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Precise astrometry11/10/2023 arXiv:0707.0558Īsaki Y, Maud LT, Fomalont EB, Phillips NM, Hirota A, Sawada T, Barcos-Muñoz L, Richards AMS, Dent WRF, Takahashi S, Corder S, Carpenter JM, Villard E, Humphreys EM (2020) ALMA high-frequency long baseline campaign in 2017: band-to-band phase referencing in submillimeter waves. Īsaki Y, Sudou H, Kono Y, Doi A, Dodson R, Pradel N, Murata Y, Mochizuki N, Edwards PG, Sasao T, Fomalont EB (2007) Verification of the effectiveness of VSOP-2 phase referencing with a newly developed simulation tool ARIS. arXiv:1808.10636Īsaki Y, Saito M, Kawabe R, Morita KI, Sasao T (1996) Phase compensation experiments with the paired antennas method. arXiv:1711.10120Īn T, Jaiswal S, Mohan P, Zhao Z, Lao B (2019) A cosmic microscope to probe the Universe from Present to Cosmic Dawn: dual-element low-frequency space VLBI observatory. arXiv:1510.05817Īlgaba JC, Lee SS, Kim DW, Rani B, Hodgson J, Kino M, Trippe S, Park JH, Zhao GY, Byun DY, Gurwell M, Kang SC, Kim JY, Kim JS, Kim SW, Lott B, Miyazaki A, Wajima K (2018) Exploring the variability of the flat spectrum radio source 1633+382. Īlgaba JC, Zhao GY, Lee SS, Byun DY, Kang SC, Kim DW, Kim JY, Kim JS, Kim SW, Kino M, Miyazaki A, Park JH, Trippe S, Wajima K (2015) Interferometric monitoring of gamma-ray bright active galactic nuclei II: frequency phase transfer. In: 14th European VLBI network symposium and users meeting, p 081. Kluwer, Dordrecht, p 523Īlef W, Tuccari G, Dornbusch S, Wunderlich M, Pantaleev M, Flygare J, Tercero F, Schoonderbeek G, Hargreaves J, de Wild R, Bezrukovs V, D GJ, López-Pérez JA (2018) BRAND-the next generation receiver for VLBI. In: Reid MJ, Moran JM (eds) The impact of VLBI on astrophysics and geophysics, IAU symposium, vol 129. Īlef W (1988) Test of phase-reference mapping for switched observations. These will enable the addressing of a host of innovative open scientific questions in astrophysics.Ībellán FJ, Martí-Vidal I, Marcaide JM, Guirado JC (2018) Core-shifts and proper-motion constraints in the S5 polar cap sample at the 15 and 43 GHz bands. We foresee a revolution coming from: ultra-high-precision radio astrometry, large surveys of many objects, improved sky coverage, and at new frequency bands other than those available today. Based on these perspectives, the future of radio astrometry is bright. ![]() We review the small but growing number of major astrometric surveys in the radio, to highlight the scientific impact that such projects can provide. The next-generation methods are fundamental in allowing this. One of the key potentials is that astrometry will become generally applicable, and, therefore, unbiased large surveys can be performed. The next generation of methods will allow ultra-precise astrometry to be performed at a much wider range of frequencies (hundreds of MHz to hundreds of GHz). From the historical development, we predict the future potential astrometric performance, and, therefore, the instrumental requirements that must be provided to deliver these. ![]() We review the opportunities provided by the next generation of instruments coming online, which are primarily: SKA, ngVLA, and pathfinders, along with EHT and other (sub)mm-wavelength arrays, Space-VLBI, Geodetic arrays, and optical astrometry from GAIA. ![]() ![]() We cover the developments that have been fundamental to allow high accuracy and precision astrometry to be regularly achieved. We present a technique-led review of the progression of precise radio astrometry, from the first demonstrations, half a century ago, until to date and into the future.
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