PPT-The Detectability of Lyα Emission from Galaxies during

the Epoch of Reionization Dijkstra Mesinger Wyithe JC 2114042 Alex Fry The physics of reionization comoving star formation rate number of ionizing photons above 912 nm or 137 . JWST Workshop. – . STScI. Baltimore. June 8, 2011. Mid-Infrared Observation of High . Redshift. Galaxy Evolution. Most star formation activity occurs behind dust . Chary & Pope . 2011. Bouwens. Adam Leroy. National Radio Astronomy Observatory. HERITAGE (. Meixner. et al.). Dust in Dwarf Galaxies. Adam Leroy. National Radio Astronomy Observatory. HERITAGE (. Meixner. et al.). SAGE (. Meixner. Lecture 8: Dusty starburst galaxies. Prof.. . Dr.. M. . Baes. (. UGent. ). Prof.. . Dr.. C. . Waelkens. (KUL). Academic year 2015-2016. The interstellar medium. The space between the stars in a galaxy is not empty. as Seen at . Very High Energies. Elisa Prandini . Dipartimento. . di. . Fisica. & INFN Padova. . prandini@pd.infn.it. Dipartimento. . di. . Astronomia. , . Padova, 23. rd. June 2011. Outline. Li Jiang-Tao. 1. Service d’Astrophysique, CEA, Saclay, France. 2. . Department. of . Astronomy. , . University. of Michigan, Ann Arbor, USA. Outline. 1. Introduction. 2. Diffuse X-ray . observation. :. Active Galactic Nuclei: powerful energy sources in . “nuclei” . (. central ~1 pc) . of some galaxies. Main types. : . Seyferts. , radio galaxies and quasars. Other variants we’ll skip.. Power source: accretion of matter onto a supermassive black . 2. Emission and Active Transformation within Compact Groups . Image Credit: NASA,ESA and the Hubble SM4 ERO Team . Michelle Cluver . mcluver@aao.gov.au. Collaborators. Philip Appleton (NHSC/Caltech). 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. Hydrogen Gas. AAO. . Colloquium . . 5th February 2015. Philip Lah. Collaborators:. Frank Briggs (ANU. ). Jayaram Chengalur (NCRA) . Matthew Colless (. ANU). Roberto De Propris (FINCA. 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 . z. >3.5 galaxies with. AKARI-FUHYU NIR spectroscopy. Chris Sedgwick. Stephen Serjeant. Chris Pearson. The Open University. on behalf of the FUHYU mission program. Phase III FUHYU Mission Program. 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. around Abell 370, . a galaxy cluster at z = 0.37. International SKA . Forum 2010 . Philip Lah. A New Golden Age for Radio Astronomy. Collaborators:. . Frank Briggs (ANU). . Michael Pracy . 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.