Interferometry and Synthesis in Radio Astronomy

By J. Baars. 2017

1,694 citations recorded by the source corpus.

Preface to the Second Edition. Preface to the First Edition. Introduction and Historical Review. Introductory Theory of Interferometry and Synthesis Imaging. Analysis of the Interferometer Response. Geometric Relationships and Polarimetry. Antennas and Arrays. Response of the Receiving System. Design of the Analog Receiving System. Digital Signal Processing. Very-Long-Baseline Interferometry. Calibration and Fourier Transformation of Visibility Data. Deconvolution, Adaptive Calibration, and Applications. Interferometer Techniques for Astrometry and Geodesy. Propagation Effects. Van Cittert-Zernike Theorem, Spatial Coherence, and Scattering. Radio Interference. Related Techniques. Principal Symbols. Author Index. Subject Index.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ad342b248088268a31b542c4c3b21bd555882d1d

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In Astronomy and Astrophysics

1. L. Hernquist
2. P. Hopkins
3. Ramesh Narayan
4. E. Quataert
5. Volker Springel
6. R. Genzel
7. A. Dekel
8. T. Johannsen

Citations in the corpus

• DiFX-2: A More Flexible, Efficient, Robust, and Powerful Software Correlator (2011, methodology): “Thompson et al. (1994) contains a detailed explanation of the challenges inherent in wide– field imaging.”
• THE PRECISION ARRAY FOR PROBING THE EPOCH OF RE-IONIZATION: EIGHT STATION RESULTS (2009, methodology): “Gain Linearization Mitigating the effects of data quantization in the PAPER correlator requires that power levels be carefully set for optimal SNR and that output data be converted to a linear power scale (see Ch. 8 of Thompson et al. (2001)).”
• THz imaging and sensing for security applications—explosives, weapons and drugs (2005, methodology): “It can be shown that the mutual coherence function of the electric fields at detector placements r1 = (x1 ,y 1) and r2 = (x2 ,y 2) can be written as [58, 62 ]”
• CASA, the Common Astronomy Software Applications for Radio Astronomy (2022, background): “Radio astronomy is a discipline that heavily relies on computational resources to image the sky at wavelengths ranging from roughly 10m - 300µm (e.g., Condon & Ransom 2016; Thompson et al. 2017).”
• DETECTING FLARING STRUCTURES IN SAGITTARIUS A* WITH HIGH-FREQUENCY VLBI (2008, background): “constant sampling rate, 2-bit quantization achieves sensi tivity levels very nearly approaching that of 1-bit quantization at half the observing bandwidth ( Thompson et al. 2001 ), which is limited by the hardware at certain telescopes (§3.2).”
• The visibility function in interferometric aperture synthesis radiometry (2004, methodology): “The term in (6) is the radiometric antenna temperature seen by the receiver in the conditions of Fig. 1 and in (7) a correlation temperature called visibility due to the similarity of the term used in radioastronomy [ 16 ].”
• Optical interferometry in astronomy (2003, background): “We refer the reader to Thompson et al. (2001) for a discussion of the development of radio interferometry beginning with the first radio interferometer built by Ryle and Vonberg in 1946.”
• The Atacama Large Millimeter/Submillimeter Array (2009, background): “, [35], or to improve the separation in 2SB front ends.”
• VLBA Determination of the Distance to Nearby Star-forming Regions. II. Hubble 4 and HDE 283572 in Taurus (2007, background): “This task provides an estimate of the position error (cols. [3] and [5] of Table 1) based on the expected theoretical astrometric precision of an interferometer: ¼ k 2 B 1 SNR ; ð1Þ where k is the wavelength, B the baseline, and SNR the image signal-to-noise ratio (Thompson et al. 1986).”
• Foregrounds for observations of the cosmological 21 cm line - I. First Westerbork measurements of Galactic emission at 150 MHz in a low latitude field (2009, background): “In the image plane the primary beam represents a simple multiplicative e ff ect whereas it is a convolution in the u v plane (Thompson et al. 1986).”
• First M87 Event Horizon Telescope Results. IV. Imaging the Central Supermassive Black Hole (2019, methodology): “The EHT utilizes standard 2-bit recording, for which ηQ=0.88 (Thompson et al. 2017).”
• Detection of orbital motions near the last stable circular orbit of the massive black hole SgrA* (2018, background): “The corresponding delay measured in an interferometer D = b n0 sin(z0) = b n sin(z) is constant and is equal to the delay in free space (Thompson et al. 2017).”