The W Lacertae field is another one that Charles Scovil asked me to observe about four years ago, but which I haven't got around to until now. I worked from an (e)-scale chart (10"/mm) he supplied that was last revised in April 1978 and whose sequence is based largely on visual estimates. I observed the six selected stars below on 13 and 16 October 1996 UT using the Lowell 53cm photometric telescope with a 19-arcsec diaphragm and Stromgren b and y filters. About a dozen standards were observed on each night whose rms residuals were between 0.004 and 0.007 mag. in V and b-y. The AAVSO preliminary magnitudes have a consistent and significant zero-point error, amounting to 0.3-0.5 mag. (AAVSO too bright). The sequence is unfortunately rather widely spaced in brightness because several of the comp stars marked on the chart are pairs, and there were no suitable replacements. The stars "91" (BD+36 4767), "108" (GSC 3198-1622), and "106" (GSC 3198-1470, actually V=11.1) are all readily visible double stars. Using the 19-arcsec aperture, I was able to measure the last star without interference from the faint companion. There is also the wide pair Ali 696, indicated on the chart near the variable itself. The few remaining single stars will be entirely adequate for CCD use, but visual observers will find it inconvenient. (sorry guys!) In regard to W Lac itself, it is identifiable as IRAS 22053+3729 and also GSC 3198-1060 at: 22 07 29.9 +37 44 07 (2000). Keenan et al. (1975 ApJ Suppl. 28,271) give a spectral type of M8-e, obtained on 12 July 1968, apparently near maximum light. Photometry of stars in the field of W Lacertae Name RA (2000) Dec V b-y n spec BD+36 4769 22 08 53.3 +37 39 34 9.296 0.653 2 K2 .000 .011 GSC 2732-0698 22 07 38.7 +37 29 38 10.199 0.383 2 .013 .007 GSC 3198-1470 22 07 39.9 +37 54 55 11.126 0.540 2 .004 .001 AG+37 2188 22 07 19.5 +37 43 25 12.327 0.341 2 .021 .008 GSC 3198-1366 22 07 12.1 +37 42 39 13.00 0.46 1 .03 .04 GSC 3198-1646 22 07 12.8 +37 43 41 13.79 0.75 2 .07 .07 \Brian Skiff (bas@lowell.edu)