Neil Rowlands

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Verified

Neil verified their affiliation via an institutional email.

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• PhD
• Engineer Fellow at Honeywell

Astronomy and Space Domain Awareness are limited by the size of available telescope optics, the cost for which scales steeply due to the exquisitely ground and polished primary mirrors, typically made of glass or other lightweight substrates. Liquid mirrors (LMs) may break this unfavorable cost scaling. When rotated at a constant angular velocity,...

Astronomy and Space Domain Awareness are limited by the size of available telescope optics, the cost for which scales steeply due to the exquisitely ground and polished primary mirrors, typically made of glass or other light-weight substrates. Liquid mirrors (LMs) may break this unfavorable cost scaling. When rotated at a constant angular velocity,...

Under the Defense Advanced Research Projects Agency (DARPA) Zenith program, a novel concept has been developed for a self-assembling ferrofluidic ionic liquid mirror (FILM) telescope utilizing a Halbach array of permanent neodymium magnets. The primary mirror will be constructed from two immiscible liquids containing reflective and magnetic nanopar...

The Near-Infrared Imager and Slitless Spectrograph (NIRISS) is the science module of the Canadian-built Fine Guidance Sensor onboard the James Webb Space Telescope (JWST). NIRISS has four observing modes: (1) broadband imaging featuring seven of the eight NIRCam broadband filters, (2) wide-field slitless spectroscopy at a resolving power of ∼150 be...

The Near Infrared Imager and Slitless Spectrograph instrument (NIRISS) is the Canadian Space Agency contribution to the suite of four science instruments of the James Webb Space Telescope. As one of the three NIRISS observing modes, the Single Object Slitless Spectroscopy (SOSS) mode is tailor-made to undertake time-series observations of exoplanet...

The Near Infrared Imager and Slitless Spectrograph instrument (NIRISS) is the Canadian Space Agency (CSA) contribution to the suite of four science instruments of JWST. As one of the three NIRISS observing modes, the Single Object Slitless Spectroscopy (SOSS) mode is tailor-made to undertake time-series observations of exoplanets to perform transit...

The Near-Infrared Imager and Slitless Spectrograph (NIRISS) is the science module of the Canadian-built Fine Guidance Sensor (FGS) onboard the James Webb Space Telescope (JWST). NIRISS has four observing modes: 1) broadband imaging featuring seven of the eight NIRCam broadband filters, 2) wide-field slitless spectroscopy (WFSS) at a resolving power...

We present a spectroscopic redshift catalogue of the SMACS J0723.3−7327 field (‘Webb’s First Deep Field’) obtained from JWST/NIRISS grism spectroscopy and supplemented with JWST/NIRSpec and VLT/MUSE redshifts. The catalogue contains a total of 190 sources with secure spectroscopic redshifts, including 156 NIRISS grism redshifts, 123 of which are fo...

Twenty-six years ago a small committee report, building on earlier studies, expounded a compelling and poetic vision for the future of astronomy, calling for an infrared-optimized space telescope with an aperture of at least $4m$. With the support of their governments in the US, Europe, and Canada, 20,000 people realized that vision as the $6.5m$ J...

This paper characterizes the actual science performance of the James Webb Space Telescope (JWST), as determined from the six month commissioning period. We summarize the performance of the spacecraft, telescope, science instruments, and ground system, with an emphasis on differences from pre-launch expectations. Commissioning has made clear that JW...

The James Webb Space Telescope’s Near Infrared Imager and Slitless Spectrograph (JWST-NIRISS) flies a 7-hole non-redundant mask (NRM), the first such interferometer in space, operating at 3–5 μ m wavelengths, and a bright limit of ≃4 mag in W2. We describe the NIRISS Aperture Masking Interferometry (AMI) mode to help potential observers understand...

We present a spectroscopic redshift catalogue of the SMACS J0723.3$-$7327 field ("Webb's First Deep Field") obtained from JWST/NIRISS grism spectroscopy and supplemented with JWST/NIRSpec and VLT/MUSE redshifts. The catalogue contains a total of 190 sources with secure spectroscopic redshifts, including 156 NIRISS grism redshifts, 123 of which are...

The James Webb Space Telescope's Near Infrared Imager and Slitless Spectrograph (JWST-NIRISS) flies a 7-hole non-redundant mask (NRM), the first such interferometer in space, operating at 3-5 \micron~wavelengths, and a bright limit of $\simeq 4$ magnitudes in W2. We describe the NIRISS Aperture Masking Interferometry (AMI) mode to help potential ob...

This document characterizes the actual science performance of the James Webb Space Telescope (JWST), as known on 12 July 2022. Following six months of commissioning to prepare JWST for science operations, the observatory is now fully capable of achieving the discoveries for which it was built. A key part of commissioning activities was characterizi...

We present the wide field slitless spectroscopy mode of the NIRISS instrument on the James Webb Space Telescope. This mode employs two orthogonal low-resolution (resolving power $\approx 150$) grisms in combination with a set of six blocking filters in the wavelength range 0.8 to $2.3\,\mu$m to provide a spectrum of almost every source across the f...

We present the wide field slitless spectroscopy mode of the NIRISS instrument on the James Webb Space Telescope. This mode employs two orthogonal low-resolution (resolving power ≈150) grisms in combination with a set of six blocking filters in the wavelength range 0.8–2.3 μ m to provide a spectrum of almost every source across the field-of-view. Wh...

1. Abstract The James Webb Space Telescope (JWST) extreme sensitivity, as well as its optical performance, requires that beam clipping (vignetting) at the instrument internal pupils and at the Optical Telescope Element (OTE) exit pupil is to be avoided as much as possible. The other concern is related to stray light suppression. The OTE is an open...

NASA’s James Webb Space Telescope (JWST) is a 6.5m diameter, segmented, deployable telescope for cryogenic IR space astronomy. The JWST Observatory includes the Optical Telescope Element (OTE) and the Integrated Science Instrument Module (ISIM), that contains four science instruments (SI) and the Fine Guidance Sensor (FGS). The SIs are mounted to a...

The Integrated Science Instrument Module (ISIM) for the James Webb Space Telescope (JWST) has successfully completed its final cryogenic performance verification tests. The performance of the newly upgraded Fine Guidance Sensor (FGS) / Near Infrared Imager and Slitless Spectrometer (NIRISS) was evaluated in these tests. We describe some of the key...

The James Webb Space Telescope (JWST) is a 6.5 m diameter, passively cooled, deployable telescope that will orbit the Lagrange 2 Earth–Sun point beginning in 2018. NASA is leading the development of the JWST mission with their partners, the European Space Agency and the Canadian Space Agency. The Canadian contribution to the mission is the Fine Gui...

COM DEV's compact Sapphire optical payload is currently providing Space Situational Awareness (SSA) in a dedicated low earth orbit mission to better than 16 th visual magnitude. This Low Earth Orbit (LEO) instrument is sufficient for imaging the vast majority of large Geosynchronous Earth Orbit (GEO) satellites, but misses a significant population...

L'imageur SFSI est un spectromètre imageur couvrant le domaine spectral du proche infrarouge, dans la région allant de 1220 nm à 2420 nm, pour utilisation en télédétection aéroportée. Le capteur a été conçu pour acquérir des données dans toute cette bande avec, simultanément, une haute résolution spectrale (10,4 nm) et une haute résolution spatiale...

The Cosmological Advanced Survey Telescope for Optical and UV Research (CASTOR) is a proposed Canadian Space Agency (CSA) mission that would provide panoramic, high-resolution imaging of 1/8th of the sky in the UV/optical (150-550 nm) spectral region. This small-satellite class mission would provide high angular resolution ultra-deep imaging in thr...

The James Webb Space Telescope Fine Guidance Sensor makes use of three 2048×2048 five micron cutoff H2RG HgCdTe detectors from Teledyne Imaging Systems. The FGS consists of two Guider channels and a Near-InfraRed Imager and Slitless Spectrograph (NIRISS) channel. We report here on detailed tests results from the Guider channels originating in both...

Frequency domain multiplexing (fMux) is an established technique for the readout of transition-edge sensor (TES) bolometers in millimeter-wavelength astrophysical instrumentation. In fMux, the signals from multiple detectors are read out on a single pair of wires reducing the total cryogenic thermal loading as well as the cold component complexity...

The Fine Guidance Sensor (FGS) is one of the four science instruments on the James Webb Space Telescope (JWST). FGS features two modules: an infrared camera dedicated to fine guiding of the observatory and a science camera module, the Near-Infrared Imager and Slitless Spectrograph (NIRISS), covering the wavelength range between 0.7 and 5.0 pm with...

The Fine Guidance Sensor (FGS) is one of the four science instruments on board the James Webb Space Telescope (JWST). FGS features two modules: an infrared camera dedicated to fine guiding of the observatory and a science camera module, the Near-Infrared Imager and Slitless Spectrograph (NIRISS) covering the wavelength range between 0.7 and 5.0 μm...

The flight model Fine Guidance Sensor (FGS) on the James Webb Space Telescope (JWST) has successfully completed its performance verification tests. The FGS cryogenic test is described along with some of the key guider performance results which have been obtained. In particular we describe the noise equivalent angle (NEA) performance as a function o...

The Fine Guidance Sensor (FGS) on the James Webb Space Telescope (JWST) has a science observing capability that was to be provided by a tunable Fabry-Pérot etalon incorporating dielectric coated etalon plates with a small vacuum gap and piezoelectric actuators (PZTs). The JWST etalon was more challenging than our existing ground-based operational s...

The James Webb Space Telescope Fine Guidance Sensor makes use of three 2048x2048 five micron cutoff HAWAII-2RG HgCdTe detectors from Teledyne Imaging Systems. The FGS consists of two Guider channels and a Near-InfraRed Imager and Slitless Spectrograph (NIRISS) channel. We report here on the characterization of the flight detectors at the sub-system...

The scanning capability of a tunable filter represents an attractive option for performing high-contrast imaging through spectral differential imaging (SDI), a speckle-suppression technique widely used by current ground-based high-contrast imaging instruments. The performance of such a tunable filter is illustrated through the Tunable Filter Imager...

The development of the James Webb Space Telescope (JWST) is an international collaboration led by NASA in partnership with the European Space Agency and the Canadian Space Agency (CSA). The Canadian contribution to the mission is the Fine Guidance Sensor (FGS). The FGS-Guider images two fields of view onto two detectors. For testing, Optical Ground...

The Tunable Filter Imager of the James Webb Space Telescope will be based on blocking filters and a tunable Fabry- Perot etalon with an average resolution of about 100. It will operate in two wavelength bands from 1.6 mum to 2.5 mum and from 3.1 mum to 4.9 mum at a cryogenic temperature of about 35K. It will respectively be used to study the First...

The James Webb Space Telescope Fine Guidance Sensor makes use of three 2048×2048 five micron cutoff HAWAII- 2RG HgCdTe detectors from Teledyne Imaging Systems. The FGS consists of two Guider channels and one Tunable Filter Imager (TFI) channel. We report here on our efforts to optimize the performance of the FGS detector sub-system consisting of th...

One of the four science instruments aboard the James Webb Space Telescope (JWST) is the Tunable Filter Imager (TFI) provided as part of the Canadian contribution of the JWST Fine Guidance Sensor. The TFI features a low-order Fabry-Perot etalon which enables imaging spectroscopy at an average resolving power of 100. TFI also includes a coronagraph f...

The 'IMAKA (Imaging from MAuna KeA) instrument is a wide field visible light imager incorporating Ground Layer Adaptive Optics (GLAO) to take maximum advantage of the excellent seeing available at the Canada-France-Hawaii Telescope (CFHT). It requires better than 0.3" image quality simultaneously over a total field of view of approximately one squa...

Frequency multiplexed readout systems for large TES bolometer arrays are in use for ground and balloonbased mm-wavelength telescopes. New digital backend electronics for these systems implement advanced signal processing algorithms on FPGAs. Future satellite instruments will likely use similar technology. We address the challenges of operating FPGA...

The JWST Tunable Filter Imager (TFI) is a sensitive camera that shares the optical bench of the Fine Guidance Sensor (FGS). It provides JWST with the capability of imaging a 2.20 × 2.20 field-of-view through narrow-band filters over a wavelength range of 1.5 - 5.0 mum, with a non-functional region between 2.5 and 3.2 mum. The narrow-band filters ar...

The primary function of the Fine Guidance Sensor (FGS) is to provide continuous pointing information to the Observatory. The FGS will image two separate regions of the JWST field of view onto two independent 2k x 2k infrared focal planes arrays, which will cover a wavelength range of 0.6 to 5 mum. Once in fine guiding, the FGS will provide continuo...

The potential of a return of human presence to the Moon, raises the possibility of significant lunar infrastructure and with it the possibility of astronomical installations which can make use of the lunar surface as a stable platform and take advantage of the lack of atmosphere. Studies have been done in the US and Canada on the feasibility of suc...

The Fine Guidance Sensor (FGS) on the James Webb Space Telescope (JWST) has a science observing capability provided by the Tunable Filter Imager (TFI). The TFI incorporates dielectric coated Fabry-Perot etalon plates with a small vacuum gap. The separation of the plates is controlled by the Etalon Control Electronics (ECE) board, using piezoelectri...

The James Webb Space Telescope (JWST) is a 6.5 m diameter, passively cooled, deployable telescope that will orbit the L2 Earth-Sun point beginning in 2014. The National Aeronautics and Space Administration (NASA) is leading the development of the JWST mission with their partners, the European Space Agency and the Canadian Space Agency. The Canadian...

The Fine Guidance Sensor (FGS) of the James Webb Space Telescope (JWST) features a tunable filter imager (TFI) module covering the wavelength range from 1.5 to 5.0 µm at a resolving power of 100 over a field of view of 2.2'x2.2'. TFI also features a set of occulting spots for coronagraphy and a non-redundant mask for very high contrast imaging appl...

The Flamingos-2 Tandem Tunable filter is a tunable, narrow-band filter, consisting of two Fabry-Perot etalons in series, capable of scanning to any wavelength from 0.95 to 1.35 microns with a spectral resolution of R~800. It is an accessory mode instrument for the near-IR Flamingos-2 imaging-spectrograph designed for the Gemini South 8m Observatory...

The Engineering Test Unit (ETU) of the Fine Guidance Sensor (FGS) for the James Webb Space Telescope (JWST) is currently in fabrication. Extensive modeling of the key FGS-Guider performance parameters has been used throughout the design process and continues to be used to evaluate the expected performance of the as-built instrument. A key parameter...

We present the prototyping results and laboratory characterization of a narrow band Fabry-Perot etalon flight model which is one of the wavelength selecting elements of the Tunable Filter Imager. The latter is a part of the Fine Guidance Sensor which represents the Canadian contribution to NASA's James Webb Space Telescope. The unique design of thi...

The Arctic is a region of rapid climate change with warming temperatures and depleting summer ice which may be exacerbated by transport of soot and other anthropogenic material from mid-latitudes. It is also the source of winter storms delivering cold air to lower latitudes. Currently data is available for these areas from polar orbiting satellites...

The Fine Guidance Sensor (FGS) of the James Webb Space Telescope (JWST) features a tunable filter imager (TFI) module covering the wavelength range from 1.6 to 4.9 mu m at a resolving power of similar to 100 over a field of view of 2.2 ' x2.2 '. TFI also features a set of 4 occulting spots for coronagraphy. A review of the current design and develo...

The Measurement of Aerosol Extinction in the Stratosphere and Troposphere Retrieved by Occultation (MAESTRO) instrument on the SCISAT satellite is a simple, compact spectrophotometer for the measurement of atmospheric extinction, ozone, nitrogen dioxide, and other trace gases in the stratosphere and upper troposphere as part of the Atmospheric Chem...

The Fine Guider Sensor (FGS) of the James Webb Space Telescope (JWST) a tunable filter imager (TFI) with a spectral resolution of ~100 covering the 1.5 to 5 micron wavelength range. A set of 4 reflective Gaussian occulting spots / bars on the pick-off mirror of the instrument along with four apodizing masks located in the pupil wheel enable coronag...

Direct detection of extrasolar Jovian planets is a major scientific motivation for the construction of future extremely large telescopes such as the Thirty Meter Telescope (TMT). Such detection will require dedicated high-contrast AO systems. Since the properties of Jovian planets and their parent stars vary enormously between different populations...

COM DEV Ltd. is building a tandem tunable Fabry-Perot etalon to be mounted inside the Flamingos-2 imaging spectrograph on the Gemini South Telescope. The Flamingos-2 Tandem Tunable Filter has a target spectral resolution of R~800 and a clear aperture of 60 mm, and will be fed by the telescope's Multi-Conjugate Adaptive Optics system. The system is...

(on behalf of the Canadian FGS Team) The James Webb Space Telescope (JWST) is a 6.5 m, passively cooled deployable telescope, which will orbit the L2 earth-sun point beginning in 2013. NASA is leading the development of the Observatory with their partners the European Space Agency and the Canadian Space Agency. The Canadian contribution to the miss...

The technology behind the Tunable Filter Imager (TFI) science instrument on the James Webb Space Telescope (JWST) Fine Guidance Sensor (FGS) was developed by COM DEV Ottawa (formerly EMS Technologies) through the Canadian Space Agency (CSA) Space Technology Development Program (STDP). This paper describes the scientific objectives of the FGS-TFI, a...

We describe the design of the FGS guider for the James Webb telescope, and its integration into the instrument complement of the observatory. The guider is required to provide 5mas guide star positions, updated at 16Hz, and to have at least 95% guide star probability anywhere in the sky, with full redundancy. We describe the performance modelling o...

1] SCISAT-1, also known as the Atmospheric Chemistry Experiment (ACE), is a Canadian satellite mission for remote sensing of the Earth's atmosphere. It was launched into low Earth circular orbit (altitude 650 km, inclination 74°) on 12 Aug. 2003. The primary ACE instrument is a high spectral resolution (0.02 cm À1) Fourier Transform Spectrometer (F...

Tight resource allocations are a driving concern for interplanetary remote sensing instruments. Through ongoing development work on Earth-orbiting sensor instruments EMS Space Science has developed the expertise to build extremely efficient and compact spectrometers for multiple planetary applications. We compare the Superiority of high resolution...

Gravity waves are ubiquitous in the Earth's atmosphere transporting energy and momentum between regions. GWIM is a satellite instrument that will use airglow intensity variations to measure gravity wave parameters. A major interest lies in the correlation of the presence of gravity waves with their sources near the surface or in the lower atmospher...

The James Webb Space Telescope (JWST) Observatory, the follow-on mission to the Hubble Space Telescope and to the Spitzer Space Facility, will yield astounding breakthroughs in the realms of infrared space science. The science instrument suite for this Observatory will consist of a Near-Infrared Camera, a Near-Infrared Spectrograph, a Mid-Infrared...

The science instrumentation for the James Webb Space Telescope (JWST) has concluded its Phase A definition stage. We have developed a concept for the JWST Fine Guidance Sensor (FGS), which will form the Canadian contribution to the mission. As part of the JWST re-plan in early 2003, the FGS design was recast to incorporate a narrow-band (R~100) sci...

The Fine Guider Sensor (FGS) of the James Webb Space Telescope (JWST) features two tunable filter (R~100) modules covering the 1.2-2.4 mum and 2.4-4.8 mum wavelength ranges, respectively. A set of occulting spots/bars mounted on a small slide located at the edge of the 2.3"x 2.3" field of view (FOV) along with apodizing masks located in the filter...

The Canadian contribution to the James Webb Space Telescope (JWST) mission will be the Fine Guidance Sensor (FGS), incorporating a science-observing mode using tunable filters. We describe here the requirements, the opto-mechanical design concept and bread-board test results for the JWST FGS tunable filters. The FGS requires two continuously tunabl...

The James Webb Space Telescope (JWST) Observatory, the follow-on mission to the Hubble Space Telescope and to the Spitzer Space Facility, will yield astounding breakthroughs in the realms of infrared space science. The science instrument suite for this Observatory will consist of a Near-Infrared Camera, a Near-Infrared Spectrograph, a Mid-Infrared...

The Canadian contribution to the James Webb Space Telescope (JWST) mission will be the Fine Guidance Sensor (FGS), incorporating a science-observing mode using tunable filters. We describe here the requirements, the opto-mechanical design concept and bread-board test results for the JWST FGS tunable filters. The FGS requires two continuously tunabl...

Airglow imaging has proven to be a useful technique for measuring gravity wave activity, allowing retrieval of parameters such as the wave amplitude, horizontal wavelength, direction of propagation, phase velocity, and wave period. Mars atmosphere is composed mainly of CO2, with small amounts of N2 and Ar. There is considerable evidence of vertical...

Instrumentation for the Next Generation Space Telescope (NGST) is currently in the Phase A definition stage. We have developed a concept for the NGST Fine Guidance Sensor or FGS. The FGS is a detector array based imager which resides in the NGST focal plane. We report here on tradeoff studies aimed at defining an overall configuration of the FGS wh...

To date there have not been any direct measurements of winds in the Martian atmosphere. Measurements such as these are needed in order to understand the nature of the circulation and the transport of constituents in the atmosphere of this planet. In this paper, a conceptual design for a small visible/near-IR imaging interferometer capable of fulfil...

The increasing use of research and operational airborne hyperspectral imaging systems such as AVIRIS and CASI is establishing the characteristics of an emerging market for imaging spectrometer data. Hyperspectral data are beginning to be used for a wide range of applications in environmental and resource management. The Canadian Space Agency, in cl...

Tunable etalons will be an important component of the NGST NIRCam instrument. NASA recently selected the University of Arizona, Lockheed-Martin NIRCam design for implementation. In addition to broadband imager modules, this design uses two sets of tunable Fabry-Perot etalons to cover the spectral ranges of ˜4.5 microns in separate fields. These fil...

The Waves Michelson Interferometer (WAMI) is designed to provide simultaneous measurements of dynamical and constituent signatures in the upper stratosphere, mesosphere and lower thermosphere. It is being included as part of the Waves Explorer mission (G. Swenson, P.I. being proposed for NASA's MIDEX program. It is a field-widened Michelson interfe...

Knowledge of the dynamics is crucial to understanding the behaviour of planetary atmospheres. One technique which has proved valuable for measurements in the terrestrial atmosphere is the field-widened Michelson interferometer. The Wind Imaging Interferometer (G.G. Shepherd, P.I.) on NASA's Upper Atmosphere Research Satellite successfully applied t...

Passive radiative cooling is desirable for space borne detectors because it is generally cheaper, less massive and power consumptive than cooling by a mechanical refrigerator or expendable cryogens. Our interest is space borne nadir imaging the OH airglow in Q-branch features of the 9->6 band at approximately 1382.3 nm, and the 2->0 band at approxi...

SWIFT is a small (< 85 kg, approximately 0.5 m3, < 100 W) satellite instrument which is designed to accurately measure global horizontal winds and ozone concentrations in the stratosphere. SWIFT is similar to the highly successful WINDII instrument currently operating on the UARS satellite. Both use a field-widened Michelson interferometer set at h...

The Stratospheric Wind Interferometer For Transport studies (SWIFT) is a Canadian satellite instrument designed to measure wind profiles between 20 and 45 km in the stratosphere with an accuracy of about 5 m s^-1. It simultaneously provides co-located ozone density profiles with an accuracy of ~5%. SWIFT is a follow on to the highly succe...

Visible imaging is essential to the main scientific program of the Next Generation Space Telescope. An optimized Visible Imager would provide unprecedented resolution and sensitivity. It would enable detailed studies of the morphology of distant galaxies, star formation, gravitational lensing, and would provide a definitive age for the oldest white...

Proof of concept narrow-band etalon filters have been fabricated and characterized for the SWIFT instrument program. The Stratospheric Wind Interferometer For Transport studies is a limb viewing satellite instrument which is intended to measure stratospheric horizontal wind velocities in the altitude range of 20 to 40 km. In addition to providing t...

Proof of concept narrow-band etalon filters have been fabricated and characterized for the SWIFT instrument program. The Stratospheric Wind Interferometer For Transport studies is a limb viewing satellite instrument which is intended to measure stratospheric horizontal wind velocities in the altitude range of 20 to 40 km. In addition to providing t...

Doppler imaging is the method of measuring winds in the atmosphere by taking images of airglow emissions through a field widened Michelson interferometer. This is the method used by the Wind Imaging Interferometer (WINDII) on UARS, the Upper Atmosphere Research Satellite. Efforts are under way to develop similar instruments for the infrared in orde...

A proof of concept Michelson Interferometer has been fabricated and characterized for the SWIFT instrument program. The Stratospheric Wind Interferometer For Transport Studies is a limb viewing satellite instrument which will measure stratospheric horizontal wind velocities in altitude range of 20 to 50 km with a precision of 5 m/s. In addition to...

The SWIR full spectrum imager is an imaging spectrometer covering the short-wave infrared from 1220 to 2420 nm, which has been developed for remote sensing from an airborne platform. The sensor has been designed to acquire the full spectrum at high spectral resolution and the full image swath at high spatial resolution simultaneously. The instrumen...

The SWIR full spectrum imager (SFSI) is a hyperspectral push-broom imager, acquiring imagery in 120 0.010 micrometers wide bands simultaneously covering the 1.20 micrometers to 2.47 micrometers spectral region. During the first flights of the instrument hyperspectral imagery was acquired over a calcite quarry and a dolomite quarry. Both these miner...

The Stratospheric Wind Interferometer for Transport Studies (SWIFT) is a satellite-born limb-viewing instrument which will be capable of globally measuring horizontal winds at altitudes of between 20 and 40 km with a precision of < 5 m/s, a vertical resolution of 2 km and a horizontal resolution on the order of a hundred km. SWIFT will map stratosp...

We present sub-arcsecond (FWHM <0".7) R, J, H, K, and L′ images of the bright IRAS galaxy VV 114 obtained on the Canada-France-Hawaii Telescope and the NASA Infrared Telescope Facility. These observations have unveiled two very strong infrared (IR) sources (VV 114 East) located ˜15" east of the main optical nucleus (VV 114 West). These two sources,...

We present high resolution images in the photometric bands V, R, I, J, H and K of a remarkable bipolar nebula we named the "Flying Ghost Nebula" (FGN) from both its optical shape and its lack of detection by the IRAS satellite. We interpret these images in term of a central young bright star of intermediate mass surrounded by a circumstellar disk s...

The SWIR full spectrum imager (SFSI) is an imaging spectrometer, covering the short-wave infrared (SWIR) from 1200 to 2400 nm, which has been developed for remote sensing from an airborne platform. The sensor has been designed to acquire the full spectrum at high spectral resolution (10 nm) and the full image swath at high spatial resolution (50 cm...

The electro-optical laboratory at the Canada Centre for Remote Sensing has been developed for the calibration of a variety of sensor types. Presented are techniques for use with pushbroom imagers, both multi-spectral line array sensors and area array imaging spectrometers. These calibrations encompass radiometric, absolute and relative, spectral, a...

A near-infrared (1.0-2.5 micron) camera in use at the Canada-France-Hawaii Telescope and at the Observatoire du Mont Megantic 1.6-m telescope is described. The camera is based on a NICMOS3 256 x 256 HgCdTe array detector. While it is used for broad-band imaging and polarimetry through the standard J, H, and K filters, a distinguishing feature of it...

We present (Ne V) 24.32 micrometer and 3426 A emission-line fluxes for NGC 6302 and NGC 6537. These fluxes along with those of (Ne V) 14.3 micrometer allow us to determine the physical conditions within the highly ionized regions of these nebulae. The electron densities found via the (Ne V) line ratios are similar to those found in studies of the l...

The Montreal Infrared Camera (MONICA) consists of a LN2 cryostat enclosing a NICMOS3 array, re-imaging optics and a filter wheel mechanism containing broad-band and circular variable filters. A polarimetry mode with a warm half wave plate and a cold polarizer/filter combination is also supported. At the CFHT 0.5″ (FWHM) images are routinely obtaine...