ISAAC is an infrared (1 - 5 μm) imager and spectrograph mounted on the Nasmyth A focus of UT3. It has two independent arms, one equipped with a 1024 x 1024 Hawaii Rockwell array and the other with a 1024 x 1024 InSb Aladdin array from Santa Barbara Research Center. The Hawaii arm is used at short wavelengths (1 - 2.5 μm). The Aladdin arm is used predominantly at long wavelengths (3 - 5 μm) but is also available for short wavelength imaging with broad band filters. Below we summarize in two tables the operational modes and predicted performance of ISAAC. Those tables are intended as a quick feasibility references only: proposers should refer to the detailed information (e.g. User's Manual, Exposure Time Calculator). All instrument modes are offered in both Visitor Mode and in Service Mode).
|Instrument Mode||Scale||FOV||limit magnitude|
|SW Imaging||0.148||152 x 152||J=24, H=23, Ks=22|
|SW Polarimetry||0.148||3 x 20 x 150||J=23, H=22, Ks=21|
|LW Imaging||0.071||73 x 73||L~16, M_NB ~ 13|
|LW Imaging 3.21, 3.28μm||0.148||152 x 152||L ~16|
 In polarimetry the FOV consists of three non-overlapping strips each of 20 x 150 arcsec^2.
The limit magnitudes in the table are the J (1.25μm), H (1.65μm), Ks (2.2μm), and L (3.8μm) background limited magnitudes for a point source which would give a S/N of 5 in one hour of typical background conditions and a seeing FWHM of 0.65''. In addition to the standard J, H, Ks, and L broadband filters, ISAAC is equipped with a wide selection of narrow bands (typically = 0.015μm) filters. It is not possible to observe with ISAAC with user supplied filters.
|Instrument Mode||λ/Δλ||Scale||limit magnitude range|
|SW LRes Spectroscopy||500||0.147||18-20.5|
|SW MRes Spectroscopy||3000||0.147||17.5-19.5|
|LW LRes Spectroscopy||500||0.147||11-14|
|LW MRes Spectroscopy||2000||0.147||10-13|
The limit magnitudes given in the above table are the short wavelength (SW) and long wavelength (LW) magnitudes of a point source spectrum which would give a S/N of 5 per resolution element in the continuum in one hour under typical background conditions, seeing FWHM of 0.65'', and using a 1.0'' slit. Limits on IR spectroscopic capabilities vary strongly with wavelength due to the absorption/emission spectrum of the atmosphere, the range of limit magnitudes given in the table reflects this variation.
This document was last updated: 2010-11-30