Author
Zetocha, PaulAffiliation
Kirtland Air Force BaseIssue Date
2003-10

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Copyright © International Foundation for TelemeteringCollection Information
Proceedings from the International Telemetering Conference are made available by the International Foundation for Telemetering and the University of Arizona Libraries. Visit http://www.telemetry.org/index.php/contact-us if you have questions about items in this collection.Abstract
There is an increasing desire in many organizations, including NASA and the DoD, to use constellations or fleets of autonomous spacecraft working together to accomplish complex mission objectives. At the Air Force Research Laboratory’s (AFRL) Space Vehicles Directorate we are investigating and developing architectures for commanding and controlling a cluster of cooperating satellites. For many space missions, large monolithic satellites are required to meet mission requirements. In many cases this results in costly satellites which are more complex, more susceptible to failure, and which have performance characteristics that are less than optimal due to realistic physical size limitations. Recently various organizations have begun to explore how distributed clusters of cooperating satellites can replace their larger monolithic counterparts resulting in an overall cost reduction, enhanced mission performance, and increased system fault tolerance. Large clusters of satellites flying in formation are required to have some level of on-board autonomy in order to: fly within specified tolerance levels; perform collision avoidance; address fault detection, isolation, and resolution (FDIR); share knowledge; and plan and schedule activities. In addition, from an operations standpoint, commanding and controlling a large cluster of satellites can be very burdensome for ground operators. At AFRL we are addressing these issues by development of an on-board Cluster Management system which will, in essence, provide the capability to treat a cluster of satellites as a single virtual satellite. A systems level approach is being taken, therefore from a ground perspective the ground control station must also be able to treat the cluster as a virtual satellite. [1] This paper will describe our Cluster Management system, which is the intelligent entity that is responsible for making cluster level decisions and which enables the satellite cluster to function as a virtual satellite. The cluster manager functionality can be broken down into the following five areas: • Command and control • Cluster data management • Formation flying • Fault management • On-board Planning This paper will contain a detailed description of the Cluster Manager architecture along with its various modules.Sponsors
International Foundation for TelemeteringISSN
0884-51230074-9079
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Precise radial velocities of giant starsOrtiz, Mauricio; Reffert, Sabine; Trifonov, Trifon; Quirrenbach, Andreas; Mitchell, David S.; Nowak, Grzegorz; Buenzli, Esther; Zimmerman, Neil; Bonnefoy, Mickaël; Skemer, Andy; et al. (EDP SCIENCES S A, 2016-10-28)Context. For over 12 yr, we have carried out a precise radial velocity (RV) survey of a sample of 373 G- and K-giant stars using the Hamilton Echelle Spectrograph at the Lick Observatory. There are, among others, a number of multiple planetary systems in our sample as well as several planetary candidates in stellar binaries. Aims. We aim at detecting and characterizing substellar and stellar companions to the giant star HD 59686 A (HR 2877, HIP 36616). Methods. We obtained high-precision RV measurements of the star HD 59686 A. By fitting a Keplerian model to the periodic changes in the RVs, we can assess the nature of companions in the system. To distinguish between RV variations that are due to non-radial pulsation or stellar spots, we used infrared RVs taken with the CRIRES spectrograph at the Very Large Telescope. Additionally, to characterize the system in more detail, we obtained high-resolution images with LMIRCam at the Large Binocular Telescope. Results. We report the probable discovery of a giant planet with a mass of m(p) sin i = 6.92(-0.24)(+0.18) M-Jup orbiting at a(p) = 1.0860(-0.0007)(+0.0006) aufrom the giant star HD 59686 A. In addition to the planetary signal, we discovered an eccentric (e(B) = 0.729(-0.003)(+0.004)) binary companionwith a mass of m(B) sin i = 0.5296(-0.0008)(+0.0011) M-circle dot orbiting at a close separation from the giant primary with a semi-major axis of a(B) = 13.56(-0.14)(+0.18) au. Conclusions. The existence of the planet HD 59686 Ab in a tight eccentric binary system severely challenges standard giant planet formation theories and requires substantial improvements to such theories in tight binaries. Otherwise, alternative planet formation scenarios such as second-generation planets or dynamical interactions in an early phase of the system's lifetime need to be seriously considered to better understand the origin of this enigmatic planet.
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AN AUTONOMOUS SATELLITE TRACKING STATIONAnderson, Mike; Militch, Peter; Pickens, Hugh; AlliedSignal Technical Services (International Foundation for Telemetering, 1999-10)In 1998, AlliedSignal Technical Services (ATSC) installed three fully autonomous 13-meter satellite tracking systems for the Integrated Program Office of the National Oceanic and Atmospheric Administration (NOAA) at the Command and Data Acquisition Station near Fairbanks, Alaska. These systems track and command NOAA Polar Orbiting Weather Satellites and Defense Meteorological Satellites. Each tracking system operates for extended periods of time with little intervention other than periodic scheduling contacts. Schedule execution initiates equipment configuration, including establishing the RF communications link to the satellite. Station autonomy is achieved through use of a robust scheduler that permits remote users and the System Administrator to request pass activities for any of the supported missions. Spacecraft in the mission set are scheduled for normal operations according to the priority they have been assigned. Once the scheduler resolves conflicts, it builds a human-readable control script that executes all required support activities. Pass adds or deletes generate new schedule scripts and can be performed in seconds. The systems can be configured to support CCSDS and TDM telemetry processing, but the units installed at Fairbanks required only telemetry and command through-put capabilities. Received telemetry data is buffered on disk-storage for immediate, post-pass playback, and also on tape for long-term archiving purposes. The system can autonomously support up to 20 spacecraft with 5 different configuration setups each. L-Band, S-Band and X-Band frequencies are supported.
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Optimizing Ground-based Observations of O2 in Earth AnalogsLópez-Morales, Mercedes; Ben-Ami, Sagi; Gonzalez-Abad, Gonzalo; GarcÃa-MejÃa, Juliana; Dietrich, Jeremy; Szentgyorgyi, Andrew; Univ Arizona, Dept Astron; Univ Arizona, Steward Observ (IOP PUBLISHING LTD, 2019-06-18)We present the result of calculations to optimize the search for molecular oxygen, O-2, in Earth analogs transiting around nearby, low-mass stars using ground-based, high-resolution Doppler shift techniques. We investigate a series of parameters, namely spectral resolution, wavelength coverage of the observations, and sky coordinates and systemic velocity of the exoplanetary systems, to find the values that optimize detectability of O-2. We find that increasing the spectral resolution of observations to R similar to 300,000-400,000 from the typical R similar to 100,000 more than doubles the average depth of O-2 lines in planets with atmospheres similar to Earth's. Resolutions higher than similar to 500,000 do not produce significant gains in the depths of the O-2 lines. We confirm that observations in the O-2 A-band are the most efficient except for M9V host stars, for which observations in the O-2 near-infrared (NIR) band are more efficient. Combining observations in the O-2 A, B, and NIR bands can reduce the number of transits needed to produce a detection of O-2 by about one-third in the case of white noise limited observations. However, that advantage disappears in the presence of typical levels of red noise. Therefore, combining observations in more than one band produces no significant gain versus observing only in the A band, unless red noise can be significantly reduced. Blending between the exoplanet's O-2 lines and telluric O-2 lines is a known problem. We find that problem can be alleviated by increasing the resolution of the observations, and by giving preference to targets near the ecliptic.