## Appendix FFCFs by Time of Night

Figure F.1 shows the Beam (Peak) FCFs at 450 and 850 $\mu$m as a function of UT time for observations of the primary calibrator, Uranus along with secondary calibrators CRL 2688, and CRL 618. The Peak FCF is larger in the evening and morning primarily because thermal deformations of the dish dilute the flux from the main beam into the secondary (error) component (see Mairs et al. 2021 [16]). There is no significant change to the Arcsecond FCFs in the early evening or late morning.

Figure F.2 show the Peak FCF trends in detail for evening and morning observations of Uranus and CRL 2688. The data are bootstrap-fitted with linear functions and “rs” indicates the Spearman rank correlation of the fit.

The Peak FCFS DECREASE in the evening as the ambient temperature cools and the dish settles, while the Peak FCFS INCREASE in the morning as the ambient temperature warms and the dish becomes unstable to thermal gradients. Table F summarises the rate of change. As of Starlink Release 2021A, Orac-dr does not apply these corrections by default. If you wish to apply these corrections, the FCFs must be modified manually (see Section 8.1.3).

 Wavelength Time Range (UTC) Peak FCF Correction (% hr${}^{-1}$) $450\phantom{\rule{0.3em}{0ex}}\mu$m 03:00–07:00 $9.1±0.5$ $450\phantom{\rule{0.3em}{0ex}}\mu$m 17:00–22:00 $7.2±0.6$ $850\phantom{\rule{0.3em}{0ex}}\mu$m 03:00–07:00 $3.2±0.1$ $850\phantom{\rule{0.3em}{0ex}}\mu$m 17:00–22:00 $3.1±0.1$