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:

<latex>\rho _{dm}=\frac{3H_{0}^{2}}{8\pi G}\frac{\Omega _{0}-\Omega_b}{\Omega_0}\frac{\delta_{c}}{cx(1+cx)^{2}}</latex>
where:
<latex> c=r_{200}/r_s </latex>,
<latex> x=r/r_{200},</latex>
<latex>r_{200}=1.63\times 10^{-2}\left(\frac{M_{200}}{h^{-1}M_{\odot}}\right)^{\frac{1}{3}} h^{-1},</latex>
and:
<latex>\delta_c = \frac{200}{3} \frac{c^3}{\left[\ln(1+c) - c/(1+c)\right]}.</latex>

We assume <latex>\Omega_0=0.266=1-\Omega_{\Lambda}</latex>, <latex>\Omega_{\rm b}=0.044</latex>, and <latex>H_0=71{\rm kms^{-1}Mpc^{-1}}</latex>. A live N-body disc is initially set up and simulated for several Gyr. The data file provides the position, velocity and mass of the disc particles. If you have any question, please email d.kawata (at) ucl (dot) ac (dot) uk.

ASCII data file format:
x,y,z,vx,vy,vz,mp
… format(7(1pE13.5))

x,y,z … position (kpc)
vx,vy,vz … velocity (km/s)
mp … particle mass (Msun)

Model	Description	<latex>M_{200}/M_\odot</latex>	<latex>c</latex>	<latex>N</latex>	Data file	Plot
GD1	Smooth disc	1.75e12	20	99,9982	gcdpdnf1.dat.gz
GD2	Barred disc	2.0e12	9	1,000,000	gcdpdbar1.dat.gz

Additionally, we provide the target GD2 in equatorial coordinates, with and without a Gaia-type error, treating the particles as tracers for a single stellar population, in this case M0 Giants.

The errors are computed following Gaia science performance estimates (credit to Mercè Romero Gómez & Francesca Figueras.)

The sun is located at (-8,0,0) kpc in cartesian coordinates. (Note that this does not take into account extinction)

ASCII data file format and units:
output.txt

For the GD1-RC stars for the challenge, the velocity of the sun w.r.t the GC is (0, 228.14, 0) km/s with the sun again at (-8,0,0) kpc.

If using these test data, please cite the Gaia Challenge wiki and Hunt, Kawata & Martel (2013).

Building on the similar challenge from last years workshop, we provide the data from an N-body galaxy in a known NFW dark matter halo potential, this time with dust extinction and Gaia like errors, for M0III tracers and Red Clump tracers as shown in Hunt & Kawata (2014).

For the GD3 stars for the challenge, the velocity of the sun w.r.t the GC is (0, 228.14, 0) km/s with the sun again at (-8,0,0) kpc. The fixed Navarro, Frenk & White (1997) dark matter halo profile is applied:

<latex>\rho _{dm}=\frac{3H_{0}^{2}}{8\pi G}\frac{\Omega _{0}-\Omega_b}{\Omega_0}\frac{\delta_{c}}{cx(1+cx)^{2}}</latex>
where:
<latex> c=r_{200}/r_s </latex>,
<latex> x=r/r_{200},</latex>
<latex>r_{200}=1.63\times 10^{-2}\left(\frac{M_{200}}{h^{-1}M_{\odot}}\right)^{\frac{1}{3}} h^{-1},</latex>
and:
<latex>\delta_c = \frac{200}{3} \frac{c^3}{\left[\ln(1+c) - c/(1+c)\right]}.</latex>

We assume <latex>\Omega_0=0.266=1-\Omega_{\Lambda}</latex>, <latex>\Omega_{\rm b}=0.044</latex>, and <latex>H_0=71{\rm kms^{-1}Mpc^{-1}}</latex>. A live N-body disc is initially set up and simulated for several Gyr. The data file provides the position, velocity and mass of the disc particles. If you have any question, please email d.kawata (at) ucl (dot) ac (dot) uk.

(Note that the mock data was edited on 24/10/14 to provide data with a similar bar angle to the Milky Way)

(The pre-edit data is here: m0iii-tracers.dat.gz)

ASCII data file format and units:
For extinction data: output.txt
For full data: (x,y,z,vx,vy,vz,mass) (kpc, kms^-1, M_solar). The Galactic centre is (0,0), the sun should be at (-8,0) to match extinction added data.

(Observed M0III data for V<16.5 mag, cartesian co-ordinates, with and without observational error)

Format: x,y,z,vx,vy,vz,Vmag (kpc & kms^-1)

If using these test data, please cite the Gaia Challenge wiki and Hunt & Kawata (2014).