PPT-Clusters of galaxies

With a widefield multiIFU spectrograph Cluster studies Clusters provide large samples of galaxies in a moderate field Unique perspective on the interaction of galaxies with their environment As they operate much as a closed box they are useful as tracers of galaxy evolution and of cosmology. Thorsten Naab . MPA, . Garching. . What regulates galaxy formation? . Leiden, April, 22. nd. How do massive galaxies get their gas and stars?. Gas accretion involves dissipation – energy can be radiated away . Anja. von . der. Linden et al., 2007, MNRAS, 379, 867. On the prevalence of radio-loud active galactic nuclei in brightest cluster galaxies: implications for AGN heating of cooling flows. P. N. Best et al., 2007, MNRAS, 379, 894. Paul . Nulsen. (. CfA. ), Christine Jones (. CfA. ), . William Forman (. CfA. ), Eugene . Churazov. (MPA),. Laurence David (. CfA. ), Brian McNamara (Waterloo),. Steven Murray (. CfA. ) . AGN Outbursts in Giant . The Milky Way Galaxy. When you look into the hazy band of light across the sky, you are actually looking at our galaxy from the inside. While an awesome sight, you can only truly begin to see it if you get away from city lights on a moonless night. . . 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.. 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. David Roberts, Jake Cohen, & Jing Lu. Brandeis University. Lakshmi . Saripalli. & Ravi . Subrahmanyan. Raman Research Institute. 1. Radio Galaxies. X-Shaped Radio Galaxies. Cheung’s Sample. Paul . Nulsen. (. CfA. ), Christine Jones (. CfA. ), . William Forman (. CfA. ), Eugene . Churazov. (MPA),. Laurence David (. CfA. ), Brian McNamara (Waterloo),. Steven Murray (. CfA. ) . AGN Outbursts in Giant . H.-W. Rix IMPRS Galaxies Course March 11, 2011. Goal:. Determine . n. *. (M. *. ,. t. age. ,[Fe. /H],. R. ). . for a population of galaxies. How many stars of what mass and metallicity . formed when and where in galaxies?. Giuseppina. . Battaglia. Instituto. de . Astrofisica. de Canarias, Tenerife. Credit. : ESO/. H.H.Heyer. Credit. : ESO/L. . Calçada. Karachentsev. et al. 2014. Individual . Red . Giant Branch . stars. 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 . 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 . 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 .