Discussion: Examples of the time series are shown in Figure 2. Images of Active Galactic Nuclei (AGN) sources generally become more compact with increasing frequency, as shown in Figure 3. It has often been assumed that VLBI source positions, as determined by measuring the source’s VLBI phase center, should be more stable at higher frequencies. This is the assumption we are testing with these comparisons. But we find that these comparisons are difficult to make and interpret due to the different nature of the X/S and K sessions and the different networks used. The X/S and K VLBA astrometry sessions mostly look at different sources. The IVS X/S R1, R4 and RDV/RV sessions have larger networks than the VLBA, particularly with better North-South extent and with baselines crossing the equator, leading to smaller declination uncertainties and less asymmetry. However, the East- West coverage of the IVS networks vs the VLBA are not so different, and the data gives a slight edge to K band in right ascension in terms of WRMS scatter. There is no reason to expect that the true average source position variability would be systematically greater in declination than right ascension and there is also no reason to expect that the true average source position variability would increase from the northern to the southern part of the sky. Therefore we attribute the larger WRMS scatter for K band in declination to be a network effect and we believe the indication is that the true position variability is less at K band than at X/S band. Figure 3: Near-simultaneous images of NRAO140/J0336+3218 at S (2.3 GHz), X (8.6 GHz), K (24 GHz) and Q (43 GHz) bands from a study of VLBA observations of 453 ICRF sources from April - June 2021 (Hunt et al, 2022, de Witt et al, 2022), which shows that VLBI images of ICRF sources become more compact with increasing frequency. Note how the jet in this example fades with increasing frequency. The VLBA synthesized beam is shown as the grey ellipse in each sub-figure. Conclusion: Sources do appear to be more stable at K than X/S band, on average. However our ability to measure and quantify this is limited by network differences and the limited amount of overlapping source data at the two bands. Acknowledgements: The authors acknowledge use of the Very Long Baseline Array under the US Naval Observatory's time allocation. This work supports USNO's ongoing research into the celestial reference frame and geodesy. The VLBA is operated by the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. K vs X/S comparisons: Both the X/S and K band data required some additional editing to remove positions that were very noisy or where there were too few observations in the session. For a source to be used we required that it be in at least 10 sessions with at least 10 observations in each session and have uncertainties of no more than 1.0 milli-arc-second (mas) in each session. Then, two methods were used to estimate the scatter for each source in each band. In the first method, weighted root mean squares (WRMS’s) about the mean of each source’s position were computed in RA and declination using the RA and declination formal errors for weighting. The WRMS’s of 417 common sources were then compared. Itn this method, ~56% of the sources exhibit less scatter in RA, but only ~36% exhibit less scatter in declination at K band. In the second method, a more complicated procedure was used to compute WRMS’s about the means by using the full covariance matrix for each session, but the results are similar. In this method, ~60% of the sources show less scatter in RA but only ~34% show less scatter in declination at K band. We show this graphically in Figure 1 for the second method where the logarithm of the ratio of the WRMS’s at K vs X/S is plotted vs declination for each matched source. Values greater than zero indicate less scatter in