PPT-The cosmological formation of massive galaxies

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 . Richard B. . Larson. Yale University. Conclusions. Compact objects such as stars and black holes generally form in larger systems such as binaries, multiple systems, star clusters, or galaxies.. Gravitational interactions in these larger systems play a major role in the formation of compact objects by transporting angular momentum.. The Cosmic Time Machine. Astronomical telescopes can’t help viewing the past.. . Distance and time are always mixed in astronomical observations.. The finite speed of light means that we always see things after they have happened–a delay of 8 minutes for the Sun and about 12 billion years for the most distant galaxies we can observe. In other words,. Anatomy of Extragalactic . R. adio Sources. Miley. Symposium May, 2013, Chris Carilli NRAO. ‘Radio Galaxies as beacons to early, massive galaxy formation’. Anatomy at low redshift. High luminosity (FRII, L. Emil . Björnson. ‡*. , . Michail . Matthaiou. ‡§. , and . Mérouane. . Debbah. ‡. ‡. Alcatel-Lucent Chair on Flexible Radio, . Supélec. , France. *. Dept. Signal Processing, KTH, and Linköping University, Sweden. 1. The ". Q". word and its meaning. Is quenching a good word to describe the end of star-formation in galaxies ? . What are the timescale(s) for quenching? . Pablo , Jarle. Is quenching due to starvation or gas expulsion? . 23. vs. .. 1. First spiral nebula found in 1845 by the Earl of . Rosse. . Speculated it was beyond our Galaxy.. 1920 - "Great Debate" between Shapley and Curtis on whether spiral nebulae were galaxies beyond our own. Settled in 1924 when Edwin . Michael Fall. STScI. . CoolSci. Talk. . Specific Angular Momentum . vs. Mass. Fall 1983. . j. = J/M . α. . M. α. with . α. ≈ . 2/3. S and E galaxies offset by ~6x. D. Calzetti (Univ. of Massachusetts). a. nd the LEGUS . Team. https://. legus.stsci.edu. /. HUBBLE2020: Hubble’s 25. th. Anniversary Symposium. STScI. , Baltimore, April 20-24, 2015. NGC3344. NGC1566. Division of Particle and Astrophysical Science, Nagoya University, JAPAN. with. SKA-Japan high-. z. galaxy and cosmology WG. East-Asia SKA core member meeting, 29 May, 2012, ASIAA, Taipei, Taiwan. Fluctuation, Stars, and Galaxies: Light and Shadow of the Cosmic Structure Formation through H. 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 . Here’s the Story We’ll Unfold for You…. Hubble’s galaxy classifications: Spirals, . ellipticals. , irregulars. . Structural parts of galaxies: disk, halo, nucleus, bulge. Spiral arms – tracers of star formation. homgeneity. of the universe.. 2. understand how Hubble’s law is used to map the universe, and look back in time.. 3. Know each of the major predictions of the Big Bang theory, and corresponding confirmations by observation.. How Galaxies form Stars – August 24 2016 . Robbert. Verbeke. 1. Bert . Vandenbroucke. Sven De . Rijcke. Ghent University. 1. Robbert.verbeke@ugent.be. @. Rbhfd. Λ. CDM. Standard model for cosmology. GUViCS. ). IV. The role of the cluster environment on galaxy evolution. Speaker: Xinkai Chen. Sample. Sample:. Extended Source . Catalogue of Voyer+14. recessional . velocity < . 3500kms-1. , Virgo cluster region.