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Journal articles on the topic 'Very long baseline interferometry'

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Published: 4 June 2021
Last updated: 29 July 2024

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1

Schilizzi, R. T. "Very long baseline interferometry." Radio Science 21, no. 4 (July 1986): 665–79. http://dx.doi.org/10.1029/rs021i004p00665.

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2

Moran, J. M. "Very Long Baseline Interferometry." Highlights of Astronomy 8 (1989): 553–54. http://dx.doi.org/10.1017/s1539299600008303.

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The technique of very long baseline interferometry (VLBI) has undergone two decades of steady growth and refinement since its inception in 1967. In the beginning, only crude measurements of visibility on single baselines were possible. Now 18-station arrays have been used to produce images with dynamic ranges exceeding 2000:1; relative motions of cosmic masers have been tracked at the microarcsecond level of accuracy; and angular size measurements have been made with baseline lengths up to 2 two earth diameters with an orbiting satellite as a receiving element.
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3

McAlister, Harold A. "Overview of Multiple–Aperture Interferometry Binary Star Results from the Northern Hemisphere." Proceedings of the International Astronomical Union 2, S240 (August 2006): 35–44. http://dx.doi.org/10.1017/s1743921307003778.

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AbstractLong-baseline optical interferometry (LBI) can nearly close the gap in selection space between astrometric and spectroscopic detection of binary star systems, bringing the complementary powers of astrometry and spectroscopy to bear on a complete dynamical understanding of such systems, particularly including the determination of the masses of the individual stellar components. In the case of double-lined spectroscopic systems, their resolution by long-baseline interferometry also yields the orbital parallax and hence the luminosities of the individual stars. In some of these cases, the angular diameters of one or more components are accessible, and so a complete specification of a star in terms of its mass, radius and luminosity is made.The northern hemisphere is now equipped with several interferometers of unprecedented capability in terms of their baseline sizes, numbers of telescopes and telescope apertures. These instruments, most notably the Palomar Testbed Interferometer at Mt. Palomar Observatory, have produced very significant results of a number of interesting systems fulfilling interferometry's promise to produce fundamental astrophysical data at levels of accuracy that challenge or confirm astrophysical theory.This paper presents basic principles of long-baseline interferometric study of binary stars and summarizes results from northern interferometers with specific examples of their broad impact on binary star astronomy.
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4

Schilizzi, R. T. "Very Long Baseline Interferometry (VLBI)." Europhysics News 19, no. 4 (1988): 46–52. http://dx.doi.org/10.1051/epn/19881904046.

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5

Stee, Ph, D. Bonneau, F. Morand, D. Mourard, and F. Vakili. "Current studies and future prospects in stellar-structure imaging with the GI2T." Symposium - International Astronomical Union 176 (1996): 191–98. http://dx.doi.org/10.1017/s0074180900083224.

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The capability of optical long baseline interferometry for measuring the angular diameter of stars or binary separation is now well established. However, for the imaging of photospheric disk structures one needs very long baseline interferometers operated in the multi-telescope phase-closure technique. In this paper we will stress the capability of spectro-interferometric measurements to constrain the physics of hot stars. We will report our study of the interacting binary, β Lyrae, and the mass-losing Be star γ Cassiopeiae. We will look at the interpretation of both the modulus and phase data recorded by the long baseline interferometer GI2T in the southern France. The performances and limitations of spectro-interferometric techniques will also be discussed through some of the most exciting prospects within the reach of current interferometers.
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6

Chesneau, O., K. Rousselet-Perraut, and F. Vakili. "Interferometry and Stellar Magnetism." International Astronomical Union Colloquium 175 (2000): 174–77. http://dx.doi.org/10.1017/s0252921100055792.

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AbstractThe classical detection of magnetic fields in Be stars remains a challenge due to the sensitivity threshold and geometrical cancelation of the field effects. We propose to study the Zeeman effect using Spectro-Polarimetric INterferometry (SPIN) which consists of the simultaneous use of polarimetry and very high angular resolution provided by long baseline interferometers. As monitoring of the instrumental polarisation is mandatory in order to calibrate interferometric observations in any case, the polarised signal is a natural by-product of interferometers. This method will be tested on the GI2T interferometer thanks to its high spectral resolution and its polarimetric capabilities.
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7

Tomasi, P., T. Clark, and J. Campbell. "Measurement technique. Very long baseline interferometry." Journal of Geodynamics 25, no. 3-4 (May 1998): 179–93. http://dx.doi.org/10.1016/s0264-3707(97)00034-3.

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8

Robertson, Douglas S. "Geophysical applications of very-long-baseline interferometry." Reviews of Modern Physics 63, no. 4 (October 1, 1991): 899–918. http://dx.doi.org/10.1103/revmodphys.63.899.

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9

Carter, W. E., and D. S. Robertson. "Very-Long-Baseline Interferometry Applied to Geophysics." Symposium - International Astronomical Union 156 (1993): 133–44. http://dx.doi.org/10.1017/s0074180900173115.

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Very-long-baseline Interferometry (VLBI) has opened for study a broad new spectrum of geophysical phenomena including: direct observation of the tectonic motions and deformations of the Earth's crustal plates, observations of unprecedented detail of the variations in the rotation of the Earth, and direct measurement of the elastic deformations of the Earth in response to tidal forces. These new measurements have placed significant constraints on models of the interior structure of the Earth; for example, measurements of the variations in the Earth's nutation have been shown to be particularly sensitive to the shape of the core-mantle boundary. The VLBI measurements will allow us to construct a global reference frame accurate at the centimeter level. Such a frame will be essential to studying long-term global changes, especially those changes related to sea-level variations as recorded by tide gauge measurements.
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10

ACCIOLY, ANTONIO, JOSÉ HELAYËL-NETO, and ESLLEY SCATENA. "PHOTON MASS AND VERY LONG BASELINE INTERFEROMETRY." International Journal of Modern Physics D 19, no. 14 (December 2010): 2393–403. http://dx.doi.org/10.1142/s021827181001844x.

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A relation between the photon mass, its frequency, ν, and the deflection parameter, γ, determined by experimentalists (that characterizes the contribution of space curvature to gravitational deflection) is found. This amazing result allows us to conclude that the knowledge of the parameters ν and γ is all we need to set up gravitational bounds on the photon mass. By considering as inputs the most recent measurements of the solar gravitational deflection of radio waves obtained via the Very Long Baseline Interferometry, upper bounds on the photon mass are estimated.
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11

Teke, Kamil, Emine Tanır Kayıkçı, Johannes Böhm, and Harald Schuh. "Modelling Very Long Baseline Interferometry (VLBI) observations." Journal of Geodesy and Geoinformation 1, no. 1 (2012): 17–26. http://dx.doi.org/10.9733/jgg.120512.1.

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12

Pyne, Ted, Carl R. Gwinn, Mark Birkinshaw, T. Marshall Eubanks, and Demetrios N. Matsakis. "Gravitational Radiation and Very Long Baseline Interferometry." Astrophysical Journal 465 (July 1996): 566. http://dx.doi.org/10.1086/177443.

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13

An, Tao, Xiaoyu Hong, Weimin Zheng, Shuhua Ye, Zhihan Qian, Li Fu, Quan Guo, et al. "Space very long baseline interferometry in China." Advances in Space Research 65, no. 2 (January 2020): 850–55. http://dx.doi.org/10.1016/j.asr.2019.03.030.

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14

Fallon, F. W., and W. H. Dillinger. "Crustal velocities from geodetic very long baseline interferometry." Journal of Geophysical Research 97, B5 (1992): 7129. http://dx.doi.org/10.1029/92jb00351.

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15

Wietfeldt, R. D., D. Baer, W. H. Cannon, G. Feil, R. Jakovina, P. Leone, P. S. Newby, and H. Tan. "The S2 very long baseline interferometry tape recorder." IEEE Transactions on Instrumentation and Measurement 45, no. 6 (1996): 923–29. http://dx.doi.org/10.1109/19.543987.

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16

Bietenholz, M. F., A. M. Soderberg, and N. Bartel. "VERY-LONG-BASELINE INTERFEROMETRY OBSERVATIONS OF SN 2008D." Astrophysical Journal 694, no. 1 (February 23, 2009): L6—L10. http://dx.doi.org/10.1088/0004-637x/694/1/l6.

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17

Carter, William E., and Douglas S. Robertson. "Studying the Earth by Very-Long-Baseline Interferometry." Scientific American 255, no. 5 (November 1986): 46–54. http://dx.doi.org/10.1038/scientificamerican1186-46.

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18

Gurvits, L. I., K. I. Kellermann, and S. Frey. "Measuring Cosmological Parameters with Very Long Baseline Interferometry." Symposium - International Astronomical Union 183 (1999): 67. http://dx.doi.org/10.1017/s0074180900132127.

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Very Long Baseline Interferometry (VLBI) allows us to study a core of AGN with a sub-parsec resolution. We analyze the dependencies “apparent angular size – redshift” and “apparent motion – redshift” which contain an imprint of the source's properties and cosmology. We present data on the “angular size – redshift” relation obtained with VLBI at 5 GHz on a sample of 300 AGN distributed over the widest available range of redshifts 0.016 ≤ z ≤ 4.5. The sample exceeds those used in similar studies earlier by Kellermann (1993, 79 sources) and Wilkinson et al. (1997, 160 sources). Unlike extended source, the angular size-redshift for compact radio sources appears consistent with the predictions of standard Friedmann world models with qo ≃ 0.5 without taking into account evolutionary effects or selection effects due to a “linear size – luminosity” or “linear size – spectral index” dependences. We discuss different approaches allowing us to disentangle intrinsic evolutionary properties of sources and parameters of the cosmological model. Recent estimates of parameters of the cosmological model are given. We also discuss a perspective of conclusive cosmological tests using the VLBI technique.
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19

Robertson, D. S. "The Astrometric Possibilities of Very-Long-Baseline Interferometry." Symposium - International Astronomical Union 109 (1986): 143–55. http://dx.doi.org/10.1017/s007418090007649x.

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In the application of Very-Long-Baseline Interferometry (VLBI) to astrometric problems the fundamental observable is the difference in the arrival times of a wavefront at two widely separated receiving stations. Since the radio sources being observed are sufficiently distant that the arriving wavefront can be considered to be a plane wave, the differential arrival time is a measure of the component of the baseline in the direction of the source. Equivalently, if the baseline is known, the differential arrival time is sufficient to determine a circle on the sky containing the source. It is easy to show that a minimum of ten observations distributed among three different sources is sufficient to determine all of the source coordinates and the baseline coordinates simultaneously (Robertson, 1975).
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20

MacMillan, D. S. "Atmospheric gradients from very long baseline interferometry observations." Geophysical Research Letters 22, no. 9 (May 1, 1995): 1041–44. http://dx.doi.org/10.1029/95gl00887.

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21

Lambert, S. B., and C. Le Poncin-Lafitte. "Determining the relativistic parameterγusing very long baseline interferometry." Astronomy & Astrophysics 499, no. 1 (April 1, 2009): 331–35. http://dx.doi.org/10.1051/0004-6361/200911714.

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22

Takahashi, F., T. Kondo, Y. Takahashi, and Y. Koyama. "Very long baseline interferometer." IEEE Aerospace and Electronic Systems Magazine 17, no. 8 (August 2002): 43–44. http://dx.doi.org/10.1109/maes.2002.1028083.

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23

Phipps, Jr. "The very long baseline interferometry (VLBI) system’s unfinished business." Physics Essays 23, no. 1 (March 1, 2010): 206–8. http://dx.doi.org/10.4006/1.3311821.

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24

Martellosio, Andrea, Marco Pasian, Remi Rayet, Steve Rawson, and Thomas Bonhoure. "Wideband Cryogenic Receiver for Very Long Baseline Interferometry Applications." IEEE Antennas and Wireless Propagation Letters 17, no. 2 (February 2018): 275–78. http://dx.doi.org/10.1109/lawp.2017.2785958.

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25

Clivati, Cecilia, Giovanni A. Costanzo, Matteo Frittelli, Filippo Levi, Alberto Mura, Massimo Zucco, Roberto Ambrosini, et al. "A coherent fiber link for very long baseline interferometry." IEEE Transactions on Ultrasonics, Ferroelectrics, and Frequency Control 62, no. 11 (November 2015): 1907–12. http://dx.doi.org/10.1109/tuffc.2015.007221.

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26

MacMillan, D. S., and C. Ma. "Evaluation of very long baseline interferometry atmospheric modeling improvements." Journal of Geophysical Research: Solid Earth 99, B1 (January 10, 1994): 637–51. http://dx.doi.org/10.1029/93jb02162.

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27

Herring, T. A. "Submillimeter horizontal position determination using very long baseline interferometry." Journal of Geophysical Research: Solid Earth 97, B2 (February 10, 1992): 1981–90. http://dx.doi.org/10.1029/91jb02649.

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28

Heinkelmann, Robert, and Harald Schuh. "Very long baseline interferometry: accuracy limits and relativistic tests." Proceedings of the International Astronomical Union 5, S261 (April 2009): 286–90. http://dx.doi.org/10.1017/s1743921309990524.

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AbstractWe present a review on relativistic effects and best estimates of the relativistic PPN parameter γ obtained by analysis of data from the International VLBI Service for Geodesy and Astrometry (IVS). Relativistic implications are also considered in view of the upcoming new generation VLBI System: VLBI2010.
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29

Spencer, R. E. "Very Long Baseline Interferometry: current status and future prospects." Vistas in Astronomy 34 (January 1991): 61–68. http://dx.doi.org/10.1016/0083-6656(91)90020-s.

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30

Herring, T. A., P. M. Mathews, and B. A. Buffett. "Modeling of nutation-precession: Very long baseline interferometry results." Journal of Geophysical Research: Solid Earth 107, B4 (April 2002): ETG 4–1—ETG 4–12. http://dx.doi.org/10.1029/2001jb000165.

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31

Middelberg, Enno, and Uwe Bach. "High resolution radio astronomy using very long baseline interferometry." Reports on Progress in Physics 71, no. 6 (May 2, 2008): 066901. http://dx.doi.org/10.1088/0034-4885/71/6/066901.

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32

Vennebusch, Markus, Sarah Böckmann, and Axel Nothnagel. "The contribution of Very Long Baseline Interferometry to ITRF2005." Journal of Geodesy 81, no. 6-8 (November 23, 2006): 553–64. http://dx.doi.org/10.1007/s00190-006-0117-x.

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33

Emardson, T. R., G. Elgered, and J. M. Johansson. "External atmospheric corrections in geodetic very-long-baseline interferometry." Journal of Geodesy 73, no. 7 (August 25, 1999): 375–83. http://dx.doi.org/10.1007/s001900050256.

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34

Hyland, L. J., M. J. Reid, S. P. Ellingsen, M. J. Rioja, R. Dodson, G. Orosz, C. R. Masson, and J. M. McCallum. "Inverse Multiview. I. Multicalibrator Inverse Phase Referencing for Microarcsecond Very Long Baseline Interferometry Astrometry." Astrophysical Journal 932, no. 1 (June 1, 2022): 52. http://dx.doi.org/10.3847/1538-4357/ac6d5b.

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Abstract Very Long Baseline Interferometry (VLBI) astrometry is a well established technique for achieving ±10 μas parallax accuracies at frequencies well above 10 GHz. At lower frequencies, uncompensated interferometer delays associated with the ionosphere play the dominant role in limiting the astrometric accuracy. Multiview is a novel VLBI calibration method, which uses observations of multiple quasars to accurately model and remove time-variable, directional-dependent changes to the interferometer delay. Here we extend the Multiview technique by phase-referencing data to the target source (“inverse Multiview”) and test its performance. Multiple observations with a four-antenna VLBI array operating at 8.3 GHz show single-epoch astrometric accuracies near 20 μas for target–reference quasar separations up to about 7°. This represents an improvement in astrometric accuracy by up to an order of magnitude compared to standard phase-referencing.
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35

Gabányi, K. É., S. Frey, S. Satyapal, A. Constantin, and R. W. Pfeifle. "Very long baseline interferometry observation of the triple AGN candidate J0849+1114." Astronomy & Astrophysics 630 (September 23, 2019): L5. http://dx.doi.org/10.1051/0004-6361/201936519.

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Context. In the hierarchical structure formation model, galaxies grow through various merging events. Numerical simulations indicate that mergers can enhance the activity of central supermassive black holes in galaxies. Aims. A system of three interacting galaxies, called J0849+1114, has recently been identified and multi-wavelength evidence of all three galaxies containing active galactic nuclei has recently been found. The system has substantial radio emission; we aim to investigate the origin of this radio emission with a high-resolution radio interferometric observation and to discover whether it is related to star formation or to one or more of the active galactic nuclei in the system. Methods. We performed high-resolution continuum observation of J0849+1114 with the European Very Long Baseline Interferometry Network at 1.7 GHz. Results. We detected one compact radio emitting source at the position of the easternmost nucleus. Its high brightness temperature and radio power indicate that the radio emission originates from a radio-emitting active galactic nucleus. Additionally, we found that significant amount of flux density is contained in ∼100 milliarcsec-scale feature related to the active nucleus.
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36

Domiciano de Souza, A., J. Zorec, S. Jankov, F. Vakili, and L. Abe. "Modelling Stellar Rotation for Optical Long Baseline Interferometry." Symposium - International Astronomical Union 215 (2004): 187–88. http://dx.doi.org/10.1017/s007418090019552x.

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Optical long baseline interferometry is a technique sensitive to sky projected brightness distributions, constituting a powerful tool for the study of detailed stellar surface structures. Moreover, by combining high spectral and angular resolution we obtain a technique called differential interferometry that is also sensitive to mechanisms that induce chromatic signatures, such as stellar spots and large scale mass motions (e.g. rapid rotation, non-radial pulsations, shear currents produced by hydrodynamical instabilities). We present here a study of the signatures of stellar rotation on differential interferometry observables showing that they are very sensitive to differential rotation and stellar inclination.
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37

Veres, Patrik Milán, Krisztina Éva Gabányi, and Sándor Frey. "Very Long Baseline Interferometry Observations of the Proposed Radio Counterpart of an EGRET Source." Symmetry 12, no. 9 (September 15, 2020): 1516. http://dx.doi.org/10.3390/sym12091516.

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We present high-resolution radio interferometric imaging observations of the radio source NVSS J182659+343113 (hereafter J1826+3431), the proposed radio counterpart of the γ-ray source, 3EG J1824+3441 detected by the Energetic Gamma Ray Experiment Telescope (EGRET) on board the Compton Gamma Ray Observatory satellite. We analyzed eight epochs of archival multi-frequency very long baseline interferometry data. We imaged the asymmetric core–jet structure of the source, and detected apparent superluminal motion in the jet. At the highest observing frequency, 15.3 GHz, the core shows high brightness temperature indicating Doppler boosting. Additionally, the radio features undergo substantial flux density variability. These findings strengthen the previous claim of the association of the blazar J1826+3431 with the possible γ-ray source, 3EG J1824+3441.
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38

Broderick, Avery E., Dominic W. Pesce, Paul Tiede, Hung-Yi Pu, and Roman Gold. "Hybrid Very Long Baseline Interferometry Imaging and Modeling with themis." Astrophysical Journal 898, no. 1 (July 17, 2020): 9. http://dx.doi.org/10.3847/1538-4357/ab9c1f.

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39

MacMillan, D. S., and John M. Gipson. "Atmospheric pressure loading parameters from very long baseline interferometry observations." Journal of Geophysical Research: Solid Earth 99, B9 (September 10, 1994): 18081–87. http://dx.doi.org/10.1029/94jb01190.

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40

Herring, T. A. "Precision of vertical position estimates from Very Long Baseline Interferometry." Journal of Geophysical Research 91, B9 (1986): 9177. http://dx.doi.org/10.1029/jb091ib09p09177.

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41

Hummel, C. A., J. T. Armstrong, A. Quirrenbach, D. F. Buscher, D. Mozurkewich, N. M. ,. II Elias, and R. E. Wilson. "Very high precision orbit of Capella by long baseline interferometry." Astronomical Journal 107 (May 1994): 1859. http://dx.doi.org/10.1086/116995.

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42

Robertson, Douglas S., Jim R. Ray, and William E. Carter. "Tidal variations in UT1 observed with very long baseline interferometry." Journal of Geophysical Research: Solid Earth 99, B1 (January 10, 1994): 621–36. http://dx.doi.org/10.1029/93jb03178.

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43

Doeleman, Sheperd, Tao Mai, Alan E. E. Rogers, John G. Hartnett, Michael E. Tobar, and Nitin Nand. "Adapting a Cryogenic Sapphire Oscillator for Very Long Baseline Interferometry." Publications of the Astronomical Society of the Pacific 123, no. 903 (May 2011): 582–95. http://dx.doi.org/10.1086/660156.

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44

Robertson, D. S., W. E. Carter, J. Campbell, and H. Schuh. "Daily Earth rotation determinations from IRIS very long baseline interferometry." Nature 316, no. 6027 (August 1985): 424–27. http://dx.doi.org/10.1038/316424a0.

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45

Lu, R. S., T. P. Krichbaum, and J. A. Zensus. "High-frequency very long baseline interferometry studies of NRAO 530." Monthly Notices of the Royal Astronomical Society 418, no. 4 (November 18, 2011): 2260–72. http://dx.doi.org/10.1111/j.1365-2966.2011.19537.x.

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46

Kiuchi, H. "Parallel bit stream correlation system for very long baseline interferometry." Radio Science 40, no. 5 (October 2005): n/a. http://dx.doi.org/10.1029/2005rs003282.

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47

Molotov, I., A. Kovalenko, V. Samodurov, B. Lipatov, A. Dementiev, A. Antipenko, S. Snegirev, et al. "INTERNATIONAL LOW-FREQUENCY VERY-LONG-BASELINE INTERFEROMETRY NETWORK PROJECT MILESTONES." Astronomical & Astrophysical Transactions 22, no. 4-5 (August 2003): 743–52. http://dx.doi.org/10.1080/10556790310001609205.

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48

Lavallée, D., and G. Blewitt. "Degree-1 Earth deformation from very long baseline interferometry measurements." Geophysical Research Letters 29, no. 20 (October 2002): 28–1. http://dx.doi.org/10.1029/2002gl015883.

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49

Jankov, S. "Astronomical optical interferometry, II: Astrophysical results." Serbian Astronomical Journal, no. 183 (2011): 1–35. http://dx.doi.org/10.2298/saj1183001j.

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Optical interferometry is entering a new age with several ground- based long-baseline observatories now making observations of unprecedented spatial resolution. Based on a great leap forward in the quality and quantity of interferometric data, the astrophysical applications are not limited anymore to classical subjects, such as determination of fundamental properties of stars; namely, their effective temperatures, radii, luminosities and masses, but the present rapid development in this field allowed to move to a situation where optical interferometry is a general tool in studies of many astrophysical phenomena. Particularly, the advent of long-baseline interferometers making use of very large pupils has opened the way to faint objects science and first results on extragalactic objects have made it a reality. The first decade of XXI century is also remarkable for aperture synthesis in the visual and near-infrared wavelength regimes, which provided image reconstructions from stellar surfaces to Active Galactic Nuclei. Here I review the numerous astrophysical results obtained up to date, except for binary and multiple stars milliarcsecond astrometry, which should be a subject of an independent detailed review, taking into account its importance and expected results at microarcsecond precision level. To the results obtained with currently available interferometers, I associate the adopted instrumental settings in order to provide a guide for potential users concerning the appropriate instruments which can be used to obtain the desired astrophysical information.
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50

Ipatov, A. V., I. A. Bezrukov, A. G. Mikhailov, A. I. Sal’nikov, I. Yu Belousov, Yu A. Mironov, A. A. Manzarov, and M. B. Petelina. "An electronic-very long baseline interferometry mode on the quasar-KVO radio interferometric complex." Instruments and Experimental Techniques 56, no. 5 (September 2013): 536–39. http://dx.doi.org/10.1134/s0020441213050163.

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