FMARS Sponsors	Flashline Mars Arctic Research Station Research Objectives A Proposal For A Mars Analog Microbial Observatory and the Need for Baseline Biodiversity Studies at MDRS, FMARS And Mars-Oz Lead - Shannon Rupert Robles & Edward Martinez Introduction: The National Science Foundation has acknowledged the value of studying microbial ecology, and to that end, has instituted a program of research devoted to the development of microbial observatories. This program was designed to develop a network of sites all working toward the discovery of unique microorganisms and the study of the diversity and ecological processes of microorganisms in various ecosystems. In addition, these microbial observatories each follow an established long-term ecological research (LTER) program, while allowing for additional research specific to the environment of the study. The Mars Desert Research Station (MDRS) in the United States, Flashline Station (FMARS) in Canada, and MARS-OZ in Australia give us the unique opportunity to develop a worldwide microbial observatory, based on ecological principles and using the same research criteria as other established microbial observatories, within the framework of Mars analog environments. However, most established microbial observatories are environment specific and in order to develop a single microbial observatory encompassing all of the Mars Analog Research Stations, we first need to measure the biodiversity at each location. Background: During the 2002 field season at MDRS, a project looking at distribution of microbial communities based on water availability was instituted. We applied the requirements used to assess the long-term distribution patterns of microbial life at established microbial observatories to our study. This work was continued in 2003 by the science teams of Expedition One, and the resulting data represent the equivalent of a four-month intensive field study. Proposed Research: The establishment of a worldwide Mars Analog Microbial Observatory would allow for collaborative biological projects, such as microbial taxonomy and LTER studies, at all sites. However, the locations for MDRS, FMARS and MARS-OZ were selected based on their geological analogous characteristics, and not biological ones. This is understandable, considering our lack of knowledge regarding past and/or present life on Mars. A baseline biodiversity study is needed to give researchers information on biological richness and diversity at the macro-scale level, which can then be applied to processes at the micro-scale level. These baseline surveys include transect monitoring of plant communities and macroinvertebrate identification counts at water sources. These two main biological components of an ecosystem have been established as indicators of total diversity. From these data, biodiversity indices can be calculated to indicate the sameness between ecosystems. We completed these surveys at MDRS in the spring of 2004 and now will complete them at FMARS during the summer 2004 field season. The selection of a site for MARS-OZ will be part of a month long expedition in August 2004 at Arkaroola in the Australia Outback and we will complete these same surveys there. This will give us a measure of diversity for three of the four Mars Analog Research Stations. A Field Methodology Approach Between An Earth-Based Remote Science Team And A Mars-Based Field Crew Leads - Stacy T. Sklar & Shannon Rupert Robles During a Mars mission, astronauts will be communicating their research and observations to scientists back on earth. Remote Science Teams (RST) are currently playing the role of the backroom scientists on earth in support of science teams at Mars analog sites worldwide. The main goal of our project is to discover the best approach to data collection, storage, and analysis from both the Mars crews and the RST by implementing different strategies and methodologies. The Scouting Exploration Methodology Study (SEMS) is the first step into this project. In the study of planetary field exploration, different methodologies will need to be studied, so that both field crews and remote scientists will be able to analyze and collaborate with different datasets. Our definition of planetary also includes asteroids, natural satellites, extreme earth environments, etc. We are exploring one such methodology, the SEMS, during the 2004 field seasons at three of the four Mars analog research stations. The approached used is similar to landing on the surface of another planetary body (going from a global perspective to a regional perspective to a local perspective to a microscopic perspective). When exploring, field scientists should approach their investigations by documenting their sites by going from the largest to the smallest of perspectives. The Scouting Exploration Methodology Study (SEMS) was created by Sklar after a preliminary study during MDRS's Crew 21 and it was further developed by Sklar and Rupert during Crew 25 in order for both field crews and remote scientists to analyze and collaborate with different datasets. For these first field tests (Phase One), non-geologists were used in the field. Phase Two was conducted during the Mobile Agents MDRS Crew 29 rotation using geologists and robotic field support. Phase Three will involve implement of the revised methodology during the FMARS 2004 Field Season and Phase Four will be conducted at MARS-OZ during a joint venture in August by the Mars Society Australia, the Mars Expedition Research Council and the Mars Society Canada called Expedition Two. The goal for the methodology study will be to conduct half of the EVA's using the methodology approach and to further define both geological and biological methodologies within the Scouting Exploration Methodology Study (SEMS) in collaboration with the RST. The difference between Phases Three and Four will be that Four will be conducted using dataloggers, while at FMARS we will focus more on the scientific validity of the methodology. Geophysical Survey Lead - Louise Wynn Devon Island's Haughton meteorite impact crater is a focus of Mars analog research because of its similarity to impact craters on Mars. However, its size (20 km diameter) and age (about 23 million years old) make it difficult for close-up geologic examination in a limited field season; even if could roam around the inside of the crater, we would find backfall from the original impact that has substantially re-filled the crater, as well as erosion of the wall surface. In other meteorite impact craters that have been studied extensively, the materials thrown out of the earth by the impact (the ejecta) are scattered around the outside of the crater in a pattern that reflects, in reverse order, the stratigraphy of the ground where the meteorite fell. Thus the layering that reflects the geologic history of the earth from the Paleozoic Era to the present will be revealed on the surface around the crater. The proposed geophysical survey will determine the radioactivity and mineralogical content of the ejecta from the impact explosion, which information can be extrapolated to infer the properties of the material from as deep into the earth as the hole gouged out by the meteorite (about 1.7 km). In general, the dense mafic and ultramafic rocks from lower in the earth, which fall closer to the rim of the crater, will show relatively high readings on the magnetic susceptibility meter, while the felsic and sedimentary layers from closer to the surface, which are lighter and can be carried farther by the original explosion and wind-sorting, will have lower magnetic readings. Conversely, we may expect higher radioactivity readings from the felsic than from the mafic and ultramafic rocks. The geophysical survey will measure radioactivity and magnetic susceptibility of the surface rocks going out from the rim of the crater at regular intervals in at least two 1-km to 2-km-long survey lines. In addition to taking measurements on site, we will collect samples of rocks with anomalous readings for further lab analysis. Possible results of these surveys: Understanding the mixing and wind-sorting process that carried debris away from the meteorite impact site; --Seeing, by inference, rock types correlated to their depth and age; and --Demonstrating the utility of these geophysical surveys in conducting similar research on Mars, to better understand the geologic history of the Red Planet. Language Learning & Communication in a Multi-lingual Crew Lead - Louise Wynn The international FMARS Crew 9, Summer 2004, is a perfect testing ground for theories of language learning. Some of the questions we will ask: How much will the English language abilities of non-English crewmembers improve in one month of living and working together with English-speaking crewmembers? What kinds of strategies will the native-English and non-native-English speakers on the crew develop to communicate with each other? Lorenz Force Analysis of High Latitude Geomagnetic Environments Lead - Bill Butler, Andrew Palfreyman, & Jason Held The Lorenz force is a force realized with a point charge moving along a wire in a magnetic field, producing a force at right angles to both the current and the magnetic field. Using a high performance ultra-capacitor and coil, the Lorenz forces capable at high latitude will be measured and logged to test specific designs and fields to maximize this force for other applications. This research is sponsored by Space Magnetics, LLC. Details TBD Ground magnetic deviation due to Geomagnetic Storms Lead - Jason Held Geomagnetic storms cause inaccuracies in both satellite (GPS) and magnetic (compass) navigation. In these cases, soldiers and aircraft can be made aware of GPS errors and commonly refer to their standard issue compass for directional control, under the assumption that the Earth's magnetic field and read values of magnetic north, are accurate. Geomagnetic storms occur when radioactive particles (primarily Alpha and Beta) from the Sun slam into the Earth's magnetosphere at high speeds. The magnetic field reacts like a punching bag hit by a boxer-it concaves on the sun-side, causing oscillations in the entire field. Distortions and oscillations of the Earth's magnetic field will naturally affect magnetic navigation, based on the following criteria: Storm Strength. Naturally, the stronger the storm, the greater potential effect can occur. Latitude. Due to the shape of the Earth's magnetic field, space weather effects are more strongly felt closer to magnetic poles than the equator. Typically, the stronger the storm, the lower latitude (N or S) you can be to experience effects. This includes proof of concept geomagnetic storm research and analysis, to determine the validity and relevance of employing magnetometers for tactical detection of geomagnetic storms. Further study will entail development of ruggedized magnetometers for specific employment by various transportation and other government agencies. Objectives: Measure the effect of X and M class geomagnetic storms on Earth's magnetic field at ground level (altitude less than 3000 feet AGL). Identify possible effects of magnetic and electromagnetic compass systems, measured in degrees of deviation, and listed by strength of storms. Identify the changes in near ground level effects due to changes in latitude. Video Documentary Lead - Joan Roche My main project while at FMARS this summer will be to shoot a video documentary about our mission. My long term goal is to edit all this into a 90-minute video that would be presented to the public in the 2005-2006 season of "Les Grands Explorateurs", which is specialized in adventure/tourism movies presented with live commentary by the director of each movie. They have been presenting movies in France, Belgium and Québec for the past 30 years at least and are very well respected. I may also use the video material for shorter documentaries on various TV stations here in Canada, maybe in France, and who know where. "Ground-up" Digital Survey and Localization Lead - Judd Reed Correlating features in digital photos from precisely known locations and triangulate to compute elevations for specific landmarks can be used to interpolate a nice elevation map of the FMARS neighbourhood. The scientific merit here is not to come up with new methods of localization but to use this as a metaphor for the type of work which will be required of an actual mars exploration team. The end project goal is to use this as a possible method of ground-up local Digital Terrain and Elevation Data (DTED) database construction. ExoMars Modelling - Analysis of Hydrothermal Stuctures in Haughton Crater Lead - Ákos Kereszturi Present and future rovers on Mars will analyse locations are important for astrobiology. Based on the results of the last decade a good way to find them is the "follow the water" strategy. It also has been turned out that substantial climate changes took place on Mars in the past so paleoclimate indicators are of high interest too. We have analysed past water related environments on Mars with the Vikings (northern plain), Pathfinder (entry of Ares Vallis), Spirit (Gusev Paleolake), Opportunity (Sinus Mereidiani). Future rovers will probably also analyse water related environments and paleoclimate indicators like the high latitude layered sediments, thick sediments in Valles Marineris, former craterlakes. One of these proposed rovers is the ExoMars planned by ESA. The effective planning of rovers' work in an impact paleolake requires better knowledge on the surface and subsurface structure of large impact craters in the point of view of astrobiology. Based on theoretical calculations 10-20 km sized craters can hold the impact melted subsurface water above freezing point for 10^4-10^6 years depending on starting conditions. Unfortunately subsurface structure of craters in this category are poorly known. The analysis of craters on the Earth together with theoretical models could help to achieve better knowledge. After the impact in the subsurface zone water travels along fault zones formed by the impact. Wider the fault is the most important for subsurface water flow. At impact craters the large characteristic faults are: faults between the blocks of the fall-back breccia (in the impact breccia cavity fillings in Haughton crater) faults below the crater formed by basin rebound (its negative gravity anomaly was observed at Haughton crater) listric faults formed by large wall slumpings (observed at Haughton crater in the form of faulted annulus) For effective analysis of any hydrothermal structures in martian craters it is necessary to find out their characteristic locations and appearance for various sized impact craters. Haughton can serve as good analogy for this. The purpose of my work here is to find out: how would an ExoMars category rover realize these locations what basic characteristics could be observed there I would like to analyse as much locations as possible in and around Haughton crater. The methods are simple visual observations, observations with optical glass, map drawing of the distribution of various observable structures (rock/mineral types, faults, topography, location according to the crater, surface debris cover). The purpose of this is to find out what and how could be realized by an ExoMars category rover based on the structures observed at Haughton crater. ExoMars Modelling, Channel Analysis & EVA Optimization Lead - Ákos Kereszturi Around Haughton crater several channels and valleys can be observed which are resembling to martian valley networks. The basis of the analogy are: weak vegetation at Haughton crater weakly cemented debris low annual precipitation low annual temperature, mostly below freezing point permafrost 1-2 meter below the surface ExoMars modelling: simple analysis of possible targets of the planned ExoMars rover. Purposes: to find out important locations for astrobiology near the perimeter of a 20-25 km sized impact crater with simple geologic analysis to find out the surface signs of important localities Runoff channel analysis. Purposes: to find out connection between channel morphology and lithology, breccia covering. Methods: 1. morphometric analysis; 2. in situ analysis of debris size, shape, etc. EVA Optimization to Mars analog terrain, can be realized during any EVA. Subtopics: To make EVAs compatible realized by different groups/times/locality and improve the real-time documentation. "Do geology during traveling": simple methods for geologic work during traveling by foot and by ATVs. Predicted best traverse: At MDRS we defined some best traverses for desert terrain types. At FMARS the "cold terrain" versions can be tested. The purpose is to find out basic morphological and sedimentary characteristics of these channels. Methods: cross section analysis with morphometry based on photos with known scale structures on them. sedimentary analysis at the lowest part of the valleys based on artificial outcrops. This requires visual observations at least along 2 channels at 4 locations each, and sedimentary analysis at least with 2 channels at 2 locations each. Human Factors Study Lead - Dr Tamarak Czarnik, Mars Society Flight Surgeon This is a continuation of research conducted by the 2003 FMARS crew using WinSCAT, software used also on Space Shuttle and International Space Station flights. WinSCAT is a 15-20 spaceflight Cognitive Assessment Tool for Windows. This is a battery of tests rating performance of memory and concentration, meant to be taken at least twice before the rotation, then several times during the rotation as directed. This data will compliment 2003 FMARS season recordings. The Remote Science Team will also receive results to complete data for their Human Factors continuing experiment
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