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Vol 6, No. 8                 30 Aug 1996                    ISSN 1065-3597
	  (C) 1996, Regents of the University of California

Notes from the Editor
   by Brett A. Stroozas, EUVE Science Operations Manager

   Welcome to the electronic newsletter for NASA's Extreme Ultraviolet
Explorer (EUVE) satellite, compiled and published monthly by 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 Recent EUVE Science Highlights
    1.2 Abstracts of Recently *Accepted* EUVE Papers
 2. EUVE Science Operations News
    2.1 EUVE Outsourced Extended Mission Status Report
    2.2 Public GO/RAP Data Release for 1 Sep 1996
    2.3 On-Line Access to EUVE
 3. CEA Science Education News
    3.1 Science Information Infrastructure Project
    3.2 Interactive University Project
    3.3 Astro-QUERY Project
    3.4 Advisory Board Meeting
 4. CEA Job Listings

To comment on or make suggestions for the EUVE electronic newsletter,
please send e-mail to (Internet).

   The EUVE observatory performed well throughout the month of Jul
1996, conducting observations of the following Guest Observer (GO) and
Right-Angle Program (RAP) targets (name and spectral type information
taken from the SIMBAD or internal CEA databases; "NOIDs" are
unidentified objects):

 Target            EUVE           Spectral     Observation
  Name             Name            Type        GMT Date(s)        Notes

NGC 5548         EUVE J1417+25.1  AGN:Sy1   26 Jun - 07 Jul 1996  EGO,CO1
TON S 180        EUVE J0057-223   AGN:Sy1   08 Jul - 17 Jul 1996  EGO,CO2,TCO
1908+0734        --------         NeutSt    08 Jul - 17 Jul 1996  RAP
BRI 0021-02      --------         M         17 Jul - 23 Jul 1996  EGO
AG Dra           --------         K0:Simb   23 Jul - 27 Jul 1996  EGO,TOO
BRI 0021-02      --------         M         27 Jul - 27 Jul 1996  EGO
HU Aqr           --------         CV        27 Jul - 30 Jul 1996  EGO
rxrad            --------         AGN       27 Jul - 30 Jul 1996  RAP
Diffuse Bkgd     --------         Bkgd      30 Jul - 02 Aug 1996  EGO,TCO

Key to Notes:
	EGO = Guest Observer observation
	RAP = Right Angle Program observation
	CO1 = observation coordinated with the Galilleo satellite
	CO2 = observation coordinated with the ASCA satellite
	TCO = time-critical observation
	TOO = target of opportunity observation

1. EUVE Science News

1.1 Recent EUVE Science Highlights
	by Dr. Pierre Chayer, EUVE/CEA Scientist


   Drs. B.C. Monsignori Fossi, M. Landini, and G. Del Zanna from the
Dipartimento di Astronomia e Scienza dello Spazio at the Universita di
Firenze in Italy, and Dr. S. Bowyer from CEA, observed and analyzed
the EUVE spectrum of AU Mic.  AU Mic is a flaring and rapidly rotating
M2 Ve star at a distance of 8.8 pc.  EUVE detected AU Mic both in the
scanning mode and with the Deep Survey/Spectrometer, which is equipped
with a direct broadband imaging detector and three spectrometers to
cover the short (70-190 A, SW), medium (140-380 A, MW), and long
(280-760 A, LW) extreme-ultraviolet wavelengths.  These instruments
allow simultaneous imaging and spectroscopy with a spectral resolution
of 0.5, 1, and 2 A in the SW, MW, and LW detectors, respectively.

   Two flares were detected in the course of the observation of AU
Mic. A first large flare was detected in all three spectrometer
channels, followed by a decaying phase.  A second, smaller flare was
observed in the SW and MW channels. The large flare peaked very
quickly, while the descending phase lasted about three hours. The star
remained active between the two flares and returned to the quiescent
level only after the second flare.

   The EUVE spectrometers allow individual line identifications and
detailed spectroscopic analysis. In the AU Mic observation, several
highly ionized iron lines were well detected (Fe XV, XVI, XVIII, XIX,
XX, XXI, XXII, XXIII, XXIV).  These lines were used to characterize
the temperature region logT = 5.8 - 7.3 and to provide the
differential emission measure (DEM).

   Dr. Monsignori Fossi and her colleagues also performed an analysis
of the DEM as a function of time. They found that a high-temperature
component is present in the flaring and decay phases of the flares
that shifts toward higher temperatures at the flare peaks. The
enhancement of this hot component may be easily followed during this
time and is responsible for most of the flare brightening.

   Finally, using the Fe XXI 142.2 A blend spectral line,
Dr. Monsignori Fossi's group showed that both the line ratios and the
synthetic spectrum computed during quiet and flaring conditions
suggest an increase of electron density during flares, ranging between
3.0E+12 and 2.0E+13 cm^(-3). The densities obtained for the AU Mic
flares are more than an order of magnitude larger than the values
found in solar flares.

	NOTE: The EUVE science team are deeply saddened by the loss of
	their colleague and friend, Brunella Monsignori Fossi, who
	died unexpectedly on 22 January 1996.

1.2 Abstracts of Recently *Accepted* EUVE Papers

   Included below are abstracts of EUVE-related papers recently
*accepted* for publication.  For those papers authored by CEA
personnel, the CEA publication numbers are indicated.  Unless
otherwise noted, researchers may obtain preprints of the CEA papers by
sending an e-mail request containing the publication number(s) of
interest to

   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 site.
Please send all abstracts or preprints to


C.W. Mauche
To appear in Astrophysical Journal.

   Data obtained by the Extreme Ultraviolet Explorer satellite are
used to determine the EUV spectrum of the quasi-coherent oscillations
of the dwarf nova SS Cygni. It is found that the spectrum of the
oscillations is neither blue nor red nor grey relative to the net
(oscillation-phase integrated) spectrum, and hence that the
oscillations cannot be explained by variations in the effective
temperature, absorbing column density, or effective area,
respectively.  Instead, it is found that the amplitude of the
oscillations is high at the relative maxima of the net spectrum, and
low to zero at the relative minima of the net spectrum. This behavior
can be explained by either variations in the emission line flux atop a
constant underlying continuum, or variations in the optical depth of a
haze of overlapping absorption lines, in which case the optical depths
must be tau < 1 at the relative maxima of the net spectrum, and tau >>
1 at the relative minima.


K. Alcorn, F. Kronberg, and I. Hawkins
ISIS Newsletter, I, 38, 23, 1996.  [CEA publication #749]

   The Center for EUV Astrophysics (CEA) at UC Berkeley is developing
a World Wide Web information server tailored to the needs of
time-starved teachers.  This server will allow teachers to quickly
develop lesson plans incorporating NASA's latest discoveries.


R. Hemphill, J. Edelstein, and D. Rogers
To appear in Applied Optics.  [CEA publication #755]

   The quantum detection efficiency (QDE) of photon counting
microchannel plate detector channels can be increased by a factor of
two in the extreme ultraviolet bandpass, from 256 A to 1024 A, by
subjecting the input channel plate to a chemical solution treatment.
The efficiency increase has proven insensitive to the exposure of
laboratory atmosphere and is stable over the extracted charge lifetime
equivalent of multi-year astrophysical observations.  Chemically
treated microchannel plates that are overcoated with opaque
photocathodes of KBr and CsI show a factor of two QDE increase from
834 A to 1100 A in comparison with previous measurements using
conventional untreated microchannel plates.

M. Lampton, R. Lieu, J.H.M.M. Schmitt, S. Bowyer, W. Voges, J. Lewis,
  and X. Wu
To appear in Astrophysical Journal Supplement.  [CEA publication #756]

   We present a list of 534 objects detected jointly in the Extreme
Ultraviolet Explorer (EUVE) 100 A all-sky survey and in the ROSAT
X-Ray Telescope 0.25 keV band.  The joint selection criterion permits
use of a low count rate threshold in each survey. This low threshold
is roughly 60% of the threshold used in the previous EUVE all-sky
surveys, and 166 of the objects listed here are new EUV sources,
appearing in neither the Second EUVE Source Catalog nor the ROSAT Wide
Field Camera Second Catalog.  The spatial distribution of this all-sky
catalog shows three features: an enhanced concentration of objects in
Ursa Major, where the Galactic integrated HI column reaches its global
minimum; an enhanced concentration in the third quadrant of the Galaxy
(l_II from 180 deg to 270 deg) including the Canis Major tunnel where
particularly low HI columns are found to distances beyond 200 pc; and
a particularly low number of faint objects in the direction of the
fourth quadrant of the Galaxy, where nearby intervening HI columns are
appreciable.  Of particular interest is the composition of the 166
detections not previously reported in any EUV catalog.  We offer
preliminary identifications for 105 of these sources. By far the most
numerous (81) of the identifications are late-type stars (F,G,K,M),
while 18 are other stellar types, only 5 are white dwarfs (WDs), and
none is extragalactic.  The paucity of WDs and extragalactic objects
may be explained by a strong horizon effect wherein interstellar
absorption strongly limits the effective new-source search volume and,
thereby, selectively favors low-luminosity nearby sources over more
luminous but distant objects.


J.F. Kartje, A. Konigl, C.-Y. Hwang, and S. Bowyer
To appear in Astrophysical Journal.  [CEA publication #757]

   We carried out a spectroscopic observation of the BL Lacertae
object Mrk 421 with the Extreme Ultraviolet Explorer satellite over a
11-day period in late April/early May 1995 (~242 ksec useful time).
During this period the source underwent a flare that was detected also
in X-rays and TeV gamma-rays.  The best continuous coverage of the
flare was obtained by EUVE, which resolved the smooth rise and fall of
the flux, measuring the variability of as much as a factor of ~1.5
over a span of ~2 days.  The detected spectrum extended from ~65-100 A
and could be fit with a power law of energy spectral index alpha_EUV
~= 3.5 +/- 0.8 for the measured Galactic hydrogen column density.  The
EUV spectrum is much steeper than the mean 1.5 - 5.0 keV X-ray
spectrum, alpha_X = 1.63 +/- 0.02, measure simultaneously by the ASCA
satellite.  Furthermore, a simple power-law fit to the observed fluxes
at 85 A and 1.5 keV (excluding the data from the first 3 days, the
time of maximum variability) significantly overestimates the flux at
the shortest detected EUV wavelengths.  These two findings imply that
strong absorption is occurring between ~65 and ~75 A.  Such absorption
is quite similar to that detected previously in our observation of the
BL Lacertae object PKS 2155-304.  We demonstrate that this absorption
can be attributed to a superposition of Doppler-smeared absorption
lines originating in high-velocity, QSO-type nuclear clouds of total
column density ~5E+21 cm^(-2) that are ionized by the beamed continuum
of the associated relativistic jet.  We identify the lines as mostly
L- and M-shell transitions of Mg and Ne.  The data suggest that the
velocity range spanned by the clouds is relatively small (from v_i ~=
0.05c to f_v ~= 0.1c).  We find that such a range is consistent with a
scenario in which the clouds are initially accelerated to v_i by a
magnetized outflow from a nuclear accretion disk, with radiation
pressure further accelerating them to V-f after they enter the beamed
emission cone of the jet.  We also compute the expected cloud
absorption lines in the UV and soft X-ray regimes and use these
results to constrain the clouds' physical parameters and chemical


2. EUVE Science Operations News

2.1 EUVE Outsourced Extended Mission Status Report
	by Brett Stroozas, EUVE Science Operations Manager

   Since the launch of EUVE in Jun 1992, CEA has been the operations
center for the command and control of the EUVE science payload.  The
payload is mounted on the Explorer Platform spacecraft (EP), which has
been operated since launch by a Lockheed-Martin (L-M) Flight
Operations Team (FOT) under the management of GSFC.

   In Apr 1996 CEA submitted an unsolicited proposal to NASA for an
EUVE outsourced extended mission (OEM) in which CEA would take over
from GSFC the management of EP operations.  The OEM plan was for CEA
to team with an industrial partner (IP; e.g., L-M) who would then
perform the actual daily EP operations, with CEA performing the
overall project operations management.  The idea behind this proposal
was that CEA would manage/operate the entire satellite at an overall
lower cost by streamlining EP operations (similarly to what CEA has
done for the payload), by providing integrated payload and EP
operations management, and by reducing the reliance on NASA
institutional support elements (e.g., the Packet Processor and Flight
Dynamics Facilities).  This OEM plan outlined a scheduled
management/operations hand-over to occur in early 1997.

   CEA's proposal was approved by NASA in May 1996.  In Apr CEA
released a Request for Proposals (RFP) calling on all potential IPs to
bid for the EUVE OEM operations contract under CEA management.  The
RFP called for the IP to perform two major functions: (1) to operate
the EP on a daily basis, and (2) to set up the EP command and control
center; all of this was to be done under a firm, fixed-priced (FFP)
contract.  A handful of companies expressed initial interest in
bidding and attended a bidder's conference held at CEA in late Apr;
unfortunately, when the proposal acceptance period closed in late May
CEA had received no bids.  In follow-up discussions with some of the
applicable companies the major reasons given for not bidding were
working under a FFP contract and the perceived high risk of not making
a large enough profit margin given the work to be performed.  So,
based on the null result of the RFP, CEA put into effect its backup
plan: CEA would do it all -- manage and operate the EP -- from an EP
Operations Center (EPOC) to be set up at and by CEA.

   Based on the results of the RFP process, NASA revised the OEM plan
into the following two phases:

 o Phase 1, Operations Management -- CEA will take over from GSFC the
   EP management and operations in mid-Feb 1997.  Until that time,
   GSFC will extend the operations contract of the incumbent L-M FOT.
   Under this contract extension the L-M FOT will be additionally
   tasked with providing EP operations training to the newly-hired CEA
   FOT personnel.
 o Phase 2, Science Management -- Upon completion of Phase 1, CEA will
   take over from GSFC all EUVE science management activities (e.g.,
   management of the Guest Observer Program).  During the Phase 1
   work, transfer of the science management activities will commence
   and be incrementally phased in.

   Although the details of the Phase 2 transition are still under
discussion with NASA, the following are some of the major
accomplishments to date for Phase 1:

 o In Jun CEA sent a draft of its OEM implementation plan to GSFC for
   review.  A "working group" telecon was held between GSFC and CEA on
   27 Jun in order to review and comment on this plan.  A number of
   Review Item Discrepancies (RIDs) were generated that require
   follow-up actions and/or clarifications to the plan; work on
   revising the OEM implementation plan based on these RIDs is in
 o A Cooperative Agreement between NASA GSFC and CEA has been signed
   off, making the OEM official.
 o CEA has chosen to use the Transportable Payload Operations Control
   Center (TPOCC) as the basis for EP operations in the CEA EPOC.
   TPOCC is a workstation-based command and control system that has,
   for the past few years, been under development at and by GSFC for
   EUVE; EUVE TPOCC is scheduled for final delivery in mid-Oct 1996.
   In lieu of TPOCC CEA had been seriously considering going with a
   commercial command and control system (in particular, CEA had been
   focusing on the possible use of a system called EPOCH 2000 from
   Integral Systems, Inc.).  However, the use of TPOCC was chosen over
   that of a commercial system due to a combination of cost, schedule,
   and risk considerations.
 o The development of the EPOC at CEA is in full swing.  The EPOC
   systems, which will leverage heavily off of those currently (or
   soon to be) in operations for EUVE at GSFC, will be supplied to CEA
   as government-furnished equipment (GFE).  Initial shipments of GFE
   from CEA have included a spare package of the Command Management
   System (CMS) hardware and software, the EP Planning System (EPPS)
   software, and the current release of the TPOCC software.
 o Hiring and staffing of the EPOC FOT is in progress and will be
   completed soon.  The newly-hired FOT staff will then be sent to
   GSFC for ~2 months of training with the incumbent L-M FOT.

Some of the major upcoming Phase 1 schedule milestones include the

 o Complete EPOC FOT Hiring/Staffing	09/02/96
 o EPOC FOT Training at GSFC		09/16/96 - 11/22/96
 o GSFC OEM Review			~11/96 (tentative)
 o Complete EPOC Development		12/01/96
 o Begin Shadow Operations Period	01/06/97
 o Complete Operations Hand-over	02/15/97

As noted above, a full-up detailed review of CEA's OEM implementation
plan/progress will probably occur sometime in the late-Oct or
early-Nov timeframe (exact date TBD).  This review will ensure that
all of the relevant major issues have been properly addressed, and
that the overall implementation is progressing according to the
planned schedule.  A "shadow operations" period is slated for Jan/Feb
1997, in which CEA will progressively take on more and more of the
daily EP operational responsibilities.  A final operations hand-over
from GSFC to CEA is scheduled to occur in mid-Feb 1997, at which point
the outsourcing will be complete.

2.2 Public GO/RAP Data Release for 1 Sep 1996
        by Dr. Nahide Craig, EUVE User Support Scientist

   The table below lists the GO/RAP observations that become public on
1 Sep 1996.  For each observation is given the target name, the
approximate exposure time in ksec, the GMT start/end dates, the
target's spectral type, and the data identification code (GO and RAP
data are marked accordingly).  All public data sets can 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.  Processed data sets are shipped via postal mail on 8mm tape
or (if requested) on CD-ROM.

   The data rights policies for observations state that Principal
Investigators (PIs) have proprietary rights to the data for a given
period of time 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 proprietary period begins after the PI is sent the final
piece of the completed observation.

   Target        ~Exp      Observation Dates      SpT      DataID
    Name        (ksec)    Start           End

  GO Data Sets Available 1 Sep 1996:

  GR Burster        8    01 Jul - 01 Jul 1995     GRB      go0373
  Mrk 421         566    07 May - 13 May 1995     BLLac    go0374 
  HZ 43             3    27 May - 27 May 1995     WD:DAw   go0375 *
  Moon              4    09 Jun - 09 Jun 1995     SolSys   go0376     
  LoTr 5           60    07 Jun - 09 Jun 1995     PlanNeb  go0377 
  LoTr 5          100    10 Jun - 13 Jun 1995     PlanNeb  go0378 
  LoTr 5           78    13 Jun - 16 Jun 1995     PlanNeb  go0379 
  LoTr 5          100    16 Jun - 20 Jun 1995     PlanNeb  go0380 
  LoTr 5           39    20 Jun - 21 Jun 1995     PlanNeb  go0381 
  VW Hyi          100    08 Jul - 11 Jul 1995     DwNova   go0382
  VW Hyi          100    11 Jul - 15 Jul 1995     DwNova   go0383 
  VW Hyi           96    15 Jul - 18 Jul 1995     DwNova   go0384 
  TON S 180       100    18 Jul - 22 Jul 1995     QSO      go0385 
  EUVE J2324+458    3    18 Jul - 18 Jul 1995     NOID     go0386
  TON S 180        53    22 Jul - 24 Jul 1995     QSO      go0387 
  RE 2156-543     100    24 Jul - 27 Jul 1995     WD:DA    go0388 
  RE 2156-543      55    27 Jul - 29 Jul 1995     WD:DA    go0389 
  RE 2324-544     100    29 Jul - 02 Aug 1995     WD:DA    go0390 
  RE 2324-544      94    02 Aug - 05 Aug 1995     WD:DA    go0391 
  II Peg          101    05 Aug - 09 Aug 1995     RSCVn    go0392
  Moon              1    07 Aug - 07 Aug 1995     SolSys   go0393 
  Feige 24         28    31 Oct - 01 Nov 1995     WD:DA    go0394 *

	Note:  "*" indicates calibration target

  RAP Data Sets Available 1 Sep 1996:

  EUVE J0325+012    8    19 Oct - 19 Oct 1995     NOID     rap0043


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)

   telnet 200 (for those without a WWW browser)

 o anonymous FTP

	Name:  anonymous
	Password:  type_your_full_e-mail_address

 o anonymous gopher


 o EUVE Electronic Newsletters

     Past issues -- available via the CEA WWW site
     Subscriptions -- mail ("subscribe
     Post message (moderated) to all subscribers:

 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 more information see the CEA
     WWW site or contact the Archive (

 o Public RAP

     The Public Right Angle Program (RAP) is a simple and 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
     (  Mail all proposals to

 o Contact information for the EUVE Science Archive or EGO Center:

		     Center for EUV Astrophysics
			  2150 Kittredge St.
		       Berkeley, CA  94720-5030
			 510-642-3032 (voice)
			  510-643-5660 (fax)

3. Science Education News
	by Dr. Isabel Hawkins, CEA Science Education Director

3.1 Science Information Infrastructure Project

   Year two of this exciting project is underway. The San Francisco
Exploratorium, the Berkeley Lawrence Hall of Science, and the National
Air and Space Museum will continue to develop and pilot-test their
classroom modules with their teachers, while Science Museum of
Virginia will be pilot-testing the activities independently to ensure
that they can be used in a variety of classroom situations.  The
Exploratorium's "Aurorae -- Paintings in the Sky" lesson plan (URL: has been selected by
PacBell for their on-line "Bluewebn" award.

3.2 Interactive University Project

   CEA is a member of the UCB campus-wide coalition "The Interactive
University" for the purpose of carrying out effective outreach to the
community.  The Interactive University Project has become the
technology arm of the "Berkeley Pledge" which is the UCB Chancellor's
official outreach program to the neighboring school districts.  As
part of this coalition, CEA has partnered with the Oakland and San
Francisco School Districts in Technology Challenge Grants submitted to
the U.S. Department of Education.  These grants would be used to
develop an articulated program for all grade levels that will
successfully integrate technology into the Districts' math and science
curricula.  As part of the Berkeley Pledge CEA has received funding
for three years beginning in October 1996.  The CEA's contribution to
the collaboration will be the Science On-Line Program methodology,
which will be adopted by the two school districts to carry out their
teacher professional development program for science. An important
component of this effort will include the design and implementation of
a feasible methodology for the participation and contribution of
scientists to education.

3.3 Astro-QUERY Project

   Science Education activities at CEA will continue to rely on the
Internet as their primary publishing tool, and its use will be
facilitated by the development of an innovative information server
based on hypertext markup language (HTML) forms -- a familiar
interface to World Wide Web users. The Astro-QUERY CEA Information
Server will give users the ability to retrieve information on the EUVE
satellite mission and data archive that is tailored to their level of
expertise.  Astro-QUERY, being developed for the Science Education
Program, will allow the user to specify parameters that indicate the
desired levels of complexity, breadth, scope, format (e.g., text or
graphics), etc. of the requested information topic. The K-12 education
materials for the Astro-QUERY Information Server are being developed
at CEA via a teacher intern program. Dr. Nellie Levine, a physics
teacher from Galilleo High School in San Francisco, created outlines
for the following two tutorials, which will access a variety of
relevant resources from the EUVE mission and data:

 o "Be an Engineer -- Learn How to Operate a Satellite"
 o "Be a Scientist -- Learn How to Become a Space Researcher"

Dr. Levine and two of her high school students are spending one month
this summer at CEA, funded by a planning grant obtained from the UC
Office of the President.  To support full implementation of this
project, CEA is submitting to the Corporation of Public Broadcasting a
proposal that includes the new San Francisco Public Library.  A paper
describing this project has been submitted to the American Education
Research Association.

3.4 Advisory Board Meeting

   The next science education advisory board meeting will take place
at CEA on 19 August 1996.  CEA is looking forward to sharing its
progress with its colleagues.

4.0 CEA Job Listings
	by Cathie Jones, CEA Personnel Manager


   Multiple opportunities exist on NASA's Extreme Ultraviolet Explorer
(EUVE) satellite project.  Current experience on Multi-Mission
Satellite operations is desired for all positions.  Candidates will be
temporarily located at GSFC, Greenbelt, MD, until the new Explorer
Platform Operations Center is complete at the Center for EUV
Astrophysics, University of California, Berkeley.  To apply, send
resume and three references to UC Personnel Office, 2200 University
Ave, Berkeley, CA 94720-3540.  Cite the box number given for the
position in which you are interested.


	    Platform Operations Manager ($47.7K - $59.7K)

   Coordinate all satellite operations personnel in the performance of
operations tasks.  Extensive experience in aerospace field, including
significant managerial experience.  Demonstrated capabilities in
spacecraft systems engineering; spacecraft mission planning and
scheduling; spacecraft-to-ground interfaces, including TDRSS and DSN;
spacecraft monitoring, command, and control; spacecraft attitude
control systems, power systems, thermal systems, on-board
communications systems, and on-board data handling systems.


		Subsystem Engineers ($43.4K - $54.3K)

   Experience in spacecraft operations with proficiency in two or more
of the following: spacecraft communications and data handling systems;
spacecraft power systems; attitude control systems; spacecraft thermal
systems and analysis; spacecraft mission planning and console
operations; spacecraft tracking, orbit determination, and analysis.


	       Ground System Engineer ($43.4K - $54.3K)

   Significant experience in spacecraft ground systems design,
development, maintenance, or operations, and experience in spacecraft
command, telemetry, and data processing systems; engineering and
operations; and development and execution of system test plans and
computer systems user support.


	       Satellite Controllers ($32.6K - $40.8K)

   Experience with spacecraft data acquisition, TDRSS scheduling,
spacecraft telemetry monitoring and command.  Console operations or
multi-mission satellite spacecraft experience is desired.

  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. Roger F.
  Malina and Professor Stuart Bowyer.  Newsletter Editor: Brett A.
  Stroozas.  Funded by NASA contract NAS5-29298.  Send newsletter
  correspondence to

  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, Mission
  Director.  NASA HQ: Dr. Guenter Riegler, Program Manager.
  Information on the EUVE GO Program is available from Dr. Yoji Kondo,
  Mail Code 684, GSFC, Greenbelt, MD 20771 at (301) 286-6247 or e-mail

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