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At least 397 records · Page 22
All sourcesNASA NTRSDOE OSTI
NASA NTRS2000

Improvement of VLBI EOP Accuracy and Precision

In the CORE program, EOP measurements will be made with several different networks, each operating on a different day. It is essential that systematic differences between EOP derived by the different networks be minimized. Observed biases between the simultaneous CORE-A and NEOS-A sessions are about 60-130 micro(as) for PM, UT1 and nutation parameters. After removing biases, the observed rms differences are consistent with an increase in the formal precision of the measurements by factors ranging from 1.05 to 1.4. We discuss the possible sources of unmodeled error that account for these factors and the biases and the sensitivities of the network differences to modeling errors. We also discuss differences between VLBI and GPS PM measurements.

MacMillan, Daniel↗
NASA NTRS2000

The S2 VLBI Systems: DAS, RT/PT and Correlator

The S2 VLBI system synthesizes wide IF bandwidths by rapidly switching the local oscillator (LO) frequency in a small (1-4) number of baseband converters (BBC's). Data are recorded on video cassettes using an array of 8 VHS transports. Characteristics of the S2 Data Acquisition System (DAS), the S2 Record and Playback Terminals (RT and PT) and the S2 Correlator are summarized. The bandwidth synthesis (BWS) frequency switching sequence used in a series of system validation experiments is presented.

Petrachenko, William T.↗
NASA NTRS2001

Future Evolution of NASA's SLR and VLBI Networks

Over the first half of this decade the NASA Space Geodesy Program is planning a major transformation of its existing (Satellite Laser Ranging) SLR network of stations and also further evolutionary changes to its network of (Very Long Base Interferometry) VLBI stations. These network changes will be made to meet the ever more demanding requirements of the earth and space science programs that these networks support while seeking through automation and electronic data communications to increase efficiency and decrease cost of operations and maintenance. The major aspects of the NASA plan will be outlined and the benefits to the scientific community will be addressed.

Bosworth, John M.↗
NASA NTRS2001

GSFC VLBI Analysis Center

This report presents the activities of the Goddard Space Flight Center's Very Long Base Interferometry (VLBI) Analysis Center during the period from March 1, 1999 through December 31, 2000. The center's primary software development, analysis, and research activities axe reported, and the responsible staff members are described. Plans for 2001 are also presented.

Gordon, David↗
NASA NTRS2002

International VLBI Service for Geodesy and Astrometry: General Meeting Proceedings

This volume contains the proceedings of the second General Meeting of the International VLBI Service for Geodesy and Astrometry (IVS), held in Tsukuba, Japan, February 4-7, 2002. The contents of this volume also appear on the IVS Web site at http://ivscc.gsfc.nasa.gov/publications/gm2002. The key-note of the second GM was prospectives for the future, in keeping with the re-organization of the IAG around the motivation of geodesy as 'an old science with a dynamic future' and noting that providing reference frames for Earth system science that are consistent over decades on the highest accuracy level will provide a challenging role for IVS. The goal of the meeting was to provide an interesting and informative program for a wide cross section of IVS members, including station operators, program managers, and analysts. This volume contains 72 papers and five abstracts of papers presented at the GM. The volume also includes reports about three splinter meetings held in conjunction with the GM: a mini-TOW (Technical Operations Workshop), the third IVS Analysis Workshop and a meeting of the analysis working group on geophysical modeling.

Vandenberg, Nancy R.↗
NASA NTRS2002

Geodetic Results from Mark 4 VLBI

We present geodetic results of a series of 30 VLBI experiments recorded in Mark 4 mode at rates of 128 and 256 Mbps. The formal uncertainties of UT1, polar motion, and nutation offsets derived from these experiments are better than the corresponding uncertainties from NEOS-A experiments by a factor of 1.3-2. Baseline length repeatability for the series of 32 experiments over a period of one year is about 0.9 ppb. For comparison, NEOS-A length repeatability is about 1.4 ppb. We will discuss optimal use of Mark 4 in the design of future observing networks.

MacMillan, Daniel↗
NASA NTRS2000

Space VLBI observations of 3C 279 at 1.6 and 5 GHz

We present VLBI Space Observatory Programme (VSOP) observations of the gamma-ray blazar 3C 279 at 1.6 and 5 GHz made on 1998 January 9-10 with the HALCA satellite and ground arrays including the Very Long Baseline Array (VLBA).

Extragalactic radio-sources baseline interferometr↗
NASA NTRS1994

Earth Rotation Parameters from DSN VLBI: 1994

In this report, Earth Rotation Parameter (ERP) estimates ahve been obtained from an analysis of Deep Space Network (DSN) VLBI data that directly aligns its celestial and terrestrial reference frames with those of the International Earth Rotation Service (IERS).

Earth rotation TEMPO↗
NASA NTRS1992

Multi-Epoch 8.4GHz VLBI Observations of the Nucleus of Centaurus A

We present the results of several 8.4 GHz VLBI observations of the nucleus of Centaurus A. We fing that the source possesses a classical core-jet structure with the inner portion of the jet expanding at a proper motion of 4.o mas yr or an apparet velocity of 0.26c along the jet.

Nucleus of Centaurus A↗
NASA NTRS1993

Prospects for VLBI Detection of Planets

Astrometric VLBI observations of radio stars are being made to connect the Hipparcos star catalog to the extragalactic radio reference frame. Typically, the antennas are moved between a star and a strong, compact reference source a few degrees away every 2-3 minutes. After correlation, the strong reference source fringes are used to determine the exact delay and rate of the weak radio star fringes, allowing the visibilities to be measured and coherently integrated for the duration of the experiment. As a result accurate astrometry has been possible on radio stars with flux densities as low as 2 mJy...

Jones, D. L.↗
NASA NTRS1993

Sub-Milliarcsecond Astrometry with Phase-Referenced VLBI

Astrometric VLBI observations of radio stars are being made to connect the Hipparcos optical reference frame and the extragalactic radio reference frame. The antennas are switched between a star and a strong, compact reference source a few degrees away every 2-3 minutes. After correlation, the strong reference source fringes are used to determine the exact delay and rate of the weak radio star fringes, allowing the visibilities to be measured and coherently integrated for the duration of the experiment. As a result accurate astrometry has been possible on radio stars with flux densities as low as 2 mJy. All five astrometric parameters (two positions, two proper motions, and one parallax) have been obtained for several stars, with formal errors and epoch-to-epoch residuals less than 1 milliarcsecond.

Jones, D. L.↗