WWW.DISSERTATION.XLIBX.INFO
FREE ELECTRONIC LIBRARY - Dissertations, online materials
 
<< HOME
CONTACTS



Pages:   || 2 |

«Abstract We show two slightly-different designs for a simple, small, effective, radio telescope capable of observing the Sun, and the galactic plane ...»

-- [ Page 1 ] --

A 21cm Radio Telescope for the Cost-Conscious

Marcus Leech, Science Radio Laboratories, Inc

Abstract

We show two slightly-different designs for a simple, small,

effective, radio telescope capable of observing the Sun, and

the galactic plane in both continuum and spectral modes,

easily able to show the hydrogen line in various parts of

the galactic plane.

Introduction

The emergence of new, relatively-inexpensive tools for the RF tinkerer has allowed a re-examination of

the “bottom end” of small-scale and amateur radio astronomy. Until quite recently, anyone on a very small budget, or with outdoor space constraints would likely be stuck with a simple radio telescope such as the IBT1. While such an instrument is an excellent device for portable classroom demonstrations of the very-basic principles of radio astronomy, this author wished to explore that space further. Specifically, the possibility of an instrument with a roughly 1m reflector, capable of observing the hydrogen line, and the continuum emissions from the galactic plane, in addition to the Sun. Since the IBT is only really capable of observing the Sun, it was felt that a richer educational experience might be realized by having a slightly-more-capable instrument within a similar budgetary envelope.

Software Defined Radio In the past, having a radio astronomy receiver that was capable of providing spectral information was out of budgetary reach of the small-classroom environment. Fine instruments such as the SpectraCyber made by Radio Astronomy Supplies, for example, are easily affordable by most higher-eduction institutions, but usually not at the high-school level.

In the past few years, Software Defined Radio (SDR) has emerged as an exciting new technology that is increasingly being leveraged by amateur radio astronomers to expand their experimental horizons relatively cheaply. With an SDR, the RF signals are typically converted to so-called “baseband” form, and then digitized at one or two megasamples/second, and then forwarded to a PC for further processing. In this way, the signals are presented in their “rawest” form, so that they may be processed in many different ways to extract different types of experimental data. With SDR, there is no hardware that is specifically dedicated to continuum observations, or spectral observations, or other types of specialized modes. All the processing happens in software, rather than analog hardware.

Software “frameworks”, such as Gnu Radio have significantly simplified the ad-hoc construction of software-based signal-processing “chains”, allow many different types of experiments to be conducted on real-time radio telescope data, using SDR receivers as input.

1 See, for example: http://www.gb.nrao.edu/epo/ibt.shtml Receiver Hardware: RTLSDR In early 2012, it was discovered that certain DVB-T “dongles” (USB devices intended to allow you to watch over-the-air DVB-T broadcast television) had a special “mode” that allow them to be used as crude SDR receivers. In this mode, the digital base-band samples bypass the DVB-T demodulator/decoder in the RTL2832U chip, and are sent over USB. Normally, these devices send partially-decoded MPEG transport frames over the USB, but in this “SDR” mode, they send raw I/Q base-band samples instead.

These “dongles” are typically shipped with one of two or three different tuner chips, and the most popular ones, the R820T and E4000 tuners both allow tuning to the hydrogen-line frequency of 1420Mhz.

These devices, being mass-market consumer devices, are available very cheaply, usually under $20.00 from on-line sellers on eBay, AliExpress, Nooelec2, etc.

A driver library was quickly produced3 based on the information gleaned from datasheets and a bit of reverse engineering. The driver library can be used stand-alone, or in concert with a “plug in” for Gnu Radio that allows Gnu Radio applications to use the RTLSDR devices.

These devices, while quite inexpensive, have some noticeable drawbacks:

Dynamic range is quite limited, due to use of an 8-bit ADC, roughly 45dB SFDR  Phase and amplitude balance is quite poor, leading to image problems  Frequency accuracy is extremely poor, typically +/- 70PPM or worse  Phase noise, due to the poor crystals used, is also very poor  Temperature stability is poor, leading to gain drift, and frequency drift  Shielding is non-existent, so you have to add that yourself  Despite all of the above, it’s possible to obtain entirely-adequate results with appropriate “aftermarket” re-engineering of the devices.

Hardware: Ettus Research B100+WBX combo package Since 2005, Ettus Research have been designed and manufacturing a growing line of Software Defined Radios that offer extremely good performance at very competitive prices. Unlike the RTLSDR hardware described above, the Ettus radios are purpose-built for SDR applications.

Comparing the B100+WBX combination package to the RTLSDR:

Higher dynamic range, using 12-bit ADCs, giving roughly 70dB of SFDR  Much better frequency precision: +/- 2.5PPM  Much lower phase noise  Much better phase/amplitude balance  2 See: http://www.nooelec.com/store/software-defined-radio/tv28tv2.html 3 See: http://sdr.osmocom.org/trac/wiki/rtl-sdr Shielded enclosure  The author has used Ettus hardware in radio astronomy projects since 2005 and finds that they are an exceptional value.





The radios are priced as you might expect for a “niche market” item intended for technology developers, however, in that market they are extremely competitively priced. For a school wishing to get noticeably-better results, the Ettus B100+WBX4 combination package is an excellent choice.

Hardware: ~1m offset dish The IBT uses an offset-fed satellite dish that is typically 0.5M in diameter or somewhat larger. While such a dish affords excellent portability, the aperture is somewhat too small for sensitive observations of the galactic plane at 21cm.

The author has achieved excellent results using an offset-fed satellite dish, measuring 93cm x 85cm, and it is suggested that experimenters try to find a dish of roughly this size. Such small, offset-fed dishes are available online5 from a number of online satellite retailers as well as eBay. In many large cities, there are still “brick and mortar” satellite equipment retailers where such dishes may be purchased reasonably cheaply.

Occasionally, you may find people discarding these dishes, having migrated back to cable television away from satellite television.

It’s important that any dish acquired include the feed-arm hardware. There are also many “package deals” that will sell you a dish and a Ku-band LNB. The Ku-band LNB may be used in other experiments, but primarily it helps to give a good notion of how to position the 21cm feed-horn assembly that is described later in this article.

The feed-arm hardware will have to be modified to accommodate the much-larger 21cm feed-horn assembly.

Alternative hardware: ~1m prime-focus dishes There are also small prime-focus dishes available from some places, roughly 1.3m in diameter. These have the advantage that they’re easier to point, but are generally significantly more expensive, and harder to find, than the offset dishes of roughly the same diameter. Manufacturers such as Jonsa and Foretec Star6 make such dishes, but it can often be hard to find local distributors.

The feed assembly for these dishes is less complicated to make as well, since they tend to be deeper (0.38 to 0.42 F/D).

Hardware: Feed assembly The feed assembly will have to be hand-made. Fortunately, making one is very straightforward. We start with a so-called “2lb” tin-plated coffee can. These cans are 6” in diameter, and usually 7” to 8” tall, containing 2 to 2.5lb of coffee.

4 See: https://www.ettus.com/product/details/USRP%20Instant%20SDR%20B100%20Bundle%20-%20B100%20+ %20WBX%20Bundle%20%2850-2200MHz%29%20+%20LiveUSB 5 See: http://www.sadoun.com/Sat/Order/Dishes/Free-to-air-satellite-dish.htm 6 See: http://angelelectronics.ca/shop/satellite/dishes/fortecstar-fc06 You’ll need to empty the can, either through gradual consumption of the contents, or something a bit more draconian.

The cans are usually sealed with a thin aluminum membrane as well as the plastic lid. If making a feed for a prime-focus/deep dish, retain the plastic lid, it will make a useful weather cover.

Once you’ve removed the sealing membrane, there will be a little ring of aluminum still attached to the can. Use a can-opener to remove it.

Wash and dry the can using a bit of dish soap.

Drill a hole through the side of the can for your chosen connector. Type ‘N’ is popular, but this author used a tin-plated type ‘F’ since all his “plumbing” is type-F compatible. The hole should be 3” from the bottom of the coffee can, as shown below.

If you’re using a tin-plated type ‘F’ bulkhead or PCB edge-mount connector, you can solder the connector directly to the coffee can. You’ll need to use a soldering-gun to do that to provide the extra heat that will be necessary.

If you use a type ‘N’ or other connector, you’ll have to drill holes as appropriate. Choose a connector that is compatible with whatever LNA you’ll be using, with minimum adaptors required, to reduce front-end losses.

One thing to note is that drilling thin steel sheet requires considerable care, and it’s usually necessary to step your drill sizes up gradually, so as not to try to remove too much material at a time.

You’ll need to solder a probe to the center conductor of the connector, approximately 1.8” long, and made from 10 or 12-gauge copper wire. Brass tubing also works well.

If using a prime-focus dish with a F/D of 0.38 to 0.45, the coffee-can feed alone is sufficient to produce acceptable results. Put the plastic lid back on, and cut a small “cross” with a sharp knife in the middle of the lid—this allows pressure equalization so you don’t get moisture “pumping” into the can interior.

Before you do this, you can also give the can exterior and interior a couple of light coats of clear lacquer spray-paint – this will slow down the inevitable corrosion of the steel. Dont forget to tape-off the connector when you’re doing this!

If using a shallow offset-fed dish, you’ll need to augment the coffee-can feed with a pair of tapered adapters that increase the gain of the feed, to properly illuminate the dish.

Go to your nearest HVAC equipment/ducting supplier and get a 6” to 8” round galvanized tapered adapter, and another 8” to 10” adapter. If you can, get the type that are crimped on one side, so that they mesh together easily. Otherwise, you’ll need to use tin-snips to create a few slots—one set to allow the 6” to 8” adaptor to fit the coffee can, and the other to allow the 6” to 10” adaptor to fit into

the 6” to 8” adaptor. Once you have them all fit together it should look, in profile, roughly like this:

Drill some small holes, and use self-tapping 3/8” long, #6 sheet-metal screws to hold all pieces together. Use them liberally to improve mechanical rigidity, and electrical conductivity between all the pieces.

Again, apply a couple of light coats of clear lacquer to the assembly (although tape the connector, since you don’t want to make it non-conductive).

A sheet of clear polyethylene over the end will keep birds from wanting to nest in the feed. Make sure there’s a small vent hole somewhere.

Hardware: Feed Arm Modifications If using an offset-fed dish, modifications to the feed arm assembly will be necessary to make sure that the focus is in the middle of the 10” throat of the feed. Some amount of inventiveness will be required here, since the feed-arm arrangements are different on different dishes.

On the authors 93cm offset dish, there’s a single support arm that comes from behind the dish around to the front. Removal of roughly 12cm of feed arm allowed for the 10” horn throat to be at roughly the correct location at the focus.

The feed should be aimed so that it’s pointing at just below the center of the dish. Again, a certain amount of inventiveness will be required, and it’s likely that post-construction signal measurements will need to be made to optimize the feed location and pointing.

If all the feed hardware was supplied for the dish, along with a cheap LNB, you can use that as a guide as to where the focal point is, and adjust accordingly for the much-larger feed-horn for 21cm.

The author uses an L bracket attached to the front of the feed, and bent so that the feed points at the correct location on the dish, with the other side of the L bracket attached with band clamps to the feed arm.

Hardware: Low Noise Amplifier (LNA) It is vital that the first stage of amplification in a radio telescope have as little self-noise as practical.

This is known as the Noise Figure of the amplifier. Since the signals we’re looking for are very faint, having a low noise figure improves our chances of detecting them. In selecting a low-noise amplifier it

should be:

1dB noise figure (NF)  20dB gain  Ideally, it should be filtered to allow only the 21cm band to pass  Optionally, it can be powered via the output connection, so that DC can be fed up the coax.

 Such LNAs are available from a few suppliers on the Internet, including Radio Astronomy Supplies, and Down East Microwave.

Hardware: Line amplifiers You’ll very likely need two more stages of amplification before the signal is presented to your receiver.

The most convenient method is to use CATV/SAT-TV “line amplifiers” that offer between 10 and 20dB of gain, but have poor noise figures. These units are usually available for about $5.00 each, and are powered over the coaxial connection on their output.

If you choose to power the amplifier-chain via the coax, it is also necessary to obtain a DC power injector—available from the same suppliers as the line amplifiers.



Pages:   || 2 |


Similar works:

«ApJS in press On Validating an Astrophysical Simulation Code A. C. Calder1,2, B. Fryxell1,3, T. Plewa1,2,4, R. Rosner1,2,3, L. J. Dursi1,2, V. G. Weirs1,2, T. Dupont1,5, H. F. Robey6, J. O. Kane6, B. A. Remington6, R. P. Drake7, G. Dimonte6, M. Zingale1,8, F. X. Timmes1,2, K. Olson1,8, P. Ricker1,2, P. MacNeice8, and H. M. Tufo1,5 ABSTRACT Center for Astrophysical Thermonuclear Flashes, The University of Chicago, Chicago, IL 60637 Department of Astronomy & Astrophysics, The...»

«National Aeronautics and Space Administration Exploring Stars in the Milky Way i Exploring Stars in the Milky Way Space Math http://spacemath.gsfc.nasa.gov ii Math textbooks routinely provide ‘real world’ examples for students using familiar examples drawn from every-day situations, but there are many other areas where proportional relationships and working with large numbers aid in understanding our physical world. This collection of activities is intended for students looking for...»

«Sistema de Retiro del Servicio Civil (CSRS) Sistema de Retiro de Empleados Federales (FERS) ¿Está pensando en su retiro? Una visión general de las cosas más importantes que los empleados federales deben hacer cuando planeen su retiro. Oficina de Administración de Personal Federal (OPM) Servicio de Retiro y Seguro RI 83-11SP Revisado en octubre de 1997 La edición de octubre de 1996 aún está vigente. Información adicional sobre el retiro y todas las publicaciones de la Oficina de...»

«L-AP “Exploring Creation With Astronomy” Lessons 1-14 Lapbook Package PLEASE NOTE: This product includes BOTH lapbooks for this book. One lapbook covers lessons 1-6, and the other covers lessons 7-14. This lapbook has been specifically designed for use with the book, “Exploring Creation with Astronomy” by Jeannie Fulbright and Apologia Science. Templates are printed with colors that best improve information retention according to scientific research. Designed by Cyndi Kinney of...»

«Newsletter November 2013 Issue 9 President’s Report Welcome to the November edition of AANSW newsletter Orbits. The month starts with an auspicious Hybrid Solar eclipse – meaning that the eclipse starts as an Annular then moves into a Total. When it comes to solar eclipses this eclipse numbered astronomically as Saros 143, or astrologically Saros 16 North belongs to a friendly family (Brady, Eagle & Lark). Born on February 15th 1599 o.s, @ 6 degrees Pisces, at the North Pole, with Sun/Moon...»

«Bull. Astr. Soc. India (2013) 41, 1–17 The discovery of quasars K. I. Kellermann National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA, 22901, USA Received 2013 February 01; accepted 2013 March 26 Abstract. Although the extragalactic nature of quasars was discussed as early as 1960, it was rejected largely because of preconceived ideas about what appeared to be an unrealistically high radio and optical luminosity. Following the 1962 occultations of the strong radio...»

«VII Simposio Internacional y XII Jornadas Nacionales de Investigación Acción en Turismo CONDET Congreso Internacional de Turismo – ANET Facultad de Turismo – UNCo Neuquén – Octubre 2015 EJE: Políticas públicas en turismo Turismo, conservación y políticas públicas en espacios de frontera. El rol de los parques nacionales en la Norpatagonia andina argentina (1916-1976) Laila Vejsbjerg Dependencia institucional: Instituto de Investigaciones en Diversidad Cultural y Procesos de Cambio...»

«MEGALITHIC SITES IN BRITAIN BY A. THOM Chapter 1. Introduction Chapter 2. Statistical Ideas Chapter 3. Astronomical Background Chapter 4. Mathematical Background Chapter 5. The Megalithic Yard Chapter 13. The Extinction Angle Chapter 14. Conclusions List of Figures, Tables and Sites (added) OXFORD AT THE CLARENDON PRESS [ 1971 ] 1. INTRODUCTION–Selected from hundreds of small-scale copies of surveys made by Professor Thom over the past thirty years, examples are chosen to illustrate some of...»

«Photometric Observations of a Very Young Family-Member Asteroid (832) Karin Fumi Yoshida1 Budi Dermawan2,3 Takashi Ito4 Yu Sawabe5 Masashige Haji5 Ryoko Saito5 Masanori Hirai5 Tsuko Nakamura1 Yusuke Sato6 Toshifumi Yanagisawa7 and Renu Malhotra4 1 National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo, 181-8588, Japan yoshdafm@cc.nao.ac.jp 2 School of Science, University of Tokyo, Bunkyo, Tokyo 113-0033 3 Department of Astronomy, Bandung Institute of Technology, Bandung 40132,...»

«Research Giulio Magli The Megalithic Building of S. Erasmo di Dipartimento di Matematica Cesi: Architecture, Astronomy, and Politecnico di Milano Landscape Pzza. Leonardo da Vinci 32 20132 Milano, ITALY Giulio.Magli@polimi.it Abstract. One of the most enigmatic megalithic buildings of Italy is the structure which lies on the S. Erasmo hill near Cesi, in Umbria, a Nicola huge complex encompassing an area of around 8000 square meters and enclosed by refined cyclopean walls. Although its date is...»

«On-Sky Tests of an A/R Coated Silicon Grism on board NICS@TNG F. Vitali*a, V. Fogliettib, D. Lorenzettia, E. Ciancic, F. Ghinassid, A. Harutyunyand, S. Antoniuccia, C. Riverold, L. Riverold a INAF Osservatorio Astronomico di Roma, Via Frascati 33, 00040-I Monte Porzio Catone Italy b CNR Istituto di Struttura della Materia, Area della Ricerca Roma 1, Montelibretti, Via Salaria, Km. 29,300, 00016-I Monterotondo Italy c CNRIstituto per la Microelettronica e Microsistemi, Laboratorio MDM, Via C....»

«Carl Sagan / The Nuclear Winter http://www.cooperativeindividualism.org/sagan_nuclear_winter.html.. The Nuclear Winter Carl Sagan Carl Sagan, a modern-day Renaissance man of science, was horn in 1934 in New York. After graduating with both a B.A. and a B.S. degree from the University of Chicago, Sagan completed his M.S. in physics and earned a Ph.D. in astronomy and astro-physics in 1960. Sagan was nominated to join the Smithsonian Astrophysical Observatory in 1962. At the same time, he also...»





 
<<  HOME   |    CONTACTS
2016 www.dissertation.xlibx.info - Dissertations, online materials

Materials of this site are available for review, all rights belong to their respective owners.
If you do not agree with the fact that your material is placed on this site, please, email us, we will within 1-2 business days delete him.