Introductory+Meeting

toc =Introductory Meeting= =Tuesday, 16 September, 2008= **2.00pm ** 
 * Small Seminar Room, KITP**

The video and audio of this meeting can be viewed [|online].

The following is a transcription of the contents of the blackboard at the end of the meeting. Please add/edit anything that you think was missed and add links to branch off new pages from here. If you want to add a comment on some item, click on the //discussion// tab at the top of this page.

=COSMOLOGICAL CONTEXT= =STRUCTURE & DYNAMICS= =ABUNDANCES= =MISCELLANEOUS/OTHER=
 * ==Dark matter==
 * Or no dark matter......?
 * ==Satellites Accretion history==
 * Gas flows
 * Star formation rate/Accretion rate discrepancy
 * ==How isolated is the Milky Way?==
 * Influence of M31
 * Simulations
 * Observations
 * ==Milky Way analogues==
 * Select by, e.g.
 * gas content
 * environment
 * ==Indirect dark matter detection (gamma rays)==
 * Why do different groups get different results
 * Streams/small scale distribution
 * ==Satellite dynamics==
 * Satellite/stream disconnect (i.e. don't see progenitors of streams)
 * Except for Sagittarius
 * Is this expected in simulations?
 * Are larger or deeper surveys more useful?
 * Do many streams come from one progenitor?
 * ==Globular clusters==
 * Are some of them really dwarf galaxies?
 * Are they of any use in Milky Way studies?
 * ==Next generation of simulations==
 * More realizations?
 * Better resolution?
 * More physics?
 * Baryons
 * How accurate are pure dark matter simulations (e.g. for gamma ray fluxes)
 * ==Baryonic content==
 * 2-3 times below expection of universal baryon fraction
 * Where is the halo gas? (COS)
 * Hidden at high temperature?
 * Can't match Tully-Fisher with 100% of universal baryon fraction
 * Can feedback solve the problem?
 * How robust is the data?
 * How well do we know virial mass
 * ==Bulge/Bar/Spirals/Non-axisymmetric features==
 * Ages?
 * ==Dynamical structures in disk==
 * Streams
 * Disk transients
 * ==Shape==
 * Fundamental parameters
 * Anisotropic distribution of satellites
 * ==Details of structure==
 * Quantify input/output responses
 * Connecting small scales to larger scales
 * Astrophysics is complicated!
 * ==Detailed abundances==
 * Currently only for 10's of stars
 * WFMOS
 * Disk/Halo/Satellites
 * Better techniques to measure?
 * ==ISM Data==
 * Milky Way + external galaxies
 * LMT
 * Theory
 * Still sub-grid
 * ==Galactic Center==
 * ==Stellar IMF==