Very Long Baseline Interferometry with the SKA

Paragi, Zsolt; Godfrey, L.; Reynolds, C.; Rioja, María; Deller, Adam; Zhang, Bo; Gurvits, Leonid; Bietenholz, M. F.; Szomoru, Arpad; Bignall, Hayley; Boven, Paul; Charlot, P.; Dodson, Richard; Frey, Sándor; Garrett, M. A.; Imai, Hiroshi; Lobanov, A. P.; Reid, M. J.; Ros, E.; Langevelde, H. J. van; Zensus, J. A.; Zheng, Xing Wu; Alberdi, A.; Agudo, I.; An, Tao; Argo, M. K.; Beswick, R.; Biggs, A. D.; Brunthaler, A.; Campbell, R. M.; Cimò, G.; Colomer, F.; Corbel, S.; Conway, J.; Cseh, D.; Deane, Roger; Falcke, H.; Gabányi, K. É.; Gawroński, M.; Gaylard, M. J.; Giovannini, G.; Giroletti, M.; Goddi, C.; Goedhart, S.; Gómez, José L.; Gunn, Alastair G.; Kharb, P.; Klöckner, Hans-Rainer; Körding, Elmar; Kovalev, Yurii Yu.; Kunert-Bajraszewska, M.; Lindqvist, Michael; Lister, M. L.; Mantovani, F.; Martí-Vidal, Iván; Mezcua, Mar; McKean, J. P.; Middelberg, E.; Miller-Jones, J. C. A.; Moldón, J.; Muxlow, T. W. B.; O’Brien, T. J.; Pérez-Torres, M. Á.; Pogrebenko, S. V.; Quick, J.; Rushton, A.; Schilizzi, R. T.; Smirnov, O.; Sohn, Bong Won; Surcis, G.; Taylor, G. J.; Tingay, Steven; Tudose, V.; Horst, Alexander van der; Leeuwen, J. van; Venturi, T.; Vermeulen, R. C.; Vlemmings, Wouter; Witt, Aletha de; Wucknitz, O.; Yang, Jun

doi:10.22323/1.215.0143

Cited by 40 publications

(36 citation statements)

References 66 publications

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“…Deller et al 2013). In addition to being an independent source of information, unaffected by low-frequency GWs, VLBI astronomy gives higher precision than is possible via timing in almost all cases (see Paragi et al 2015, for more details). A caveat is that at present transferral from the ICRF to the Solar system barycentric frame reduces the usefulness of the VLBI-derived reference position values, as the uncertainty in the frame tie (presently ∼milliarcseconds) is orders of magnitude larger than the formal uncertainty (but see however the third point below).…”

Section: The Role Of Vlbimentioning

confidence: 99%

Gravitational Wave Astronomy with the SKA

Janssen¹,

Hobbs

McLaughlin

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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On a time scale of years to decades, gravitational wave (GW) astronomy will become a reality. Low frequency (∼10 −9 Hz) GWs are detectable through long-term timing observations of the most stable pulsars. Radio observatories worldwide are currently carrying out observing programmes to detect GWs, with data sets being shared through the International Pulsar Timing Array project. One of the most likely sources of low frequency GWs are supermassive black hole binaries (SMBHBs), detectable as a background due to a large number of binaries, or as continuous or burst emission from individual sources. No GW signal has yet been detected, but stringent constraints are already being placed on galaxy evolution models. The SKA will bring this research to fruition. In this chapter, we describe how timing observations using SKA1 will contribute to detecting GWs, or can confirm a detection if a first signal already has been identified when SKA1 commences observations. We describe how SKA observations will identify the source(s) of a GW signal, search for anisotropies in the background, improve models of galaxy evolution, test theories of gravity, and characterise the early inspiral phase of a SMBHB system. We describe the impact of the large number of millisecond pulsars to be discovered by the SKA; and the observing cadence, observation durations, and instrumentation required to reach the necessary sensitivity. We describe the noise processes that will influence the achievable precision with the SKA. We assume a long-term timing programme using the SKA1-MID array and consider the implications of modifications to the current design. We describe the possible benefits from observations using SKA1-LOW. Finally, we describe GW detection prospects with SKA1 and SKA2, and end with a description of the expectations of GW astronomy.Advancing Astrophysics with the Square Kilometre Array

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Section: The Role Of Vlbimentioning

confidence: 99%

Gravitational Wave Astronomy with the SKA

Janssen¹,

Hobbs

McLaughlin

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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351

302

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“…Precision astrometry seemed to be under-represented (Paragi et al 2015;Loinard et al 2015;Green et al 2015). Over the last decade, the VLBA and EVN have demonstrated the power of precision astrometry in areas of Galactic structure, star formation, pulsars, and cosmology.…”

Section: What Was Missing?mentioning

confidence: 99%

Square Kilometre Array key science: a progressive retrospective

Carilli¹

2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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I summarize the science drivers presented at the workshop for Phase I of the Square Kilometre Array: 'Advancing Astrophysics with the Square Kilometre Array'. I build from the historical perspective of the original Key Science programs: 'Science with a Square Kilometre Array', and consider progress in astrophysics since 2004. I then present my 'score card' of the primary science drivers proposed by the Science Working Groups, and further developed in the white papers and presentations at the meeting, assuming a conservative high frequency of 3GHz. The science case for the SKA phase I is compelling, with the right mix of killer applications (eg. pulsars and gravity, 21cm cosmology), foundational radio astronomy (eg. cosmic magnetism, baryon cycle, high energy phenomena), and high risk-high return 'game-changing' programs (eg. fast radio bursts, BAO intensity mapping, SETI). A strong case was made at the conference for band 5 (4 to 15GHz), in particular in the area of planet formation and exobiology. Such a capability engages the rapidly growing exoplanet community, and enables fundamental break-throughs in most of the key science areas. The case for real-time data spigots that allow for commensal observing is also strong. Ultimately, the greatest discoveries that will come from the SKA are likely even richer still, and beyond prognostication.

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“…The general requirements for VLBI with the SKA are detailed in Paragi et al (2015), but here we highlight specific requirements relevant for astrometric maser measurements, both in the 'traditional' sense of phase referencing and in the 'multi-view' sense of in-beam calibration. The antenna positions must be accurately known (to a precision of a few millimetres) and there must be adequate calibrator sources with precise positions (positional accuracies of ≤1 milliarcsecond when used for removing the differential atmospheric delay residual).…”

Section: The Requirements For Vlbi Maser Astrometry With the Skamentioning

confidence: 99%

“…Honma et al 2008), to maximise the improved astrometry the SKA will facilitate. As described in Paragi et al (2015), VLBI with the SKA will utilise multiple beams for calibration, which will aid the atmospheric calibration with in-beam phase referencing, providing an alternative to the 'traditional' process described above, significantly reducing overheads (which often exceed 50%). The experiments described in Sections 3 and 4 assume this 'multi-view' method of observing.…”

Section: The Requirements For Vlbi Maser Astrometry With the Skamentioning

confidence: 99%

“…The second phase of the SKA (SKA2) has the prospect to allow for studies of water (H 2 O) masers (at 22.235 GHz). This frequency coverage, in joint operation with one or more Very Long Baseline Interferometry (VLBI) network(s) (Paragi et al 2015), will allow revolutionary science to be done in the field of Galactic and extragalactic structure and dynamics during all phases of the SKA.…”

Section: Introductionmentioning

confidence: 99%

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Maser Astrometry with VLBI and the SKA

Green¹,

Langevelde²,

Brunthaler³

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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We discuss the unique opportunities for maser astrometry with the inclusion of the Square Kilometre Array (SKA) in Very Long Baseline Interferometry (VLBI) networks. The first phase of the SKA will enable observations of hydroxyl and methanol masers, positioning the latter to an accuracy of 5 microarcseconds, and the second phase may allow water maser observations. These observations will provide trigonometric distances with errors as small as 1%. The unrivalled sensitivity of the SKA will enable large-scale surveys and, through joint operations, will turn any VLBI network into a fast astrometry device. Both evolved stars and high mass star formation regions will be accessible throughout the (Southern) Milky Way, completing our understanding of the content, dynamics and history of our Galaxy. Maser velocities and proper motions will be measurable in the Local Group of galaxies and beyond, providing new insights into their kinematics and evolution.Advancing Astrophysics with the Square Kilometre Array

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Very Long Baseline Interferometry with the SKA

Cited by 40 publications

References 66 publications

Gravitational Wave Astronomy with the SKA

Gravitational Wave Astronomy with the SKA

Square Kilometre Array key science: a progressive retrospective

Maser Astrometry with VLBI and the SKA

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