The development of the Infrared Camera and Spectrograph called CAMILA is described. It is based on a NICMOS 3 HgCdTe detector developed by Rockwell with a spectral response of 1-2.5 /im. The initial configuration of the system was recently concluded and consists of the following components: detector cryostat , detector control electronics, low noise preamplifiers, detector-PC interface, operating system and optics. The characterization of the electronics and the science grade chip are presented. The complete optical configuration allows the following modes of operation: direct imaging (12 filter positions), polarimetry and spectroscopy on three dispersion modes (low, medium and high resolution). Preliminary spectroscopic results at the H band with R=1500 are presented. The project is a collaborative effort of groups from IAUNAM and UMASS (Amherst) and will be used mainly at the 2.1 m telescope of San Pedro Mártir, B.C. (Mexico).
Wc arc developing an instrumcnt to study the morphology and kinematics of tIic molecular gas (H2) and its interrelationship with the ionized gas in star forming regions. planetary nebulae and supernova remnants in our Galaxy fl(1 other galaxies, as well as the kinematics of the infrared emitting gas in starl)urst and interacting galaxies. This instrument consists of a water-free fused silica scanning Fabry-Perot interferometer (SFPI) optimized in the spectral range from 1.5 to 2.4 im with high spectral resolution (11=27000 at 1.5 tm). It will he installed in the collimated beam of a nearly 2:1. focal reducer, (Iesigne(I for the Cassegrain focus of the 2.1 m telescope of the San Pedro Mártir National Astronomical Observatory. Mexico. in its f/7.5 configuration, yielding a field of view of 11.6 arc-mm. It will provi(Ie direct images as well as interferograms to be focused on a 1024x 1024 HAWAII array. covering a spectral range from 0.9 to 2.5 m.
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