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One set of blank sky images in these bands is taken once per semester for fringe frame generation. GMOS images show some fringing in z' and Y bands. Other readout modes can use the same flat fields when the ratios of the gains for the different readout modes are taken into account. The typical noise in the avarage of the twilight flats that can be obtained in a given run is 0.75 percent.Дome flats may also be taken, but are not guaranteed to be part of the baseline calibration set.ДЄll flat fields are obtained in slow read, low gain mode. All twilight flats from a 10-14 night dark period are combined in order to built a high S/N flat field. Imaging twilight flats are taken each day as the weather allows. The bad pixel mask for the imaging mode will show the areas outside the imaging field of view as bad pixels, even though the pixels are not strictly bad, just not illuminated by the imaging field of view. May be derived more often if changes in the detector array are found. GMOS Imaging ModeДerived each semester from dome flats and bias images. All raw data is available as well as processed biases, imaging twilight flats, and some standards.

spectrophotometric standard stars will not be taken with Nod-and-Shuffle.ДЄll calibration data is available through the Gemini ObservatoryВ Archive. Any time required for additional calibrations requested by the PI will be charged to that particular program.ДЇor Nod-and-Shuffle observations all baseline calibrations (with the exception of the Nod & Shuffle Darks) will be taken without Nod-and-Shuffle, e.g.

The time will be charged in proportion to the number of programs that receive the calibration data. it is part of the time accounting used to balance partner usage). Any time used between the hours of nautical sunset and sunrise to obtain baseline calibrations will not be explicitly charged to the program but will be charged to the partner country whose NTAC recommended time (i.e. Note that all calibrations, including baseline arcs, flats, spectral response standards and Nod & Shuffle Darks must be included in the Phase II science program.Д«aseline calibration data may be shared between programs and will be distributed to the users as part of their dataset. If additional calibrations are deemed necessary by applicants, for example to achieve a precision beyond that achievable via the baseline set, then these must be included explicitly as part of the Phase I proposal and Phase II science program. The required 'Night Basecal Time' per observation is automatically calculated by the Phase I Tool (PIT). SinceВ 2017B the time required for nighttime baseline calibrations has to be included inВ the 'Total Time' requestedВ during Phase I. The baseline calibration set varies from instrument to instrument and from mode to mode. Baseline calibrations will be obtained for all observations, both queue and classical.ДЇor all queue observations a set of standard calibrations (the 'baseline calibrations'), shown in the tables below, will be taken by Gemini Staff to ensure the long-term utility of data in the archive. Flat-fielding is done with GCAL or on the sky during twilight. Wavelength calibration of GMOS is obtained using GCAL, the facility calibration unit.

Gemini In The Era of Multi-Messenger Astronomy.

Gemini Telescopes, Science and Technologies.

Timing information in Gemini Instruments.

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