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The Development of the VLBI2010 Global Observing System (VGOS)
C. Ma, Code 698 and
D. Behrend, NVI Inc.
Solar System Exploration Seminar for the Director of
Science and Exploration Wednesday, August 22, 2012
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Geode7c VLBI: How does it work?
cτ
A network of antennas observes a Quasar
The delay between 7mes of arrival of a signal is measured
Using the speed of light, the delay is interpreted as a distance
The distance is the component of the baseline toward the source
By observing many sources, all components of the baseline can be determined.
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Launch of VGOS in March 2012
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VLBI2010: Why do we need it? • Aging systems
• New technology • New requirements
• phenomena to be observed have magnitudes of a few millimeters mm accuracy!
• VLBI2010: response of the IVS to significantly improve geode7c VLBI and reach this high level of accuracy
• 2003-‐2005: IVS Working Group 3 „VLBI2010“ -‐ goals and requirements
-‐ strategies and recommenda7ons
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IVS WG 3 Final Report
hAp://ivscc.gsfc.nasa.gov/about/wg/wg3/IVS_WG3_report_050916.pdf
• Vision paper • Published Sept 2005
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Goals of the next genera7on system
VLBI2010 Goals
1-‐mm posi3on accuracy (based on a 24-‐hour observaQon)
Con3nuous measurements of sta3on posi3on and EOP
Turnaround 3me to ini3al products < 24-‐hrs
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VLBI2010 – V2C Progress Report " “Design Aspects of the VLBI2010 System”
Current VLBI2010
antenna size 5–100 m dish ~ 12 m dish
slew speed ~20–200 deg/min ≥ 720 deg/min
sensitivity 200–15,000 SEFD ≤ 2,500 SEFD
frequency range S/X band ~2–14 (18) GHz
recording rate 128, 256 Mbps 8–16 Gbps
data transfer usually ship disks, some e-‐transfer
e-‐transfer, e-‐VLBI, ship disks when required
Rp://ivscc.gsfc.nasa.gov/pub/misc/V2C/TM-‐2009-‐214180.pdf
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VGOS Network in 2012
radio telescope
radio telescope
radio telescope
upgrade legacy
twin radio telescope
VLBI2010 very fast
VLBI2010 fast
[Hase et al., 2011]
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VGOS Network in 2017
radio telescope
radio telescope
radio telescope
upgrade legacy
twin radio telescope
VLBI2010 very fast
VLBI2010 fast
[Hase et al., 2011]
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Int’l VLBI Service for Geodesy and Astrometry
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IVS Components (August 2012)
• The IVS currently has about 80 permanent components supported by roughly 40 insQtuQons in 20 countries.
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GGAO 12-‐m antenna
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Odd channels from each pol’n for one band output to each Mk5C.
2 Gigabits/sec recorded on each Mk5C.
Total data rate: 8 Gbps
Feed and LNAs cooled to ~20K
Both senses of linear polarization used Antenna
Control room
RF filter phase/noise cal
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VLBI2010 signal chain
• Cooled broadband QRFH feed and LNAs (Caltech) • UpDown Converters (4) (Haystack)
– Select frequency bands in the range 2 to12 GHz • RDBE digital back ends (4) (Digicom)
– PFB to get 16 32-‐MHz channels (8 from each pol’n) – Noise diode control for power measurement for Tsys – In use by VLBA and NASA
• Mark5C recorder (4) (Conduant) – In use by VLBA and NASA
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Quad-Ridge Flared Horn (Caltech)
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• Antennas – GGAO12M
• 12m VLBI2010 antenna • At Goddard Space Flight Center, Maryland, USA • Full VLBI2010 signal chain
– Wesjord • 18m prime focus antenna • At Haystack Observatory, Massachuseks, USA • Full VLBI2010 signal chain
– Baseline length approximately 600 km.
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Observa7ons
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• Objec7ves – Several hours on one source to check system. – Observe a source with polariza7on rota7on
• Scans – Five minute scans for high SNR – Source 3C345 – Approximately four hours total
• Frequency bands – Con7guous bands spanning 2 GHz: 6.4 – 8.4 GHz
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Observa7ons – 2012 Jan 19
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• Objec7ves – Geode7c schedule – Observe a number of sources over en7re sky
• Scans – 30-‐second observa7ons – 6 hours total
• Frequency bands – Four bands at 3.5, 5.5, 6.6 and 9.6 GHz
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Observa7ons – 2012 May 16
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Fully coherent ionosphere-‐corrected full-‐polariza7on delays using all four RF bands (100 scans, 6 hr) WRMS post-‐fit residuals: 20 ps Posi7on formal errors: 8 mm ver7cal, 2 mm horizontal
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• Twin Telescope Wekzell (Germany), Vertex Antennas
New VLBI2010 antennas: TTW
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Twin Telescope Wekzell, April 2012