As of July 2022 the noise problem on CCD2 and CCD1 persists.

Users have been advised to choose an appropriate dither strategy (*) minimizing the effects of the bad amplifier on their science data and/or to place targets or spectral features of interest on other parts of the detector. See this document for further description. For MOS and IFU-R, the same strategy can be applied as well (does not work for IFU-2).  The main additional difficulty is the wavelength calibration since some arc lines are wiped out and the autoidentify task may fail. In this case, the lines identification has to be done interactively.

GMOS-S is scheduled for troubleshooting at the CPO Instrument Lab starting July 18th. It will be unavailable from the mentioned date, and back online once the telescope shutdown concludes (August 26th).

(*) For dithers we recommend +/-30 arcseconds in P (across the detector columns) in the case of imaging, and for spectroscopy a spectral dither size of at least +/-15nm for B1200, +/-25 nm for R831, +/-30nm for B600, and +/-45nm for R400.