- Gemini Home
- Telescopes and Sites
- Science Visitors at Gemini
- Observing With Gemini
- Retired Instruments
- 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:
NIRI Sensitivity Tables (no AO)
The values in these tables are based on results from the NIRI Integration Time Calculator. They assume 70-percentile (IQ70, ~average) image quality for all categories, photometric conditions (CC50), and an airmass of less than 1.2 for the sensitivites presented here. At 3 to 5 microns median water vapor (WV50) and shorter wavelengths "any" water vapor were assumed; water vapor has little impact on the near-IR imaging sensitivity, or on spectroscopic sensitivity in the middles of the J, H, and K windows, but does significantly effect the edges of the JHK windows where absorption by telluric water vapor is strong. The estimates also use the measured telescope, camera, and detector performances. Note that some sky conditions vary outside of those stated above. For example, OH emission, although scaled by airmass, can intrinsically vary by over a factor of two from night to night and over much shorter timescales - which can alter S/N and sensitivity by +/- sqrt2 in the J, H, and K bands. Thus observers should use both the table and the ITC with some caution and conservatism.
Regarding readout noise and detector well depth, note that:
- 1-2.5um narrow band faint source imaging and spectroscopy used the shallow well and low read noise mode
- JHKsK'K imaging used the shallow well and medium read noise mode
- All thermal IR (3-5um) imaging and spectroscopy used the deep well and high read noise mode
|NIRI IMAGING SENSITIVITY (S/N=5 IN 1 HOUR, N.I. OVERHEADS) - NO ADAPTIVE OPTICS|
|Filter||Center wavelength (µm)||Point Sources||Extended Sources||Individual Exposure (sec)||Approx. Total Throughput|
|H2 1-0 S(1)||2.122||21.5||1.7E-03||21.6||1.5-03||600|
- The estimates in the table are for exposures that are background-limited in all cases. As a result, in imaging mode there is very little difference in achieved sensitivities between the different cameras. The f/6 camera provides the best sampling and field-of-view for tip-tilt corrected images without adaptive optics correction. Because of the high and varying (with weather and airmass) background levels in the thermal IR , observations at L band and M band use the f/32 camera to prevent saturating on the sky background.
- For imaging, the ITC calculates the S/N in an aperture that maximizes S/N, given the predicted image quality for the observing conditions and wavelength requested. The sensitivity values in the table below use this optimum ITC aperture. For accurate photometry much larger apertures usually must be used, and sensitivities are reduced, typically by a factor of 2 or more.
- Approximate total throughput values in the imaging table are as measured for the entire system, including the telescope, instrument, and detector.