Wide binary data to test the validity of Newtonian gravity considering the perspective effects

In arXiv:2507.13177, we used wide binary data to test Newtonian gravity by considering the perspective effects. In particular, we used CSV files, basically following Chae's format in his following Zenodo repository, but slightly modified to consider the perspective effects. A statistical sample of pure wide binaries and python scripts to test gravity with stacked velocity profiles Python scripts to test gravity with the dynamics of wide binary stars We added two columns: 'mu1ra_perspec[mas/yr]' and 'mu1dec_perspec[mas/yr]'. To calculate the relative velocity of wide binaries by considering the perspective effects, use these two columns, instead of 'mu1ra[mas/yr]' and 'mu1dec[mas/yr]'. As explained at the end of Section 2, we merged two data sets to produce one data set for most of our analysis in the paper. 'penoyre.csv', containing 8095 wide binaries, was obtained from the condition that both stars have fractional proper motion uncertainties less than 0.5%. 'sigma_vp50_penoyre.csv', containing 8806 wide binaries, was obtained from the condition that both stars have the error of the relative (sky-projected) 2D velocity smaller than 50 m/s. They mostly overlap, and we obtained 'merge.csv' by merging these two files. 'merged_format.csv' is obtained from 'merged.csv' by replacing the columns 'mu1ra[mas/yr]' and 'mu1dec[mas/yr]' by 'mu1ra_perspec[mas/yr]' and 'mu1dec_perspec[mas/yr]' so that it can be run directly by Chae's codes. 'merged_format_flame.csv' is obtained by replacing the masses with GAIA FLAME masses when they are available. (42.7% of stars had GAIA FLAME masses.) It is used to draw the right panel of Fig. 6. 'mergedruwe11_format.csv' and 'mergedruwe13_format.csv' were obtained by the condition ruwe<1.1 and ruwe<1.3, respectively, instead of ruwe<1.2, and were used to draw Fig. 12. 'belokurov_fomat.csv' was obtained from 'merged_format.csv' by imposing a stricter condition in the Color-Magnitude Diagram as explained in Appendix C. It was used to draw Fig. 14. 'merged_format_bothRV.csv' was obtained from 'merged_format.csv' by filtering the ones with both radial velocities available and was used to draw Fig. 15. In all these files, a fake value of radial velocity error of 10,000 km/s was entered if the radial velocity of a star is unavailable. For such a star, the radial velocity is assumed to be the same as the radial velocity of its counterpart. As we removed binaries if neither of their two radial velocities is available, every star has a nominal value of radial velocity.