'Galaxy formation' presentation slideshows

Galaxy Formation and Evolution Galactic Archaeology

Galaxy Formation and Evolution Galactic Archaeology. Chris Brook Modulo 15 Room 509 email: cbabrook@gmail.com. Lecture 5: Galactic Archeology. The Structure of our Galaxy. Old components of the Milky Way. Formation of the Milky Way. Formation of the Milky Way.

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The Current State of Observational Cosmology

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Parallel Programming & Cluster Computing Overview: What the Heck is Supercomputing?

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Unstructured grids for Astrophysics Gas dynamics and radiative transfer

Unstructured grids for Astrophysics Gas dynamics and radiative transfer. C.P. Dullemond Max Planck Institute for Astronomy Heidelberg, Germany. Overview. Radiative transfer (RT) in astrophysics: Small introduction to the physics of radiative transfer

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Large-Scale Structure in the DEEP2 Galaxy Redshift Survey

Large-Scale Structure in the DEEP2 Galaxy Redshift Survey. Jeffrey Newman Lawrence Berkeley National Laboratory. And The DEEP2 Team.

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High Redshift Quasar Survey

Survey Science Group Workshop, 2013 High1 Resort. High Redshift Quasar Survey. Yiseul Jeon, Myungshin Im, W.-K. Park, J. H. Kim, M. Karouzos, J.-W. Kim, S.-K. Lee, H. Jun, C. Choi, D. Kim, D. Kim, J. Hong, M. Hyun, and Y. C. Taak

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Search for winter break

Search for winter break. Are we there yet?. IDea. A. Individuals with Disabilities Education Act B. Individual Development and Educational Assessment C. International Debate Education Association D. Institutional Diagnostic and Evaluation Activity. Intro to Astronomy diagnostic.

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Thermal History

Thermal History. Prof. Guido Chincarini Here I give a brief summary of the most important steps in the thermal evolution of the Universe. The student should try to compute the various parameters and check the similarities with other branches of Astrophysics.

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Comparing with redshift surveys of galaxies

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Photometric and Morphological Properties of LBGs at z~1

Photometric and Morphological Properties of LBGs at z~1. Chenggang Shu Key Lab for Astrophysics, Shanghai Normal University (ShNU) with Zhu Chen (ShNU), Denis Burgarella, V eronique B uat (OAMP), Jiasheng Huang (CfA) & Zhijian Luo (ShNU).

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SINS high redshift galaxy S pectroscopic I maging survey in the N ear-IR with S INFONI

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Observations of AGN Outflows and Their Contribution to Feedback

Observations of AGN Outflows and Their Contribution to Feedback. Gordon Richards Drexel University. With thanks to Sarah Gallagher, Karen Leighly , Pat Hall, Paul Hewett, Nahum Arav , Daniel Proga , TJ Cox, and John Everett. Merger Scenario w / Feedback. merge gas-rich galaxies

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Future Radio Interferometers

Future Radio Interferometers. Jim Ulvestad National Radio Astronomy Observatory. Radio Interferometer Status in 2012. ALMA Covers much of 80 GHz-1 THz band, with collecting area of about 50% of VLA, for a cost exceeding $1 billion Higher frequencies ?infrared

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Lecture 7. Galaxy Formation

w Cen. 47 Tuc. Lecture 7. Galaxy Formation. After decoupling, overdense regions collapse IF Collapse time for all sizes. More small ripples than large waves . --> Universe dominated by globular clusters (?!). Caveats.

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Open Questions

Open Questions. Satellite galaxies II (and other stuff). Data rich subject. Lots of data out there: Observers have quantified how satellite properties depend on stellar mass halo mass redshift But what do these trends mean?. Take-away message from yesterday:

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http://chandra.harvard.edu/photo/2007/m51/

http://chandra.harvard.edu/photo/2007/m51/. Confronting Stellar Feedback Simulations with Observations of Hot Gas in Elliptical Galaxies . 3-D stellar feedback simulation. NGC 4697: X-ray intensity contours. Q. Daniel Wang, Shikui Tang, Yu Lu, Houjun Mo (UMass)

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Search for Galaxies at z>~7 in the GOODS-N field

Search for Galaxies at z>~7 in the GOODS-N field. Masami Ouchi (STScI). Figure credit: Kajisawa. Overview. 1) Motivation & background of our z>7 galaxy search: I highlight some results from our deep and wide-field survey of Subaru for z=5-6 galaxies.

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A tale of Two Universes

A tale of Two Universes. Radaition vs Matter Dominance. Matter energy density and radiation energy density have difference dependence on expansion factor R: Radiation density falls more rapidly than matter energy density. Radiation vs Matter. Radiation Dominated Era.

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