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ELECTRONIC NEWSLETTER OF THE EUVE OBSERVATORY
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Vol 5, No. 8 25 Aug 1995 ISSN 1065-3597
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Notes from the Editor
=====================
by Brett A. Stroozas, ISO Manager
Welcome to the electronic newsletter for NASA's Extreme Ultraviolet
Explorer (EUVE) satellite, compiled and published monthly by the
Integrated/Intelligent Science Operations (ISO) group at the Center for
EUV Astrophysics (CEA) at the University of California, Berkeley (UCB).
The contents of this issue of the EUVE electronic newsletter are as
follows:
1. EUVE Science News
1.1 VW Hyi Caught In Outburst As TOO
1.2 EUVE Optical Identification Discovery Announced in IAUC
1.3 Abstracts of *Accepted* EUVE Papers
2. Science Operations News
2.1 Dead Spot Becomes Live Spot
2.2 Public Data Release for 1 Sep 1995
2.3 On-Line Access to EUVE
3. CEA Teams with ARC on BU's TERRIERS Mission
4. EUVE Project to Hire Scientists for Extended Mission
To comment on or make suggestions for the EUVE electronic newsletter,
please send e-mail to ceanews@cea.berkeley.edu (Internet).
The EUVE observatory performed well throughout the month of June,
performing observations of the following guest observer (GO) targets
(alternate name and spectral type information taken from the SIMBAD
or internal CEA databases; "NOIDs" are unidentified objects):
===================================================================
Target Alternate Spectral Observation
Name Name Type GMT Date(s) Notes
===================================================================
EUVE J1706-763 -------- NOID 30 Jun - 1 Jul 1995 ---
1932+1059 -------- NeutSt 30 Jun - 1 Jul 1995 RAP
GR Burster -------- NOID 1 Jul - 1 Jul 1995 ---
PG 1444+407 -------- Star 1 Jul - 2 Jul 1995 ---
Mk 478 RE 1442+352 Sy1 2 Jul - 5 Jul 1995 ---
EUVE J1854-324 -------- NOID 2 Jul - 5 Jul 1995 RAP
EUVE J2115-586 -------- NOID 5 Jul - 5 Jul 1995 ---
EUVE J2301-392 -------- NOID 5 Jul - 5 Jul 1995 ---
EUVE J2114+503 -------- NOID 5 Jul - 5 Jul 1995 ---
EUVE J1856-216 -------- NOID 5 Jul - 5 Jul 1995 ---
0712-68 -------- NeutSt 5 Jul - 5 Jul 1995 RAP
HR 120 HD 2726 F2V 5 Jul - 8 Jul 1995 ---
VW Hyi -------- A0 8 Jul - 15 Jul 1995 TOO
Moon -------- SolSys 15 Jul - 15 Jul 1995 TOO
VW Hyi -------- A0 15 Jul - 18 Jul 1995 TOO
EUVE J2324+458 -------- NOID 18 Jul - 18 Jul 1995 ---
EUVE J2041-368 -------- NOID 18 Jul - 18 Jul 1995 RAP
cmaIH2032-358 -------- AGN 18 Jul - 18 Jul 1995 RAP
TON S180 EUVE J0057-223 Sy1 18 Jul - 24 Jul 1995 ---
RE 2156-543 EUVE J2156-546 DA 24 Jul - 29 Jul 1995 ---
RX J2117.1+3412 -------- PlanNeb 24 Jul - 29 Jul 1995 RAP
RE 2324-544 EUVE J2324-546 DA 29 Jul - 5 Aug 1995 ---
ER Vul HD 200391 G0V+ 29 Jul - 5 Aug 1995 RAP
===================================================================
Key to Notes:
RAP = simultaneous Right Angle Program (RAP) imaging observation
TOO = Target Of Opportunity
1. EUVE Science News
====================
1.1 VW Hyi Caught In Outburst As TOO
------------------------------------
by Dr. Antonella Fruscione, EUVE Scientist
Christopher Mauche (LLNL), John Raymond (CfA), Janet Mattei (AAVSO),
and Jay Holberg (LPL/UA) report the recent observation by EUVE of the
dwarf nova VW Hydri in outburst and the subsequent quiescent period
during the interval 8-18 July 1995.
This pre-approved target-of-opportunity (TOO) EUVE observation began
less than four hours after an alert from the AAVSO (American Association
of Variable Star Observers) that the source had gone into outburst.
The source produced a count rate of about 0.2 cnts/s in the Deep Survey
photometer for approximately the first four hours of the observation and
then rose rapidly to about 4 cnts/s, approximately 12 hours after the
rise of the optical flux. Over the course of the next day, the count
rate declined slowly to its value before the outburst.
In addition to EUVE, the Voyager spacecraft was observing this source
simultaneously, and should produce spectroscopy in the waveband from
912 to 1150 Angstroms to complement the EUV spectroscopy that, for this
for this source, extends from 80 to 350 Angstroms.
Simultaneous optical, far-UV, and EUV measurements are important to
the study of dwarf novae because these bandpasses measure the flux
produced by, respectively, the outer disk, the inner disk, and the
boundary layer between the disk and the surface of the white dwarf.
These measurements place important constraints on the mechanism
responsible for dwarf nova outbursts, which is thought to be an
instability in the thermal state of disk material due to the sharp
increase of the opacity and specific heat of gas due to the partial
ionization of hydrogen at a temperature of about 6,000 degrees.
1.2 EUVE Optical Identification Discovery Announced in IAUC
-----------------------------------------------------------
by Dr. Nahide Craig, EUVE Science Archive Scientist
The following is an EUVE optical identification discovery notice
that has been excepted from IAU Circular 6201, 4 Aug 1995:
EUVE J1429-38.0
N. Craig, University of California at Berkeley, communicates:
"The field of EUVE J1429-38.0 (R.A. = 14h29m24s.0, Decl. = -38d04'05",
equinox 2000.0) was observed as part of the EUVE Optical ID Campaign
on May 21.169 UT at Cerro Tololo InterAmerican Observatory with the
1.5-m telescope (+ CCD GEC10). The proposed optical counterpart of
EUVE J1429-38.0 (R.A. = 14h29m27s, Decl. = -38d04'10", equinox 2000.0)
is a star lying 46" from the reported EUV center and is well within
the source error circle. The estimated apparent magnitude is mv = 12.0.
[This may be NSV 06680 = HV 7408--Ed.] Its optical spectrum clearly
shows the characteristics of a cataclysmic variable spectrum, with the
typical Balmer emission lines, as well as lines of He I, Ca II and strong
He II emission. The continuum increases toward the blue at short
wavelengths and toward the red at long wavelengths, indicating the
presence of a secondary red star. However, the inferred contribution
of the companion is not sufficiently strong to allow absorption lines
to be detected. EUVE J1429-38.0 was detected serendipitously through
the EUVE Right Angle Program (RAP) conducted with the survey (imaging)
scanners. As a result of the long exposures typical of spectrometer
and Deep Survey observations, the RAP program is up to 20 times more
sensitive than the EUVE all-sky survey. The source was detected in the
EUVE Lexan/B band on 1993 Mar. 4 with 0.009 cts/s. A further EUVE RAP
observation of this previously unidentified source was obtained during
1995 Mar. 22-Apr. 4. These later data sets yield a countrate of 0.001
cts/s, indicating that the source is variable in the EUV. Monitoring
photometric and spectroscopic observations is urged. Any detection of
optical outbursts should be reported to the EUVE Associate Project Scientist
R. Oliversen (oliversen@stars.gsfc.nasa.gov) for possible EUVE TOO (target
of opportunity) observations."
1.3 Abstracts of *Accepted* EUVE Papers
---------------------------------------
Included below are abstracts of EUVE-related papers recently *accepted*
for publication. For those papers authored by CEA scientists, the EUVE
publication numbers are indicated. Unless otherwise noted, researchers may
obtain preprints of CEA papers by sending an e-mail request containing the
publication number(s) of interest to pub@cea.berkeley.edu.
Researchers are encouraged to contribute *accepted* EUVE-related abstracts
for inclusion in future editions of this newsletter; abstracts or preprints
will also be posted under the CEA WWW Home Page. Please send all abstracts
or preprints to archive@cea.berkeley.edu.
--------------------------------------------------------------
ESTIMATING THE TOTAL RADIATIVE POWER OUTPUT FROM THE HOT OUTER LAYERS
OF LATE-TYPE STELLAR ATMOSPHERES: HOW MANY LINES ARE REQUIRED?
J.G. Doyle
To appear in Astronomy & Astrophysics.
The total radiative power output from the hot outer layers of six
late-type stars (of different spectral types and luminosity class) is
derived via an emission measure technique. This analysis was based
on observational data from the spectral range 100 A to 3000 A obtained
as a result of three separate satellite missions, i.e. Hubble Space
Telescope, International Ultraviolet Explorer and the Extreme Ultraviolet
Explorer. Solar observational data of active regions, coronal holes,
sunspots, "quiescent" regions and flares were also used. Based on the
derived total power output from all of these different plasma, it is
shown that a linear relationship involving a single transition region
line can be used to provide an accurate estimate of the total power
output as previously shown for the Sun. The derived relationship does
not include losses due to hydrogen, nor the UV continuum which can be
a large contributor, particularly for very active stars.
--------------------------------------------------------------
THE 0.8-DAY ORBIT OF THE PRE-CATACLYSMIC BINARY EUVE J1016-053
J.R. Thorstensen, S. Vennes, and S. Bowyer
To appear in Astrophysical Journal. [CEA publication #664]
The optical counterpart of the new extreme ultraviolet source EUVE
J1016-053 (=RE 1016-053) is known to show intermittent sharp Balmer and
He I emission and traces of an M-dwarf associated with a white dwarf
optical spectrum. We present extensive optical spectroscopy showing
the emission lines vary in velocity and intensity on a period of
0.78929 +/- 0.00003 days. The phase of the emission line strengths
lags that of the velocities by 0.237 +/- 0.013 cycle, consistent with
the quarter-cycle offset expected if emission arises from the side of
the secondary facing the hot white dwarf. EUVE J1016-053 is another
example of an extreme ultraviolet (EUV) illumination-effect binary,
which only recently emerged from a common-envelope phase of binary
evolution. Based on spectroscopic measurements and new BVR photometry,
we find that the M-dwarf secondary's contribution to the combined light
is smaller than previously reported, probably because of the difficulty
of avoiding contamination from a third star 3.2" distant. The velocity
of the weak He II absorption is in antiphase to the emission, suggesting
that it originates in the white dwarf photosphere. The mass function
implied by the emission line motion is f(M) = 0.28 +/- 0.08 M_o.
Assuming the He II absorption does follow the white dwarf, the mass
ratio M_WD / M_dM is 1.8 +/- 0.5, and the gravitational redshift is
45 +/- 14 km/s. The modulation of the emission lines suggests the
inclination i > 40 deg, but plausible masses demand the inclination
be well above this value.
--------------------------------------------------------------
EUVE OBSERVATIONS OF JUPITER DURING THE IMPACT OF COMET SHOEMAKER-LEVY 9
G.R. Gladstone, D.T. Hall, and J.H. Waite Jr.
Science, 268, 1595-1597, 1995. [CEA publication #665]
The Extreme Ultraviolet Explorer (EUVE) satellite conducted extensive
observations of the jovian system before, during, and after the impact of
the fragments of comet Shoemaker-Levy 9 in July 1994. About 2 to 4 hours
after the impacts of several of the larger fragments, the brightness of
the neutral helium (He I) resonance line at 58.4 nanometers temporarily
increased by a factor of about 10. The transient 58.4-nanometer
brightenings are most simply explained by resonant scattering of sunlight
from the widespread high-altitude remnants of the larger impact plumes.
Other possible sources of emission, such as electron impact excitation
of He or radiative recombination of He+, may contribute to the observed
signal.
--------------------------------------------------------------
A LOW-COST, AUTONOMOUS, UNMANNED GROUNDSTATION OPERATIONS CONCEPT AND
NETWORK DESIGN FOR EUVE AND OTHER EARTH-ORBITING SATELLITES
A. Abedini, J. Moriarta, D. Biroscak, L. Losik, and R.F. Malina
To be published in proceedings of the International Telemetering
Conference 1995, 30 October-2 November, 1995, Las Vegas, NV. [CEA
publication #667]
The Extreme Ultraviolet Explorer (EUVE) satellite was designed to
operate with the Tracking and Data Relay Satellite System (TDRSS) and
Deep Space Network (DSN). NASA, the Jet Propulsion Laboratory and the
Center for EUV Astrophysics have been evaluating a commercially available
ground station already used for NASA's Low Earth Orbit (LEO) weather
satellites. This ground station will be used in a network of unattended,
autonomous ground stations for telemetry reception, processing, and routing
of data over a commercial, secure data line. Plans call for EUVE to be
the initial network user. This network will be designed to support many
TDRSS/DSN compatible missions. It will open an era of commercial, low-cost,
autonomous ground station networks. The network will be capable of
supporting current and future NASA scientific missions, and NASA's LEO
and geostationary weather satellites. Additionally, it could support
future, commercial communication satellites in low, and possibly medium,
Earth orbit. The combination of an autonomous ground station and an
autonomous telemetry monitoring system will allow reduction in personnel.
The EUVE Science Operations Center has already reduced console work from
three shifts to one by use of autonomous telemetry monitoring software.
--------------------------------------------------------------
RE-ENGINEERING THE EUVE PAYLOAD OPERATIONS INFORMATION FLOW PROCESS TO
SUPPORT AUTONOMOUS MONITORING OF SPACECRAFT TELEMETRY
F. Kronberg, P. Ringrose, L. Losik, D. Biroscak, and R.F. Malina
To be published in proceedings of the International Telemetering
Conference 1995, Las Vegas, NV, 30 October-2 November, 1995. [CEA
publication #668]
The UC Berkeley Extreme Ultraviolet Explorer (EUVE) Science Operations
Center (ESOC) is developing and implementing knowledge-based software to
automate the monitoring of satellite payload telemetry. Formerly, EUVE
science payload data were received, archived, interpreted, and responded
to during round-the-clock monitoring by human operators. Now, knowledge-based
software will support, augment, and supplement human intervention. In
response to and as a result of this re-engineering project, the creation,
storage, revision, and communication of information (the information flow
process) within the ESOC has been redesigned. We review the information
flow process within the ESOC before, during, and after the re-engineering
of telemetry monitoring. We identify six fundamental challenges we face in
modifying the information flow process. (These modifications are necessary
because of the shift from continuous human monitoring to a knowledge-based
autonomous monitoring system with intermittent human response.) We describe
the innovations we have implemented in the ESOC information systems,
including innovations in each part of the information flow process for
short-term or dynamic information (which changes or updates within a week)
as well as for long-term or static information (which is valid for more
than a week). We discuss our phased approach to these innovations, in which
modifications were made in small increments and the lessons learned at each
step were incorporated into subsequent modifications. We analyze some
mistakes and present lessons learned from our experience.
--------------------------------------------------------------
RE-ENGINEERING EUVE TELEMETRY MONITORING OPERATIONS: A MANAGEMENT
PERSPECTIVE AND LESSONS LEARNED FROM A SUCCESSFUL REAL-WORLD
IMPLEMENTATION
D. Biroscak, L. Losik, and R.F. Malina
To be published in proceedings of the International Telemetering
Conference 1995, Las Vegas, NV, 30 October-2 November, 1995.
[CEA publication #669]
The Extreme Ultraviolet Explorer (EUVE) Science Operations Center at
UC Berkeley was recently successful in implementing an automated monitoring
system that allowed reduced operations staffing from 24 hours per day to
9 hours per day. The payload safety is monitored exclusively by artificial
intelligence (AI) telemetry-processing systems for 16 hours per day. At
launch, the EUVE Science Operations Center was staffed and operated as a
typical satellite control center, receiving real-time and tape recorder
data 24 hours per day. From September 1993 through February 1995, EUVE
science operations were redesigned in a phased, low-cost approach. A key
factor in the implementation was to utilize existing personnel in new roles
through additional training and reorganization. Throughout this period,
EUVE guest observers and science data collection were unaffected by the
transition in science operations. This paper describes the original and
actual implementation plan, staffing phases, and cost savings for this
project. We present the lessons learned in the successful transition from
three-shift to one-shift operations.
--------------------------------------------------------------
2. Science Operations News
==========================
2.1 Dead Spot Becomes Live Spot
-------------------------------
by Anne Miller, EGO Center Technical Writer
Last month's newsletter [V5.7, 19 Jul 1995] reported on plans to reduce
the lower pulse height threshold of the Deep Survey detector from 30 to 20
(engineering units). The first results show that the Deep Survey detector
dead spot has been effectively revived by decreasing the pulse height
threshold. The dead spot at the detector center shows increased efficiency,
due to the electronics passing the smaller pulses from this area of reduced
gain. Tests are being conducted to determine the new efficiency of the dead
spot area. The lower threshold also offsets more gradual gain losses over
the entire detector, an effect seen in all the EUVE detectors, and treated
by the same means.
2.2 Public Data Release for 1 Sep 1995
--------------------------------------
by Dr. Nahide Craig, EUVE Science Archive Scientist
The table below lists the GO observations which become public on 1 Sep
1995. For each entry is given the target name, the approximate exposure
time in kiloseconds, the GMT start and end date(s) for the observation, the
spectral type of the target, and the data identification code. All public
data sets may be ordered from the archive via WWW and electronic or postal
mail (see addresses below). Please be sure to include in your order the
DataID(s) of interest.
The data rights policy for GO observations states that GOs have
proprietary rights to the data for one year from the date (s)he receives
it. It is often the case that long observations are broken up over many
months; e.g., an observation approved for 60 ksec may actually be observed
for 10 ksec one month, 20 ksec the next and 30 ksec three months later. In
such cases the one-year proprietary period begins after the GO is sent the
final piece of the completed observation.
===============================================================
Target ~Exp Observation Date(s) SpT DataID
Name (ksec) Start End
===============================================================
Data Sets Available 1 Sep 1995:
3C 273 100 11 Jun - 15 Jun 1994 QSO go0190
3C 273 54 15 Jun - 17 Jun 1994 QSO go0191
3C 273 28 17 Jun - 18 Jun 1994 QSO go0192
44 Boo 100 02 May - 05 May 1994 GOVnvar go0193
44 Boo 51 05 May - 07 May 1994 GOVnvar go0194
alpha Eri 74 26 Jul - 29 Jul 1994 Be go0195
beta CMa 100 27 Feb - 03 Mar 1994 B1II/III go0196
beta CMa 74 03 Mar - 05 Mar 1994 B1II/III go0197
epsilon CMa 50 08 Mar - 09 Mar 1994 B2Iab go0198
epsilon CMa 50 09 Mar - 11 Mar 1994 B2Iab go0199
HR 4804 58 09 May - 11 May 1994 Be go0200
HZ 43 67 20 May - 23 May 1994 DAw go0201
HZ 43 43 23 May - 24 May 1994 DAw go0202
HZ 43 40 24 May - 26 May 1994 DAw go0203
Jupiter 63 04 Jun - 06 Jun 1994 SolSys go0104
M15/AC211 47 06 Jul - 08 Jul 1994 LMXB go0105
Mueller 1993A 55 09 Jun - 11 Jun 1994 comet go0106
PKS 2155-304 100 11 May - 15 May 1994 BLLac go0207
PKS 2155-304 100 15 May - 19 May 1994 BLLac go0208
PKS 2155-304 54 19 May - 20 May 1994 BLLac go0209
RE 2009-60 100 09 Jul - 13 Jul 1994 DA go0210
RE 2009-60 5 13 Jul - 16 Jul 1994 DA go0211
V1974 CYGNI 79 06 Jun - 09 Jun 1994 nova go0212
Wolf 630 100 30 Jul - 03 Aug 1994 Me3Ve go0213
Wolf 630 100 03 Aug - 07 Aug 1994 Me3Ve go0214
Wolf 630 41 07 Aug - 08 Aug 1994 Me3Ve go0215
===============================================================
2.3 On-Line Access to EUVE
--------------------------
Listed below are the various methods for on-line access to EUVE:
o CEA World Wide Web (WWW)
URL http://www.cea.berkeley.edu/
telnet www.cea.berkeley.edu 200 (for those without a WWW browser)
o anonymous FTP
ftp ftp.cea.berkeley.edu
Name: anonymous
Password: type_your_full_e-mail_address
o anonymous gopher
gopher ftp.cea.berkeley.edu
o EUVE Electronic Newsletters
Past issues -- available via the CEA WWW site
Subscriptions -- mail majordomo@cea.berkeley.edu ("subscribe euvenews")
Post message to all subscribers: mail euvenews@cea.berkeley.edu
o GI Program
Are you interested in finding out about or using EUVE data? Do you
need help in understanding EUVE data sets? Do you need help in using
the available EUVE data analysis software tools? If you answer "yes"
to any of the above, the Guest Investigator (GI) Program at CEA can
help YOU! For further information see the CEA WWW site or contact the
Archive (archive@cea.berkeley.edu).
o Public RAP
The Public Right Angle Program (RAP) is an easy method for researchers
to propose for long-exposure EUVE imaging data. For more information
on the Public RAP and the simple proposal process see the CEA WWW site
or contact the EGO Center (egoinfo@cea.berkeley.edu). Mail all
proposals to euverap@cea.berkeley.edu.
o Contact information for the EUVE Science Archive or GO Center:
Center for EUV Astrophysics
2150 Kittredge St.
Berkeley, CA 94720-5030
Archive EGO Center
510-642-3032 (voice) 510-643-8727 (voice)
510-643-5660 (fax) 510-643-5660 (fax)
archive@cea.berkeley.edu egoinfo@cea.berkeley.edu
3. CEA Teams with ARC on BU's TERRIERS Mission
==============================================
by Tom Morgan, EUVE Test-Bed Manager
The Information Systems Development and Test-Bed groups at CEA have
teamed with Code IC (Computational Sciences) at Ames Research Center (ARC)
to provide assistance to Boston University (BU) on the construction of
the Payload Operations Control Center (POCC) software for their TERRIERS
project.
BU was awarded one of two University Space Research Association
Student Explorer Demonstration Initiatives programs for the 1994 pilot
program round. TERRIERS is a 239 lb. spacecraft that will perform
tomographic experiments of the earth's upper atmosphere using recombinative
ionospheric extreme ultraviolet and radio sources.
TERRIERS is scheduled to launch in early 1997 on an Orbital Sciences
Corporation Pegasus XL rocket. The mission consists of a compact spin
stabilized spacecraft in a sun-synchronous 9am/9pm orbit. A ground
station located in Herndon, Virginia, will have two passes 90 min apart,
10-20 min each, every 12 hours, roughly at 9am and 9pm local time.
AeroAstro is the prime contractor for both the spacecraft and the ground
station. BU is responsible for instrument construction and integration,
as well as instrument scheduling and data processing.
CEA and ARC have been working in cooperation to design the software
to meet the TERRIERS POCC requirements. CEA is calling upon its history
in maintenance and design of POCC software and ARC is relying on its long
history with Artificial Intelligence, network design, and security issues.
CEA maintains an in-depth working knowledge of the EUVE end-to-end system
and architecture, the basic philosophy and structure of which are being
applied to the TERRIERS mission. The CEA/ARC team provides TERRIERS with
a unique combination of both innovation and experience.
4. EUVE Project to Hire Scientists for Extended Mission
=======================================================
by Cathie Jones, CEA Personnel Manager
CEA is in the process of advertising new positions for scientists on
the EUVE project at UCB. Positions are for one year, with the likelihood
of renewal for an additional year, and are 50% service work (either assisting
guest observers or working on the EUVE Operations Innovation Test-Bed) and
50% independent research. Interested scientists should check the AAS job
register or contact Ms. Cathy Jones (cjones@cea.berkeley.edu) for more
information.
---------------------------------------------------------------------------
The EUVE Electronic Newsletter is issued by the Center for Extreme
Ultraviolet Astrophysics, University of California, Berkeley, CA 94720,
USA. The opinions expressed are those of the authors. EUVE Principal
Investigators and Newsletter Publishers: Dr. R.F. Malina and Professor
C.S. Bowyer. EUVE Science and Technology Manager: Dr. C.A. Christian.
ISO Manager and Newsletter Editor: B.A. Stroozas. Funded by NASA contracts
NAS5-30180 and NAS5-29298. Send newsletter correspondence to:
ceanews@cea.berkeley.edu. The EUVE project is managed by NASA's GSFC:
Paul Pashby, GSFC Project Manager; Dr. Yoji Kondo, Project Scientist;
Dr. Ronald Oliversen, Deputy Project Scientist; Mr. Kevin Hartnett,
Project Operations Director. NASA HQ: Dr. Robert Stachnik, Program
Scientist; Dr. G. Riegler, Program Manager. Information on the EUVE
Guest Observer Program is available from: Dr. Y. Kondo, Mail Code 684,
GSFC, Greenbelt, MD 20771 at (301) 286-6247 or e-mail to
euve@stars.span.nasa.gov.
END-----------EUVE------------ELECTRONIC---------------NEWS-------------END
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