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radio-astronomy-expert

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

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luokai0/ai-agent-skills-by-luo-kai

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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

PitfallFix
RFI contaminationFlag affected data before imaging
Insufficient UV coverageObserve at multiple hour angles or add more antennas
CLEAN divergenceUse appropriate CLEAN depth and mask region
Confusing flux density and luminosityAlways specify distance when quoting luminosity

Related Skills

  • astrophysics-expert
  • physics/electromagnetism-expert
  • computer-science/signal-processing

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