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2.2 Flux Reproducibility for Point Sources

The following Table 2.3 provides the flux reproducibility both for bright and faint sources. The bright source was measured in standard off-on mode, while the faint sources were measured in optimised faint source observing modes: telescope nodding for PHT-P and mini-map for PHT-C.

The flux reproducibility, a relative photometric accuracy, is not only determined by the detector stability, but also, in particular for wavelengths m by the structure of the sky background, since, due to the rotation of the focal plane on the sky, different background fields are seen at different times.

 

Table 2.3:   1 Flux Reproducibility per Detector for Bright and Faint Fluxes from Monitoring Programs. For the wavelength range of the detector system, please refer to Table 1.1.

	detector	target	flux	standard deviation	no. of meas.
				1
			[Jy]	[%]
	P1	NGC 6543	8	5	15
	P1	HD 172323	0.085	10	23
	P2	NGC 6543	100	2	14
	P2	HR 5986	0.67	12	15
	P3	NGC 6543	100	7	15
	P3	HR 7310	0.67	7	15
	C100	NGC 6543	50	3	15
	C100	HR 7310	0.23	20	23
	C200	NGC 6543	15	10	15
	C200	HR 6705	0.67	7	23