urn:nasa:pds:context:instrument:apxs.msl 1.0 1.7.0.0 Product_Context 2016-10-01 1.0 extracted metadata from PDS3 catalog and modified to comply with PDS4 Information Model urn:nasa:pds:context:instrument_host:spacecraft.msl::1.0 instrument_to_instrument_host Clark, B.C., et al., Evidence for montmorillonite or its compositional equivalent in Columbia Hills, Mars, J. Geophys. Res. 112, E06S01, doi:10.1029/2006JE002756, 2007. reference.CLARKETAL2007 Gellert, R., et al. (2006), Alpha Particle X-Ray Spectrometer (APXS): Results from Gusev crater and calibration report, J. Geophys. Res., 111, E02S05, doi:10.1029/2005JE002555. reference.GELLERTETAL2006 Gellert, R., et al., The Alpha-Particle-X-ray-Spectrometer for the Mars Science Laboratory (MSL) Rover Mission, LPSC XL #2364, 2009. reference.GELLERTETAL2009 Rieder, R., H. Wanke, T. Economou, and A. Turkevich, Determination of the Chemical Composition of Martian Soil and Rocks: The Alpha Proton X Ray Spectrometer, J. Geophys. Res., 102, 4027-4044, 1997. reference.RIEDERETAL1997A Rieder, R., T. Economou, H. Wanke, A. Turkevich, J. Crisp, J. Bruckner, G. Dreibus, H.Y. McSween Jr., The Chemical Composition of Martian Soil and Rocks Returned by the Mobile Alpha Proton X-ray Spectrometer: Preliminary Results from the X-ray Mode, Science, 278, 1771-1774, 1997. reference.RIEDERETAL1997B Rieder, R., et al., The New Athena Alpha Particle X-Ray Spectrometer (APXS) for the Mars Exploration Rovers, Journal of Geophysical Research- Planets, 2003. reference.RIEDERETAL2003 Rieder, R., et al., APXS on Mars: Analyses of soils and rocks at Gusev Crater and Meridiani Planum, LPSC XXXV #2172, 2004. reference.RIEDERETAL2004 ALPHA PARTICLE X-RAY SPECTROMETER Spectrometer not applicable not applicable Instrument Overview =================== The APXS (Alpha-Particle X-ray Spectrometer) for MSL is an improved version of the APXS that flew successfully on Pathfinder and the Mars Exploration Rovers Spirit and Opportunity [RIEDERETAL1997A, RIEDERETAL1997B, RIEDERETAL2003, GELLERETAL2006]. The MSL APXS takes advantage of a combination of the terrestrial standard methods Particle-Induced X-ray Emission (PIXE) and X-ray Fluorescence (XRF) to determine elemental chemistry. It uses curium-244 sources for X-ray spectroscopy to determine the abundance of major elements down to trace elements from sodium to bromine and beyond. The instrument consists of a main electronics unit in the rover's body and a sensor head mounted on the robotic arm. Measurements are taken by deploying the sensor head towards a desired sample, placing the sensor head in contact or hovering typically less than 2 cm away, and measuring the emitted X-ray spectrum for 15 minutes to 3 hours without the need of further interaction by the rover. At the end of the measurement, the rover retrieves the science data of 32 kilobytes, containing up to 13 consecutively taken spectra and engineering data. The internal APXS software splits the total measurement into equal time slots with an adjustable cycle time parameter. This allows us to check for repeatability and to select spectra with sufficient spectral quality. The MSL APXS can activate an internal Peltier cooler for the X-ray detector chip. This results in a sufficient spectral resolution (FWHM) of below 200 eV at 6.4 keV below ~ -5 deg C and best FWHM of < 150 eV below ~ -15 deg C environmental temperature. Compared to the APXS on MER, where the best FWHM was reached at temperatures below ~ -45 deg C, this allows a significantly larger operational time window for APXS analysis. The MSL APXS has approximately 3 times the sensitivity for low Z (atomic number) elements and approximately 6 times for higher Z elements than the MER APXS. A full analysis with detection limits of 100 ppm for Ni and ~ 20 ppm for Br now requires 3 hours, while quick look analysis for major and minor elements at ~ 0.5% abundance, such as Na, Mg, Al, Si, Ca, Fe, or S, can be done in 10 minutes or less. On MER, the elements detected by the APXS in rock and soil samples are typically Na, Mg, Al, Si, P, S, Cl, K, Ca, Ti, Cr, Mn, Fe, Ni, Zn, and Br [RIEDERETAL2004] [GELLERTETAL2006]. Elevated levels of Ge, Ga, Pb, and Rb were found in some of the MER samples [CLARKETAL2007]. The sampled area is about 1.7 cm in diameter when the instrument is in contact with the sample. A standoff results in gradually lower intensity and an increased diameter of the measured spot. Low Z element X-rays stem from the topmost 5 microns of the sample, higher Z elements like Fe are detected from the upper ~50 microns. Sample preparation is not needed; the APXS results average the composition over the sampled area and the oxide abundances measured are renormalized to 100%. However, on MSL, a dust removal tool (brush) is available to remove loose material from a rock surface before making an APXS measurement. The major improvements and changes compared to the MER APXS are: * Improved sensitivity by a factor 3 giving full analysis within ~3 hours * Additional improved sensitivity for high Z elements by increased X-ray source strength * Operable during Martian day by using Peltier cooler for the X-ray detector * Basaltic calibration target mounted on the rover (on the robotic arm azimuth actuator housing), dedicated for the APXS * No alpha channel (no Rutherford Backscattering spectroscopy) * Compressed short duration X-ray spectra ( ~10 seconds ) can be used to steer the arm movement in a 'proximity mode' Principal Investigator ---------------------- The APXS Principal Investigator is Ralf Gellert, University of Guelph, Canada. The MSL APXS is funded by the Canadian Space Agency, with MDA Corporation as prime subcontractor. Funding for the science team comes from CSA, NASA, and the University of Guelph. Scientific Objectives ===================== The main objective of the APXS is to characterize the geological context of the rover surroundings and to investigate the processes that formed the rocks and soils. The high precision and low detection limits, especially for salt forming elements like S, Cl, and Br, allow identification of local anomalies and guided in-situ sample selection for the analytical instruments of MSL. The rover observation tray for processed samples allows the APXS to provide additional characterization of the samples collected and prepared for the analytical instruments, connecting the analytical instrument results with the in-situ samples. MSL sample preparation with the brush allows in-situ APXS investigations of thin alteration rinds or near-surface layers or veins which cannot be collected by the drill for the analytical instruments. Another important aspect of the APXS investigation is to relate the chemical composition of the MSL landing site and the results from the MSL payload to what has been found by the previous landed missions, which used similar X-ray spectroscopy methods. The elemental data can be used to extract normative mineralogy either from scratch or using constraints from the mineralogy provided by CheMin. A newly developed method [CAMPBELLETAL2008] using the backscattered peaks of the primary X-ray radiation allows detection of X-ray invisible compounds like bound water or carbonates, if present in significant amounts ( greater than ~5% by weight). Calibration =========== The APXS was fully calibrated using standard geological samples in the laboratory. An onboard basaltic rock slab, surrounded by a nickel plate, is used periodically to check the performance and calibration of the instrument. The data analysis is theoretically well understood and delivers unambiguous element identification and accuracy on the order of ~10%, mainly limited by microscopic sample heterogeneity (i.e., grain size effects). The APXS data analysis is fast and allows a quick turnaround of results used for tactical rover operations. Operational Considerations ========================== The APXS instrument showed an abnormal behavior on Mars, unseen in the lab during calibration and not seen in any other APXS instrument so far. In some integrations the instrument stopped counting any real x-ray counts in the midst of the data acquisition. If this happens the last sub-spectra don't contain real events, only artificial counts around the lowest detectable energy channel. This behavior, dubbed 'lockup', is currently under investigation. After any powercycle, the effect is gone. To mitigate the loss of scientific data, for longer data acquisitions the integration is therefore split into two integrations with a power cycle in the middle. This is to mitigate the risk that all data is lost if the lockup happens early in a single integration.