ra769_calculate_entry

pycraf.protection.ra769_calculate_entry(frequency, bandwidth, T_A, T_rx, mode='continuum', scale='dB', integ_time=<Quantity 2000. s>)

Limits (single entry) for spectral line, continuum, and VLBI observations according to ITU-R Rec RA.769.

Parameters:

frequencyQuantity

Center frequency [Hz]

bandwidthQuantity

Assumed bandwidth [Hz]

Note, if mode='vlbi' the bandwidth is irrelevant, since only the spectral power flux density is calculated.

T_AQuantity

Minimum antenna noise temperature [K]

T_rxQuantity

Receiver noise temperature [K]

modestr, optional

Observing mode: ‘continuum’, ‘spectroscopy’, or ‘vlbi’ (default: ‘continuum’)

scalestr, optional

Default scale to use: ‘linear’, ‘dB’ (default: ‘linear’)

integ_timeQuantity, optional

Integration time [s] (default: 2000)

Note, if mode='vlbi' integration time is irrelevant, because the limits are based on 1% of the receiver noise plus antenna temperature.

Returns:

T_rmsQuantity

System noise after integration [K]

P_rms_nuQuantity

System noise power spectral density [W/Hz, dB(W/Hz)]

PlimQuantity

Power limit [W, dB(W)]

Plim_nuQuantity

Spectral power limit [W/Hz, dB(W/Hz)]

SlimQuantity

Power flux density (pfd) limit [W/m^2, dB(W/m^2)]

Slim_nuQuantity

Spectral power flux density limit [Jy, dB(W/m^2/Hz)]

EfieldQuantity

Electrical field strength limit [uV/m, db(uV^2/m^2)]

Efield_normQuantity

As Efield but normalized to 1 MHz bandwidth [uV/m, db(uV^2/m^2)]

Note, if mode='vlbi' only Slim_nu is returned.

Notes

Because all columns are Astropy Quantities (see Quantity), one can easily convert between linear and log-scale at a later stage. the scale parameter just defines the scale to use initially.