# Radio Astronomy Expert

> Expert-level radio astronomy covering radio telescopes, interferometry, VLBI, pulsars, spectral line observations, fast radio bursts, and aperture synthesis imaging.

- Skill: `luokai0/radio-astronomy-expert` (Agent Skill, multi-file: 2 files)
- Install (CLI): `npx skillmds@latest add luokai0/radio-astronomy-expert`
- Raw SKILL.md: https://api.skillmd.com/api/skills/luokai0/radio-astronomy-expert/raw
- Safety review: pending (external: skill-scanner PASS, skillspector PASS)
- Works with: Claude Code, Claude.ai, OpenAI Codex
- Category: AI & ML
- Author: luokai0 (https://skillmd.com/u/luokai0)
- Updated: 2026-09-08
- Page: https://skillmd.com/skills/luokai0/radio-astronomy-expert

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# Radio Astronomy Expert

## Before Starting
1. Which frequency band? cm, mm, or sub-mm?
2. Continuum or spectral line?
3. Single dish or interferometry?

## Core Expertise Areas

### Radio Telescopes
Single dish: large collecting area, resolution limited by diffraction.
Parabolic reflector: focuses radio waves to receiver at prime or secondary focus.
FAST: 500m dish in China, most sensitive single dish in the world.
Receiver systems: LNA amplifiers, mixers, spectrometers, cryogenic cooling.
System temperature: receiver noise plus sky background limits sensitivity.

### Radio Interferometry
Baseline: separation between two antennas, determines angular resolution.
Visibility: complex number measured by each baseline, Fourier transform of sky.
UV plane: spatial frequency coverage determines image quality.
Aperture synthesis: Earth rotation fills UV plane over time.
CLEAN algorithm: iterative deconvolution of dirty beam from dirty image.

### VLBI
Very long baseline interferometry: intercontinental baselines, microarcsecond resolution.
Atomic clocks: GPS and hydrogen masers synchronize stations.
EHT: global VLBI at 1.3mm imaged black hole shadows of M87 and Sgr A star.
Space VLBI: RadioAstron satellite extended baselines beyond Earth diameter.

### Radio Sources
Pulsars: rotating neutron stars, stable rotation used as precise clocks.
Pulsar timing arrays: gravitational wave background detection method.
FRBs: fast radio bursts, millisecond transients, largely extragalactic origin.
HI 21cm line: neutral hydrogen spin-flip transition traces galaxy structure.
Molecular lines: CO, OH, NH3 probe cold gas in star-forming regions.

## Best Practices
- Always check for radio frequency interference before analysis
- Calibrate amplitude and phase with known calibrator sources
- Apply proper motion and parallax corrections for astrometry
- Assess image dynamic range and sensitivity limits carefully

## Common Pitfalls
| Pitfall | Fix |
|---|---|
| RFI contamination | Flag affected data before imaging |
| Insufficient UV coverage | Observe at multiple hour angles or add more antennas |
| CLEAN divergence | Use appropriate CLEAN depth and mask region |
| Confusing flux density and luminosity | Always specify distance when quoting luminosity |

## Related Skills
- astrophysics-expert
- physics/electromagnetism-expert
- computer-science/signal-processing