Lecture 1 By Tom Wilson Lecture 1 page

Lecture 1 By Tom Wilson

Lecture 1 page 1 history Maxwell: Equations Hertz: Reality Marconi: Practical wireless Fessenden, Armstrong: Voices on wireless, Heterodyne De Forrest: Amplifiers Jansky: Cosmic radio sources Radio Astronomy: Pawsey, Bolton, Oort, Ryle… 1963 -8: Quasars, Molecular Clouds, Pulsars…

The 20. 5 MHz Sky (Jansky)

Lecture 1 page 2 Galactic Continuum Sources Sn in Jy is 10 -26 W m-2 Hz-1 (intensity integrated over the source)

Lecture 1, page 3 M 82 in the radio, mm, sub-mm and FIR ranges Atomic Lines, Molecular Lines Free-Free (Bremstrahlung) & Synchrotron Continuum Emission Dust continuum

Lecture 1, page 4 Opacity of the Atmosphere ionosphere mm and sub-mm range

=2 n 2/c 2. k. T Lecture 1 page 5 Peak of black body: T=3 K, l=1 mm T=10 K, l=0. 3 mm

Lecture 1, page 6 Rayleigh-Jeans: In Jy, or 10 -26 Wm-2 Hz-1 Cassiopeia A At 100 MHz, Sn= 3 104 Jy, qs=4’ (source size), l = 3 m = 300 cm

Lecture 1, page 7 Three Types of Radio Sources Non-Thermal: Sources such as Cassiopeia A. At 3 mm, find that Cas A has a peak temperature of about 0. 8 K. Is this consistent with the flux density shown in the first plot? Thermal: HII Regions such as Orion A q= 5’ (FWHP) at 100 MHz, l=300 cm, the flux density is 10 Jy. Find that T=104 K At 1. 3 cm, find that T=24 K True Black Bodies: Regions such as the Moon Find that T=220 K (approximately). Note that Sn increases with frequency squared.

Lecture 1, page 8 Development Radiative Transfer Receivers Receiver Calibration Atmosphere

Lecture 1 page 9 One Dimensional Radiative Transfer Suppose absorption, Assume and , and emission, in 1 dimension : are constants w. r. t. s. Then Integrating at , Kirchhoff ’s law: . So when is the Planck Function

Lecture 1 page 10 Radio: , for T=10 K, Then: Radio Range (Definition) (Rayleigh-Jeans) Emission from Atmosphere Absorption of Source (all for a frequency Receiver sees noise from Moon, plus noise fro atmosphere minus loss of source noise in atmosphere. Need calibration to relate receiver output to temperature. For spectral lines, Source (e. g. MOON) , so atmosphere If T=T 0, see no emission or absorption (could be species with T=T 0=2. 73 K) )

Lecture 1 page 11 Types of Receivers Fractional Resolution

Lecture 1 page 12 Analog Coherent Receiver Block Diagram Time Frequency=n, f Total Amplification=1016 Suppose you measure Cas A with a dish of collecting area 50 m 2 at 100 MHz with a bandwidth of 10 MHz: what is the input power?

Lecture 1, page 13 Hot-cold load measurements (to determine receiver noise contribution) Absorber at a given temperature Input to receiver

Lecture 1, page 14 Hot and Cold Load Calibration Ratio of Ph to Pl is defined as ‘y’

Lecture 1 page 15 Suppose you have y=2, 2. 5, or 3. What is the receiver noise?

Lecture 1 page 16 Basic Elements of Coherent Receivers • • Mixers (HEB, SIS, Schottky) Amplifiers (Mostly for ) Attenuators (Adjust power levels) Circulators, Filters Noise temperature of an amplifier chain: G 1: Gain of the stage 1, in cm range, G 1 is larger than 103 typically, so that TS 1 dominates Sometimes (as in mm or sub mm), stage 1 has loss, then For example, 3 d. B loss in common 100. 3 =2, so (divided by Gain of element 1) =TS 1+10 K

Lecture 1, page 17 Current Receiver Noise Temperatures Tmin=hn/k for coherent receivers

Lecture 1, page 18 Noise

Lecture 1 page 19 (See problem 4 -14 in ‘Tools Problems’) (See problem 4 -14 in ‘Tools Problems’ for a derivation) RECEIVERS Fundamental Relation: Time 1 sec 1 hour 16 hours 64 hours • For broadband measurements, try to keep TSYS small, but also good to have Dn large (bolometers) • For very narrow spectral lines, coherent receivers have Dn as small as you want. For example one can have Dn = 10 -9 n 0 • For a 1/100 signal-to-noise ratio in 1 sec, have about 1 -to-1 in 1 hour, 2. 5 -to-1 in 16 hours

Lecture 1, page 20 Systematic Effects increase Noise RMS (See 4 -27 in ‘Tools Problems’)

Lecture 1, page 21 Dicke Switching to Cancel Systematic Effects But switching against a reference will increase the random noise

Lecture 1, page 22 Effect of Mixing in Frequency Space Difference Frequency L. O. frequency Signal Frequency

Lecture 1, page 23 Double Sideband Mixers 111 GHz

Lecture 1, page 24 (See 4 -24 in ‘Tools Problems’)

Lecture 1, page 25 Heterodyne receivers at the HHT

Lecture 1 page 26 BACKENDS Want to have S(n). Output of front end is V(t). Problem is how to get S(n) from V(t) in the best way. The most Common solutions in Radio Astronomy are: • Filter bank • Autocorrelator • “Cobra” • AOS • Chirp transform spectrometer

Lecture 1, page 27 Wiener-Kinchin

Lecture 1, page 30 F. T. n tt ( )2 F. T. (Must be careful with limits in integral of periodic functions)

Lecture 1, page 31 Graphical Correlation (Problem 4 -11 in ‘Tools Problems’. Correlations are useful in many different areas)

Time behavior of input Lecture 1, page 32 Frequency behavior Sampling function in time Sampling function in frequency undersampled Sufficiently sampled (see 4 -12 in ‘Tools Problems’)

Lecture 1, page 29 Autocorrelator Current Sample (A) Delayed Sample (B) The correlation of A with B; examples are the correlation of two sine waves or two squares

Lecture 1, page 33 Filter Bank Spectrometers

Lecture 1 page 34 BOLOMETERS These devices are temperature sensors, so • Do not preserve phase • Thus no quantum limit to system noise • Wide bandwidths are easier to obtain • No L. O. needed • Thus multi-pixel cameras are ‘easier’ to build • On earth, Bolometers are background limited; outer space is better & outer space with cooled telescopes better still! • Today get NEP ≈ 10 -16 watts Hz -1/2 • (Problem: Relate to flux density sensitivity of the 30 -m) For those who prefer ΔTRMS, one can use the following relation:

Lecture 1, page 35 0. 8 mm Bolometer Passband

Lecture 1, page 36 19 channel Bolometer at the HHT