Characteristics measurement of Baghdad University radio telescope for hydrogen emission line

Jallod, Uday E.; Abood, Kamal M.

doi:10.1063/1.5138521

Cited by 3 publications

(1 citation statement)

References 10 publications

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“…Dipole antennas are used because they are able to receive signals of varying frequencies in a balanced manner. It also aids the device in resolving reception issues brought on by competing signals [13]. Radio astronomy signals travel through the air in a straight line, are reflected from layers of the ionosphere or clouds, or are relayed by satellites in space are weak of man-made radio signal noise, or a sign that interferes with blocking radio astronomers' astronomical signals is called radio frequency interference (RFI) [14].…”

Section: Introductionmentioning

confidence: 99%

Study of Sky Radio Frequency Interference Background Level Behavior During the Partial Solar Eclips on 25 Oct. 2022 at The Baghdad University Location

Kahdim,

Abood

2024

Al-Mustansiriyah Journal of Science

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Radiofrequency interference (RFI) describes the weakening of radio astronomy transmissions caused by man-made radio signal noise in radio telescope observation indicates the level of radio frequency noise in the sky at all times, regardless of any astronomical sources. This noise is affected by various sources, including Earth's atmosphere or solar activity and all communications equipment operating near the radio telescope. In this study, the background noise which includes RFI was measured using HSA2000 series receiver spectrum analyzer, which connected with two dipole antennas in different frequency bands (15-80 MHz) low band antenna, and (110-240 MHz) high band antenna during the partial solar eclipse in Baghdad on October 25, 2022, at (12:00-15:00), as a simple radio telescope to observe the radio astronomical background level in the sky. It is clear that the average amount of RFI level during a partial solar eclipse (-83.249 dBm for LBA decreased by about (0.93) from the value on a normal day (-77.495 dBm). And For HBA -84.711 dBm decreased by about (0.85) from the value on a normal day (-72.784 dBm). Also, it was noticed that these amounts are approximately equal to the RFI level at night (-82.352 dBm for LBA and -82.739 dBm for HBA). It is (0.98) for LBA and (0.97) for HBA, respectively. This research confirms that despite the short duration of the partial eclipse, the average value during the partial eclipse period is close to the average values during the night period due to the decrease in the electronic density of the ionosphere, especially at low frequencies, and the FRI of ground disturbances as a result of the activities of human from the surrounding the monitoring area. also, found that at the monitoring point, there is a good relationship between the time of the maximum partial eclipse and the peaks of signal gain strength.

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Section: Introductionmentioning

confidence: 99%

Study of Sky Radio Frequency Interference Background Level Behavior During the Partial Solar Eclips on 25 Oct. 2022 at The Baghdad University Location

Kahdim,

Abood

2024

Al-Mustansiriyah Journal of Science

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Observations results improvement using switching technique and noise source calibration unit

Hameed

Abood²

2022

AIP Conference Proceedings

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Simulation of Small Radio Telescope Antenna Parameters at Frequency of 1.42 GHz

Jallod

Mahdi

Abood

2022

IJP

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The paper presents an overview of theoretical aspects of small radio telescope antenna parameters. The basic parameters include antenna beamwidth, antenna gain, aperture efficiency, and antenna temperature. These parameters should be carefully studied since they have vital effects on astronomical radio observations. The simulations of antenna parameters were carried out to assess the capability and the efficiency of small radio telescopes to observe a point source at a specific frequency. Two-dimensional numerical simulations of a uniform circular aperture antenna are implemented at different radii. The small diameter values are chosen to be varied between (1-10) m. This study focuses on a small radio telescope with a diameter of 3 m since this telescope is very common in the world. The simulated results of this study illustrated that the power pattern of a 3 m antenna has a half-power beamwidth of approximately 5 degrees. Also, the maximum peak antenna temperature is estimated to be more than 3000 K. All of these results were in good agreement with observations of the neutral hydrogen spectral line at the frequency of 1.42 GHz using a small radio telescope.

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Characteristics measurement of Baghdad University radio telescope for hydrogen emission line

Cited by 3 publications

References 10 publications

Study of Sky Radio Frequency Interference Background Level Behavior During the Partial Solar Eclips on 25 Oct. 2022 at The Baghdad University Location

Study of Sky Radio Frequency Interference Background Level Behavior During the Partial Solar Eclips on 25 Oct. 2022 at The Baghdad University Location

Observations results improvement using switching technique and noise source calibration unit

Simulation of Small Radio Telescope Antenna Parameters at Frequency of 1.42 GHz

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