Propagation Background and Noise

Author(s):  
Michael E. Thomas

Noise from the detector and source is always considered in a system design study. However, as an optical field propagates, it acquires additional noise and background radiance from the path defined by the source and by the field of view of the detector. This is typically in the form of propagation path emission and background emission, and bulk scattering within the propagation medium and surface scattering at the propagation medium boundaries of hot-object radiation (e.g., the sun) into the sensor field of view. In many cases this severely limits system performance. Also, in a passive system when no source is present, the background radiance is the signal of interest. Path emission can be modeled by the radiation transfer equation given by Eq. 2.85a. The source function, ℘+(s), must now be given an explicit representation. Figure 11.1 illustrates the incremental emittance per incremental length and bandwidth along an optical path in thermal equilibrium.

2020 ◽  
Vol 494 (1) ◽  
pp. 1229-1236 ◽  
Author(s):  
Nicola T Locatelli ◽  
Gianni Bernardi ◽  
Germano Bianchi ◽  
Riccardo Chiello ◽  
Alessio Magro ◽  
...  

ABSTRACT Fast radio bursts (FRBs) remain one of the most enigmatic astrophysical sources. Observations have significantly progressed over the last few years, due to the capabilities of new radio telescopes and the refurbishment of existing ones. Here, we describe the upgrade of the Northern Cross radio telescope, operating in the 400–416 MHz frequency band, with the ultimate goal of turning the array into a dedicated instrument to survey the sky for FRBs. We present test observations of the pulsar B0329+54 to characterize the system performance and forecast detectability. Observations with the system currently in place are still limited by modest sky coverage (∼9.4 deg2) and biased by smearing of high dispersion measure events within each frequency channels. In its final, upgraded configuration, however, the telescope will be able to carry out unbiased FRB surveys over a ∼350 deg2 instantaneous field of view up to z ∼ 5, with a (nearly constant) $\sim 760 \, (\tau /{\rm ms})^{-0.5}$ mJy rms sensitivity.


1979 ◽  
Vol 50 ◽  
pp. 26-1-26-25
Author(s):  
David L. Fried

AbstractThe concepts of speckle interferometry as developed by Labeyrie, and of speckle imagery as formulated by Knox and Thompson are analyzed for dependence on field-of-view size. The preliminary analysis, assuming isoplanatism rederives the results of Korff, and derives the result previously inferred by Knox and Thompson from computer simulation, that allowable spatial frequency separation for difference of phase shift determination must be less than r0/λ When the assumption of isoplanatism is dropped, results are obtained for the expected object power spectrum in speckle interferometry and for the expected bispectrum in speckle imagery, showing the dependence on angular spread for an object consisting of a pair of point sources. An angle, ϑ, is defined (in terms of an integral over the strength of turbulence distribution along the propagation path), which bounds the range within which there are no significant anisoplanatism effects. It is noted that the effect of anisoplanatism is not to attenuate the information bearing signal but rather to impose incorrect information on the signal. Thus anisoplanatism can result in incorrect conclusions with no indication that there is a problem.


2012 ◽  
Vol 85 (1) ◽  
Author(s):  
J. Leach ◽  
R. E. Warburton ◽  
D. G. Ireland ◽  
F. Izdebski ◽  
S. M. Barnett ◽  
...  

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