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Vol 6, No. 4                 26 Apr 1996                    ISSN 1065-3597
	  (C) 1996, Regents of the University of California
Precedence: bulk

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

 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 New EUVE Software and Reference Data Releases
    2.2 2nd EUVE Source Catalog in ADS
    2.3 Public Data Release for 1 May 1996
    2.4 On-Line Access to EUVE

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 Mar
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

    44i Boo          HD 133640       G0V+    26 Feb - 03 Mar 1996  ---
    Capella          HD 34029        G5IIIe+ 03 Mar - 07 Mar 1996  ---
    GD 253           WD 1254+223     DAw     03 Mar - 07 Mar 1996  RAP
    EUVE J1250+209   --------        NOID    03 Mar - 07 Mar 1996  RAP
    EUVE J1303+22.4  --------        NOID    03 Mar - 07 Mar 1996  RAP
    WD 1234+482      PG 1234+482     sd:B    07 Mar - 10 Mar 1996  ---
    V1159 Ori        CSV 579         DwNva   10 Mar - 12 Mar 1996  ---
    Test             --------        ----    12 Mar - 12 Mar 1996  TST
    WD 1234+482      PG 1234+482     sd:B    12 Mar - 16 Mar 1996  ---
    LHS 2065         LP 666-9        M:      16 Mar - 20 Mar 1996  ---
    LHS 3003         LP 914-54       M+      16 Mar - 20 Mar 1996  RAP
    PSR J1024-0719   --------        Pulsar  20 Mar - 21 Mar 1996  ---
    Comet 1996 B2    Hyakutake       Comet   21 Mar - 25 Mar 1996  ---
    PSR J1024-0719   --------        Pulsar  25 Mar - 27 Mar 1996  ---
    RE J1746-703     EUVE J1746-706  NOID    27 Mar - 05 Apr 1996  ---
    3C 273           PKS 1226+02     QSO     27 Mar - 05 Apr 1996  RAP
    1219+044         --------        AGN     27 Mar - 05 Apr 1996  RAP
    1227+024         --------        AGN     27 Mar - 05 Apr 1996  RAP
   Key to Notes:
	RAP = simultaneous Right Angle Program imaging observation
	TST = orbital daytime test in preparation for observation of
		Comet B2 1996 (Hyakutake)

1. EUVE Science News

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

   *** EUVE Observations of the B Giant Star beta Canis Majoris ***

      Drs. 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 obtained and analyzed the EUVE spectrum of the bright
   variable star beta CMa (B1 II-III).  This star is one of the
   strongest EUV sources detected with the long-wavelength (LW)
   spectrometer in the wavelength region lambda > 504 A even though it
   is at a distance of 206 pc. Dr. Cassinelli and his collaborators
   derived from the EUVE data a neutral hydrogen column density of
   ~2E+18 cm^(-2) and a lower limit for the neutral helium column
   density of 1.4E+18 cm^(-2) toward beta CMa, showing that along this
   sight line much of the hydrogen is ionized while helium is neutral.
   Dr.  Cassinelli and his team made a comparison between the emergent
   flux and the predictions of model atmospheres and showed that the
   predicted energy distribution does not match observations in all
   wavelength regions, so they propose additional photospheric opacity
   sources.  As beta CMa is among the brightest of the beta Cephei
   class of variable stars, Dr. Cassinelli's group also analyzed the
   star's pulsation properties from the EUV observations.  They found
   that the semi-amplitude of the effective temperature change
   associated with the pulsation is 108 K for the primary period.

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 Home
Page.  Please send all abstracts or preprints to


K. Hurley, P. Li, F. Vrba, C. Luginbuhl, D. Hartmann, C. Kouveliotou,
  C. Meegan, G. Fishman, S. Kulkarni, D. Frail, S. Bowyer, and M.
To appear in The Astrophysical Journal (Letters).

   The location of the soft gamma repeater SGR1900+14 was recently
reduced to two ~5 arcmin^2 alternate error boxes by the network
synthesis method.  We have used the ROSAT High Resolution Imager to
observe the error box which is closest to the supernova remnant
G42.8+0.6.  A quiescent, steady, point X-ray source was found at
alpha(2000) = 19h 07m 14.15s, delta(2000) = 9 deg 19' 19.06" whose
unabsorbed flux is 3E-12 erg cm^(-2) s^(-1).  Its position is also
consistent with a peculiar double infrared source.  We have also
examined this region using the VLA, and have obtained upper limits to
the extreme ultraviolet flux of this object using the EUVE spacecraft.


K.S. Long, C.W. Mauche, J.C. Raymond, P. Szkody, and J.A. Mattei
To appear in The Astrophysical Journal.

   We have observed U Gem during the peak and declining phases of a
wide outburst in 1993 December with the Extreme Ultraviolet Explorer
(EUVE) Satellite.  At peak, U Gem was one of the brightest EUV sources
in the sky.  The spectrum of the source is complex.  Fitted to a
blackbody spectrum, the apparent temperature at peak is 140,000 K, the
luminosity is 4E+34 (D/90 pc)^2 erg/s, and the minimum size of the
emitting region is comparable to that of the white dwarf.  If the EUV
emission arises primarily from the boundary layer, then the boundary
layer luminosity in U Gem is comparable to the disk luminosity.  The
EUV source is partially eclipsed at orbital phases 0.6-0.8.  The
eclipse spectrum, which we associate with a wind emerging from the
vicinity of the white dwarf, is dominated by emission features.  The
identification of these emission features with transitions expected in
a relatively cool (T < 160,000 K), photoionized plasma helps to
resolve a controversy concerning the ionization state of winds of
dwarf novae.  The EUV lines arise from the dominant ionization states
of the wind, and their strengths suggest that the wind mass loss rate,
at least in U Gem, is a substantial fraction of the WD accretion rate.


N.S. Brickhouse
To appear in Proceedings of the Tenth 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.


  GD 50 
S. Vennes, S. Bowyer, and J. Dupuis
Astrophysical Journal (Letters), 461, L103.  [CEA publication #727]

   Extreme ultraviolet (EUV) spectroscopy of the hot, hydrogen-rich
white dwarf GD 50 reveals an unusual photospheric mixture of hydrogen
and helium. This hot DA white dwarf is also remarkable for its mass
(~1.2 M_solar) near the Chandrasekhar limit. The spectra obtained with
the Extreme Ultraviolet Explorer (EUVE) show a prominent He II
resonance line series and constrain its atmospheric parameters to
T_eff = 40,300 +/- 100 K and n(He)/n(H) = (2.4 +/- 0.1)E-04 (assuming
log g =9.0).  We also constrain the local interstellar medium column
densities of neutral helium and hydrogen to n_HeI = 6E+16 and n_HI =
9E+17 cm^(-2). The presence of helium in an isolated, massive DA white
dwarf is paradoxical.  We examine and rule out a few scenarios
(radiative levitation, accretion from the ISM or a hypothetical
companion), but we suggest that if massive white dwarfs do result from
stellar mergers, large orbital angular momentum may be preserved and
result in a large meridional circulation current, possibly dredging-up
helium from the envelope.  Although we find evidence of large
rotational velocity in EUV He II line profiles, we propose additional
observational tests of the dredge-up model.

S. Vennes, P.A. Thejll, D.T. Wickramasinghe, and M.S. Bessell
To appear The Astrophysical Journal.  [CEA publication #728]

   We present optical spectroscopy of the Balmer line series (H-beta
through H8) of a sample of 18 hot white dwarfs obtained at the Mount
Stromlo and Siding Spring Observatories; the stars are a subset of the
white dwarfs detected in the Extreme Ultraviolet Explorer (EUVE)
all-sky survey.  We analyze the Balmer line profiles conjointly with
EUV photometric measurements and provide new effective temperature and
surface gravity determinations.  We also provide determinations of the
neutral hydrogen column density in the interstellar medium toward
these lines of sight.  The spectral and photometric properties of most
objects in our sample are consistent with emission from pure-hydrogen
atmospheres.  However, we find evidence for the presence of trace
absorbers in the photospheres of 5 out of 18 objects from the sample
-- EUVE J0230-479, EUVE J0809-729, EUVE J1546-370, EUVE J2004-560, and
EUVE J2324-547.  The star EUVE J0230-479 figures among the group of DA
white dwarfs with the highest level of metallicity, while EUVE
J0809-729 is one of the coolest DA stars (~30,000 K) to show evidence
of trace elements.  We also report the discovery of three new massive
white dwarf stars -- EUVE J1546-367 (M ~ 1.0 M_solar), EUVE J1727-360
(M ~ 1.2 M_solar), and EUVE J1746-706 (M ~ 1.4 M_solar); excluding the
two high-mass (M > 1.1 M_solar) objects from our sample, we obtain an
average white dwarf mass of 0.64 M_solar.


F. Machi, J. E. Marsden, and W. G. McKay
TUGBoat, 16(4), 358, 1995.  [CEA publication #730]

   FasTeX is a system of keyboard shortcuts for speeding up the typing
of TeX from the keyboard.  FasTeX is currently available for the
Macintosh and UNIX. It replaces any keyboard shortcut by the
equivalent TeX command or group of commands in Plain TeX, AmSTeX,
AmSLaTeX, or LaTeX.


S. Vennes, P. Chayer, M. Hurwitz, and S. Bowyer
To appear in The Astrophysical Journal.  [CEA publication #732]

   High-dispersion observations of the far ultraviolet spectra of the
hot DA white dwarfs G191-B2B and MCT 0455-2812 reveal the presence of
two previously undetected elements in white dwarf photospheres: sulfur
and phosphorus.  The spectra, obtained with the Berkeley EUV/FUV
spectrometer and the ORFEUS telescope aboard the space platform
Astro-SPAS, show characteristic Lyman line series and extend beyond
the H I interstellar medium (ISM) absorption edge in the extreme
ultraviolet.  We provide new effective temperature and surface gravity
measurements based on a detailed fit to the Lyman line series which
show an interesting dependence on the heavy element abundance.  Weak
absorption lines are identified with C III lambda 977.02, N III lambda
989.799, Si IV lambdas 1066.629, 1122.486, 1128.325, P V lambdas
1117.978, 1128.007, and S IV lambdas 1062.671, 1072.990.  The origin
of the carbon and nitrogen features is uncertain, but the silicon,
phosphorus, and sulfur detection provides the basis for new
photospheric abundance measurements: log(Si/H) = -6.4, log(P/H) = -7.7,
and log(S/H) = -6.7 in G191-B2B, and log(Si/H) = -5.7, and log(P/H) =
-7.6 in MCT 0455-2812.  We also provide upper limits to the abundance
of helium and chlorine.  These measurements provide a critical insight
into spectral evolution of white dwarf stars and we find strong
evidence of heavy element depletion possibly associated to previous
mass loss episodes in these hot, therefore young, white dwarfs.  On
the other hand, we confirm an excess of silicon that could be
explained if these stars currently accrete solid particles from their
immediate environment.


J.J. Drake
To appear in Proceedings of the 9th Cambridge Workshop, "Cool Stars,
  Stellar Systems, and the Sun", ed. R. Pallavicini and A. K. Dupree,
  PASP Conference Series (San Francisco: ASP), 1996.  [CEA publication

   Progress in the understanding of stellar coronae resulting from 3
years of EUVE spectroscopic observations is briefly reviewed.


J.J. Drake, R.A. Stern, G. Stringfellow, M. Mathioudakis, J.M. Laming,
  and D.L. Lambert
To appear in The Astrophysical Journal.  [CEA publication #734]

   We report the detection of quiescent EUV emission from the very low
mass dwarf VB8 by the Extreme Ultraviolet Explorer (EUVE) in the
Lexan/B band (65-190 A).  We interpret this emission in terms of a hot
coronal plasma and combine this information with previous X-ray
detections to estimate the quiescent plasma temperature and emission
measure.  The combined observations made by EINSTEIN, ROSAT and EUVE
between 1979 and 1994 are consistent with a quiescent coronal plasma
temperature of 2-6 million degrees, and indicate the same emission
measure to within a factor of about 2: the non-flaring corona of VB8
then appears relatively constant over time scales of more than 10
years. Our results are consistent with the picture of a
turbulently-driven or distributive dynamo for VB8, rather than with a
large-scale field dynamo which appears to dominate the solar corona.
Evidence from X-ray and optical data concerning the long term coronal
variability of the more active stars of higher mass also points
towards the idea that active late-type stars in general are dominated
by a turbulent dynamo.

2. EUVE Science Operations News

2.1 New EUVE Software and Reference Data Releases
	by Dr. Mark Abbott, EGO Center Scientist

[Editor's note:  Please direct all queries regarding the information
  in this section to]

  The EGO Center announces the release of version 1.6.1 of the EUV
software IRAF layered package and version 1.12 of the EGODATA
calibration data set.  The brief descriptions below should help users
determine if they need to update their installations of these
products.  All data sets currently sent to investigators by the EGO
Center contain the new versions -- please check the cover letter that
accompanies each data set for version information.

  What's New In EUV 1.6.1

    This is a maintenance and pipeline-processing release.  We have
fixed some bugs, made some minor changes, and done some other work to
support the processing of GO data here at the EGO Center.  Most users
should not be greatly affected by this release.  One important bug fix
is described below.  For more details, see the release notes that
accompany the software.

  'qprst' bug fixed

   A bug in the task 'qprst' that appeared in version 1.6 of the EUV
package has been fixed.  The most common symptom was that QPOE files
created with 'qprst' were subsequently unusable with tasks such as
'qpdup' in the EUV package or 'timsort' and 'qpcopy' in the PROS
package.  This bug was described in a 15 Dec 1995 message on this
mailing list, at which time a patch was made available to fix the

   The bug has been corrected in the EUV1.6.1 release.  Any QPOE files
created with the faulty version of 'qprst', however, will remain
damaged.  If you need to use one of the above tasks with such a QPOE,
it will have to be recreated using the fixed version of 'qprst'.

  What's New in EGODATA 1.12

  New spectrometer wavelength calibration

   A new revision of the EUVE spectrometer wavelength calibration has
been implemented.  A detailed description of how this calibration was
carried out will appear in a paper that has recently been
submitted to The Astrophysical Journal (Supplement):

   "The Calibration of the EUVE Spectrometers. I.  Wavelength
   Calibration and Resolution" by M.J. Abbott, W.T. Boyd, P. Jelinsky,
   C. Christian, A. Miller-Bagwell, M. Lampton, R.F. Malina, and
   J.V. Vallerga.

A preprint of this paper will be sent to all EUVE GOs in the near

   The new calibration has RMS wavelength errors of 0.11 A in the SW
spectrometer, 0.14 A in the MW, and 0.24 A in the LW, which are slight
improvements over the previous calibration.  There is substantially
more data included in the new calibration, which means that there
should be fewer gaps in wavelength coverage.  Some emission line
identifications have been improved based on recently published results
from EUVE GOs.  A more detailed analysis has been done of the causes
and effects of the residual offsets in imaging angle that are known to
be present in EUVE spectral data.

   To apply the new calibration to previous data sets, the pipeline
task 'cep' must be rerun.  See Chapter 5 of the EUVE Guest Observer
Software User's Guide or contact the EGO Center for help with this.

  New Definition of Earth Blockage

   The definition of earth blockage has been changed.  An observation
is now considered blocked if EUVE is pointed at an angle larger than
102 degrees from the spacecraft's local zenith direction; an angle of
roughly 107.4 degrees was used previously.  Earth blockage is
described further in section 4.3.2 of the EUVE Guest Observer Data
Products Guide.  Also, see the memo posted on the CEA WWW site at URL

  New Count Rate Limits

   A study of the typical count rates in the EUVE spectrometers was
done.  Count rates from 28 million seconds of pointed spectrometer
data were used to choose optimal upper limits for the ADct monitors
used to eliminate times with unusually high background (typically due
to passage through the South Atlantic Anomaly).  Previously, no upper
limits were set on the data during the nominal reduction.  The new
upper limits are: 80 counts/sec in the SW spectrometer, 130 in the MW,
and 150 in the LW.  These limits are now used in the EGO Center
nominal reduction to generate the "valid time" filters,, and that are used (along with earth-blockage
filters) when producing spectral images.  There has been no change in
the amount of data delivered to GOs, only in the filtering done in the
nominal reduction.  A detailed memo about the count rate analysis is
available on the CEA WWW site at URL

2.2 2nd EUVE Source Catalog in ADS
        by Dr. Nahide Craig, ISO User Support Scientist

   The 2nd EUVE Source Catalog (Bowyer, 1996), which contains
information on 734 sources detected by EUVE, is now available on-line
via NASA's Astrophysics Data System (ADS).  ADS is an environment that
provides the astronomical community with a wealth of data (e.g.,
source catalogs) and information sources (e.g., abstracts and papers)
via various on-line electronic services.

   The 2nd Catalog supplements previous EUVE catalogs, all of which
are available via ADS:

 o euve_bsl -- "The Extreme Ultraviolet Explorer Bright Source List"
	(Malina, 1994)
 o euve_cat1 -- "The First EUVE Source Catalog" (Bowyer, 1994)
 o euve_cat1supp -- supplement to "The First EUVE Source Catalog"
	(Bowyer, 1994)
 o euve_rap -- "Serendipitous EUV Sources Detected during the First
	Year of the Extreme Ultraviolet Explorer Right Angle Program"
	(McDonald, 1994)
 o euve cat2 -- "The Second EUVE Source Catalog" (Bowyer, 1996)

To access these or other astronomical catalogs just follow the
appropriate links under "ADS Data Catalogs" on the ADS HomePage (URL

2.3 Public Data Release for 1 May 1996
        by Dr. Nahide Craig, ISO User Support Scientist

   The table below lists the GO observations that become public on 1
May 1996.  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

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

     Data Sets Available 1 May 1996:

      YY Gem         100     20 Feb - 24 Feb 1995    dMe      go0283   
      YY Gem         100     24 Feb - 27 Feb 1995    dMe      go0291
      YY Gem          90     27 Feb - 02 Mar 1995    dMe      go0292

     NOTE: There were some typographical errors in the list of data
     released on 1 Apr 1996 (see newsletter V6, #3).  The correct list
     reads as follows:

     Data Sets Available 1 Apr 1996 (Corrected):

      Feige 24        29     22 Oct - 23 Oct 1994    WD       go0288
      Vela           139     04 Feb - 09 Feb 1994    SN	      go0168
      Vela            43     18 Mar - 20 Mar 1994    SN       go0289
      Vela            73     25 Nov - 27 Nov 1994    SN       go0290


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 to all subscribers:  mail

 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 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
     (  Mail all proposals to

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

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


 o Bowyer, 1994 -- "The First EUVE Source Catalog", S. Bowyer, et al.,
   Astrophysical Journal (Supplement), 93(2), 569, 1994.  [CEA
   publication #565]
 o Bowyer, 1996 -- "The Second EUVE Source Catalog,", S. Bowyer,
   et al., Astrophysical Journal (Supplement), 102, 129-160, 1996.
   [CEA publication #649]
 o Malina, 1994 -- "The Extreme Ultraviolet Explorer Bright Source
   List", R. Malina, et al., Astronomical Journal, 107(2), 751-764,
   1994.  [CEA publication #553]
 o McDonald, 1995 -- "Serendipitous EUV Sources Detected during the
   First Year of the Extreme Ultraviolet Explorer Right Angle
   Program," K. McDonald, et al., Astronomical Journal, 108,
   1843-1853, 1994.  [CEA publication #593]

  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 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, Project
  Operations 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

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