University%20of%20California,%20Berkeley%20Space%20Sciences%20Lab

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University of California, BerkeleySpace Sciences
Lab

• Established 1958
• Supports science by UCB faculty
• Balloons, rockets, and satellites
• SETI_at_Home

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CHIPSA NASA University ExplorerAstronomy
Mission

• Will Marchant
• UC Berkeley Space Sciences Lab

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CHIPS Program Overview

• PI-Mode Mission awarded in 99 to UCB Space
  Science Lab
• Principle Investigator Dr. Mark Hurwitz
• Management, Systems Eng., Instrumentation,
  Mission Ops at SSL
• Spacecraft Bus provided by SpaceDev, Inc.
• Small 64kg SC carrying a single extreme
  ultraviolet (EUV) Spectrometer
• First University Explorer (UNEX) to make it to
  orbit
• Launched from VAFB on January 12th, 2003
• Secondary Payload on a Delta II Launch Vehicle
• Mission Objectives
• Measure extreme ultraviolet emissions from the
  interstellar medium (90 to 260 Å)
• Test competing theories on the formation of hot
  interstellar gas plasma surrounding our solar
  system.
• Initial science results presented at AAS High
  Energy Astrophysics Division, March 2003.

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Soft X-ray Sky Map (from ROSAT)
Soft X-ray sky map of Snowden et al. Most of the
diffuse local emission is believed to arise in a
hot (106 K) plasma within the nearest 100 pc.
Discrete features include supernova remnants,
etc. The diffuse background brightens generally
near, but not precisely at, the Galactic poles.
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Emission Line Spectrum of 106 K Gas with Local
ISM Attenuation
Emission spectrum of 106 K gas attenuated by
local cloud of 2E18 cm-2. Solar abundance and
collisional ionization equilibrium are assumed.
Brightest lines Fe X 174.6Å, Fe IX 171.1Å, Fe
XI180.4Å, Fe XII 186.9Å
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CHIPS Observational / Science Goals

• Perform spectroscopic sky mapping at EUV
  wavelengths (90 - 260 Å) of diffuse emission from
  hot plasma in the local bubble.
• Characterize properties of the local hot plasma
  (temperature, abundances, ionization state /
  history, density / morphology, etc.).
• Test models of the cooling rate of hot plasma in
  the local bubble, and by inference, elsewhere.

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Spacecraft Bus

• 70 kg
• 3-axis stabilized
• /- 2 attitude
• no propulsion
• survival solar panels
• S-band links
• Full hemisphere RF
• 18 month design

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Spacecraft 1
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Spacecraft 2
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Spacecraft Block Diagram
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Science Instrument Layout
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Science Instrument Layout
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CHIPS Instrument Summary

• Six entrance slits (adjustable closed / wide /
  narrow limited cycles)
• Three pick-off mirrors to coalign fields of view
  in one dimension
• Six identical replica cylindrical VLS
  diffraction gratings
• Master ruled by Hitachi Naka Works
• All substrates, replication by Hyperfine Inc.
• Single MCP detector XDL anode thin-film
  filters
• Filters by Luxel Corp.
• Once-open vacuum box door
• All actuators shape-memory alloy

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CHIPS Diffraction Grating Array
The six credit-card sized diffraction gratings of
the CHIPS spectrograph
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CHIPS Detector Door
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Calibration Image Spectrum Coordinate System
Field of view filled w/ collimated beam sweeps
multiple source spectra coadded
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Field of View
4.5 º
25 º
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CHIPS Performance Overview

• Field of View 5º x 25º no imaging within
  field
• Useful Bandpass 90 260 Å
• FWHM Spectral Resolution
• Narrow Slits 1.4 Å peak 2 Å at bandpass
  edges
• Wide Slits 3.7 Å
• Sensitivity to Key Iron Lines in Sky Survey
  Resel 15º x 25º
• Narrow Slits 26 photons / (cm2 sec ster)
• Wide Slits 12 photons / (cm2 sec ster)

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Satellite During Environmental Testing at KAFB
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Integration with Launch Vehicle
CHIPS integration into DPAF lower cone
CHIPS Enclosed, ICESAT, ? FAIRING
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Launch VAFB 12 January 2003
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Deployment Sequence
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Key Event Time-Line

• Launch 1/12/03
• First Communication with Spacecraft 1/12/03
• SC commanded from Safehold to Nominal Mode
  1/15/03
• SC commanded to Detumble Mode 1/20/03
• SC commanded to Pointing Mode 1/23/03
• CHIPS Instrument powered on 1/24/03
• Vacuum Box Door opened 1/26/03
• Instrument High Voltage turned on 1/29/03
• All Covers opened to wide slits 2/01/03
• 1st Lunar Pointing 2/15/03
• 1st Lunar Calibration 3/17/03
• All Covers moved to narrow slits 4/07/03
• 2nd Lunar Calibration 4/16/03

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Early CHIPS Targets
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Flight Detector Image (wide slits)
He II Lyman ? and ? (256, 243 Å)
Zr/Al
Artifacts
Hot spot removed in ground s/w
Poly/Al
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Preliminary Limits on Raymond Smith Undepleted
Plasma

• Emission measure lt 0.0004 cm-6 pc (95
  confidence) at low / moderate galactic latitudes
• Equivalently, combined strength of iron features
  lt 20 photons / cm2 sec ster (95 confidence)

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How Do We Know CHIPS is Working as Designed?

• Pre-flight calibration of components showed
  fair-to-average efficiencies not unrealistic /
  overly optimistic values
• Pre-flight end-to-end calibration in excellent
  agreement (15) with product of components
  despite months of abuse (repeated vibration
  tests of optical subsytem, etc.)
• Instrument purged with N2 virtually continuously
  after end-to-end calibration. TQCM data show
  negligible contamination during thermal-vacuum
  test.
• On-orbit response to geocoronal He II Lyman
  series consistent with nominal response curve
• On-orbit response to stray He I (in aluminum
  panels) consistent with nominal response curve
• On-orbit response to full moon consistent with
  nominal response curve

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Spectrum of Full Moon 3/18/03 (10,500 s)
(Poly/Al)
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More Recent CHIPS Target on ROSAT 0.1 2 keV NGP
Image
NGP 4
102º
l 90
NPS
l 0
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Mission Operations

• End-to-end use of the Internet
• Early systems integration
• Test the same way youll fly
• Appropriate levels of security

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Description of Ground Segment

• CHIPSat uses the Internet as the backbone for
  carrying telemetry and commands to and from the
  spacecraft
• In addition, the RF link is IP-based
• Ground stations contain a router and Switchbox
  connected to the Internet
• Security provided by VPN to ground stations
• Ground stations
• BGS at UC Berkeley (aka the R-HESSI station)
• ITR at Univ. of S. Australia (aka the Adelaide
  station)
• WFF (Wallops Flight Facility)

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How It Stacks Up
Satellite RF
Ethernet or HDLC
IP
UDP
TCP
Custom Sockets SNTP
FTP
Telnet
Downlink FTP - Stored Science Data FTP - Stored
H/Keeping Data Uplink FTP Stored timed-file
commands
Downlink UDP - Real-Time Science Data UDP -
Real-Time H/Keeping Data Uplink UDP - All
real-time commanding
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Ground Segment / Communications Overview
Berkeley
G/S
SOC
LAN
SpaceDev Router
switch
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MCC client
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VPN
Berkeley
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CHIPSat
MCC server
INTERNET
LAN
VPN
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VPN
2
MCC client
G/S
LAN
SpaceDev Router
3
(e.g.) Adelaide (ITR)
switch
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Satellite Ground Track
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MCC S/C Core Telemetry Page
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MCC ACS Telemetry Page
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MCC S/C Core Telemetry Line Graphs
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Flatsat and Hardware In the Loop (HWIL or HITL
or HWITL) ACS Simulator

• Any new command, script, or software change is
  tested on the s/c flatsat and ACS HWIL simulator
  prior to be sent to CHIPSat
• ACS sensor/actuator simulator provides ability to
  test a variety of environmental scenarios on the
  ACS code
• Flatsat has its own MCC and Router for end-to-end
  testing

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Secure Networking I

• VPN utilizes multiple Internet Protocol Security
  (IPSec) tunnels
• Provides Authentication and Encryption
• As used in corporate transactions
• Only pre-authorized computers have access to s/c
  resources
• MCC Computers are password protected
• Written details of architecture secure
• Implementation can be at any site with a fixed
  IP-address, PC and Windows OS

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Secure Networking II
Features are Ground Segment Wide
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UCB Operations Center
BGS Antenna, Equipment Racks and FOT Workstations
at the UCB Mission Operations Center
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Missions Supported
Mission FAST RHESSI CHIPS
Launch 21 Aug 1996 05 Feb 2002 13 Jan 2003
Duration 2 Years 2 Years 1 Year
Orbit 345x3820 km, 83 565x590 km, 38 575x590 km, 94
BGS Passes 1 / Week 6 / Day 2-4 / Day
Support Type TLM / CMD TLM / CMD TLM / CMD
Max Data Rate 2250.0 kbps 4000.0 kbps 115.2 kbps
Data Volume 20 Gbits / Day 11 Gbits / Day 166.4 Mbits / Day
FAST mission operations transferred from GSFC
to UCB in October 1999. Current Orbit
Geometry. FAST science and engineering data
recovered at Poker Flat, Wallops Island and
McMurdo Base with typically 11 passes / day. BGS
is back-up ground station.
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UCB Operations Center
Dedicated, Secure 600 ft2 MOC Facility at UCB/SSL
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Berkeley Ground Station

• Technical Highlights
• Antenna
• Model 300 Pedestal (L-3 Com, EMP Systems)
• 11-m Parabolic Reflector with Prime Focus Feed
• Three Axis Drive System
• Azimuth / Elevation / Cross-Elevation
• Autotracking with Conical Scan Feed System
• RF Systems
• S-Band Telemetry and Command Capabilities
• Receive Polarization Diversity
• Figure of Merit (G/T) gt 24.0 dB/K at 5 º
  Elevation
• Transmit Power 100 W (63 dBW), LHCP or RHCP
• Data Processing
• Dual CCSDS Frontend Processors
• IP Router for Internet-in-space Communications
• Telemetry Data Routing

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Network Configuration
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NASA Ground Network

• http//www.wff.nasa.gov/code452/
• Primarily government LEO
• Small (8 to 11 meter) dishes

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IT Security

• IT Network Security Plan In Place
• Following NPG 2810.1, NPD 2810.1 and IONet Access
  Protection Policy and Requirements (GSFC 290-004)
  
• Covers FAST and RHESSI Operations
• New Revised Version Includes CHIPS Operations
• Secure Computer Network and T-1 Line to GSFC
• Restriction of Physical Access to MOC
• Cardkey Entry System
• Access to MOC Controlled by U.C. Police
  Department
• Access Restricted to Personnel Essential for
  Flight and Ground Station Operations
• Alarm System Tied into U.C. Police Department
• Video Surveillance Systems Record Activities

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Normal Operations

• Highly Autonomous Operations Planned for CHIPSat
• 4-8 Passes per day
• 2-4 Automated BGS passes per day daytime passes
  staffed during week days
• 2 Automated Wallops passes per day lights-out
  unless command support
• 2 Automated Adelaide passes per day lights-out
  unless command support
• Use Internet-in-space technology
• Stored files downlinked automatically using ftp
• CHIPS batch files are uplinked automatically
  using ftp
• All real-time and stored SOH processed by
  TlmMonitor and RedMonitor
• Limit violations result in email and pages sent
  to FOT
• FOT produces and analyzes spacecraft trend plots
• Mission Operations Manager present during any
  unusual commanding

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Contingency Operations

• Anomalies May be Detected in Real-time or by
  TlmMonitor
• Spacecraft Controller on-shift/on-call evaluates
  severity of anomaly
• Two-way alpha-numeric pager provides information
  on limit violated
• Controller can view recent telemetry on-line
• Controller notifies Mission Operations Manager
• Instrument specialists or spacecraft engineers
  called in as necessary
• Mission Director, PI and Project Managers
  notified in a timely manner
• Anomaly Resolution
• Spacecraft Controllers are trained and authorized
  to respond immediately to anomalies when
  necessary
• With short passes, controllers must be ready to
  safe the spacecraft quickly, before seeking
  outside authorization
• Anytime the spacecraft is not in immediate
  danger, Mission Operations Manager will be
  contacted before proceeding
• New contingency procedures developed and
  implemented with system experts, on an as needed
  basis
• Lessons learned used to update existing
  contingency procedures

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Data Archiving- Telemetry

• Stored on spacecraft until downlinked
• Manual delete after confirmation
• MCC backup on removable optical media
• Permanently stored on command SOC computer
• Permanently stored on data SOC computer
• Daily backup to disk
• Weekly backup to tape
• Weekly off-site backup of tape

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Data Archiving- Science Products

• Daily backup to disk partition
• Weekly backup to tape

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Data Processing- Engineering

• Spacecraft to SOC is fully automated
• S/C ? MCC?cSOC ?dSOC
• Engineering pipeline on dSOC produces
• Limit scans and notifications
• Engineering summaries- text and graphs
• FITS format raw photon lists for further science
  processing

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- Read in basic parameters from file- Load the
Distortion Maps and Detector XY scale ratio-
Read a CHIPS photon-event FITS file in snapshot
format- Use the Stim pulsers to correct the XY
data for thermal drift.- Determine the deadtime
from the Stim pulsers- Determine the exposure
time- Bring the XY data to a common plate
scale- Apply the detector distortion
correction- Rotate the XY pairs to bring a
monochromatic spectral image into the Y
direction- Display a detector image for
convenience- Exclude all events beyond a given
radius near hot spots- Apply time filters-
Apply Pulse Height Thresholds- Extract raw
counts Spectra- Subtract dark counts spectra, if
set- Create fluxed spectra (divide by
effective area, effective field of view, and
exposure time)- Write out spectra in FITS
format coadd as required
Science Data Reduction
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-Read in coadded spectra in FITS format
-Generate backgrounds during characteristic
periods High particle count-rate High scattered
light-Generate model spectra Raymond Smith
plasma emission lines Solar spectrum convolved
with predicted lunar albedo-Fold through
instrument response Wide- or narrow-slit
sensitivity (from preflight calibration) Wide-
or narrow-slit line spectral line profiles (from
raytrace)-Compare models with data
Science Data Analysis
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-Have proposed preliminary archiving plan to MAST
(Myron Smith is point of contact)-Final data
reduction tools still evolving-All instrument
data is available real time on publicly
available web site
Science Data Archiving
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Web Access to CHIPS Data 1
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Web Access to CHIPS Data 2
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• Education Public Outreach
• Receiving Review
• Dr. Nahide Craig E/PO Scientist
• UCB/SSL 22 April 2003

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• Phase E Plans
• Educational Brief for K-14 and Educators
• Exploring the Interstellar Medium
• Dissemination of resources
• Teacher professional Workshops NSTA/AAPT
• Printable PDF Science Journal to use with web
  lesson and activities includes vocabulary and
  questions from lesson
• Summer 2003 _at_UC Berkeley
• Academic Talent Development Program for 8-10
  graders-w/ High School Teacher Collaboration
• Short Course at NSTA 2004 for Educators

• Accomplishments
• CHIPS E/PO website
• http//cse.ssl.berkeley.edu/chips_epo/
• Coordination w/ SEU Education Forum
• CHIPS Lithographs
• The Local Bubble
• What are the ISM and the Local Bubble?
• CHIPS presentation for SEU Ambassadors at
  Sonoma State
• CHIPS Launch
• Collaboration with Science_at_NASA
• Near-Earth Supernovas
• Launch Media Coverage
• CAL Day Open House
• Guided Tours of MOC/SOC
• PI and scientist participation

PI Dr. M. Hurwitz participating in public events
CHIPS Teacher professional development workshop
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CHIPS coverage

• Integration times greater than 150,000 seconds
• Coadded targets within 10
• 20 of celestial sphere

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Observatory Status

• Narrow slits in April 2003
• Wide slits in January 2004
• One short duration HVPS anomaly
• Pulse height filtering software added

• 6 resets (radiation?)
• Spurious Engineering
• Several per week?
• Data storage good
• Several dropped files
• Communications good
• Pointing good
• One reaction wheel showing communications retries
• Power good
• Thermal good
• Lunar pointing good
• Daylight scattering

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IP Protocols

• Mission going well!
• No problems with time synchronization
• Real time data via UDP minor dropouts
• Real time commands via UDP minor drops
• FTP transfers work well 16 MB/day

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Ground Station Network

• Minor issues
• Adelaide, Australia
• RF moved low noise amplifier closer to antenna
• Several antenna tracking problems
• Several power outages
• Berkeley, California
• Several antenna tracking problems
• Several power outages
• Several network outages
• NASA Wallops Flight Facility
• Amplifier
• Manual configuration
• Antenna ran to limits

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Control Center Status

• Several minor issues
• Mission Control Center
• Several network outages
• Science Operations Center
• Several network outages
• Public Server at SSL
• Public server hack
• Configuration control on software installs

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EUVE comet Hyakutake
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CHIPS the future

• CHIPS initial results are puzzling and exciting.
  The Fe line cluster is far fainter than
  expected, and appears dominated by a single,
  surprisingly cool ionization state (Fe IX).
• Make pioneering measurements of three comets in
  the EUV (NEAT C/2001 Q4 and LINEAR C/2002 T7)
  and comet 9P/Tempel 1 that is the subject of
  NASAs Deep Impact mission.
• Carry out a study of He emission from Earths
  plasmasphere.

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Summary / Conclusions

• CHIPS is on orbit and working well
• IP protocols and tools work well
• Adds complexity because of factors not under
  project control wiring, routers, power, etc.
• Reduces costs of special infrastructure
• Increases flexibility
• Preliminary constraints well below the reported
  detection of iron line complex by McCammon et al.
  (Ap.J. 576, 188)
• Tight constraints on strength of iron emission
  line near 170-180 Å
• Canonical sun-centered local hot bubble seems
  ruled out unless abundances and/or ionization
  conditions anomalous
• Observational challenges posed
• Properties of hot gas in the local cavity
• What ionizes the helium and other elements in
  warm interstellar clouds?

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References
CHIPS Science Web Page chips.ssl.berkeley.edu Uni
versity Class Explorers Office www.wff.nasa.gov/pa
ges/code850.html GSFC OMNI Project Ipinspace.gsfc
.nasa.gov