  Based on gas-phase laboratory spectra at 6 K, Campbell et al. (2015)
confirmed that the diffuse interstellar bands (DIBs) at 9632.7 and 9577.5A are
due to absorption by the fullerene ion C60+. They also reported the detection
of two other, weaker bands at 9428.5 and 9365.9A. These lie in spectral regions
heavily contaminated by telluric water vapour lines. We acquired CFHT ESPaDOnS
spectra of HD183143 close to the zenith and chopped with a nearby standard to
correct for the telluric line absorption which enabled us to detect a DIB at
9365.9A of relative width and strength comparable to the laboratory absorption.
There is a DIB of similar strength and FWHM at 9362.5A. A stellar emission
feature at 9429A prevented detection of the 9428.5A band. However, a CFHT
archival spectrum of HD169454, where emission is absent at 9429A, clearly shows
the 9428.5A DIB with the expected strength and width. These results further
confirm C60+ as a DIB carrier.
