Interferometry And Synthesis In Radio Astronomy

2016

1,188 citations recorded by the source corpus.

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Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8a8a07caf24a425c942ef5225f48b3bfc3b2cd63

Citations in the corpus

• BlackHoleCam: Fundamental physics of the galactic center (2016, background): “In the presence of strong magnetic fields, a massive supply of ordered vertical magnetic flux builds-up near the BH until reaching saturation; as a consequence, the MRI is marginally suppressed and the accreting material enters the so-called magnetically arrested disk (MAD) state.(125,156) To determ”
• SURVEYING THE BRIGHT STARS BY OPTICAL INTERFEROMETRY. I. A SEARCH FOR MULTIPLICITY AMONG STARS OF SPECTRAL TYPES F-K (2016, background): “However, the finite bandwidth of our beam combiner’s 16 spectral channels reduces visibility contrast, and, as is wellknown from radio interferometry, it produces radial smearing over a large interferometric field of view (Bridle & Schwab 1999; Thompson et al. 2001).”
• A Circumplanetary Disk around PDS70c (2021, background): “We note that the nominal positional accuracy is defined as beamFWHM/S/N/0.9 (Thompson et al. 2017, and ALMA Cycle 8 2021 Technical Handbook), with 0.9 a factor to account for a nominal 10% signal decorrelation.”
• 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).”
• Multi-Person Localization via RF Body Reflections (2015, methodology): “In the radio astronomy community, these techniques are referred to as CLEAN algorithms and, similarly, have a large number of instantiations [14, 29, 30].”
• Imaging the Schwarzschild-radius-scale Structure of M87 with the Event Horizon Telescope Using Sparse Modeling (2017, methodology): “In particular, this is a serious problem in VLBI observations performed at different sites (see Thompson et al. 2001).”
• Hydrogen Epoch of Reionization Array (HERA) (2016, background): “Since the thermal noise per visibility baseline may be expressed as VN = ( 2kB λ2 )( Tsys√ 2Bt ) ΩbB (3) where t is the integration time (see e.g. Thompson et al. 2001), to determine the sensitivity of an instrument to the power spectrum per baseline we can substitute the thermal noise per baseline…”
• First light for GRAVITY: Phase referencing optical interferometry for the Very Large Telescope Interferometer (2017, methodology): “At this time radio interferometry was already well advanced with first imaging synthesis arrays and with very long baseline interferometry (VLBI) for highest angular resolution and astrometry (see, e.g., Thompson et al. 2017, and references therein).”
• First M87 Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole (2019, neutral): “2 The array has a nominal angular resolution of λ / L , where λ is the observing wavelength and L is the maximum projected baseline length between telescopes in the array ( Thompson et al. 2017 ) .”