivers (multi-beam) - Digital back-ends - Fiber optic connection -Transmitting capability

19. 19 Quality of the site: Low rain Low atm opacity Low RFI Low wind S. Basilio

20. 20 Observing time (in %) with an expected atmospheric opacity τ<0.1 23.8 GHz 31.4 GHz 100 GHz (Ambrosini et al.)

21. 21 Digital Spectrometer Pulsars 1 GHz BW, 1024 channels Spectrometer 60 MHz BW Dual Band Total Power Analogic Back-end 7x2 outputs, 2 GHz BW RECEIVERS 310-420 MHz 1.3-1.8 GHz Primary focus 5.7-7.7 GHz Mono-feed BWG focus 18-26 GHz Multi-feed 7 pixels Gregorian focus BACK-ENDS First light: 4 BANDs

22. 22 13 September 2009 First light of SRT: 2010 http://www.srt.inat.it/webcam

23. 23 3. Science with the SRT In collaboration with Isabella Prandoni SRT Project Scientist

24. 24 Radio Astronomy Science ● VLBI – eVLBI : x2 sensitivity ≤ 22 GHz x5 > 22 GHz mm-VLBI  43 GHz (7 mm) [VSOP2]  86 GHz (3 mm) [GMVA /ALMA] ● Italian VLBI ● Single dish Space Science (20%) ● Data down link ● Space science : Radio science, Deep Space Network 1.4 GHz 5 GHz

25. 25 Medicina Noto Cagliari Italian context 64 m 32 m Matera

26. 26 18-22 GHz Multifeed Surveys H 2 O Megamasers Extragalactic CO

27. 27 18-26 GHz Multi-feed - Pulsars: - Search for Recycled/msec pulsars in the Galactic Center  binary systems msec pulsar/BH  gravitazional tests - Continuum Surveys : - Map of free-free emission on the Galactic Plane  Ultra-Compact HII Regions - Deep Fields [ SRT confusion limit: 50-70  Jy (rms) ]  information @  10 GHz  high z AGN/low luminosity - Line Surveys : - Search for H 2 O masers in the Local Group  Distance and 3D motions  Dark matter Cosmology - Unbiased Mapping NH 3 in the Galactic Plane  Star forming regions, T of Molecular clouds, Prestellar cores, Gas and dust properties Surveys 2 deg 0.5 deg Centro Galattico Courtesy A. Possenti Courtesy J. Brand Lagoon Nebula Z = 6

28. 28 CO(1-0) Cold component of molecular gas in high-z galaxies EXTRA-GALACTIC CO Weiss et al. 2005 GBT/Effelsberg: 20hr on source Large BW (1-2 GHz), Tsys  20-25 K Future: 90–115 GHz 70-90 GHz 35-50 GHz 26-36 GHz Redshift Machines: eg 14 GHz BW @ 26-40 GHz  redshifted CO 1<z<7 J  J-1 J  4 CO(4-3) CO(3-2) CO(2-1) CO(1-0) CO(1-0)  K band @ 3.5<z<5.5

29. 29 Observational Policy Open sky Fraction reserved to KSP (possibly larger in early SRT operations)

30. 30 Thank you