tests:discs

Discussion on 19-23 Aug, 2013

Anonymous (anonymous@undisclosed.example.com) — 2022-10-24T12:26:58+00:00

Discussion on 19-23 Aug, 2013 These are ideas and initial results of the challenges discussed in the Surrey workshop week. However, please feel free to post your mock data, grab the data and do your own challenge. Please also feel free to discuss off-line and build up collaborations.

Results in Gaia Challenge 2013 (Surrey)

Anonymous (anonymous@undisclosed.example.com) — 2022-10-24T12:26:58+00:00

Results in Gaia Challenge 2013 (Surrey) Challenge A Using GD1 by Hunt & Kawata Bovy See his presentation K$_{z,1.1}$ is similar to the target galaxy. Chemin See his presentation Recover rotation curve and pattern speed of the bar and spirals.

Local Dark Matter Density

Anonymous (anonymous@undisclosed.example.com) — 2022-10-24T12:26:58+00:00

Local Dark Matter Density Here you find simple 1D mocks and full N-body mocks for trying to recover the Local Dark matter density, * Simple 1D mocks * Full N-body mocks The method being used by Hamish Silverwood and Sofia Sivertsson is described in this paper (Silverwood, Sivertsson, Steger, Read, Bertone, 2015).

Pattern Speed of the Bar and Spiral Arms

Anonymous (anonymous@undisclosed.example.com) — 2022-10-24T12:26:58+00:00

Pattern Speed of the Bar and Spiral Arms Who Chemin, Pfenniger, Romero-Gomez, Hunt, Kawata Objectives Recover Bar and Spiral arm pattern speed from Mock data using different methods Methods * Tremaine-Weinberg Method (Chemin, Romero-Gomez)

Identifying Stellar Motions associating different Spiral Arm Scenarios

Anonymous (anonymous@undisclosed.example.com) — 2022-10-24T12:26:59+00:00

Identifying Stellar Motions associating different Spiral Arm Scenarios Who R. Grand, S. Roca-Fabrega, L. Jilkova, C. Martinez-Barbosa, H. Abedi, J. Hunt Objectives Identifying Stellar Motions associating different Spiral Arm Scenarios Results Line of sight velocity of an axisymmetric distribution as function of galactic longitude:

Short Talks Programme (27 Oct. 2014)

Anonymous (anonymous@undisclosed.example.com) — 2022-10-24T12:26:58+00:00

Short Talks Programme (27 Oct. 2014) 5 min talk + 5 min question time Time Name 14:30-14:40 Daisuke Kawata Welcome 14:40-14:50 Jose Fernandez-Trincado The Besancon Galaxy Model with a triaxial bar 14:50-15:00 Robert Grand Spiral Arms 15:00-15:10

Victor Debattista's Model R1

Anonymous (anonymous@undisclosed.example.com) — 2022-10-24T12:26:58+00:00

Victor Debattista's Model R1 This is the Milky Way scaled version of Model R1 of , which is selected one of the best Milky Way model in . Model Description Data file Moderl R1 Barred N-body simulation Publication policy If using these data, please cite the Gaia Challenge wiki and

N-body models from Elena D'Onghia

Anonymous (anonymous@undisclosed.example.com) — 2022-10-24T12:26:58+00:00

N-body models from Elena D'Onghia Snapshots provided by Elena D'Onghia from her simulations in , which have 100 million disk particles. Ask Jo Bovy to get these from a USB stick. The simulation and data consists of snapshots at 0 Myr (initial conditions), 250 Myr, and 1 Gyr (snap_000.hdf5, snap_005.hdf5, snap_020.hdf5).

GCD+ N-body disc model by Hunt & Kawata

Anonymous (anonymous@undisclosed.example.com) — 2022-10-24T12:26:58+00:00

GCD+ N-body disc model by Hunt & Kawata N-body disc models simulated with GCD+ (Kawata & Gibson 2003). These are the target disc models used in Hunt, Kawata & Martel (2013). The fixed Navarro, Frenk & White (1997) dark matter halo profile is applied: \rho _{dm}=\frac{3H_{0}^{2}}{8\pi G}\frac{\Omega _{0}-\Omega_b}{\Omega_0}\frac{\delta_{c}}{cx(1+cx)^{2}}

Analytic global models with a known distribution function and background potentials

Anonymous (anonymous@undisclosed.example.com) — 2022-10-24T12:26:58+00:00

Analytic global models with a known distribution function and background potentials N-body representations of an analytical distribution function of the form used by McMillan and Binney (2012), evaluated in two different potentials. The distribution function represents a single

Local models/mocks

Anonymous (anonymous@undisclosed.example.com) — 2022-10-24T12:26:58+00:00

Local models/mocks These mock data give positions and velocities for stars in and around the Solar neighbourhood, relevant for recovering the local Galactic potential and e.g. dark matter content. Simple 1D data sampled from a distribution function of vertical energy

Full N-body models (with local cuts)

Anonymous (anonymous@undisclosed.example.com) — 2022-10-24T12:26:58+00:00

Full N-body models (with local cuts) These are full collisionless N-body simulations. The first two were published and analysed in and . The latter two include a perturbing satellite at low and high inclination. There are four simulations: Simulation

Barcelona Mock data Suite

Anonymous (anonymous@undisclosed.example.com) — 2022-10-24T12:26:58+00:00

Barcelona Mock data Suite Test particles data (Barred potential) Data provided by UB team (Romero-Gomez et al.). The simulation is described [here]. Ascii file: 21635205 Red Clump particles with Grvs<16.1 (from a sample of 72M) -In each row: G ,Grvs ,Xreal (Kpc),Yreal (Kpc),Zreal (Kpc),VXreal (Km/s),VYreal (Km/s),VZreal (Km/s),Xobs (Kpc),Yobs (Kpc),Zobs (Kpc), VXobs (Km/s),VYobs (Km/s),VZobs (Km/s)