ASTR 472 · Lecture 05

Lecture 05: Interferometry: Coherence and Complex Visibility

Radio Astronomy

A pair of antennas measures a spatial Fourier component of the sky, encoded in a complex correlation.

Objectives and route

  1. Derive the two-element fringe phase from geometric delay.
  2. Interpret complex visibility amplitude and phase for a point-source pair.
  3. Convert baseline in wavelengths to fringe spacing and assess angular sensitivity.

Route: identify what the receiver measures, derive the physical/instrument relation, calculate a scale, then test its assumptions against a diagnostic.

Terms for This Lecture

Complex visibility

Definition: The complex cross-correlation measured by an antenna pair for one projected spatial frequency.

Why it matters here: It is needed to answer A point source moves east by one fringe spacing. What happens to its visibility phase on a fixed baseline? Why does amplitude not change for an ideal point source? and to interpret Correlating voltages preserves phase information that single-dish total-power measurements do not contain.

Relationships: Use it with Fringe phase and Geometric delay; the lecture model is \(V(u,v)=\iint I(l,m)e^{-2\pi i(ul+vm)}\,dl\,dm,\qquad\theta_{\rm fringe}\simeq\lambda/B_{\rm proj}\).

Boundary or common confusion: The flat-sky Fourier relation assumes a narrow field and ignores the w-term; wide-field imaging needs non-coplanar-baseline correction.

Observation before interpretation

A pair of antennas measures a spatial Fourier component of the sky, encoded in a complex correlation.

Keep four layers distinct in your notebook: raw correlation or spectrum, calibrated product, model parameter, and physical claim.

Physical model

For a small sky field (l,m), a baseline vector (u,v) measured in wavelengths yields V(u,v)=integral I(l,m) exp[-2 pi i (u l+v m)] dl dm. For a point source at l0, visibility amplitude is its flux and phase is -2 pi u l0 for a one-dimensional baseline. The fringe spacing is approximately lambda/B_proj; it is not necessarily the final synthesized-beam FWHM.

\(V(u,v)=\iint I(l,m)e^{-2\pi i(ul+vm)}\,dl\,dm,\qquad\theta_{\rm fringe}\simeq\lambda/B_{\rm proj}\)

Define each quantity and convention before substitution. A relation is useful only inside its stated regime.

Worked calculation

Inputs: nu=1.4 GHz, B_proj=3.0 km, source offset=10 arcsec.

fringe spacing = 14.72 arcsec; phase = -244.5 deg (115.5 deg modulo 360)

The flat-sky Fourier relation assumes a narrow field and ignores the w-term; wide-field imaging needs non-coplanar-baseline correction.

Independent audit: carry SI units through the derivation, then check the limiting direction and scale.

Read the geometry or data relation

projected baseline Bsource directionequal-phase wavefronts
Correlating voltages preserves phase information that single-dish total-power measurements do not contain.

Identify what is directly encoded in the figure and which inference requires an instrument model or physical assumption.

Where the inference can fail

The flat-sky Fourier relation assumes a narrow field and ignores the w-term; wide-field imaging needs non-coplanar-baseline correction.

Reasoning prompt

A point source moves east by one fringe spacing. What happens to its visibility phase on a fixed baseline? Why does amplitude not change for an ideal point source?

Write the predicted scaling first; then identify which measurement would falsify it.

Connection to the observing workflow

This lecture feeds into the paired lab: Baseline Geometry and Visibility Sampling. Preserve the raw-to-calibrated-to-inferred chain and carry the same units and assumptions into the analysis.

For a real observation, archive the project identifier, correlator setup, antenna configuration, calibration version, flags, beam, and data-release citation.

Synthesis

Interferometry: Coherence and Complex Visibility is one stage in a measurement chain: celestial signal → antenna and receiver → sampled data → calibration → image/spectrum → uncertainty-aware inference.

Next: connect this result to Aperture Synthesis and Image Formation.

References and scope

OpenStax Astronomy 2e §6.4, especially its discussion of interferometer separation and resolution; ALMA Basics §Interferometry formalizes the visibility transform.

Primary/authoritative material and provenance levels are recorded in ../reference-log.md. Numeric examples are reproducibly calculated by ../src/generate_astr472_package.py; figure geometry is original and lecture-specific.