Radio Astronomy – VLBI Technique Maria J

Advanced Topic in Astrophysics, Lecture 4!

Radio Astronomy – VLBI technique Maria J. Rioja, ICRAR, UWA Outline!

What is VLBI?!

From connected interferometry to VLBI!

Spatial Resolution with VLBI !

Sensitivity with VLBI! Radio Telescopes: Resoluon

• Resolving power (how small of a thing you can “see”) depends on the size of the telescope and the wavelength of the light

For radio waves, this λ is large… size So this must also be large

• “Size” = diameter of telescope for single dish; maximum distance between telescopes for arrays Radio Telescopes: Resoluon

Green Bank Telescope, WV Very Large Array, NM

Size

Size

Single Dish Connected Arrays European VLBI Network!

Very Long Baseline Interferometry!

p.5 VLBI array Beyond Earth limitaons: Space VLBI – VSOP What is VLBI? (Very Long Baseline Interferometry)

• Radio interferometry with unlimited baselines – For high resoluon – milliarcsecond (mas) or beer – Baselines up to an Earth diameter for ground based VLBI – Can extend to space (VSOP) • Tradionally uses no IF or LO link between antennas – Atomic clocks for me and frequency– usually hydrogen masers – Disk based systems to record data – Delayed correlaon, aer media for data storage shipped – Real me over fiber is a reality now! • Can use antennas built for other reasons • Not fundamentally different from linked interferometry

VLBI ‐‐ Craig Walker Synthesis Imaging Summer 7 School 2002 What is VLBI?!

DELAY

D Processing of VLBI observations! What is VLBI?! (Very Long Baseline Interferometry)!

• Radio interferometry with unlimited baselines – For high resoluon – milliarcsecond (mas) or beer – Baselines up to an Earth diameter for ground based VLBI – Can extend to space (HALCA) • Tradionally uses no IF or LO link between antennas – Atomic clocks for me and frequency– usually hydrogen masers – Disk based systems to record data – Delayed correlaon, aer media for data storage shipped – Real me over fiber is a reality now! • Can use antennas built for other reasons • Not fundamentally different from linked interferometry

VLBI ‐‐ Craig Walker Synthesis Imaging Summer 10 School 2002 DATA REDUCTION! VLBI vs LINKED INTERFEROMETRY! • VLBI is not fundamentally different from linked interferometry • Differences are a maer of degree – Separate clocks allow rapid changes in instrumental phase – Independent atmospheres give rapid phase variaons and large gradients • Different source elevaons exacerbate the effect – Sources bright enough to be both easily detectable and compact to VLBI are small, highly energec, and variable • There are no flux calibrators • There are no polarizaon posion angle calibrators • There are no good point source amplitude calibrators – Model uncertaines are can be large • Source posions, staon locaons, and the Earth orientaon are difficult to determine to a small fracon of a wavelength – Oen use antennas not designed for interferometry. Not very phase stable

VLBI ‐‐ Craig Walker Synthesis Imaging Summer 11 School 2002 VLBI arrays like the EVN & VLBA have most of their telescopes located in the Northern hemisphere. The uv-coverage for sources in the southern sky (-ve declinations) is poor. The EVN can make use of telescopes located in the Southern hemisphere at European longitudes e.g. South africa: UV Coverages = Fourier sampling!

At lower source declinationsEVN + (< VLBA +15 degrees)! the coverage of the EVN + VLBAEVN array (“Global+ SouthAfrica VLBI”) becomes! foreshortened (above left), resulting in an increasingly elongatedEVN beam and poorer uv-coverage. For the EVN this can be improved in the N-S direction by including Hartebeesthoek, in South Africa (above right). UV coverage for VSOP observations!

Space Baseline length: 400 x 106 x 6 cm = 24000 km

Resoluon = 1/ (400 e6) rad = = 0.5 mas VLBI provides…..

HIGHER SPATIAL RESOLUTION: High fidelity imaging and high precision astrometry – What they look like and where they are

TRADE‐OFF WITH SENSITIVITY: Targets: Very bright, compact e.g.: Acve Galacc Nuclei (AGNs), astrophysical masers THE QUEST FOR RESOLUTION

Atmosphere gives 1" limit without corrections which are easiest in radio

Jupiter and Io as seen from Earth 1 arcmin 1 arcsec 0.05 arcsec 0.001 arcsec

Simulated with Galileo photo Radio jets & Black Hole physics Cygnus A

VLA

Jet = collimang ejecta that have opening angles =< 15o

VLBI offers highest resolution! What is Sensivity & Why Should You Care? • Measure of weakest detectable radio emission • Important throughout research program – Technically sound observing proposal – Sensible error analysis in publicaon • Expressed in units involving Janskys – Unit for interferometer is Jansky (Jy) – Unit for synthesis image is Jy beam‐1 • 1 Jy = 10‐26 W m‐2 Hz‐1 = 10‐23 erg s‐1 cm‐2 Hz‐1 • Common to use milliJy or microJy

J.M. Wrobel ‐ 19 June 2002 17 SENSITIVITY Sensivity – Antenna Performance

• One antenna

– System temperature Tsys – Gain G • Overall antenna performance is measured by “System Equivalent Flux Density” (SEFD):

SEFD = Tsys /G – Units Jy

€Credit: J.M. Wrobel Interferometer Sensivity • Antennas performance

– SEFDi = Tsysi / Gi and SEFDj = Tsysj / Gj – Each antenna collects bandwidth • Interferometer built from these antennas has – Accumulaon me , system efficiency – Sensivity

Credit: J.M. Wrobel Interferometer Sensivity

• For SEFDi = SEFDj = SEFD drop subscripts

[Units Jy]

Image Sensivity

. Interferometer sensivity

• No. of interferometers

• Sensivity of synthesis image:

Units Jy beam‐1

How affects Image Sensivity?

• Eg: VLBA connuum, 8.4 GHz – Observed ‐1 • T: Ipeak = 2 milliJy beam • B: Gaussian noise = 90 microJy beam‐1

– Posion error from sensivity?

• Gaussian beam = 1.5 milliarcsec • Then = 34 microarcsec • Other posion errors dominate

Credit: J.M. Wrobel Radio Telescopes: Sensivity • Sensivity (how faint of a thing you can “see”) depends on how much of the area of the telescope/array is actually collecng data – VLA B‐array: Total telescope collecng area is only 0.02% of land area • More spread‐out arrays can only image very bright, compact sources Brightness Temperature Sensivity

• Tb sensivity = Tbs × Filling Factor

– Tbs = Tb sensivity of equivalent area single dish

Filling factor ∝1/ D2 so VLBI can only see very “Bright” sources

Credit: C.Walker

VERA : VLBI Exploraon of Radio Astrometry Construcon completed in 2002 Regular observaons from 2004

Mizusawa

Iriki

Ishigaki‐jima Ogasawara

Target sources : Galacc masers (H2O@22GHz, SiO@43GHz) New aspect: dual‐beam for phase‐referencing Very Long Baseline Array (VLBA)

• Larger arrays give you beer and beer resoluon • Trade‐off with sensivity (collecng area stays the same Size while diameter increases) END!

Next lesssons! Monday next week:! - VLBI Science, by Phil Diamond (2pm - 3pm)! - VLBI Astrometry, by Maria Rioja (3pm – 4pm)! Location: ICRAR/UWA!

March 29 ,Board room of the ICRAR/Curtin Brodie-Hall ! Building at 1 Turner Ave, Technology Park, Bentley!