The Thick Disks of Spiral Galaxies as Relics from Gas-Rich, Turbulent, Clumpy Disks at High Redshifts Frédéric Bournaud, Bruce G. Elmegreen, and Marie.
Nearby Galaxies (mostly) at mm and IR wavelengths Adam Leroy (MPIA Heidelberg) Christof Buchbender (IRAM Granada)
STELLAR NURSERIES .
Density Waves and Migrating Planets 3 December 2014.
Understand Galaxy Evolution with IR Surveys: Comparison between ISOCAM 15- m and Spitzer 24- m Source Counts as a Tool Carlotta Gruppioni – INAF OAB.
Stellar Formation 1)Solar Wind/Sunspots 2)Interstellar Medium 3)Protostars 4)A Star is Born October 23, 2002.
Stellar Evolution: Parts of Chapters 12,13,15,16 Stellar Evolution: Parts of Chapters 12,13,15,16 Stars lose energy - hence they must evolve. Stars lose.
Rich cluster [M ~ 10 15 M sun ] Large groups (Small clusters) [M ~ 10 13 - 10 14 M sun ] Environmental effects on neutral and molecular hydrogen of galaxies.
Looking for the siblings of the Sun Borja Anguiano & RAVE collaboration.
Star Formation. Classifying Stars The surface temperature of a star T is compared to a black body. –Luminosity L –Radius R The absolute magnitude calculates.
12 April 2005AST 2010: Chapter 221 The Death of Stars.
Sub-mm/mm astrophysics: How to probe molecular gas Yasuo Fukui Nagoya University Summer School The Gaseous Universe Oxford, 21-23 July 2010 1.