A short history of space VLBI

Schilizzi, R. T.

doi:10.22323/1.163.0010

Cited by 4 publications

(3 citation statements)

References 7 publications

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“…The early history of space VLBI is described in references [12] and [13]. After the successful participation in the Japanese VSOP-HALCA mission, JIVE and ASTRON staff led by Leonid Gurvits were also eager to contribute to the Russian RadioAstron mission when it was finally launched in 2011.…”

Section: Space Vlbimentioning

confidence: 99%

Very Long Baseline Interferometry: the EVN, WSRT, and JIVE

Langevelde¹,

Schilizzi²,

Ardenne³

et al. 2019

Proceedings of Westerbork Telescope 50th Anniversary — PoS(Westerbork)

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Section: Space Vlbimentioning

confidence: 99%

Very Long Baseline Interferometry: the EVN, WSRT, and JIVE

Langevelde¹,

Schilizzi²,

Ardenne³

et al. 2019

Proceedings of Westerbork Telescope 50th Anniversary — PoS(Westerbork)

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“…In particular it is very powerful for near-field correlation to measure spacecraft signals. This technique could be useful to help the correlation of Space VLBI data such as from the current RadioAstron mission [7][3] [10].…”

Section: Next Generation Correlatormentioning

confidence: 99%

Future of VLBI

Langevelde¹,

Jan²

2012

Proceedings of Resolving the Sky - Radio Interferometry: Past, Present and Future — PoS(RTS2012)

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Almost two decades after the establishment of the Joint Institute for VLBI in Europe (JIVE), the European VLBI Network is a thriving scientific infrastructure with a significant user community and a healthy proposal pressure. It offers opportunities to address a breadth of important scientific topics, which feature in national and European astronomy roadmaps. Most of these science themes call for further enhancements of the sensitivity and image quality delivered by VLBI networks. The exceptional progress of e-VLBI over the last five years demonstrates how sensitive VLBI should be done in the future. At the same time JIVE is pushing the technology for large capacity correlators that can connect VLBI networks with many elements in real-time. Indeed, many new initiatives to build or outfit telescopes for VLBI are emerging from around the world. The technological VLBI developments have a great synergy with the SKA preparations. This is recognized in the SKA pathfinder role that e-VLBI has in the European VLBI Network for exploring connectivity and real-time science techniques. Moreover, VLBI with its locally visible elements offers great possibilities for training and outreach. With the new scientific capabilities, especially those complementary to other SKA pathfinders, VLBI will be a flourishing scientific instrument for the future.Resolving the Sky -Radio Interferometry: Past, Present and Future

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“…Since the early detection and imaging of the compact core and radio jet in M87 by VLBI technique (e.g., Reid et al 1982), the source has been observed by modern VLBI facilities, to study the structure, dynamics, and physical origin of the jet (see, e.g., Event Horizon Telescope Collaboration et al 2019 and references therein). Along with those studies, decades-long efforts have been made to improve angular resolution toward M87 by adopting orbiting antenna as a VLBI station, thus realizing a space VLBI array with a virtual aperture larger than the Earth diameter (see, e.g., Burke 2009;Hirabayashi 2012;Schilizzi 2012;Gurvits 2020;Gurvits et al 2021 for a review). Previous space VLBI programs including tests with the NASA Tracking and Data Relay Satellite System (Levy et al 1986(Levy et al , 1989Linfield et al 1989Linfield et al , 1990 and the VLBI Space Observatory Programme (Hirabayashi et al 1998(Hirabayashi et al , 2000 provided not only proof of the concept but also the possibility of imaging M87 at exceptionally high angular resolution (e.g., Dodson et al 2006).…”

Section: Introductionmentioning

confidence: 99%

RadioAstron Space VLBI Imaging of the Jet in M87. I. Detection of High Brightness Temperature at 22 GHz

Kim

Savolainen

Voitsik

et al. 2023

ApJ

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We present results from the first 22 GHz space very long baseline interferometric (VLBI) imaging observations of M87 by RadioAstron. As a part of the Nearby AGN Key Science Program, the source was observed in 2014 February at 22 GHz with 21 ground stations, reaching projected (u, v) spacings up to ∼11 Gλ. The imaging experiment was complemented by snapshot RadioAstron data of M87 obtained during 2013–2016 from the AGN Survey Key Science Program. Their longest baselines extend up to ∼25 Gλ. For all of these measurements, fringes are detected only up to ∼2.8 Earth diameter or ∼3 Gλ baseline lengths, resulting in a new image with angular resolution of ∼150 μas or ∼20 Schwarzschild radii spatial resolution. The new image not only shows edge-brightened jet and counterjet structures down to submilliarcsecond scales but also clearly resolves the VLBI core region. While the overall size of the core is comparable to those reported in the literature, the ground-space fringe detection and slightly superresolved RadioAstron image suggest the presence of substructures in the nucleus, whose minimum brightness temperature exceeds T B , min ∼ 10 12 K. It is challenging to explain the origin of this record-high T B , min value for M87 by pure Doppler boosting effect with a simple conical jet geometry and known jet speed. Therefore, this can be evidence for more extreme Doppler boosting due to a blazar-like small jet viewing angle or highly efficient particle acceleration processes occurring already at the base of the outflow.

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A short history of space VLBI

Cited by 4 publications

References 7 publications

Very Long Baseline Interferometry: the EVN, WSRT, and JIVE

Very Long Baseline Interferometry: the EVN, WSRT, and JIVE

Future of VLBI

RadioAstron Space VLBI Imaging of the Jet in M87. I. Detection of High Brightness Temperature at 22 GHz

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