TEAM MEMBERS

 

         James R. LeMire                   Arnold E. Lupe Jr.                   Oscar Munoz         

     

 

 

 

PROJECT SPONSORS

 

 

University of Texas at El Paso 

 Dr.  Jorge A. Lopez PhD       Physics Dept.

  Dr. William G. Durrer PhD     Physics Dept.

 Dr. Joseph H. Pierluissi  PhD   Electrical Engineering Dept.

 

 

 

 

 

    ABSTRACT

 

This project consists of building a radio telescope, using a very small array of two to four 8 satellite dishes. The telescope will be used by the Physics Department, from the University of Texas at El Paso (UTEP), to study various levels of neutral hydrogen gases that exists in space.

 

 

 

OBJECTIVE

 

         Construct a Radio Telescope using a small array of satellite dishes

         Targeted receiving frequency of 1420 MHz  +/- 600 KHz 

         Project Completion;  April 2004

         To remain within our sponsors $5,000 budget

         Meet all project deadlines in timely and efficient manners

 

 

 

 

METHOD OF COMPLETION

 

Our team will attempt to build a radio telescope using two to four satellite antennas formed into a linear array. The signal of the antennas will be combined, and connected into a hydrogen spectrometer.  The spectrometer will then display the data as a function of time vs. frequency.

To solve the problem, our team organized itself into three technical sections. Carlos Munoz is working with interferometry and radiation patterns, James LeMire is responsible for the antennas, transmission lines, and the amplifiers.  Arnold Lupe is handling the output of the signal from the spectrometer to the display.

A linear array pattern allows the Radio Telescope to focus in on a single frequency.  This radiation pattern will create one central lobe, in order to keep the beam width at the smallest value possible.   The beam width, which is the angular width of the radiation lobes, will need to be at about 1 degree. This pattern will provide the antenna's feed horn with the best possible lobe with which to gather information.  

The telescope will be placed on top of the UTEP Physics Department Building at approximately 200 feet apart in line with East and West.  The satellite antennas will initially be pointed straight up into the sky at a 90o angle with respect to our horizon. 

 250 feet of coaxial cable will be attached to each satellite with Low Noise Amplifiers (LNA) emplaced at 50-foot intervals.  The amplifiers are to ensure the data will reach the Spectrometer since the cable has a attenuation factor of 10 dB per 50 feet. 

 Once at the Spectrometer, the data will then be converted to a 70 MHz signal.  From this point the data will be interpreted by the Spectrometers software at a rate of 2400 baud, for an 8 bit data form.  This will result in a visual graph of the incoming 1420 MHz Hydrogen line spectrum.  The graph will be displayed as a frequency vs. time scale with a +/- 600 KHz to accommodate the Doppler Shift.  

This initial emplacement will provide the Physics Dept with an initial reference point to collect and interpret the data.  Additional adjustment will be made as needed by the Physics Dept. 

 

 

 

 

BLOCK DIAGRAM

 

                                         

 

 

 

 

 

 

ISSUES

      Obtaining two additional antennas to strengthen the interferometry to improve the Radio Telescope's resolution.

       Transportation of the dish antennas to the projected location.       

 

 

 

 

 

CURRENT STATE OF PROJECT

The team has obtained enough peripheral equipment to support two satellite antennas.  However, with only one antenna feed-horn it would be difficult to accurately test all equipment.  A single antenna will only provide a wide central lobe.  This wide central lobe will yield a poor resolution at the spectrometer output, which is not ideal for frequency specific data research.