1. The Radio Sky Chris Salter NAIC/Arecibo Observatory

2. “Suppose that our eyes responded to radio waves, rather than light, how different would the Night Sky appear?” I find a very steady hiss type static of unknown origin Whose direction of arrival goes almost around the Compass in 24 hours Karl Jansky -- 1932

3. Our Radio Eyes Angular Resolution = /Diameter GBT 100-m telescope (WV, USA)‏ Effelsberg 100-m telescope (FRG)‏ Arecibo 305-m telescope (Puerto Rico)‏ IRAM 30-m mm-wave telescope (Spain)‏ Ooty Radio Telescope 530  30 m (India)‏

4. Emission Mechanisms Thermal emission is unpolarized. a) Solid body; e.g. planet, you, me. b) Free-free emission from a hot ionized gas. c) Dust particles. d) Thermal spectral line emission. Recombination Lines near 5 GHz Non-thermal emission is generally polarized. a) Synchrotron Emission due to helical trajectories of ultra-relativistic electrons crossing interstellar magnetic fields. b) Maser-like line emission, e.g. OH, H 2 O, CH 3 OH and SiO. Water maser line

5. The Whole Radio Sky (408 MHz – λ73 cm) ‏ Galactic Center North Polar Spur SMC & LMC Cas-A Cen-A Cyg-X; (the local Main St.)‏ Synchrotron Emission

6. Cosmic Micwave Background (WMAP; 90 GHz – λ3 mm) Cosmic Micwave Background (WMAP; 90 GHz – λ3 mm)‏

7. The Celestial Neutral Hydrogen (HI) Emission HI Continuum

8. The Radio Solar System Saturn -- VLA Moon -- (IRAM 30-m telescope; 230 GHz)‏ Jupiter -- VLA As seen by a “Passive” Radio Astronomer

9. Jupiter 2.3 GHz ( 13 cm)‏1.4 GHz ( 22 cm)‏ (Continuum spectrum, including decametric bursts)‏

10. True Radio Stars X-ray Binary SS433 Radio Image(Artist’s Impression)‏ Radio Light Curve X-Ray Image

11. Supernova Remnants Cas A – about 1680 ADCrab Nebula – 1054 AD (AD 1572)‏ W 50 Supernova 1987A (Optical)‏

12. Pulsars PSR 0329+54 Discovery of Pulsars (1967)‏ The Double Pulsars (Artist’s Impression)‏ About 1600 pulsars are currently known. Pulsar periodicities are between 0.0014 and 8.5 sec. All pulsars are slowing down.

13. HII Regions – The Youngest Stars Orion Nebula: Optical Radio Continuum Mm-wave Line Spectrum Free-free emission When a molecule changes its rotation, vibration or bending state to one of lower energy, it radiates a photon. If the change of energy is very small, the photon is a radio photon. rotation

14. Spiral Galaxies M31 -- Optical M31 -- Radio Continuum M31 -- HI I

15. Elliptical Galaxies Centaurus A (Optical)‏ Cygnus A -- (Radio; FR II)‏ M 87 -- Optical Centaurus A (High-resolution Radio; FR I)‏

16. Radio Source Image Gallery 3C31 (Source in galaxy group)‏ 3C296 (Double-jet radio galaxy)‏ NGC 1265 (Narrow-angled tail cluster galaxy)‏ 3C175 (Double-lobed quasar)‏ Fornax A (Nearby radio galaxy)‏ J0204+1514 (Compact Quasar)‏

17. The Canonical Model of AGNs OpticalRadio MODEL

18. Superluminal Motion & Gravitational Lensing 4C 05.51 CLASS B1359+154