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ELECTRONIC NEWSLETTER OF THE EUVE OBSERVATORY
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Vol 5, No. 9 25 Sep 1995 ISSN 1065-3597
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Notes from the Editor
=====================
by Brett A. Stroozas, ISO Manager
Welcome to the electronic newsletter for NASA's Extreme Ultraviolet
Explorer (EUVE) satellite, compiled and published monthly by the
Integrated/Intelligent Science Operations (ISO) group at the Center for
EUV Astrophysics (CEA) at the University of California, Berkeley (UCB).
The contents of this issue of the EUVE electronic newsletter are as
follows:
1. Science News
1.1 Recent EUVE Science Highlights
1.2 Abstracts or Recently *Accepted* EUVE Papers
2. Science Operations News
2.1 Cycle 4 GO Proposals Due 6 Oct 1995
2.2 NRA Appendix E: Update on Observations
2.3 New On-Line Search Tools for Proposal Database
2.4 New Version of EUVE Software User's Guide
2.5 New EGO Center Software Status WWW Page
2.6 Spiral Dithering Test Results
2.7 Cycle 3 Observation Scheduling Status Report
2.8 Public Data Release for 1 Oct 1995
2.9 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 ceanews@cea.berkeley.edu (Internet).
The EUVE observatory performed well throughout the month of August,
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
===================================================================
RE 2324-544 EUVE J2324-546 DA 29 Jul - 05 Aug 1995 ---
ER Vul HD 200391 G0V+ 29 Jul - 05 Aug 1995 RAP
II Peg HD 224085 K0V 05 Aug - 07 Aug 1995 ---
2155-56 -------- NeutSt 05 Aug - 07 Aug 1995 RAP
MOON -------- SolSys 07 Aug - 07 Aug 1995 ---
II Peg HD 224085 K0V 07 Aug - 09 Aug 1995 ---
2155-56 -------- NeutSt 07 Aug - 09 Aug 1995 RAP
HR 120 HD 2726 F2V 09 Aug - 16 Aug 1995 ---
VW HYI RE 0408-711 CVDN 16 Aug - 23 Aug 1995 ---
GD 984 WD 0131-164 DA 23 Aug - 31 Aug 1995 ---
epsilon Eri HD 22049 K2V 31 Aug - 04 Sep 1995 ---
===================================================================
Key to Notes:
RAP = simultaneous Right Angle Program (RAP) imaging observation
1. Science News
===============
1.1 Recent EUVE Science Highlights
----------------------------------
by Dr. Antonella Fruscione, EUVE Scientist
S. Rosen (Leicester), J. Mittaz (Mullard Space Science Laboratory),
D. Buckley (South African Astronomical Observatory), A. Layden (Cerro
Tololo Inter-American Observatory), C. McCain (Mt. Stromlo
Observatory), J.P. Osborne (Leicester) and M. Watson (Leicester)
report on the first detailed EUVE observations of the AM Her star, QS
Telescopii.
This AM Her binary contains a strongly magnetic white dwarf
accreting material from a cool companion star. Our EUVE observations
of the star found it in a bright state, displaying a double peaked EUV
light curve, indicative of accretion onto two poles. This contrasts
with the single peaked (single pole) light curves of earlier ROSAT
observations and the very faint, weakly accreting state observed in
early (IOC and survey) EUVE data. The change in accretion geometry is
probably related to a higher mass transfer rate and may reflect the
ability of dense filaments within the accretion flow to penetrate the
magnetic field and reach the second pole which is inaccessible when
the accretion rate (filament density) is lower.
The EUVE data also uncovered a deep orbital dip in the light curve,
most probably caused when the accretion flow between the stars occults
the EUV emission region. The lack of a strong energy dependence in
the dip profile disfavours photoelectric absorption by cold material
but may be consistent with partial covering by opaque blobs/filaments
in the flow.
The EUVE spectrum is consistent with a low temperature (~15eV)
blackbody-like distribution, suggesting a very large bolometric soft
X-ray flux and hence a large ratio of the fluxes of the soft and hard
spectral components. However, we also find tentative evidence of an
edge at 85 A and absorption lines at 98 A and 116 A due, perhaps, to
Ne VI, Ne VIII, and Ne VII respectively. If confirmed, the range of
ionization states observed and the absence of a strong O VI edge raises
important questions about the heating mechanism in the accretion region.
Further monitoring of this star by EUVE and X-ray satellites may
provide improved insights into the cause of accretion mode changes in
AM Her stars and on the properties of the accretion flow.
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
scientists, the EUVE 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 Home
Page. Please send all abstracts or preprints to
archive@cea.berkeley.edu.
--------------------------------------------------------------
THE STEEP SOFT X-RAY SPECTRUM OF THE HIGHLY VARIABLE ACTIVE NUCLEUS
IN MRK 478
H.L. Marshall, T.E. Carone, J. Michael Shull, M.A. Malkan, and M. Elvis
To appear in The Astrophysical Journal.
We present the first moderate resolution spectrum of the soft X-ray
excess in an active galactic nucleus. Mrk 478 was detected in the
70-100 A spectral region using the Extreme Ultraviolet Explorer (EUVE)
Spectrometer. The spectrum shows no significant spectral features and
is consistent with a very steep power law. The neutral hydrogen
absorbing column is consistent with the Galactic value. The spectral
slope is poorly determined if the absorbing column is allowed to vary;
alpha = 27 +/- 9 (f_nu is proportional to nu^(-alpha)) and the best-fit
column density (cm^(-2)) is log N_H = 20.6. If the column density is
fixed at the Galactic value, log N_H = 20.0, then alpha = 4.70 +/- 0.65.
The lack of emission lines and significant variability indicate
that the soft X-ray continuum is not due to emission from a thin
thermal plasma or a leaky neutral or warm absorber. There is marginal
evidence that the spectrum hardens as it brightens, which is consistent
with thermal variations rather than absorption changes. If this component
is the Wien tail of a blackbody spectrum, then the temperature at the
inner edge of the accretion disk must be of order 1E6 K. For an accretion
disk model from Sun & Malkan (1991), we require a mass of 1.3E8 M_sun,
an accretion rate of 0.3 M_sun/yr and a highly inclined disk, with
cos i = 0.50, in order to keep L < L_Edd.
--------------------------------------------------------------
EUVE SPECTROSCOPY OF BETA CANIS MAJORIS (B1 II-III) FROM 500 A TO 700 A
J.P. Cassinelli, D.H. Cohen, J.J. MacFarlane, J.E. Drew, A.E. Lynas-Gray,
I. Hubeny, J.V. Vallerga, B.Y. Welsh, and M.G. Hoare
To appear in The Astrophysical Journal.
Observations of the bright variable star beta CMa (B1 II-III) made
with the Extreme Ultraviolet Explorer (EUVE) are presented. We report
on the continuous energy distribution, photospheric line identification,
and the variability of the star, as well as the physical implications
for the structure of the local interstellar medium. The star is one of
the strongest EUV sources in the long wavelength spectrometer of EUVE,
and one of only two early-type stars whose photospheric continuum was
detected by the EUVE spectrometers. This paper is primarily concerned
with the portion of the spectrum that lies between the neutral helium
ionization edge at 504 A and an effective cutoff by interstellar absorption
near 700 A. As in our EUV analysis of the B2 II star epsilon CMa, we
found that line-blanketed model atmospheres are not capable of predicting
an energy distribution which matches observations in all wavelength regions.
Consequently, we derived two set of basic parameters for the star (T_eff
= 24,800 K, log g = 3.7; and T_eff = 23,250 K, log g = 3.5), depending
whether we accept the measured angular diameter, or require an exact
agreement between models and the observed visual flux. For the higher
T_eff model, the predicted EUV flux is in agreement with observations,
while for the the lower T_eff the star's EUV continuum is about 5 times
brighter than the predictions. In either case, the star does not show the
order of magnitude EUV excess that was seen in epsilon CMa. Neither model
fits the data near 2200 A, and additional photospheric opacity is proposed.
The EUVE data also provide information concerning the low density
interstellar medium in the direction of beta CMa. We derive a neutral
hydrogen column density of ~2E18 cm^(-2) and estimate a lower limit for
the neutral helium column density of 1.4E18 cm^(-2). This indicates that
along this sight line much of the hydrogen is ionized while the helium
is neutral. The EUVE spectrum shows many strong photospheric absorption
features, similar to that of epsilon CMa. Evidence for a stellar wind is
seen in the O V 630 A absorption feature.
There is special interest in beta CMa because it is among the brightest
of the beta Cephei class of variables. The pulsations in this class of
star manifest themselves primarily as periodic effective temperature
changes. We find that the semi-amplitude of the change is 108 (-32/+31) K
for the primary period. This result is consistent with that derived from
an an analysis of the UV continuum by Beeckmans & Burger (1977), but our
68% confidence limits are significantly smaller than their 1 sigma error
bars. The general agreement implies that the pulsations do propagate
between the layers where the optical and UV continua are formed and the
layers where the EUV continuum forms, which is about six density scale
heights higher in static models. The possibility that some pulsational
energy deposition could occur within the outer photosphere is discussed.
Our observations, taken over two time intervals separated by 70 days,
resulted in the detection of the beat phenomenon owing to the three
oscillation periods of beta CMa.
--------------------------------------------------------------------
EVIDENCE FOR WIND ATTENUATION AND A MULTI-TEMPERATURE PLASMA IN THE
COMBINED EUVE AND ROSAT OBSERVATIONS OF EPSILON CANIS MAJORIS (B2 II)
D.H. Cohen, R.G. Cooper, J.J. MacFarlane, S.P. Owocki, J.P. Cassinelli,
and P. Wang
To appear in The Astrophysical Journal.
We use both EUVE and ROSAT data sets to test three general pictures --
coronal, wind shock, and external -- for the production of the observed
high energy emission from the B giant, epsilon CMa (B2 II). Because of
the very low interstellar opacity along its line of sight, epsilon CMa
is the only early-type star that has strong emission lines detected with
the EUVE spectrometers. The line spectrum provides the first solid
observational evidence that the emission is thermal. Theoretical EUV
spectra based upon two-temperature model fits to the ROSAT data predict
too much flux, especially in the iron line complex near 175 A. We use
progressively more complex models until we are able to achieve a fit to
the combined data sets. We find that both a temperature distribution
in the emitting plasma and some attenuation of the EUV and soft X-ray
emission by the ionized stellar wind must be included in the models. The
model fitting indicates that only 13 to 21 percent of the emission line
complex near 175 A escapes the wind. This amount is consistent with the
wind shock model, in which the emitting material is distributed throughout
the stellar wind. It is much more absorption than is predicted by the
external source model, where all of the emitting material is at radii
beyond the cold stellar wind. And it is significantly less absorption
than is expected in the coronal model, given what is known about the
star's mass loss rate. The derived temperature distribution and wind
filling factor of hot gas are also qualitatively consistent with our
numerical simulations of wind shocks. We conclude that although the
observed flux from epsilon CMa in the interval 54 eV < E < 100 eV is
approximately the same as that above 100 eV, because of wind attenuation
the total generated radiation in the EUV band between 54 eV and 100 eV
is 5 times greater than that in the X-ray region.
--------------------------------------------------------------
X-RAY SELECTED EUV GALAXIES: SCRAPING THE BOTTOM OF THE "INVISIBLE" BARREL
A. Fruscione
To appear in The Astrophysical Journal. [CEA publication #670]
Using data from the public archive of the Extreme Ultraviolet
Explorer (EUVE) all-sky survey, we have systematically searched for
extreme ultraviolet (EUV) emission (58-174 A, 0.07-0.21 keV) around
approximately 2500 distinct positions in the sky corresponding to
known X-ray emitting extragalactic sources. We find that 20 X-ray
galaxies are EUV bright and were detected with a significance above 4
sigma during the EUVE survey: 8 are reported here for the first time
(MS 0037.7-0156, Mrk 142, M 65, EXO 1128.1+6908, M 87, Mrk 507, PKS
2005-489, and 1H 2351-315.A). Sixty-eight additional galaxies are
detected with a lower significance (3 < sigma < 4), but the list is
affected by a high percentage of spurious sources. We comment on the
properties of the eight new EUV galaxies (six Seyfert galaxies and two
BL Lacertae objects) and discuss their possible spectral shapes at EUV
wavelengths.
--------------------------------------------------------------
THE FIP EFFECT AND ABUNDANCE ANOMALIES IN LATE-TYPE STELLAR CORONAE
J.J. Drake, J.M. Laming, and K.G. Widing
To appear in Proceedings of IAU Colloquium 152, "Astrophysics in the
Extreme Ultraviolet", ed. S. Bowyer and R.F. Malina (Dordrecht:
Kluwer), 1995. [CEA publication #671]
"Yes, it will be a long time before people know what I know. How
much of iron and other metal there is in the sun and the stars is
easy to find out, but anything which exposes our swinishness is
difficult, terribly difficult" (Tolstoy 1889).
In the solar corona, the abundances of elements appear to differ from
the photospheric values in a manner related to the element first ionization
potential (FIP): species with FIP <= 10 eV are observed to be enhanced
relative to the photosphere by factors of ~3-4. The first studies of stellar
coronal composition with EUVE suggest that some stars exhibit a solar-like
FIP effect, whereas others do not. We briefly review the latest results,
and we argue that element abundance anomalies, such as the FIP effect, can
provide potentially powerful new coronal diagnostics. Moreover, knowledge
of the composition of a stellar corona is crucial for interpreting its
spectrum -- for understanding its structure and energy balance, and for
testing its possible heating mechanisms: We must begin to understand coronal
abundance anomalies and the compositions of active stars in order to begin
to understand their coronal physics.
--------------------------------------------------------------
ELEMENT ABUNDANCES IN STELLAR CORONAE
J.J. Drake, J.M. Laming, and K.G. Widing
To appear in Proceedings of IAU Colloquium 153, "Magnetodynamic Phenomena
in the Solar Atmosphere: Prototypes of Stellar Activity", held at Makuhari,
Japan, May 22-26, 1995. [CEA publication #672]
About two years ago, the intrigue of the solar "FIP Effect" -- that
coronal abundances of elements with a low FIP (~< 10 eV; e.g Fe, Mg, Si,
Ca) are observed to be enhanced relative to those of high FIP elements
(~> 10 eV; e.g. O, Ne, S; see e.g., the review by Meyer 1993) -- prompted
us to study stellar coronal abundances based on new EUV spectra obtained
with the Extreme Ultraviolet Explorer (EUVE). Our results to-date indicate
that some stars appear to show a solar-like FIP Effect, whereas others do
not (Drake et al., 1995abc; Laming et al., 1995ab).
--------------------------------------------------------------
DETECTION OF THE FIP EFFECT IN THE CORONA OF ALPHA CENTAURI
J.J. Drake, J.M. Laming, and K.G. Widing
Presented at the 11th Colloquium on UV and X-ray Spectroscopy of
Astrophysical and Laboratory Plasmas, held at Nagoya, Japan, May 29
- Jun 2, 1995. [CEA publication #673]
An analysis of intensity ratios of lines due to species with high and
low first ionization potentials (FIP) measured from Extreme Ultraviolet
Explorer (EUVE) spectra of the nearby binary alpha Cen AB (G2 V, K0 V)
suggest that the FIP effect appears to be operating in the dominant
coronal emission. A recent EUVE observation of alpha Cen carried out
with a satellite roll angle designed to separate maximally the two
components in the MW spectrometer indicates that the stars are approximately
of equal brightness at temperatures up to log T ~6, while at higher
temperatures alpha Cen B is brighter than alpha Cen A by about a factor
of two.
--------------------------------------------------------------
THE MRK 421 MULTIWAVELENGTH CAMPAIGN: EUVE OBSERVATION
A. Fruscione, F. Bruhweiler, K.P. Cheng, C.R. Hall, M. Kafatos, E. Ramos,
and Y. Kondo
Presented at the 11th Colloquium on UV and X-ray Spectroscopy of
Astrophysical and Laboratory Plasmas, held at Nagoya, Japan, May 29
- Jun 2, 1995. [CEA publication #675]
We present the extreme ultraviolet (EUV) spectrum and light curve of the
BL Lacertae object Markarian 421, obtained with the Extreme Ultraviolet
Explorer (EUVE). The EUVE observation was part of a large multiwavelength
campaign covering radio to gamma-ray energies. Preliminary analysis of the
EUV spectrum indicates a smooth continuum in the 75-115 A range with no
evidence of absorption features. The light curve shows variability of up
to factors of two on a time-scale of a few days.
--------------------------------------------------------------
2. Science Operations News
==========================
2.1 Cycle 4 GO Proposals Due 6 Oct 1995
---------------------------------------
by Dr. Ron Oliversen, EUVE Associate Project Scientist
The is a reminder that the EUVE Cycle 4 GO Proposals are due on 6 Oct
1995. Proposals are being solicited for observations during an 11-month
period starting in February 1996. Proposals are being accepted for using
the EUVE spectrometer, the deep-survey instrument, and the scanning
telescopes.
There are several modifications from the 3rd episode including the
following:
(1) The scheduling of time critical observations will be more constrained.
The response time for a Target of Opportunity will also be affected.
(2) The data proprietary period has been decreased to six months.
(3) Large Research Programs are being encouraged and will be scheduled
through the end of mission (Sept 1997).
(4) GO grant money is available at approximately half the amount of previous
episodes.
(5) No budget page or institutional signature are required to be submitted
at this stage.
The NRA and associated appendices may be obtained via anonymous file transfer
protocol (ftp) from ftp.cea.berkeley.edu (under the directory /pub/nra95),
or hard copies may be requested from the Project Science Office at
euve@stars.gsfc.nasa.gov. Additional information about this NRA or EUVE may
be obtained from Dr. Ronald J. Oliversen, EUVE Associate Project Scientist
(oliversen@stars.gsfc.nasa.gov), Dr. Damian Christian, EUVE GO Support
Scientist (egoinfo@cea.berkeley.edu), or on the CEA WWW site
(http://www.cea.berkeley.edu/).
2.2 NRA Appendix E: Update On Observations
-------------------------------------------
by Anne Miller-Bagwell, EGO Center Technical Writer
Appendix E of the current EUVE NRA, "LIST OF EUVE OBSERVATIONS", has
been updated by GO scientist Dr. Damian Christian to include approved
scheduling for observations through 13 Oct. As before, the exposure times
for targets not yet observed are as awarded by NASA, and cannot be guaranteed.
Copies of the updated appendix are now available on the CEA ftp site
(directory /pub/nra95/) and on the CEA WWW site.
2.3 New On-Line Search Tools for Proposal Database
--------------------------------------------------
by Holly Jessop, Research Associate, ISO User Support Team
Access to the EUVE proposal database has been significantly improved
with the introduction of a new on-line search service. Users may now
search the database by any of six EUVE target criteria: object type
(e.g., White Dwarf), spectral type (e.g., DA), position (equatorial or
galactic coordinates), target name (includes stellar aliases), dithering
mode (none, raster, or spiral), and data collection mode (XY or WSZ).
The service returns target name, position, spectral type, and the unique
EUVE GO proposal identifier associated with the target. This search
capability should facilitate the location of information regarding approved
GO proposals and their targets, and should be especially useful for those
researchers preparing proposals in response to the Cycle 4 NRA. This
service is accessible from CEA's WWW site.
2.4 New Version of EUVE Software User's Guide
---------------------------------------------
by Anne Miller-Bagwell, EGO Center Technical Writer
Version 1.5 of the EGO Center Software User's Guide was released on
15 Sep. The Guide is available now on the CEA ftp site (directory
/pub/documents/docs1.5) as a set of compressed PostScript files or as a
single tarfile. The revised Guide brings the documentation up to date
with the current release of the IRAF/EUV guest observer software, and
includes descriptions of the following new tasks:
o qpmkim -- makes spectral images from QPOE files, with deadtime correction
o divea -- divides spectra by effective order to produce them in flux units
o suborder -- subtracts higher order contributions from spectra
The following tasks, which have been changed extensively since version 1.4,
are also fully documented:
o specmod -- creates simulated EUVE spectra from models
o euvextract -- extracts EUVE spectra from a user defined aperture
o compspec -- does statistical comparisons on spectra
Version 1.5 of the Guide also contains improved documentation for all the
IRAF/EUV tasks, plus examples of creating data quality filters, extracting
EUVE spectra, and more. Copies are being mailed to all Cycle II and III
GOs.
2.5 New EGO Center Software Status WWW Page
-------------------------------------------
The EUVE Guest Observer Center has a new WWW page that contains current
status information and links to the IRAF/EUV GO software available on the
CEA ftp site. Links to release notes provide information on changes, bugs,
and patches for each version of the software. This page is still under
construction, so please send us your comments and requests using the egoinfo
mail link at the bottom of the page.
2.6 Spiral Dithering Test Results
---------------------------------
A test observation of the calibration source HZ43, made with a new
spiral dithering pattern, have been analyzed and the results released.
The new pattern allowed the spacecraft pointing to drift through roughly
4.5 turns of an Archimedes spiral during an observation of 30 ksec. The
signal to noise ratio (S/N) of the resulting spectra were compared to
those from a single-pointing observation and to a superposition of three
randomly dithered observations. The resulting S/N for all spectra are
shown below with the S/N expected from pure Poisson statistics, along
with the exposure times for each. Exposures are rounded to the nearest
ksec.
------------------------------------------------------------------
| S/N | Exposure
Observation | SW MW LW | SW MW LW
| 120-130 A 183-203 A 310-325 A | (ksec)
------------------------------------------------------------------
dithering | 24 14 14 | 38 29 27
(Poisson) | 32 40 68 |
------------------------------------------------------------------
random dither | 50 49 33 | 143 131 133
(Poisson) | 62 73 112 |
------------------------------------------------------------------
Spiral dither | 28 30 39 | 29 29 27
(Poisson) | 28 33 48 |
------------------------------------------------------------------
The spiral dither pattern seems to be the most efficient method to
date for eliminating the fixed pattern noise in bright continuum spectra.
Spiral dithering was found to introduce a time variability of about 20% in
the MW and LW spectra, which is probably due to the changing transmission
of the collimators as the spiral moves the target off boresight. This
effect is similar to variations seen in randomly dithered observations as
well. Since the collimator transmissions are well-calibrated, it should
be possible for EUVE scientists to produce a time-dependent correction for
the variation.
2.7 Cycle 3 Observation Scheduling Status Report
------------------------------------------------
by Dave Meriwether, Science Planner, ISO Observation Support Team
The table below indicates the status of the scheduling for all Cycle
3 EUVE observations. For each type of observation -- Type I (guaranteed
to be observed) and II (not guaranteed to be observed) -- is given the
number of, as well as the available time (in megasec; Msec) for, these
observations. These categories are further broken down by those scheduled
and available, along with the ratio (percentage) of the two.
CYCLE 3 OBSERVATIONS: SCHEDULED VS. TOTAL
--------------------------------------------
Observations Time (Msec)
--------------------------------------------
Type I 30 70 43% 3.6 6.7 54%
Type II 22 62 35% 1.8 5.0 37%
--------------------------------------------
Totals 52 132 39% 5.4 11.7 46%
--------------------------------------------
For example, 43% (30 out of 70) of all approved Type I observations have
been scheduled to date, amounting to 3.6 Msec -- 54% of the available
Type I time for the year.
It is expected that EUVE will observe 100% of all Cycle 3 Type I
observations during the normal cycle so that none need be carried over
into Cycle 4. For Type IIs, however, only ~350 ksec of Type II time
remains available so that EUVE will only observe ~44% of these observations.
2.8 Public Data Release for 1 Oct 1995
--------------------------------------
by Dr. Nahide Craig, Archive Scientist, ISO Science Support Team
The table below lists the GO observations that become public on 1 Oct
1995. For each entry is given the target name, the approximate exposure
time in ksec, the GMT start and end date(s) for the observation, the spectral
type of the target, and the data identification code. All public data sets
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 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 observation.
===============================================================
Target ~Exp Observation Date(s) SpT DataID
Name (ksec) Start End
===============================================================
Data Sets Available 1 Oct 1995:
EUVE J2214-493 100 12 Aug - 16 Aug 1994 DA go0216
EUVE J2214-493 37 16 Aug - 17 Aug 1994 DA go0217
EX Hyi 100 26 May - 29 May 1994 CV go0218
EX Hyi 87 29 May - 01 Jun 1994 CV go0219
HR 1099 31 24 Aug - 25 Aug 1994 RSCVn go0220
HR 1099 81 25 Aug - 28 Aug 1994 RSCVn go0221
LVC 88+36 100 18 Jun - 22 Jun 1994 HI go0222
LVC 88+36 17 22 Jun - 23 Jun 1994 HI go0223
LVC 88+36 76 26 Jun - 29 Jun 1994 HI go0224
LVC 88+36 20 17 Jun - 17 Jun 1994 HI go0225
MOON 2 25 Aug - 25 Aug 1994 SolSys go0226
RE 1844-743 100 17 Aug - 21 Aug 1994 CV go0227
RE 1844-743 81 21 Aug - 24 Aug 1994 CV go0228
SS Cyg 88 23 Jun - 26 Jun 1994 CV go0229
SS Cyg 100 29 Jun - 02 Jul 1994 CV go0230
SS Cyg 24 02 Jul - 03 Jul 1994 CV go0231
===============================================================
NOTE: There was an error in the assigned DataID numbers for three entries
in last month's data release list. The correct entries are as
follows:
Jupiter 63 04 Jun - 06 Jun 1994 SolSys go0204
M15/AC211 47 06 Jul - 08 Jul 1994 LMXB go0205
Mueller 1993A 55 09 Jun - 11 Jun 1994 comet go0206
2.9 On-Line Access to EUVE
--------------------------
Listed below are the various methods for on-line access to EUVE:
o CEA World Wide Web (WWW)
URL http://www.cea.berkeley.edu/
telnet www.cea.berkeley.edu 200 (for those without a WWW browser)
o anonymous FTP
ftp ftp.cea.berkeley.edu
Name: anonymous
Password: type_your_full_e-mail_address
o anonymous gopher
gopher ftp.cea.berkeley.edu
o EUVE Electronic Newsletters
Past issues -- available via the CEA WWW site
Subscriptions -- mail majordomo@cea.berkeley.edu ("subscribe euvenews")
Post message to all subscribers: mail euvenews@cea.berkeley.edu
o GI Program
Are you interested in finding out about or using EUVE data? Do you
need help in understanding EUVE data sets? Do you need help in using
the available EUVE data analysis software tools? If you answer "yes"
to any of the above, the Guest Investigator (GI) Program at CEA can
help YOU! For further information see the CEA WWW site or contact the
Archive (archive@cea.berkeley.edu).
o Public RAP
The Public Right Angle Program (RAP) is an easy method for researchers
to propose for long-exposure EUVE imaging data. For more information
on the Public RAP and the simple proposal process see the CEA WWW site
or contact the EGO Center (egoinfo@cea.berkeley.edu). Mail all
proposals to euverap@cea.berkeley.edu.
o Contact information for the EUVE Science Archive or GO Center:
Center for EUV Astrophysics
2150 Kittredge St.
Berkeley, CA 94720-5030
Archive EGO Center
510-642-3032 (voice) 510-643-8727 (voice)
510-643-5660 (fax) 510-643-5660 (fax)
archive@cea.berkeley.edu egoinfo@cea.berkeley.edu
3. CEA Job Listings
===================
by Cathie Jones, CEA Personnel Manager
Programmer Analyst II, Job # 09-323-30 (full-time career position)
Serve as a software engineer at the Center for EUV Astrophysics. Design
prototype software systems for low cost automated satellite operations and
human computing. General programming areas will be supporting Artificial
Intelligence (AI) research in model/rule/constraint-based reasoning as
applied to orbiting vehicles and data acquisition/control loops.
Qualifications include a strong background in Electrical Engineering,
Computer Science, Space Engineering, and/or Information Systems, with proven
software development experience required. Experience with the design and
implementation of AI software, and orbiting vehicle ground/flight software
design required. Experience in a combination of the following: UNIX (SUN,
SGI, HP), C, C++, LISP, Fortran, and scripting; development of intelligent
image processing systems, fault diagnosis, fuzzy controllers, network
algorithms and protocols, network based parallel computing; product design
experience. CASE tool experience a plus. Experience with WWW (Netscape,
Mosaic), GUI development, windowing systems preferred.
To apply, formal resume MUST be submitted to:
Personnel Office #3540
Box 09-323-30
2200 University Ave.
Berkeley, CA 94720-3540
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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. ISO Manager and Newsletter Editor: B.A. Stroozas. Funded
by NASA contracts NAS5-30180 and NAS5-29298. Send newsletter
correspondence to: ceanews@cea.berkeley.edu.
The EUVE project is managed by NASA's GSFC: Paul Pashby, GSFC Project
Manager; Dr. Yoji Kondo, Project Scientist; Dr. Ronald Oliversen, Deputy
Project Scientist; Mr. Kevin Hartnett, Project Operations Director. NASA
HQ: Dr. Robert Stachnik, Program Scientist; Dr. G. Riegler, Program
Manager. Information on the EUVE Guest Observer Program is available
from: Dr. Y. Kondo, Mail Code 684, GSFC, Greenbelt, MD 20771 at (301)
286-6247 or e-mail to euve@stars.span.nasa.gov.
END-----------EUVE------------ELECTRONIC---------------NEWS-------------END
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