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This page includes documentation and information related to the development and
ongoing maintenance of Z39.50; development of future versions of Z39.50; and
information related to the implementation and use of the Z39.50 protocol.
ZADEH,
Farhad Yusef
( Northwestern Univ. )
ZARITSKY,
Dennis
( Steward Observatory )
ZAVATTI,
Franco
( Dept. of Astronomy, Bologna University, Italy )
Structure
of central regions of (elliptical) galaxies; Statistical distribution of true
axial ratios; Deconvolution from PSF; M31 globular clusters; Teacher at Science
Faculty: Physics Laboratory at Astronomy course; Probability and Statistics at
Computer Science course;
ZENSUS,
Anton
( MPIfR )
Director
at the Max-Planck-Institut fuer Radioastronomie, Bonn, Germany.
Zielona
Gora Astronomical Centre
Our general subject is pulsar radiation, especially pulsar observations and
modelling of pulsar radiation . We also work on relativistic astrophysics,
plasma physics and extinction of interstellar dust.
ZINCHENKO,
Igor
( IAP RAS )
Radio
astronomy, studies of dense interstellar molecular clouds
ZOONEMATKERMANI,
Saeid
( Stony Brook Radio Astronomy )
ZUBKO,
Victor
( Technion, Haifa, Israel )
Research
interests: physics of cosmic dust, dust formation around RCB and WR stars,
carbon condensate in a white dwarf atmosphere, optical properties of dust
grains, computational methods in dust astrophysics.
ZUCKER,
Dan
( Univ.Washington )
Zurich
Solar Radio Spectrometer
The Radio
Astronomy Group (RAG)
of ETH
in Zurich, Switzerland, recorded solar radio spectrograms with an analog
spectrometer called Daedalus (1974-1993) in the range of 100-1000 MHz. Its observation
list can be
accessed directly. Two digital spectrometers, Ikarus
(1978--1985) and PHOENIX
(1988--1994), cover a range from 100--1000 MHz and 0.1--3 GHz, respectively. And
since 1998 the new and improved Phoenix-2
Spectrometer covers a range from 0.1 -4 GHz. These data can be accessed by the
ASPECTimage retrieval system. Their observation list contains references to
frequency programs that indicate which frequencies were observed. More
information can be obtained from RAG members.