These mock data are designed to mimic the Milky Way disc - either locally or globally. Key questions include, for the local problem:

(1) What quality of data are required to determine the local dark matter density? (2) Do multiple populations (e.g. split by abundance/age) help? (3) Is 1D modelling sufficient?

And for the global problem:

(1) Can global models simultaneously recover the disc phase space distribution function and the gravitational potential? (2) What are the key degeneracies in the problem and how can these be broken?

If posting new tests, please try to approximately follow the template set out for the “spherical collisionless tests” here.

Key working group coordinator: Daisuke Kawata

• Local Dark Matter Density

• Pattern Speed of the Bar and Spiral Arms

• Identifying Stellar Motions associating different Spiral Arm Scenarios

Can you recover V_LSR=218.4 km/s and (U,V,W)=(11,12,7) km/s from:

1. An axisymmetric disc galaxy without extinction or error?
2. The same galaxy with dust extinction added?
3. The same galaxy with dust extinction and Gaia like errors added?

The ascii data is provided with the following format:

The code has been updated to compute the astrometric and photometric errors for a fraction of the operation data.

• https://github.com/mromerog/Gaia-errors

• Simple 1D data sampled from a distribution function of vertical energy (Read)

• GCD+ N-body disc models (Hunt & Kawata)

• Analytic global models with a known distribution function and background potentials (McMillan)

• Full N-body models (with local cuts) from Justin Read

• N-body models from Elena D'Onghia

• Barcelona mock data suite

• Victor Debattista's Model R1

• Summary Talk of Disc Working Group at Gaia Challenge 2014 (Heidelberg) disc-summary14.pdf

• Short Talks Programme at Splinter Session 1 (27 Oct. 2014)

• Discussion in Gaia Challenge 2013 (Surrey)

• Results from Gaia Challenge 2013 (Surrey)