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NOEMA instrumental modes
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IRAM Memo 2025-1 NOEMA
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IRAM Memo 2025-1 NOEMA
Contents
NOEMA instrumental modes
The interferometric point source sensitivity
Power and sensitivity measured at the correlator output for one baseline
Quantization efficiency
From the temperature power to the flux
Collecting the measurements from all baselines
Signal decorrelation
Noise vs signal
Summary and interpretation
The interferometric extended source sensitivity
Yielding the interferometric extended source sensitivity
Interpretation
The system temperature
Definition
Line vs continuum system temperature
Receiver temperature
In practice
Line vs continuum system temperature
The number of polarizations
Actual computations
Elapsed telescope time vs on-source time
Sensitivity for a single-source, single-field observations
Sensitivity for track-sharing, single-field observations
Sensitivity for mosaicking
References
A few reminders: Flux vs brightness in radio-astronomy
Antenna power pattern, solid angles, associated efficiencies
Source and observed flux density
Observed brightnesses
Basic relation between received spectral power and sky brightness
Brightness temperature
Effective aperture and aperture efficiency
Relationship between effective aperture and antenna solid angle