Relevant bibliographies by topics / VLBI

Academic literature on the topic 'VLBI'

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Published: 4 June 2021
Last updated: 20 February 2023

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Journal articles on the topic "VLBI"

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Zhang, B., X. W. Zheng, J. L. Li, Y. Xu, and J. F. Wu. "Tropospheric correction in VLBI phase-referencing using GPS data." Proceedings of the International Astronomical Union 3, S248 (October 2007): 212–13. http://dx.doi.org/10.1017/s174392130801911x.

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AbstractComparing the tropospheric zenith delays derived from VLBI and GPS data at VLBA stations collocated with GPS antenna, the systematic biases and standard deviations of the difference are both found to be at the level of a sub-centimeter. Based on this agreement, we used GPS data to correct the tropospheric effects in VLBI phase-referencing, resulting in close peak-to-noise ratios of images after tropospheric correction using GPS and VLBI data.
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Rogers, Alan E. E. "Tape recorders for VLBI." International Astronomical Union Colloquium 131 (1991): 65–75. http://dx.doi.org/10.1017/s0252921100013075.

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AbstractMagnetic tape recorders developed for VLBI have taken advantage of the best available technology to achieve high data rates and large storage capacity. The Mark I, II and III VLBI recording systems have data rates of 0.72, 4 and 224 Mbits/sec respectively. The recorder developed for the VLBA has a data rate of 256 Mbits/sec and can store 5.5 Terabits of data on one tape.
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Murphy, D. W. "Imaging of Extragalactic Radio Sources with the VSOP Space VLBI Mission." Symposium - International Astronomical Union 175 (1996): 531–32. http://dx.doi.org/10.1017/s0074180900081754.

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In September 1996 the first dedicated VLBI spacecraft, VSOP, will be launched. This Japanese spacecraft operating in conjunction with ground-based VLBI arrays such as the EVN or VLBA will enable observers to routinely undertake VLBI observations with maximum baseline lengths of 2.6 Earth diameters and a resolution of 55 μas at the highest operating frequency of 22 GHz. In this paper we present a brief overview of the imaging capability of the VSOP mission together with an example of an imaging simulation.
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Wietfeldt, R. D., and L. R. D’Addario. "Compatibility issues in VLBI." International Astronomical Union Colloquium 131 (1991): 98–101. http://dx.doi.org/10.1017/s0252921100013130.

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AbstractNew VLBI systems are under development in many countries in preparation for large dedicated arrays, including orbiting radio telescopes to be launched in the 1990s. In particular, several new recording systems and correlators are being constructed: the VLBA in the U.S., the S2 in Canada, and the K4/VSOP in Japan. This paper reviews the issues of technical compatibility among these systems in an effort to facilitate global VLBI experiments.
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Kemball, A. J., and P. J. Diamond. "Continuum VLBI Polarimetry of 3C454.3 at 43 GHz." Symposium - International Astronomical Union 175 (1996): 33–34. http://dx.doi.org/10.1017/s0074180900079900.

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Polarization VLBI calibration at high frequencies has traditionally been difficult due to poor sensitivity and high antenna instrumental polarization across inhomogeneous networks. The higher observing frequency and increased spatial resolution diminishes the chances of finding ideal VLBI polarization calibrators. The advent of the Very Long Baseline Array (VLBA), which has standardized feeds with low instrumental polarization, has minimized these observational difficulties. Recent work in polarization calibration has suggested that somewhat resolved sources may be used in an iterative polarization calibration scheme (Cotton 1993). A full generalization of this method has been developed by Leppanen, Zensus and Diamond (1995) in calibrating 22 GHz polarization observations with the VLBA.
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Kovalev, Y. Y., D. C. Gabuzda, T. P. Krichbaum, W. Alef, and A. Witzel. "A Multi-Frequency VLBI Total Intensity and Polarization Study of the BL Lacertae Object 0716+714." International Astronomical Union Colloquium 164 (1998): 173–74. http://dx.doi.org/10.1017/s0252921100045061.

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AbstractNew polarization-sensitive global VLBI and VLBA images of the BL Lacertae object 0716+714 at 6 cm (1991.4) and 3.6 cm/1.3 cm (1994.2) are presented. The source shows a compact, one-sided core–jet structure in structural position angle ~ 13°. The 3.6 cm total intensity image shows the jet beginning to curve toward the arcsecond-scale structure, which lies in position angle ~ −45°. Comparison with previously published data suggests that the apparent velocity of a 6 cm jet component is > 1.09 ± 0.15c, if the red shift of 0716+714 is z > 0.3. Linear polarization from the VLBI core was detected at all three frequencies; in addition, polarization from the innermost jet component was detected at 1.3 cm. This compact jet polarization appears to be quite high, ~ 50%, and to be aligned with the jet direction, which can be understood if it is a transverse shock. The VLBI core polarization at our earlier epoch was perpendicular to the VLBI jet direction, but had rotated to align with the jet direction by the later epoch, about a year later. This rotation may indicate the imminent birth of a new VLBI component (shock).
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Herrera Ruiz, N., E. Middelberg, A. Deller, V. Smolčić, R. P. Norris, M. Novak, I. Delvecchio, et al. "VLBA+GBT observations of the COSMOS field and radio source counts at 1.4 GHz." Astronomy & Astrophysics 616 (August 2018): A128. http://dx.doi.org/10.1051/0004-6361/201832969.

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We present very long baseline interferometry (VLBI) observations of 179 radio sources in the COSMOS field with extremely high sensitivity using the Green Bank Telescope (GBT) together with the Very Long Baseline Array (VLBA) (VLBA+GBT) at 1.4 GHz, to explore the faint radio population in the flux density regime of tens of μJy. Here, the identification of active galactic nuclei (AGN) is based on the VLBI detection of the source, meaning that it is independent of X-ray or infrared properties. The milli-arcsecond resolution provided by the VLBI technique implies that the detected sources must be compact and have large brightness temperatures, and therefore they are most likely AGN (when the host galaxy is located at z ≥ 0.1). On the other hand, this technique only allows us to positively identify when a radio-active AGN is present, in other words, we cannot affirm that there is no AGN when the source is not detected. For this reason, the number of identified AGN using VLBI should be always treated as a lower limit. We present a catalogue containing the 35 radio sources detected with the VLBA+GBT, ten of which were not previously detected using only the VLBA. We have constructed the radio source counts at 1.4 GHz using the samples of the VLBA and VLBA+GBT detected sources of the COSMOS field to determine a lower limit for the AGN contribution to the faint radio source population. We found an AGN contribution of >40−75% at flux density levels between 150 μJy and 1 mJy. This flux density range is characterised by the upturn of the Euclidean-normalised radio source counts, which implies a contribution of a new population. This result supports the idea that the sub-mJy radio population is composed of a significant fraction of radio-emitting AGN, rather than solely by star-forming galaxies, in agreement with previous studies.
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Romney, Jonathan D. "The Very Long Baseline Array." Symposium - International Astronomical Union 129 (1988): 461–68. http://dx.doi.org/10.1017/s0074180900135272.

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The Very Long Baseline Array (VLBA) will be the world's first large-scale dedicated VLBI facility. It is planned as a multipurpose instrument, supporting continuum, spectroscopic, astrometric/geodetic, multi-frequency, bandwidth synthesis, polarization, and pulsar measurements – with a variety of bandwidths, sampling rates, quantization schemes, and multi-band modes. The Array will consist of ten new 25-m precision antennas, in an optimized geographical configuration. Extremely low-noise receivers will support observations with dual polarization in nine frequency bands from 330 MHz to 43 GHz, including almost all conventional VLBI bands. A wideband, high-density recording system will allow unattended operation at a sustained data rate of 128 Mbit/s for 24 hours, and peak rates up to 512 Mbit/s. The VLBA correlator, planned as a 20-station system to support processing of all observations involving the Array, will be by far the largest ever built for VLBI. The Array will be operated remotely, from a new operations and data-reduction center to be built in Socorro, NM.
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Britzen, S., R. C. Vermeulen, G. B. Taylor, R. M. Campbell, I. W. Browne, P. Wilkinson, T. J. Pearson, and A. C. S. Readhead. "CJ-F: The Kinematics of 241 AGN." Symposium - International Astronomical Union 205 (2001): 106–9. http://dx.doi.org/10.1017/s0074180900220615.

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We present first results from the analysis of multi-epoch VLBI observations of 241 sources in the CJ-F sample (Caltech Jodrell-Flat-spectrum, Taylor et al. 1996). We have been obtaining 5 GHz VLBI (global and VLBA) snapshot observations of the CJ-F sources (complete with 293 sources) since 1990 in order to create a valid database for thorough statistical tests of pc-scale jet motion in AGN. All 241 CJ-F AGN have been observed at least three times with the VLBA, which enables us to investigate jet component motions and paths. In particular, we concentrate on the analysis of those properties supposed to be essential for gamma-ray production, i.e., superluminal motion and bending.
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Breiding, Peter, Sarah Burke-Spolaor, Tao An, Karishma Bansal, Prashanth Mohan, Gregory B. Taylor, and Yingkang Zhang. "Deep Very Long Baseline Interferometry Observations Challenge Previous Evidence of a Binary Supermassive Black Hole Residing in Seyfert Galaxy NGC 7674." Astrophysical Journal 933, no. 2 (July 1, 2022): 143. http://dx.doi.org/10.3847/1538-4357/ac7466.

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Abstract Previous Ku-band (15 GHz) imaging with data obtained from the Very Long Baseline Array (VLBA) had shown two compact, subparsec components at the location of a presumed kiloparsec-scale radio core in Seyfert galaxy NGC 7674. It was then presumed that these two unresolved and compact components were dual radio cores corresponding to two supermassive black holes (SMBHs) accreting surrounding gas and launching radio-bright relativistic jets. However, utilizing the original VLBA data set used to claim the detection of a binary SMBH, in addition to later multiepoch/multifrequency data sets obtained from both the VLBA and the European very long baseline interferometry (VLBI) network, we find no evidence to support the presence of a binary SMBH. We place stringent upper limits to the flux densities of any subparsec-scale radio cores that are at least an order of magnitude lower than the original VLBI radio-core detections, directly challenging the original binary SMBH detection claim. With this in mind, we discuss the possible reasons for the nondetection of any VLBI radio cores in our imaging, the possibility of a binary SMBH still residing in NGC 7674, and the prospect of future observations shedding further light on the true nature of this active galactic nucleus.
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Dissertations / Theses on the topic "VLBI"

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Casey, Simon Paul. "The development of e-VLBI." Thesis, University of Manchester, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.489523.

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Since its introduction, Very Long Baseline Interferometry has enabled high resolution imaging of astronomical sources. The work presented in this thesis demonstrates the feasibility of transmitting VLBI data over the UDP protocol at constant bit rates. Previously TCP had been used for e-VLBI, but TCP is not a good choice of protocol for an application that requires constant bandwidth.
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Gontier, Graffan Anne-Marie. "Orientation de la Terre par mesure VLBI : contribution à la chaîne d'analyse de VLBI astrométrique GLORIA." Observatoire de Paris (1667-....), 1992. https://hal.science/tel-02095270.

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Ce travail de thèse se situe dans le cadre du développement d'une chaîne originale d'analyse de VLBI (Very Large Baseline Interferometry) astrométrique et géodésique GLORIA (GLObal Radio Interferometric Analysis) par des équipes de l'Observatoire de Paris et de l'Institut Géographique National. Nous avons dans un premier temps développé et testé une modélisation astronomique et géophysique originale dans le cadre de la relativité générale avec une précision de 10 picosecondes. Dans un deuxième temps nous avons utilisé cette modélisation originale pour analyser trois ans d'observations du programme VLBI dédié à l'étude de la rotation terrestre. Nous avons développé un protocole statistique, basé sur des résolutions en norme l1 et en norme l2, permettant de détecter les observations atypiques. Les solutions obtenues, 747 évaluations journalière de temps universel, UT1-TAI, pour 1988-1990, ont une précision de 0,001 qui est celle attendue théoriquement étant donné la stratégie d'observation de ce programme.
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Mignard, François, and Sergei Klioner. "Gaia DR1 compared to VLBI positions." Cambridge University Press, 2017. https://tud.qucosa.de/id/qucosa%3A70690.

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Tsioumis, Anastasios K. "VLBI studies of compact radio sources." Thesis, The University of Sydney, 1987. https://hdl.handle.net/2123/25997.

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Radio observations of a complete sample of 44 flat spectrum southern radio sources plus an additional 11 sources of particular interest are presented. Trends in the properties of the complete sample are discussed. All sources of special interest and 19 of the sources in the complete sample were observed with the Southern Hemisphere VLBI Experiment (SHEVE). This was the first extensive VLBI array in the southern hemisphere and its characteristics are presented in some detail. The data reduction methods and, in particular, the calibration of the large SHEVE dataset are described as this is critical to the quality of the final images. The imaging techniques are illustrated by detailed imaging of the radio source 1934-638. Since few closure phase and closure amplitude relations are present self—calibration methods cannot be employed. It was found that the appropriate imaging method for the SHEVE data was modelfitting with Gaussian components. A detailed image of 1934—638 is presented and the source structure compared with previous VLBI observations. All sources observed in SHEVE were fitted with Gaussian component models. The models are presented in a table and source images shown to illustrate the source structure. The SHEVE data and the fits of the models are also shown. All sources in the complete sample and six of the additional VLBI sources were mapped at low resolution using the Molonglo Observatory Synthesis Telescope (MOST) at 843 MHz and the Fleurs Synthesis Telescope at 1415 MHz. Special techniques were used at both instruments to gain direct access to the higher spatial frequency data and hence increased effective resolution. This is necessary since most of the sources in the sample are compact with little or no arcsecond-level structure. The results are summarised in tables and maps are presented at both frequencies for all sources. In addition, accurate radio positions were measured and were compared with other radio and optical positions. Significant pointing offsets were revealed for both instruments. The present results and other source information were then assembled to construct an extensive data base of source properties. Four new optical identifications were made and all objects but one have been identified except in the region obscured by the galactic plane. The database information was used to search for trends in the properties of the complete sample of radio sources. A brief account is given of the sources not in the complete sample and detailed analysis of two special sources is presentedin two appendices. The thesis concludes with an examination of and suggestions for future VLBI observationsin Australia.
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Doeleman, Sheperd S. (Sheperd Samuel). "Imagining active galactic nuclei with 3mm-VLBI." Thesis, Massachusetts Institute of Technology, 1995. http://hdl.handle.net/1721.1/32655.

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Xu, Wenge Readhead Anthony C. S. Readhead Anthony C. S. "The first Caltech-Jodrell Bank VLBI survey /." Diss., Pasadena, Calif. : California Institute of Technology, 1995. http://resolver.caltech.edu/CaltechETD:etd-10262007-132906.

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Kirsten, Franz [Verfasser]. "Pulsar astrometry with VLBI and beyond / Franz Kirsten." Bonn : Universitäts- und Landesbibliothek Bonn, 2014. http://d-nb.info/1060787172/34.

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Despringre, Vincent. "Observation et modélisation des jets extragalactiques observés en VLBI." Toulouse 3, 1996. http://www.theses.fr/1996TOU30212.

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Les jets extragalactiques sont une des manifestations de l'activite intense de certains noyaux actifs de galaxies. Ce sont de gigantesques ejections de plasma du cur de la galaxie, a des distances atteignant parfois plusieurs centaines de kiloparsecs. La physique qui les entoure reste encore relativement mysterieuse. Le developpement de la vlbi (very large base interferometry) ou interferometrie continentale, a permis d'atteindre une resolution de l'ordre du milliarcseconde. Son utilisation pour l'observation des jets extragalactiques, a abouti a la decouverte de l'existence de jets proche du cur et a l'echelle du parsec. On les appelle des jets vlbi. Le but de cette these est l'etude de ces objets. A l'aide du reseau d'interferometrie continentale europeen, l'evn (europeen vlbi network), et du reseau connecte merlin, j'ai cartographie la radiosource 3c66b a la frequence de 5 ghz. J'ai alors decouvert, au cur de cette source, un jet vlbi jusque la inconnu. Les premieres cartes de ce jet ainsi qu'une etude detaillee de sa structure et des flux emis sont presentees dans cette these. La structure des jets vlbi, a l'echelle du parsec, montre une architecture relativement complexe: ils presentent un certain nombre de nodosites qui se deplacent le long du jet sur des trajectoires non rectilignes avec, parfois, des vitesses superluminiques. J'ai developpe un modele permettant d'expliquer les observations vlbi: les nodosites seraient des nuages relativistes, formes de paires electron-positron, se deplacant sur une trajectoire helicoidale enroulee autour d'un jet, non ou faiblement relativiste. Les premiers resultats de cette simulation ainsi qu'une comparaison aux observations font l'objet de la seconde partie de cette these
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Deller, Adam Travis. "Precision VLBI astrometry instrumentation, algorithms and pulsar parallax determination /." Swinburne Research Bank, 2009. http://hdl.handle.net/1959.3/48485.

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Thesis (PhD) - Faculty of Information and Communication Technology, Faculty of Life and Social Sciences, Swinburne University of Technology, 2009.
Submitted in total fulfilment of the requirements for the degree of Doctor of Philosophy, Faculty of Information and Communication Technology, Swinburne University of Technology, 2009. Typescript. Bibliography: p. 165-186.
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Blecher, Tariq. "MEQSILHOUETTE: a mm-VLBI observation and signal corruption simulator." Thesis, Rhodes University, 2017. http://hdl.handle.net/10962/40713.

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The Event Horizon Telescope (EHT) aims to resolve the innermost emission of nearby supermassive black holes, Sgr A* and M87, on event horizon scales. This emission is predicted to be gravitationally lensed by the black hole which should produce a shadow (or silhouette) feature, a precise measurement of which is a test of gravity in the strong-field regime. This emission is also an ideal probe of the innermost accretion and jet-launch physics, offering the new insights into this data-limited observing regime. The EHT will use the technique of Very Long Baseline Interferometry (VLBI) at (sub)millimetre wavelengths, which has a diffraction limited angular resolution of order ~ 10 µ-arcsec. However, this technique suffers from unique challenges, including scattering and attenuation in the troposphere and interstellar medium; variable source structure; as well as antenna pointing errors comparable to the size of the primary beam. In this thesis, we present the meqsilhouette software package which is focused towards simulating realistic EHT data. It has the capability to simulate a time-variable source, and includes realistic descriptions of the effects of the troposphere, the interstellar medium as well as primary beams and associated antenna pointing errors. We have demonstrated through several examples simulations that these effects can limit the ability to measure the key science parameters. This simulator can be used to research calibration, parameter estimation and imaging strategies, as well as gain insight into possible systematic uncertainties.
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Books on the topic "VLBI"

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Alef, W. European VLBI handbook. Bologna, Italy: Istituto di Radioastronomia del CNR, 1991.

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Clark, T. A. Deformations in VLBI antennas. Greenbelt, Md: National Aeronautics and Space Administration, Goddard Space Flight Center, 1988.

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Kikō), VLBI Gijutsu ni Yoru Uchū Kenkyū Shinpojūmu (2006 Uchū Kōkū Kenkyū Kaihatsu. VLBI Gijutsu ni Yoru Uchū Kenkyū Shinpojūmu. Kanagawa-ken Sagamihara-shi: Uchū Kōkū Kenkyū Kaihatsu Kikō Uchū Kagaku Kenkyū Honbu, 2006.

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Lowe, Stephen T. Theory of post-block 2 VLBI observable extraction. Pasadena, Calif: National Aeronautics and Space Administration, Jet Propulsion Laboratory, California Institute of Technology, 1992.

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Henstock, David Robert. A VLBI search for milliarcsecond-scale gravitational lenses. Manchester: University of Manchester, 1996.

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Lowe, Stephen T. Theory of post-block 2 VLBI observable extraction. Pasadena, Calif: National Aeronautics and Space Administration, Jet Propulsion Laboratory, California Institute of Technology, 1992.

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Reid, Mark J., and James M. Moran, eds. The Impact of VLBI on Astrophysics and Geophysics. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2949-4.

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Lowe, Stephen T. Theory of post-block 2 VLBI observable extraction. Pasadena, Calif: National Aeronautics and Space Administration, Jet Propulsion Laboratory, California Institute of Technology, 1992.

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Mantovani, Franco, and Andrzej Kus, eds. The Role of VLBI in Astrophysics, Astrometry and Geodesy. Dordrecht: Kluwer Academic Publishers, 2005. http://dx.doi.org/10.1007/1-4020-2406-1.

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F, Mantovani, Kus A. J, and North Atlantic Treaty Organization, eds. The role of VLBI in astrophysics, astrometry, and geodesy. Dordrecht: Kluwer Academic, 2004.

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Book chapters on the topic "VLBI"

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Rouan, Daniel. "VLBI." In Encyclopedia of Astrobiology, 1750. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-11274-4_1667.

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Rouan, Daniel. "VLBI." In Encyclopedia of Astrobiology, 2612. Berlin, Heidelberg: Springer Berlin Heidelberg, 2015. http://dx.doi.org/10.1007/978-3-662-44185-5_1667.

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Rouan, Daniel. "VLBI." In Encyclopedia of Astrobiology, 1. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-642-27833-4_1667-2.

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Reynolds, J. E. "VLBI Astrometry." In Very High Angular Resolution Imaging, 437–44. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0880-5_89.

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Wright, Melvyn. "Millimeter VLBI." In Submillimetre Astronomy, 91–92. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-015-6850-0_35.

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Ronnang, B. O. "Geodesy-VLBI Observables." In Very Long Baseline Interferometry, 289–302. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2428-4_15.

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Moran, J. M. "Introduction to VLBI." In Very Long Baseline Interferometry, 27–45. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2428-4_3.

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Fromm, Christian. "VLBI Kinematic Analysis." In Spectral Evolution in Blazars, 59–90. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-10768-4_4.

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Linfield, R. P. "VLBI with TDRSS." In Observatories in Earth Orbit and Beyond, 271–74. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-011-3454-5_30.

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Wresnik, Jörg, Johannes Böhm, and Harald Schuh. "Vienna VLBI Simulations." In Geodetic Reference Frames, 61–65. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00860-3_9.

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Conference papers on the topic "VLBI"

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Molera Calvés, Guifré, Jan Wagner, Jouko Ritakari, and Ari Mujunen. "European 4 Gbps VLBI and e-VLBI." In The 8th International e-VLBI Workshop. Trieste, Italy: Sissa Medialab, 2009. http://dx.doi.org/10.22323/1.082.0083.

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Salnikov, Alexandre, Andrey Finkelstein, Alexander Ipatov, Michael Kaidanovsky, Ilia Bezrukov, Andrey Mikhailov, Igor Surkis, and Elena Skurikhina. "e-VLBI Technology in VLBI Network "Quasar"." In The 8th International e-VLBI Workshop. Trieste, Italy: Sissa Medialab, 2009. http://dx.doi.org/10.22323/1.082.0098.

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Bietenholz, Michael. "Supernova VLBI." In The 9th European VLBI Network Symposium on The role of VLBI in the Golden Age for Radio Astronomy and EVN Users Meeting. Trieste, Italy: Sissa Medialab, 2009. http://dx.doi.org/10.22323/1.072.0064.

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FREY, Sandor. "VLBI surveys." In 8th European VLBI Network Symposium. Trieste, Italy: Sissa Medialab, 2007. http://dx.doi.org/10.22323/1.036.0001.

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Krichbaum, T. P., Uwe Bach, Dave A. Graham, W. Alef, Alan Roy, A. Witzel, Anton Zensus, Michael Bremer, and Savador Sanchez. "Towards mm-VLBI." In The 9th European VLBI Network Symposium on The role of VLBI in the Golden Age for Radio Astronomy and EVN Users Meeting. Trieste, Italy: Sissa Medialab, 2009. http://dx.doi.org/10.22323/1.072.0001.

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Jones, Dayton L. "Low frequency VLBI." In AIP Conference Proceedings Volume 174. AIP, 1988. http://dx.doi.org/10.1063/1.37596.

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Szomoru, Arpad, Huib Jan van Langevelde, Harro Verkouter, Mark Kettenis, Bauke Kramer, Friso Olnon, James Anderson, Cormac Reynolds, Zsolt Paragi, and Mike Garrett. "VLBI in transition." In SPIE Astronomical Telescopes + Instrumentation, edited by Larry M. Stepp. SPIE, 2006. http://dx.doi.org/10.1117/12.671144.

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Doi, Akihiro, Kenta Fujisawa, Keiichiro Harada, Takumi Nagayama, Kousuke Suematsu, Koichiro Sugiyama, Asao Habe, et al. "Japanese VLBI Network." In 8th European VLBI Network Symposium. Trieste, Italy: Sissa Medialab, 2007. http://dx.doi.org/10.22323/1.036.0071.

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van Langevelde, Huib Jan. "Future of VLBI." In Resolving The Sky - Radio Interferometry: Past, Present and Future. Trieste, Italy: Sissa Medialab, 2012. http://dx.doi.org/10.22323/1.163.0048.

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Jung, Tae Hyun, Bong Won Sohn, and Do-Young Byun. "Mm-VLBI Phase correction capability with the korean VLBI Network." In 12th European VLBI Network Symposium and Users Meeting. Trieste, Italy: Sissa Medialab, 2015. http://dx.doi.org/10.22323/1.230.0086.

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Reports on the topic "VLBI"

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Boboltz, David A., Alan L. Fey, Nicole Geiger, Chris Dieck, and David M. Hall. U. S. Naval Observatory VLBI Analysis Center. Fort Belvoir, VA: Defense Technical Information Center, June 2013. http://dx.doi.org/10.21236/ada583997.

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Luzum, Brian, and Axel Nothnagel. Improved UT1 Predictions through Low-Latency VLBI Observations. Fort Belvoir, VA: Defense Technical Information Center, March 2010. http://dx.doi.org/10.21236/ada524037.

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Ruddick, Ryan. 2010 Katherine VLBI Observatory local tie survey : technical report. Geoscience Australia, 2014. http://dx.doi.org/10.11636/record.2014.035.

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Hu, Chenming. VLSI Reliability Research. Fort Belvoir, VA: Defense Technical Information Center, August 1992. http://dx.doi.org/10.21236/ada254883.

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O'Leary, Gerald C. Restructurable VLSI Program. Fort Belvoir, VA: Defense Technical Information Center, March 1985. http://dx.doi.org/10.21236/ada160935.

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O'Leary, Gerald C. Restructurable VLSI Program. Fort Belvoir, VA: Defense Technical Information Center, September 1985. http://dx.doi.org/10.21236/ada165718.

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Pina, Cesar A. ARPA/CSTO Rapid VLSI Implementation. Fort Belvoir, VA: Defense Technical Information Center, July 1993. http://dx.doi.org/10.21236/ada269170.

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Liem, Meei-Chiueh Y. Declarative Descriptions for VLSI Generators. Fort Belvoir, VA: Defense Technical Information Center, June 1986. http://dx.doi.org/10.21236/ada169952.

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Roberts, Richard A. VLSI Implementations for Digital Signal Processing. Fort Belvoir, VA: Defense Technical Information Center, December 1987. http://dx.doi.org/10.21236/ada189612.

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Ringhofer, Christian. Mathematical Models for VLSI Device Simulation. Fort Belvoir, VA: Defense Technical Information Center, November 1987. http://dx.doi.org/10.21236/ada191125.

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