MOSFIRE Exposure Time Calculator - Details

For a source flux fλ in erg s-1 cm-2 Å the following equation is used used to produce a value of counts per resolution element:

fλ(λ) Astop(band) texp dλ(band) η(λ) (h c)-1 λ

where the quantities are as follows:

Note that slit loss is calculated assuming a Gaussian seeing profile so that for a seeing value of FWHM the loss is: 1-erf(1.665 slit width/FWHM) in appropriate units. For typical seeing of 0.75" and slit width of 0.7" (2.9 pix) the loss is about 3% (seems LOW, CHECK!).

The detected noise is estimated assuming counting statistics for the source object and sky. A square-root-of-two penalty is applied assuming that the image is subtracted from itself as is the case with A-B subtraction.

The detector noise was measured and reported in the PSR. Read noise is estimated assuming a Fowler 16 readout and is measured to be 4.9 e- per pixel. The dark current is 0.008 e-/s/pix and again counting statistics are applied to the dark current. Note that for the dark-current noise to equal the read noise an integration time of 50 minute is required.

Noise calculations often require the number of extraction pixels (Npix). The number of pixels is equal to the width of the resolution element described above (Nspec) times the number of extraction pixels (Nsptial) which we estimate as 2/3 x (seeing FWHM) where the spatial pixel scale is 0.18" per pixel. For typical seeing of 0.7" and slitwidth this amounts to: Nspec=2.9 and Nspatial=2.6. The number of extracted pixels is typically Npix=8.

Thus, after converting the signal from erg to DN, the total noise is estimated as follows:

noise = (2 source DN + 2 sky DN + (RN2 Npix) + (DC Npix texp))1/2
Systematics will dominate the faint reach (and ultra high SNR) capabilities of MOSFIRE, because it is hard to simulate these, they are not included in this simple simulator. Depending on your application the following sources of systematic uncertainty may limit your performance:
PSR : Pre ship review report.