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The IBEX-Lo Sensor |
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| Authors: | S A Fuselier P Bochsler D Chornay G Clark G B Crew G Dunn S Ellis T Friedmann H O Funsten A G Ghielmetti J Googins M S Granoff J W Hamilton J Hanley D Heirtzler E Hertzberg D Isaac B King U Knauss H Kucharek F Kudirka S Livi J Lobell S Longworth K Mashburn D J McComas E Möbius A S Moore T E Moore R J Nemanich J Nolin M O’Neal D Piazza L Peterson S E Pope P Rosmarynowski L A Saul J R Scherrer J A Scheer C Schlemm N A Schwadron C Tillier S Turco J Tyler M Vosbury M Wieser P Wurz S Zaffke |
| Institution: | 1. Lockheed Martin Advanced Technology Center, 3251 Hanover St, Palo Alto, CA, 94304, USA 3. Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012, Bern, Switzerland 5. Goddard Space Flight Center, Greenbelt, MD, 20771, USA 2. University of New Hampshire, 39 College Road, Morse Hall, Durham, NH, 03824, USA 13. MIT Kavli Institute for Astrophysics and Space Research, 77 Massachusetts Ave, Cambridge, MA, 02139, USA 4. Southwest Research Institute, 6220 Culebra Rd., San Antonio, TX, 78238, USA 10. Sandia Laboratory, Mail Stop 1415, PO Box 5800, Albuquerque, NM, 87185, USA 9. ISR Division MS B241, Los Alamos National Laboratory, Los Alamos, NM, 87535, USA 8. Montana State University, Bozeman, MT, USA 11. University of Arizona, Tuscon, AZ, USA 7. Applied Physics Laboratory, Johns Hopkins University, 11100 Johns Hopkins Road, Laurel, MD, 20723, USA 12. Boston University, 725 Commonwealth Ave, Boston, MA, 02215, USA 6. Swedish Institute of Space Physics, Box 812, 98128, Kiruna, Sweden |
| Abstract: | The IBEX-Lo sensor covers the low-energy heliospheric neutral atom spectrum from 0.01 to 2 keV. It shares significant energy overlap and an overall design philosophy with the IBEX-Hi sensor. Both sensors are large geometric factor, single pixel cameras that maximize the relatively weak heliospheric neutral signal while effectively eliminating ion, electron, and UV background sources. The IBEX-Lo sensor is divided into four major subsystems. The entrance subsystem includes an annular collimator that collimates neutrals to approximately 7°×7° in three 90° sectors and approximately 3.5°×3.5° in the fourth 90° sector (called the high angular resolution sector). A fraction of the interstellar neutrals and heliospheric neutrals that pass through the collimator are converted to negative ions in the ENA to ion conversion subsystem. The neutrals are converted on a high yield, inert, diamond-like carbon conversion surface. Negative ions from the conversion surface are accelerated into an electrostatic analyzer (ESA), which sets the energy passband for the sensor. Finally, negative ions exit the ESA, are post-accelerated to 16 kV, and then are analyzed in a time-of-flight (TOF) mass spectrometer. This triple-coincidence, TOF subsystem effectively rejects random background while maintaining high detection efficiency for negative ions. Mass analysis distinguishes heliospheric hydrogen from interstellar helium and oxygen. In normal sensor operations, eight energy steps are sampled on a 2-spin per energy step cadence so that the full energy range is covered in 16 spacecraft spins. Each year in the spring and fall, the sensor is operated in a special interstellar oxygen and helium mode during part of the spacecraft spin. In the spring, this mode includes electrostatic shutoff of the low resolution (7°×7°) quadrants of the collimator so that the interstellar neutrals are detected with 3.5°×3.5° angular resolution. These high angular resolution data are combined with star positions determined from a dedicated star sensor to measure the relative flow difference between filtered and unfiltered interstellar oxygen. At the end of 6 months of operation, full sky maps of heliospheric neutral hydrogen from 0.01 to 2 keV in 8 energy steps are accumulated. These data, similar sky maps from IBEX-Hi, and the first observations of interstellar neutral oxygen will answer the four key science questions of the IBEX mission. |
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