These are the full MCMC chains used for the main suite of results from McMillan (2017, MNRAS, 465, 76). Each line gives the parameters of a single model, with some of its derived properties, and an associated weight (the number of steps that the chain stayed at this model). The parameters are described in the README file, and further detail can be found in the original paper. The disc density profiles are of the form (\begin{equation} \rho_d(R,z)=\left{\begin{array}{lc}\frac{\Sigma(R)}{2z_d},\textrm{exp}\left(\frac{-\mid z\mid}{z_d}\right) & \textrm{for }z_d > 0 \ \frac{\Sigma(R)}{4(-z_d)},\textrm{sech}^2\left(\frac{z}{2,z_d}\right) & \textrm{for } z_d < 0,\\end{array}\right. \end{equation}) where (\begin{equation} \Sigma(R)=\Sigma_0;\textrm{exp}\left(-\frac{R_0}{R}-\frac{R}{R_d}+ \epsilon\textrm{cos}\left(\frac{\pi R}{R_d}\right)\right), \end{equation} ) with parameters (\Sigma_0, R_d, z_d, R_0, \epsilon) (note that (R_0) here is not the position of the Sun, and that (\epsilon) is not used). Spheroids have (\begin{equation} \rho_s=\frac{\rho_0}{(r^\prime/r_0)^\gamma(1+r^\prime/r_0)^{\beta-\gamma}}; \textrm{exp}\left[-\left(r^\prime/r_{cut}\right)^2\right], \end{equation} ) where (\begin{equation} r^\prime = \sqrt{R^2 + (z/q)^2} \end{equation} ) with parameters ( \rho_0, q, \gamma, \beta, r_0, r_{cut}) (note that (r_0) is different again)

These are the full MCMC chains used for the main suite of results from McMillan (2017, MNRAS, 465, 76). Each line gives the parameters of a single model, with some of its derived properties, and an associated weight (the number of steps that the chain stayed at this model). The parameters are described in the README file, and further detail can be found in the original paper. The disc density profiles are of the form (\begin{equation} \rho_d(R,z)=\left{\begin{array}{lc}\frac{\Sigma(R)}{2z_d},\textrm{exp}\left(\frac{-\mid z\mid}{z_d}\right) & \textrm{for }z_d > 0 \ \frac{\Sigma(R)}{4(-z_d)},\textrm{sech}^2\left(\frac{z}{2,z_d}\right) & \textrm{for } z_d < 0,\\end{array}\right. \end{equation}) where (\begin{equation} \Sigma(R)=\Sigma_0;\textrm{exp}\left(-\frac{R_0}{R}-\frac{R}{R_d}+ \epsilon\textrm{cos}\left(\frac{\pi R}{R_d}\right)\right), \end{equation} ) with parameters (\Sigma_0, R_d, z_d, R_0, \epsilon) (note that (R_0) here is not the position of the Sun, and that (\epsilon) is not used). Spheroids have (\begin{equation} \rho_s=\frac{\rho_0}{(r^\prime/r_0)^\gamma(1+r^\prime/r_0)^{\beta-\gamma}}; \textrm{exp}\left[-\left(r^\prime/r_{cut}\right)^2\right], \end{equation} ) where (\begin{equation} r^\prime = \sqrt{R^2 + (z/q)^2} \end{equation} ) with parameters ( \rho_0, q, \gamma, \beta, r_0, r_{cut}) (note that (r_0) is different again)

Distance estimates used by "Gaia Early Data Release 3: The Galactic anticentre", Gaia Collaboration, Antoja et al. These are Bayesian distances with an iterative prior, referred to as d_PM within the paper (Appendix C). A parallax zero-point correction of 17µas has been applied before calculation. Any use of these distances should cite that paper.

Distance estimates used by "Gaia Early Data Release 3: The Galactic anticentre", Gaia Collaboration, Antoja et al. These are Bayesian distances with an iterative prior, referred to as d_PM within the paper (Appendix C). A parallax zero-point correction of 17µas has been applied before calculation. Any use of these distances should cite that paper.

Bayesian distance estimates for stars with radial velocities and parallaxes published in Gaia DR2. Our method and prior is designed to apply to this specific subset of stars in Gaia DR2.The method is published in "Simple distance estimates for Gaia DR2 stars with radial velocities", McMillan 2018, arXiv:1806.00426The code used to produce the estimates is here: https://doi.org/10.5281/zenodo.1270548

Bayesian distance estimates for stars with radial velocities and parallaxes published in Gaia DR2. Our method and prior is designed to apply to this specific subset of stars in Gaia DR2.The method is published in "Simple distance estimates for Gaia DR2 stars with radial velocities", McMillan 2018, arXiv:1806.00426The code used to produce the estimates is here: https://doi.org/10.5281/zenodo.1270548