In situ observation of the ICME resulting from the 2011 October 22 solar event. Shown from top to bottom are the magnetic field magnitude B, field inclination angle θ (with respect to the ecliptic plane), azimuthal angle ϕ (0 deg pointing to the Sun), three components (V_x, V_y, V_z) of the solar wind velocity in the GSE coordinate system, proton density N_p, proton temperature T_p (superimposed by T_p/T_exp, where T_exp is an empirical temperature determined from solar wind speed), plasma β, and half of the field-line length assuming that the flux-rope axial length is in the range 2–π AU. The dashed red curves show the model fitting results with the uniformly twisted flux-rope (Gold-Hoyle) solution. The closest approach of the observational path to the flux-rope axis d is 0.37 in terms of the rope radius; the goodness of fit χ_n is 0.21, which is the normalized root mean square of the difference between the fitting and observation.