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SPACETRC / DISCOVERY AND RESEARCH

Astronomy Foundations

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SPACETRC / OPEN LEARNING LAB

Astronomy Foundations

Investigate a scientific question through light, spectra, transits and observation records.

3 LEARNING TRACKS12 SHORT LESSONSTR / EN
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Before you begin 3 questions
What happens to travel time when distance doubles at constant speed?
A 500 nm line is measured at 505 nm. What is z?
Which information best helps locate the same observation?
01

LEARNING OBJECTIVE

Use light as a measure

Distinguish distance from light-travel time.

Not yet practised

An image reaches us after light has travelled. Distance and travel time are different quantities; compare them only after keeping the units consistent.

This exercise assumes a constant distance and the speed of light in vacuum. The actual distance between Earth and a spacecraft may change.

WORKED EXAMPLE / MODELt = d / c

Model example: a 300,000 km distance / 300,000 km/s speed = 1 s. These rounded inputs illustrate the relationship only.

What happens to travel time when distance doubles at constant speed?
Explore the primary source: JPL · Astrodynamic parameters ↗
02

LEARNING OBJECTIVE

Measure a spectral shift

Calculate a dimensionless shift from wavelengths.

Not yet practised

Compare a spectral line’s laboratory and observed wavelengths. Interpreting the shift depends on its physical context.

Here we calculate only z. It is not automatically a distance or a velocity valid in every regime. The line must first be identified correctly.

WORKED EXAMPLE / MODELz = (λobs − λrest) / λrest

Teaching inputs: 500 nm → 505 nm. z = (505 − 500)/500 = 0.01. Both wavelengths use the same unit.

A 500 nm line is measured at 505 nm. What is z?
Explore the primary source: NASA · Spectroscopy 101 ↗
03

LEARNING OBJECTIVE

Read a transit light curve

Separate a measured dip from a simple radius model.

Not yet practised

A transit may cause a dip as an object passes between the observer and a star. Other effects can also produce a single decrease.

For a uniformly bright stellar disc and a small dark planet, depth is approximately the square of the radius ratio. Limb darkening and noise affect real analysis.

WORKED EXAMPLE / MODELδ = 1 − Fin/Fout; Rp/Rs ≈ √δ

If normalized flux falls from 1.00 to 0.99, the model depth is 0.01. In the simple model, Rp/Rs ≈ √0.01 = 0.10.

Which radius ratio corresponds to a 1% depth in this simple model?
Explore the primary source: NASA · What is a transit? ↗
04

LEARNING OBJECTIVE

Preserve observation provenance

Record a dataset’s time, instrument and processing.

Not yet practised

A graph becomes interpretable with its source and processing steps. Observation and download dates may differ.

Recording product identifier, time system, unit, quality flag and processing version lets another person inspect the same selection.

WORKED EXAMPLE / MODELGözlem ≠ erişim ≠ işleme / Observation ≠ retrieval ≠ processing

Keep observation time, retrieval time and product identifier in separate fields instead of reporting only “downloaded on 24 October”.

Which information best helps locate the same observation?
Explore the primary source: MAST · Data archive ↗
Check your learning 3 questions
What happens to travel time when distance doubles at constant speed?
A 500 nm line is measured at 505 nm. What is z?
Which information best helps locate the same observation?

The same short self-check before and after practice helps you review what changed. It does not measure expertise independently.

Turn practice into a research report.

Write a question, record your inputs, compare results and discuss uncertainty.

Start this project

YOUR WORK / YOUR COPY

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Download offline study pack ↓

Study pack: release 4.0.0 · content dated 24 October 2026 · self-contained lessons, exercises, project templates and source-labelled sample data. Unzip and open index.html. No external API is required.

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