SINFONI Exposure Time Calculator

Infrared Adaptive Optics Spectroscopy Mode Version P100.2
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Target Input Flux Distribution

Template Spectrum Redshift
z =
Target Magnitude and Mag.System:   
= Vega
Magnitudes are given per arcsec2 for extended sources
MARCS Stellar Model
Upload Spectrum
Blackbody Temperature: K
Power Law Index:           F(λ) ∝ λindex
Emission Line
Lambda: nm
Flux: 10-16 ergs/s/cm2 (per arcsec2 for extended sources)
FWHM: nm

Spatial Distribution: Point Source
Extended Source (per pixel)
Extended Source, area Ω: arcsec2

Reference Source Parameters

The ETC will not be able to compute performance estimates when the effective separation between the science target and the guide star is larger than 30"(NGS) or 60" (TTS in LGS), respectively

Adaptive Optics:
noAO AO not enabled
NGS Natural Guide Star Target / Reference Source
Separation: arcsec [0-30]
Reference Source
R mag: [9.3-16.3] B-R color:
LGS Laser Guide Star LGS / TipTilt Star
Separation: arcsec [0-60]
TipTilt Star
R mag: [10-18 (in V)] B-R color:
SE Seeing Enhanced

Sky Conditions

Airmass: range:[1, 3]
Seeing/Image Quality:
For point sources and non-AO instrument modes, the S/N reference area is defined by the Image Quality. The IQ is not considered with AO-modes, a model of the AO-corrected PSF is used instead. See the helpfile for details.
Seeing: arcsec FWHM in V-band at zenith (use this value in the proposal)
              Probability ---% of realising the seeing ≤ 1.00 arcsec
IQ: arcsec FWHM at the airmass and wavelength of observation (to be used for the OB constraint set)
              The corresponding seeing and probability will be indicated in the ETC output page
Image Quality is not a parameter in AO modes

Instrument Setup

Angular Resolution Scale: milliarcsec
Grating: Note for H+K (R=1500): The reference wavelength lies in a region with low atmospheric transmission and therefore the spectral plot should be activated in order to consult the spectral region of interest.


S/N ratio: S/N = DIT = s
Exposure Time: NDIT =

The total exposure time is the product of DIT (Detector Integration Time) by NDIT (number of DITs). Instrument and telescope overheads are not taken into account.

Plots: Toggle All / No Plots

Resultant spectrum including sky
Object Spectrum only
Sky Emission Spectrum
Sky Radiance Spectrum in physical units (ph/s/m2/micron/arcsec2)
Sky Transmission Spectrum
S/N as a function of wavelength
Total Efficiency and Wavelength Range
Input spectrum in physical units