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Z39.50 Maintenance Agency

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.