MAMA Spectral Offsetting

For the FUV-MAMA, the repeller wire produces a small shadow on the detector with a depth of ~10% which is apparent on FUV-MAMA flat field images (see MAMA Properties). To avoid first-order mode spectra falling on the repeller wire shadow, all data taken with the G140L and G140M gratings are projected to fall 3 arcseconds or ~120 low-resolution pixels below the repeller wire (to AXIS2 = 392) from the detector center (see also "MAMA ACCUM Mode" on page 216). This offsetting is done using the Mode Select Mechanism to tilt the grating. For these modes the projected field of view is therefore asymmetric with respect to the specified target coordinates. Note that in Cycle 7, prior to March 15, 1999, the offset from the detector center was done in the opposite direction (to AXIS2 = 632). However, as this caused G140L and G140M point source spectra to fall onto the region of the FUV-MAMA with the highest dark current, this was changed to the current setting. Observers who wish to match the field of views of Cycle 7 observations will need to take this difference into account.

For both the FUV- and the NUV-MAMA, the projection of the spectra on the detector for all spectroscopic modes is shifted slightly each month. This procedure is performed in order to minimize uneven charge depletion in the microchannel plates which would increase the non-uniformity of the flat fields. These monthly charge-offsetting shifts can shift the spectrum ±30 low-resolution pixels in AXIS1 (dispersion) and ±80 low-resolution pixels in AXIS2 (cross-dispersion). Hence observers are advised to select settings that keep wavelength ranges of interest away from the extremes of wavelength settings and targets of interest away from the extreme ends of the long slits.