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Thermal and non-thermal emission from galaxy clusters: X-ray and LOFAR observations

Discover the thermal and non-thermal emission from galaxy clusters through X-ray and LOFAR observations at the workshop held at Observatoire de la Côte d’Azur, Nice, France. Learn about diffuse radio emission, radio/X-ray comparisons, radio halos & relics study, and more to delve into this fascinating research field. Uncover the importance of non-thermal emission analysis with LOFAR and explore open questions in the study. Credits to C. Pfrommer and other primary models for accelerating phenomena in galaxy clusters. Compare radio and thermal X-ray profiles to study the non-thermal cluster component in depth along with magnetic field measurements and cold front analysis. Dive into the nature of relativistic electrons and their origin through insightful discussions and collaborations at the workshop.

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Thermal and non-thermal emission from galaxy clusters: X-ray and LOFAR observations

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  1. Chiara Ferrari Observatoire de la Côte d’Azur, Nice, FRANCE Thermal and non-thermal emission from galaxy clusters: X-ray and LOFAR observations LOFAR Wokshop

  2. LOFAR Wokshop Outline of the talk • Diffuse radio emission in clusters • Radio/X-ray comparison • Importance for the study of radio halos & relics • Open questions • Study of non-thermal emission with LOFAR • Conclusions

  3. LOFAR Wokshop Diffuse radio emission in clusters • S(ν)ν-α • α 1 • Relativistic electrons: γ>>1000 • Magnetic fields: ~ 0.1 – 1 μGauss A2163: VLA observations Feretti et al. 2001, 2004

  4. LOFAR Wokshop • Radio halos: • extended ( 1 Mpc) radio sources • at the cluster centre • regular morphology (~X-ray) • Radio mini halos: • smaller sources ( 500 kpc) • at the centre of clusters with: • AGN • cooling-core • Radio relics: • extended (~1 Mpc) radio sources • cluster outskirts • elongated morphology + polarised Feretti, Fusco-Femiano et al. 2001 A2163: XMM + VLA Gitti, Ferrari et al. 2007 X-ray images + radio contours Ferrari, Arnaud et al. 2006 RX J1347-11: XMM + VLA A521: Chandra + VLA

  5. LOFAR Wokshop 30 arcmin z ~ 0.2 A2163: radio halo Feretti et al. 2001 Dimensions: ~1 Mpc Crossing time e-: ~9.5 Gyr Life time of e-: ~0.1 Gyr Origin of relativistic electrons

  6. LOFAR Wokshop credits: C. Pfrommer • Primary models: (re-)acceleration due to shocks/turbulence • (e.g. Enßlin et al. 1998; Brunetti et al. 2001, 2004; Cassano & Brunetti 2005) • Secondary models:hadronic collisions of relativistic p+with the ICM • (e.g. Dennison 1980; Blasi & Colafrancesco 1999; Dolag & Enßlin 2000) • Prim. + Sec. models: a combination of the two • (e.g. Pfrommer et al. 2008; Cassano et al. 2008) Origin of relativistic electrons

  7. LOFAR Wokshop Measure of intracluster magnetic fieldsDiscrepant results • Equipartition assumption: ~0.1 – 1 μGauss • Compton scattering of CMB photons: ~0.1 – 0.3 μGauss • Faraday rotation measure: ~1 - 10 μGauss • X-ray analysis of cold fronts: ~10 μGauss

  8. LOFAR Wokshop Radio + Thermal X-ray Radio / X-ray comparison Nature of the non-thermal cluster component (1) • Radio + Non-Thermal X-ray

  9. LOFAR Wokshop Radio + Thermal X-ray A2163: Feretti et al. 2001 XMM (image) + VLA (contours) A2255: Govoni et al. 2001 Radio / X-ray comparison Nature of the non-thermal cluster component (1) • Radio X-ray morphologies

  10. LOFAR Wokshop Radio + Thermal X-ray A2256: Clarke & Enßlin 2006 Chandra (image) + VLA (contours) Radio / X-ray comparison Nature of the non-thermal cluster component (1) • Radio X-ray morphologies • Halos & Relics  Cluster mergers

  11. LOFAR Wokshop Radio + Thermal X-ray Brunetti et al. 2007 Radio / X-ray comparison Nature of the non-thermal cluster component (1) • Radio X-ray morphologies • Halos & Relics  Cluster mergers • P1.4GHz LX (TX )

  12. LOFAR Wokshop Radio + Thermal X-ray A665: Feretti et al. 2004 Radio / X-ray comparison Nature of the non-thermal cluster component (1) • Radio X-ray morphologies • Halos & Relics  Cluster mergers • P1.4GHz LX (TX ) • Radio spectral index  Distance from the X-ray centroid

  13. LOFAR Wokshop Radio + Thermal X-ray A773: Orrù et al. 2007  327 MHz1400 MHZ TX (keV) Radio / X-ray comparison Nature of the non-thermal cluster component (1) • Radio X-ray morphologies • Halos & Relics  Cluster mergers • P1.4GHz LX (TX ) • Radio spectral index  Distance from the X-ray centroid • Radio spectral index TX

  14. LOFAR Wokshop TICM + radio contours Govoni et al. 2004 A773 Giant radio halos & relics: cluster mergers Johnston-Hollitt et al. 2002 Relics  ICM shocks A3667 X-ray + radio contours Giant halos  turbulence

  15. LOFAR Wokshop Radio + Thermal X-ray XMM (image) + VLA (contours) TX A773: Orrù et al. 2007  327 MHz1400 MHZ X-ray surf. bright. Radio surf. bright. TX (keV) Radius RX J1347: Gitti, Ferrari et al. 2007 Radio / X-ray comparison Nature of the non-thermal cluster component (1) • Radio X-ray morphologies • Halos & Relics  Cluster mergers • P1.4GHz LX (TX ) • Radio spectral index  Distance from the X-ray centroid • Radio spectral index TX • Mini-halos AGN + cooling-core

  16. LOFAR Wokshop Radio + Thermal X-ray ROSAT (image) + VLA (contours) A 2255: Govoni et al. 2001 6 cm 3.6 cm Radio / X-ray comparison Nature of the non-thermal cluster component (2) • Magnetic field mesurements • Rotation Measure • Cold front analysis

  17. LOFAR Wokshop Radio + Thermal X-ray Chandra A 3667: Vikhlinin et al. 2001 Magnetic layer Radio / X-ray comparison Nature of the non-thermal cluster component (2) • Magnetic field mesurements • Rotation Measure • Cold front analysis

  18. LOFAR Wokshop Chandra (red/yellow) + VLA (blue & contours) Beppo-SAX HXR excess Fusco-Femiano et al. 2000 Clarke & Ensslin 2006 Radio / X-ray comparison Nature of the non-thermal cluster component (3) Radio + Non-thermal X-ray • Relativistic electrons: γ>>1000 • CMB photons Inverse Compton emission (hard X-ray &  domain) A 2256 e- energy distribution synchrotron emissivity IC flux

  19. LOFAR Wokshop Main limits of current analyses • Low statistics •  60 clusters with detected diffuse radio emission • < 15 clusters with detected hard X-ray excess • < 10 clusters with detailed radio spectral index maps • Lack of current intruments’ sensitivity • Distribution on the Lradiovs. LX plane: bimodal or not? • Radio relics: associated to ICM shocks? • Low significance of the hard X-ray excess ( < 5) • Systematic errors in the background level • Lack of spatial information & ICMmulti-temperature plasma • Contamination by AGNs

  20. LOFAR Wokshop Radio / X-ray comparison : some open questions • Origin of relativistic particles • Primary models (  halos & relics  new tracers of large-scale structure formation) • Secondary models • Primary + Secondary (Pfrommer et al. 2008: unified model for all halos and relics) • Intra-cluster magnetic fields • Intensity & Structure • Non-thermal cluster component • Effects on the thermal ICM (energy budget, heat conduction, overall pressure) • Detection of the non-thermal HXR emission •  e.g. Fusco-Femiano et al. 1999, 2004, 2007 (Beppo-SAX), Repaheli et al. 1999, 2002 (RXTE), Eckert et al. 2008 (INTEGRAL), ... • e.g. Rossetti & Molendi 2004 (Beppo-SAX), Eckert et al. 2007 (INTEGRAL), Ota et al. 2008 (Suzaku), Ajello et al. 2008 (Swift/BAT), ...

  21. LOFAR Wokshop Study of non-thermal emission with LOFAR:multi-wavelength comparison coll.: Ferrari, Arnaud, Feretti, Tagger, Aghanim, ... & «Clusters of galaxies» working group in the« Extragalactic Survey » Key Project • Statistical studies of diffuse radio emissionvs. global cluster porperties(mass, dynamical state, LX, ...) & z • (based on « All Sky Survey » – Röttgering et al. 2008) • Detailed radio/X-ray comparisons for a cluster sub-sample • Thermal X-ray emission: Chandra & XMM • Non-thermal X-ray emission: Simbol-X • (based on «Deep Survey» – Röttgering et al. 2008)

  22. LOFAR Wokshop Ferrari 2008 Brightness profile Brunetti et al. 2007 1023 W/Hz 1024 W/Hz 1025 W/Hz 1026 W/Hz L1.4GHz =1 Cassano et al. 2007 Diffuse radio sources with LOFAR

  23. LOFAR Wokshop  = 1 Rhalo as a function of P1.4GHz 80% of flux detected at 10  sig. level Statistical studies Diffuse radio emission vs. global cluster properties & z All Sky Survey sensitivity limits – Röttgering et al. 2008 Ferrari 2008 LX z

  24. LOFAR Wokshop  = 1 Rhalo as a function of P1.4GHz 80% of flux detected at 10  sig. level  = 1.5 Rhalo as a function of P1.4GHz 50% of flux detected at 10  sig. level Statistical studies Diffuse radio emission vs. global cluster properties & z All Sky Survey sensitivity limits – Röttgering et al. 2008 Ferrari 2008 LX z

  25. LOFAR Wokshop  = 1 Rhalo as a function of P1.4GHz 80% of flux detected at 10  sig. level  = 1 Rhalo = 0.5 Mpc 80% of flux detected at 10  sig. level Statistical studies Diffuse radio emission vs. global cluster properties & z All Sky Survey sensitivity limits – Röttgering et al. 2008 Ferrari 2008 LX z

  26. LOFAR Wokshop  = 1 Rhalo as a function of P1.4GHz 80% of flux detected at 10  sig. level  = 1 Rhalo = 0.5 Mpc 50% of flux detected at 10  sig. level Statistical studies Diffuse radio emission vs. global cluster properties & z All Sky Survey sensitivity limits – Röttgering et al. 2008 Ferrari 2008 LX z

  27. LOFAR Wokshop  = 1 Rhalo as a function of P1.4GHz 80% of flux detected at 10  sig. level  = 1 Rhalo = 0.5 Mpc 80% of flux detected at 20  sig. level Statistical studies Diffuse radio emission vs. global cluster properties & z All Sky Survey sensitivity limits – Röttgering et al. 2008 Ferrari 2008 LX z

  28. LOFAR Wokshop  = 1 Rhalo as a function of P1.4GHz 80% of flux detected at 10  sig. level  = 1.5 Rhalo as a function of P1.4GHz 50% of flux detected at 10  sig. level Statistical studies Diffuse radio emission vs. global cluster properties & z All Sky Survey sensitivity limits – Röttgering et al. 2008 Ferrari 2008 LX z

  29. LOFAR Wokshop Radio luminosity of diffuse radio sources vs. • Physical properties of their host systems (dyn. state, mass, LX, TX) • Redshift (possible connections with the Planck cluster catalogue) Statistical studies Diffuse radio emission vs. global cluster properties & z Ferrari 2008  = 1.0 (e.g. Orrù et al. 2007) Rhaloas a function of P1.4GHz 80% of flux detected at 20  s.l. All Sky Survey (Röttgering et al. 2008)

  30. LOFAR Wokshop Radio luminosity of diffuse radio sources vs. • Physical properties of their host systems (dyn. state, mass, LX, TX) • Redshift (possible connections with the Planck cluster catalogue)  = 1.5 (e.g. Brentjens 2008) Rhaloas a function of P1.4GHz 80% of flux detected at 20  s.l. All Sky Survey (Röttgering et al. 2008)  = 1.0 (e.g. Orrù et al. 2007) Rhaloas a function of P1.4GHz 80% of flux detected at 20  sig. level Statistical studies Diffuse radio emission vs. global cluster properties & z Ferrari 2008  = 1.0 (e.g. Orrù et al. 2007) Rhaloas a function of P1.4GHz 80% of flux detected at 20  s.l. All Sky Survey (Röttgering et al. 2008)

  31. LOFAR Wokshop Detailed radio/X-ray comparisons Deep Survey sensitivity limits – Röttgering et al. 2008 Adapted from Cassano et al. 2006 • 30 MHz • Resolution ~ 20 arcsec • 20 detection - 80% of the radio flux Ferrari 2008

  32. LOFAR Wokshop z = 0.1 Detailed radio/X-ray comparisons Deep Survey sensitivity limits – Röttgering et al. 2008 Adapted from Cassano et al. 2006 • 30 MHz • Resolution ~ 20 arcsec • 20 detection - 80% of the radio flux Ferrari 2008

  33. LOFAR Wokshop z = 0.2 Detailed radio/X-ray comparisons Deep Survey sensitivity limits – Röttgering et al. 2008 Adapted from Cassano et al. 2006 • 30 MHz • Resolution ~ 20 arcsec • 20 detection - 80% of the radio flux Ferrari 2008

  34. LOFAR Wokshop z = 0.3 Detailed radio/X-ray comparisons Deep Survey sensitivity limits – Röttgering et al. 2008 Adapted from Cassano et al. 2006 • 30 MHz • Resolution ~ 20 arcsec • 20 detection - 80% of the radio flux Ferrari 2008

  35. LOFAR Wokshop z = 0.4 Detailed radio/X-ray comparisons Deep Survey sensitivity limits – Röttgering et al. 2008 Adapted from Cassano et al. 2006 • 30 MHz • Resolution ~ 20 arcsec • 20 detection - 80% of the radio flux Ferrari 2008

  36. LOFAR Wokshop z = 0.5 Detailed radio/X-ray comparisons Deep Survey sensitivity limits – Röttgering et al. 2008 Adapted from Cassano et al. 2006 • 30 MHz • Resolution ~ 20 arcsec • 20 detection - 80% of the radio flux Ferrari 2008

  37. LOFAR Wokshop z = 0.6 Detailed radio/X-ray comparisons Deep Survey sensitivity limits – Röttgering et al. 2008 Adapted from Cassano et al. 2006 • 30 MHz • Resolution ~ 20 arcsec • 20 detection - 80% of the radio flux Ferrari 2008

  38. LOFAR Wokshop z = 0.8 Detailed radio/X-ray comparisons Deep Survey sensitivity limits – Röttgering et al. 2008 Adapted from Cassano et al. 2006 • 30 MHz • Resolution ~ 20 arcsec • 20 detection - 80% of the radio flux Ferrari 2008

  39. LOFAR Wokshop z = 1.0 Detailed radio/X-ray comparisons Deep Survey sensitivity limits – Röttgering et al. 2008 Adapted from Cassano et al. 2006 • 30 MHz • Resolution ~ 20 arcsec • 20 detection - 80% of the radio flux Ferrari 2008

  40. LOFAR Wokshop Ferrari 2008 LX z Detailed radio/X-ray comparisons Adapted from Cassano et al. 2006 z=0.2 LOFAR estimates: Ferrari 2008 z=0.1 • 30 MHz • Resolution ~ 20 arcsec • 20 detection • 80% of the radio flux

  41. LOFAR Wokshop Ferrari 2008 LX • Simbol-X • Spectro-Imager • 0.5-80 keV • ~15“ angular resolution • ~12‘ F.o.V. z Detailed radio/X-ray comparisons Adapted from Cassano et al. 2006 • 30 MHz • Resolution ~ 20 arcsec • 20 detection • 80% of the radio flux z=0.2 LOFAR estimates: Ferrari 2008 z=0.1

  42. LOFAR Wokshop Brunetti et al. 2007b F 60-100 keV = 10-13 erg cm-2 s-1 5 x10-12 erg cm-2 s-1 # clusters with detected HXR 10-12 erg cm-2 s-1 B=0.2 G Ferrari 2008 LX B=0.2 G B=2.0 G Simbol-X limits z Detailed radio/X-ray comparisons Adapted from Cassano et al. 2006 z=0.2 LOFAR estimates: Ferrari 2008 z=0.1 • 30 MHz • Resolution ~ 20 arcsec • 20 detection • 80% of the radio flux

  43. LOFAR Wokshop Optimal for the detection of radio relics A2163 (z~0.2) + Simbol-X F.o.V Ferrari 2008 LX Arnaud 2008 z Detailed radio/X-ray comparisons @ z  0.2 !!! Adapted from Cassano et al. 2006 z=0.2 LOFAR estimates: Ferrari 2008 z=0.1 • 30 MHz • Resolution ~ 20 arcsec • 20 detection • 80% of the radio flux

  44. LOFAR Wokshop • + Complementary studies • Statistical studies : e.g. possible comparison with Planck cluster catalogue • Detailed studies : e.g. energetics of the ICM & AGN feedback Conclusions Galaxy clusters  hierarchical scenario of structure formation  Physics of formation and evolution of galaxy clusters  Nature and origin of the non-thermal cluster component • Statistical studies : halos/relics presence & luminosity • vs. • global clusters properties (e.g. mass, dyn. state) & z • Detailed studies : radio emission in galaxy clusters • vs. • thermal and non-thermal X-ray emission

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