Instrumentation


Professionally I have been a designer/builder of optical systems for visible and infrared instrumentation (see below).  I have worked on both spaced based and ground based telescopes for astronomy and remote sensing applications.  Currently I work for the Caltech Optical Observatories that design/build instrumentation for the W. M. Keck and Palomar Telescopes.

KCWI: 2010 – Current

The Keck Cosmic Web Imager (KCWI) is a wide field, seeing limited, integral field spectrograph (IFS) optimized for precision sky limited spectroscopy of low surface brightness phenomena.  KCWI will feature high throughput and flexibility in field of view (FOV), spatial sampling, bandpass, and spectral resolution. KCWI will provide full wavelength coverage (0.35 to 1.05 μm) using optimized blue and red channels. KCWI is based on the Cosmic Web Imager (CWI) recently commissioned at the Palomar Observatory. CWI is a single channel instrument with a fixed spatial sampling scale and a single adjustable VPH grating and an articulated camera with 2k x 4k mid-band optimized CCD. KCWI will build on the heritage of CWI with a two channel design offering three selectable spatial sampling scales and a selection of VPH gratings. KCWI will be located at the right Nasmyth focus of the Keck II telescope.

WFIRST: 2010-Current

TRICK: 2011-Current

MOSFIRE:  2007 – 2010

MOSFIREMOSFIRE will provide NIR multi-object spectroscopy over a field of view of 6.1 x 6.1 arcminutes, one atmospheric band at a time: Y band (0.97-1.12μm), J band (1.15-1.35μm), H band (1.46-1.81μm), or K band (1.93-2.45μm). The spectra cover most or all of the atmospheric band for slits placed anywhere within the field.  A multiplex advantage of up to 46 slits will be possible using a unique cryogenic robotic slit mask system that is reconfigurable electronically in less than 5 minutes without any thermal cycling of the instrument. The Configurable Slit mask Unit (CSU) is based on a prototype developed for the James Webb Space Telescope by the Swiss Centre for Micro-Electronics (CSEM). Using a single state of the art Teledyne H2RG HgCdTe detector with 2K x 2K pixels, MOSFIRE will capture most or all of an atmospheric window in a single exposure for any slit placed within a 6 x 3 arcminute field, and the instrument will employ a single, fixed diffraction grating used in multiple orders (3, 4, 5, and 6) for dispersion in the K, H, J and Y (a.k.a. Z) bands, respectively. In addition, MOSFIRE has been designed to be located at the Cassegrain focus of the Keck I telescope where it will provide faint object imaging and spectroscopic capabilities entirely complementary to the dual-beamed optical (0.3-1µm) spectrograph, LRIS.

VIIRS:  2002 – 2007

VIIRSThe Visible/Infrared Imaging Radiometer Suite (VIIRS) project is the main sensor on the National Polar-orbiting Operational Environmental Satellite System (NPOESS) spacecraft.  It is a satellite system used to monitor global environmental conditions, and collect and disseminate data related to: weather, atmosphere, oceans, land, and near-space environment.  VIIRS will provide imagery of clouds under sunlit conditions in about a dozen bands, and will also provide coverage in a number of infrared bands for night and day cloud imaging applications.  VIIRS will have multi-band imaging capabilities to support the acquisition of high-resolution atmospheric imagery and generation of a variety of applied products including visible and infrared imaging of hurricanes and detection of fires, smoke, and atmospheric aerosols.  VIIRS will also provide capabilities to produce higher-resolution and more accurate measurements of sea surface temperature than currently available as well as provide an operational capability for ocean-color observations and a variety of derived ocean-color products.