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Clusters of galaxies and future studies with SRT

Clusters of galaxies and future studies with SRT. Luigina Feretti INAF Istituto di Radioastronomia. Radio sources in Clusters of galaxies Status of the Sardinia Radio Telescope Science with the SRT. Radio sources in Clusters of galaxies. phenomenology related to the evolutionary

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Clusters of galaxies and future studies with SRT

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

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

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

  4. A2029 Lewis et al 2003

  5. relaxed: cool core merging

  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 M E R G E R R E L A X E D

  7. The cluster Macs J0717+3745 (Bonafede et al 2009) most distant & most powerful radio halo z= 0.55, P1.4 GHz~1.6 1026 W/Hz

  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 M E R G E R R E L A X E D

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

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

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

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

  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. FUTURE PROSPECTS 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

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

  20. Observing time (in %) with an expected atmospheric opacity τ<0.1 23.8 GHz31.4 GHz100 GHz(Ambrosini et al.)

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

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

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

  26. 18-22 GHz Multifeed • Surveys • H2O Megamasers • Extragalactic CO

  27. 0.5 deg 2 deg Lagoon Nebula Courtesy J. Brand 18-26 GHz Multi-feed Surveys - 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 mJy (rms)]  information @  10 GHz high z AGN/low luminosity - Line Surveys : - Search for H2O masers in the Local Group  Distance and 3D motions  Dark matter Cosmology - Unbiased Mapping NH3 in the Galactic Plane  Star forming regions, T of Molecular clouds, Prestellar cores, Gas and dust properties Centro Galattico Courtesy A. Possenti Z = 6

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

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

  30. Thank you

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