the only instrument that uses the chopping mode of the secondary mirror. MIRSI has a selection of broad-band and narrow-band filters, as well as a CVF. MORIS MORIS (MIT Optical Rapid Imaging System) s a high-speed, visible-wavelength camera for use on IRTF using an electron multiplying CCD. MORIS is mounted on the side window of SpeX, and is fed by the internal cold dichroic in SpeX. The design is based on POETS (Portable Occultation, Eclipse, and Transit Systems), which were developed by a collaboration between MIT and Williams College. MORIS is available for open use on IRTF and its user interface has been converted to the IRTF standard interface. In addition to visible light photometry, MORIS is also used as a visible light guider for SpeX, allowing guiding on targets as faint as V=20. The guiding software includes atmospheric dispersion correction to move the visible light guide box to keep the IR image on the SpeX slit. Visiting instruments IRTF also hosts a number of visitor instruments, usually thermal infrared spectrographs. These have recently included TEXES, EXES, BASS, and HIPWAC. And others. Future instruments The IRTF staff are currently developing SPECTRE, an optical-to-infrared seeing-limited integral field unit. Past instruments CSHELL was retired when iSHELL began operations at IRTF. CSHELL was a 1 - 5.5 µm high resolution single-order echelle spectrograph which uses a 256 x 256 pixel InSb detector array. Each pixel was 0.2" on the sky and the spectroscopic dispersion is 100,000 per pixel. Slits from 0.5" to 4.0" provided spectral resolutions of up to 30,000. CSHELL also had an IR imaging mode for source acquisition which covers a 30" x 30" field. An internal CCD with a 1' FOV allows for guiding. NSFCAM2 was a 1-5 µm camera, built at the Institute for Astronomy, (IfA), for the NASA Infrared Telescope Facility (IRTF). The camera used a 2048x2048 Hawaii 2RG detector array. The image scale was 0.04 arcsec/pixel and the field of view is 82x82 arcsec. It contained two filter wheels. The first was a 28 position wheel containing broad-band and narrow-band filters, and a wire-grid polarizer. The second contained a 1.5-5 µm CVF and grisms. for low-resolution spectroscopy. A third wheel, located at the F/38 telescope focal plane inside the camera, contained grism slits and field lenses. An external wheel containing a waveplate could be used with a polarizer in the CVF wheel for polarimetry. NSFCam2 was taken