The Nature and Orbit of the Ophiuchus Stream

<p>The *_chain.txt files contain Markov chains that model the line-of-sight<br /> velocity (RV_chains.txt), color-magnitude diagram (CMD_chains.txt), and<br /> proper motion and the extent of the Ophiuchus stellar stream (PM_chains.txt). By randomly selecting rows from these files, one can sample the corresponding probability density functions.The columns in each file are briefly described below.</p> <p>RV_chains.txt:</p> <p>&nbsp;&nbsp;&nbsp; column 1: line-of-sight velocity at {ell}_0=5deg,<br /> &nbsp;&nbsp;&nbsp; column 2: gradient in line-of-sight velocity, d(v_los)/d({ell})<br /> &nbsp;&nbsp;&nbsp; column 3: additional scatter in line-of-sight velocities, s</p> <p>CMD_chains.txt:<br /> &nbsp;&nbsp;&nbsp; column 1: age, t<br /> &nbsp;&nbsp;&nbsp; column 2: mass-loss parameter, eta<br /> &nbsp;&nbsp;&nbsp; column 3: metallicity content, Z<br /> &nbsp;&nbsp;&nbsp; column 4: offset in reddening with respect to the Schlegel et al. (1998)<br /> &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp; [1998ApJ...500..525S] reddening, (E(B-V)_off)<br /> &nbsp;&nbsp;&nbsp; column 5: distance modulus at {ell}_0=5deg,<br /> &nbsp;&nbsp;&nbsp; column 6: gradient distance modulus, d(DM)/d({ell})<br /> &nbsp;&nbsp;&nbsp; columns 7-11: uncertainty in isochrone magnitudes, {sigma}_iso_m,<br /> &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp; where m=[g,r,i,z,y,]</p> <p>PM_chains.txt:<br /> &nbsp;&nbsp;&nbsp; column 1: fraction of stars associated with the field population, 1-f<br /> &nbsp;&nbsp;&nbsp; column 2: natural logarithm of the width of the stream in the<br /> &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp; galactic latitude direction, ln({sigma}_b)<br /> &nbsp;&nbsp;&nbsp; column 3: natural logarithm of the width of the field population in the<br /> &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp; galactic latitude direction, ln({sigma}_p_b)<br /> &nbsp;&nbsp;&nbsp; column 4: A_p<br /> &nbsp;&nbsp;&nbsp; column 5: B_p<br /> &nbsp;&nbsp;&nbsp; column 6: ln({sigma}_pm)<br /> &nbsp;&nbsp;&nbsp; column 7: ln({sigma}_p_pm)<br /> &nbsp;&nbsp;&nbsp; column 8: &lt;{mu}_{ell}&gt;<br /> &nbsp;&nbsp;&nbsp; column 9: d({mu}_{ell})/d({ell})<br /> &nbsp;&nbsp;&nbsp; column 10: &lt;{mu}_b&gt;<br /> &nbsp;&nbsp;&nbsp; column 11: d({mu}_b)/d({ell})<br /> &nbsp;&nbsp;&nbsp; column 12: &lt;{mu}_p_{ell}&gt;<br /> &nbsp;&nbsp;&nbsp; column 13: d({mu}_p_{ell})/d({ell})<br /> &nbsp;&nbsp;&nbsp; column 14: &lt;{mu}_p_b&gt;<br /> &nbsp;&nbsp;&nbsp; column 15: d({mu}_p_b)/d({ell})<br /> &nbsp;&nbsp;&nbsp; column 16: {ell}_min<br /> &nbsp;&nbsp;&nbsp; column 17: {ell}_max<br /> &nbsp;&nbsp;&nbsp; column 18: A<br /> &nbsp;&nbsp;&nbsp; column 19: B<br /> &nbsp;&nbsp;&nbsp; column 20: C</p> <p>&nbsp;</p>