radio astronomy an introduction · radio astronomy an introduction references thompson, moran &...
TRANSCRIPT
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Felix James “Jay” LockmanNRAO
Green Bank, WV
Radio Astronomy An Introduction
References
Thompson, Moran & Swenson Kraus (1966)Christiansen & Hogbom (1969)Condon & Ransom (nrao.edu)Single Dish School Proceedings (2002) ADS
GOLDSMITH CAMPBELL
LISZT ★★★★
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Astronomy at Radio Wavelengths
More than 130 interstellar molecules
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Astronomy at Radio Wavelengths
More than 130 interstellar molecules
HCN from Comet Hale-Bopp -- Jewit & Saney
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D. Balser GBT image
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Breton et al (2008)
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GASS HI Survey (McClure-Griffiths et al 2009)
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GASS HI Survey (McClure-Griffiths et al 2009)GBT Image of Hydrogen
in Smith’s Cloud
(Lockman et al 2008)
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Astronomy at Radio Wavelengths -- Why is it Different?
AtmosphereLow Energy Photons
DiffractionCoherent Signal Processing
Noise
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Astronomy at Radio Wavelengths -- Why is it Different?
AtmosphereLow Energy Photons
DiffractionCoherent Signal Processing
Noise
What does every radio telescope shown so far have in common?
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The Radio Window0.01 GHz - 1000 GHz
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The Radio Window0.01 GHz - 1000 GHz
Transparency of the Atmosphere depends on altitude and H2O
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Radiative Transfer -- Specific Intensity
Linear Absorption Coefficient + emissivity
Optical Depth
Absorption + emission
Relations through black-body radiation
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EMISSION: Blackbody Radiation
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I!(thermal) =2h!3
c2
1exp(h!/kT )! 1
I!(th) =2kT
!2 !(GHz) << 22 T(K)
Blackbody radiation
!max (GHz) = 59 T (K)
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I! = I0e!"!
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!
Radio source
!A
An “aperture” in the abstract
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!
Radio source
P (0, 0) = 1
!A
Wm =Ae
2
!
4!I"(!,") P"(!,") d! Watts Hz!1
Power Pattern
Power Received
An “aperture” in the abstract
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I!(th) =2kT
!2
Wm =kAe
!2
!
4!Tb"(",#) P"(",#) d! Watts Hz!1
When " << 22 T
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From Condon & Ransom http://www.cv.nrao.edu/course/astr534
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I!(th) =2kT
!2
Wm =kAe
!2
!
4!Tb"(",#) P"(",#) d! Watts Hz!1
Power from a resistor
W = kT (watts Hz!1)
Ta =Ae
!2
!
4!Tb"(", #) P"(",#) d! (K Hz!1)Antenna
Temperature
When " << 22 T
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Ta =Ae
!2
!
4!Tb"(", #) P"(",#) d! (K Hz!1)
Enclose the antenna in a blackbody of temperature Tb
Ta =TbAe
!2
!
4!P"(",#) d!
!a =!
4!P"(!,") d!defining
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Ta =Ae
!2
!
4!Tb"(", #) P"(",#) d! (K Hz!1)
But we are looking through the atmosphere!
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Specific Intensity (Brightness)
Flux Density
A flux density per unit area is actually a brightness!
I!(!,") (Watts m!2 Hz!1 str!1)
S! =!
!s
I!(!, ") d! (Watts m!2 Hz!1)
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Specific Intensity (Brightness)
Flux Density
A flux density per unit area is actually a brightness!
I!(!,") (Watts m!2 Hz!1 str!1)
S! =!
!s
I!(!, ") d! (Watts m!2 Hz!1)
What determines P?
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Aperture Plane
“Boxcar” Function
“Sinc” Function
FT
Uniform Illumination
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For Uniform Illumination
Airy rings
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Main Beam and Sidelobes
Main Beam Efficiency
(from Kraus 1966)
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• In the far field, the electric-field pattern, f, of an aperture antenna is the Fourier transform of the electric field illuminating the aperture. And the power pattern, P, is the square of the modulus of f.
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Wm =Ae
2
!
4!I"(!,") P"(!,") d! Watts Hz!1
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Wm =Ae
2
!
4!I"(!,") P"(!,") d! Watts Hz!1
What is Ae?
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Geometric Area
Effective Area
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Geometric Area
Effective Area
Reciprocity: f(t) = f(-t)
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Reciprocity in action
1: Forward Spillover2: Rear Spillover3: Surface defect
4: Blockage
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Reciprocity in action
1: Forward Spillover2: Rear Spillover3: Surface defect
4: Blockage
Diffractive Optics: 4m at 5000Å = 8x106 #100m at 21cm = 475 #
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Spillover wastes power and can increase the noise, so taper the illumination
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from S. Srikanth (1992)
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November 15, 1988
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November 16, 1988
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Effects of surface errors -- phase errors
Scatter power out of main beamCreate a sidelobe
Reduce Ae
Ruze equation for rms error $
Ae reduced by factor of 2 for $=#/16
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Effects of surface errors -- phase errors
Scatter power out of main beamCreate a sidelobe
Reduce Ae
Ruze equation for rms error $
Ae reduced by factor of 2 for $=#/16
Where does it go? Atm phase errors
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Sources of Noise
Radio Astronomical Signals must be distinguished from a background of naturally occurring “noise”
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Measurement error arising from noise
Example: detect the HI line from a cloud with NH=2x1018 and FWHM=20 km/s.
Expected TL = 0.05 K
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Blockage
(from Goldsmith 2002)
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Effects of blockage on dynamic range
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Effects of blockage on dynamic range
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Effects of blockage on dynamic range
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The marvelous radio receivers/detectors
From Condon & Ransom http://www.cv.nrao.edu/course/astr534
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Talkin’ about telescopes
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A radio telescope must:
Talkin’ about telescopes
SurviveFocusPointTrack
So it has a
MountSurfaceOptics
Receiver
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Parkes 210-ft
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