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ELECTRONIC NEWSLETTER OF THE EUVE OBSERVATORY
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Vol 6, No. 9 30 Sep 1996 ISSN 1065-3597
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(C) 1996, Regents of the University of California
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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 AO4 Proprietary Data Rights
1.3 Abstracts of Recently *Accepted* EUVE Papers
2. EUVE Science Operations News
2.1 Safe-Hold Event Summary
2.2 New Science Planner
2.3 Public GO/RAP Data Release for 1 Oct 1996
2.4 On-Line Access to EUVE
3. EUVE Outsourced Extended Mission (OEM) Status Report
3.1 Formation of EUVE Science Advisory Board (ESAB)
3.2 Announcement of Joint EUVE Users Group/ESAB Meeting at CEA
3.3 ESAB to Meet at AAS in Toronto
3.4 Recent OEM Highlights
To comment on or make suggestions for the EUVE electronic newsletter,
please send e-mail to archive@cea.berkeley.edu (Internet).
The EUVE observatory performed well throughout the month of Aug
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
=======================================================================
Diffuse Bkgd -------- Bkgd 30 Jul - 02 Aug 1996 EGO,TCO
NGC 246 EUVE J0037-11.8 PN 02 Aug - 05 Aug 1996 EGO
WD 1845+019 EUVE J1847+019 WD:DA 02 Aug - 05 Aug 1996 RAP
Safe-Hold -------- ---- 05 Aug - 10 Aug 1996 SAF
NGC 246 EUVE J0037-11.8 PN 10 Aug - 10 Aug 1996 EGO
WD 1845+019 EUVE J1847+019 WD:DA 10 Aug - 10 Aug 1996 RAP
QS Tel EUVE J1938-46.2 CV:AM 10 Aug - 11 Aug 1996 EGO
0006+18 -------- NeutSt 10 Aug - 11 Aug 1996 RAP
UV Cet EUVE J0138-17.9 M5.5V:e 11 Aug - 21 Aug 1996 EGO
QQ Vul EUVE J2005+22.6 CV:AM 11 Aug - 21 Aug 1996 RAP
NGC 6853 EUVE J1959+22.7 PN 11 Aug - 21 Aug 1996 RAP
Survey -------- ---- 21 Aug - 22 Aug 1996 ENG
RE J0317-853 EUVE J0317-85.5 Star 22 Aug - 28 Aug 1996 EGO
EUVE J2231+017 EUVE J2231+017 NOID 22 Aug - 28 Aug 1996 RAP
Jupiter -------- SolSys 28 Aug - 31 Aug 1996 EGO,COO
0119-286 -------- AGN 28 Aug - 31 Aug 1996 RAP
QS Tel EUVE J1938-46.2 CV:AM 31 Aug - 01 Sep 1996 EGO
0006+18 -------- NeutSt 31 Aug - 01 Sep 1996 RAP
=======================================================================
Key to Notes:
EGO = Guest Observer observation
RAP = Right-Angle Program observation
TCO = Time-critical observation
COO = Observation coordinated with the Galileo satellite
1. EUVE Science News
====================
1.1 Recent EUVE Science Highlights
----------------------------------
by Dr. Pierre Chayer, EUVE/CEA Scientist
*** EUVE OBSERVATIONS OF EUVE J0720-317 AND EUVE J0723-277 ***
Drs. Stephane Vennes, Jean Dupuis, and Stuart Bowyer from CEA
observed and analyzed the EUVE spectra of the hot DAO white dwarf EUVE
J0720-317, member of a pre-cataclysmic binary system, and the nearby
hot white dwarf EUVE J0723-277.
They noted that the column densities in the line of sight of EUVE
J0720-317 and EUVE J0723-277 are very different even though these two
stars are less than five degrees apart on the celestial sphere. The
measured interstellar medium column densities of neutral hydrogen
N(HI), neutral helium N(HeI), and ionized helium N(HeII) in the line
of sight of EUVE J0720-317 are, respectively, 2.1E+18 cm^(-2), 1.3E+18
cm^(-2), and smaller than 0.5E+18 cm^(-2), although in the line of
sight of EUVE J0723-277 the column densities are, respectively,
0.9E+18 cm^(-2), 0.1E+18 cm^(-2), and 0.2E+18 cm^(-2). They point out
that the N(HeI) to N(HI) ratio, along the sight line of EUVE
J0720-317, is unusually high with a value of 0.6 compared to the
typical values of 0.05 to 0.08 observed in the line of sight of other
hot white dwarfs.
They propose two possibilities to explain the high N(HeI) to N(HI)
ratio toward EUVE J0720-317. They suggest that this line of sight
might very well represent a direction in the local interstellar medium
where the hydrogen is strongly ionized. For example, if (N(HI) +
N(HII)) / (N(HeI) + N(HeII)) is equal to 10, they derive a ionization
fraction of 90% for hydrogen and 30% for helium. The other
possibility comes from the fact that EUVE J0720-317 is member of a
pre-cataclysmic binary that went through a common envelope evolution
phase in the past.
Dr. Vennes and his group put forward the idea that some fossil
circumbinary material might attenuate the EUV emission produced by the
white dwarf. The results of these observations were presented by Dr.
Dupuis at the 10th European Workshop on White Dwarfs in June 1996, in
Blanes, Spain.
1.2 AO4 Proprietary Data Rights
-------------------------------
by Dr. Ron Oliversen, EUVE Deputy Project Scientist (GSFC)
This is to remind EUVE GOs, as stated in the NASA Research
Announcement (NRA), that beginning with the Announcement of
Opportunity (AO) for Cycle 4 the proprietary period was decreased from
12 to 6 months. However, to facilitate this change the Cycle 4 data
will start to become public on January 1, 1997 or 6 months after the
data has been delivered to the GOs, whichever comes later.
1.3 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 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 site.
Please send all abstracts or preprints to archive@cea.berkeley.edu.
--------------------------------------------------------------
EUV OBSERVATIONS OF EX HYDRAE: 10^7 K GAS NEAR A WHITE DWARF SURFACE
M. Hurwitz, M. Sirk, S. Bowyer, and Y.-K. Ko
To appear in Astrophysical Journal. [CEA publication #759]
We have observed the intermediate polar EX Hydrae for 180,000 s
with the Extreme Ultraviolet Explorer. The EUV flux is strongly
modulated at both the binary period (98 min) and the white dwarf spin
period (67 min). The secondary star eclipse is total, with a duration
of 41 +/- 2 s. The ingress and egress of the secondary eclipse have a
duration < 3 s (68% confidence). The centroid of the secondary
eclipse is independent of the white dwarf spin phase to within 6 s.
The eclipse attributed to the disk bulge has an energy dependence
consistent with photoelectric absorption through a neutral column of
about 1.3E+20 cm^(-2). Folded on the white dwarf spin period, the EUV
flux is modulated by a factor of 3.7. The shape of the light curve
can be accurately matched with a simple geometrical absorption model,
although the variation in modulation depth with energy (e.g., EUV vs.
X-rays) requires a more sophisticated model. The EUV spectrum reveals
many narrow emission lines characteristic of a plasma around 10^7 K,
and possibly features indicating temperatures as low as 10^6 K.
Assuming optically thin emission we find a volume emission measure
around 3E+54 cm^(-3) for the 10^7 K plasma, and an accretion rate
around 3E+16 gm/s. By direct geometrical arguments we constrain the
EUV emission region to a region extending over less than 4% of the
white dwarf surface area located within 0.5 white dwarf radii (in the
orbital plane) and 4.5 white dwarf radii (perpendicular to the plane)
relative to the center of the white dwarf. Two independent arguments
lead to the conclusion that the electron density is > 1E+13 cm^(-3),
probably > 1E+15 cm^(-3), in the EUV-emitting region.
--------------------------------------------------------------
EXTREME ULTRAVIOLET FLUX FROM THE VIRGO CLUSTER: FURTHER EVIDENCE
FOR A 500,000 KELVIN COMPONENT
S. Bowyer, M. Lampton, and R. Lieu
To Appear In Science. [CEA publication #760]
A surprising discovery in X-ray astronomy was that clusters of
galaxies often contain vast quantities of hot (20 million Kelvin)
diffuse gas. Substantial diffuse extreme ultraviolet emission has
recently been detected in the Virgo cluster of galaxies. Depending
upon the character of the interstellar medium in our Galaxy, this
emission could be either an aspect of the hot cluster gas, or a new
500 thousand Kelvin component. We analyzed the observational data in
combination with the interstellar medium and found the extreme
ultraviolet flux cannot be an effect of the interstellar medium.
Hence a warm cluster component appears likely.
--------------------------------------------------------------
DIFFUSE EXTREME ULTRAVIOLET EMISSION FROM THE COMA CLUSTER -- EVIDENCE
FOR A COOL COMPONENT AT SUB-MK TEMPERATURES
R. Lieu, J.P.D. Mittaz, S. Bowyer, J.O. Breen, F.J. Lockman, E.M.
Murphy, and C.-Y. Hwang
To appear in Science. [CEA publication #761]
The central region of the Coma cluster of galaxies was observed in
the 0.065 - 0.245 keV energy band by the deep survey (DS) telescope
aboard the Extreme Ultraviolet Explorer (EUVE). A diffuse emission
halo of angular diameter ~30 arcmin was detected. The EUV emission
level significantly exceeds that expected from the well-measured X-ray
temperature gas in Coma. Similar "soft excesses" are also evident in
the Roentgen Satellite (ROSAT) Position Sensitive Proportional Counter
(PSPC) data. The phenomenon cannot be explained by an arbitrary
reduction of the Galactic H and He column densities. Rather, it
suggest the presence of two more phases in the emitting gas, one at a
temperature of ~2E+06 K and the other ~8E+05 K. The latter cools
rapidly and, in steady state, would have produced cold matter of mass
~1E+14 solar masses (M_solar) within the EUV halo. Although a similar
EUV enhancement was discovered in the Virgo cluster, this is the first
detection of its presence in a non-cooling flow system.
--------------------------------------------------------------
2. EUVE Science Operations News
===============================
2.1 Safe-Hold Event Summary
---------------------------
by Brett Stroozas, EUVE Science Operations Manager
On 5 Aug at 03:04 GMT, during a real-time contact with the EUVE
spacecraft, a software anomaly in its On-Board Computer (OBC) caused
the spacecraft to transition to its Safe-Hold Mode (SHM). During a
nominal SHM transition, the Solar Array Drives (SADs) are
hardware-commanded to the INDEX position, which moves the SAs
perpendicular to the spacecraft body. The Attitude Control
Electronics (ACE) then use coarse sun sensor data to reorient the
spacecraft body to the sunline. In this occurrence however, the SADs
never received the SHM signal from the ACE so that the solar arrays
did not go to the INDEX position and, consequently, the spacecraft
body did not reorient either. This left the spacecraft in a "partial"
SHM -- in a rate-damping attitude control mode at its last inertial
attitude (~55 degrees off the sunline).
Ground personnel began working the problem immediately. At 04:56
GMT a radio frequency (RF) switch was made to the omni antennae in
order to enable communications in the absence of high-gain antenna
(HGA) pointing capability. The SAs were reoriented by hardware
command to the INDEX position to force the generation of this control
signal back to the ACE. Ground personnel later determined that an
"automode enable" signal on Power Switching Unit A (PSU-A) was
disabled, preventing the SHM signal from properly reaching the SADs.
After enabling this signal however, the spacecraft still did not move
to the sunline. After some analysis, it was determined that there was
a hardware failure in the safe-hold card in PSU-A, and commands were
sent to switch to the redundant B side. Upon switching, the ACE
received the INDEX signal, the spacecraft moved as expected, and the
transition to full SHM was completed. The ground then dumped the OBC
memory for analysis by GSFC Flight Software (FSW) personnel.
While this FSW analysis was in progress, the Flight Operations Team
(FOT) at GSFC manually commanded the Modular Antenna Pointing System
(MAPS) to shade the HGA gimbals as they were approaching their high
red temperature limit. At another extreme, the payload was getting
extremely cold because all of the survival heaters were not enabled.
This was corrected via ground commands.
Some power/battery management steps were also quickly taken. The
spacecraft was commanded to voltage/temperature (V/T) level 3 and the
battery temperatures were manually tracked and maintained within a
determined temperature range by sending ground commands to the battery
heaters. This function is normally controlled by the OBC.
After detailed investigation, FSW personnel determined the cause of
the OBC crash. Two OBC Executive Requests, one a relative time
sequence (RTS) command request and the other a form of "I'm OK"
request, interfered with one another resulting in the OBC
relinquishing control to the ACE electronics and then halting. This
is a very obscure bug in the FSW that has been resident in these NASA
Standard Spacecraft Computers (NSSC-I) for many years. A FSW patch
was made on 29 Aug to correct the error in the code; FSW personnel are
also communicating information on this bug to all other missions
(e.g., UARS, TOPEX, and GRO) that are currently flying a NSSC-Is.
The OBC was restarted on 8 Aug and the spacecraft was back in
inertial mode by 21:16 GMT of the same day. On 9 Aug the RF was
switched back to the HGA and the spacecraft slewed back to the
original science plan target, NGC 246. Full reconfiguration of the
EUVE science payload instruments were completed on 10 Aug, a few
minutes more than five days after the initial SHM event. A hearty
congratulations is due to the entire SHM event response team who did
an excellent job in identifying the problems and successfully
recovering the spacecraft.
2.2 New Science Planner
-----------------------
by Dr. Damian Christian, EUVE Observation Support Scientist
GOs should be aware that there is a new science planner at EUVE.
Dave Meriwether, the EUVE science planner for the last 2+ years, has
moved on to an operations position on the Gravity Probe B mission at
Stanford University. We wish Dave the best in his new position and
thank him for all of his hard work and dedication on the EUVE Project.
Bryce Roberts is filling Dave's shoes as the new EUVE science
planner. Bryce has moved up through the ranks, from his beginnings as
a UCB undergraduate student Engineering Aide in the data analysis area
and optical identification program, to his current role as science
planner. Although Bryce can be reached via e-mail
(broberts@cea.berkeley.edu), GOs are encouraged to plan or discuss
their observing strategies directly with the GO scientists, Drs.
Damian Christian (damian@cea.berkeley.edu; 510-642-9908) or Brian
Flynn (flynn@cea.berkeley.edu; 510-642-4224).
2.3 Public GO/RAP Data Release for 1 Oct 1996
---------------------------------------------
by Dr. Nahide Craig, EUVE User Support Scientist
The table below lists the GO/RAP observations that become public on
1 Oct 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 OCT 1996:
HR 120 100 09 Aug - 13 Aug 1995 F2V go0395
HR 120 100 13 Aug - 16 Aug 1995 F2V go0396
HR 120 7 16 Aug - 16 Aug 1995 F2V go0397
VW Hyi 180 16 Aug - 23 Aug 1995 DwNova go0398
EUVE J0134-161 100 23 Aug - 26 Aug 1995 WD:DA go0399
EUVE J0134-161 100 26 Aug - 30 Aug 1995 WD:DA go0400
EUVE J0134-161 39 30 Aug - 31 Aug 1995 WD:DA go0401
epsilon Eri 92 31 Aug - 04 Sep 1995 K2V go0402
epsilon Eri 100 05 Sep - 09 Sep 1995 K2V go0404
epsilon Eri 104 09 Sep - 13 Sep 1995 K2V go0405
Moon 2 12 Sep - 12 Sep 1995 SolSys go0406
The following earlier datasets are also public as of 1 Oct 1996.
Unfortunately, due to various problems the release of these data
sets has been delayed until now and we apologize for any
inconvenience.
AT Mic 41 03 Jul - 05 Jul 1992 M4Ve go0407 *
Moon 3 24 Dec - 25 Dec 1993 SolSys go0408 *
EX Hya 21 26 Jan - 27 Jan 1994 CV go0409
beta Cen 24 27 Mar - 28 Mar 1994 B go0410
beta Cen 20 30 Mar - 31 Mar 1994 B go0411
EUVE J1847+019 40 13 Apr - 14 Apr 1994 WD:DA go0412
Jupiter 68 29 Apr - 02 May 1994 SolSys go0413
VW Hyi 61 01 Jun - 04 Jun 1994 DwNova go0414
Cyg 1992 17 20 Nov - 20 Nov 1994 DwNova go0415
Note: "*" --> calibration targets
RAP DATA SETS AVAILABLE 1 OCT 1996:
EUVE J0647-506 92 19 Nov - 22 Nov 1995 NOID rap0044
EUVE J0700-03.4 84 25 Dec - 28 Dec 1995 NOID rap0045
EUVE J1127+42.1 149 21 Jan - 27 Jan 1996 NOID rap0046
================================================================
2.4 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 (moderated) 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 more information see the CEA
WWW site or contact the Archive (archive@cea.berkeley.edu).
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
(egoinfo@cea.berkeley.edu). Mail all proposals to
euverap@cea.berkeley.edu.
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)
archive@cea.berkeley.edu
egoinfo@cea.berkeley.edu
3. EUVE Outsourced Extended Mission (OEM) Status Report
-------------------------------------------------------
3.1 Formation of EUVE Science Advisory Board (ESAB)
---------------------------------------------------
by Dr. Roger Malina, EUVE Observatory Director
The EUVE Science Advisory Board (ESAB) is currently being
established to provide overall policy and operations oversight for the
EUVE Observatory during the OEM. The letter included below (bounded
by "*****") describes NASA's view of EUVE operations after the
outsourcing to CEA/UCB is complete. CEA/UCB is currently establishing
the ESAB and developing its charter for presentation to NASA and to
the EUVE Users Group (EUG). Designated members of the new ESAB are as
follows:
Chair Designate:
Dr. Steve Howell, U. of WY
Members Designate:
Dr. Andrea Dupree, SAO
Dr. Chris Mckee, UCB (ex officio)
(One or two additional members are being contacted.)
Member Designate, EUVE Time Allocation Committee (TAC):
Dr. J. Liebert, U. of AZ
(Additional members are being contacted.)
Technology Program Advisor:
Mr. Peter Hughes, NASA-GSFC
Education Program Advisor:
Not yet designated.
EUVE users may contact Dr. Steve Howell (showell@mothra.uwyo.edu) with
any issues that they feel should be addressed as the new ESAB is set
up.
*******************************************************
SR September 6, 1996
TO: GSFC/EUVE Project Scientist
GSFC/EUVE Deputy Project Scientist
UCB/EUVE Instrument Principal Investigator
FROM: Chief Scientist,
Research Program Management Division
Office of Space Science
SUBJECT: Outsourcing of Extreme Ultraviolet Explorer (EUVE)
Operations and Science Management
Dear Yoji, Ron, and Roger:
The recent signing of the Cooperative Agreement between the NASA
Goddard Space Flight Center and the University of California at
Berkeley represents a major, innovative step for the EUVE Project
towards outsourcing of EUVE responsibilities. "Outsourcing"
includes a training/education component, continuation of technology
testbedding under the stewardship of Dr. Peter Hughes
(GSFC/Operations Directorate), and transition of full operations
responsibility. It is understood that, under the terms of this
NASA-University partnership, UCB will provide open, peer-reviewed
access to 90% of available observing time; technology testbedding
may use up to 25% of available observing time, and additional time
losses due to higher risk acceptance may occur. This outsourcing
effort fulfills both the letter and the spirit of the
Administration's "Reinventing Government" directives, as well as the
NASA Administrator's guidelines and the recommendations formulated
by the "Zero-Based Review" team. Please convey my appreciation for
their excellent work to your colleagues at GSFC's Mission Operations
and Data System Directorate, the Space Science Directorate, the
Program Procurement Division, and at UCB's Center for Extreme
Ultraviolet Astrophysics. I trust that this successful step in our
collaboration will pave the way for future NASA-University
partnerships.
Just as the Cooperative Agreement envisions a phased transition of
[operations] responsibilities from GSFC to UCB, science management
should also transition from GSFC to UCB. This means that science
direction - embodied in the Project Scientist role - should
transition from GSFC to UCB, including solicitation of proposals for
guest observations, selection, and formulation of a new, independent
external advisory board. I ask the EUVE Project Scientists to
discuss these changes with the current EUVE Users Group, to forward
any comments or recommendations they wish to offer to UCB (I have
just received a letter [from] J. Holberg with some suggestions which
deserve further consideration), and to release the group of their
advisory responsibilities. A key role for the new independent
external advisory board will be to advise UCB on the fairness and
scientific excellence of the observation selection and execution
process. Although this advisory board will report to UCB, my
colleagues at NASA Headquarters and I would appreciate occasional,
informal reports from the board chairperson on his/her assessment of
the integrity of the observation selection and execution process.
In the unlikely case that UCB and the advisory board (or other
members of the external science community) cannot reach agreement on
any policy or implementation issues, NASA Headquarters will be the
arbiter of last resort.
At least in the near term, NASA will retain responsibility for
financial support to Guest Observers, most likely through a combined
multi-wavelength grants program as suggested by the science
community.
Again, we in the Office of Space Science wish you and your
colleagues success in making this transition, bringing control of a
very productive scientific observatory closer to the science
community.
Sincerely,
Guenter Riegler
*******************************************************
3.2 Announcement of Joint EUVE Users Group/ESAB Meeting at CEA
--------------------------------------------------------------
by Dr. Steve Howell, ESAB Chair Designate
The recent signing of the Cooperative Agreement between NASA GSFC
and CEA/UCB represents a major, innovative step for the EUVE Project
towards outsourcing of EUVE responsibilities. The Cooperative
Agreement envisions a phased transition of responsibilities, including
those of science management, from GSFC to UCB. The planning of future
operations and scientific programs for EUVE is of interest to the
community and will serve as a model for future NASA satellite
programs. In order to discuss and plan this transition the EUG is
planning to have a joint meeting with the newly formed ESAB on 7-8 Nov
1996 at CEA in Berkeley, California.
The tentative agenda for the combined EUG/ESAB meeting will include
status reports on the following:
o EUVE spacecraft
o EUVE permanent data archive
o User (GO) services
o OEM: plan, status, possible complications, budget, etc.
o ESAB draft charter: data rights, interaction of ESAB/GO's/CEA/TAC,
science constraints due to funding decrease, etc.
o science planning
o AO for Cycle 5
o upcoming Jan 1997 AAS meeting
We invite all EUVE users to send additional topics that they would
like addressed, comments, and/or any recommendations that they wish to
offer to the EUG via Drs. Jay Holberg (holberg@argus.lpl.arizona.edu)
and/or Steve Howell (howell@kaya.uwyo.edu) by 1 Nov 1996.
3.3 ESAB to Meet at AAS in Toronto
----------------------------------
by Dr. Steve Howell, ESAB Chair Designate
The newly formed ESAB will hold a public meeting at the Jan 1997
meeting of the American Astronomical Society (AAS) in Toronto, Canada.
The public ESAB Meeting will be held on Tuesday, 14 Jan from
14:00-17:00 in Room "Pier 7". As you may be aware, the EUVE satellite
is the first NASA Astrophysics Mission to be "privatized" or
"outsourced", as part of NASA's directive to move spacecraft
operations to industry and universities. The planning of future
operations and scientific programs for EUVE is of interest to the
community and will serve as a model for future NASA satellites. Please
plan on attending this round-table discussion. See you at the AAS!
3.4 Recent OEM Highlights
-------------------------
The following are some of the recent OEM highlights:
o The Cooperative Agreement between NASA GSFC and CEA/UCB was signed
on 12 Aug, making the OEM official.
o Hiring activities for CEA's Flight Operations Team (FOT) are in
full swing and proceeding well.
o A following Government Furnished Equipment (GFE) items were
received at CEA and installed in the EUVE Platform Operations
Center (EPOC): the hardware and software for the spare Command
Management System (CMS), the software (release 3) for the
Transportable Payload Operations Control Center (TPOCC), and the
FORMATS software that interfaces between CMS and the GSFC Flight
Dynamics Facility (FDF). All of the above are now undergoing
preliminary interface tests.
---------------------------------------------------------------------------
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 archive@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, 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
to euve@stars.span.nasa.gov.
END-----------EUVE------------ELECTRONIC---------------NEWS-------------END
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