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

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

3 phenomenology related to the evolutionary status of the cluster MACSJ Ma et al. 2008, Radio sources in Clusters of galaxies

4 Lewis et al 2003 A2029

5 merging relaxed: cool core

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

8 A2345 Bonafede et al. 2009

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

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

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

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  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 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 2. Status of the Sardinia Radio Telescope

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

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

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 MHz GHz Primary focus GHz Mono-feed BWG focus GHz Multi-feed 7 pixels Gregorian focus BACK-ENDS First light: 4 BANDs

22 13 September 2009 First light of SRT:

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

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 Medicina Noto Cagliari Italian context 64 m 32 m Matera

GHz Multifeed Surveys H 2 O Megamasers Extragalactic CO

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:  Jy (rms) ]   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 CO(1-0) Cold component of molecular gas in high-z galaxies EXTRA-GALACTIC CO Weiss et al GBT/Effelsberg: 20hr on source Large BW (1-2 GHz), Tsys  K Future: 90–115 GHz GHz GHz GHz Redshift Machines: eg 14 GHz 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 3.5<z<5.5

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

30 Thank you