CanariCam is the facility mid-infrared (MIR) instrument for the Gran Telescopio Canarias (GTC), a 10.4m
telescope at the Observatorio del Roque de los Muchachos on La Palma. One of the science drivers for CanariCam is the study of active galactic nuclei (AGN). We will exploit the instrument's high sensitivity in imaging,
spectroscopy, and polarimetry modes to answer fundamental questions of AGN and their host galaxies. Dust in
the nucleus of an active galaxy reprocesses the intrinsic radiation of the central engine to emerge in the MIR.
Current work demonstrates that the hot dust immediately associated with the AGN, which blocks direct views of
the AGN from some lines of sight, is confined to small (parsec) scales. Thus, high spatial resolution is essential to
probe the "torus" of unified AGN models separate from the host galaxy. CanariCam provides a 0.08" pixel scale
for Nyquist sampling the diffraction-limited point spread function at 8μm, and narrow (0.2") spectroscopy slits
(with R=120-1300). New observations with the GTC/CanariCam will provide key constraints on the physical
conditions in the clumpy torus, and we will sensitively determine AGN obscuration as a function of nuclear
activity. We will therefore address the fueling process and its relationship to the torus, the interaction with the
host galaxy, and dust chemistry. These data will be essential preparation for the next generation of telescopes
that will observe the distant universe directly to explore galaxy and black hole formation and evolution, and the
GTC/CanariCam system uniquely provides multiple modes to probe AGN.
Mid-infrared polarimetry remains an underexploited technique; where available it is limited in spectral coverage from
the ground, and conspicuously absent from the Spitzer, JWST and Herschel instrument suites. The unique characteristics
of SOFIA afford unprecedented spectral coverage and sensitivity in the mid-infrared waveband. We discuss the
preliminary optical design for a 5-40μm spectro-polarimeter for use on SOFIA, the SOFIA Mid-InfraRed Polarimeter
(SMIRPh). The design furthers the existing 5-40μm imaging and spectroscopic capabilities of SOFIA, and draws on
experience gained through the University of Florida's mid-IR imagers, spectrometer and polarimeter designs of T-ReCS
and CanariCam. We pay special attention to the challenges of obtaining polarimetric materials suitable at both these
wavelengths and cryogenic temperatures. Finally, we (briefly) present an overview of science highlights that could be
performed from a 5-40μm imaging- and spectro-polarimeter on SOFIA. Combined with the synergy between the
possible future far-IR polarimeter, Hale, this instrument would provide the SOFIA community with unique and exciting
science capabilities, leaving a unique scientific legacy.
Mid-infrared polarimetry remains an underexploited technique; where available it is limited in spectral coverage from
the ground, and conspicuously absent from both the Spitzer and JWST instrument suites. The unique characteristics of
SOFIA affords unprecedented spectral coverage and sensitivity in the mid-infrared waveband, offering new vistas in the
exploration of astrophysical objects, including (a) galaxies and AGN, (b) star formation regions and (c) debris disks.
Furthering the existing 5-40μm imaging and spectroscopic capabilities of SOFIA, and the University of Florida's mid-IR
imagers, spectrometer and polarimeter designs of T-ReCS and CanariCam, we present an overview of science highlights
that could be performed from a ~5-40μm imaging- and spectro-polarimeter on SOFIA. A secondary science driver is the
inclusion of low- to moderate- resolution (total flux) spectroscopy at these wavelengths. Such an instrument concept
would plug an unfilled area of both SOFIA and space-based instrumentation, providing SOFIA with unique and exciting
science capabilities.
In 1996, it was proposed to build a near-infrared imager for the 3.8-m UK Infrared Telescope in Hawaii, to exploit the 1024 pixel format detectors that were then becoming available. In order to achieve a fast delivery, the instrument was kept simple and existing designs were reused or modified where possible. UFTI was delivered within 2.5 years of the project start. The instrument is based around a 1k Rockwell Hawaii detector and a LSR Astrocam controller and uses the new Mauna Kea optimized J,H,K filter set along with I and Z broad-band filters and several narrow-band line filters. The instrument is cooled by a CTI cry-cooler, while the mechanisms are operated by cold, internal, Bergelahr stepping motors. On UKIRT it can be coupled to a Fabry-Perot etalon for tunable narrow-band imaging at K, or a waveplate for imaging polarimetry through 1-2.5 μm; the cold analyzer is a Barium Borate Wollaston prism. UFTI was designed to take full advantage of the good image quality delivered by UKIRT on conclusion of the upgrades program, and has a fine scale of 0.09 arcsec/pixel. It is used within the UKIRT observatory environment and was the first instrument integrated into ORAC, the Observatory Reduction and Acquisition Control System. Results obtained during instrument characterization in the lab and over the last 3 years on UKIRT are presented, along with performance figures. UFTI has now been used on UKIRT for several hundred nights, and aspects of instrument performance are discussed.
Science workshops were held throughout the Gemini partnership during the second half of 1997 with the aims of identifying and quantifying the supporting capabilities required to enhance the utility and efficiency of the Gemini 8m telescopes. These workshops, held separately in the US, UK, Canada and South America, ensured representation programs were considered in detail sufficient to understand the requirements for their execution on Gemini as well as for any preparatory observations. The desire for wide-field optical and near-IR imaging was frequently identified with an average of one-half to one night of these survey observations per night of Gemini follow-up. Two other common themes were high angular resolution imaging and rapid response to target-of-opportunity events.
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