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IA 2019 5a
- 3. MULTI-WAVELENGTH ASTRONOMY Radio Continuum (408 MHz) Atomic Hydrogen (21cm) Radio Continuum (2.4 GHz) Molecular Hydrogen Far Infrared Mid Infrared Near Infrared Optical X-Ray Gamma Ray
- 7. SIZE OF YOUR TELESCOPE • Remember the PSF – That tells you how good your resolution is • To get the same resolution at different wavelengths takes different size collectors Limited by ability to focus Limited by size Angle to first minimum for a circular aperture diameter d: sin 𝜃 = 1.22 𝑑
- 9. RADIO AND MICROWAVE Signals combined UsingCorrelators Antenna is: Reflector, Driven Element, and Directors
- 10. INTERFEROMETERS LOFAR (Down the road) VLA (New Mexico) SKA (South Africa & Western Australia) ALMA (Chile)
- 16. X-RAY FROM SPACE ONLY XMM (ESA) Chandra (NASA)
- 17. GAMMA Compton Effect Spark Detector Scintillation Detectors
- 18. GAMMA RAYS • From Space – Satellites like GRO • From Earth – Look for Compton Effect in the Atmosphere (e.g. VERITAS array) • [Once thought there would be no gamma ray astronomy, and satellites were launched just to spy on the USSR – then found Gamma ray bursts from space!]
- 19. WAVE – PARTICLE DUALITY Low energy astronomers talk in Waves and use Wavelengths (and frequencies too at lowest energies) High energy astronomers talk in Particles and use Energies (usually in MeV) 𝐸 = ℎ𝑓 = ℎ = ℎ𝑐 𝑐 = 𝑓 = 1eV = 1.6022 × 10 − 19 J ℎ = 6.6261 × 10 − 34 J s 𝑐 = 299,792,458 ms−1
- 20. NON-LIGHT: NEUTRINOS • Searching for the signals of interacting neutrinos • Solar Neutrino Problem – Not enough are observed!
- 21. NON-LIGHT: COSMIC RAYS • Produce relativistic Muons in the upper atmosphere which you can detect the particle cascade on Earth
- 23. QUESTIONS? • More Depth? See book chapter 3
- 24. CONCEPT BANK Multiwavelength Astronomy Resolution Different Emission Radio Astronomy Interferometer Arrays Infrared Astronomy Visual Astronomy UV Astronomy X-Ray Astronomy Gamma Ray Astronomy Compton Scattering Neutrino Astronomy Cosmic Ray Astronomy Gravitational Wave Astronomy