PPT-Ay 124 Structure and Dynamics of Galaxies

R Ellis amp S G Djorgovski Winter 2011 Class Logistics All info lecture notes useful links homeworks exams announcements etc will be on the class website httpwwwastrocaltecheduschenkeray124. CoEPP. , University . of Melbourne. June . 26 2014. Explaining galactic structure and direct detection experiments with mirror dark matter. 1. For further details see review:. See this review for detailed references to the literature. (Resolved by Galileo). Milky Way:. Galactic Structure and Dynamics. Milky Way has spiral structure. . Galactic Bulge surrounds the Center. . Powerful radio source Sagittarius A at Center. C. ontains Super-Massive Black Hole . 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. By Dr. Frank Elwell. Introduction. In the last lecture . I presented . the universal structure of all societies and categorized the various parts of sociocultural systems. This categorization makes it possible to examine the relationships among the component parts and to see how the components affect each other.. 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. metallicity. star-forming dwarf galaxies. Diane Cormier . ITA, ZAH, University of Heidelberg – group of Frank . Bigiel. Suzanne Madden, . Vianney. . Lebouteiller. , . Sacha. . Hony. , Fr. é. d. 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 . . Why Spiral Arms?. Why not just an undisturbed uniform disk?. Well, remember that . the innermost parts rotate faster than those farther out.. This suggests . one . obvious possibility: some linear structure forms, then . Immigration. Emigration. Population. Biomass. Growth. Natural Mortality. Fishing Mortality. Recruitment. Size Structure Methods. Length frequencies. Proportional Size Distribution (PSD). was “Proportional Stock Density”. Spiral Structure. . The Astronomical Context. By the 1920’s, we knew that the once-mysterious spiral nebulae were flattened galaxies. . Our Milky . Way is . also. flattened. . Two obvious . questions arose:. Priest Associate Professor of Physics. Galaxies. 9/4/18. Milky Way Galaxy Contents & Motions. 9/11/18. Milky Way Environment & the Local Group. 9/18/18. Other Galaxies & Clusters of Galaxies. 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 . . Craig Roberts. Collaborators: 2014-Present. Jing CHEN (Peking U.). Bo-Lin LI (Nanjing U.). Ya. LU (Nanjing U.). Khépani. RAYA (U . Michoácan. ). ;. Chien. -Yeah SENG (UM-Amherst) ;. Chen . CHEN.