PPT-Diffuse Synchrotron Emission in Clusters of Galaxies - What's Next?

Summary Talk Craig Sarazin University of Virginia Observations of radio halos minihalos and relics review Tiziana Venturi Nice overview p roperties of halos relics minihalos. . CDM Cosmology. Oleg . Gnedin. (University of Michigan. ). What we knew before HST: globular clusters are old, dense, compact – a distinct type of stellar spheroids. Kormendy. (1985). Over 20 years the Hubble Space Telescope has revealed young massive star clusters in interacting and gas-rich galaxies.. POWER . RADIO. GALAXIES AS BEACONS FOR CLUSTERS TO “FILL THE GAP”. AT 1<z<2. Marco Chiaberge. Space Telescope Science Institute. A. . Capetti. INAF- OATO. G. Tremblay RIT. P. . Tozzi. INAF-OATS. 2013/12/18. Speaker . : Yu-. Hsun. Cheng. Professor: Yosuke Mizuno. Introduction. Supernova remnants(SNR):. . This is . the structure resulting from the explosion of a star in a supernova. . It is formed by that the interactive between interstellar and . 이민웅. Shader. Study. Wrapped Diffuse. 팀 포트리스 . 2. 에서 사용. subsurface scattering, area light source, . 더 부드러운 . reflectance . 를 표현하기 위해서 . Hemisphere(. Most of the power of galaxies come from the stars. Almost all nearby galaxies. Some galaxies have very bright sources right at the center. Can be as bright as a galaxy!. Or even much brighter. Called . The Hubble Tuning-Fork Diagram. This is the traditional scheme for classifying galaxies:. Elliptical Galaxies. Elliptical galaxies. have smooth, round distributions of stars. They resemble globular clusters, except they are much larger. They . Craig Sarazin. University of Virginia. M86. (. Randall et al. 2008). . Abell. 2052. (Blanton et . al. . 2011). Optical light dominated by bulge. Last star formation typically billions of years ago. Galaxy Morphology and Environment. Main relation – . E’s more common in clusters than field. f(E. ) = fraction of ellipticals . f(Sp. ) = fraction of spirals. regular, symmetric cluster – . f(E. diffuse X-ray emission – a survey of highly inclined disk galaxies. How is the emission correlated with galaxy properties?. How . are observations compared to simulations. ?. Nature of the emission – X-ray line spectroscopy. Sources. 1. Sources of high-energy particles. We now have clear observational diagnostics for particle acceleration. synchrotron radiation (radio, sometimes X-ray). inverse Compton scattering (X-ray, . remnants. Rino Bandiera. INAF – . Arcetri. Astrophysical Obs.. FOE17 Fifty-One Erg. Corvallis, OR, June 5-8, 2017. The . many. . reasons. to . study. . SNRs. 2. Debris. of a stellar . explosion. Rybicki. & . Lightman. Chapter 6. Also Course notes for “Essential Radio Astronomy” at NRAO, . Condon & Ransom. http://www.cv.nrao.edu/course/astr534/ERA.shtml. Synchrotron Theory: Summary of Results. Laura . Magrini. INAF- . Osservatorio. . Astrofisico. di . Arcetri. In Our Galaxy. Open clusters (disc population): . Many (~2200 known clusters). . even more new candidates in the inner disc from infrared surveys . TIME - - RAY COMPUTED TOMOGRAPHY AS A TOOL FOR GROUNDWATER REMEDIATION Nathaly Lopes Archilha 1 Gabriel Schubert Costa 1 , Tannaz Pak 2 1 Brazilian Synchrotron Light Laboratory (LNLS/CNPEM) and 2 T