[1] The optical microscope onboard the Phoenix spacecraft has returned color images (4 mm pixel −1 ) of soils that were delivered to and held on various substrates. A preliminary taxonomy of Phoenix soil particles, based on color, size, and shape, identifies the following particle types [generic names in brackets]: (1) reddish fines, mostly unresolved, that are spectrally similar to (though slightly darker than) global airborne dust [red fines], (2) silt-to sand-sized brownish grains [brown sand], (3) silt-to sand-sized black grains [black sand], and (4) small amounts of whitish fines, possibly salts [white fines]. Most particles have a saturation magnetization in the range 0.5-2 Am 2 kg −1 as inferred from their interaction with magnetic substrates. The particle size distribution has two distinct peaks below 10 mm (fines) and in the range 20-100 mm (grains), respectively, and is different from that of ripple soils in Gusev crater. In particular medium to large sand grains appear to be absent in Phoenix soils. Most sand grains have subrounded shape with variable texture. A fractured grain (observed on sol 112) reveals evidence of micrometer-sized crystal facets. The brown sand category displays a large diversity in color including shiny, almost colorless particles. Potential source regions for these grains may be the Tharsis volcanoes or Heimdal crater (20 km east of the landing site). The black grains are suggested to belong to a more widespread population of particles with mafic mineralogy. The absence of black/brown composite grains is consistent with different formation pathways and source regions for each grain type. Citation: Goetz, W., et al. (2010), Microscopy analysis of soils at the Phoenix landing site, Mars: Classification of soil particles and description of their optical and magnetic properties,

[1] The Phoenix microscopy station, designed for the study of Martian dust and soil, consists of a sample delivery system, an optical microscope, and an atomic force microscope. The combination of microscopies facilitates the study of features from the millimeter to nanometer scale. Light-emitting diode illumination allows for full color optical imaging of the samples as well as imaging of ultraviolet-induced visible fluorescence. The atomic force microscope uses an array of silicon tips and can operate in both static and dynamic mode.

We are developing a stable and precise spectrograph for the Large Binocular Telescope (LBT) named "iLocater." The instrument comprises three principal components: a cross-dispersed echelle spectrograph that operates in the YJ-bands (0.97-1.30 µm), a fiber-injection acquisition camera system, and a wavelength calibration unit. iLocater will deliver high spectral resolution (R~150,000-240,000) measurements that permit novel studies of stellar and substellar objects in the solar neighborhood including extrasolar planets. Unlike previous planet-finding instruments, which are seeing-limited, iLocater operates at the diffraction limit and uses single mode fibers to eliminate the effects of modal noise entirely. By receiving starlight from two 8.4m diameter telescopes that each use "extreme" adaptive optics (AO), iLocater shows promise to overcome the limitations that prevent existing instruments from generating sub-meter-per-second radial velocity (RV) precision. Although optimized for the characterization of low-mass planets using the Doppler technique, iLocater will also advance areas of research that involve crowded fields, line-blanketing, and weak absorption lines.

[1] The Magnetic Properties Experiment (referred to as iSweep or Caltarget) onboard the Phoenix lander was executed in the arctic region of Mars during the mission's 152 sols lifetime. The iSweep experiment involved periodic multispectral imaging of a series of permanent ring magnets. It was designed to attract airborne magnetic dust particles to certain areas on the iSweeps thereby sorting all settling airborne particles at least to some degree according to their magnetic properties. The dust on the area directly above the strong magnets of the iSweep was found to be brighter than that collected on the precursor Sweep Magnet Experiment onboard the Mars Exploration Rovers near Mars' equator, and also this dust is found to be brighter than both surface soil near the lander and soil in the region surrounding the lander. As most other dust and soils on Mars, the Phoenix dust lacks strong spectral signatures of highly crystalline phases. For the first time, based on the complete calibrated data set of images of the iSweeps, spectra were extracted of the putative dust falling on the magnetically protected areas of the iSweeps. These areas are accessible only for particles with a magnetic susceptibility below 10 −3 . Spectra of this nonmagnetic dust are interpreted as signals from nonmagnetic minerals such as tectosilicates or glasses pigmented by poorly crystalline ferric oxides. Rates of dust settling were determined to be 1.08 mm/sol on the magnets and 0.06 mm/sol for the magnetically protected areas.

Abstract. The Surface Stereo Imager (SSI), a stereoscopic, multispectral camera on the Mars Polar Lander, is described in terms of its capabilities for studying the Martian polar environment. The camera's two eyes, separated by 15.0 cm, provide the camera with range-finding ability. Each eye illuminates half of a single CCD detector with a field of view of 13.8 ø high by 14.3 ø wide and has 12 selectable filters between 440 and 1000 nm. The f/18 optics have a large depth of field, and no focusing mechanism is required; a mechanical shutter is avoided by using the frame transfer capability of the 528 x 512 CCD. The resolving power of the camera, 0.975 mrad/pixel, is the same as the Imager for Mars Pathfinder camera, of which it is nearly an exact copy. Specially designed targets are positioned on the Lander; they provide information on the magnetic properties of windblown dust, and radiometric standards for calibration. Several experiments beyond the requisite color panorama are described in detail: contour mapping of the local terrain, multispectral imaging of interesting features (possibly with ice or frost in shaded spots) to study local mineralogy, and atmospheric imaging to constrain the properties of the haze and clouds. Eight low-transmission filters are included for imaging the Sun directly at multiple wavelengths to give SSI the ability to measure dust opacity and potentially the water vapor content. This paper is intended to document the functionality and calibration of the SSI as flown on the failed lander. IntroductionThe [Boynton et al., this issue]. Operationally, the SSI stereoscopic imagery was designed to maintain a virtual environment needed to create command sequences for the arm and RAC. This range map can be augmented by RAC images in locations inaccessible to SSI, such as underneath the lander. Periodic images of the arm will serve to verify its true location compared to its commanded location. Images taken of the lander deck and solar panels will be valuable as troubleshooting guides when performance of various subsystems degrades.The scientific objectives for SSI fall into several broad categories: geomorphology, mineralogy, and atmospheric studies. Geomorphology, as always, is governed by the choice of landing site. The polar layered terrain affords the rare opportunity to learn the stratigraphic history of this circumpolar geologic unit. Local landforms are likely to show fine-scale layering that is likely to have been depositional in origin, but later modified by strong winds. Unlike the Viking Landers 1 and 2 and Pathfinder sites, few, if any, rocks are expected. Defining the role of ices in the formation of the layers is a prime goal for SSI. To aid in the study of the layers, the camera's multispectral imaging mode will be used. Subtle color differences between layers may indicate a different ice fraction, changes in particle size, or composition changes. We will compare the spectra to those obtained at the distant Pathfinder site to check for variations in the globally distributed d...