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Introduction to Radio Telescopes

Introduction to Radio Telescopes. Frank Ghigo, NRAO-Green Bank. The Fourth NAIC-NRAO School on Single-Dish Radio Astronomy July 2007. Terms and Concepts. Jansky Bandwidth Resolution Antenna power pattern Half-power beamwidth Side lobes Beam solid angle Main beam efficiency

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Introduction to Radio Telescopes

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  1. Introduction to Radio Telescopes Frank Ghigo, NRAO-Green Bank The Fourth NAIC-NRAO School on Single-Dish Radio Astronomy July 2007 Terms and Concepts Jansky Bandwidth Resolution Antenna power pattern Half-power beamwidth Side lobes Beam solid angle Main beam efficiency Effective aperture Parabolic reflector Blocked/unblocked Subreflector Frontend/backend Feed horn Local oscillator Mixer Noise Cal Flux density Aperture efficiency Antenna Temperature Aperture illumination function Spillover Gain System temperature Receiver temperature convolution

  2. Pioneers of radio astronomy Grote Reber 1938 Karl Jansky 1932

  3. Unblocked Aperture • 100 x 110 m section of a parent parabola 208 m in diameter • Cantilevered feed arm is at focus of the parent parabola

  4. Subreflector and receiver room

  5. On the receiver turret

  6. Basic Radio Telescope Verschuur, 1985. Slide set produced by the Astronomical Society of the Pacific, slide #1.

  7. Signal paths

  8. Intrinsic Power P (Watts)Distance R (meters)Aperture A (sq.m.) Flux = Power/Area Flux Density (S) = Power/Area/bandwidth Bandwidth () A “Jansky” is a unit of flux density

  9. Antenna Beam Pattern (power pattern) Beam solid angle (steradians) Main Beam Solid angle Pn = normalized power pattern Kraus, 1966. Fig.6-1, p. 153.

  10. Some definitions and relations Main beam efficiency, M Antenna theorem Aperture efficiency, ap Effective aperture, Ae Geometric aperture, Ag

  11. Detected power (W, watts) from a resistor R at temperature T (kelvin) over bandwidth (Hz) Power WA detected in a radio telescope Due to a source of flux density S power as equivalent temperature. Antenna Temperature TA Effective Aperture Ae

  12. another Basic Radio Telescope Kraus, 1966. Fig.1-6, p. 14.

  13. Aperture Illumination FunctionBeam Pattern A gaussian aperture illumination gives a gaussian beam: Kraus, 1966. Fig.6-9, p. 168.

  14. Gain(K/Jy) for the GBT Including atmospheric absorption: Effect of surface efficiency

  15. System Temperature = total noise power detected, a result of many contributions Thermal noise T = minimum detectable signal For GBT spectroscopy

  16. Convolution relationfor observed brightness distribution Thompson, Moran, Swenson, 2001. Fig 2.5, p. 58.

  17. Smoothing by the beam Kraus, 1966. Fig. 3-6. p. 70; Fig. 3-5, p. 69.

  18. Physical temperature vs antenna temperature For an extended object with source solid angle s, And physical temperature Ts, then for for In general :

  19. Calibration: Scan of Cass A with the 40-Foot. peak baseline Tant = Tcal * (peak-baseline)/(cal – baseline) (Tcal is known)

  20. More Calibration : GBT Convert counts to T

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