Astronomical Observing Techniques Lecture 7: Your Favorite Sta<on at 1420 MHz
|
|
- Julie Carroll
- 5 years ago
- Views:
Transcription
1 Astronomical Observing Techniques Lecture 7: Your Favorite Sta<on at 1420 MHz Christoph U. Keller
2 Overview 1. Introduc9on 2. Radio Emission 3. Observing 4. Antenna Technology 5. Receiver Technology 6. Back Ends 7. Calibra9ons
3 (c) National Radio Astronomy Observatory / Associated Universities, Inc. / National Science Foundation
4 The First Radio Astronomers Karl Guthe Jansky ( ) hkp://en.wikipedia.org/wiki/radio_telescope hkp://en.wikipedia.org/wiki/radio_astronomy Grote Reber ( ) Karl Jansky built (at Bell Telephone Laboratories) antenna to receive radio waves at 20.5 MHz (λ~14.6m) à turntable of 30m 6m à first detec9on of astronomical radio waves (à 1 Jy = W m 2 Hz 1 ) Grote Reber extended Jansky's work, conducted first radio sky survey. For nearly a decade he was the world's only radio astronomer.
5 Radio Astronomy Discoveries radio (synchrotron) emission of the Milky Way (1933) first discrete cosmic radio sources: supernova remnants and radio galaxies (1948) 21-cm line of atomic hydrogen (1951) Quasi Stellar Objects (1963) Cosmic Microwave Background (1965) Interstellar molecules ó star forma9on (1968) Pulsars (1968)
6 Radio Observa<ons through the Atmosphere Radio window from ~10 MHz (30m) to 1 THz (0.3mm) Low-frequency limit given by (reflec9ng) ionosphere High frequency limit given by molecular transi9ons of atmospheric H 2 O and N 2.
7 Radio: PhotonsàElectric Fields Directly measure electric fields of electro-magne9c waves Electric fields excite currents in antennae Currents can be amplified and split electrically.
8 Radio Emission Mechanisms Most important astronomical radio emission mechanisms 1. Synchrotron emission 2. Free-free emission (thermal Bremsstrahlung) 3. Thermal (blackbody) emission (also from dust grains) 4. Spectral lines Comparison of three emission components (for the starburst galaxy M82) Synchrotron radia9on dominates at low frequencies. Thermal dust emission dominates at high frequencies. Free-free emission
9 Synchrotron Emission Caused by highly rela9vis9c electrons, spiraling around galac9c magne9c field lines Polarized Con9nuous spectrum
10 Free-Free Emission Free-free emission produced by free electrons scakering off ions (e.g. in HII regions) without being captured: con9nuous spectrum Sun5GHz.jpg
11 Thermal Emission Rayleigh-Jeans tail of thermal emission from e.g. dust grains produces radio emission.
12 The HI 21cm ( MHz) Line Hendrik van de Hulst predicted in 1944 that neutral hydrogen could produce radia9on at ν = MHz due to two closely spaced energy levels in the ground state of the hydrogen atom. Hendrik van der Hulst ( ) First observed in 1951 by Ewen and Purcell at Harvard University, then by Dutch astronomers Muller and Oort. A$er 1952 the first maps of the neutral hydrogen in the Galaxy were made and revealed, for the the spiral structure of the Milky Way.
13 Map of the Milky Way Determine loca9on of hydrogen emission from rota9onal Doppler shis Contour plot of hydrogen concentra9on as seen from the top High concentra9ons in red
14 Astronomical Relevance of HI 21cm Line Main applica9ons: 1. Distribu9on of HI in galaxies 2. Big Bang cosmology: redshised HI line can be observed from 200 MHz to about 9 MHz: mapping redshised 21 cm provides the maker power spectrum aser recombina9on provides info on how the Universe was reionized (HI which has been ionized by stars or quasars will appear as holes) But the signals are intrinsically weak and plagued by radio interferences. Thilker, Braun & Walterbos (1998)
15 Famous Radio Telescopes (Single Dish) Parkes 64m Jodrell Bank 76m Arecibo, Puerto Rico, 305m Dwingeloo, 25m Effelsberg, 100m Greenbank, USA after structural collapse
16 ALMA: Atacama Large Millimeter Array
17 Antennae: The Hertz Dipole Antennae required to focus power into feed Feed is device that efficiently transfers power in the electromagne9c wave to the receiver Proper9es of antennae (beam pakerns, efficiencies, ) are the same for transmission and recep9on. Hertz dipole: total power radiated from Hertz dipole of length Δl carrying an oscilla9ng current I at a wavelength λ is: P = 2c IΔl 3 2λ 2
18 Radia<on from Hertz Dipole Radia9on is linearly polarized Electric field lines along direc9on of dipole Radia9on pakern has donut shape, defined by zone where phases match sufficiently well to combine construc9vely Along the direc9on of the dipole, the field is zero Best efficiency: size of dipole = 1/2 λ
19 Radio Beams, PSFs and Lobes Similar to op9cal telescopes, angular resolu9on given by D θ = k λ Radio beams show just like the Airy pakerns of op9cal PSFs pakerns of lobes at various angles, direc9ons where the radiated signal strength reaches a maximum, separated by nulls, angles at which the radiated signal strength falls to zero. where k ~1.
20 Main Beam and Sidelobes Highest field strength in main lobe, other lobes are called sidelobes (unwanted radia9on in undesired direc9ons) Side lobes may pick up interfering signals, and increase the noise level in the receiver. The side lobe in the opposite direc9on (180 ) from the main lobe is called the back lobe.
21 Ω A = Main Beam Efficiency The beam solid angle Ω A in steradians of an antenna is given by: 4π 2π π ( ϑ, ϕ) dω P ( ϑ, ϕ) sinϑdϑdϕ Pn = 0 0 With the normalized power pakern Hence, P n = 1 for Ω A for an ideal antenna. Main beam solid angle Ω MB is: Ω MB = P n main lobe ( ϑ ϕ), dω And the main beam efficiency η B is: n 1 P ( ϑ, ϕ) P( ϑ, ϕ) P n = (This is the frac9on of the power concentrated in the main beam.) η B = Ω Ω MB A max
22 Coherent (Heterodyne) Receivers Problems with detec9ng and amplifying signals (electromagne9c waves): 1. The signals are usually very weak 2. The frequencies are too high for standard electronics λ = 1 µm ó ν = 300 THz ó Δt = s λ = 100 µm ó ν = 3 THz ó Δt = s λ = 1 cm ó ν = 30 GHz ó Δt = 33 ps Solu9on: Mixing (mul9plica9on) of the source signal with a reference wave (provided by a local oscillator):
23 encodes signal over a wide wavelength range à ideal for spectroscopy typically, power(ω LO )» power(ω S ) à amplifica9on by oscillator signal down-conversion to frequencies where low-noise electronics exist Principle of Frequency Mixing 1. Signal S 1 is mixed with local oscilla9ng field S 2 2. The mix produces a down-converted difference, intermediate, or beat frequency at ω S1 ω S2 (and ω S1 + ω S2 ).
24 Mixer Technology Example of a mixer: Source signal à Local oscillator signal à Mixing element Problem: good & fast tradi9onal photo-conductors do not exist for ν < 7.5 THz è SchoKky diodes SIS junc9ons Hot electron bolometers
25 Mixer Output linear device (a) yields no output power at any frequency. non-linear device (b,c) can convert power from the original frequencies to the beat frequency even if the mixer has an odd func9on of voltage around the origin (b) the conversion efficiency is zero. but if biased above zero (A) the average change in current is larger for posi9ve than for nega9ve voltage peaks. If I ~ V 2 (as in a diode) then output ~ (field strength) 2 ~ power, which is exactly what we want to measure!
26 Basic Heterodyne System local oscillator signal wave diplexer mixer Back End specifies the devices following the IF amplifiers. Many different back ends have been designed for specialized purposes such as con9nuum, spectral or polariza9on measurements.
27 Polarimeters Antennas with fixed-dipole feeders or horn feeders receive only the frac9on that is polarized in the plane of the orienta9on of the feeder. Rota9on can be measured by rota9ng the feeder about the antenna s beam axis or by two orthogonally polarized antenna feeders. Heterodyne dual polariza9on receiver = two iden9cal systems, connected to the same local oscillator, and sensi9ve to only one of the two orthogonal polariza9ons. Can provide values of all polariza9on parameters simultaneously.
28 Mul<channel Spectrometer The IF input signal is divided among the bandpass filters ( filter bank ) and the output of each is processed by a detector/integrator stage. The outputs of these stages are switched sequen9ally to the computer where the spectrum can be displayed. Such mul9-channel spectrometers can have up to 512 parallel channels.
29 Acousto-Op<cal Spectrometer (AOS) AOS converts frequencies to ultrasonic waves that disperse a monochroma9c light beam onto an array of visible light detectors. from Wikipedia The acous9c wave can be created in a crystal ( Bragg-cell ) and modulates the refrac9ve index à induces a phase gra9ng. The angular dispersion is a measure of the IF-spectrum.
30 Autocorrela<on Spectrometer Reminder: f ~ f ~ f ~ f ( x) ( s) = FT{ f ( x) } ( s) 2 2 ( s) = f ( x) f ( x) Function Fourier transform of f(x) Spectral density or power spectrum of f(x) Wiener - Khinchine (autocorrelation) theorem k + ( x) = f ( u) f ( u + x) Autocorrelation 1. Given: time dependent IF signal f(x) 2. Want: Power spectrum I(v) = f(s) 2 3. f(s) 2 could be computed via FT{f(x)} du 4. Better and faster: compute autocorrelation function of f(x) 5. à Digitize and delay x(t) n-times and compute autocorrelation
31 True Brightness Temperature Rayleigh-Jeans approxima9on: B RJ ( T ) ν = 2ν c, 2 brightness and effec9ve temperature are strictly propor9onal Can use brightness temperature to describe source intensity: T B 2 c = 2 2kν B RJ Note: usually only fulfilled if source fills beam (very extended sources) If the source is a real black body hv << kt, then T B is independent of v If the emission is non-bb (e.g., synchrotron, free-free, ) T B will depend on v but the brightness temperature is s9ll being used 2 = kt 2 λ 2k B RJ
32 Main Beam Brightness Temperature Rela9on between flux density S v and intensity I v : For discrete sources, the source extent is important and we need to combine the above equa9on with the previous one to: or simplified for a source with a Gaussian shape: Generally, for an antenna beam size θ beam the observed source size is: which relates the true brightness temperature with the main beam brightness temperature: S Sν = Jy ν = Ω B I ν 2kν c ( θ ϕ) 2 Sν = T 2 B T MB T B, cosθ dω ΔΩ θ arcsec θ = θ + θ 2 observed ( 2 2 ) 2 θ + θ = T θ source 2 source beam 2 2 beam λ mm B 2 source
33 Noise Temperature The power spectral density (PSD) entering the receiver is given by P = kt ν and is also called the antenna temperature. A receiver shall increase the input power level. The amplifica9on involves a noise factor F, defined via the S/N as: F = S S input output output For coherent receivers this noise factor is expressed as noise temperature: / / N N input ( F 1) K T R = 290
34 Receiver Calibra<on Noise temperature (receiver temperature) can be measured by comparing the signals of two ar9ficial sources with effec9ve temperatures T 1 and T 2. The total power is given by: where P α = Gkδν 1 ( T + T ) and P = ( T T ) = α α R 1 2 R + depends on gain G and bandwidth δν. 2 Now we can define a Y-factor as: Y = P P 2 1 With the Y-factor and solving for the receiver temperature T R we get: T R T2 YT = Y 1 1
35 Receiver Stability and Dicke Switching Source signals are weak à gain must be high à small gain instabili9es can dominate the thermal receiver noise. à Compare source signal with a stable reference signal by beam switching or Dicke switching (1946). It also compensates for atmospheric changes. Disadvantage: 50% of total 9me is spent to look at flux reference. Robert Henry Dicke ( )
36 Spectral Line Observa<ons Three common observing modes to detect weak spectral lines: 1) Posi9on Switching and Wobbler Switching: The signal on source is compared with a measurement of a nearby sky posi9on. Obviously, there should be no line radia9on coming from the sky posi9on. 2) On the Fly Mapping (extension of method (1)): spectral line data is taken at a rate of perhaps one spectrum or more per second while the telescope slews (scans) con9nuously across the source field. The background/con9nuum emission is reconstructed from the en9re data set. 3) Frequency Switching: For most sources, the spectral line radia9on is restricted to a narrow band. Changing the frequency of the receiver on a short 9me by ~10Δν produces a comparison signal with the line well shised. The line is measured all of the 9me, so this is an efficient observing mode.
Astronomische Waarneemtechnieken (Astronomical Observing Techniques)
Astronomische Waarneemtechnieken (Astronomical Observing Techniques) 7 th Lecture: 15 October 01 1. Introduction. Radio Emission 3. Observing 4. Antenna Technology 5. Receiver Technolgy 6. Back Ends 7.
More informationIntroduction to Radio Astronomy
Introduction to Radio Astronomy The Visible Sky, Sagittarius Region 2 The Radio Sky 3 4 Optical and Radio can be done from the ground! 5 Outline The Discovery of Radio Waves Maxwell, Hertz and Marconi
More informationA Crash Course in Radio Astronomy and Interferometry: 1. Basic Radio/mm Astronomy
A Crash Course in Radio Astronomy and Interferometry: 1. Basic Radio/mm Astronomy James Di Francesco National Research Council of Canada North American ALMA Regional Center Victoria (thanks to S. Dougherty,
More informationIntroduction to Radio Astronomy!
Introduction to Radio Astronomy! Sources of radio emission! Radio telescopes - collecting the radiation! Processing the radio signal! Radio telescope characteristics! Observing radio sources Sources of
More informationSubmillimeter (continued)
Submillimeter (continued) Dual Polarization, Sideband Separating Receiver Dual Mixer Unit The 12-m Receiver Here is where the receiver lives, at the telescope focus Receiver Performance T N (noise temperature)
More informationFundamentals of Radio Astronomy. Lyle Hoffman, Lafayette College ALFALFA Undergraduate Workshop Arecibo Observatory, 2008 Jan. 13
Fundamentals of Radio Astronomy Lyle Hoffman, Lafayette College ALFALFA Undergraduate Workshop Arecibo Observatory, 2008 Jan. 13 Outline Sources in brief Radiotelescope components Radiotelescope characteristics
More informationReceiver Performance and Comparison of Incoherent (bolometer) and Coherent (receiver) detection
At ev gap /h the photons have sufficient energy to break the Cooper pairs and the SIS performance degrades. Receiver Performance and Comparison of Incoherent (bolometer) and Coherent (receiver) detection
More informationGuide to observation planning with GREAT
Guide to observation planning with GREAT G. Sandell GREAT is a heterodyne receiver designed to observe spectral lines in the THz region with high spectral resolution and sensitivity. Heterodyne receivers
More informationIntroduction to Radio Astronomy. Richard Porcas Max-Planck-Institut fuer Radioastronomie, Bonn
Introduction to Radio Astronomy Richard Porcas Max-Planck-Institut fuer Radioastronomie, Bonn 1 Contents Radio Waves Radio Emission Processes Radio Noise Radio source names and catalogues Radio telescopes
More informationMore Radio Astronomy
More Radio Astronomy Radio Telescopes - Basic Design A radio telescope is composed of: - a radio reflector (the dish) - an antenna referred to as the feed on to which the radiation is focused - a radio
More informationCoherent Receivers Principles Downconversion
Coherent Receivers Principles Downconversion Heterodyne receivers mix signals of different frequency; if two such signals are added together, they beat against each other. The resulting signal contains
More informationSignal Flow & Radiometer Equation. Aletha de Witt AVN-Newton Fund/DARA 2018 Observational & Technical Training HartRAO
Signal Flow & Radiometer Equation Aletha de Witt AVN-Newton Fund/DARA 2018 Observational & Technical Training HartRAO Understanding Radio Waves The meaning of radio waves How radio waves are created -
More informationAST 443 / PHY 517. Photon Detectors
AST 443 / PHY 517 Photon Detectors Photons Light is electro- magne>c radia>on Crossed electric and magne>c vectors Self- propaga>ng Travels at speed of light c c=2.99792 x 10 8 m/s (vacuum) λν = c n=c/v
More informationMillimetre and Radio Astronomy Techniques for Star Forma:on Studies II
Millimetre and Radio Astronomy Techniques for Star Forma:on Studies II John Conway Onsala Space Observatory, Sweden &Nordic ALMA ARC node (john.conway@chalmers.se) Today prac:cal details... For details
More informationSingle Dish Observing Techniques and Calibration
Single Dish Observing Techniques and Calibration David Frayer (NRAO) {some slides taken from past presentations of Ron Maddalena and Karen O Neil} What does the telescope measure: Ta = antenna temperature
More informationAntennas. Greg Taylor. University of New Mexico Spring Astronomy 423 at UNM Radio Astronomy
Antennas Greg Taylor University of New Mexico Spring 2011 Astronomy 423 at UNM Radio Astronomy Radio Window 2 spans a wide range of λ and ν from λ ~ 0.33 mm to ~ 20 m! (ν = 1300 GHz to 15 MHz ) Outline
More informationAntennas. Greg Taylor. University of New Mexico Spring Astronomy 423 at UNM Radio Astronomy
Antennas Greg Taylor University of New Mexico Spring 2017 Astronomy 423 at UNM Radio Astronomy Outline 2 Fourier Transforms Interferometer block diagram Antenna fundamentals Types of antennas Antenna performance
More informationSources classification
Sources classification Radiometry relates to the measurement of the energy radiated by one or more sources in any region of the electromagnetic spectrum. As an antenna, a source, whose largest dimension
More informationRichard Dodson 1/28/2014 NARIT-KASI Winter School
Goals: Technical introduction very short So what to cover? Things which are essential: How radio power is received - I How an interferometer works -II Antenna Fundamentals Black Body Radiation Brightness
More informationWhat does reciprocity mean
Antennas Definition of antenna: A device for converting electromagnetic radiation in space into electrical currents in conductors or vice-versa. Radio telescopes are antennas Reciprocity says we can treat
More informationRadio Interferometry. Xuening Bai. AST 542 Observational Seminar May 4, 2011
Radio Interferometry Xuening Bai AST 542 Observational Seminar May 4, 2011 Outline Single-dish radio telescope Two-element interferometer Interferometer arrays and aperture synthesis Very-long base line
More informationTo print higher-resolution math symbols, click the Hi-Res Fonts for Printing button on the jsmath control panel.
To print higher-resolution math symbols, click the Hi-Res Fonts for Printing button on the jsmath control panel. Radiometers Natural radio emission from the cosmic microwave background, discrete astronomical
More informationIF/LO Systems for Single Dish Radio Astronomy Centimeter Wave Receivers
IF/LO Systems for Single Dish Radio Astronomy Centimeter Wave Receivers Lisa Wray NAIC, Arecibo Observatory Abstract. Radio astronomy receivers designed to detect electromagnetic waves from faint celestial
More informationTHEORY OF MEASUREMENTS
THEORY OF MEASUREMENTS Brian Mason Fifth NAIC-NRAO School on Single-Dish Radio Astronomy Arecibo, PR July 2009 OUTLINE Antenna-Sky Coupling Noise the Radiometer Equation Minimum Tsys Performance measures
More informationRadio Astronomy for Amateurs. Presented by Keith Payea AG6CI
Radio Astronomy for Amateurs Presented by Keith Payea AG6CI Outline Radio Astronomy Basics: What, How, Why How Amateurs can participate and contribute What is Radio Astronomy? The Study of the non-visible
More informationThe Cosmic Microwave Background Radiation B. Winstein, U of Chicago
The Cosmic Microwave Background Radiation B. Winstein, U of Chicago Lecture #1 Lecture #2 What is it? How its anisotropies are generated? What Physics does it reveal? How it is measured. Lecture #3 Main
More informationSpectral Line Imaging
ATNF Synthesis School 2003 Spectral Line Imaging Juergen Ott (ATNF) Juergen.Ott@csiro.au Topics Introduction to Spectral Lines Velocity Reference Frames Bandpass Calibration Continuum Subtraction Gibbs
More informationFundamental Sensi.vity Limits for Coherent and Direct Detec.on. Jonas Zmuidzinas Caltech
Fundamental Sensi.vity Limits for Coherent and Direct Detec.on Jonas Zmuidzinas Caltech Coherent vs. Direct Detec.on %! (31+'()*&',#!*,4*#,%(1$%(!!" #$!" #$#!%&'() %! %! #$#!%&'()!"#$#!%&'()!"#$#!%&'()!"#$%&'()*(#+!!+,-
More informationAntenna Engineering Lecture 3: Basic Antenna Parameters
Antenna Engineering Lecture 3: Basic Antenna Parameters ELC 405a Fall 2011 Department of Electronics and Communications Engineering Faculty of Engineering Cairo University 2 Outline 1 Radiation Pattern
More informationAntennas and Receivers in Radio Astronomy
Antennas and Receivers in Radio Astronomy Mark McKinnon Eleventh Synthesis Imaging Workshop Socorro, June 10-17, 2008 Outline 2 Context Types of antennas Antenna fundamentals Reflector antennas Mounts
More informationSub-Millimeter RF Receiver. Sub-Millimeter 19Receiver. balanced using Polarization Vectors. Intrel Service Company
Sub-Millimeter RF Receiver balanced using Polarization Vectors Intrel Service Company iscmail@intrel.com Sub-Millimeter Week of RF 19Receiver August 2012 Copyright Intrel Service Company 2012 Some Rights
More informationPhased Array Feeds & Primary Beams
Phased Array Feeds & Primary Beams Aidan Hotan ASKAP Deputy Project Scientist 3 rd October 2014 CSIRO ASTRONOMY AND SPACE SCIENCE Outline Review of parabolic (dish) antennas. Focal plane response to a
More informationObservational Astronomy
Observational Astronomy Instruments The telescope- instruments combination forms a tightly coupled system: Telescope = collecting photons and forming an image Instruments = registering and analyzing the
More informationA Quick Review. Spectral Line Calibration Techniques with Single Dish Telescopes. The Rayleigh-Jeans Approximation. Antenna Temperature
Spectral Line Calibration Techniques with Single Dish Telescopes A Quick Review K. O Neil NRAO - GB A Quick Review A Quick Review The Rayleigh-Jeans Approximation Antenna Temperature Planck Law for Blackbody
More information레이저의주파수안정화방법및그응용 박상언 ( 한국표준과학연구원, 길이시간센터 )
레이저의주파수안정화방법및그응용 박상언 ( 한국표준과학연구원, 길이시간센터 ) Contents Frequency references Frequency locking methods Basic principle of loop filter Example of lock box circuits Quantifying frequency stability Applications
More informationarxiv: v1 [astro-ph.im] 4 Nov 2011
Techniques of Radio Astronomy T. L. Wilson 1 Code 7210, Naval Research Laboratory, 4555 Overlook Ave., SW, Washington DC 20375-5320 tom.wilson@nrl.navy.mil arxiv:1111.1183v1 [astro-ph.im] 4 Nov 2011 Abstract
More informationPhased Array Feeds A new technology for multi-beam radio astronomy
Phased Array Feeds A new technology for multi-beam radio astronomy Aidan Hotan ASKAP Deputy Project Scientist 2 nd October 2015 CSIRO ASTRONOMY AND SPACE SCIENCE Outline Review of radio astronomy concepts.
More informationInformation in Radio Waves
Using History of Radio presentation: Slide 1: The History of Radio and Radio Astronomy - Introduce the purpose of the overall lesson, which is to give perspective on where all their household technology
More information2.5.3 Antenna Temperature
ECEn 665: Antennas and Propagation for Wireless Communications 36.5.3 Antenna Temperature We now turn to thermal noise received by an antenna. An antenna in a warm environment receives not only a signal
More informationIntroduction to DSTV Dish Observations. Alet de Witt AVN Technical Training 2016
Introduction to DSTV Dish Observations Alet de Witt AVN Technical Training 2016 Outline Theory: - Radio Waves - Radio Telescope Antennas - Angular Sizes - Brightness Temperature and Antenna Temperature
More informationIntroduction to Radioastronomy: Interferometers and Aperture Synthesis
Introduction to Radioastronomy: Interferometers and Aperture Synthesis J.Köppen joachim.koppen@astro.unistra.fr http://astro.u-strasbg.fr/~koppen/jkhome.html Problem No.2: Angular resolution Diffraction
More informationLECTURE 20 ELECTROMAGNETIC WAVES. Instructor: Kazumi Tolich
LECTURE 20 ELECTROMAGNETIC WAVES Instructor: Kazumi Tolich Lecture 20 2 25.6 The photon model of electromagnetic waves 25.7 The electromagnetic spectrum Radio waves and microwaves Infrared, visible light,
More information17. Atmospheres and Instruments
17. Atmospheres and Instruments Preliminaries 1. Diffraction limit: The diffraction limit on spatial resolution,, in radians 1.22 / d, where d is the diameter of the telescope and is the wavelength ( and
More informationFundamentals of the GBT and Single-Dish Radio Telescopes Dr. Ron Maddalena
Fundamentals of the GB and Single-Dish Radio elescopes Dr. Ron Maddalena March 2016 Associated Universities, Inc., 2016 National Radio Astronomy Observatory Green Bank, WV National Radio Astronomy Observatory
More informationRECOMMENDATION ITU-R S.733-1* (Question ITU-R 42/4 (1990))**
Rec. ITU-R S.733-1 1 RECOMMENDATION ITU-R S.733-1* DETERMINATION OF THE G/T RATIO FOR EARTH STATIONS OPERATING IN THE FIXED-SATELLITE SERVICE (Question ITU-R 42/4 (1990))** Rec. ITU-R S.733-1 (1992-1993)
More informationIntroduction to interferometry with bolometers: Bob Watson and Lucio Piccirillo
Introduction to interferometry with bolometers: Bob Watson and Lucio Piccirillo Paris, 19 June 2008 Interferometry (heterodyne) In general we have i=1,...,n single dishes (with a single or dual receiver)
More informationPhased Array Feeds A new technology for wide-field radio astronomy
Phased Array Feeds A new technology for wide-field radio astronomy Aidan Hotan ASKAP Project Scientist 29 th September 2017 CSIRO ASTRONOMY AND SPACE SCIENCE Outline Review of radio astronomy concepts
More informationMultiplying Interferometers
Multiplying Interferometers L1 * L2 T + iv R1 * R2 T - iv L1 * R2 Q + iu R1 * L2 Q - iu Since each antenna can output both L and R polarization, all 4 Stokes parameters are simultaneously measured without
More informationThe Heterodyne Instrument for the Far-Infrared (HIFI) and its data
The Heterodyne Instrument for the Far-Infrared (HIFI) and its data D. Teyssier ESAC 28/10/2016 Outline 1. What was HIFI and how did it work 2. What was HIFI good for science cases 3. The HIFI calibration
More informationLOFAR: Special Issues
Netherlands Institute for Radio Astronomy LOFAR: Special Issues John McKean (ASTRON) ASTRON is part of the Netherlands Organisation for Scientific Research (NWO) 1 Preamble http://www.astron.nl/~mckean/eris-2011-2.pdf
More informationA 3 GHz instantaneous bandwidth Acousto- Optical spectrometer with 1 MHz resolution
A 3 GHz instantaneous bandwidth Acousto- Optical spectrometer with 1 MHz resolution M. Olbrich, V. Mittenzwei, O. Siebertz, F. Schmülling, and R. Schieder KOSMA, I. Physikalisches Institut, Universität
More informationof-the-art Terahertz astronomy detectors Dr. Ir. Gert de Lange
State-of of-the-art Terahertz astronomy detectors Dr. Ir. Gert de Lange Outline Introduction SRON Origin, interest and challenges in (space) THz radiation Technology Heterodyne mixers Local oscillators
More informationChapter 23 Electromagnetic Waves Lecture 14
Chapter 23 Electromagnetic Waves Lecture 14 23.1 The Discovery of Electromagnetic Waves 23.2 Properties of Electromagnetic Waves 23.3 Electromagnetic Waves Carry Energy and Momentum 23.4 Types of Electromagnetic
More informationIntroduction to Radio Interferometry Sabrina Stierwalt Alison Peck, Jim Braatz, Ashley Bemis
Introduction to Radio Interferometry Sabrina Stierwalt Alison Peck, Jim Braatz, Ashley Bemis Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very
More informationUNIT Write short notes on travelling wave antenna? Ans: Travelling Wave Antenna
UNIT 4 1. Write short notes on travelling wave antenna? Travelling Wave Antenna Travelling wave or non-resonant or aperiodic antennas are those antennas in which there is no reflected wave i.e., standing
More informationBasic Calibration. Al Wootten. Thanks to Moellenbrock, Marrone, Braatz 1. Basic Calibration
Basic Calibration Al Wootten Thanks to Moellenbrock, Marrone, Braatz 1 Basic Calibration Outline Sketch of a typical observation Short discussion of formalism Types of calibration A priori A posteriori
More informationIntroduction to Interferometry. Michelson Interferometer. Fourier Transforms. Optics: holes in a mask. Two ways of understanding interferometry
Introduction to Interferometry P.J.Diamond MERLIN/VLBI National Facility Jodrell Bank Observatory University of Manchester ERIS: 5 Sept 005 Aim to lay the groundwork for following talks Discuss: General
More informationEC ANTENNA AND WAVE PROPAGATION
EC6602 - ANTENNA AND WAVE PROPAGATION FUNDAMENTALS PART-B QUESTION BANK UNIT 1 1. Define the following parameters w.r.t antenna: i. Radiation resistance. ii. Beam area. iii. Radiation intensity. iv. Directivity.
More informationDetrimental Interference Levels at Individual LWA Sites LWA Engineering Memo RFS0012
Detrimental Interference Levels at Individual LWA Sites LWA Engineering Memo RFS0012 Y. Pihlström, University of New Mexico August 4, 2008 1 Introduction The Long Wavelength Array (LWA) will optimally
More informationSpectral Line Calibration Techniques with Single Dish Telescopes. K. O Neil NRAO - GB
Spectral Line Calibration Techniques with Single Dish Telescopes K. O Neil NRAO - GB A Quick Review Review: The Rayleigh-Jeans Approximation Planck Law for Blackbody radiation: B= 2hν 3 1 If ν~ghz, often
More informationTSEK02: Radio Electronics Lecture 6: Propagation and Noise. Ted Johansson, EKS, ISY
TSEK02: Radio Electronics Lecture 6: Propagation and Noise Ted Johansson, EKS, ISY 2 Propagation and Noise - Channel and antenna: not in the Razavi book - Noise: 2.3 The wireless channel The antenna Signal
More informationINTERFEROMETRY: II Nissim Kanekar (NCRA TIFR)
INTERFEROMETRY: II Nissim Kanekar (NCRA TIFR) WSRT GMRT VLA ATCA ALMA SKA MID PLAN Introduction. The van Cittert Zernike theorem. A 2 element interferometer. The fringe pattern. 2 D and 3 D interferometers.
More informationIntroduction to Radio Interferometry Anand Crossley Alison Peck, Jim Braatz, Ashley Bemis (NRAO)
Introduction to Radio Interferometry Anand Crossley Alison Peck, Jim Braatz, Ashley Bemis (NRAO) Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope
More informationCommissioning Report for the ATCA L/S Receiver Upgrade Project
Commissioning Report for the ATCA L/S Receiver Upgrade Project N. M. McClure-Griffiths, J. B. Stevens, & S. P. O Sullivan 8 June 211 1 Introduction The original Australia Telescope Compact Array (ATCA)
More informationWide-Band Imaging. Outline : CASS Radio Astronomy School Sept 2012 Narrabri, NSW, Australia. - What is wideband imaging?
Wide-Band Imaging 24-28 Sept 2012 Narrabri, NSW, Australia Outline : - What is wideband imaging? - Two Algorithms Urvashi Rau - Many Examples National Radio Astronomy Observatory Socorro, NM, USA 1/32
More informationLecture 6 Fiber Optical Communication Lecture 6, Slide 1
Lecture 6 Optical transmitters Photon processes in light matter interaction Lasers Lasing conditions The rate equations CW operation Modulation response Noise Light emitting diodes (LED) Power Modulation
More informationModule 5: Experimental Modal Analysis for SHM Lecture 36: Laser doppler vibrometry. The Lecture Contains: Laser Doppler Vibrometry
The Lecture Contains: Laser Doppler Vibrometry Basics of Laser Doppler Vibrometry Components of the LDV system Working with the LDV system file:///d /neha%20backup%20courses%2019-09-2011/structural_health/lecture36/36_1.html
More informationTechnical Considerations: Nuts and Bolts Project Planning and Technical Justification
Technical Considerations: Nuts and Bolts Project Planning and Technical Justification Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long
More informationBritish Astronomical Association Radio Astronomy Group Starbase and the Plug & Play Observatory
British Astronomical Association Radio Astronomy Group Starbase and the Plug & Play Observatory David Farn BSc (Hons) (Open) British Astronomical Association Radio Astronomy Group 21cm Spectrometer Development
More informationObserving Modes and Real Time Processing
2010-11-30 Observing with ALMA 1, Observing Modes and Real Time Processing R. Lucas November 30, 2010 Outline 2010-11-30 Observing with ALMA 2, Observing Modes Interferometry Modes Interferometry Calibrations
More informationUniversity of Groningen. The logistic design of the LOFAR radio telescope Schakel, L.P.
University of Groningen The logistic design of the LOFAR radio telescope Schakel, L.P. IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it.
More informationAntenna Arrays. EE-4382/ Antenna Engineering
Antenna Arrays EE-4382/5306 - Antenna Engineering Outline Introduction Two Element Array Rectangular-to-Polar Graphical Solution N-Element Linear Array: Uniform Spacing and Amplitude Theory of N-Element
More informationObserving Techniques and Calibration. David Frayer (Green Bank Observatory)
Observing Techniques and Calibration David Frayer (Green Bank Observatory) The GBT provides a lot of observing choices Pick receiver based on frequency Pick backend based on observing type (line, continuum,
More informationVLBI Post-Correlation Analysis and Fringe-Fitting
VLBI Post-Correlation Analysis and Fringe-Fitting Michael Bietenholz With (many) Slides from George Moellenbroek and Craig Walker NRAO Calibration is important! What Is Delivered by a Synthesis Array?
More informationPractical Radio Interferometry VLBI. Olaf Wucknitz.
Practical Radio Interferometry VLBI Olaf Wucknitz wucknitz@astro.uni-bonn.de Bonn, 1 December 2010 VLBI Need for long baselines What defines VLBI? Techniques VLBI science Practical issues VLBI arrays how
More informationPractical Radio Interferometry VLBI. Olaf Wucknitz.
Practical Radio Interferometry VLBI Olaf Wucknitz wucknitz@astro.uni-bonn.de Bonn, 23 November 2011 VLBI Need for long baselines What defines VLBI? Techniques VLBI science Practical issues VLBI arrays
More informationREDUCTION OF ALMA DATA USING CASA SOFTWARE
REDUCTION OF ALMA DATA USING CASA SOFTWARE Student: Nguyen Tran Hoang Supervisor: Pham Tuan Anh Hanoi, September - 2016 1 CONTENS Introduction Interferometry Scientific Target M100 Calibration Imaging
More informationMulti-octave radio frequency systems: Developments of antenna technology in radio astronomy and imaging systems
Multi-octave radio frequency systems: Developments of antenna technology in radio astronomy and imaging systems Professor Tony Brown School of Electrical and Electronic Engineering University of Manchester
More informationIF/LO Systems for Single Dish Radio Astronomy cm-wave Receivers
IF/LO Systems for Single Dish Radio Astronomy cm-wave Receivers Lisa Wray, Arecibo Observatory NRAO/NAIC Single Dish Summer School August 2003 Introduction to Receivers a specialized class of microwave
More informationAstronomical Observing Techniques Lecture 6: Op:cs
Astronomical Observing Techniques Lecture 6: Op:cs Christoph U. Keller keller@strw.leidenuniv.nl Outline 1. Geometrical Op
More informationExperiment 5: Spark Gap Microwave Generator Dipole Radiation, Polarization, Interference W14D2
Experiment 5: Spark Gap Microwave Generator Dipole Radiation, Polarization, Interference W14D2 1 Announcements Week 14 Prepset due Fri at 8:30 am PS 11 due Week 14 Friday at 9 pm in boxes outside 26-152
More informationThe Parkes Ultra- Wideband Receiver
The Parkes Ultra- Wideband Receiver Dick Manchester July 30, 2015 CSIRO ASTRONOMY AND SPACE PHYSICS Wideband Receivers for Parkes Need to improve opera6onal efficiency of Parkes while maintaining high-
More informationPractical Radio Interferometry VLBI. Olaf Wucknitz. Bonn, 21 November 2012
Practical Radio Interferometry VLBI Olaf Wucknitz wucknitz@mpifr-bonn.mpg.de Bonn, 21 November 2012 VLBI Need for long baselines What defines VLBI? Techniques VLBI science Practical issues VLBI arrays
More informationsuppose we observed a 10 Jy calibrator with CARMA for 1 year, 24 hrs/day how much energy would we collect? S ηa Δν t
3 hardware lectures 1. receivers - SIS mixers, amplifiers, cryogenics, dewars, calibration; followed by antenna tour; later, take apart a 6-m dewar 2. correlator (James Lamb) 3. local oscillator system
More informationAntennas & Receivers in Radio Astronomy
Antennas & Receivers in Radio Astronomy Mark McKinnon Fifteenth Synthesis Imaging Workshop 1-8 June 2016 Purpose & Outline Purpose: describe how antenna elements can affect the quality of images produced
More informationL- and S-Band Antenna Calibration Using Cass. A or Cyg. A
L- and S-Band Antenna Calibration Using Cass. A or Cyg. A Item Type text; Proceedings Authors Taylor, Ralph E. Publisher International Foundation for Telemetering Journal International Telemetering Conference
More informationCancellation of Space-Based Interference in Radio Telescopes 1. Lou Nigra 2. Department of Astronomy University of Wisconsin Madison, Wisconsin
Cancellation of Space-Based Interference in Radio Telescopes 1 Lou Nigra 2 Department of Astronomy University of Wisconsin Madison, Wisconsin Abstract A concept is presented that was developed at the National
More informationAntennas & Receivers in Radio Astronomy Mark McKinnon. Twelfth Synthesis Imaging Workshop 2010 June 8-15
Antennas & Receivers in Radio Astronomy Mark McKinnon 2010 June 8-15 Outline Context Types of antennas Antenna fundamentals Reflector antennas Mounts Optics Antenna performance Aperture efficiency Pointing
More informationFundamentals of Radio Interferometry. Robert Laing (ESO)
Fundamentals of Radio Interferometry Robert Laing (ESO) 1 ERIS 2015 Objectives A more formal approach to radio interferometry using coherence functions A complementary way of looking at the technique Simplifying
More informationCHAPTER 6 THE WIRELESS CHANNEL
CHAPTER 6 THE WIRELESS CHANNEL These slides are made available to faculty in PowerPoint form. Slides can be freely added, modified, and deleted to suit student needs. They represent substantial work on
More informationRECEIVING SYSTEMS FOR RADIO ASTRONOMY
RECEIVING SYSTEMS FOR RADIO ASTRONOMY SHUBHENDU JOARDAR B.Tech. (Electronics, NIT Calicut) M.S. (Microwaves, IIT Madras) F.I.E.T.E. (IETE, India) Ph.D. (Physics, University of Kalyani) License This presentation
More informationUNIT Explain the radiation from two-wire. Ans: Radiation from Two wire
UNIT 1 1. Explain the radiation from two-wire. Radiation from Two wire Figure1.1.1 shows a voltage source connected two-wire transmission line which is further connected to an antenna. An electric field
More informationAntenna Fundamentals. Prof. Ryszard Struzak Na8onal Ins8tute of Telecommunica8ons, Poland r.struzakatieee.org
Antenna Fundamentals Prof. Ryszard Struzak Na8onal Ins8tute of Telecommunica8ons, Poland r.struzakatieee.org Beware of misprints!!! These materials are preliminary notes intended for my lectures only and
More information9. Microwaves. 9.1 Introduction. Safety consideration
MW 9. Microwaves 9.1 Introduction Electromagnetic waves with wavelengths of the order of 1 mm to 1 m, or equivalently, with frequencies from 0.3 GHz to 0.3 THz, are commonly known as microwaves, sometimes
More informationSubmm and Radio. Chapter 8: Submillimeter and Radio Astronomy
Chapter 8: Submillimeter and Radio Astronomy 8.1. Introduction The submillimeter and millimeter-wave regime roughly 0.2 mm to 3 mm - represents a transition between infrared and radio methods. Because
More informationTSEK02: Radio Electronics Lecture 6: Propagation and Noise. Ted Johansson, EKS, ISY
TSEK02: Radio Electronics Lecture 6: Propagation and Noise Ted Johansson, EKS, ISY 2 Propagation and Noise - Channel and antenna: not in the Razavi book - Noise: 2.3 The wireless channel The antenna Signal
More informationMulti-band Dual-Polarization Lens-coupled Planar Antennas for Bolometric CMB Polarimetry
Multi-band Dual-Polarization Lens-coupled Planar Antennas for Bolometric CMB Polarimetry Adrian T. Lee Department of Physics, University of California, Berkeley CA 9472 Physics Division, Lawrence Berkeley
More informationRec. ITU-R F RECOMMENDATION ITU-R F *
Rec. ITU-R F.162-3 1 RECOMMENDATION ITU-R F.162-3 * Rec. ITU-R F.162-3 USE OF DIRECTIONAL TRANSMITTING ANTENNAS IN THE FIXED SERVICE OPERATING IN BANDS BELOW ABOUT 30 MHz (Question 150/9) (1953-1956-1966-1970-1992)
More informationProgress Towards Coherent Multibeam Arrays
Progress Towards Coherent Multibeam Arrays Doug Henke NRC Herzberg Astronomy and Astrophysics, Victoria, Canada August 2016 ALMA Band 3 Receiver (84 116 GHz) Dual linear, 2SB Feed horn OMT (two linear
More informationSpectral Line Bandpass Removal Using a Median Filter Travis McIntyre The University of New Mexico December 2013
Spectral Line Bandpass Removal Using a Median Filter Travis McIntyre The University of New Mexico December 2013 Abstract For spectral line observations, an alternative to the position switching observation
More information