VLBI/e-VLBI An Introduction for Networkers Tasso Tzioumis, ATNF, CSIRO.
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Transcript of VLBI/e-VLBI An Introduction for Networkers Tasso Tzioumis, ATNF, CSIRO.
VLBI/e-VLBI
An Introduction for
Networkers
Tasso Tzioumis, ATNF, CSIRO
Outline
• Caveat: A Basic introduction– Not a review of the latest techniques and
results
• Radio Interferometry & VLBI
• Why: Science with VLBI
• How: Technology
• e-VLBI: Impact
Radio Interferometry
Simple InterferometerSimple Interferometer
Fringe PatternFringe Pattern
• Baseline B: Distance between antennas
• “Virtual” telescope of diameter B.cos (projected baseline)
• Fringe pattern provides information on structure and position of the radio source
Earth Rotation Aperture Synthesisuv- diagram
• Baseline length and orientation (as viewed from the source) changes as the Earth rotates new information on source structure.• uv-diagram - an indicator of imaging “quality” of an array of antennas
• more antennas filled uv better image fidelity
Connected Element Arrays
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VLA
• Baselines up to 10s of kms• “Real-time” detections• Full-time operation
ATCA
MERLIN
• Baselines 5-200 kms• Radio-linked “real-time” Operation• e-MERLIN - fibre links under construction
VLBI Arrays
LBA
x New Norcia
x NTD
VSOP
Resolution Resolution = Observing wavelength / Telescope diameterAngularResolution
Optical (5000A)Diameter Instrument
Radio (4cm)Diameter Instrument
1′ 2mm Eye 140m GBT+1″ 10cm Amateur Telescope 8km VLA-B0.″05 2m HST 160km MERLIN0.″001 100m Interferometer 8200km VLBI
Jupiter and Io as seen from Earth1 arcmin 1 arcsec 0.05 arcsec 0.001 arcsec
Simulated with Galileo photo
Atmosphere gives 1" limit without corrections which are easiest in radio
Why?
Unique VLBI ScienceZooming in!
Cen A
Active Galactic NucleusModel
Hercules A
3C236
Superluminal motion
Wide-field Imaging - surveying
Gravitational lensingDouble-quasar 0957+561 - VLBA+EVN, 18cm
PKS1830-211Einstein RingMERLIN, 5cm
NGC 4258
• Galaxy with disk• Radio continuum jet• Jet on one side obscured• H2O masers• Continuum amplifies maser
emission (in green)• Tangential to disk maser
emission – faint red & blue spots at Keplerian (point mass) rotation
• First real measurement of nuclear Black Hole mass
• Add time dimension (4D): geometric distance!
– Image courtesy: Lincoln Greenhill
M82 Starburst
SN1993J
Bartel et al
Mira Variable TX Cam• 43 GHz SiO maser
emission around a star
• No continuum emission at all
• Actually many frequencies with masers; composite
• movie!– Image courtesy: Phil Diamond
& Athol Kembal
SS433• X-ray binary
• Precessing jets
• 0.26c jet speed
• Baryonic jets
Model
Movie of VLBIObservations
Astrometry & Geodesy
Baseline Length
Baseline transverse
10 cm
10 cm
1984-1999
• Fundamental reference frames – International Celestial Reference
Frame (ICRF)– International Terrestrial Reference
Frame (ITRF)– Earth rotation and orientation relative
to inertial reference frame of distant quasars
• Tectonic plate motions measured directly• Earth orientation data used in studies of
Earth’s core and Earth/atmosphere interaction
• General relativity tests – Solar bending significant over whole
sky
SGR A* - The Galactic CentreMeasures rotation of the Milky Way Galaxy
Spacecraft Navigation• Astrometry relative to background radio
sources• Can measure micro-arcsecond position
differences
Huygens spacecraft at Titan:–January 2005, VLBI tracking–Determine probe position during descent–Accuracy ~1 km–Fringes detected but data still being reduced
How? - current systems• Data recorded on
tape or disk systems at < 1 Gbps
• Transported (slow!) to correlator facilities
• Data processing by correlator
VLBI Recorders - Mkx
S2 VLBI RecorderLBA Disk system
The Future
e-VLBI
e-VLBI global data transport
e-VLBI Science Impact• Real-time operation (cf ATCA, VLA,…)
– Fast response to “targets of opportunity” like flaring or exploding stars
– Monitoring of evolving events– Immediate assessment of results
• Higher sensitivity from high data rates– imaging sources at the edge of the universe– Very high quality imaging– (very efficient way to increase sensitivity cf building larger
antennas)
• Support high data rates of processed data – Facilitate “wide-field” imaging– Utilise GRID computing? – Database “mining”
SKA - an e-VLBI array?
1Tbit/s data transportrequirement in inner array
100 Gbit/s data transportrequirement in outer array
SKA
Operational Impact• Flexible scheduling
– Fast response to astronomical events
• Robust operation– Real-time performance monitoring
• Immensely easier data transport
• Remote antenna operation
• Remote data analysis
• Distribution of processed data to users
Lower operating costs?
Summary
• VLBI offers a unique look at the universe - a “zoom” camera
• e-VLBI will revolutionise VLBI operations
• e-VLBI will enhance VLBI sensitivity, response time and flexibility
• SKA will be an e-VLBI array• Networking is the future for VLBI
VLBA
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The VLBAThe VLBA
Ten 25m Antennas, 20 Station Correlator327 MHz - 86 GHz
National RadioAstronomy Observatory
A Facility of the National Science
Foundation
EVN
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Kx recorders