a  Proper motion calculated from apparent velocity data in the reference.
b  Map by Cawthorne et al. (1993ApJ...416..496C) agrees with same proper motion.
c  Measurement is consistent with earlier 6cm map by Preuss (1983, in 
c   Astrophysical Jets, ed. A. Ferrari & A.G. Pacholczyk (Dordrecht: Reidel), 1)
d  Redshift from C. Lawrence, private communication.
e  Only an upper limit to the proper motion is available.
f  Also called 0235+285.
g  Redshift from Richstone & Schmidt (1980ApJ...235..361R).
h  Inner component.
i  Consistent data exist at other wavelengths.
j  Redshift from Burbidge & Strittmatter (1972ApJ...174L..57B).
k  Double model from data taken in 1973-74. No optical identification.
l  Error from K.I. Kellermann, private communication.
m  Redshift from Sargent (1977ApJ...212L.105S).
n  An error estimate is not available.
o  Most of the points are at 6 cm.
p  Motion also published as upper limit by Schalinski et al. (1992, in 
p   Variability of Blazar, ed. E. Valtaoja & M. Valtonen (Cambridge: Cambridge 
p   Univ. Press), 225
q  Strong intraday variability has been observed, see Quirrenbach  et al.
q   (1992A&A...258..279Q).
r  Conway et al., (1990, in compact Steep-Spectrum and GHz-peaked Spectrum
r   Radio Sources, Ed, C. Fanti, C.P. O'Dea & R.T. Schilizzi (Bologna: CNR 
r   Instituto di Radioastronomia), 157) say component is "static". Variable 
r   structure between 2 stationary components may have led to earlier report of 
r   {mu}=-0.13+-.02 in Readhead et al. (1984, in VLBI and compact Radio Sources,
r   Proc. IAU Symp. 110, ed. R. Fanti, K. Kellerman & G. Setti (Dordrecht: 
r   Reidel), 131). See also Cawthorne et al., (1993ApJ...416..496C) .
s  This object has no redshift.
t  Absorption redshift, lower limit to emission redshift.
u  Proper motion is an average of 2 values in the reference.
v  See also the single-epoch results at 1.3cm by Baath, Zhang, & Shu 
v   (1991A&A...250...50B).
w  Redshift from Stickel & Kuhr (1993, Cat. <J/A+AS/100/395>).
x  0.0 is the fitted value for proper motion.
y  Upper limit is not directly stated by authors but can be inferred from their 
y   discussion.
z  Proper motion is weighted fit to four positions, but first position may be 
z   affected by blending; deceleration cannot be ruled out.
aa Possible deceleration in fourth epoch. See Simon et al. (1988IAUS..129...21S)
bb Redshift from Phillips (1977ApJ...215..746P).
cc Consistent data exist at 1.3 and 2.8cm.
dd Redshift is average of values in Lynds (1967ApJ...147..837L) and Burbidge & 
dd  Kinman (1966ApJ...145..654B).
ee Component 7a is considered as component 7 at later epochs (Cohen et al.
ee  1987ApJ...315L..89C, Zensus et al., 1990AJ....100.1777Z).
ff Redshift from an assumed distance of 20Mpc, with H_0_=60km/s/Mpc.
gg Measurements from 1970-72 with a two-element interferometer; amplitudes 
gg  modelled with a double.
hh Redshift is average of values in Lynds et al. (1965ApJ...142.1667L) and 
hh  Burbidge & Rosenberg (1965ApJ...142.1673B).
ii Gabuzda et al. (1993ApJ...410...39G) suspect that this high luminosity object
ii  might be a quasar rather than a BL Lac object.
jj Redshift from an assumed distance of 4Mpc, with H_0_=60km/s/Mpc.
kk Proper motion errorbar given in Meier et al. (1993, in Subarcsecond Radio 
kk  astronomy, ed. R.J. Davis & R.S. Booth (Cambrige: Cambridge Univ. Press), 
kk  201 is misprint (Meier, priv.com.)
ll Proper motion error represents range of quoted values in northern jet.
mm Proper motion is our fit to positions at 2 epochs given by Jones 
mm  (1986ApJ...309L...5J).
nn Redshift from Wagget et al. (1977MNRAS.181..465W).
oo Proper motion is weighted combination of values given by Biretta et al.
oo  (1986ApJ...308...93B).
pp Component appeared to accelerate in 1982. Values are for the 
pp  post-accelaration motion.
qq Possible acceleration.
rr Tentative redshift, based on one emission line (Stickel et al., 1989,
rr  Cat. <III/175>).
ss Cawthorne et al. (1993ApJ...416..496C) report {mu}~0.15mas/yr.
tt Upper limit is at 3.6cm; higher limit known at 6cm. Evidence exists for 
tt  structural variations close to core.
uu Earlier sequence suggested different motions (Wilkinson et al., 1990, in 
uu  Parsec-Scale Radio Jets, ed. J.A. Zensus & T.J.  Pearson (Cambridge: 
uu  Cambridge Univ. Press), 152), which are in turn not supported by a map at 
uu  intermediate epoch of Cawthorne et al. (1993ApJ...416..496C). Motion and 
uu  brightness changes may be hard to disentangle.
vv We adopted proper motion and error from Polatidis et al (1993, in 
vv  Subarcsecond Radio astronomy, ed. R.J. Davis & R.S. Booth (Cambrige: 
vv  Cambridge Univ. Press), 225); neither their stated {beta}_app_ nor its 
vv  stated error are obtained for their stated cosmology.
ww Hybrid map compared to model from early data. Error determined by us from 
ww  quoted position errors.
xx Baath (1987) measured a faster velocity at 966MHz.
yy Motion measured with respect to component B1.