Data & Inference

Statistical reasoning, measurement uncertainty, and the connection between data and physical models. Learn how astronomers extract meaning from observations.

4 exhibits
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Suggested sequence

Not mandatory, but this order builds concepts incrementally.

  1. Parallax Distance: Measuring the Stars 12 min
  2. Doppler Shift of Light 14 min
  3. Cluster Census: Sampling Stars from the Initial Mass Function 15 min
  4. Galaxy Rotation Curves 16 min

Parallax Distance: Measuring the Stars

Key idea: This demo makes the full causal chain legible: Earth moves, line-of-sight changes, and the target star appears to shift against fixed backgr

This demo makes the full causal chain legible: Earth moves, line-of-sight changes, and the target star appears to shift against fixed backgr

Data & Inference 10–20 min Both
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Galaxy Rotation Curves

Key idea: Explore why spiral-galaxy rotation curves stay nearly flat at large radius and what that implies about dark matter across scales.

Explore why spiral-galaxy rotation curves stay nearly flat at large radius and what that implies about dark matter across scales.

near-ready GalaxiesCosmologyData & Inference 10–20 min Both
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Key concepts

Learning goals aggregated from all exhibits in this topic.

  • Describe the initial mass function as a distribution, and state that low-mass stars dominate by number.
  • Explain why the most massive star in a cluster varies a lot between clusters of the same size.
  • Read a cluster's age from the main-sequence turnoff.
  • Distinguish a model's output from the range over which the model is valid.
  • Relate radial motion to observed wavelength and frequency shifts in spectral lines.
  • Interpret redshift z and convert between z and radial velocity with the correct formula.
  • Decide when non-relativistic Doppler is acceptable and when relativistic Doppler is required.
  • Use lab-vs-observed spectral comparisons to infer motion direction and speed.
  • Interpret galaxy rotation curves as velocity-versus-radius observables inferred from Doppler measurements.
  • Compare visible-matter-only Keplerian predictions to flat observed curves and infer missing mass.
  • Relate bulge, disk, and halo component models to total curve shape and enclosed-mass growth.
  • Use baryon fraction and dark-to-visible ratio readouts to reason about mass budgets at large radius.
  • Trace causality: Earth moves in orbit, line-of-sight changes, apparent star position shifts.
  • Infer parallax from two captures using measured shift and effective baseline.
  • Connect smaller inferred parallax to larger inferred distance.
  • Describe why uncertainty and weak baseline geometry limit inference quality.

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