SMEX 8&9 UPDATE

1. SMEX 8&9 UPDATE AWG Meeting October 26, 2000 Paul Hertz

2. SMEX 8&9 Program Scope • Description • Space Science Investigations relevant to: • Astronomical Search for Origins • Structure and Evolution of the Universe • the Sun-Earth Connection • SMEX • Complete investigation: Phase A through Phase E • Total cost to OSS < $75M • Launch by September 2004 • Mission of Opportunity • Participate in non-OSS space mission including ISS • Total cost to OSS < $35M • NASA commitment by sponsoring organization required prior to December 31, 2001 • No restriction on launch date

3. SMEX 8&9 AO Initiatives • Requirement for mission implementation details in proposal reduced --deferred to Phase A • Requirement for detailed E/PO plan deferred to Phase A • Long Duration Balloons added as launch option for SMEX • Contribution limit for SMEX increased to 100% of proposed OSS cost • Spartan 400 offered as GFE spacecraft (fixed cost, to be included in proposed cost) • Technology funding possible only for SMEX Category III proposals • MO cost cap increased from $21M to $35M • MO expanded to include NASA (non-OSS) missions • ISS EXPRESS Pallet offered as a MO option • NASA GSFC services explicitly offered in AO, beginning with Phase A

4. SMEX 8&9 ProgramProposal Statistics • 58 Notices of Intent Received • 46 Proposals submitted • All passed compliance check and were evaluated • Statistics by Theme: • 20 Structure and Evolution of the Universe • 21 Sun-Earth Connection • 5 Astronomical Search for Origins • Statistics by type: • 33 Small Explorers (29 ELV, 3 LDB, 1 Shuttle) • 13 Missions of Opportunity (with 5 proposed for ISS)

5. SMEX 8&9 includes Mission of Opportunity • AO Release: November 15, 1999 • NOI Due: December 16, 1999 • Proposals Due: February 17, 2000 • Evaluations: March-April 2000 • Selection for Study: September 2000 • Downselection for Flight: August 2002 • SMEX 8 launch by: February 2004 • SMEX 9 launch by: February 2005

6. Preproposal Conference December 2 Release AO November 15, 1999 Return Proposal to PI Receive Proposals through 4 pm February 17, 2000 Perform Compliance Check If not compliant, notify Program Scientist Log in Proposals Distribute Proposals to Individual Science Reviewers March 15 Steering Committee Review June 12-13 Individual Science Evaluations March - April Science Pane Review April Categorization May 22-23 Selection Meeting with AA and Science Directors Distribute Proposals to Individual Mini- TMC Reviewers February 21 Individual Mini-TMC Evaluations February - April Mini-TMC Panel Review April Debrief Non-Selectees Post Selection Process Mini-TMC Kickoff March 7 Debrief Non-Selectees Initiate process for any technology funding candidates Contract Award for Phase A Concept Studies October 2001 Downselection Meeting with AA and Science Directors Receive Concept Study Reports April 2002 Final Review Team Meeting Post Downselection Process Initial Review Team Meeting Site Visits Exercise Contract Option for Selected Investigations SMEX 8 & 9 EVALUATION PROCESS (for debriefs)

7. SMEX 8 & 9Downselection Draft Calendar All Dates are Estimates • Concept Study Kickoff Meeting -- August 2001 @ DC area • Concept Study Starts -- October 1, 2001 • Phase A Funding Begins -- August 2002 • Concept Study Reports Due -- April 1, 2002 • Evaluation Period -- April-July 2002 • Site Visits -- June 2002 • (Potential) Science Briefing to AA and Science Directors -- July 2002 • Downselection -- August 2002 • Bridge Phase Begins -- August 2002 • Phase B Funding Begins -- October 2002 • Nominal Launch Dates -- February 2004 and February 2005 Draft 25 September 2000

8. Future Explorer Calendar • MIDEX AO : Summer 2001 • SMEX AO: NET Winter 2002 • UNEX AO: indefinite delay • Technology NRA: under review

9. SMEX Selections MO for Flight: CINDI Roderick Heelis, U. Texas Dallas SEC SMEX for Study: AIM James Russell, Hampton U. SEC HNX Robert Binns, Washington U. SEU JMEX Nicholas Schneider, U. Colorado SEC Joule Richard Kelley, GSFC SEU PRIME Wei Zheng, Johns Hopkins U. ASO STEP Francis Everitt, Stanford U. SEU SPIDR Supriya Chakrabarti, Boston U. SEU MO for Study: SPEAR Jerry Edelstein, U.Cal. Berkeley SEU

10. Aeronomy of Ice in the Mesosphere (AIM) • James Russell, Hampton University • Resolve why Polar Mesospheric Clouds (PMCs) form and why they vary. • Measure PMC abundances, morphology, trends, particle size distributions and gravity waves and by conduct precise, vertical profile measurements of temperature, H2O, OH, CH4, O3, CO2, NO, and aerosols over the altitude range from 10 km to 110 km • Provide the basis for study of long-term mesospheric climate variability and its relationship to global change. • Four instruments: an infrared solar occultation radiometer; a UV interferometer; an in-situ dust detector. • Pegasus rocket will launch the AIM satellite into a 550 km, 12:00 PM sun-synchronous orbit.

11. The Heavy Nuclei Explorer (HNX) • Robert Binns, Washington University • Determine the origin of galactic cosmic rays by measuring the abundances of each individual element from neon through the actinides. • Key questions are the age of the cosmic rays and the roles of volatility and first ionization potential at the cosmic ray source. • Two instruments, ENTICE and ECCO, cover the ranges 10<=Z<=82 and 70<=Z<=100 respectively. • ENTICE is a 4 m2 instrument utilizing silicon solid-state detectors, Cherenkov counters, and scintillating optical fibers. • ECCO utilizes 23 m2 glass track detectors, which require recovery for data analysis. • HNX will be launched as a free-flyer by Space Shuttle and recovered three years later.

12. The Jupiter Magnetospheric Explorer (JMEX) • Nicholas Schneider, University of Colorado • Offer a global study of the Jovian magnetosphere, allowing an in-depth comparison with Earth's magnetosphere. • Earth-orbiting UV telescope with imaging and spectroscopic capabilities optimized for remote sensing of emissions from Jupiter's multiple auroral processes, from Io's atmosphere, and from the plasma torus. • Continuous observations of Jupiter's UV emissions will reveal the nature, variability and interrelation of the underlying Jovian plasma processes. • Comparison of processes at the giant, rotation-dominated magnetosphere of Jupiter with those at Earth extends and tests our understanding of Sun-Earth Connections.

13. Joule • Richard Kelley, NASA’s Goddard Space Flight Center • Address pressing questions on the origin and evolution of large scale structure, life cycles of matter in the universe, and strong gravity close to black holes. • Will recover the lost Astro-E science by flying an imaging spectrometer that has high sensitivity and 10 times better spectral resolution than CCDs. • Incorporates a 32 pixel microcalorimeter array with a demonstrated resolution of 12 eV at 6 keV. • Well suited for extended sources and the iron K band, which compliments the capabilities of Chandra and XMM-Newton. • Mission duration will be at least 2 yr, with all the time allocated via a funded guest observer program; all data will immediately enter the public archives.

14. The Primordial Explorer (PRIME) • Wei Zheng, The Johns Hopkins University • Conduct a deep infrared survey of  steradians in four bands spanning 0.9-3.5 microns. • Find the youngest galaxies and quasars that are observable, thereby establishing the epoch of galaxy formation. • Find hundreds of Type Ia supernovae to z=5, enabling discrimination between competing cosmologies. • Delineate the evolution of clusters of galaxies at 3<z<5. • Find hundreds of brown dwarfs. • Survey will be ~1000 times deeper than 2MASS, and will be the first survey in the waveband between 2.5-3.5 microns. • 75 cm passively cooled (150K) IR telescope, 8-array 1024^2 HgCdTe passively cooled (80K) camera providing PSF of ~1”.

15. Small Explorer mission for Spectroscopy and Photometry of IGM's Diffuse Radiation (SPIDR) • Supriya Chakrabarti, Boston University • Detect, map, and quantify the "cosmic web" of hot intergalactic filaments to answer fundamental questions about the structure and evolution of the universe. • Use measurements of warm/hot (10^5 - 10^7 K) gas to map the "cosmic web". • Foreground observations provide new information about hot gas in a variety of environments, including the Local Bubble, Galactic supernova remnants, the Galactic halo, and nearby galaxies. • Measure the interstellar UV emissions by observing both the molecular ISM through H_2 fluorescence as well as warm/hot gas emission lines such as O VI and C IV.

16. Satellite Test of the Equivalence Principle (STEP) • Francis Everitt, Stanford University • Advance measurement accuracy of the Equivalence Principle by five orders of magnitude. • Laboratory tests confirm the Equivalence Principle to ~5E-13. • Most modern approaches to Grand Unification incorporate alongside gravity very weak scalar fields or moduli that couple to matter in Equivalence-violating ways. • Four separate differential accelerometers with SQUID detectors in a drag-free spacecraft maintained at cryogenic temperatures. • A collaborative NASA-ESA program with well-developed technologies and a well-established US-European team. Development of the payload is NASA-led; ESA supplies the spacecraft service module.

17. Coupled Ion-Neutral Dynamics Investigation (CINDI) • Roderick Heelis, University of Texas at Dallas • Investigate the multi-scale coupling processes between the ion and neutral gases near 400-km altitude. • Furnish two instruments, Ion Velocity Meter and Neutral Wind Meter, to complement the in-situ E, B, Ne (electric and magnetic field and electron density) measurements planned for Air Force C/NOFS satellite. • CINDI+C/NOFS mission will make the first simultaneous measurements of E, U, and Vion in the equatorial F-region, study how neutral winds impact the generation of electric fields and the distribution of plasma in the low-latitude ionosphere, examine how winds and electric fields destabilize the post-sunset ionosphere, and, explain the generation, evolution, and day-to-day variability of equatorial spread-F. • C/NOFS database will become available to the community.

18. The Spectroscopy of Plasma Evolution from Astrophysical Radiation (SPEAR) • Jerry Edelstein, University of California at Berkeley • Trace the balance and flow of energy through the hot interstellar medium. • A diffuse, far-ultraviolet (FUV) spectrometer to fly on the Korean KAISTSAT-4 mission. • Measure the structure, mixing, and cooling of this hot IS plasma in our Galaxy, allowing us to test multi-phase models of the ISM, to examine hot gas interaction in superbubbles, to understand shock interactions between supernovae and the ISM, and to understand plasma phenomena found in galactic fountains and halos, active galaxies, galactic clusters, and possibly the intergalactic medium.