Astronomical source definition

Spatial profile and brightness: (more info)
Choose one of point, extended or user-defined source profile and the brightness in any filter/wavelength
Point source (nominal PSF) with spatially integrated brightness (e.g. 19.3 mag or 2e-17 W/m²/µm)
Extended source having ...(When this option is selected the image quality selection in section 3 of the ITC is disabled.)
Gaussian profile with full width half maximum (including seeing) of arcsec and spatially integrated brightness of (e.g. 19.3 mag or 2e-17 W/m²/µm)
Uniform surface brightness (e.g. 21.6 mag/arcsec²)
with the above brightness normalisation applied in filter band


Spectral distribution: (more info)
Choose one SED, the redshift and extinction
Library spectrum of a non-stellar object
Library spectrum of a star with spectral type
Single emission line at wavelength micron with line flux and line width km/s on a flat (in wavelength) continuum of flux density
Model black body spectrum with temperature K
Model power-law spectrum (S_lambda = lambda ^ )
User-defined spectrum read from file (size < 1MB)
with the spectrum mapped to a redshift z = or a radial velocity v = km/s

 

Instrument (NIFS), telescope, and Altair configuration

Instrument optical properties:
Filter:
Grating: Spectrum central wavelength: µm
Detector properties:
Read mode:
Medium background for observations of bright objects, e.g. standard stars (Read noise = 15.4 e-)
Low background for observations of faint objects, e.g. science targets (Read noise = 8.1 e-)
Very low background for observations of the faintest targets (Read noise = 4.6 e-)
Dark current:   0.01 e-/s
Telescope configuration: (more info)
Mirror coating: silver
Instrument port: up-looking port
Wavefront sensor for tip-tilt compensation: PWFS Altair
Altair properties: (more info)
AO guide star separation: arcsec AO guide star brightness (R-band): mag
Field Lens: OUT IN (Required for LGS) Altair Mode: NGS LGS

 

Observing condition constraints

Note: you should read the explanatory notes for the meaning of the percentiles and to ensure that your selected conditions are appropriate for the observing wavelength. Further details are available on the observing condition constraints pages.
Image quality: 20%/Best 70%/Good 85%/Poor Any
Sky transparency (cloud cover): 50%/Clear 70%/Cirrus 80%/Cloudy Any
Sky transparency (water vapour): 20%/Low 50%/Median 80%/High Any
Sky background: 20%/Darkest 50%/Dark 80%/Grey Any/Bright
Typical air mass during observation: <1.2 1.5 2.0

 

Details of observation

Calculation method: (more info)
Total S/N ratio resulting from exposures each having coadds with exposure time of secs and with a fraction of exposures that observe the source
Telescope offset:(more info)
Dither offset size: arcsec
Analysis Method:
Select multiple IFU elements to be summed : by apertures(each one 0.103x0.042 arcsec)
Select an individual IFU element offset by arcsec from the center
Select multiple IFU elements along a radius with offsets of to arcsec
Output:
For spectroscopy, autoscale or specify limits for plotted spectra (lower wavelength micron and upper wavelength micron)