How is the gain of a radio antenna at 230GHz calculated?

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SUMMARY

The calculation of radio antenna gain at 230 GHz involves understanding the power radiated by the source, specifically bolometric luminosity, which is noted as 1036 erg/s in this discussion. The Event Horizon Telescope serves as a relevant example of a mm-VLBI instrument that operates effectively at this frequency, utilizing the CARMA array for observations. The discussion highlights the significance of 230 GHz as it corresponds to strong transition lines for carbon monoxide, making it crucial for detecting radio jets and mapping black hole jets. Additionally, the resolution of millimeter VLBI is well-suited for studying inner disk physics around black holes.

PREREQUISITES
  • Understanding of bolometric luminosity and its implications in radio astronomy
  • Familiarity with millimeter-wave Very Long Baseline Interferometry (VLBI) techniques
  • Knowledge of the Event Horizon Telescope and its operational principles
  • Basic principles of blackbody radiation and brightness temperature calculations
NEXT STEPS
  • Research the calculation methods for radio antenna gain at high frequencies, specifically at 230 GHz
  • Explore the principles of brightness temperature and its relevance in radio astronomy
  • Study the operational techniques of the CARMA array and its applications in millimeter-wave observations
  • Investigate the effects of general relativity on black hole imaging and the significance of black hole shadows
USEFUL FOR

Astronomers, astrophysicists, and researchers involved in radio astronomy, particularly those focusing on high-frequency observations and black hole studies.

isha89
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Is it feasible to perform space VLBI at 230 GHz? Also how does one detect the radio jets at 230 GHz?
 
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I don't know if it has been done before, but take a look at the event horizon telescope. It is designed to be a mm-VLBI instrument.

Why are you interested in 230 GHz? It happens to be among the strongest transition lines for the carbon monoxide molecule (2nd most abundant molecule after H_2). Either way, 230 Ghz corresponds to a wavelength of 1.3mm, which means it is easily accessible to the CARMA, which is an array of millimeter to centimeter telescopes. It uses up to 23 dishes which can be moved around depending on the observations.

At this frequency, we are stepping out of the radio regime. Black hole jets emit most of the synchrotron radiation at much lower wavelengths. In general, though, we can map out a jet by taking measurements of the intensity of the light at different locations on the sky. One can also take measurements of different frequencies at a point on the sky. Most radio/mm observations do both.
 
Well, the resolution of millimeter and submillimeter wavelength VLBI is well matched to the scale of inner disk physics. Base- lines from Hawaii or Western Europe to Chile provide fringe spacings as small as 30 μas (3 RS) at 230 GHz and 20 μas at 345 GHz. Millimeter VLBI thus has the potential to de- tect signatures of hot spot and jet models proposed to explain the rapid variability of Sgr A* as well as strong general relativistic effects, such as the black hole silhouette or shadow. Also the man made noise will also be eliminated if we use a space based technique.

What I'm confused about now is how to calculate the gain of the radio antenna at 230GHz. Because the gain requires the power radiated by the source. I only managed to obtain a value for bolometric luminosity which is 10^36 erg/s. But can this be used to calculate gain?
How do I calculate brightness temperature ?? I do not know the value of blackbody temperature T.
T = Bn(T)c2/2kn2
 

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