Presentation is loading. Please wait.

Presentation is loading. Please wait.

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

Similar presentations


Presentation on theme: "1 Clusters of galaxies and future studies with SRT Luigina Feretti INAF Istituto di Radioastronomia."— Presentation transcript:

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 MACSJ Ma et al. 2008, 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 ~ 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 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< 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 MHz GHz Primary focus GHz Mono-feed BWG focus GHz Multi-feed 7 pixels Gregorian focus BACK-ENDS First light: 4 BANDs

22 22 13 September 2009 First light of SRT: 2010

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 GHz Multifeed Surveys H 2 O Megamasers Extragalactic CO

27 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 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

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

30 30 Thank you


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

Similar presentations


Ads by Google