- Gemini Home
- Telescopes and Sites
- Science Visitors at Gemini
- Observing With Gemini
- Retired Instruments
- Status and Availability
- Nod and Shuffle
- Spectroscopy Overview
- Long-slit Spectroscopy
- Multi-Object Spectroscopy
- Integral Field Spectroscopy
- ITC, Sensitivity and Overheads
- Guiding Options
- Observation Preparation
- Data Format and Reduction
- Visiting Instrument Policy
- Visiting Instrument Telescope Interfaces
- DSSI Speckle Camera
- TEXES (North)
- Integration Time Calculators
- Magnitudes and Fluxes
- Near-IR Resources
- Mid-IR Resources
- Observing Condition Constraints
- Performance Monitoring
- SV/Demo Science
- Future Instrumentation & Current Development
- Queue and Schedules
- Data and Results
- Gemini Research Staff
Change page style:
The commissioninig of the GMOS-N Hamamatsu detector array and the corresponding web page updates are ongoing.
GMOS-N and GMOS-S use identical gratings and all gratings are available with each GMOS. However, some gratings are more heavily used than others and therefore spend more time in the instruments; see the grating statistics for recent semesters. Note in particular that the R600 grating is rarely installed in either GMOS; queue programs should carefully consider whether their science requirements could be accommodated with either the R400 or R831 gratings instead.
A new R150 grating has been available at GMOS-N since December 2016. See details here.
There is a new B600 grating available at GMOS-N since May 2009. See details here.
The table lists the properties of the GMOS gratings based on laboratory measurements. The resolving power R is given at the blaze wavelength, and refers to the resolution achieved with a slit width of 0.5 arcsec. The effective slit width of the IFU in the dispersion direction is 0.31arcsec, see the IFU grating/filter combination page for details.
Efficiency curves based on laboratory data are available. Note that the new GMOS-S Hamamatsu detectors have significant quantum efficiency at 1 µm, falling below 5 percent for wavelengths longer than ~ 1.07 µm (see GMOS-S Hamamatsu array page for more details). The quantum efficiency of the old GMOS-S EEV detectors was below 5 percent for wavelengths longer than 1000 nm. The grating efficiencies assumed by the GMOS-N ITC are extrapolations for wavelengths longer than 1 µm and will be updated once all the gratings have been characterized with the new GMOS-N Hamamatsu detectors. There is no laboratory data available for these gratings longward of 1 µm.
None of the gratings are currently officially offered in 2nd order; however tests have shown that the second order mode for the R600 and R831 gratings may be of interest for some applications. Contact your GMOS instrument scientist for more information.
|Grating name||Grating number*||Ruling density
|B600|| (G5303 replaced 05/2009)
|R150|| (G5306 replaced 12/2016)
*The grating name is the concatenation of grating and grating number e.g.R831_G5302 for the Gemini North R831 grating.
**The R600 grating is under-utilized and queue programs may have difficulty with completion due to competition for the three grating slots from the other five gratings. Hence the R600 grating is not available for regular queue programs. Classical programs may still request the R600 grating.