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\begin{document}
\IBVShead{4250}{25 September 1995}

\title{A New Variable in the field of V778 Cygni}

\begintext

Observations of the V778 field in Cygnus indicate 
a possible new variable star.  The coordinates of this from
the Guide Star Catalog are
$\alpha_{2000}=20^{\rm h}36^{\rm m}34^{\rm s},
 \delta_{2000}=60\degr 06'45''$. The star is not listed as a variable in 
the General Catalog of Variable Stars (Kholopov {\it et al}., 1985), the New 
Catalog of Suspected Variable Stars
 (Kholopov {\it et al}., 1982), the 72nd Name-List of Variable Stars
(Kazarovets and Samus, 1995) or SIMBAD; nor has a reference to it appeared
in the IBVS bulletins during 1994-1995.  Thus, we conclude the star has not 
previously been noted as a variable.
The V magnitude of the star is about 12.9 from the Guide Star
Catalog, and the star appears to be redder than V778 Cygni.

In 1993, observers at Wellesley College began observations of V778 Cygni
 to determine its photometric behavior,
using a 0.6 meter telescope with a Photometrics CCD camera.
   One of the comparison stars used in this analysis exhibits larger
variations in its magnitude than other comparisons.  

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Figure 1: Light curves of a new variable in the V778 Cyg field
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Figure 2:  A finder chart for the new suspected variable star.  North is
up and East is left.  The field shown is approximately nine arcminutes
per side.
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\noindent
As shown in Figure 1, the amplitude of the variation of the new variable
with respect to a comparison
is approximately 0.6 magnitudes in V and R and 0.3 magnitudes in I.  In
contrast, the amplitude of the differential magnitude of the two comparisons 
in V, R, and I is
0.04 magnitudes, 0.16 magnitudes, and 0.13 magnitudes respectively.
Figure 2 identifies the new variable.

Upon discovery of the new variable, we examined the star for
periodicity.
No significant periodicity for periods between 0.001 and 1000
days was found using a Fourier transform period fitting program
written by Charles Prosser at Harvard Center for Astrophysics.  
Subsequent observations of the star indicate that it does not change in
magnitude
significantly during one night's observing. 

Acknowledgements:
We thank the W. M. Keck Foundation for a summer internship (ER) and support
of astronomy at Wellesley College through the Keck Northeast Astronomy
Consortium.  This research was also partially supported by funds from the
National Science Foundation (through AAS/REU and AST9417359), 
the Dudley Observatory, and
a Bunting Science Fellowship funded through the Office of Naval Research.
This research has made use of the Simbad database operated at CDS,
Strasbourg, France.

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\beginauthors
ERIK ROSOLOWSKY
Swarthmore College
Swarthmore, Pennsylvania
19081, USA
[email: eros1@sccs.swarthmore.edu]
\authorsrightcol
PRISCILLA BENSON
Wellesley College
Wellesley, Massachusetts
02181, USA
[pbenson@wellesley.edu]                           %email
\vskip 2mm
\endauthors

\references
Kazarovets, E.V. and Samus, N.N., 1995, {\it IBVS},  No.\,4014

Kholopov, P.N., 1985, {\it General Catalog of Variable Stars}, Moscow

Kholopov, P.N., 1982, {\it New Catalogue of Suspected Variable Stars}, 
Moscow

Space Telescope Science Institute, 1992, {\it The Guide Star Catalog v1.1},
Baltimore

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