  We applied our earlier numerical method to compute the thermal emission from
a dusty resonant structure around Vega and compared the new observational
evidence for a ring arc at 95 AU near Vega with our modeling. Our high
resolution simulations indicate that Vega may have an outerm ost planet at a
distance of 90-100 AU with coordinates near 18 35'16.25" (right ascension,
B1950) and 38 44'15" (declination). Another symmetrical position, 18 35'14.75"
and 38 44'32.5", of the planet is also possible. Radii of the observed clumps
(and planet's orbital radius) may be smaller, e.g. ~60-75 AU. In this case the
planet stays approximately on the line between the two possible positions
above. From our modeling we make following conclusions: 1.Dust clumps rotate
around Vega exactly wi th the planet orbital speed, 0.6-1.2 deg/year, as
function of orbital radius of parent planet. 2. Orbital radius of the planet is
approximately the same as the orbital radius of clumps (90-100 AU from
observation by Koerner, Sargent & Ostroff, 2001 or 60-75 AU from observation by
Wilner, Holman, Ho & Kuchner, 2002). 3. The most dense clump is ahead of the
planet in the direction of the orbital motion. 4. The orbit of the planet may
be circular or with a small eccentricity. 5. Absence of dust i n the inner part
of Vega planetary system is a signature of inner planet(s) with orbital radii
<50-60 AU.
