ISTP NEWSLETTER Vol 7, No. 1 March, 1997
The ISTP "Observatory" tracks a Sun-Earth Connections Event.
IN THIS ISSUE
Title Author
Editor:
Michael Cassidy
CASSIDY@ISTP1.GSFC.NASA.GOV
Contributing Editors:
Steven Curtis - Science Editor
U5SAC@LEPVAX.GSFC.NASA.GOV
Doug Newlon - Data Distribution Facility
NEWLON@IPDGW1.NASCOM.NASA.GOV
Kevin Mangum - Central Data Handling Facility
MANGUM@ISTP1.GSFC.NASA.GOV
Dr. Mauricio Peredo - Science Planning and Operations Facility
PEREDO@ISTP1.GSFC.NASA.GOV
Dick Schneider - ISTP Project Office
SCHNEIDER@ISTP1.GSFC.NASA.GOV
Jim Willett - NASA Headquarters
WILLETT@USRA.EDU
Key Parameter Cumulative Index search on the Web
William H. Mish
In 'Data Products' off of the ISTP Home Page there is provided a new capability to search the cumulative index of the most recent Key Parameter CD-ROMs (non image and image CDs). Thus one can enter time span, a particular mission (e.g., WI), data type (K0 is the default), descriptor (e.g., SWE), version number and the search will return the files and CD-ROM numbers meeting the search criteria. Use of this tool is well documented on the Page itself and use is straight forward. For direct access, the URL for this page is here
William H. Mish
ISTP Deputy Project Scientist for Data Systems
Code 690.0
Goddard Space Flight Center
Greenbelt, Md. 20771
Email to William Mish
wmish@istp1.gsfc.nasa.gov
Key Parameter Cumulative Index search on the Web
William H. Mish
Introduction
Resident on the CDHF and on both the Level Zero and Key Parameter
CD-ROMs are orbit, spacecraft attitude, despun platform attitude
and spacecraft body spin phase (Level Zero CDs only) daily files
which provide the spacecraft orbital position and attitude of the
spacecraft body and despun platform at one minute resolution, as
well as the spin phase of the spacecraft body. Orbit and
spacecraft attitude are in GCI, GSE and GSM. These files are all
encapsulated as Common Data Format (CDF) files.
I) Addition of EDMLT, Magnetic Latitude and "L" Shell:
It was apparent that the auroral physics being studied by the Polar
spacecraft instruments would benefit by having available, as a
function of the spacecraft position, the Magnetic Local Time
(EDMLT), (which is magnetic longitude in units of hours), Magnetic
Latitude (in units of degrees) and the associated "L" Shell
parameter (in units of Re). These parameters are computed using
the eccentric dipole (ED) and 1995 IGRF 1995 magnetic field model
coefficients (with secular variations included).
The above discussed parameters are now included in the Polar Orbit
CDFs at the standard one minute time resolution of the orbital
position and are available to the Key Parameter Generation Software
in the CDHF via a call to ICSS_COMPUTE_EDMLT. The bottom 3 panels
of Figure 1 show these parameters plotted for a portion of December
17, 1996 from the Polar Definitive CDF.
II) Inclusion of a reference orbit number in the Polar Orbit CDF:
The Polar Orbit CDFs now contain a reference orbit number defined
as follows:
An orbit is defined to start from the ascending node (when the
Polar spacecraft orbit crosses the Earth's equator). The first
fractional orbit before reaching the ascending node is numbered
zero and the subsequent orbits numbers increase monotonically . See
Data Format Control Document, Revision 2, May 1996 p. 3-135 for
instructions on how to access the orbit number from the Orbit CDF.
III) Additions to the despun platform attitude CDF
At the Polar Despun Platform Meeting - 8/1/95 the PI teams with
instruments of the despun platform requested that additional
information be included in the despun platform CDF. (Note that the
presently provided GCI, GSE and GSM pitch, roll and yaw are to be
retained). Requested were: a) The despun platform attitude in GCI,
GSE and GSM (this is the same coordinate system provided for the
attitude of the spacecraft body); b) The despun platform offset angle
from Nadir; c) A despun platform in-lock flag and DPA indicator; and d)
during slewing, the dynamic position of the platform as a function
of time.
The top 3 panels in Figure 1 display the DSP offset angle, DPA
indicator (see description below) and DSP lock status (see description below)
as a function of time for December 17, 1996. Figure
1 is a blow up of hours 17.5 - 22.5 which shows the presence of the
dynamic position of the platform as it slews to various positions.
Note that the lock status is 0 during these slews indicating an
out-of-lock condition. TABLE I below summarizes what these files
contain.
IV) Discussion of the Orbit Precision Metric:
The orbit precision metric (Note: located in the Global data of the
CDF) has been developed by constructing a difference vector between
time-coincident ephemeris positions (e.g., time overlapping
ephemeris positions computed from separate tracking data) to be compared
by measuring the components of this difference
vector in a coordinate system fixed at the position of the
spacecraft in the first ephemeris. Calling the coordinate system
Sx, Sy, Sz, the Sx-axis is coincident with the geocenter radius
vector to the spacecraft and is measured positive in the direction
of the Earth's center. The Sy-axis is perpendicular to Sx in the
plane and direction of the satellite motion. The Sz-axis is
perpendicular to the plane of the motion and completes the right-
handed system.
The "Radial", "along track", and "cross track" items are the Sx,
Sy, and Sz components, respectively, of the difference vector. The
"delta-r" and "delta-v" items are the magnitude of the difference
vector for the position and velocity, respectively. Finally, the
RMS is the standard deviation of the component differences over the
length of the compared ephemeris. Thus the smaller this "error
ellipsoid" is, the better the agreement between tracking observations.
V) DSP Accuracy Indicator
This Indicator specifies whether the despun platform attitude is
statistically good (=0) or bad (=1). The attitude is derived from
a batch of computed attitudes at a fixed offset angle. Thus data
are accumulated until either all the required data are collected or
the offset angle is changed to a new value. A statistically good
attitude from a batch is one in which no more than 1/9 of the
original points were deleted during the least-squares fit process.
VI) The Tsyganenko model
The Tsyganenko model (T89C) (Tsyganenko, N.A.:1989,"A
Magnetospheric Magnetic Field Model with a Warped Tail Current
Sheet", Planetary Space Sci.37,5) using a Kp= 3-,3,3+, is now
available to the Key Parameter Software via an ICSS call (ICSS_TSY)
in the CDHF. And this model can be used to trace magnetic field
lines down to 100 Km altitude. This is the same model that is used
by the ISTP/GGS Science Planning and Operations Facility in support
of science planning.
VII) Auroral Oval Models
The Science Planning and Operations Facility (SPOF) employs various
models of regions of geospace as part of its planning and analysis
functions. One key tool used by the SPOF is the Satellite
Situation Center (SSC) software which contains an integrated set of
models for various regions comprising the Solar-Terrestrial system.
These models were presented at several ISTP Science Working Group
meetings, and are summarized on the Web
In order to carry out its DSP Pointing plan generation functions,
the SPOF uses an auroral oval model that differs from that used in
the SSC. The rationale for using a different model is that DSP
pointing strategies dictate that the SPOF maximize the likelihood
of imaging the entire auroral oval, or selected regions of the
oval. To this end, the Holzworth and Meng model (GRL Sept. 75, vol
2 no. 9 pg. 377) was selected because it includes variations in
oval size and location with magnetic activity. The SPOF products
for DSP pointing thus include an auroral oval computed in corrected
geomagnetic coordinates (using IGRF 1995) where the equatorward
edge of the oval is computed for high geomagnetic activity (Q-index
of 6), while the poleward edge is computed for low activity (Q-
index of 0). This choice of activity levels implies that the
instantaneous auroral oval will likely fall within the oval used
for planning purposes.
The ISTP Sun-Earth Connection Event of Jan 6-11, 1997: First ever tracking
of a solar event from "cradle to grave "
Mauricio Peredo, Nicola Fox and Barbara Thompson
For the first time ever, the satellites of the International Solar
-Terrestrial Physics (ISTP) "Observatory" have tracked a solar eruption all
the way, from a Coronal Mass Ejection (CME) expelled from the Sun, through
interplanetary space, until it hit the Earth's magnetic environment,
causing there violent disturbances and spectacular auroral displays. The
initial expulsion occurred on the Sun on January 6, 1997, and a resulting
magnetic cloud hit the Earth on January 10 (see Figure 1).
The Sun often erupts. It flings out white-hot ionized gas
(actually hotter than white-hot, to where it glows in X-rays) with explosive
violence. Only occasionally is this gas aimed at Earth, however, and it is
even more unusual for scientists to be watching the potentially disruptive
mass ejection (as they were in this case) just as it leaves the Sun. This
made it possible to alert other scientific teams of possible activity they
might observe two to three days later, that being the time normally
required for such ejecta to traverse the 93-million mile void from Sun to
Earth. Thus, while this was not the first , or the largest, event of this
nature to be detected, the ISTP "Observatory" includes a complement of
spacecraft and ground-based missions that allow study of this "space storm"
on a scale never accomplished before.
Initial evidence of the event was reported during an ISTP Science
Workshop at NASA's Goddard Space Flight Center on January 7-9, 1997.
Scientists from the joint NASA-European Space Agency satellite Solar and
Heliospheric Observatory (SOHO) showed evidence that a CME, directed
towards Earth, had been emitted from the Sun (see Figure 2).
Based on
previous observations of such events, they predicted it would arrive at
Earth on January 10. SOHO and NASA's WIND spacecraft in interplanetary
space ( Figure 3) between the Sun and the Earth confirmed the passage of a
magnetic cloud 30 million miles thick and taking about 24 hours to pass
through on its journey through interplanetary space.
As the cloud engulfed
Earth, it's magnetic field and a trailing burst of plasma 30 times denser
than the normal solar wind generated a "One-Two Punch" that compressed the
front of the magnetosphere (the magnetic bubble that shields Earth from the
energetic particles spewed from the Sun) inside geosynchronous orbit (Figure
4) at 6.6 Earth radii (normally it lies about 10 Earth radii away), and
resulted in intense geomagnetic activity (Figure 5). Preliminary estimates
suggest that at the height of the event the electrical power dissipated in
the aurora (both northern and southern hemispheres) was about 1400
Gigawatts, almost double the electrical power generating capacity of the
United States (approximately 700 Gigawatts).
The ISTP science teams are thus trying to assemble the anatomy of
this event, as it evolved from start to finish. This includes its
three-dimensional structure and evolution as it influenced the
magnetosphere. A theoretical effort is also underway to help fill in
observational gaps (Figure 6).
Fortunately, the data covers the event fairly
thoroughly and can readily be used to gauge the ability of theoretical or
numerical models to "predict" the effect of events like this one. The
results will be available to agencies which are interested in directing
technical investigations regarding possible reported effects on
communications systems and geosynchronous spacecraft.
An event home page has been setup on the world wide web to
disseminate information on the event and to provide access to the available
data. The event page is accessible
Annoucement of ISTP Science Workshop on the Jan 6-11, 1997 (and similar) magnetic cloud events.
Mauricio Peredo
From: Mauricio Peredo, ISTP Science Planning and Operations Facility
Dear Colleagues:
As you all probably know, the CME-Magnetic Cloud Event of January
6-11, 1997 has attracted a large amount of attention both in the scientific
community and the media. As a result, a number of analyses are underway on
various aspects of this event. In order to promote correlative studies in
the spirit of ISTP, and maximize the scientific return of these
investigations, the ISTP project is planning a workshop to foster joint
analyses of this and similar events.
We plan to hold the workshop at Goddard Space Flight Center on
April 8-9, 1997. The key objective of the workshop is to focus ongoing
analyses towards papers to be presented at the special event session at the
Spring 97 AGU, and later on for the proposed special issue of GRL.
The current plan calls for a "hands-on" workshop with online access
to event data. A detailed plan will depend on the anticipated number of
participants. All members of the international solar, interplanetary,
magnetospheric and ionospheric physics communities are invited to attend.
Therefore we request that you let us know by March 21 if you plan to attend
(please indicate your nationality if you are not a U.S. citizen so we may
arrange for access badges with the security office). Please address
responses to one of the event coordinators at the e-mail addresses listed
below.
Background information on the event, and access to a large volume of
existing event data is available from the event web site
It must be noted that this event is also an important period for the
InterAgency Consultative Group (IACG) since it occurred during the
designated time interval for the IACG Campaigns 1 and 3. In addition, there
will be an "ESLAB" Symposium titled: "Correlated Phenomena at the Sun, in
the Heliosphere and in Geospace". This symposuium has been organized by ESA
endorsed by the IACG and will be held at ESTEC, Noordwijk, on 22-25
September 1997. The symposium will provide an important forum for
discussing the IACG Campaign results coming from the CME-Magnetic Cloud event.
Special sessions or presentations on the event are also planned during the
GEM, CEDAR and IAGA meetings later this year.
[Newsletter TOC]
The IACG Selects New Initiatives for Space Coordination
The 16th Inter-Agency Consultative Group (IACG) meeting was
held from December 10-11, 1996, at Cape Canaveral, Florida. The IACG
is made up of the science heads from ESA (Dr. R. Bonnet), IKI (Dr. A.
Galeev), ISAS (Dr. Nishida), and NASA (Dr. W. Huntress). The role of
the IACG is to facilitate the coordination between the bot
IACG space
physics missions, to acquire the data necessary to meet new science
objectives, and to promote correlative data analysis to get more quality
science out of each individual agency's missions.
In order to focus their correlative data analysis efforts, each of
the agency's core missions are participating in well defined scientific
campaigns. Four campaigns have so far been defined. The IACG has
utilized three working groups in order to plan and conduct the science
campaigns. Working Group-1 is the Science Working Group (chaired
by A. Pedersen, ESTEC) and is chartered with the planning of
coordinated science campaigns concentrating primarily on the Geotail,
Interball, Wind, Polar, and SOHO missions (referred to as the IACG
core missions). Working Group-2 (chaired by J. Green, NASA GSFC)
has facilitated data exchange between the agency missions and
scientists. Working Group-3 (chaired by K. Uesugi, ISAS) has
performed the necessary satellite orbit or orbital analysis for each of the
science campaigns. For more information about the efforts of these
working groups and the resulting campaigns please see the URL:
OR
Update on the Campaigns
A key part of this IACG meeting was to provide the agency heads
with an update on the status of the campaigns. The First IACG
Campaign is designed to study the Earth's magnetotail energy flow and
the role of non-linear dynamics. The lead coordinator for Campaign 1
is Dr. J. Green. Dr. Green gave an update on Campaign 1 which has
been very successful, benefiting from spacecraft (Wind, Geotail,
Interball and Polar in particular) in interesting locations throughout
the magnetosphere. In addition to the IACG web site, data from
selected intervals have been put on CD ROM and are available from
the ISTP Project and at the National Space Science Data Center. Dr.
Green also announced that Phase 2 of Campaign 1 was well underway
and that the important science interval chosen extended from October
1, 1996 through the end of February 1997.
The Second IACG Campaign deals with boundaries in collisionless
plasmas and is co-chaired by Dr. R. Schmidt. Dr. Schmidt gave an
overview of the Cluster situation as Cluster was a major element of
Campaign 2. Because the Cluster mission was aborted after launched
no correlative data activities are planned at this time. At the time of
the IACG meeting, a decision on a full reflight of Cluster was pending
from the ESA Science Programme Committee. At this time (early
March, 1997), no decision has been made to fly the entire mission;
however, the remaining Cluster single space spacecraft, called Phoenix,
will be launched at the end of 1997 or early 1998.
The Third IACG Campaign covers solar events and their
manifestations in interplanetary space and in geospace. Campaign 3 has
the ambitious aim of identifying a CME on the Sun and observing its
effect in geospace. A coronal mass ejection and magnetic cloud (CME-
MC) occurred on January 6-11, 1997 and has attracted a large amount of
attention both in the scientific community and the media. This CME-
MC event is an important period for the Inter-Agency Consultative
Group (IACG) since it occurred during the designated time interval for
the IACG Campaigns 1 and 3. In addition, there will be an ESLAB
Symposium titled: "Correlated Phenomena at the Sun, in the
Heliosphere and in Geospace". This symposium has been organized by
ESA endorsed by the IACG and will be held at ESTEC, Noordwijk, on
September 22-25, 1997. The symposium will provide an important
forum for discussing the IACG Campaign results coming from the
CME-MC event.
Reshaping Future Space Science Coordination
The IACG created a new working group structure to carry out its
current and future space science coordination activities. The re-
structured working groups and panels are:
Whether to continue the VLBI Panel will be decided after it
reports to the IACG at the next meeting. IKI will host the next IACG
meeting later in 1997. The new WG-1 activities will be defined by a
team (with one member from each agency) which will report at the
next IACG meeting. Future solar and planetary missions are to be
included in the new WG-1. The new Solar Terrestrial-Heliospheric
Working Group will have much the same membership as from the
previous Working Groups-1, -2 and -3, replacing the structure that the
IACG created ten years ago. This new WG-2 will ensure that the
present IACG space science campaigns will be brought to a successful
completion and that campaign results will be preserved in data bases
available to a wide science community and published in peer reviewed
journals such as the Journal of Geophysical Research. Dr. A. Pedersen
will be the head of WG-2 for the next year.
One of the goals of the IACG is to make the Space Science
Campaign data sets available to the entire scientific community for
future research. To be successful in this goal, the new archiving effort
will require support from all the agencies. The IACG, therefore, created
a new Data Archiving Working Group (WG-3) to cover all the space
science disciplines. The membership of this WG and its charter are
currently being defined. The heads of the new WG-1 and WG-3 have
not been named at this time.
The Future of Space Physics Correlative Science
It was clear from this meeting that the interagency solar-
terrestrial physics programs have produced a powerful fleet of missions
that are returning a wealth of new observations of our solar-terrestrial
environment. This international collaborative effort has been carried
out during solar minimum. The next solar maximum will start
approximately at the end of the decade, well within the expected
lifetimes of most of the current solar-terrestrial mission fleet. Thus,
this fleet can provide a unique and powerful tool for studying the
solar-terrestrial system during the rise to solar maximum and at solar
maximum. This provides an unprecedented opportunity for studying
solar variability and its effects on the heliosphere and geospace
environment. The former Working Groups-1 and -2 recommended to
the IACG that the agencies keep the solar-terrestrial missions in
operation through solar maximum. The IACG agreed with this
recommendation.
Next Meeting
The IKI will host the next IACG meeting in Russia later in 1997.
The Satellite Situation Center is Now Fully "On the Web"
Robert McGuire, Greg Galiardi, Tamara Kovalick, Rich Baldwin,
Carrie Gallap and Mauricio Peredo
Although available as a beta version for some time to those who have
known or those who have looked, the Satellite Situation Center (SSC)
software and database are now fully converted to a Web interface
(hence SSCWeb) and rehosted on a much faster server. Try the (new)
URL
The SSC system includes a database of >40 missions maintained with the
latest definitive and predictive ephemerides and supports key facility
operations of the NSSDC's Satellite Situation Center and the ISTP
Science Planning and Operations Facility (SPOF) with the same database
and software available to all users.
SSCWeb supports output of spacecraft locations in many different
coordinate systems and with various field parameters and geophysical
regions as desired. The software can also list various kinds of
conjunctions including region co-occupancy and radial or magnetic
alignments of spacecraft or spacecraft with ground stations. The
interface operates in two modes (standard and advanced) to support
both new or occasional users along with users needing to tap more
complex capabilities of the codes. The Web interface features an
innovative use of "hidden fields" to allow users to save and restore
query specifications on their local machines without the need for the
server to track their individual "sessions." Look for WWW conversion
and expanded capabilities of the older SSC's X/PEX-based graphics
shortly, to supplement the powerful listing and logical query
capabilities of this system.
The SSC and SSCWeb are a joint effort of the NASA GSFC Space Physics
Data Facility (software definition, design and development, plus
overall management), the National Space Science Data Center (the SSC
operations staff) and the ISTP SPOF (shared science leadership of the
effort and the physical server).
DATA FILE UPDATE TOOLS MATRIX
The following
table
list three tools that will be used by operations to make up
dates to the orbit and POLAR despun platform attitude data files. The table
provides descriptions for each update, the associated missions and the
effective update time interval.
Newsletter HTML Author: Michael Cassidy - RMS Technologies, Inc.
Figure 1
Image contains Approx 60K bytes
TABLE I
ORBIT CDF S/C ATTITUDE CDF DSP ATTITUDE CDF
-----------------------------------------------------------------
S/C POSITION S/C BODY(RA&DEC) PITCH/ROLL/YAW
GCI GCI GCI
GSE GSE GSE
GSM GSM GSM
EDMLT BODY SPIN RATE DPA ACCURACY
GCI_RA/DEC_ERROR INDICATOR
INV LAT (CDF Global data) ATTITUDE DSP IN
S/C FRAME OF REF
DSP IN-LOCK FLAG
L SHELL NADIR OFFSET ANG
HELIOCENTRIC
S/C VELOCITY
GCI
GSE
GSM
HELIOCENTRIC
HELIOGRAPHIC POSITION OF EARTH
HELIOGRAPHIC POSITION OF THE S/C
GREENWICH HOUR ANGLE
GCI SUN POSITION
CARRINGTON ROTATION #
ORBIT #
(CDF global data
with pointers to the
records where ascending
mode crossings occur)
ORBITAL POSITION
PRECISION METRIC
(CDF global data)
William H. Mish
ISTP Deputy Project Scientist for Data Systems
NASA
Goddard Space Flight Center
Mailstop 694.0
Greenbelt, MD 20771
wmish@istp1.gsfc.nasa.gov
Mauricio Peredo
ISTP Science Planning and Operations Facility
Goddard Space Flight Center
Mailstop 632.0
Greenbelt, MD 20771
peredo@istp1.gsfc.nasa.gov
Figure 1, Image contains Approx 99K bytes
The ISTP "Observatory" tracks a Sun-Earth Connections Event.
Figure 2
Image contains Approx 264K bytes
Observation of the Coronal Mass Ejection leaving the Sun from
the SOHO/LASCO instrument.
Figure 3
Image contains Approx 50K bytes
WIND provides remote-sensing of the radio signals from the event, and later on SOHO and WIND in-situ observations reveal a magnetic cloud is
headed towards Earth.
Figure 4
Image contains Approx 17K bytes
Schematic illustration of the location of geosynchronous
satellites during the event.
Figure 5
Image contains Approx 50K bytes
Auroral activity resulting from magnetospheric compression.
Figure 6
Image contains Approx 83K bytes
A snapshot from the computer simulation of the event showing
the (log) density pattern and volume dominated by the earth's magnetic field.
Barbara J Thompson
ARC
Goddard Space Flight Center
Mailstop 682.0
Greenbelt, MD 20771
thompson@eitv3.nascom.nasa.gov
Nicola J Fox
NRC
Goddard Space Flight Center
Mailstop 696.0
Greenbelt, MD 20771
fox@lepmfs.gsfc.nasa.gov
Mauricio Peredo
ISTP Science Planning and Operations Facility
Goddard Space Flight Center
Mailstop 632.0
Greenbelt, MD 20771
peredo@istp1.gsfc.nasa.gov
To: Members of the Space Science Community
Re: Goddard Workshop on the ISTP Sun-Earth Connections Event of Jan 6-11, 1997
Nicola J Fox
NRC
Goddard Space Flight Center
Mailstop 696.0
Greenbelt, MD 20771
fox@lepmfs.gsfc.nasa.gov
James L Green
NASA
Goddard Space Flight Center
Mailstop 630.0
Greenbelt, MD 20771
green@nssdca.nasa.gov
Mauricio Peredo
ISTP Science Planning and Operations Facility
Goddard Space Flight Center
Mailstop 632.0
Greenbelt, MD 20771
peredo@istp1.gsfc.nasa.gov
Barbara J Thompson
ARC
Goddard Space Flight Center
Mailstop 682.0
Greenbelt, MD 20771
thompson@eitv3.nascom.nasa.gov
James L. Green
New WG-1: Solar System Exploration Working Group
New WG-2: Solar Terrestrial-Heliospheric Working Group
New WG-3: Data Archiving Working Group
Panel 1 : High Energy Astrophysics Panel
Panel 2 : Infrared/submm astronomy Panel
James L Green
NASA
Goddard Space Flight Center
Mailstop 630.0
Greenbelt, MD 20771
green@nssdca.gsfc.nasa.gov"
[Newsletter TOC]
Carrie Gallap
Raytheon STX
Goddard Space Flight Center
Mailstop 632.0
Greenbelt, MD 20771
gallap@rumba.gsfc.nasa.gov
Rich Baldwin
Raytheon STX
Goddard Space Flight Center
Mailstop 632.0
Greenbelt, MD 20771
baldwin@nssdca.gsfc.nasa.gov
Tamara Kovalick
Raytheon STX
Goddard Space Flight Center
Mailstop 633.0
Greenbelt, MD 20771
kovalick@cdi.gsfc.nasa.gov
Greg Galiardi
NASA
Goddard Space Flight Center
Mailstop 632.0
Greenbelt, MD 20771
galiardi@nssdca.gsfc.nasa.gov
Robert McGuire
NASA
Goddard Space Flight Center
Mailstop 632.0
Greenbelt, MD 20771
rmcguire@pop600.gsfc.nasa.gov
Mauricio Peredo
ISTP Science Planning and Operations Facility
Goddard Space Flight Center
Mailstop 632.0
Greenbelt, MD 20771
peredo@istp1.gsfc.nasa.gov
Gerald Blackwell
Gerald Blackwell
CSC
Mailstop 510.0
Goddard Space Flight Center
Greenbelt, MD 20771
gblackwell@istp1.gsfc.nasa.gov
cassidy@istp1.gsfc.nasa.gov
