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ELECTRONIC NEWSLETTER OF THE EUVE OBSERVATORY
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Vol 5, No. 4 18 Apr 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. CEA Encourages Use of GI Program
2. Proposals Continuously Accepted for RAP
3. EUVE Guest Observer Center News
3.1 Bug-Fix Release of EGOCS Package
3.2 Alexis Transient Observed as TOO
3.3 Review of TOO Request Procedure
4. Notes from the EUVE Science Archive
4.1 GO Data Release List for 1 May 1995
4.2 On-Line Access to EUVE
5. Abstracts of Recently *Accepted* EUVE Papers
To comment on or make suggestions for the EUVE electronic newsletter, please
send e-mail to ceanews@cea.berkeley.edu (Internet).
The EUVE satellite reached another milestone on 5 Mar 1995 -- it's 1000th
day in orbit! The observatory performed well throughout the month of March,
performing observations of the following guest observer (GO) targets (alternate
name and spectral type information taken from the SIMBAD or internal CEA
databases):
-------------------------------------------------------------------
Target Alternate Spectral Observation
Name Name Type GMT Date(s) Notes
-------------------------------------------------------------------
YY Gem HD 60179 M1Ve 20 Feb - 03 Mar 1995 ---
Alpha Cen HD 128620 G+.. 03 Mar - 05 Mar 1995 CAL
Alpha Col HD 37795 B7IVe 05 Mar - 08 Mar 1995 ---
AM Her 1H 1814+498 CV 08 Mar - 13 Mar 1995 TOO*
LHS 2471 -------- M+.. 08 Mar - 13 Mar 1995 RAP
PG 1123+189 WD 1123+189 DAw 13 Mar - 19 Mar 1995 ASCA
EUVE J1254-70.3 -------- NOID 13 Mar - 19 Mar 1995 RAP
JUPITER -------- SolSys 19 Mar - 19 Mar 1995 ---
ALEXIS Transient -------- NOID 19 Mar - 19 Mar 1995 TOO
JUPITER -------- SolSys 19 Mar - 22 Mar 1995 ---
GL 411 HD 95735 M2V 22 Mar - 04 Apr 1995 ---
EUVE J1429-38.0 -------- NOID 22 Mar - 04 Apr 1995 RAP
EUVE J1436-38.2 -------- NOID 22 Mar - 04 Apr 1995 RAP
-------------------------------------------------------------------
Key to Notes:
ASCA = coordinated observation with the ASCA satellite
CAL = calibration observation
RAP = simultaneous Right Angle Program (RAP) imaging observation
TOO = Target of Opportunity; the observation marked "*" was a
coordinated observation between the ASCA, ROSAT, STS-67 (Space
Shuttle Astro II Mission), and EUVE satellites
1. CEA Encourages Use of GI Program
===================================
To promote research using EUVE data, CEA recently announced the EUVE
Guest Investigator (GI) Program. The GI Program provides interested
researchers with information, services, education, and training in the use
of EUVE data.
Benefits to GIs include quick and easy access to all public EUVE data
sets, hands-on training in the use of these data sets and in the supporting
processing and analysis software (i.e., the IRAF/EUV package), and dedicated
individual personal support from knowledgeable and experienced CEA scientific
and technical staff members.
CEA encourages users of EUVE data to become GIs! CEA has so far serviced
nine individual GIs, half as local visitors to CEA and half remotely via
the Internet and telephone/e-mail. Supported topics have varied from
general introductory overviews of the EUVE data sets and of the data
processing and analysis software (IRAF/EUV), to flux analysis and light
curve generation from photometric data, to detailed spectral reduction and
extraction using spectrometer data.
Anyone can become a GI -- astronomers, technologists, educators, or the
general public! It's very simple to become a GI and there are currently open
slots available. For more information please contact the EUVE Science Archive
(archive@cea.berkeley.edu; 510-642-3032) or submit the simple GI registration
form via the Archive section of the CEA WWW site (http://www.cea.berkeley.edu;
telnet www.cea.berkeley.edu 200).
2. Proposals Continuously Accepted for RAP
==========================================
The EUVE Right Angle Program (RAP) attempts to utilize the full capacity
of EUVE by observing and analyzing data collected by the three "scanning"
telescopes during GO spectrometer observations. The scanners are mounted
at right angles (hence the name RAP) to the deep survey/spectrometer (DS/S)
telescope and provide imaging capabilities that allow for long exposure
(40-600 ksec) EUV photometry over an area of up to 19.6 square degrees in
four distinct EUV wavelength regions. Although the primary GO observations
constrain the area of sky visible to the scanners, it is often possible
to position and simultaneously observe RAP targets in the scanner fields
of view during GO observations.
CEA recently announced the Public RAP, which allows researchers world-wide
to quickly and easily submit proposals to use the scanners during the primary
GO spectrometer observations. Brief proposals (a paragraph or two for the
scientific justification) are submitted electronically via a prototype of the
proposal process to be used during the EUVE extended mission. Once approved
by the Project Office, the targets are scheduled as constraints allow into
the GO science plans. Upon the completion of a RAP observation the proposer
will be notified and arrangements made for data reduction and delivery.
The EUVE Public RAP is a simple method for researchers to acquire
long-exposure EUV photometric data, and we encourage all interested researchers
to submit RAP proposals! Just follow the simple directions provided on the
CEA WWW site (http://www.cea.berkeley.edu; telnet www.cea.berkeley.edu 200)
or contact the EGO Center (egoinfo@cea.berkeley.edu) for more information.
3. EUVE Guest Observer Center News
==================================
by Anne Miller, EGO Center Technical Writer
3.1 Bug-Fix Release of EGOCS Package
------------------------------------
A new revision of the EGOCS software package (IRAF/EUV) has been released,
and is now available on the CEA/EUVE ftp site (www.cea.berkeley.edu; in
the directory /pub/software/euv1.5.1). This release primarily fixes an
incompatibility problem between the euvtools/qprst task and tables1.3.3/strfits
(qprst would segfault when it was run on tables that were extracted using
tables1.3.3/strfits). Any version of strfits should now work properly with
qprst.
A problem which produced a segmentation fault on a Silicon Graphics system
when the task qpmkim was run has also been remedied. Most users will not
notice this change unless they have had a similar problem.
The following is a summary of the euv1.5.1 changes:
* qprst made compatible with tables1.3.3/strfits
* qpmkim portability bugs fixed
* backmon 'ds' to list of possible detectors in backmon
3.2 Alexis Transient Observed as TOO
------------------------------------
On 17 Mar 1995 the ALEXIS satellite observed a transient x-ray source near
the position RA 175.51, Dec -68.9. The EUVE DS/S instrument was pointed at
this target of opportunity (TOO) from 19 Mar 1995 1:13 PM to 22 Mar 1995
11:00 AM GMT. Although the transient was not detected by EUVE during the 46
orbits of observation, the resulting data should produce upper limits on
this source's EUV intensity in the EUVE DS/S wavelength regions (67-178 A;
157-364 A).
3.3 Review of TOO Request Procedure
-----------------------------------
Requests for observations of unanticipated TOOs in the EUV may be submitted
at any time to the EUVE Project Science Office at GSFC:
EUVE Project Science Office
Code 684
Building 21, Room G59
Goddard Space Flight Center
Greenbelt, MD 20771 USA
phone: (301) 286-7664
email: euve@stars.gsfc.nasa.gov
The request must identify a principal investigator (PI), and must include
a compelling scientific justification and target coordinates, preferably in a
completed target summary form (available electronically from the CEA/EUVE FTP
site in the file /pub/nra94/Form.txt, lines 130-195).
Although the EUVE Science Operations Center (ESOC) has converted to
single-shift operations, PI's can now forward their *approved* TOO requests
directly to the science planner at CEA; GOs will be instructed regarding
the specific details of how to do this. Investigators should expect to see
no change in EUVE's response time for TOO observations; the current average
response time is about eight hours.
4. Notes from the EUVE Science Archive
======================================
by Brett A. Stroozas, ISO Manager
4.1 GO Data Release List for 1 May 1995
---------------------------------------
The table below lists the GO observations which become public on 1 May
1995; with this release all Cycle 1 observations will now be publicly available.
For each entry is given the target name, the approximate exposure time in
kiloseconds, the GMT start and end date(s) for the observation, the spectral
type of the target, and the data identification code. All public data sets
may be ordered from the archive via WWW and electronic or postal mail (see
addresses below). Please be sure to include in your order the DataID(s) of
interest.
The data rights policy for GO observations states that GOs have proprietary
rights to the data for one year from the date (s)he receives it. It is often
the case that long observations are broken up over many months; e.g., an
observation approved for 60 ksec may actually be observed for 10 ksec one
month, 20 ksec the next and 30 ksec three months later. In such cases the
one-year proprietary period begins after the GO receives the final piece of
the completed observation.
===============================================================
Target ~Exp Observation Date(s) SpT DataID
Name (ksec) Start End
===============================================================
Data Sets Available 1 May 1995:
G191-B2B 61 05 Mar 1994 - 08 Mar 1994 DA go171
Jupiter/SL9 87 03 Jul 1994 - 06 Jul 1994 SolSys g0172
Jupiter/SL9 81 13 Jul 1994 - 16 Jul 1994 SolSys g0173
Jupiter/SL9 247 17 Jul 1994 - 26 Jul 1994 SolSys go174
Jupiter/SL9 54 29 Jul 1994 - 30 Jul 1994 SolSys go175
===============================================================
There is also one correction to the list published in last month's newsletter.
The Vela observation of 4-9 Feb 1994 (go0168) was mistakenly published as
public as of 1 Apr 1995; this observation will remain proprietary until late
1995. The Archive apologizes for any inconvenience this may cause.
4.2 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/ (for those with WWW browsers)
telnet www.cea.berkeley.edu 200 (for those without WWW browsers)
o anonymous FTP/gopher: ftp.cea.berkeley.edu
o EUVE Electronic Newsletters (past issues available via CEA WWW):
Subscriptions: mail majordomo@cea.berkeley.edu ("subscribe euvenews")
Post message to all subscribers: mail euvenews@cea.berkeley.edu
o For additional information contact the Archive:
The EUVE Public Science Archive
Center for EUV Astrophysics
2150 Kittredge St.
Berkeley, CA 94720-5030
510-642-3032 (voice) or 510-643-5660 (fax)
archive@cea.berkeley.edu
5. 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 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 full papers
will also be posted under the CEA WWW Home Page. Please send all abstracts
or papers to archive@cea.berkeley.edu.
--------------------------------------------------------------
EUVE/CEA EVALUATION AND DESCRIPTION OF THE JPL SELECTIVE MONITOR
(SELMON) PART I.
S. Taleb-Agha, T. Morgan, and R.F. Malina
A Technology Innovation Publication. [CEA publication #646]
Selmon, a "selective monitoring program," uses complex monitoring strategies
to identify and draw attention to satellite sensor anomalies. Selmon derives
sensor characteristics from present telemetry monitors and historical sensor
behavior and can be useful to the Engineering Analyst for detecting anomalies.
CEA has adapted Selmon for use as a client of an RTworks data server. Selmon
employs both an RTworks graphical interface and an X-Windows interface. CEA
is considering adopting Selmon into its monitoring system. The Jet Propulsion
Laboratory (JPL) designed the Selmon software package to selectively monitor
satellite sensors. It is designed as a client program to receive sensor values
from a data server, process them, and display the results on a graphical user
interface. Selmon's main contributions are: (1) identifying more complex
anomaly patterns by comparison to historical data distributions and computing
a number of indicators, and (2) highlighting the subset of sensors Selmon
determines are critical and require operator attention.
--------------------------------------------------------------
THE ATMOSPHERIC PARAMETERS AND ELEMENTAL ABUNDANCES OF THE NEARBY
F5 SUBGIANT PROCYON
J.J. Drake and J.M. Laming
To appear in The Observatory. [CEA publication #645]
We present a review of the status of current knowledge of the atmospheric
parameters and elemental abundances of the nearby F5 IV star Procyon. Based
on the available evidence, our adopted values for these quantities are
Effective temperature, T_eff = 6650 +/- 100 K
Surface gravity, log g = 4.0 +/- 0.1
Microturbulence, xi = 2.0 +/- 0.2 km/s
Metallicity, [M/H] = 0.0 +/- 0.1
There is no evidence for deviation of any of Procyon's photospheric element
abundance from the solar photospheric mixture. Procyon's coronal abundances
appear to be identical to the photospheric abundances; unlike the Sun, Procyon
does not appear to exhibit a "FIP effect".
--------------------------------------------------------------
EXTREME ULTRAVIOLET SPECTROSCOPY AND PHOTOMETRY OF EQ PEGASI
B. Monsignori-Fossi, M. Landini, A. Fruscione, and J. Dupuis
To appear in The Astrophysical Journal. [CEA publication #644]
We present the first spectroscopic extreme ultraviolet observations of the
star EQ Pegasi (dM4e+dM6e) obtained during a guest observer pointing with the
Extreme Ultraviolet Explorer satellite (EUVE). EQ Peg was detected in all
three spectrometer channels (70-760 A) and was successfully monitored at the
same time by the EUVE Deep Survey photometer (67-178 A). We have identified
the main features observed in the spectra and conclude that a number of lines
are produced by the highest ionization stages of iron. The detections in the
280-760 A range are mainly caused by second-order throughput, except for the
HeII 304 A line. Evidence of activity modulation during the observation is
present in both the photometric and spectroscopic data.
--------------------------------------------------------------
THE EXTREME ULTRAVIOLET SPECTRUM OF THE BL LACERTAE OBJECT PKS 2155-304
A. Konigl, J.F. Kartje, S. Bowyer, S.M. Kahn, and C.-Y. Hwang
To appear in The Astrophysical Journal. [CEA publication #633]
We carried out two spectroscopic observations of the BL Lacertae object
PKS 2155-304 with the Extreme Ultraviolet Explorer during 1993 June (~111 ksec)
and July (~157 ksec). The source was detected in the ~75-110 A range during
both epochs, but the two spectra differ in detail, and the flux has increased
by ~60% between the two observations. A power-law fit to the data yields an
energy spectral index alpha ~3-4 for the measured Galactic H I column density
and likely choices of the He I and He II abundances: such values are
inconsistent with the soft X-ray spectral index of 1.65 measured by the ROSAT
PSPC, which approximately corresponds also to the observed EUV to X-ray flux
ratio. Fitting a power law with alpha = 1.65 to the EUV data implies strong
absorption at the source between ~75 and ~85 A. We argue that this absorption
is not due to continuum opacity and demonstrate that it can be attributed,
instead, to a superposition of Doppler-smeared absorption lines originating in
high-velocity (~< 0.1 c), radially localized Broad Emission Line-type clouds
of total column density ~5E20 cm^(-2) that are ionized by the beamed continuum
of the associated relativistic jet. We identify the lines as mostly L- and
M-shell transitions of Mg, Ne, and Fe. The same model also implies a pronounced
O VII K-alpha X-ray absorption feature at roughly the same energy as the feature
detected in 1990 by BBXRT, which provides strong support for the apparent
association of this object with a galaxy at z=0.116. We suggest that the
higher-energy X-ray absorption feature detected in 1980 by the Einstein OGS
and identified with a broadened O VIII Ly-alpha line might have originated in
outflowing clouds that had a higher abundance of O VIII than of O VII, possibly
because they crossed our line of sight closer to the continuum source.
--------------------------------------------------------------
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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
C.S. Bowyer. EGO and Archive Science Manager: C.A. Christian. Archive
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.
The GSFC Project Manager: Paul Pashby, Project Scientist: Dr. Yoji
Kondo, Deputy Project Scientist: Dr. Ronald Oliversen. NASA HQ Program
Scientist: Dr. Robert Stachnik, Program Manager: Dr. G. Riegler. GSFC
Project Operations Director: Mr. Kevin Hartnett. 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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