2005A&A...444..319H

The ``Synthetic Field Method'' (SFM) was introduced by Gonzalez et al. (1998ApJ...506..152G) to calibrate numbers of distant galaxies as a probe of extinction in a foreground spiral disk. Gonzalez et al. (2003AJ....125.1182G) studied the effect of the foreground disk on these numbers using simulations of current and future instruments for fields in the LMC, M31 and NGC 4536, a galaxy in Virgo. They concluded that: (1) the brighter centers of disks were unsuitable; (2) the granularity of the disk at a fixed surface brightness is the limiting factor in the detection of distant galaxies; and (3) the optimum distance for measurements would be that of the Virgo cluster for the current instruments on board HST. At this distance the foreground disk is smoothed with distance, improving detection of distant background galaxies. Holwerda et al. (2005AJ....129.1381H) automated the SFM and Holwerda et al. (2005AJ....129.1396H) applied it to a large set of WFPC2 fields. In this paper, the quality of the extinction measurement in these fields is compared to their distance, granularity, surface brightness and structure. The average surface brightness of the of a field is shown to directly influence the accuracy of the SFM. This restricts meaningful measurements to the disks of spiral galaxies. Large structures such as spiral arms have a similar effect. The granularity or small scale structure in a field influences the detection of distant galaxies, limiting the SFM measurements in nearby disks. From the trends in the accuracy and maximum practical field-of-view considerations, the minimum and maximum distance for SFM application, approximately 5 and 35Mpc respectively. Using the same instrument and detection method, the relations with SFM parameters and field characteristics can be used to forgo the synthetic fields altogether. For the wealth of ACS fields becoming available in the archive, these relations can be used to select those fields based on expected SFM accuracy.