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Vol 6, No. 6                 29 Jun 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 Public GO Data Release for 1 Jul 1996
    2.2 Initial Public RAP Data Release
    2.3 2nd EUVE Source Catalog Available Via SIMBAD
    2.4 On-Line Access to EUVE
 3. 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 May
1996, conducting 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

    V824 Ara         HD 155555       K1Vp    30 Apr - 03 May 1996  ---
    AD Leo           SAO 81292       M4.5Ve  03 May - 06 May 1996  ---
    NGC 4051         UGC 7030        Sy1     06 May - 06 May 1996  ---
    EUVE J1429-38.0  --------        NOID    06 May - 06 May 1996  RAP
    EUVE J1436-38.2  --------        NOID    06 May - 06 May 1996  RAP
    Survey           --------        ----    06 May - 06 May 1996  CAL
    VW Hyi           EUVE J0409-71.2 DwNova  07 May - 10 May 1996  TOO
    EUVE J1521-16.8  --------        NOID    07 May - 10 May 1996  RAP
    MRK 421          UGC 6132        BLLac   10 May - 11 May 1996  TOO
    VW Hyi           EUVE J0409-71.2 DwNova  11 May - 14 May 1996  TOO
    EUVE J1521-16.8  --------        NOID    11 May - 14 May 1996  RAP
    PKS 2155-304     EUVE J2158-30.2 BLLac   15 May - 20 May 1996  ---
    1607-0032        --------        NeutSt  15 May - 20 May 1996  RAP
    NGC 4051         UGC 7030        Sy1     20 May - 29 May 1996  ---
    HU Aqr           EUVE J2108-05.3 CV:AM   29 May - 03 Jun 1996  ---
    1455-3330        --------        NeutSt  29 May - 03 Jun 1996  RAP
   Key to Notes:
	RAP = simultaneous Right Angle Program imaging observation
	TOO = target of opportunity
	CAL = star tracker calibration

1. EUVE Science News

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

   Drs. Martin Laming (Naval Research Laboratory), Jeremy Drake (SAO),
   and Kenneth Widing (Naval Research Laboratory) obtained and
   analyzed the EUV spectrum of the K2 dwarf star, Epsilon Eridani,
   recorded by the Extreme Ultraviolet Explorer satellite (EUVE).

    Because the EUVE spectrometer has a sufficient resolution and
   sensibility to allow studies of elemental abundances in stellar
   coronae based on individual spectral lines, Dr. Laming's team
   identified many lines from different elements in the spectrum of
   Epsilon Eridani. They used the measured relative intensities of
   these lines to investigate the emission measure (EM) distribution
   and the coronal element abundances in order to determine whether
   the FIP effect is operating or not in Epsilon Eridani.  The FIP
   effect is observed in the solar corona where elements with low
   first ionization potential (FIP) (less or equal to 10 eV) are
   overabundant by average factors of about 4 compared with elements
   with high FIP (> 10 eV).

    The EUVE data suggest that a solar-like FIP effect is in operation
   in Epsilon Eridani, although the limited number of high-FIP lines
   detected, together with the sharply peaked shape of the EM
   distribution and low signal-to-noise ratio of the spectra, preclude
   a definitive judgment according to Dr. Laming's group. However,
   they can conclude that there cannot be an enhancement of low-FIP
   species in the corona of Epsilon Eridani significantly larger than
   that seen in the average solar corona, which may imply that the
   magnitude of the FIP effect does not seem to increase with
   increasing stellar activity.

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


S.R. Rosen., J.P.D. Mittaz, D.A.H. Buckley, A.C. Layden, K.L. Clayton,
  C. McCain, G.A. Wynn, M.M. Sirk, J.P. Osborne, and M.G. Watson
To appear in Monthly Notices of the Royal Astronomical Society

   Pointed EUVE and ROSAT observations of the AM Her type binary, QS
Tel, are reported, together with complementary contemporaneous optical
measurements. The EUVE data reveal a double-peaked orbital light
curve, dramatically different from the "bright-faint" morphology seen
during the ROSAT WFC survey discovery observations, indicating that
two accretion sites were active. A deep dip is present during one of
the EUVE flux maxima and probably arises from occultation of the
emission site by the accretion flow rather than via an eclipse by the
companion star. This dip, which does not appear to be accompanied by
significant spectral hardening, possesses a slow (~300 s) ingress but
much more rapid (~40 s) egress. Both ingress and a restricted phase
interval near mid-dip are affected by strong flare-like activity.
Blackbody representations of the EUVE spectra yield a low emission
temperature ~15\tev. The inferred estimates of the soft component flux
point to a large soft/hard component flux ratio (>~ 15). However, we
also find tentative evidence of an ionization edge at 85 A and
absorption lines at 98 A and 116 A, possibly due to Ne VI, Ne VIII and
Ne VII respectively. Contemporaneous optical photometry shows the
light curve to vary substantially over 3 days but, where we have
simultaneity, there is no significant correlation between the optical
and EUV fluxes.  During the earlier ROSAT pointed observation, the
source was in a single pole mode but the intensity of the bright
interval had declined by a factor ~5 relative to the survey
observation. A counterpart to the EUVE dip was seen in both the WFC
and PSPC bands during the bright interval, the WFC event being similar
in morphology to the EUVE dip and more protracted than the PSPC dip.
Quasi-simultaneous V and I band photometry shows a broad dip centered
on the X-ray event with greater depth at red wavelengths. A hard
spectral component is detected in the ROSAT spectrum.  This collection
of observations highlights the variable behaviour of QS Tel but also
provides a rather clean, simple example of a change of accretion mode
in an AM Her system. We consider the implications of this result and
also discuss the nature of the accretion flow.


J.P. Halpern, C. Martin, and H.L. Marshall
To appear in The Astrophysical Journal.

We obtained a light curve for the 5.75 ms pulsar J0437-4715 in the
65-120 A range with 0.5 ms time resolution using the Deep Survey
instrument on the EUVE satellite.  The single-peaked profile has a
pulsed fraction of 0.27 +/- 0.05, similar to the ROSAT data in the
overlapping energy band.  A combined analysis of the EUVE and ROSAT
data is consistent with a power-law spectrum of energy index alpha =
1.2-1.5, intervening column density N_H = (5-8)E+19 cm^(-2), and
luminosity 5.0E+30 ergs/s in the 0.1-2.4 keV band.  We also use a
bright EUVE/ROSAT source only 4.2 arcmin from the pulsar, the Seyfert
galaxy RX J0437.4-4711 (= EUVE J0437-471 = 1ES 0435-472), to obtain an
independent upper limit on the intervening absorption to the pulsar,
N_H < 1.2E+20 cm^(-2).

Although a blackbody spectrum fails to fit the ROSAT data,
two-component spectral fits to the combined EUVE/ROSAT data are used
to limit the temperatures and surface areas of thermal emission that
might make partial contributions to the flux.  A hot polar cap of
radius 50-600 m and temperature (1.0-3.3)E+06 K could be present.
Alternatively, a larger region with T = (4-12)E+05 K and area less
than 200 km^2, might contribute most of the EUVE and soft X-ray flux,
but only if a hotter component were present as well.  Any of these
temperatures would require some mechanism(s) of surface reheating to
be operating in this old pulsar, the most plausible being the impact
of accelerated electrons and positrons onto the polar caps.  The
kinematically corrected spin-down power of PSR J0437-4715 is only
4E+33 ergs/s, which is an order of magnitude less than that of the
lowest-luminosity gamma-ray pulsars Geminga and PSR B1055-52.  The
absence of high-energy gamma-rays from PSR J0437-4715 might signify an
inefficient or dead outer gap accelerator, which in turn accounts for
the lack of a more luminous reheated surface such as those
intermediate-age gamma-ray pulsars may have.


J.P. Halpern and H.L. Marshall
To appear in The Astrophysical Journal.

We monitored the soft X-ray-selected Seyfert galaxy RX J0437.4-4711
with the EUVE satellite continuously for 20 days in 1994
October-November.  The Seyfert was detected in the 70-110 A range,
both in the short-wavelength spectrometer and in the Deep Survey
imager.  Its light curve shows large-amplitude variability by a factor
of 4 over the 20 day period, and a minimum doubling time of 5 hr.  Its
power spectrum in the frequency range 1E+06.0 to 1E-04.1 Hz is fitted
by a power law of slope -1.25 +/- 0.25.  A possible period of 0.906
+/- 0.018 days is also apparent in the light curve and power spectrum.
This is a timescale that might correspond to orbital motion in the
inner accretion disk around a ~1E+08 M_solar black hole.  The
divergence of the power at low frequencies indicates that even longer
observations in the EUV would be necessary to characterize the
variability of the bulk of the Seyfert luminosity.  The ROSAT PSPC
spectrum from a pointed observation of RX J0437.4-4711 in 1992
September is well fitted by a power law of energy index alpha = 1.56
+/- 0.09 and N_H = (1.01 +/- 0.16)E+20 cm^(-2).  The EUVE spectrum is
consistent with these parameters and shows no evidence of emission
lines.  We also present an IUE spectrum that reveals a flat continuum
in nu f_nu, and a Ly alpha line at z = 0.052 with FWHM ~4000 km/s.  In
all of its properties, RX J0437.4-4711 appears to be an ordinary
Seyfert 1 galaxy.


N.S. Brickhouse
To appear in proceedings of the 10th APS Topical Conference on Atomic
  Processes in Plasmas.

The EUV spectral region contains a wealth of plasma diagnostics for
stellar coronae (T_e ~5E+05 to 2E+07 K). Of particular importance for
understanding coronal structure are the observable emission lines of
highly ionized iron (Fe VIII-XXIV), which allow the determination of
electron temperatures (and the detailed temperature distributions) and
electron densities. Comparison of continuum emission and lines from
other elements with the iron lines provides diagnostics for relative
abundances in the stellar atmospheres.

Recent work in both solar and stellar coronal physics has greatly
changed our picture of the corona, with EUV spectroscopy providing
critical pieces of the puzzle. Here we discuss some important new
spectral diagnostic results, examining in particular the quality of
the theoretical atomic physics used in the data interpretation.


A.K. Dupree
To be published in Ninth Cambridge Workshop on Cool Stars, Stellar
  Systems, and the Sun (R. Pallavicini and A. K. Dupree, eds.), ASP
  Conference Series, 1996.

EUVE spectra have been analysed from a sample of binaries of RS CVn
and W UMa-type (44 iota Boo, HR 1099, UX Ari, Capella, VY Ari, and
lambda And).  Coronal material occurs at all coronal temperatures
(1E+06-1E+07.3 K).  A narrow high temperature enhancement (a "bump") is
present in the emission measure distributions for short-period (P <=
~13 d) binary systems similar to that originally found in Capella.
Previous analysis of rapidly rotating single stars revealed similar
emission measure enhancements.  Coronas of rapidly rotating stars
contain a new structure that is absent in coronas of slowly-rotating
stars like the Sun.  This structure may be the coronal manifestation
of the high-latitude or polar spots identified in the photosphere
through Doppler imaging and photometric studies.


A.K. Dupree
To appear in "UV and X-Ray Spectroscopy of Astrophysical and
  Laboratory Plasmas", Universal Academy Press.

The Extreme Ultraviolet Explorer (EUVE) satellite of NASA is acquiring
EUV spectra of cool single stars and cool stars in binary systems.
These spectra are typically dominated by iron emission lines (Fe IX to
Fe XXIV) and many spectra appear similar to the spectra obtained from
a Tokamak plasma.  Emission measure distributions derived for the
emitting plasma in stellar coronas are continuous in temperature, and
show enhancements over narrow temperature regions. Electron densities
can be high (typically ~1E+12 cm^(-3)) near 1E+07 K.


N.S. Brickhouse, A.K. Dupree, and J.C. Raymond
To be published in Ninth Cambridge Workshop on Cool Stars, Stellar
  Systems, and the Sun (R. Pallavicini and A. K. Dupree, eds.), ASP
  Conference Series, 1996.

Spectra of Capella (Alpha Aur; HD 34029) obtained with the EUVE
satellite contain a number of lines formed at transition region
temperatures. As noted by Dupree et al. (1993, ApJ, 418, L41) many of
these lines are weaker than expected from the UV line intensities, as
measured by IUE, HST, and ORPHEUS.  These results might be explained
by Lyman continuum absorption or nonequilibrium ionization associated
with flows.

Using the emission measure distribution determined from the UV lines,
we compare predictions based on ionization equilibrium models to the
observed line intensities for the summed EUVE spectrum of Capella (a
total of 2.8E+05 sec with four pointings). For example, the
discrepancies for lines from O III-VI range from factors of 3 to as
much as 20. We discuss the uncertainties for individual lines or upper
limits, which include statistics, calibration, correction for
interstellar absorption, blending, and high order flux contributions,
as well as atomic data uncertainties from the model predictions. We
also discuss the connection from the transition region to the corona,
in particular, the EUV lines which determine the minimum in the
emission measure distribution at T_e ~1E+06 K.


C.K. Mitrou, M. Mathioudakis, J.G. Doyle, and E. Antonopoulou
To appear in Astronomy & Astrophysics

We performed a study of 104 RS CVn systems in the extreme ultraviolet
(EUV) using the all-sky survey data obtained by the Extreme
Ultraviolet Explorer (EUVE). The present sample includes several new
RS CVn detections; 11 more than in the published EUVE catalogs and 8
more than in the ROSAT Wide Field Camera catalog. The ratio of
detections to non-detections remained constant throughout the sky,
implying that our detections are not limited by the exposure time but
are most likely limited by absorption from the interstellar medium. A
general trend of increasing Lex/B (50-180 A) flux with decreasing
rotational period is clear. The dwarf systems exhibit a leveling-off
for the faster rotators. In contrast, the evolved systems exhibit no
such effect. For the RS CVn systems the losses in the EUV represent a
smaller fraction of the coronal radiative losses, as compared to
active late-type dwarfs.


V.J. Foster, M. Mathioudakis, F.P. Keenan, J.J. Drake, and K.G. Widing
To appear in The Astrophysical Journal.

Theoretical electron density sensitive emission line ratios involving
Fe X 3s^2 3p^5 - 3s^2 3p^4 3d transitions in the 170-190 A wavelength
range are compared with observational data for solar active regions
and flares, obtained during the Skylab mission, and alpha Cen and
Procyon observations from the Extreme Ultraviolet Explorer (EUVE)
satellite.  Electron densities derived from the majority of the ratios
are consistent for the events, but in poor agreement with the values
of Ne estimated from diagnostic lines in other species observed in the
spectra, casting doubt on the accuracy of the theoretical line ratio
calculations and hence the atomic data of Mohan et al. used in their
derivation.  At low Ne, the present ratios are significantly different
from those of Young et al., while the latter imply densities that are
in somewhat better agreement with densities derived from other
diagnostics.  This would appear to indicate that the electron impact
excitation rates of Bhatia & Doschek adopted by Young et al. are to be
preferred over the Mohan et al. results.


J. Vallerga
To appear in "The Heliosphere in the Local Interstellar Medium",
  ed. R. von Steiger, R. Lallement, and M. Lee, Space Science Reviews,
  1996.  [CEA publication #742]

Because of the strong absorption of extreme ultraviolet radiation by
hydrogen and helium, almost every observation with the Extreme
Ultraviolet Explorer (EUVE) satellite is affected by the diffuse
clouds of neutral gas in the local interstellar medium (LISM).  This
paper reviews some of the highlights of the EUVE results on the
distribution and physical state of the LISM and the implications of
these results with respect to the interface of the LISM and the
heliosphere.  The distribution of sources found with the EUVE all-sky
surveys shows an enhancement in absorption toward the galactic center.
Individual spectra toward nearby continuum sources provide evidence of
a greater ionization of helium than hydrogen in the Local Cloud with
an mean ratio of H I/He I of 14.7.  The spectral distribution of the
EUV stellar radiation field has been measured, which provides a lower
limit to local H II and He II densities, but this radiation field
alone cannot explain the local helium ionization.  A combination of
EUVE measurements of H I, He I, and He II columns plus the measurement
of the local He I density with interplanetary probes can place
constraints on the local values of the H I density outside the
heliosphere to lie between 0.15 and 0.34 cm^(-3) while the H II
density ranges between 0.0 and 0.14 cm^(-3).  The thermal pressure
(P/k = nT) of the Local Cloud is derived to be between 1700 and 2300
cm^(-3) K, a factor of 2 to 3 above previous estimates.

R. Battle and I. Hawkins
To appear in The Journal of Science Education and Technology.  [CEA
  publication #741]

In this paper we describe two aspects of an Internet-based lesson plan
development project called "Science On-Line-Earth and Space Science
for the Classroom."  First, we discuss the design of the Science
On-Line (SOL) Project, which focuses on building a community of
practice, appropriate task and setting, and contact with the
scientific workplace. Second, we examine strategies teachers used as
they approached the task of creating Internet-based science lesson
plans for the World Wide Web. Based on the analysis of data gathered
during the various project phases, results show that the
teacher-developed strategies have varying degrees of effectiveness in
facilitating Internet-based lesson plan design, information-gathering,
and organization. We describe how the strategies began to evolve into
formulated practices for Internet-based lesson development within the
SOL teacher community. The SOL investigation develops a case study of
the strategies and emerging practices in the context of the creation
and pilot-testing of Internet-based lesson plans. This case study may
serve as an exemplar of tested Internet-based lesson development
strategies and practices for the educational community.


J.H.M.M. Schmitt, J.J. Drake, and R.A. Stern
Astrophysical Journal Letters, 465, L51.  [CEA publication #739]

A challenge to the classical assumption that the radiative losses from
stellar coronae are optically thin has been raised by Schrijver, van
den Oord, & Mewe, who argued that some of the stronger emission lines
detected in the high-resolution spectra of cool stars observed with
the Extreme Ultraviolet Explorer (EUVE) satellite are optically
thick. If they assume all radiation optically thin, an explanation of
the short-wavelength (SW) part of the EUVE spectrum requires large
amounts of emission measure at very high temperatures (T ~1E+08 K),
which is unlikely the case for rather inactive stars. We show that the
soft X-ray pulse height spectrum obtained with the Position Sensitive
Proportional Counter (PSPC) on board ROSAT is inconsistent with such
high-temperature emission and inconsistent with the assumption that
the EUV line emission is optically thick. We further demonstrate via
an analysis of fit residuals that the observed count fluctuations in
the EUVE SW spectrum are inconsistent with the hypothesis that the
bulk of the observed flux arises from a continuum. Therefore,
resonance scattering does not appear to be required for the
interpretation of the EUV and X-ray spectra of inactive cool stars.


I. Crawford, N. Craig, and B. Welsh
To appear in Astronomy & Astrophysics.  [CEA publication #738]

We present ultra-high-resolution (0.35 km/s FWHM) observations of the
interstellar Ca K line towards eight nearby stars (six of which are
closer than 30 pc). The spectral resolution is sufficient to resolve
the line profiles fully, thereby enabling us to detect hitherto
unresolved velocity components, and to obtain accurate measurements of
the velocity dispersions (b-values).  Absorption components due to the
Local Interstellar Cloud (LIC) and/or the closely associated "G Cloud"
are identified towards all but one star (gamma Oph), but only in one
case (51 Oph) are both clouds reliably detected towards the same
star. Most of these nearby clouds have velocity dispersions (b ~2
km/s) which suggest physical conditions similar to those inferred for
the LIC (T_k ~7000 K, v_t ~1 km/s), although at least three lines of
sight (towards gamma Aqr, beta Cen and rho Cen) also sample cooler
and/or less turbulent material. The spectrum of the nearby Vega-excess
star 51 Oph is of particular interest, owing to evidence that several
of the absorption components arise in the circumstellar environment.


2. EUVE Science Operations News

2.1 Public GO Data Release for 1 Jul 1996
        by Dr. Nahide Craig, EUVE User Support Scientist

   The table below lists the GO observations that become public on 1
Jul 1996.  For each entry is given the target name, the approximate
exposure time in ksec, the GMT start and end dates for the
observation, the spectral type of the target, and the data
identification code.  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 DataIDs of interest.
Processed data sets are shipped on 8mm tape (or, if requested, on
CD-ROM) via postal mail.

   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

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

     GO Data Sets Available 1 Jul 1996:

     Moon              2    27 Mar - 27 Mar 1994     SolSys   go0320 
     Moon              2    16 Sep - 16 Sep 1994     SolSys   go0321	
     Moon              1    23 Sep - 23 Sep 1994     SolSys   go0322 
     Moon              1    13 Oct - 13 Oct 1994     SolSys   go0323 
     Moon              2    11 Feb - 11 Feb 1995     SolSys   go0324	
     Moon              1    17 May - 17 May 1995     SolSys   go0325 
     Feige 24         38    22 Jan - 24 Jan 1995     WD:DA    go0326	
     EUVE J1147+025   35    26 May - 27 May 1995     NOID     go0327	
     EUVE J1636-285   44    28 May - 30 May 1995     NOID     go0328 
     31 Com          100    17 Apr - 20 Apr 1995     G0IIIp   go0329 
     31 Com          100    20 Apr - 24 Apr 1995     G0IIIp   go0330 
     31 Com           33    24 Apr - 25 Apr 1995     G0IIIp   go0331 
     Jupiter         100    30 May - 02 Jun 1995     SolSys   go0332 
     Jupiter          40    02 Jun - 04 Jun 1995     SolSys   go0333
     RE 1307+53      100    15 May - 18 May 1995     CV       go0334 
     RE 1307+53      100    18 May - 22 May 1995     CV       go0335 
     RE 1307+53       76    22 May - 25 May 1995     CV       go0336 
     MRK 421         100    25 Apr - 28 Apr 1995     BLLac    go0337
     MRK 421         100    28 Apr - 02 May 1995     BLLac    go0338	
     MRK 421         100    02 May - 06 May 1995     BLLac    go0339 
     MRK 421           4    06 May - 06 May 1995     BLLac    go0340 
     EUVE J1032+534  100    07 Apr - 10 Apr 1995     WD:DA    go0341 
     EUVE J1032+534  100    10 Apr - 14 Apr 1995     WD:DA    go0342
     EUVE J1032+534   29    14 Apr - 15 Apr 1995     WD:DA    go0343	
     BE UMa           51    15 Apr - 17 Apr 1995     CV       go0344 
     PG 1116+215      16    27 May - 28 May 1995     QSO      go0345
     M 87             11    25 May - 25 May 1995     Gal      go0346
     M 87             25    25 May - 26 May 1995     Gal      go0347
     epsilon CMa      68    04 Apr - 07 Apr 1995     B2Iab    go0348 *
     GD 246            4    22 Nov - 22 Nov 1995     WD:DA    go0349 *
     Sco X-1          58    28 Jun - 30 Jun 1995     LMXB     go0350 *
     HZ 43            30    06 Jun - 07 Jun 1995     WD:DA    go0351 *
     HZ 43            56    05 Jun - 07 Jun 1996     WD:DA    go0352 *

     * --> calibration observation

     NOTE: Observation dates for UZ For (go0315) and 3C 273 (go0319)
     were incorrectly listed in the previous issue of the newsletter
     (V6#5, 31 May 1996).  The correct listings are as follows:

     3C 273           46    03 Jan - 15 Jan 1995     QSO      go0319
     UZ For          107    15 Jan - 19 Jan 1995     CV:AM    go0315 


2.2 Initial Public RAP Data Release
        by Dr. Nahide Craig, EUVE User Support Scientist

This month's newsletter initiates the public release of EUVE
right-angle-program (RAP) data; proprietary data rights for RAP
observations are six months.  The RAP data contain imaging
observations of targets made with the scanning telescopes; since the
scanners are mounted at right angles to the deep survey/spectrometer
(DS/S) telescope, the RAP data are obtained simultaneously during
primary GO observations with the DS/S.  CEA will now be making monthly
releases of RAP data in addition to the monthly GO releases.  All
public RAP data can be ordered from the EUVE archive in the same
manner as indicated above for GO data.

CEA would like to remind the community that the RAP is a simple and
easy way for researchers to propose for and obtain long-exposure EUVE
imaging data.  For more information on the Public RAP and the simple
proposal process please see the RAP Proposal Submission Guidelines
available via the WWW at the URL

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

     RAP Data Sets Available 1 Jul 1996:

     LHS 2034  	       6    19 Jan - 19 Jan 1995     M        rap0001
     0837+0610        38    22 Jan - 24 Jan 1995     NeutSt   rap0002
     EUVE J0834+040   38    22 Jan - 24 Jan 1995     NOID     rap0003
     0459-02         150    24 Jan - 30 Jan 1995     NeutSt   rap0004
     MRK 421         108    04 Feb - 07 Feb 1995     BLLac    rap0005
     1235+269 	      63    03 Mar - 05 Mar 1995     AGN      rap0006
     1239+245  	      63    03 Mar - 05 Mar 1995     NeutSt   rap0007
     WGA J1231+25     63    03 Mar - 05 Mar 1995     AGN      rap0008
     LHS 2471 	     128    08 Mar - 13 Mar 1995     M+       rap0009
     EUVE J1254-70.3 180    13 Mar - 19 Mar 1995     NOID     rap0010
     EUVE J1436-38.2 100    22 Mar - 04 Apr 1995     NOID     rap0011
     EUVE J1429-38.0 350    22 Mar - 04 Apr 1995     NOID     rap0012
     EUVE J1355-249  229    07 Apr - 15 Apr 1995     NOID     rap0013
     Cen X-4         207    17 May - 25 May 1995     LMXB     rap0014
     1455-333        207    17 May - 25 May 1995     NeutSt   rap0015
     1304+310  	       3    27 May - 27 May 1995     AGN      rap0016
     WGA J1319+30      3    27 May - 27 May 1995     AGN      rap0017 
     EUVE J1529-471   16    27 May - 28 May 1995     NOID     rap0018
     cmaNGC4051      139    30 May - 04 Jun 1995     AGN      rap0019
     EUVE J1706-450   32    06 Jun - 07 Jun 1995     NOID     rap0020
     PKS 2005-489     43    21 Jun - 22 Jun 1995     AGN      rap0021
     1713+0747        42    23 Jun - 24 Jun 1995     NeutSt   rap0022
     EUVE J2041-368  113    24 Jun - 28 Jun 1995     NOID     rap0023
     cmaIH2032-358   113    24 Jun - 28 Jun 1995     AGN      rap0024
     EUVE J2329-477   59    28 Jun - 30 Jun 1995     NOID     rap0025
     RE J2334-471     59    28 Jun - 30 Jun 1995     WD:DA    rap0026
     1932+1059 	       9    30 Jun - 01 Jul 1995     NeutSt   rap0027
     EUVE J1854-324   92    02 Jul - 05 Jul 1995     NOID     rap0028
     EUVE J1947-110  200    08 Jul - 15 Jul 1995     NOID     rap0029
     EUVE J2041-368    3    18 Jul - 18 Jul 1995     NOID     rap0030
     cmaIH2032-358     3    18 Jul - 18 Jul 1995     AGN      rap0031
     RX J2117.1+3412 155    24 Jul - 29 Jul 1995     Star     rap0032
     EUVE J2142-549   99    05 Aug - 09 Aug 1995     NOID     rap0033
     2155-56         101    05 Aug - 09 Aug 1995     NeutSt   rap0034
     EUVE J2231+017  179    16 Aug - 23 Aug 1995     NOID     rap0035
     1857+0943        50    04 Sep - 05 Sep 1995     NeutSt   rap0036
     M 15            161    13 Sep - 18 Sep 1995     GlClus   rap0037
     EUVE J0122-603  230    27 Sep - 05 Oct 1995     NOID     rap0038
     EUVE J2010+42.6  20    05 Oct - 06 Oct 1995     NOID     rap0039
     EUVE J2013+400   20    05 Oct - 06 Oct 1995     WD       rap0040
     RX J2117.1+3412 196    06 Oct - 19 Oct 1995     Star     rap0041
     0304+1932        34    30 Oct - 31 Oct 1995     NeutSt   rap0042


2.3 2nd EUVE Source Catalog Available Via SIMBAD
        by Dr. Nahide Craig, EUVE User Support Scientist

CEA is pleased to inform readers that the 2nd EUVE Source Catalog
(Bowyer, et al., Astrophysical Journal Supplement, 102, 129-160, 1996)
is now available, with cross-identifications, via the SIMBAD database.
CEA would like to thank the SIMBAD team for their cooperation in
making the EUVE material available on-line for use by the research
community.  The SIMBAD database can be reached via WWW at URL

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)
   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)

3.0 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 onboard 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
multimission 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. R.F. Malina
  and Professor S. Bowyer.  Newsletter Editor: B.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. G. Riegler, Program Manager.  Information on
  the EUVE GO Program is available from Dr. Y. Kondo, Mail Code 684,
  GSFC, Greenbelt, MD 20771 at (301) 286-6247 or e-mail to

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