ASTR 472 · Lecture 08

Lecture 08: Calibration II: Error Budgets and Imaging Systematics

Radio Astronomy

A formal image rms is not a complete uncertainty when the flux scale, primary beam, and deconvolution add correlated errors.

Objectives and route

  1. Propagate independent fractional calibration terms in quadrature.
  2. Separate thermal noise from multiplicative and spatially correlated systematics.
  3. Design residual and jackknife checks for a calibrated image.

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

Thermal noise

Definition: Random receiver and sky fluctuations that average down approximately with the square root of independent samples.

Why it matters here: It is needed to answer Two sources share the same 5% flux-scale error but have independent 1% thermal errors. Which uncertainty cancels in their flux ratio, and which does not? and to interpret Independent small fractional errors combine in quadrature, whereas shared calibration errors correlate many image pixels.

Relationships: Use it with Jackknife test and Flux-scale uncertainty; the lecture model is \(\left(\frac{\sigma_S}{S}\right)^2=\sum_j f_j^2+2\sum_{i<j}\rho_{ij}f_i f_j\).

Boundary or common confusion: Quadrature is justified only for independent zero-mean errors; common-mode flux-scale uncertainty requires covariance-aware comparisons.

Observation before interpretation

A formal image rms is not a complete uncertainty when the flux scale, primary beam, and deconvolution add correlated errors.

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

Physical model

For a derived flux S=f(x_i), first-order propagation gives sigma_S^2=sum_i (partial f/partial x_i)^2 sigma_i^2 plus covariance terms. For independent fractional terms f_j, (sigma_S/S)^2=sum_j f_j^2. A multiplicative flux-scale term remains correlated among sources calibrated with the same solution and should not be averaged down as independent pixel noise.

\(\left(\frac{\sigma_S}{S}\right)^2=\sum_j f_j^2+2\sum_{i<j}\rho_{ij}f_i f_j\)

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

Worked calculation

Inputs: S=120 mJy; independent 5%, 3%, and 2% terms.

sigma_S = 7.397 mJy; fractional uncertainty = 0.06164; sigma_S = 7.397 mJy

Quadrature is justified only for independent zero-mean errors; common-mode flux-scale uncertainty requires covariance-aware comparisons.

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

Read the geometry or data relation

thermalgain termscommon scalecovariance changes the total
Independent small fractional errors combine in quadrature, whereas shared calibration errors correlate many image pixels.

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

Where the inference can fail

Quadrature is justified only for independent zero-mean errors; common-mode flux-scale uncertainty requires covariance-aware comparisons.

Reasoning prompt

Two sources share the same 5% flux-scale error but have independent 1% thermal errors. Which uncertainty cancels in their flux ratio, and which does not?

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

Connection to the observing workflow

This lecture feeds into the paired lab: Complex Gain Calibration and Error Propagation. 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

Calibration II: Error Budgets and Imaging Systematics 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 Spectral-Line Observing and Doppler Inference.

References and scope

NRAO VLA calibration and imaging-pipeline documentation; exact error propagation is developed here beyond introductory textbook coverage.

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.